# GCN_circulars

GRB_name: GRB130515A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14670
SUBJECT: GRB 130515A: Further Gemini Observations
DATE:    13/05/16 23:23:55 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (UC Berkeley) and A. Cucchiara (UCSC) report on behalf of a
larger collaboration:

We re-imaged the field of GRB 130515A (Malesani et al., GCN 14650) with
the Gemini Multi-Object Spectrograph mounted on the 8 m Gemini South
telescope.  Images were obtained in the r' filter beginning at 4:38 UT on
2013 May 16 (~ 1.1 days after the Swift trigger).

Comparing with our previous epoch of observations (Cenko et al., GCN
14656), we find no evidence for variability in or around the enhanced XRT
error circle (Beardmore et al., GCN 14654).  Specifically, we note that
the three sources S1, S2, and S3 identified previously (Xu et al., GCN
14653, Schmidl et al., GCN 14655, Levan et al., GCN 14677) all maintain a
constant brightness level.  Using digital image subtraction, we limit the
optical afterglow at the time of our first epoch of observations (~ 38 min
after the Swift trigger) to be R > 23.7 mag (calibrated with respect to
nearby USNO-B1 point sources).

We thank the Gemini staff for the prompt execution of these observations.


GRB_name: GRB130515A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14671
SUBJECT: GRB 130515A: IRSF NIR Observation
DATE:    13/05/17 08:07:22 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

Takahiro Nagayama (Nagoya Univ.) and Shogo Nishiyama (NAOJ)
on behalf of OISTER collaboration.

We observed the field of GRB 130515A (David Palmer, GCN Circular
14650) with the Infrared Survey Facility 1.4m telescope and
NIR camera SIRIUS (Nagayama et al., 2003) at Sutherland Observatory
in South Africa.

The observation was made with the JHKs bands simultaneously
from 2013-05-15 01:26 (UT), 5 minutes after the BAT trigger, to 04:41.

We have also detected the source detected by VLT (Dong Xu, GCN
Circular 14653) and  GROND (Sebastian Schmidl, GCN Circular 14650)
at RA=18:53:45.79, DEC=-54:16:47.1 (J2000). Preliminary photometry
results are as follows

All combined images
(Total exposure time: 154 min, 2013-05-15 01:26 - 04:41)
 J = 20.1 $B!^(B 0.2
 H = 18.6 $B!^(B 0.2
 Ks =18.7 $B!^(B 0.3

First 120 images
(Total exposure time: 60 min, 2013-05-15 01:26 - 2:45)
 J = 19.4 $B!^(B 0.2
 H = 18.9 $B!^(B 0.2
 Ks: Non detection

These magnitudes are in the Vega system and not corrected for
Galactic extinction in the direction of the GRB.


GRB_name: GRB130427A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14672
SUBJECT: GRB 130427A: Konkoly optical observations 
DATE:    13/05/18 19:56:36 GMT
FROM:    Janos Kelemen at Konkoly Obs/Hungary  <kelemen@konkoly.hu>

J. Kelemen (kelemen at konkoly.hu) on behalf of the GRB OT observing program
at the Konkoly Observatory.

Starting on the evening of 15/05/2013 we observed the field of GRB 130427A
(Maselli et al., GCN 14448) 18.5435 days after the burst, using a 60/90/180 cm
Schmidt telescope located at the Mountain Station of the Konkoly
Observatory equipped with an Apogee CCD camera through R filter. On the coadded 
R images (total exp.time 1120 sec) we detected the OT and the host galaxy as
well. 
Based on the nearby UCAC-4 stars we provide 20.90 +/- 0.05 magnitude in the R
band for the OT. The brightness of the host galaxy was not subtracted. 

time from GRB    exp    filter     Mag.       

18.5435        1120 s     R       20.9 +/-0.05


GRB_name: GRB130427A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14673
SUBJECT: VLT observations of GRB 130427A
DATE:    13/05/18 20:47:44 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

A. Melandri (INAF-OAB), V. D'Elia (ASDC), P. D'Avanzo (INAF-OAB), M.  
Della Valle (INAF-OAC), E. Pian (INAF-OAT/SNS), G. Tagliaferri (INAF- 
OAB) on behalf of a larger collaboration report:

We have observed the field of GRB 130427A (Maselli et al., GCN 14448)  
for 9 epochs from t-t0=6.7 to t-t0=18.8 days after the burst event.   
The preliminary light curve in BVR and I bands does not show any  
evidence of a bump related to a SN, and it is marginally consistent  
with a SN component, which should be at least 2 mag fainter than 98bw  
at maximum.

The spectrum (2x1800s) of 13 May, after comparison with SN2010bh  
template, is suggestive, in the range 5000A-7500A of broad GRB-SN  
features, but altogether, we don't find the good similarity that the  
GTC finds (de Ugarte-Postigo et al., CBET 3529). The spectrum of the  
transient (after subtraction of a galaxy template) is available at:

http://www.brera.inaf.it/utenti/davanzo/grb/GRB130427A/GRB130427A.png

Observations have been taken in the framework of the ESO-Program  
091.D-0291 (PI E. Pian).


GRB_name: GRB130518A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14674
SUBJECT: GRB 130518A: Fermi GBM detection
DATE:    13/05/18 20:52:02 GMT
FROM:    Shaolin Xiong at UAH  <sx0002@uah.edu>

Shaolin Xiong (UAH) reports on behalf of the Fermi GBM Team:

"At 13:54:37.53 UT on 18 May 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130518A (trigger 390578080 / 130518580).

High peak flux from the GRB caused GBM to issue a repoint request,
but the spacecraft did not slew to this burst due to the Solar TOO.

The on-ground calculated location, using the GBM trigger
data, is RA = 355.88, DEC = 46.05 (J2000 degrees,
equivalent to 23 h 43 m, 46 d 03 '), with an uncertainty
of 1 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).
The angle from the Fermi LAT boresight is 43 degrees.

The GBM light curve consists of several pulses
with a duration (T90) of about 48 s (50-300 keV).
The time-averaged spectrum from T0+10 s to T0+60 s is
adequately fit by a Band function with Epeak = 396 +/- 9 keV,
alpha = -0.86 +/- 0.01, and beta = -2.27 +/- 0.04.

The event fluence (10-1000 keV) in this time interval is
(9.3 +/- 0.06)E-5 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+25.6 s in the 10-1000 keV band
is 45.4 +/- 0.4 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB130518A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14675
SUBJECT: GRB 130518A: Fermi LAT detection
DATE:    13/05/18 21:02:32 GMT
FROM:    Julie McEnery at NASA/GSFC  <julie.e.mcenery@nasa.gov>

Nicola Omodei (Stanford) and Julie McEnery (GSFC) report on behalf of 
the Fermi-LAT team:

At 13:54:37.53 UT on 18 May 2013, Fermi LAT detected high energy 
emission from GRB 130518A, which was also detected by Fermi-GBM (trigger 
390578080 /130518580, GCN 14674).

The best LAT on-ground location is found to be RA=355.809, DEC=47.641 
(J2000) with an error radius of 0.34 deg (68% containment, statistical 
error only).

The burst was about 43 deg from the LAT boresight at the time of the 
trigger.
The data from the Fermi LAT shows emission lasting approximately 100 
seconds with a TS of 50.
Multi-peaked emission lasting roughly 40 seconds can be seen using the 
non-standard LAT Low Energy (LLE) with a significance of ~15 sigma.

A Swift TOO request has been submitted.

The Fermi LAT point of contact for this burst is Sara Cutini 
(sara.cutini@asdc.asi.it).

The Fermi LAT is a pair conversion telescope designed to cover the 
energy band from 20 MeV to greater than 300 GeV. It is the product of an 
international collaboration between NASA and DOE in the U.S. and many 
scientific institutions across France, Italy, Japan and Sweden.


GRB_name: GRB130518A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14676
SUBJECT: GRB 130518A Swift-BAT position from ground analysis
DATE:    13/05/19 00:04:25 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings (UMBC/CRESST/GSFC) reports on behalf of the BAT team


At 13:55:07.4 UT, the Swift Burst Alert Telescope (BAT) triggered on the
Fermi GBM and LAT GRB 130518A (Xiong, GCN # 14674 and Omodei et al., GCN#
14675) (BAT trigger=556113).  No significant source was found onboard.  In
ground analysis, a significant source was found at RA, Dec 355.671, +47.478
which is:
    RA(J2000)  =23h 42m 41.1s   
    Dec(J2000) = +47d 28' 41.5"
with an uncertainty of 2.9 arcmin (radius, 90% containment, including
systematic uncertainty).  This position is 11 arcmin from the LAT position,
within the LAT error circle.  BAT partial coding was 5%.  The unweighted
lightcurve shows two overlapping peaks with a duration of about 14 sec.
The peak count rate was ~9400 counts/sec (15-350 keV), at ~4 sec before the
trigger.


GRB_name: GRB130518A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14677
SUBJECT: Konus-Wind observation of GRB 130518A
DATE:    13/05/19 13:50:14 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf
of the Konus-Wind team, report:

The long-duration intense GRB 130518A
(Fermi-GBM detection: Xiong, GCN 14674;
Fermi-LAT detection: Omodei and Julie McEnery, GCN 14675;
Swift-BAT trigger 556113: Cummings, GCN 14676)
triggered Konus-Wind at T0=50097.501s UT (13:54:57.501)
against very high and variable solar particles background.

The light curve shows a bright hard pulse from ~T0-10 s to ~T0+20s,
followed by a weaker count rate increase at ~T0+33s
and a tail of soft extended emission, which is traceable out to ~T0+100s.

The emission in the main pulse is seen up to 12 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130518_T50097/

As observed by Konus-Wind, the burst
had a fluence of (1.5  0.15)x10-4 erg/cm2,
and a 64-ms peak flux, measured from T0+1.856s,
of (2.1  0.2)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+20.224 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.92  0.08,
the high energy photon index beta = -1.97  0.08,
the peak energy Ep = 370  55 keV,
chi2 = 85/94 dof.

The spectrum at the maximum count rate
(measured from T0+0.768 to T0+2.304 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.80  0.09,
the high energy photon index beta = -2.04  0.11,
the peak energy Ep = 452  72 keV,
chi2 = 95/97 dof.

For both spectra, we note a hint of counts excess
over the model flux in the spectral channels around ~10 MeV.

All the quoted results are preliminary.


GRB_name: GRB130518A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14678
SUBJECT: GRB 130518A: Swift XRT and UVOT possible afterglow
DATE:    13/05/19 16:05:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans (U.Leicester), M. de Pasquale (MSSL/UCL), M.C. Stroh (PSU)
and M. H. Siegel (PSU) report on behalf of the Swift team:

Swift conducted a series of observations, tiled on the sky, of the
Fermi/LAT GRB 130518A. In these observations we find an uncatalogued
source at RA,Dec = 355.6658, +47.4653 degrees (J2000) which is
equivalent to:

RA(J2000) =    23h 42m 39.79s
Dec (J2000) = +47d 27' 55.2"

with an uncertainty of 3.6 arcsec (radius, 90% confidence).

This source shows weak evidence of fading: a power-law fit gives a decay
index of 0.66 (+/- 0.80); at this level we therefore cannot confirm
whether this is the afterglow of GRB 130518A.

The spectrum of this source can be fitted with an absorbed power-law
with a spectral index of 2.5 (+0.8, -0.6). The best-fitting absorption
column is 2.4 (+2.2, -1.4) x 10^21 cm^-2, consistent with the Galactic
value of 1.0 x 10^21 cm^-2 (Kalberla et al., 2005).

UVOT observed the field of the XRT source in u filter between 30.5 ks
and 59.9 ks after the trigger, for a total exposure time of 2.7 ks. We
detect an optical object with magnitude  u = 19.0  0.1 just outside the
3.6 arcsec XRT error circle. The source shows weak indication of  fading
between the beginning and the end of observations.

This circular is an official product of the Swift team.


GRB_name: GRB130518A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14679
SUBJECT: GRB 130518A: RATIR Optical and NIR Observations
DATE:    13/05/19 17:59:08 GMT
FROM:    Eleonora Troja at GSFC  <eleonora.troja@nasa.gov>

Eleonora Troja (GSFC), Nat Butler (ASU), Alan M. Watson (UNAM),
Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM),
Chris Klein (UCB), Ori Fox (UCB) J. Xavier Prochaska (UCSC), Josh Bloom
(UCB), Antonino Cucchiara (UCSC), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), Jos A. de Diego (UNAM), Leonid Georgiev (UNAM),
Jess Gonzlez (UNAM), Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC),
and Harvey Moseley (GSFC) report:

We observed the field of GRB 130518A (Xiong, et al., GCN 14674; Omodei,
et al., GCN 14675) with the Reionization and Transients Infrared Camera
(RATIR;www.ratir.org) on the 1.5m Harold Johnson Telescope at the
Observatorio Astronmico Nacional on Sierra San Pedro Mrtir from
from 2013/05 19.44 to 2013/05 19.47 UTC (20.54 to 21.49 hours after
the GBM trigger), obtaining a total of 0.64 hours exposure in the r'
and i' bands, 0.27 hours exposure in the Z and Y bands, and 0.15 hours
exposure in the J, and H bands.

We detect a new, uncatalogued source at RA,Dec = 355.66781, +47.46493
(J2000) with an uncertainty of 0.5 arcsec.
This position is 5 arcsec from the XRT localization, just outside the
XRT error circle (Evans, et al., GCN 14678). In comparison with SDSS DR8
and 2MASS, we obtain the following detections:

     r'    19.38  0.02
     i'    19.10  0.02
     Z     18.83  0.04
     Y     18.65  0.04
     J     18.28  0.07
     H     18.47  0.11

These magnitudes are in the AB system and not corrected for Galactic
extinction in the direction of the GRB. We have evidence at the 2-3 sigma
level of fading in r' and i' over the duration of our observations.

Further observations are planned.

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB130518A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14680
SUBJECT: GRB 130518A: P60 Afterglow Observations
DATE:    13/05/20 04:03:37 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (UC Berkeley) reports on behalf of a larger collaboration:

We have imaged the location of the Fermi GBM (Xiong et al., GCN 14674),
LAT (Omodei et al., GCN 14675), Swift BAT (Cummings et al., GCN 14676),
and Konus-Wind (Golenetskii et al., GCN 14677) GRB 130518A with the
robotic Palomar 60 inch telescope.  Observations were obtained in the r'
and i' filters beginning at 10:24 UT on 2013 May 19 (~ 0.85 d after the
GBM trigger).

We detect the optical afterglow (Evans et al., GCN 14678; Troja et al.,
GCN 14679) in both filters.  Using several nearby point sources from SDSS
for calibration, we measure a magnitude of r' = 19.3 at this time.


GRB_name: GRB130518A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14681
SUBJECT: GRB 130518A: Confirmation of the X-ray afterglow.
DATE:    13/05/20 09:05:11 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans (U.Leicester), M.C. Stroh (PSU) and M. H. Siegel (PSU) report
on behalf of the Swift-XRT team:

Swift has performed a second observation of GRB 130518A. We collected
1 ks of data, starting 122.5 ks after the Fermi trigger (Xiong, GCN
Circ. 14674; Omodei & McEnery, GCN Circ. 14675). The XRT source reported
by Evans et al. (GCN Circ. 14678) is detected at a level of 0.013 Â±
0.005 ct/sec, significantly below the level in the previous
observations, confirming that it has faded. The best-fitting power-law
decay index is 1.1 (+0.5, -0.3).

We therefore conclude that this object is the afterglow of GRB 130518A.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB130518B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14682
SUBJECT: GRB 130518B found in ground analysis of Swift-BAT data
DATE:    13/05/20 14:04:04 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings (UMBC/CRESST/GSFC) reports on behalf of the Swift-BAT team:

At 10:50:38 UTC, Swift-BAT triggered on GRB 130418A (trigger # 556105).  A
sub-threshold source was found onboard.  In ground analysis, a source was
confirmed at RA, Dec 321.555, -20.148, which is:

RA (J2000)    21h 26m 13.2s
Dec (J2000)  -20d 08m 53s

with an estimated uncertainty of 1.8 arcmin radius (90% confidence).

The burst as seen in BAT was a single FRED peak of approximately 15 seconds
duration.

A Swift TOO request has been submitted and approved to locate the afterglow.


GRB_name: GRB130518B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14683
SUBJECT: Correction to GCN Circular 14682 (GRB 130518B)
DATE:    13/05/20 14:31:30 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

J. R. Cummings (UMBC/CRESST/GSFC) and H. A. Krimm (USRA/CRESST/GSFC) report on 
behalf of the Swift-BAT team:

In the first sentence of GCN Circular 14682 (Cummings), we incorrectly named the 
GRB.  The burst that provided Swift/BAT trigger #556105 should be named GRB 
130518B, consistent with the subject line.  We apologize for any confusion.


GRB_name: GRB130518A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14684
SUBJECT: GRB 130518A: Continued RATIR Optical Observations - Fading
DATE:    13/05/20 15:30:09 GMT
FROM:    Eleonora Troja at GSFC  <eleonora.troja@nasa.gov>

Eleonora Troja (GSFC), Nat Butler (ASU), Alan M. Watson (UNAM),
Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM),
Chris Klein (UCB), Ori Fox (UCB) J. Xavier Prochaska (UCSC), Josh Bloom
(UCB), Antonino Cucchiara (UCSC), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), Jos A. de Diego (UNAM), Leonid Georgiev (UNAM),
Jess Gonzlez (UNAM), Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC),
and Harvey Moseley (GSFC) report:

We again observed the field of GRB 130518A (Xiong, et al., GCN 14674;
Omodei, et al., GCN 14675) with the Reionization and Transients Infrared
Camera (RATIR;www.ratir.org) on the 1.5m Harold Johnson Telescope at
the Observatorio Astronmico Nacional on Sierra San Pedro Mrtir from
2013/05 20.43 to 2013/05 20.46 UTC (44.41 to 45.24 hours after the GBM
trigger), obtaining a total of 0.71 hours exposure in the r' and i' bands.

In comparison with SDSS DR8, we obtain the following detections of the source
reported earlier (Troja, et al., GCN 14678; Cenko, GCN 14680):

r'    20.47  0.04
i'    20.19  0.04

These magnitudes are in the AB system and not corrected for Galactic
extinction in the direction of the GRB.

In comparison with our earlier observations (Troja, et al., GCN 14678), the source
has faded by slightly more than 1 magnitude in r' and i' between about 21 hours
and 45 hours after the trigger. This confirms that the source corresponds to the
afterglow of GRB 130518A.

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB130518A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14685
SUBJECT: GRB 130518A: 10.4m GTC/OSIRIS redshift
DATE:    13/05/20 15:32:04 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

R. Snchez-Ramrez (IAA-CSIC), J. Gorosabel (UPV-EHU, IAA-CSIC), A. J.
Castro-Tirado (IAA-CSIC), J. Cepa and G. Gmez-Velarde (IAC), on behalf of
a larger collaboration, report:

We observed the location of the Fermi GRB 130518A (Xiong et al. GCNC 14674,
Omodei et al. GCNC 14675) -also detected by Swift and Konus (Cummings et
al. GCNC 14676, Golenetskii et al. GCNC 14677)- with the OSIRIS
spectrograph mounted at the 10.4m GTC located at Roque de los
Muchachos Observatory (La Palma, Spain). Observations began on May 20.1995
UT (i.e. 38.9 hr post burst). The optical afterglow (Evans et al. GCNC
14678, Troja et al. GCNC 14579) is well detected with the blue (R1000B)
grism and in the resulting spectrum we see a strong, broad damped-Lya
absorption feature at ~4100A, combined with many metal lines including
SII, SiII, CII, SiIV, CIV, FeII, AlII and AlIII at a common redshift of
z=2.49.

We thank E. Troja and the RATIR Team for providing the ID-chart.

[GCN OPS NOTE(20may13): Per author's request, (a) the "40.9 hr post burst"
was changed to "38.9 hr post burst", and (b) the "We thank E. Troja"
was changed to "We thank E. Troja and the RATIR Team".]


GRB_name: GRB130427A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14686
SUBJECT: GRB 130427A / SN 2013cq: Hubble Space Telescope Observations
DATE:    13/05/20 23:08:33 GMT
FROM:    Andrew S. Fruchter at STScI  <fruchter@stsci.edu>

A.J. Levan (U. Warwick), A.S. Fruchter, J. Graham (STScI), N.R. Tanvir (U. Leicester), Jens Hjorth, Johan Fynbo (Dark Cosmology Centre, Copenhagen), D. Perley (Caltech), S.B. Cenko (U.C. Berkeley), E. Pian (Trieste), Z. Cano (U. Iceland) A. Pe'er (Cork), R. Hounsell (STScI), K. Mishra (ARIES, India), C. Kouveliotou (MSFC) report:

We observed the optical/NIR counterpart of GRB 130427A (Maselli et al. GCN 14448) with the Hubble Space Telescope beginning at 02:23 UT on 20 May 2013. The afterglow is well detected in our multi-band observations in the UV (F336W), optical (F606W) and NIR (F160W) and is offset approximately 0.8" from the optical centroid of its host. The host itself also contains additional star forming complexes including a bright UV source approximately 0.25" from the GRB position.

In the three bands we measure preliminary magnitudes of the afterglow + supernova of

F336W=23.10 +/- 0.02
F606W=21.85 +/- 0.02
F160W=21.34 +/- 0.03

These magnitudes show significant curvature in the optical likely due to the underlying supernova SN 2013cq (de Ugarte Postigo CBET 3529; Xu et al. GCN 14597).    If the optical light were entirely dominated by supernova emission the absolute magnitude at z=0.34 would be M_B~ -19.1 at 17 rest-frame days post burst. However, SNe are weaker UV and IR emitters and so under the naive assumption that the UV and IR bands are dominated by power-law afterglow emission with minimal supernova contribution the inferred magnitude of the supernova in the V-band (rest frame B-band) is V~23. This corresponds to an absolute magnitude of M_B ~ -17.9, approximately a magnitude fainter than the B-band peak of SN 1998bw (which occurred at a comparable epoch of 15 days post burst).     However, the SN could contribute as much as one half of the flux we are seeing in the NIR and UV and there may be substantial host emission underneath the object in the optical and UV.   Thus the SN magnitude should be considered very approximate.  
Images of the field are posted at

http://www.star.le.ac.uk/~anl/GRB130427A

We thank the staff of STScI for their work in rapidly scheduling these observations.


GRB_name: GRB130518A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14687
SUBJECT: GRB 130518A: Gemini Redshift confirmation
DATE:    13/05/21 05:20:33 GMT
FROM:    Antonino Cucchiara at UCSC/UCO Lick  <acucchia@ucolick.org>

A. Cucchiara (UCSC), S. B. Cenko (UC Berkeley) report on behalf 
of a larger collaboration:

"We obtained spectroscopy of the afterglow of the LAT-GRB 130518A 
(Xiong et al. GCN 14674, Omodei et al. GCN 14675, Evans et al. 
GCN 14678) with Gemini-North / GMOS, beginning a May 20.60 UT 
roughly 2.05 days after the burst. 
Two different central wavelengths were observed giving a coverage 
from ~3850-6730 A. 
We identify several absorption features, including Lyman-alpha,
SiIV(1394,1402), SiII1526, and CIV(1548,1550) at the common
redshift of z=2.488.

This result is consistent with the one reported by Snchez-Ramrez
et al. (GCN 14685).

We thank the Gemini-staff for their help in performing these
observations."


GRB_name: GRB130515A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14688
SUBJECT: GRB 130515A: Suzaku WAM observation of the prompt emission
DATE:    13/05/21 14:13:58 GMT
FROM:    Masanori Ohno at Hiroshima U  <ohno@hep01.hepl.hiroshima-u.ac.jp>

W. Iwakiri(RIKEN), M. Tashiro, Y. Terada, T. Yasuda, Y. Ishida, H. Ueno,
S. Sugimoto (Saitama U.),
M. Ohno, K. Takaki, T. Kawano, R. Nakamura, S. Furui, Y. Fukazawa
(Hiroshima U.),
M. Yamauchi, N. Ohmori, M. Akiyama (Univ. of Miyazaki),
K. Yamaoka (Nagoya U.), S. Sugita (Ehime U.), Y. E. Nakagawa, M. Kokubun,
T. Takahashi (ISAS/JAXA), Y. Hanabata (ICRR),
Y. Urata (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo)
on behalf of the Suzaku WAM team, report:

The short GRB 130515A (Swift/BAT trigger #555880 ; Malesani et al., GCN
14650; Barthelmy et al., GCN 14658; Fermi-GBM detection: Jenke, GCN
14663; Konus-Wind detection : Golenetskii et al., GCN 14668) triggered
the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range
of 50 keV - 5 MeV at UT 01:21:17.679 (=T0).

The observed light curve shows a single peak starting at T0+0.1 s,
ending at T0+0.4 s with a duration (T90) of about 0.25 seconds. The
fluence in 100 - 1000 keV was 1.48 (+1.67 / -0.99) x 10-6 erg/cm2.
The 1-s peak flux measured from T0+0 s was 1.4 (+0.4/-0.8)
photons/cm2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0+0 s to
T0+0.5 s is well fitted by a single power-law with a photon index of
2.17 (+0.53/-0.36) (chi2/d.o.f = 36.6/25).

All the quoted errors are at statistical 90% confidence level, in which
the systematic uncertainties are not included.

The light curves for this burst are available at:

http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


GRB_name: GRB130518A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14689
SUBJECT: GRB 130518A: mm detection at PdBI
DATE:    13/05/21 16:39:02 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

A. J. Castro-Tirado (IAA-CSIC Granada), M. Bremer and J.-M. Winters (IRAM
Grenoble), on behalf of a larger collaboration, report:

"We conducted mm observations towards GRB 130518A (Xiong et al. GCNC
14674, Omodei et al. GCNC 14675) starting at 61 hr post burst with the
PdBI at 86.7 GHz. At the position of the optical afterglow (Evans et al.
GCNC 14678, Troja et al. GCNC 14579), we detect a ~2 mJy point source.
Further mm observations are planned."


GRB_name: GRB130518B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14690
SUBJECT: Swift XRT observation of GRB 130518B 
DATE:    13/05/21 19:24:38 GMT
FROM:    Boris Sbarufatti at INAF-OAB/IASFPA  <boris.sbarufatti@brera.inaf.it>

Boris Sbarufatti (INAF-OAB/PSU) reports on behalf of the Swift XRT team

We have analysed 4.2 ks of XRT data for GRB 130518B (Cummings GCN Circ.
14862), from 184.0 ks to 196.1 ks after the BAT trigger. The data are all
in Photon Counting (PC) mode. No bright X-ray afterglow is detected inside
the refined BAT error circle. The 3sigma upper limit is of 4.3 x 10^-3
cts/s.

This corresponds to an observed 0.3-10 keV flux of 1.6 x 10^-13 erg/cm2/s
(assuming a typical GRB spectrum with photon spectral index of 2). If we
consider the Galactic absorption in this direction (3.5 x 10^20 cm^-2;
Kalberla et al. 2005) this corresponds to an unabsorbed flux of 1.8 x
10^-13 erg/cm2/s.


GRB_name: GRB130521A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14691
SUBJECT: GRB 130521A: Swift detection of a burst
DATE:    13/05/21 22:58:17 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

C. Pagani (U Leicester), N. Gehrels (NASA/GSFC),
H. A. Krimm (CRESST/GSFC/USRA), C. J. Mountford (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL), T. Sakamoto (AGU) and
M. H. Siegel (PSU) report on behalf of the Swift Team:

At 22:49:16 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130521A (trigger=556344).  Swift could not slew to the
burst due to the Sun constraint.  The BAT on-board calculated location is 
RA, Dec 87.559, +14.452 which is 
   RA(J2000) = 05h 50m 14s
   Dec(J2000) = +14d 27' 09"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single peak
structure with a duration of about 6 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 05:50 UT on 2013 August 06. There will thus be no XRT or
UVOT data for this trigger before this time. 

Burst Advocate for this burst is C. Pagani (cp232 AT star.le.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB130521A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14692
SUBJECT: GRB 130521A: TAROT La Silla observatory optical observations
DATE:    13/05/21 23:58:12 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (IRAP-CNRS-OMP),
Boer M., Siellez K., Dereli H., Bardho O. (UNS-CNRS-OCA),
Atteia J.L. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 130521A detected by SWIFT
(trigger 556344) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 33.0s after the GRB trigger
(13.7s after the notice). The elevation of the field decreased from
14 degrees above horizon and weather conditions
were good but the event occured during the dusk
at 28 degrees from the Sun. Due to the twilight the
first image of 60s is saturated.

The second image is 30.0s exposure in tracking mode.
We do not detect any OT in the Swift BAT error box
with a limiting magnitude of:
t0+106.3s to t0+136.3s : Rlim = 15.5

We co-added a series of exposures:
t0+106.3s to t0+1795s : Rlim = 17.3

Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.

N.B. Galactic coordinates are lon=193.0037 lat= -6.5236
and the galactic extinction in R band is about 1.6 magnitude
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.


GRB_name: GRB130521A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14693
SUBJECT: GRB 130521A, Swift-BAT refined analysis
DATE:    13/05/22 14:15:36 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC), C. Pagani (U Leicester),
D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU),
T. N. Ukwatta (MSU) (i.e. the Swift-BAT team):

Using the data set from T-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 130521A (trigger #556344)
(Pagani, et al., GCN Circ. 14691).  The BAT ground-calculated position is
RA, Dec = 87.568, 14.470 deg which is
    RA(J2000)  =  05h 50m 16.3s
    Dec(J2000) = +14d 28' 10.8"
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 67%.

The mask-weighted light curve shows a single peak starting at T-2 sec, peaking
at T+0 sec and falling to near background by T+4 sec, followed by a weak tail
out to approximately T+12 sec.  At around T+120 sec, the source moved out of the 
field of view due to a pre-planned slew to another target. T90 (15-350 keV) is 
11.0 +- 2.4 sec (estimated error including systematics).

The time-averaged spectrum from T-0.64 to T+12.64 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.11 +- 0.20.  The fluence in the 15-150 keV band is 4.2 +- 0.5 x 10^-07 
erg/cm2. The 1-sec peak photon flux measured from T-0.14 sec in the 15-150 keV 
band is 1.9 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/556344/BA/


GRB_name: GRB130518B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14694
SUBJECT: GRB 130518B, Swift-BAT refined analysis
DATE:    13/05/22 14:21:30 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

H. A. Krimm (GSFC/USRA) and J. R. Cummings (GSFC/UMBC)
for the Swift-BAT team:

We report further analysis of BAT GRB 130518B (trigger #556105)
(Cummings, GCN Circ. 14682).

The time-averaged spectrum covering 10 seconds of event data (which
includes most of the burst) is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.39 +- 0.14.  The fluence in the 15-150 keV band is 8.0 x 10^-7 erg/cm2.
All the quoted errors are at the 90% confidence level.


GRB_name: GRB130514B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14695
SUBJECT: GRB 130514B: Further Swift-XRT Observations
DATE:    13/05/22 20:39:24 GMT
FROM:    Binbin Zhang at PSU  <bbzhang@psu.edu>

B.-B. Zhang (PSU), Dirk Grupe (PSU). D. Malesani (DARK/NBI) and J. Kennea (PSU) 
report  on behalf of the Swift-XRT team:

We have analyzed 6.8 ks of XRT data for the INTEGRAL-detected burst: 
GRB 130514B,  from 314.3 ks to 321.1 ks after the INTERGRAL trigger.
The data are entirely in Photon Counting (PC) mode. We confirm that 
the X-ray source reported in Zhang et al. GCN 14651 has been faded with 
current count rate of  around 3e-3 count/s.  The light curve can be modeled with  
a power-law decay with a decay index of alpha=0.98 (+0.27, -0.15). 
We therefore conclude that the X-ray source reported in Zhang et al. GCN 14651 
is the X-ray afterglow of GRB 130514B.

The results of the XRT-team automatic analysis are available at

http://www.swift.ac.uk/xrt_curves/00020275/


This circular is an official product of the Swift-XRT team.

[GCN OPS NOTE(25may13):  The "144651" hasn corrected to "14651".]


GRB_name: GRB130521B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14696
SUBJECT: IPN Triangulation of GRB 130521B
DATE:    13/05/22 22:36:40 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

K. Hurley, I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin,
on behalf of the HEND-Odyssey GRB team,

S. Golenetskii, R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks,
D. Svinkin, and T. Cline on behalf of the Konus-Wind team,

J. Goldsten, on behalf of the MESSENGER NS GRB team,

W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr, on
behalf of the GRS-Odyssey GRB team, and

K. Yamaoka, M. Ohno, Y. Hanabata, Y. Fukazawa, T. Takahashi, M. Tashiro,
Y. Terada, T. Murakami, and K. Makishima on behalf of the Suzaku WAM 
team, report:

The long-duration, moderately intense GRB 130521B has been observed by 
Konus-Wind, Suzaku (WAM), MESSENGER (GRNS), and Mars Odyssey (HEND), so 
far, at about 77073 s UT (21:24:33).

We have triangulated it to a preliminary, 3 sigma error box whose 
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   281.641 (18h 46m 34s) +22.723 (+22d 43' 21")
  Corners:
   281.980 (18h 47m 55s) +22.385 (+22d 23' 05")
   281.618 (18h 46m 28s) +22.858 (+22d 51' 30")
   281.300 (18h 45m 12s) +23.057 (+23d 03' 24")
   281.663 (18h 46m 39s) +22.587 (+22d 35' 13")
  ---------------------------------------------
The error box area is 257 sq. arcmin, and its maximum
dimension is 55 arcmin (the minimum one is 3.7 arcmin). The Sun distance 
was 120 deg.

This box can be improved.

The time history and spectrum will be given in a forthcoming GCN Circular.


GRB_name: GRB130521A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14697
SUBJECT: GRB 130521A: Skynet/PROMPT observations
DATE:    13/05/23 02:23:02 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

D. James, C. Foster, P. Taylor, M. Carroll, A. Trotter, D. Reichart, A. 
LaCluyze, J. Haislip, T. Berger, H. T. Cromartie, R. Egger, A. Foster, 
N. Frank, K. Ivarsen, M. Maples, J. Moore, M. Nysewander, E. Speckhard, 
and J. A. Crain report

Skynet observed the Swift/BAT localization of GRB 130521A (Pagani et 
al., GCN 14691, Swift trigger #556344) with four 16" telescopes of the 
PROMPT array at CTIO, Chile.  Starting at 2013-05-21, 22:49:16 UT and 
continuing until 23:01:04 UT (t=49.2s-11.8m post-trigger), it took 66 
exposures in the BVRI bands. We did not detect a fading afterglow within 
the 3 arcmin radius of the Swift/BAT error circle, which was centered on 
RA 05h50m14.2s, Dec +14d27m08.6s (J2000).

A plot of the 3-sigma limiting magnitudes in each exposure, calibrated 
to six USNO-B1/NOMAD stars in the field, is here:
http://skynet.unc.edu/grb/grb130521a.png

We stacked all the images in each band and obtained 3-sigma limiting 
magnitudes on any afterglow of:
Filter       B       V       R       I
Mag       >18.29  >18.53  >18.13  >17.07

Magnitudes are Vega magnitudes, and have not been corrected for the 
expected line-of-sight Milky Way dust extinction E(B-V)=0.38 (Schlegel 
et al. 1998).

No further Skynet observations are scheduled.


GRB_name: GRB130521B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14698
SUBJECT: Konus-Wind observation of GRB 130521B
DATE:    13/05/23 08:30:43 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf
of the Konus-Wind team, report:

The long-duration GRB 130521B
(IPN triangulation: Hurley at al., GCN 14696)
triggered Konus-Wind at T0=77073.510s UT (21:24:33.510).

The light curve shows several pulses from ~T0 s to ~T0+20s,
which, at its initial phase, form a quasi-periodic structure
with the period of ~2.5s.
The emission is seen up to ~7 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130521_77073/

As observed by Konus-Wind, the burst
had a fluence of (1.9  0.15)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+0.512s,
of (4.3  0.3)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+22.016 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.96  0.07,
the high energy photon index beta = -2.9  0.3,
the peak energy Ep = 151  9 keV,
chi2 = 97.6/97 dof.

The spectrum at the maximum count rate
(measured from T0 to T0+5.888 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.69  0.08,
the high energy photon index beta = -3.6  1.1,
the peak energy Ep = 205  12 keV,
chi2 = 107/97 dof.

For both spectra, we note a hint of counts excess
over the model flux in the spectral channels around ~10 MeV.

All the quoted results are preliminary.


GRB_name: GRB130521B
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14700
SUBJECT: GRB 130521B: Suzaku WAM observation of the prompt emission
DATE:    13/05/24 13:36:21 GMT
FROM:    Masanori Ohno at Hiroshima U  <ohno@hep01.hepl.hiroshima-u.ac.jp>

W. Iwakiri(RIKEN), M. Tashiro, Y. Terada, T. Yasuda, Y. Ishida, H. Ueno,
S. Sugimoto (Saitama U.),
M. Ohno, K. Takaki, T. Kawano, R. Nakamura, S. Furui, Y. Fukazawa
(Hiroshima U.),
M. Yamauchi, N. Ohmori, M. Akiyama (Univ. of Miyazaki),
K. Yamaoka (Nagoya U.), S. Sugita (Ehime U.), Y. E. Nakagawa, M. Kokubun,
T. Takahashi (ISAS/JAXA), Y. Hanabata (ICRR),
Y. Urata (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo)
on behalf of the Suzaku WAM team, report:

The long, IPN localized GRB 130521B (Hurley et al., GCN 14696;
Konus-Wind detection : Golenetskii et al., GCN 14698) triggered the
Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of
50 keV - 5 MeV at 21:24:31.599 UT (=T0).

The observed light curve shows a multi-peaked structure starting at
T0-0s, ending at T0+25 s with a duration (T90) of about 23 seconds. The
fluence in 100 - 1000 keV was 1.21 (+0.07/-0.08) x 10^-5 erg/cm^2. The
1-s peak flux measured from T0+1 s was 4.25 (+1.63/-0.54) photons/cm^2/s
in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-0s to
T0+25 s is well fitted by a single power-law with a photon index of 2.33
(+0.19/-0.16) (chi^2/d.o.f = 30.0/25).

All the quoted errors are at statistical 90% confidence level,in which
the systematic uncertainties are not included.

The light curves for this burst are available at:

http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


GRB_name: GRB130514A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14702
SUBJECT: GRB 130514A: Konus-Wind and Swift/BAT joint spectral analysis
DATE:    13/05/24 20:24:57 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

V. Pal'shin, S. Golenetskii, R.Aptekar, E. Mazets, D. Frederiks, D. 
Svinkin, M. Ulanov, and T. Cline on behalf of the Konus-Wind team,

T. Sakamoto (AGU), S. D. Barthelmy (GSFC), W. Baumgartner (GSFC/UMBC), 
J. Cummings (GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (GSFC),
H. Krimm (GSFC/USRA), C. Markwardt (GSFC), D. Palmer (LANL), M. 
Stamatikos (OSU) and T. Ukwatta (GWU)

report:

We performed the Konus-Wind and the Swift/BAT joint spectral analysis of 
GRB 130514A (Swift/BAT trigger #555821: Sonbas et al., GCN Circ. 14632, 
Ukwatta et al. GCN Circ. 14636). Since the Konus-Wind observed this GRB 
in the waiting mode, we only have 3 channel spectral data for the 
Konus-Wind which cover the energy range from 20 keV to 1.2 MeV.  The
joint spectral analysis of the Konus-Wind and the Swift/BAT data allows 
us to derive the broad-band spectral parameters of this burst.

The time interval of the spectral data for each instrument is chosen 
from T0(BAT)-5.1 to T0(BAT)+153.9 s where T0(BAT) is the trigger time of 
BAT at 07:13:41 UTC. This interval comprises whole burst as observed by 
Konus-Wind and contains 87% of the total fluence in the 15-150 keV as 
observed by BAT (Ukwatta et al. GCN Circ. 14636).

The energy ranges which we used in the joint spectral analysis are 
20-1200 keV and 14-150 keV for the Konus-Wind and the Swift/BAT 
respectively.  The spectral data of two instruments are fitted with the 
spectral model multiplied by the constant factor to take into account 
the systematic effective area uncertainties in the response matrices of 
each instrument.

The spectrum is well fitted with a power-law with exponential cutoff 
model: dN/dE ~ E^{alpha}*exp(-(2+alpha)*E/Epeak). No systematic residual 
from the best fit model is seen in the spectral data of each instrument. 
The BAT constant factor is 0.83(-0.08,+0.10) (the KW constant factor is 
fixed to 1). The best fit spectral parameters are: alpha = 
-1.44(-0.14,+0.17) and Epeak = 110(-21,+42) keV (chi2/dof = 41.9/57). 
The best fit spectral parameters for the GRB (Band) model fixing beta = 
-2.5 are:  alpha = -1.44(-0.15,+0.17), and Epeak = 108(-21,+45)  keV 
(chi2/dof = 43.6/57). The energy fluence in the 15-1200 keV band 
calculated by a power-law with exponential cutoff model for this 159 s 
interval is 1.40(-0.16,+0.21)x10^-5 erg/cm2.

Assuming a photo-z of 3.6 (Schmidl, Kann, and Greiner GCN Circ. 14634) 
and a standard cosmology model with H_0 = 71 km/s/Mpc, Omega_M = 0.27, 
Omega_Lambda = 0.73, the isotropic energy release is E_iso = 
4.95(-0.67,+0.85)x10^53 erg in 1 keV to 10 MeV at the GRB rest frame 
extrapolating the best exponential cutoff function fit.

All the quoted errors are at the 90% confidence level.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130514A/


GRB_name: GRB130527A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14703
SUBJECT: GRB 130527A: Swift detection of a bright burst
DATE:    13/05/27 14:31:45 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

B.P. Gompertz (U Leicester), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), M. M. Chester (PSU),
N. Gehrels (NASA/GSFC), J. A. Kennea (PSU),
A. Y. Lien (NASA/GSFC/ORAU), F. E. Marshall (NASA/GSFC),
C. J. Mountford (U Leicester), C. Pagani (U Leicester),
D. M. Palmer (LANL) and M. H. Siegel (PSU) report on behalf of the
Swift Team:

At 14:21:30 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130527A (trigger=556753).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 309.279, -24.728 which is 
   RA(J2000) = 20h 37m 07s
   Dec(J2000) = -24d 43' 39"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex peak
structure with a duration of at least 20 sec.  The peak count rate
was ~25000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 14:23:15.4 UT, 105.2 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 309.2749, -24.7244 which is equivalent to:
   RA(J2000)  = +20h 37m 5.98s
   Dec(J2000) = -24d 43' 27.8"
with an uncertainty of 5.0 arcseconds (radius, 90% containment). This
location is 18 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

The initial flux in the 2.5 s image was 2.88e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 113 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.04. 

Burst Advocate for this burst is B.P. Gompertz (bpg6 AT le.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB130527A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14704
SUBJECT: GRB 130527A: Prompt enhanced Swift-XRT position
DATE:    13/05/27 15:12:30 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team:

Using  promptly downlinked XRT event data for GRB 130527A, we find an
enhanced XRT position of the afterglow: RA, Dec: 309.2762, -24.7246
which is equivalent to:
   RA (J2000)  = 20 37 06.28
   Dec (J2000) = -24 43 28.6
with an uncertainty of 2.0 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/556753.

Position enhancement is is described by Goad et al. (2007, A&A, 476,
1401) and Evans et al. (2009, MNRAS, 397, 1177).

This circular is an official product of the Swift-XRT team.


GRB_name: GRB130527A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14705
SUBJECT: GRB 130527A: Enhanced Swift-XRT position
DATE:    13/05/27 21:08:38 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 872 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 130527A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 309.27631, -24.72515 which is equivalent
to:

RA (J2000): 20h 37m 6.32s
Dec (J2000): -24d 43' 30.6"

with an uncertainty of 1.8 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB130527A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14706
SUBJECT: GRB 130527A: BOOTES-2 & 3.5m CAHA opt/nIR observations
DATE:    13/05/28 06:34:33 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

A. J. Castro-Tirado (IAA-CSIC), J. Gorosabel (IAA-CSIC, UPV-EHU), A.
Guijarro (CAHA) and M. Jelnek (IAA-CSIC), on behalf of a larger
collaboration, report:

"Following the detection of GRB 130527A by Swift (Gompertz et al. GCNC
14703), follow-up observations have been conducted with the 0.6m TELMA
telescope (+ COLORES, i'-band) at the BOOTES-2 station in Mlaga and with
the 3.5m CAHA (+ Omega2000, zYJHK) at the German-Spanish Calar Alto
Observatory. Data was gathered starting at 2:30 UT (i.e. ~12.1 hr post
burst), at high airmass and with the moon only 11 degrees away. At the
position of the X-ray afterglow (Evans et al. GCNC 14705), no optical/nIR
source is detected down to J ~ 20. Further data analysis is ongoing."


GRB_name: GRB130527A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14707
SUBJECT: GRB 130527A: Swift-XRT refined Analysis
DATE:    13/05/28 14:32:06 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

V. Mangano (INAF-IASFPA), A. Melandri (INAF-OAB), B. Sbarufatti
(INAF-OAB/PSU), J.A. Kennea (PSU), M.C. Stroh (PSU), D.N. Burrows
(PSU), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), C. Pagani
(U. Leicester) and B.P. Gompertz report on behalf of the Swift-XRT
team:

We have analysed 5.9 ks of XRT data for GRB 130527A (Gompertz  et al.
GCN Circ. 14703),  from 94 s to 18.3 ks after the  BAT trigger. The
data comprise 203 s in Windowed Timing (WT) mode (the first 10 s were
taken while Swift was slewing) with the remainder in Photon Counting
(PC) mode. The enhanced XRT position for this burst was given by Evans
et al. (GCN. Circ 14704).

The late-time light curve (from T0+4.9 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.15 (+0.24, -0.23).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.70 (+/-0.09). The
best-fitting absorption column is  2.4 (+/-0.3) x 10^21 cm^-2, in
excess of the Galactic value of 3.7 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.67 (+0.16, -0.15)
and a best-fitting absorption column of 1.5 (+/-0.5) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 4.5 x 10^-11 (5.5 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.5 (+/-0.5) x 10^21 cm^-2
Galactic foreground: 3.7 x 10^20 cm^-2
Excess significance: 3.9 sigma
Photon index:      1.67 (+0.16, -0.15)

If the light curve continues to decay with a power-law decay index of
1.15, the count rate at T+24 hours will be 5.7 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.6 x
10^-13 (3.1 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00556753.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB130527A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14708
SUBJECT: GRB 130527A: Swift-BAT refined analysis
DATE:    13/05/28 14:55:43 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), B.P. Gompertz (U Leicester),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-700 to T+302 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 130527A (trigger #556753)
(Gompertz, et al., GCN Circ. 14703).  The BAT ground-calculated position is
RA, Dec = 309.282, -24.726 deg, which is 
   RA(J2000)  =  20h 37m 07.6s 
   Dec(J2000) = -24d 43' 35.1" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 10%.
 
The mask-weighted light curve shows many overlapping peakst starting
at ~T-10 sec, peaking at ~T+1 sec, and ending at ~T+170 sec.
T90 (15-350 keV) is 44 +- 16 sec (estimated error including systematics).
 
The time-averaged spectrum from T-2.9 to T+90.7 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.25 +- 0.06.  The fluence in the 15-150 keV band is 1.2 +- 0.04 x 10^-5 erg/cm2.
The 1-sec peak photon flux measured from T+0.06 sec in the 15-150 keV band
is 20.1 +- 1.4 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/556753/BA/


GRB_name: GRB130527A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14709
SUBJECT: GRB 130527A: RATIR Optical and NIR Observations
DATE:    13/05/28 16:17:12 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB)
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC),
Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC),
Jos A. de Diego (UNAM), Leonid Georgiev (UNAM), Jess Gonzlez (UNAM),
Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC), and Harvey Moseley (GSFC)
report:

We observed the field of GRB 130527A (Gompertz, et al., GCN 14703) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional on
Sierra San Pedro Mrtir from 2013/05 28.35 to 2013/05 28.47 UTC (18.13 to
20.91 hours after the BAT trigger), obtaining a total of 1.97 hours
exposure in the r' and i' bands and 0.73 hours exposure in the Z, Y, J, and
H bands.


For a source within the Swift-XRT error circle (Evans, et al., GCN 14705),
in comparison with USNO-B1 and 2MASS, we obtain the following upper limits
(3-sigma):

  r'    > 21.9
  i'    > 22.3
  Z     > 20.7
  Y     > 20.6
  J     > 20.6
  H     > 20.3

These magnitudes are in the AB system and not corrected for Galactic
extinction in the direction of the GRB.

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB130527A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14710
SUBJECT: GRB 130527A: NOT optical counterpart
DATE:    13/05/28 16:42:36 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

Z. Cano (U. Iceland), D. Malesani (DARK), N. R. Tanvir (U. Leicester), 
D. Xu (DARK/NBI), T. Kangas (U. Turku), and J. Kajava (NOT) report on 
behalf of a larger collaboration:

On 2013 May 28, beginning at 03:55 UT, we observed the field of GRB 
130527A (Gompertz et al., GCN 14703) with the Nordic Optical Telescope 
(NOT) equipped with the ALFOSC instrument using the z filter, for a 
total exposure time of 40 minutes. Observations were carried out at 
moderate airmass, with the bright Moon only 18 deg away, at a mean epoch 
of May 28.179 UT (13.94 hr after the GRB).

Inside the refined XRT error circle (Evans et al., GCN 14705; see also 
http://www.swift.ac.uk/xrt_positions/) we do not detect any bright 
source, but there is a faint, apparently extended object with magnitude 
z = 21.4 +- 0.2. The limiting magnitude for an isolated object in our 
coadded image is z = 22.1. Calibration has been derived using two stars 
in the USNO B1 catalog (0652-0853265 and 0652-0853288), and converting 
their R2 and I magnitudes into z using the transformation equations from 
Jordi et al. (2006, A&A, 460, 339). The source could be the GRB host.

A snapshot showing our coadded image can be found at the URL 
http://www.astro.ku.dk/~malesani/GRB/130527A/GRB130527A_finder_NOT.jpg


GRB_name: GRB130528A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14711
SUBJECT: GRB 130528A: Swift detection of a burst
DATE:    13/05/28 16:52:12 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

V. D'Elia (ASDC), D. N. Burrows (PSU), C. Gronwall (PSU),
J. A. Kennea (PSU), A. Y. Lien (NASA/GSFC/ORAU),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester) and
D. M. Palmer (LANL) report on behalf of the Swift Team:

At 16:41:23 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130528A (trigger=556870).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 138.911, +87.276 which is 
   RA(J2000) = 09h 15m 39s
   Dec(J2000) = +87d 16' 33"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multiple-peaked
structure with a duration of about 85 sec.  The peak count rate
was ~5500 counts/sec (15-350 keV), at ~8 sec after the trigger. 

The XRT began observing the field at 16:42:28.7 UT, 64.9 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 139.51074,
87.30239 which is equivalent to:
   RA(J2000)  = 09h 18m 02.58s
   Dec(J2000) = +87d 18' 08.6"
with an uncertainty of 4.1 arcseconds (radius, 90% containment). This
location is 139 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (5.18 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 1.9
(+2.14/-1.88) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 0.1 s image was 1.20e-08 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 75 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.16. 

Burst Advocate for this burst is V. D'Elia (delia AT asdc.asi.it). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB130528A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14712
SUBJECT: GRB 130528A: optical upper limit
DATE:    13/05/28 19:47:10 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), E. Litvinenko (UBAI), I. Molotov (KIAM), A. Pozanenko 
(IKI) report on behalf of  larger GRB  follow-up collaboration:

We observed the field of  GRB 130528A (D'Elia et al., GCN  14711) with 
0.4-m telescope of ISON-Kitab observatory  starting on  May 28 (UT) 
17:01:13, i.e. 20 minutes after burst trigger.  We took  several 
unfiltered images of 30 s exposure. In the first image we do not detect 
any source in XRT error circle (D'Elia et al., GCN  14711). A photometry 
   is based  on nearby USNO-B1.0 stars:

T_start,     T0+,      Exposure,  OT,    UL (3sigma)
(UT)         mid, d    (s)

17:01:13    0.01395    1x30       n/d    17.3


A finding chart can be found at 
http://grb.rssi.ru/GRB130528A/GRB130528A_Kitab_fc.png


GRB_name: GRB130521A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14713
SUBJECT: GRB 130521A: Skynet/PROMPT detection of an extremely red afterglow
DATE:    13/05/28 19:52:35 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

D. James, C. Foster, P. Taylor, M. Carroll, A. Trotter, D. Reichart, A. 
LaCluyze, J. Haislip, T. Berger, H. T. Cromartie, R. Egger, A. Foster, 
N. Frank, K. Ivarsen, M. Maples, J. Moore, M. Nysewander, E. Speckhard, 
and J. A. Crain report

Skynet observed the Swift/BAT localization of GRB 130521A (Pagani et 
al., GCN 14691, Swift trigger #556344) with four 16" telescopes of the 
PROMPT array at CTIO, Chile. Starting at 2013-05-21, 22:49:16 UT and 
continuing until 23:01:04 UT (t=49.2s-11.8m post-trigger), it took 66 
exposures in the BVRI bands. The field was 28.5 degrees from the sun at 
this time, so the duration of the observation was limited by sky 
brightness and high airmass.

In James et al. (GCN 14697) we reported that we did not detect an 
afterglow. We conducted follow-up observations two nights later, and on 
reexamination discovered that an extremely red afterglow was in fact 
detected in our first nights I and R band exposures.
The position of the afterglow is (J2000):
RA = 05h 50m 10.55s
Dec = 14d 27m 26.8s
A finder chart is at:
http://skynet.unc.edu/grb/grb130521a_finder.png

A preliminary light curve is at:
http://skynet.unc.edu/grb/grb130521a_2.png

Magnitudes are in the Vega system and are calibrated to 19 APASS stars 
in the field. We regard the V band detection to be questionable, but the 
R and I band detections are solid.

The galactic coordinates of the afterglow are l=193.3312, b=-5.9321. The 
dust emission maps of Schlegel et al. (1998) indicate E(B-V)=0.381 along 
this line of sight; the predicted extinction in each of the bands that 
we observed is:
Filter B V R I
A_lambda 1.65 1.24 1.00 0.75

The observed R band brightness is 1.5 magnitudes fainter than in the I 
band. Correcting for galactic dust extinction, the R band is still 1.25 
magnitudes fainter than in the I band. Such an extremely red afterglow 
could be due to an unusually large amount of dust extinction in the host 
galaxy or to the burst being at a redshift z-5. Follow-up observations 
are encouraged when the source is again visible in early August.

We encourage anyone who may have observed this field, particularly in 
the near infrared, to reexamine their images to see if this afterglow 
was detected in them.

No further Skynet observations are scheduled.


GRB_name: GRB130528A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14714
SUBJECT: GRB 130528A: Enhanced Swift-XRT position
DATE:    13/05/28 21:05:38 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 842 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 130528A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 139.50051, +87.30103 which is equivalent
to:

RA (J2000): 09h 18m 0.12s
Dec (J2000): +87d 18' 03.7"

with an uncertainty of 1.8 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB130527A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14715
SUBJECT: GRB 130527A: Swift/UVOT Upper Limits
DATE:    13/05/29 00:50:04 GMT
FROM:    Margaret Chester at PSU  <chester@astro.psu.edu>

M. M. Chester (PSU) and B. P. Gompertz (U Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130527A
113 s after the BAT trigger (Gompertz et al., GCN Circ. 14703).
No optical afterglow consistent with the XRT position (Evans et al. 
GCN Circ. 14705) is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposures and subsequent exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white_FC           113          263          147         >21.2
white              113         1547          392         >21.1
white             4949        12020          623         >21.8

v                  655         1596          117         >18.7
v                 5359         5559          197         >19.5

b                  581         1693          114         >20.2
b                 6179        11579          906         >21.3

u_FC               325          575          246         >20.3
u                  325         1671          343         >20.2
u                 5974        18261         1072         >21.1

w1                 704         1646           97         >19.8
w1                5769        17356         1082         >21.1

m2                 680         1621          117         >20.0
m2                5564         5764          197         >19.8

w2                 630         1572          117         >20.6
w2                5154         5354          197         >20.2

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.04 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB130528A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14716
SUBJECT: GRB 130528A: Swift-XRT refined Analysis
DATE:    13/05/29 04:52:07 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A. Melandri (INAF-OAB), B. Sbarufatti (INAF-OAB/PSU), M.C. Stroh (PSU),
D.N. Burrows (PSU), J.A. Kennea (PSU), K.L. Page (U. Leicester), C.
Pagani (U. Leicester), A.P. Beardmore (U. Leicester), G. Stratta (ASDC)
and V. D'Elia report on behalf of the Swift-XRT team:

We have analysed 9.0 ks of XRT data for GRB 130528A (D'Elia  et al. GCN
Circ. 14711),  from 68 s to 22.8 ks after the  BAT trigger. The data
comprise 842 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Goad et al. (GCN. Circ 14714).

The late-time light curve (from T0+4.9 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.06 (+/-0.12).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.69 (+/-0.07). The
best-fitting absorption column is  3.6 (+/-0.3) x 10^21 cm^-2, in
excess of the Galactic value of 5.2 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.92 (+/-0.15) and a
best-fitting absorption column of 3.6 (+/-0.6) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 4.4 x 10^-11 (6.9 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.6 (+/-0.6) x 10^21 cm^-2
Galactic foreground: 5.2 x 10^20 cm^-2
Excess significance: 8.5 sigma
Photon index:      1.92 (+/-0.15)

If the light curve continues to decay with a power-law decay index of
1.06, the count rate at T+24 hours will be 0.013 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.7 x
10^-13 (8.9 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00556870.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB130529A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14717
SUBJECT: GRB 130529A: Swift detection of a burst
DATE:    13/05/29 11:24:56 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

V. D'Elia (ASDC), S. D. Barthelmy (GSFC), J. A. Kennea (PSU),
C. Pagani (U Leicester) and M. H. Siegel (PSU) report on behalf of the
Swift Team:

At 11:15:25 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130529A (trigger=556930).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 24.259, -64.138, which is 
   RA(J2000)  =  01h 37m 02s
   Dec(J2000) = -64d 08' 17"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As is typical for image triggers, the real-time
TDRSS lightcurve does not show anything significant. 

The XRT began observing the field at 11:17:18.0 UT, 112.6 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 24.2798, -64.1493 which is equivalent to:
   RA(J2000)  = +01h 37m 7.15s
   Dec(J2000) = -64d 08' 57.5"
with an uncertainty of 5.4 arcseconds (radius, 90% containment). This
location is 52 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

The initial flux in the 2.5 s image was 1.24e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 122 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
Data from the list of sources generated on-board are not available at this
time. No correction has been made for the expected extinction corresponding to
E(B-V) of 0.02. 

Burst Advocate for this burst is V. D'Elia (delia AT asdc.asi.it). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB130528A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14718
SUBJECT: GRB 130528A: Swift-BAT refined analysis
DATE:    13/05/29 11:38:26 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
V. D'Elia (ASDC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-61 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 130528A (trigger #556870)
(D'Elia, et al., GCN Circ. 14711).  The BAT ground-calculated position is
RA, Dec = 139.405, 87.300 deg, which is 
   RA(J2000)  =  09h 17m 37.2s 
   Dec(J2000) = +87d 18' 01.5" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows several overlapping peaks starting
at ~T+0, peaking at ~T+4 sec, and ending at ~T+80 sec.
T90 (15-350 keV) is 59.4 +- 3.6 sec (estimated error including systematics).
 
The time-averaged spectrum from T+0.12 to T+79.34 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.39 +- 0.19, 
and Epeak of 118.3 +- 79.7 keV (chi squared 42.3 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 5.1 +- 0.2 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+6.06 sec in the 15-150 keV band is
3.0 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.67 +- 0.05 (chi squared 48.6 for 57 d.o.f.).  All the quoted errors
are at the 90% confidence level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/556870/BA/


GRB_name: GRB130529A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14719
SUBJECT: GRB 130529A: Prompt enhanced Swift-XRT position
DATE:    13/05/29 12:11:48 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team:

Using  promptly downlinked XRT event data for GRB 130529A, we find an
enhanced XRT position of the afterglow: RA, Dec: 24.2820, -64.1473
which is equivalent to:
   RA (J2000)  = 01 37 07.69
   Dec (J2000) = -64 08 50.2
with an uncertainty of 2.0 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/556930.

Position enhancement is is described by Goad et al. (2007, A&A, 476,
1401) and Evans et al. (2009, MNRAS, 397, 1177).

This circular is an official product of the Swift-XRT team.


GRB_name: GRB130527A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14720
SUBJECT: Konus-Wind observation of GRB 130527A
DATE:    13/05/29 14:11:48 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf
of the Konus-Wind team, report:

The long-duration intense hard-spectrum GRB 130527A
(Swift-BAT trigger 556753: Gompertz et al., GCN 14703;)
Baumgartner et al., GCN 14708)
triggered Konus-Wind at T0=51688.300s UT (14:21:28.300).

The light curve shows a bright hard multi-peaked
emission complex from ~T0 s to ~T0+10s,
followed by the weaker and softer emission out to ~T0+40s.

The emission is seen up to 10 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130527_T51688/

As observed by Konus-Wind, the burst
had a fluence of (1.1  0.05)x10-4 erg/cm2,
and a 64-ms peak flux, measured from T0+3.200s,
of (5.0  0.3)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+38.656 s)
is best fit in the 50 keV - 15 MeV range
by the cutoff power law model with the following parameters:
the photon index alpha = -1.04  0.04,
the peak energy Ep = 1380  120 keV,
chi2 = 96/90 dof.

The spectrum at the maximum count rate
(measured from T0+0.256 to T0+5.888 s)
is best fit in the 50 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
by the cutoff power law model with the following parameters:
the photon index alpha = -0.97  0.04,
the peak energy Ep = 1429  84 keV,
chi2 = 72/79 dof.

All the quoted results are preliminary.


GRB_name: GRB130528A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14721
SUBJECT: GRB 130528A: Swift/UVOT Upper Limits
DATE:    13/05/29 14:39:16 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <m.depasquale@ucl.ac.uk>

M. De Pasquale (MSSL-UCL) and V. D'Elia (ASDC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB
130528A 75 s after the BAT trigger (D'Elia et al., GCN Circ. 14711).
No optical afterglow consistent with the enhanced XRT position
(Goad et al. GCN Circ. 14714) is detected in the initial UVOT
exposures.

Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white_FC            75          225          147         >20.3
u_FC               287          537          246         >19.5
white               75        18737         1239         >21.7
v                  617        11553         1245         >19.9
b                  543        18247         1356         >20.8
u                  287        17334         1583         >21.0
w1                 667        22765         1443         >20.7
m2                 641        12459         1179         >20.7
w2                 592         7143          491         >20.5

The magnitudes in the table are not corrected for the Galactic
extinction due to the reddening of E(B-V) = 0.16 in the direction
of the burst (Schlegel et al. 1998).


GRB_name: GRB130528A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14722
SUBJECT: Konus-Wind observation of GRB 130528A
DATE:    13/05/29 15:33:52 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf
of the Konus-Wind team, report:

The long-duration GRB 130528A
(Swift-BAT trigger 556870: D'Elia et al., GCN 14711;
Cummings et al., GCN 14718)
triggered Konus-Wind at T0=60085.301s UT (16:41:25.301).

The light curve shows a pulse from ~T0-5 s to ~T0+10s,
followed by weaker and softer emission out to ~T0+60s.

The emission is seen up to 7 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130528_T60085/

As observed by Konus-Wind, the burst
had a fluence of (8.0  0.7)x10-6 erg/cm2,
and a 64-ms peak flux, measured from T0+0.640s,
of (1.7  0.2)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+57.600 s)
is best fit in the 20 keV - 15 MeV range
by the cutoff power law model with the following parameters:
the photon index alpha = -1.30  0.15,
the peak energy Ep = 93  9 keV,
chi2 = 90/98 dof.

The spectrum at the maximum count rate
(measured from T0+0.256 to T0+5.888 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.21  0.23,
the high energy photon index beta = -2.6  0.3,
the peak energy Ep = 142  14 keV,
chi2 = 70/97 dof.

All the quoted results are preliminary.


GRB_name: GRB130529A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14723
SUBJECT: GRB 130529A: Enhanced Swift-XRT position
DATE:    13/05/29 22:58:28 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 7658 s of XRT Photon Counting mode data and 9 UVOT
images for GRB 130529A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 24.28192, -64.14745 which is equivalent
to:

RA (J2000): 01h 37m 7.66s
Dec (J2000): -64d 08' 50.8"

with an uncertainty of 1.4 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB130529A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14724
SUBJECT: GRB 130529A: Swift-XRT refined Analysis
DATE:    13/05/29 23:25:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), J.A. Kennea (PSU),
M.C. Stroh (PSU), C. Pagani (U. Leicester), A.P. Beardmore (U.
Leicester), P.A. Evans (U. Leicester), G. Stratta (ASDC), P. D'Avanzo
(INAF-OAB) and V. D'Elia report on behalf of the Swift-XRT team:

We have analysed 8.6 ks of XRT data for GRB 130529A (D'Elia  et al. GCN
Circ. 14717),  from 118 s to 19.2 ks after the BAT trigger. The data
comprise 300 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Osborne et al. (GCN. Circ 14719).

The light curve can be modelled with an initial power-law decay with an
index of alpha=1.67 (+/-0.04), followed by a break at T+1862 s to an
alpha of 0.97 (+0.08, -0.14).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.36 (+0.08, -0.07). The
best-fitting absorption column is  6.8 (+2.2, -2.0) x 10^20 cm^-2, in
excess of the Galactic value of 2.7 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.32 (+0.15, -0.14)
and a best-fitting absorption column of 6.9 (+4.5, -4.0) x 10^20 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 5.3 x 10^-11 (5.7 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      6.9 (+4.5, -4.0) x 10^20 cm^-2
Galactic foreground: 2.7 x 10^20 cm^-2
Excess significance: 1.7 sigma
Photon index:      1.32 (+0.15, -0.14)

If the light curve continues to decay with a power-law decay index of
0.97, the count rate at T+24 hours will be 8.1 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.3 x
10^-13 (4.7 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00556930.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB130518A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14725
SUBJECT: GRB 130518A: Suzaku WAM observation of the prompt emission
DATE:    13/05/30 10:45:47 GMT
FROM:    Takafumi Kawano at Hiroshima U/Suzaku-HXD-WAM  <tkawano@hep01.hepl.hiroshima-u.ac.jp>

T. Kawano, M. Ohno, K. Takaki, R. Nakamura, S. Furui, Y. Fukazawa
(Hiroshima U.),
T. Yasuda, M. Tashiro, Y. Terada, Y. Ishida, H. Ueno, S. Sugimoto (Saitama U.),
M. Yamauchi, N. Ohmori, M. Akiyama (Univ. of Miyazaki),
K. Yamaoka (Nagoya U.),  S. Sugita (Ehime U.), Y. E. Nakagawa, M. Kokubun,
T. Takahashi (ISAS/JAXA), W. Iwakiri(RIKEN), Y. Hanabata (ICRR),
Y. Urata (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo)
on behalf of the Suzaku WAM team, report:


The bright, long GRB 130518A (Fermi-GBM detection: Xiong, GCN 14674;
Fermi-LAT detection: Omodei and Julie McEnery, GCN 14675;
Swift-BAT trigger 556113: Cummings, GCN 14676)
triggered the Suzaku Wide-band  All-sky Monitor (WAM) which covers an
energy range of 50 keV - 5 MeV at  UT 13:54:50.635(=T0).

The observed light curve shows a bright peak followed by a weaker emission seen
up to T0+24 s with a duration (T90) of about 22 seconds.
The fluence in 100 - 1000 keV was 7.05 (-0.34, +0.20) x10^-5 erg/cm^2.
The 1-s peak flux measured from T0+11 s was  15.9 (-0.89, +0.61) photons/cm^2/s
in the same energy range.

Preliminary result shows that the time-averaged spectrum from
T0-5 s to T0+30 s is well fitted by a GRB Band model as follows.
the low-energy photon index alpha: -1.42 (-0.18, +0.26),
the high-energy photon index beta: -2.27 (-0.22, +0.12),
and the peak energy Epeak: 550 (-91, +99) keV, (chi^2/d.o.f = 74.0/68).

Due to the brightness of this burst, a 5% systematic error was added
for low energy channels.
All the quoted errors are at statistical 90% confidence level.


The light curves for this burst are available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


GRB_name: GRB130529A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14726
SUBJECT: GRB 130529A: Swift-BAT refined analysis
DATE:    13/05/30 11:00:33 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), V. D'Elia (ASDC), E. E. Fenimore (LANL),
N. Gehrels (GSFC), A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+464 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 130529A (trigger #556930)
(D'Elia, et al., GCN Circ. 14717).  The BAT ground-calculated position is
RA, Dec = 24.274, -64.143 deg, which is 
   RA(J2000)  =  01h 37m 05.7s 
   Dec(J2000) = -64d 08' 34.8" 
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows the burst starting at ~T-20 sec,
peaking at about T+80 sec, and ending at ~T+260 sec.
T90 (15-350 keV) is 128 +- 35 sec (estimated error including systematics).
 
The time-averaged spectrum from T-15.02 to T+150.62 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.56 +- 0.17.  The fluence in the 15-150 keV band is 1.4 +- 0.2 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T+64.28 sec in the 15-150 keV band
is 0.5 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/556930/BA/


GRB_name: GRB130527A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14727
SUBJECT: GRB 130527A: Suzaku WAM observation of the prompt emission
DATE:    13/05/30 11:28:01 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

H. Ueno, M. Tashiro, Y. Terada, T. Yasuda, Y. Ishida,
S. Sugimoto (Saitama U.), M. Ohno, K. Takaki, T. Kawano,
R. Nakamura, S. Furui, Y. Fukazawa (Hiroshima U.),
M. Yamauchi, N. Ohmori, M. Akiyama (Univ. of Miyazaki),
K. Yamaoka (Nagoya U.), S. Sugita (Ehime U.), Y. E. Nakagawa,
M. Kokubun, T. Takahashi (ISAS/JAXA), W. Iwakiri(RIKEN),
Y. Hanabata (ICRR), Y. Urata (NCU), K. Nakazawa,
K. Makishima (Univ. of Tokyo) on behalf of the Suzaku WAM team, report:


The bright, long GRB 130527A (Swift-BAT detection: W. H. Baumgartner,
et al. , GCN 14708) triggered the Suzaku Wide-band All-sky Monitor (WAM)
which covers an energy range of 50 keV - 5 MeV at UT 14:21:27.030(=T0).

The observed light curve shows a multi-peaked structure starting at
T0-0.5 s, ending at T0+13 s with a duration (T90) of about 7.4 seconds.
The fluence in 100 - 1000 keV was 5.26 (-0.36, +0.39) *10^-5 erg/cm^2.
The 1-s peak flux measured from T0+4.5 s was
20.26 (-0.92, +1.12) photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from
T0-1 s to T0+13 s is well fitted by a GRB Band model as follows.
the low-energy photon index alpha: -0.87 (-0.13, +0.10),
the high-energy photon index beta: -2.68 (-0.36, +0.14),
and the peak energy Epeak: 1426 (-123, +221) keV,
(chi^2/d.o.f = 36.3/28).

Due to the brightness of this burst, a 3% systematic error was added
for low energy channels.
All the quoted errors are at statistical 90% confidence level.

The light curves for this burst are available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


GRB_name: GRB130529A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14728
SUBJECT: GRB 130529A: Swift/UVOT Upper Limits
DATE:    13/05/30 12:45:32 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (MSSL-UCL) and V. D'Elia (ASDC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130529A
123 s after the BAT trigger (D'Elia et al., GCN Circ. 14717).
No optical afterglow consistent with the XRT position
(Osborne et al. GCN Circ. 14723)
is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white_FC           123          272          147         >21.6
u_FC               281          530          246         >20.8
white              123         7633          824         >22.1
v                  611        12979         1237         >20.8
b                  536        19245         1031         >21.1
u                  281        18726         1641         >21.5
w1                 660        17812         1415         >21.6
m2                 635        13481          822         >21.0
w2                 587        12064         1275         >21.8

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.02 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB130528A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14729
SUBJECT: GRB 130528A: Fermi GBM detection
DATE:    13/05/30 15:42:30 GMT
FROM:    Peter Jenke at MSFC  <peter.a.jenke@nasa.gov>

P. Jenke (UAH) reports on behalf of the Fermi GBM Team:

"At 16:41:21.41 UT on May 28 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130528A (trigger 391452087 / 130528695),
which was also detected by the Swift/BAT (D'Elia et al., GCN  14711).
The GBM on-ground location is consistent with the Swift position.

The angle of the Fermi LAT boresight is 60 degrees from the Swift location.

The GBM light curve consists of at least three peaks
with a duration (T90) of about 55 s (50-300 keV).
The time-averaged spectrum from T0-0.9 s to T0+58.5 s is
well fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.12 +/- 0.04 and
the cutoff energy, parameterized as Epeak, is 130 +/- 7 keV.

The event fluence (10-1000 keV) in this time interval is
(9.5 +/- 0.3)E-06 erg/cm^2. The 1.0-sec peak photon flux measured
starting from T0+3.2 s in the 10-1000 keV band
is 5.5 +/- 0.2 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB130529A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14730
SUBJECT: GRB 130529A: GROND upper limits
DATE:    13/05/30 15:53:49 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

K. Varela (MPE Garching), S. Klose, A. Nicuesa Guelbenzu (both TLS 
Tautenburg), and J. Greiner (MPE Garching) report on behalf of the GROND 
team:

We observed the field GRB 130529A (Swift trigger 556930; D' Elia et al., 
GCN 14717) simultaneously in g'r'i'z'JHKs with GROND (Greiner et al. 
2008, PASP 120, 405) mounted at the 2.2m MPG/ESO telescope at La Silla 
Observatory (Chile).

Observations started at 07:10 UT on May 30, about 20 hours after the 
trigger at a mean seeing of 1.7 arcsec and a mean airmass of 2. Inside 
the enhanced 1".4 XRT error circle (Osborne et al., GCN 14723), we do not 
detect any source. Based on an observation with 150 min integration time 
in g'r'i'z' and 124 min integration time in JHKs, we estimate preliminary 
3-sigma upper limits (all in the AB system) of

g' > 24.3,
r' > 24.6,
J  > 21.8,
H  > 21.1.

We note that the field is rich in galaxies. Within 10 arcsec around the 
XRT error circle are at least three objects (also visible on DSS2), with 
the most extended one an edge-on galaxy about 6" in diameter. The bad 
seeing prevents at the moment a more detailed classification of the other 
objects.

Magnitudes are calibrated against GROND zero points (g'r'i'z') as well as 
2MASS field stars (JHKs) and, as usual, are not corrected for Galactic 
extinction along the line of sight.


GRB_name: GRB130603A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14731
SUBJECT: GRB 130603A: Swift detection of a burst
DATE:    13/06/03 06:08:14 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. Melandri (INAF-OAB), C. Gronwall (PSU),
C. B. Markwardt (NASA/GSFC), D. M. Palmer (LANL) and T. Sakamoto (AGU)
report on behalf of the Swift Team:

At 05:59:32 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130603A (trigger=557274).  Swift could not immediately slew
to the burst due to an Earth limb constraint. 
The BAT on-board calculated location is 
RA, Dec 86.954, +82.934 which is 
   RA(J2000) = 05h 47m 49s
   Dec(J2000) = +82d 56' 02"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single
FRED structure with a duration of about 100 sec.  The peak count rate
was ~1275 counts/sec (15-350 keV), at ~1 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+49.7
minutes. There will be no XRT or UVOT data until this time. 

Burst Advocate for this burst is A. Melandri (andrea.melandri AT brera.inaf.it). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB130603A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14732
SUBJECT: GRB 130603A: Swift-XRT and Swift-UVOT detections
DATE:    13/06/03 07:40:26 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

A. Melandri (INAF/OAB) reports on behalf of the Swift team:

Swift-XRT observed the field of GRB 130603A (Melandri et al., GCN  
Circ. 14731) starting at T0+49.7 minutes due to an observing  
constraint. Using promptly downlinked data we find an uncatalogued X- 
ray source located at RA, Dec = 86.8938, 82.9099 which is equivalent to:

RA  (J2000) =  05 47 34.51
DEC (J2000) =  +82 54 35.7

with an uncertainty of 3.7 arcsec (radius, 90% containment).

A source is also detected by Swift-UVOT located at RA, Dec = 86.8914,  
82.9087 which is equivalent to

RA  (J2000) =  05 47 33.9
DEC (J2000) =  +82 54 31.3

with an uncertainty of 0.8 arcsec (radius, 90% containment).

This position may be improved as more data are received. The latest  
position can be viewed at http://www.swift.ac.uk/xrt_positions.  
Position enhancement is described by Goad et al. (2007, A&A, 476,  
1401) and Evans et al. (2009, MNRAS, 397, 1177).


GRB_name: GRB130603A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14733
SUBJECT: GRB 130603A: Swift-XRT observations
DATE:    13/06/03 07:56:30 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

D.N. Burrows (PSU), J.A. Kennea (PSU), M. Perri (ASDC), G. Tagliaferri
(INAF-OAB), P.A. Evans (U. Leicester) and J.P. Osborne (U. Leicester)
report on behalf of the Swift-XRT team:

The XRT began observing the field of GRB 130603A at 06:51:16.2 UT,
3103.6 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source located at RA, Dec 86.89380, 82.90992
which is equivalent to:
   RA(J2000)  = 05h 47m 34.51s
   Dec(J2000) = +82d 54' 35.7"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 90 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (5.28 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 4.9
(+2.95/-2.45) x 10^21 cm^-2 (90% confidence). 


GRB_name: GRB130603A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14734
SUBJECT: GRB 130603A: MITSuME Okayama Optical Observation
DATE:    13/06/03 14:05:22 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ),
S. Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 130603A (Melandri et al., GCNC 14731)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.

The observation started on 2013-06-03 11:14:06 UT (~5.2 h after the burst).
We detected the previously reported afterglow (Melandri, GCNC 14732)
in all the three bands.

Photometric results of the OT are listed below.
We used SDSS catalog for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'  g'_err   Rc  Rc_err   Ic  Ic_err
-----------------------------------------------------------------------
0.22890    11:29:09    1560.0    18.3  0.3    18.4  0.2    18.1  0.3
0.24993    11:59:26    1500.0    18.9  0.3    18.8  0.2    18.2  0.3
------------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB130603B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14735
SUBJECT: GRB 130603B: Swift detection of a bright short burst
DATE:    13/06/03 16:15:25 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. Melandri (INAF-OAB), W. H. Baumgartner (GSFC/UMBC),
D. N. Burrows (PSU), J. R. Cummings (NASA/UMBC),
N. Gehrels (NASA/GSFC), C. Gronwall (PSU), K. L. Page (U Leicester),
D. M. Palmer (LANL), R. L. C. Starling (U Leicester) and
T. N. Ukwatta (MSU) report on behalf of the Swift Team:

At 15:49:14 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130603B (trigger=557310).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 172.209, +17.045 which is 
   RA(J2000) = 11h 28m 50s
   Dec(J2000) = +17d 02' 42"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single spike
structure with a duration of about 0.4 sec.  The peak count rate
was 60000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 15:50:12.8 UT, 59.0 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 172.2006, 17.0719 which
is equivalent to:
   RA(J2000)  = 11h 28m 48.16s
   Dec(J2000) = +17d 04' 18.8"
with an uncertainty of 2.7 arcseconds (radius, 90% containment). This
location is 101 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (1.93 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 6.8
(+4.00/-3.31) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 62 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 25% of
the BAT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
BAT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.02. 

The Swift star trackers were not locked at the time of the
burst, so there may be some additional error in the position. 
However the spike in the rates and the image detection is
unambiguously real. 

We note that this bright short hard GRB is near (12 arcminutes) 
the location of the nearby galaxy NGC 3691.  At z=0.003566, this
corresponds to a nominal projected distance of about 50 kpc. 

Burst Advocate for this burst is A. Melandri (andrea.melandri AT brera.inaf.it). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB130603A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14736
SUBJECT: GRB 130603A: Swift-BAT refined analysis
DATE:    13/06/03 17:33:38 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC), A. Melandri (INAF-OAB),
D. M. Palmer (LANL), T. Sakamoto (AGU), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-60 to T+243 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 130603A (trigger #557274)
(Melandri, et al., GCN Circ. 14731).  The BAT ground-calculated position is
RA, Dec = 86.859, 82.910 deg, which is 
   RA(J2000)  =  05h 47m 26.1s 
   Dec(J2000) = +82d 54' 36.7" 
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 98%.
 
The mask-weighted light curve shows mostly smooth peak starting at ~T-10 sec,
peaking at ~T+11 sec, and ending at ~T+115 sec.
T90 (15-350 keV) is 76 +- 19 sec (estimated error including systematics).
 
The time-averaged spectrum from T-19.5 to T+104.5 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.83 +- 0.12.  The fluence in the 15-150 keV band is 1.9 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+11.27 sec in the 15-150 keV band
is 0.8 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/557274/BA/


GRB_name: GRB130603A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14737
SUBJECT: GRB 130603A: Enhanced Swift-XRT position
DATE:    13/06/03 19:34:56 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 4017 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 130603A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 86.89660, +82.90853 which is equivalent
to:

RA (J2000): 05h 47m 35.18s
Dec (J2000): +82d 54' 30.7"

with an uncertainty of 1.5 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB130603A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14738
SUBJECT: Swift/UVOT observations of GRB130603A
DATE:    13/06/03 19:36:24 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <m.depasquale@ucl.ac.uk>

M. De Pasquale (MSSL/UCL) and A. Melandri (INAF/OAB) report on behalf
of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130603A
3325 s after the BAT trigger (Melandri et al., GCN Circ. 14731). The
uncatalogued source reported in Melandri et al., GCN Circ. 14732, is
detected in the summed exposures.

Preliminary detections and 3-sigma upper limits using the UVOT
photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for
the summed exposures are:

Filter      T_start(s) T_stop(s)  Exp(s)           Mag

white         3686       5322       393       19.61  0.15
v             4097       5562       197      >19.02
b             3481      16641      1278       19.71  0.15
u             3275      15729      1278       19.19  0.13
uvw1          4507       4707       197       19.62  0.39 (2.8 sigma)
uvm2          4302       4502       197      >19.63
uvw2          3892       5528       393       20.25  0.37 (2.8 sigma)

The possible detection of the optical source in uw2 filter indicates
a redshift z < ~1.5 for this event.

The magnitudes in the table are not corrected for the Galactic
extinction due to the reddening of E(B-V) = 0.06 in the direction of
the burst (Schlegel et al. 1998).


GRB_name: GRB130603B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14739
SUBJECT: GRB 130603B: Enhanced Swift-XRT position
DATE:    13/06/03 21:45:08 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 712 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 130603B, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 172.20070, +17.07112 which is equivalent
to:

RA (J2000): 11h 28m 48.17s
Dec (J2000): +17d 04' 16.0"

with an uncertainty of 2.0 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB130603A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14740
SUBJECT: GRB 130603A: Swift-XRT refined Analysis
DATE:    13/06/03 22:15:16 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

A. Melandri (INAF-OAB) reports on behalf of the Swift-XRT team:

We have analysed 13 ks of XRT data for GRB 130603A (Melandri  et al.
GCN Circ. 14731),  from 3.1 ks to 34.3 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Beardmore et al. (GCN. Circ
14737).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.52 (+/-0.07).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.32 (+0.18, -0.17). The
best-fitting absorption column is  4.7 (+0.8, -0.7) x 10^21 cm^-2, in
excess of the Galactic value of 5.3 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.8 x 10^-11 (8.5 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.7 (+0.8, -0.7) x 10^21 cm^-2
Galactic foreground: 5.3 x 10^20 cm^-2
Excess significance: 9.9 sigma
Photon index:      2.32 (+0.18, -0.17)

If the light curve continues to decay with a power-law decay index of
0.52, the count rate at T+24 hours will be 0.028 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x
10^-12 (2.4 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00557274.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB130603B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14741
SUBJECT: GRB 130603B: Swift-BAT refined analysis
DATE:    13/06/03 22:16:10 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC), A. Melandri (INAF-OAB),
D. M. Palmer (LANL), T. Sakamoto (AGU), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-61 to T+242 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 130603B (trigger #557310)
(Melandri, et al., GCN Circ. 14735).  The BAT ground-calculated position is
RA, Dec = 172.222, 17.063 deg, which is 
   RA(J2000)  =  11h 28m 53.2s 
   Dec(J2000) = +17d 03' 48.2" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows a single FRED-like spike starting
at ~T_0.000, peaking at ~T+0.012 sec, and returning to baseline at~T+0.2sec.
There is a smaller pulse ridding on the tail of the initial pulse.
T90 (15-350 keV) is 0.18 +- 0.02 sec (estimated error including systematics).
 
The time-averaged spectrum from T+0.01 to T+0.26 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
0.82 +- 0.07.  The fluence in the 15-150 keV band is 6.3 +- 0.3 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.36 sec in the 15-150 keV band
is 6.4 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/557310/BA/


GRB_name: GRB130603B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14742
SUBJECT: GRB 130603B: WHT optical afterglow candidate
DATE:    13/06/03 22:53:37 GMT
FROM:    Andrew Levan at U.of Leicester  <A.J.Levan@warwick.ac.uk>

A.J. Levan (U. Warwick), N.R. Tanvir, K. Wiersema (U. Leicester), O. Hartoog (Amsterdam), K. Kolle, J. Mendez (ING) and T. Kupfer (Nijmegan) report for a larger collaboration:

We observed the location of GRB 130603B (Melandri et al. GCN 14735) with the William Herschel Telescope, beginning at 21:39 UT approximately 5.8 hours after the burst. In our z and r-band observations we identify a galaxy present in the SDSS DR9 observations of the field with a magnitude of r=20.94.  In addition we identify a point-like source, offset approximately 1" to the SW of this source, with an approximate (+/- 1") position of;

RA(J2000) 11 28 48.16
DEC(J2000) +17:04:18.0

This source is blended with the SDSS galaxy, but appears to be brighter. We suggest this is likely to be the optical afterglow of GRB 130603B."


GRB_name: GRB130603B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14743
SUBJECT: GRB 130603B: Afterglow detection from NOT
DATE:    13/06/03 23:31:08 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), D. Malesani (DARK/NBI), D.  Xu (DARK/NBI), P. Jakobsson (U. Iceland), J. Datson (Tuorla Obs.), R.  Salinas (FINCA), T. Augusteijn (NOT), Y. Martinez-Osorio (NOT), report on behalf of a larger collaboration:

We observed the field of the short GRB 130603B (Melandri et al., GCN 14735) using the 2.5m NOT telescope beginning on 2013 Jun 3 at 21:22 UT. Observations consisted of 5x360 s in the r band. As noted by Levan et al. (GCN 14742), the refined XRT position (Evans et al., GCN 14739) straddles a galaxy detected in the SDSS, which has a photometric redshift z=0.39+/-0.11.

Our images reveal a point source superimposed over this galaxy, and consistent with the XRT posion, at the following coordinates (J2000+/-0.5"):

R.A.: 11:28:48.15
Dec.: +17:04:18.0

This source is not visible in the SDSS and it is the afterglow of GRB 130603B. We obtain a preliminary magnitude of r = 20.9 calibrated against SDSS (DR9). The afterglow is located ~0.8" SW of the host galaxy nucleus.

Our results are consistent with those of Levan et al. (GCN 14742).

[GCN OPS NOTE(06jun13):  Per author's request, the author list was changed;
1 was dropped and 4 were added.]


GRB_name: GRB130603B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14744
SUBJECT: GRB 130603B: Short GRB afterglow spectrum from GTC
DATE:    13/06/04 00:38:17 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

C. C. Thne (IAA-CSIC), A. de Ugarte Postigo (IAA-CSIC/DARK), J. Gorosabel (IAA-CSIC/UPV-EUH), N. Tanvir (U. Leicester), and J. P. U. Fynbo (DARK/NBI) report:

We obtained spectroscopy of the afterglow (GCN 14742, Levan et al, GCN 14743, de Ugarte Postigo et al.) of the short GRB 130603B (GCN 14735, Melandri et al.) with OSIRIS/GTC starting at 23:05 UT. Three spectra of 900s were obtained with grism R1000B. The afterglow lies on top of an SDSS galaxy as noted in Levan et al.

The spectrum shows a strong trace of the afterglow with absorption lines of the Ca II doublet as well as MgII and MgI. Superimposed are emission lines from the host galaxy of [OII], [OIII], Hbeta and Hgamma extended in the spatial direction. Absorption and emission lines lie at a common redshift of z=0.356. We therefore determine this to be the redshift of the short GRB and its host galaxy. 

We acknowledge the excellent support by the GTC staff, in particular Rene Rutten and David Garcia.


GRB_name: GRB130603B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14745
SUBJECT: GRB 130603B: Magellan redshift confirmation
DATE:    13/06/04 00:49:03 GMT
FROM:    Ryan Chornock at Harvard  <rchornock@cfa.harvard.edu>

R. J. Foley, R. Chornock, W. Fong, E. Berger (Harvard), S. Jha (Rutgers)
report:

We observed the field of the short-duration GRB 130603B (Melandri et
al., GCN 14735) with the Inamori Magellan Areal Camera and
Spectrograph (IMACS) mounted on the Magellan/Baade 6.5-m telescope
starting on 2013 Jun 04.004 UT (8.3-hr after the BAT trigger). In
600-s of r-band imaging, we detect the optical afterglow and host
galaxy (Levan et al., GCN 14742; de Ugarte Postigo et al., GCN
14743).  A 1200-s spectrum reveals several nebular emission lines from the host 
galaxy at a common redshift of 0.356, confirming the results of Thoene et al. 
(GCN 14744).


GRB_name: GRB130603B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14746
SUBJECT: GRB 130603B: Swift-BAT Spectral lag analysis
DATE:    13/06/04 02:39:24 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. Norris (BSU), N. Gehrels (GSFC), S. D. Barthelmy (GSFC), T. Sakamoto (AGU)

We report the spectral lag analysis for GRB 130603B (GCN Circ. 14735 & 14740)
based on the BAT data.  Using 2-ms binned light curves, the spectral lag
for the 15-25 keV to 50-100 keV bands is 0.6 +-0.7 ms, and -2.5 +-0.7 mc
for the 25-50 keV to 100-350 keV bands for both peaks combined.
These lag values and the hard spectrum (GCN Circ. 14741) place
this burst in the short burst category.  There is no evidence
for extended emission at the 0.005 cnts/det/sec level.


GRB_name: GRB130603B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14747
SUBJECT: GRB 130603B: optical follow-up and independent GTC redshift  determination and afterglow spectrum
DATE:    13/06/04 03:05:17 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

R. Snchez-Ramrez, A. J. Castro-Tirado (IAA-CSIC), J. Gorosabel
(IAA-CSIC, UPV-EHU), F. J. Aceituno (IAA-CSIC), E. Sonbas (Adiyaman
Univ.), E. Gogus, T. Gver (Sanbaci Univ.), H. Kirbiyik (TUG) and D.
Garca-Alvrez (GTC) on behalf of a larger collaboration, report:

We have observed the optical afterglow of the short-duration GRB 130603B
(Melandri  et al. GCNC  14735, Norris et al. GCNC 14746). Optical images
have been obtained with the 1.0m telescope at the Tbitak National
Observatory (Antalya, Turkey) in the R-band and with the 1.5m telescope at
Observatorio de Sierra Nevada (Granada, Spain) in the I-band, starting on
June 3. 771 and June 3.854 UT (2.69 hr and 4.69 hr post burst)
respectively. Spectra covering the range 3500-10000 A  were obtained  with
the 10.4m GTC (+OSIRIS) starting on June 3.993 UT (i.e. 8 hr post burst). 
At the position of the optical afterglow (Levan et al. GCNC  14742) the
afterglow spectrum shows Ca II in absorption, and we detect significant
contribution of the underlying host galaxy (eg. [OII], [OIII], H-beta and
H-alpha emission lines about 1 off), implying altogether a redshift of z
= 0.356, consistent with the values provided by Thoene et  al. (GCNC 
14744) and Foley et al. (GCNC 14745).


GRB_name: GRB130603B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14748
SUBJECT: GRB 130603B: Gemini Observations
DATE:    13/06/04 03:11:31 GMT
FROM:    Antonino Cucchiara at UCSC/UCO Lick  <acucchia@ucolick.org>

A. Cucchiara (UCSC/UCO Lick), D. Perley (Caltech), and
S. B. Cenko (GSFC) report on behalf of a larger collaboration:

On June 3.97 UT we start observing the optical afterglow 
of the Short GRB 130603B (Melandri et al. GCN 14735,
Evans et al., GCN 14739, Levan et al. GCN 14742, and 
de Ugarte Postigo et al. GCN 14743) with the Gemini-South
telescope equipped with the GMOS camera.
The observation sequence consists of a series of 8x3min
exposures in the g',r' and i' filters.

The OT is clearly detected in individual exposures.  
Using the coadded frames and a 0.7" aperture, 
we estimate the following magnitudes:

g = 21.7 +/- 0.2
r = 21.2 +/- 0.1
i = 20.7 +/- 0.2

These are not corrected for Galactic extinction or for 
contribution of the host galaxy, which is likely significant.
An RGB image of the field showing the optical transient has been 
posted to:
http://www.astro.caltech.edu/~dperley/gcn/130603b/130603b_gmos.png

Also, a spectroscopic sequence was obtained: based on CaHK lines and 
several emission lines we confirm the redshift of GRB 130603B to be
z=0.356 (as also reported by Thoene et al. GCN. 14744, Foley 
et al. 14745).

We thank the Gemini South Staff, in particular A. Cardwell, J. Turner
and Mischa Schirmer, for the excellent support.


GRB_name: GRB130603B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14749
SUBJECT: GRB 130603B: Swift-XRT refined Analysis
DATE:    13/06/04 04:15:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.A. Kennea (PSU), M.C. Stroh (PSU), D.N. Burrows (PSU), A.P. Beardmore
(U. Leicester), P.A. Evans (U. Leicester), B.P. Gompertz (U.
Leicester), G. Stratta (ASDC), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC)
and A. Melandri report on behalf of the Swift-XRT team:

We have analysed 6.6 ks of XRT data for GRB 130603B (Melandri  et al.
GCN Circ. 14735),  from 43 s to 28.2 ks after the  BAT trigger. The
data comprise 378 s in Windowed Timing (WT) mode (the first 9 s were
taken while Swift was slewing) with the remainder in Photon Counting
(PC) mode. The enhanced XRT position for this burst was given by Evans
et al. (GCN. Circ 14739).

The light curve can be modelled with an initial power-law decay with an
index of alpha=0.35 (+0.08, -0.09), followed by a break at T+2404 s to
an alpha of 1.46 (+0.13, -0.12).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.97 (+0.23, -0.22). The
best-fitting absorption column is  2.8 (+1.0, -0.8) x 10^21 cm^-2, in
excess of the Galactic value of 1.9 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.21 (+0.18, -0.17)
and a best-fitting absorption column of 2.5 (+/-0.5) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.6 x 10^-11 (6.2 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.5 (+/-0.5) x 10^21 cm^-2
Galactic foreground: 1.9 x 10^20 cm^-2
Excess significance: 7.7 sigma
Photon index:      2.21 (+0.18, -0.17)

If the light curve continues to decay with a power-law decay index of
1.46, the count rate at T+24 hours will be 4.7 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.7 x
10^-13 (2.9 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00557310.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB130603A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14750
SUBJECT: GRB 130603A: SON optical observations
DATE:    13/06/04 06:39:09 GMT
FROM:    Arto Oksanen at Nyrola Obs., Finland  <oksanen@nyrola.jklsirius.fi>

P. Kehusmaa, A. Oksanen and C. Harlingten report on behalf of 
the Searchlight Observatory Network:

On 2013 June 03, starting at 06:42 UT (T0+42.5 minutes), we observed 
the field of GRB130603A (Melandri et al., GCN Circ. 14731) with 
the 0.40 m NM1 telescope located in New Mexico, USA with Apogee Alta 
U42 CCD for 3x120 seconds using the V filter and 7x120 seconds unfiltered. 
The afterglow reported by Melandri et. al. (GCNC 14732) is detected in 
all unfiltered images and in the coadded V band image.
 
We report following differental photometry:

UTC (mid)            T0+(h)    Mag     Err   Filter
----------------------------------------------------------
2013-06-03T06:44:21  0.75      18.78   0.13  V 
2013-06-03T06:59:55  1.00      18.79   0.07  clear
----------------------------------------------------------

The reference magnitude from the nearby USNO B1.0 star (1729-0016610) 
with R=16.49.

A snapshot showing our coadded unfiltered image can be found at the URL
http://pilvi.dyndns.org/arto/GRB130603A_C_840s.jpg


GRB_name: GRB130603B
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14751
SUBJECT: GRB 130603B: 5.8 GHz VLA detection
DATE:    13/06/04 06:57:59 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

W. Fong, B. A. Zauderer and E. Berger (Harvard) report:

"We observed the position of the short-duration GRB 130630B (Melandri
et al., GCN 14735) with the Karl G. Jansky Very Large Array (VLA)
beginning on 2013 June 03.98 UT (7.6 hr post-burst) at a mean
frequency of 5.8 GHz. In 1 hour of observations, we detect a ~0.2 mJy
radio source in coincidence with the reported optical afterglow (Levan
et al., GCN 14742; de Ugarte Postigo et al., GCN 14743; Foley et al.,
GCN 14745; Cucchiara et al., GCN 14748).

We note that this is only the fourth detection of radio emission from
a short GRB, of which one case (GRB 120804A; Berger et al., 2013, ApJ,
765, 121) was due to host galaxy emission.

Further observations are planned. We thank the VLA staff for quickly
executing these observations."


GRB_name: GRB130604A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14752
SUBJECT: GRB 130604A: Swift detection of a burst
DATE:    13/06/04 07:08:43 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB), C. Gronwall (PSU),
C. B. Markwardt (NASA/GSFC), C. Pagani (U Leicester),
D. M. Palmer (LANL), M. H. Siegel (PSU) and
R. L. C. Starling (U Leicester) report on behalf of the Swift Team:

At 06:54:26 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130604A (trigger=557354).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 250.080, +68.210 which is 
   RA(J2000) = 16h 40m 19s
   Dec(J2000) = +68d 12' 36"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
FRED-like structure with a duration of about 70 sec.  The peak count 
rate was ~1500 counts/sec (15-350 keV), at ~5 sec after the trigger. 

The XRT began observing the field at 06:56:06.2 UT, 99.3 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source with an enhanced position: RA, Dec 250.1889,
68.2260 which is equivalent to:
   RA(J2000)  = 16h 40m 45.34s
   Dec(J2000) = +68d 13' 33.6"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 156 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper.  We cannot determine whether the source is
fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 4.70
x 10^20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 1.76e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT data are not available at this time. Analysis is awaiting the full
data set. 

Burst Advocate for this burst is A. Melandri (andrea.melandri AT brera.inaf.it). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB130604A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14753
SUBJECT: GRB 130604A: P60 optical afterglow candidate
DATE:    13/06/04 07:20:17 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) reports on behalf of a larger collaboration:

The Palomar 60-inch telescope responded automatically to GRB 130604A 
(Melandri et al., GCN 14752) and began a series of images at 06:58:16 
UT, three minutes after the alert notice.  We detect a faint (~20 mag) 
source near the center of the XRT error circle in the initial 60-second 
r-band and i-band exposures.  It is not clearly detected in z-band.  The 
coordinates of the optical transient candidate are:

RA  = 16:40:45.290
DEC = +68:13:33.58
(+/- 0.9", J2000)

Observations are continuing.


GRB_name: GRB130604A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14754
SUBJECT: GRB 130604A: KAIT optical upper limit
DATE:    13/06/04 08:41:19 GMT
FROM:    Weikang Zheng at U.of Michigan  <zwk@umich.edu>

WeiKang Zheng and Alexei V. Filippenko (UC Berkeley) report on behalf of
the KAIT GRB team:

We observed the afterglow of GRB 130604A (Melandri et al., GCN 14752)
with the 0.76-m Katzman Automatic Imaging Telescope (KAIT) located at
Lick Observatory. Observations started at 06:57:07 UT, 161 s after the
burst, with an automatic sequence in V, I, and clear filters (20 s
exposure for each image). We do not detect the afterglow at the position
reported by Perley (GCN 14753). We estimate the limiting magnitude in
our first clear-band (close to R) image to be about 18.5 at a time of
330 s after the burst. 

Continuing observations are in progress.


GRB_name: GRB130603A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14755
SUBJECT: GRB 130603A: MITSuME Akeno Optical observation
DATE:    13/06/04 09:17:36 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

K. Ito, Y. Saito, Y. Yano, R. Usui, Y. Tachibana, T. Yoshii,
S. Kurita, Y. Yatsu, and N. Kawai (Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 130603A (Melandri et al., GCNC 14731) with the 
optical three color (g, Rc, and Ic) CCD cameras attached to the MITSuME 50 cm
telescope of Akeno Observatory, Yamanashi, Japan.

The observation started on 2013-06-03 10:10:04 UT ( ~4.2 h after
the burst). And we could not find any new point source within the XRT
error circle (Beardmore et al., GCNC 14737) in all the three bands.

The results of photometry (3 sigma upper limits) are listed below.
We used GSC2.3 catalog for flux calibration.


T0+[hour]     MID-UT   T-EXP[sec]             g'             Rc                Ic
--------------------------------------------------------------------------------------------
       4.175   12:30:14              9054      >19.4        >19.4        >18.7
--------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst [hour]
T-EXP: Total Exposure time [sec]


GRB_name: GRB130604A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14756
SUBJECT: GRB 130604A: ISON-NM optical upper limit
DATE:    13/06/04 09:48:21 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

L. Elenin (KIAM),  V. Savanevych (KNURE),  A. Bryukhovetskiy (NSFCTC),  I. 
Molotov (KIAM), A. Pozanenko (IKI) report on behalf of  larger GRB 
follow-up collaboration:

We observed of  the field of  the Swift GRB 130604A (Melandri et al., GCN 
14752)  with 0.45-m telescope of ISON-NM observatory on June. 04 (UT) 
06:56:11, i.e. 105 s after burst trigger. Series of 30 s and 60 s exposures 
were obtained in clear filter. In the combined image of the first 3 images 
we do not detect afterglow candidate (Perley, GCB 14753).  Preliminary 
photometry  is based  on the USNO-B1.0 (R2)  nearby  stars:

UT start,      T0+        Exposure,  OT,              UL (3 sigma)
                   days      s

06:56:11       0.0019  3x30           n/d              19.7


GRB_name: GRB130603B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14757
SUBJECT: GRB 130603B: VLT/X-shooter redshift confirmation
DATE:    13/06/04 10:38:37 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), D.
Malesani (DARK/NBI), S. Schulze (PUC and MCSS), J. P. U. Fynbo, D. J.
Watson (DARK/NBI), V. D'Elia (ASI-SDC, INAF OAR), P. Goldoni (APC,
CEA/Irfu), M. Vestergaard (DARK/NBI) report on behalf of the X-shooter
GRB GTO collaboration:

We observed the optical afterglow of the short-duration GRB 130603B
(Melandri et al., GCN 14735; Levan et al., GCN 14742; de Ugarte
Postigo et al., GCN 14743) using the ESO VLT equipped with the
X-shooter spectrograph. The observations started on 2013-06-04 at
00:00:28 UT (i.e., 8.187 hr after the burst). A total exposure of
4x600 s was obtained, covering the spectral range from ~300 to ~2100
nm.

A continuum is detected in all the UVB/VIS/NIR arms of the spectra. We
identify several absorption features which we interpret as Ca II H & K
and Mg II from the optical afterglow, as well as emission lines such
as the [O II] doublet, [O III], H-alpha, H-beta, and [S II] from the
host galaxy, all at a common redshift of z=0.3564+/-0.0002, fully
consistent with the measurements by Thoene et al. (GCN 14744), Foley
et al. (GCN 14745), and Sanchez-Ramirez et al. (GCN 14747).

We thank the Paranal staff for enthusiastic support, in particular
Cedric Ledoux and Alex Correa.


GRB_name: GRB130604A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14758
SUBJECT: GRB 130604A: further ISON-NM optical observation
DATE:    13/06/04 11:11:35 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

L. Elenin (KIAM),  V. Savanevych (KNURE),  A. Bryukhovetskiy (NSFCTC),  I. 
Molotov (KIAM), A. Pozanenko (IKI) report on behalf of  larger GRB follow-up 
collaboration:

After further inspection of images after observation of the Swift GRB 
130604A (Melandri et al., GCN 14752)  with 0.45-m telescope of ISON-NM 
(Elenin, et al., GCN 14756) we identified faint object (S/N ~ 3) in 
coordinates (J2000) 16 40 45.34   +68 13 34.5  with uncertainty of  0.2" (in 
both coordinates). Within errors this position coincides with the afterglow 
candidate (Perley, GCB 14753) and the error circle of XRT reported by 
Melandri et al. (GCN 14752). This object is not detected in our later 
combined images and can be the afterglow of GRB 130604A. Preliminary 
photometry  of our images obtained in clear filter is based  on USNO-B1.0 
(R2)  nearby  stars:

UT start,      T0+          Exposure,  OT,                 UL (3 sigma)
                   mid,days  s

06:56:11       0.0019    3x30           n/d                  19.7
06:56:11       0.0035    9x30           20.3 +/- 0.3      20.0
06:56:11       0.0091  30x30           n/d                  20.5
06:56:11       0.0171  60x30           n/d                  20.8

Finding chart can be found at 
http://grb.rssi.ru/GRB130604A/GRB130604A_ISON_NM_9x30.png 


GRB_name: GRB130603B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14759
SUBJECT: GRB130603B: Swift/UVOT detection
DATE:    13/06/04 11:59:05 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <m.depasquale@ucl.ac.uk>

M. De Pasquale (MSSL-UCL) and A. Melandri (INAF-OAB)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130603B
62 s after the BAT trigger (Melandri et al., GCN Circ. 14735).
A source 2'' from the centre of the XRT error circle (Evans et al. GCN Circ.
14739) and coincident with the optical afterglow detected by WHT
(Levan et al., GCN circ. 14742) and NOT (de Ugarte Postigo et al., GCN circ.
14743) is detected in UVOT exposures.

The source, in UVOT images, shows no clear fading behaviour between the
first and the latest exposures.

Preliminary detections and 3-sigma upper limits using the UVOT 
photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early 
exposures are:

Filter  T_start(s)   T_stop(s)    Exp(s)           Mag

white       62         4981        383       20.81 0.17
v          605         5393        225      >19.8
b          530         6212        432       21.14 0.45 (2.5 sigma)
u          275         6007        659       20.87 0.39 (2.8 sigma)
w1         654         5802        413      >20.6
m2        3960         5597        393      >20.4
w2         580         6555        365       20.69 0.39 (2.8 sigma)


The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.02 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB130604A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14760
SUBJECT: GRB 130604A: MITSuME Okayama upper limits
DATE:    13/06/04 15:15:58 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ),
S. Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech)
report on behalf of MITSuME and OISTER collaboration:

We observed the field of GRB 130604A (Melandri et al., GCNC 14752)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.

The observation started on 2013-06-04 11:52:48 UT (~5.0 h after the burst).
We could not detect the previously reported afterglow
(Perley, GCNC 14753; Elenin et al., GCNC 14758) in all the three bands.

Three sigma upper limits of the OT are listed below.
We used GSC 2.3 catalog for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'     Rc     Ic
-----------------------------------------------------
0.24913    12:53:10    6360.0   >20.3  >20.2  >19.5
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB130603B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14761
SUBJECT: GRB 130603B: P60 Observations
DATE:    13/06/04 15:54:39 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (GSFC) and D. A. Perley (Caltech) report on behalf of a larger
collaboration:

We have imaged the field of the short-hard GRB 130603B (Melandri et al.,
GCN 14735) with the robotic Palomar 60 inch telescope.  Images were
obtained in the r' and i' filters beginning at 04:00 on 2013 June 4 (~
12.2 hr after the Swift trigger).

At the location of the optical afterglow (Levan et al., GCN 14742), we
detect a source mildly blended with the presumed host galaxy.  Using a
large aperture to include both objects, we measure a magnitude of r' =
20.8 at this time (calibrated with respect to several nearby point sources
from SDSS).


GRB_name: GRB130604A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14762
SUBJECT: GRB 130604A: Gemini North Spectroscopy
DATE:    13/06/04 16:07:17 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (GSFC), N.R. Tanvir (Leicester)D. A Perley (Caltech), A. J. Levan (U. Warwick), and
A. Cucchiara (UCSC / Lick) report on behalf of a larger collaboration:

We have obtained optical spectra of the afterglow (Perley et al., GCN
14753) of GRB 130604A (Melandri et al., GCN 14752) with the Gemini
Multi-Object Spectrograph mounted on the 8 m Gemini North telescope.
Observations began at 8:16 UT on 2013 June 4 (~ 1.3 hr after the Swift
trigger) and cover the wavelength range from 4000 - 8000 A.

Superimposed on a faint continuum, we detect a single bright emission line
at an observed wavelength of ~ 7674.0 A.  There is some evidence the
emission line is spectrally resolved.  No other obvious features (in
emission or absorption) are detected over our wavelength range.  If we
assume this feature corresponds to [O II], this implies a redshift of z =
1.06 for GRB 130604A.

[GCN OPS NOTE(04Jun13): Per author's request, NRT was added to the author list.]


GRB_name: GRB130604A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14763
SUBJECT: GRB 130604A: Enhanced Swift-XRT position
DATE:    13/06/04 16:19:19 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 832 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 130604A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 250.18823, +68.22651 which is equivalent
to:

RA (J2000): 16h 40m 45.18s
Dec (J2000): +68d 13' 35.4"

with an uncertainty of 2.1 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB130603B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14764
SUBJECT: GRB 130603B: RATIR Optical and NIR Observations
DATE:    13/06/04 17:49:36 GMT
FROM:    Eleonora Troja at GSFC  <eleonora.troja@nasa.gov>

Eleonora Troja (GSFC), Nat Butler (ASU), Alan M. Watson (UNAM),
Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM),
Chris Klein (UCB), Ori Fox (UCB) J. Xavier Prochaska (UCSC), Josh Bloom
(UCB), Antonino Cucchiara (UCSC), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), Jos A. de Diego (UNAM), Leonid Georgiev (UNAM),
Jess Gonzlez (UNAM), Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC),
and Harvey Moseley (GSFC) report:

We observed the field of GRB 130603B (Melandri, et al., GCN 14735) with the
Reionization and Transients Infrared Camera (RATIR;www.ratir.org 
<http://www.ratir.org>) on the
1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional on
Sierra San Pedro Mrtir from 2013/06 4.16 to 2013/06 4.27 UTC (12.01
to 14.78 hours after the BAT trigger), obtaining a total of 1.93 hours
exposure in the r' and i' bands and 0.81 hours exposure in the Z,
Y, J, and H bands.

At the location of the optical afterglow (Levan et al., GCN 14742),
in comparison with SDSS DR8 and 2MASS, we obtain the following detections:

    r'    20.78 +/- 0.03
    i'    20.52 +/- 0.03
    Z    20.20 +/- 0.05
    Y    19.94 +/- 0.05
    J     19.97 +/- 0.06
    H    19.55 +/- 0.06

These magnitudes are in the AB system and not corrected for Galactic
extinction in the direction of the GRB.
Photometry was performed adopting a large aperture which includes both the
afterglow and its host galaxy.

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB130604B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14765
SUBJECT: GRB 130604B: Fermi GBM detection
DATE:    13/06/04 18:03:38 GMT
FROM:    Andrew Collazzi at NASA/MSFC/ORAU  <andrew.collazzi@nasa.gov>

Andrew C. Collazzi (NASA/ORAU)
reports on behalf of the Fermi GBM Team:

"At 00:48:11.32 UT on 4 June 2013, the Fermi Gamma-ray
Burst Monitor (GBM) triggered and located GRB 130604B 
(trigger 391999694 / 130604.033).  The on-ground calculated 
location, using the Fermi GBM trigger data, is RA = 292.18,
Dec = -24.86 (J2000 degrees, equivalent to J2000 
19h 28m, -24d 51'), with a statistical uncertainty of 1.2 degrees
(radius, 1-sigma containment, statistical only; there is 
additionally a systematic error which is currently estimated to
be 2 to 3 degrees).  The angle from the Fermi LAT 
boresight is 93 degrees.

The GBM light curve shows a multi-peak burst with a duration (T90)
of about 27 s (50 - 300 keV).  The time-averaged
spectrum from T0-8.192 to T0+35.841 s is well fit by a Comptonized
spectrum with Epeak = 227.6 +/- 19.0 and alpha = -1.24 +/- 0.03.
The fluence (10-1000 keV) in this time interval is 
(1.79 +/- 0.06)E-05 erg/cm^2. The burst has a 1.024-s peak flux
(10-1000 keV) of 13.24 +/- 0.37 ph/cm^2/s that starts at
T+15.744 s.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB130604A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14766
SUBJECT: GRB 130604A: Swift-XRT refined Analysis
DATE:    13/06/05 07:08:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

M.C. Stroh (PSU), D.N. Burrows (PSU), P.A. Evans (U. Leicester), B.P.
Gompertz (U. Leicester), J.P. Osborne (U. Leicester), P. D'Avanzo
(INAF-OAB), V. D'Elia (ASDC), A. Maselli  (INAF-IASFPA), J.A. Kennea
(PSU) and A. Melandri report on behalf of the Swift-XRT team:

We have analysed 5.7 ks of XRT data for GRB 130604A (Melandri  et al.
GCN Circ. 14752),  from 105 s to 21.8 ks after the  BAT trigger. The
data comprise 146 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Goad et al. (GCN. Circ 14763).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=2.02 (+0.08, -0.06).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.10 (+0.13, -0.12). The
best-fitting absorption column is  2.8 (+/-0.4) x 10^21 cm^-2, in
excess of the Galactic value of 4.7 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.1 (+/-0.3) and a
best-fitting absorption column of 2.2 (+1.0, -0.9) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.8 x 10^-11 (5.9 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.2 (+1.0, -0.9) x 10^21 cm^-2
Galactic foreground: 4.7 x 10^20 cm^-2
Excess significance: 3.3 sigma
Photon index:      2.1 (+/-0.3)

If the light curve continues to decay with a power-law decay index of
2.02, the count rate at T+24 hours will be 5.8 x 10^-5 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.2 x
10^-15 (3.5 x 10^-15) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00557354.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB130604A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14768
SUBJECT: GRB 130604A: Swift/UVOT Upper Limits
DATE:    13/06/05 10:15:08 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (MSSL-UCL) and A. Melandri (INAF-OAB) report on behalf of 
the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130604A 
109 s after the BAT trigger (Melandri et al., GCN Circ. 14752). No 
optical afterglow consistent with the optical position (Perley, GCN 
Circ. 14753) is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system 
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first finding 
chart (FC) exposure and subsequent exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white_FC           109          258          147         >20.4
white              109        17767         1345         >21.8
v                 5004        11999         1055         >20.3
b                 4388        16933         1278         >21.5
u                  267         5818          378         >20.0
w1                5414         5613          197         >20.0
m2                5208         5408          197         >19.7
w2                4798        11112         1082         >21.3

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 0.03 in the direction of the 
burst (Schlegel et al. 1998).


GRB_name: GRB130603B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14769
SUBJECT: GRB 130603B: AMI-LA 15GHz observations
DATE:    13/06/05 11:38:07 GMT
FROM:    Tim Staley at U of Southampton  <Tim.Staley@soton.ac.uk>

T.D. Staley, G.E. Anderson, R.P. Fender (U. of Southampton),
A. Rowlinson, A.J. van der Horst (U. of Amsterdam), D.J. Titterington,
C. Rumsey (MRAO) report on behalf of the 4 Pi Sky / AMI team:

We have observed the position of the GRB 130603B afterglow at multiple
epochs with the AMI Large Array at 15 GHz. Our initial observation was
for one hour starting at 15:53:42 UT on June 3rd, just under 5 minutes
after the GRB trigger time (GCN 14735). We also made longer observations,
at 3.12 and 22.8 hours post-burst. We do not detect the afterglow
in our preliminary reductions.

Preliminary analysis gives 3-sigma upper limits as follows:

Start (Hrs post burst) | Duration (hrs) |   3-sigma upper limit
---------------------------------------------------------------------
      0.08                       |            1          |      0.6 mJy
      3.12                       |            3          |      0.21 mJy
    22.8                         |            3          |      0.3 mJy

Further observations are scheduled.

These observations were initially triggered via the system described in
Staley et. al (2013, MNRAS, 428, 3114).


GRB_name: GRB130603B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14770
SUBJECT: GRB 130603B: MASTER-Net early observations and  optical sloap limit
DATE:    13/06/05 17:11:24 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

Maria Pruzhinskaya, D.Denisenko, E. Gorbovskoy, V. Lipunov, V.Kornilov, 
D.Kuvshinov, N.Tyurina, N.Shatskiy, P.Balanutsa, D.Zimnukhov, A.Kuznetsov, 
V.V.Chazov
Sternberg Astronomical Institute, Lomonosov Moscow State University


K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk
Irkutsk State University, Irkutsk

V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov, A.Gabovich
Blagoveschensk Educational State University, Blagoveschensk

A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory

V.Krushinski, I.Zalozhnih,  A. Popov
Ural Federal University, Kourovka

Hugo Levato and Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

Claudio Mallamaci, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)



MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Tunka was pointed to GRB130603B 35 sec after Notice time
and 52 sec after Trigger time (Melandri et al., GCN 14735) in two
mutually perpendicular polarizations.

We didn't find OT at the position reported by Levan et al., GCN 14742
and A. de Ugarte Postigo et al., GCN 14743.

Our photometry (upper limits) during the first 20 minutes until the
clouds started coming in is as follows:


t_UT                   Exp T-T_trig Limit Filter   Tube
-------------------------------------------------------
2013-06-03 15:50:06    10     52    15.4    P|       EAST
2013-06-03 15:50:07    10     53    15.1    P-       WEST
2013-06-03 15:51:06    20    112    15.9    P|       EAST
2013-06-03 15:51:07    20    113    15.8    P-       WEST
2013-06-03 15:52:08    30    174    16.2    P|       EAST
2013-06-03 15:52:08    30    174    16.1    P-       WEST
2013-06-03 15:53:18    50    244    16.7    P|       EAST
2013-06-03 15:53:19    50    245    16.7    P-       WEST
2013-06-03 15:55:01    70    348    16.7    P|       EAST
2013-06-03 15:55:02    70    349    16.6    P-       WEST
2013-06-03 15:56:48    90    454    17.2    P|       EAST
2013-06-03 15:56:49    90    455    16.9    P-       WEST
2013-06-03 15:58:57   120    583    17.6    P|       EAST
2013-06-03 15:58:58   120    584    17.5    P-       WEST
2013-06-03 16:01:43   150    749    18.0    P|       EAST
2013-06-03 16:01:43   150    749    17.6    P-       WEST
2013-06-03 16:04:54   180    940    18.0    P|       EAST
2013-06-03 16:04:54   180    940    17.5    P-       WEST

The OT upper limit available on the plot :

http://master.sai.msu.ru/static/OT/grb130306B.gif

We have tried to compare our data with the photometry from the large
telescopes in the filters similar to ours. In fact, we have used the
observations in r filter.
The following data have been published so far.

Afterglow:

t+5.8 hours r=20.94  WHT  Levan et al., GCN 14742
t+5.8 hours r=20.9   NOT  A. de Ugarte Postigo et al., GCN 14743
t+7.5 hours r=21.2   Gemini-South  Cucchiara et al., GCN 14748

Large aperture to include both objects:

t+12.2 hours r'=20.8  P60 (Palomar 60 inch)  Cenko et al., GCN 14761
t+14.78 hours r'=20.78 RATIR (1.5m Harold Johnson)  Eleonora Troja et
al., GCN 14764

We were not able to use the Swift UVOT data in the white light (De
Pasquale et al., GCN 14759) since their exact times of mid-exposures
are not easy to determine.
Obviously, the last two points involve the host galaxy.
In order to constrain the slope we have used the data from WHT, NOT
and Gemini South.
The results are presented here:

http://master.sai.msu.ru/static/OT/grb130306B_all.gif

Thus, supposing the power law of the fading afterglow

F ~ t^-alpha

we are providing the following limitation:

alpha < 0.84.

The message may be cited.


GRB_name: GRB130603B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14771
SUBJECT: Konus-Wind observation of GRB 130603B
DATE:    13/06/05 17:33:26 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf
of the Konus-Wind team, report:

The bright short-duration hard GRB 130603B
(Swift-BAT trigger 557310: Melandri, et al., GCN 14735;
Barthelmy et al., GCN 14741)
triggered Konus-Wind at T0=56956.448s UT (15:49:16.448)

The light curve shows a multi-peaked structure
from ~T0-0.008 s to ~T0+0.082 s.
The total duration of the burst is ~0.090 s

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130603_T56956/

As observed by Konus-Wind, the burst
had a fluence of (6.6  0.7)x10-6 erg/cm2,
and a 16-ms peak flux, measured from T0,
of (1.0  0.2)x10-4 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The spectrum of the burst (measured from T0 to T0+0.128 s)
is best fit in the 20 keV - 15 MeV range
by the cutoff power law with the following model parameters:
the photon index alpha = -0.73  0.15,
the peak energy Ep = 660  100 keV,
chi2 = 67/69 dof.

All the quoted results are preliminary.


GRB_name: GRB130603B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14772
SUBJECT: GRB 130603B: rest-frame energetics in gamma-rays
DATE:    13/06/05 18:10:23 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

D. Frederiks, on behalf of the Konus-Wind team, report:

Assuming z=0.356 (ThÃ¶ne et al., GCN 14744),
and a standard cosmology model with H_0 = 70 km/s/Mpc,
Omega_M = 0.27, and Omega_Lambda = 0.73,
we estimate the following rest-frame parameters of GRB 130603B
from the Konus-Wind observation of the burst (Golenetskii et al., GCN 14771):
the isotropic energy release E_iso is (2.1 Â± 0.2)x10^51 erg,
the peak luminosity (L_iso)_max is (4.4 Â± 0.8)x10^52 erg/s,
and the rest-frame peak energy Ep,i = (900 Â± 140) keV


GRB_name: GRB130605A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14773
SUBJECT: GRB 130605A: Swift detection of a burst
DATE:    13/06/06 00:04:39 GMT
FROM:    Stephen Holland at STScI  <sholland@stsci.edu>

S. T. Holland (STScI), S. D. Barthelmy (GSFC),
J. R. Cummings (NASA/UMBC), N. Gehrels (NASA/GSFC),
J. A. Kennea (PSU), D. Malesani (DARK/NBI),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
A. Melandri (INAF-OAB), M. H. Siegel (PSU) and
M. Stamatikos (OSU/NASA/GSFC) report on behalf of the Swift Team:

At 23:41:42 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130605A (trigger=557508).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 134.524, -33.489 which is 
   RA(J2000) = 08h 58m 06s
   Dec(J2000) = -33d 29' 20"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single peak
with a duration of about 8 sec.  The peak count rate was ~2000 counts/sec 
(15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 23:43:14.6 UT, 92.6 seconds after
the BAT trigger. No source was detected in the 2.5-s promptly available
image. We are waiting for the full dataset to detect and localise the
XRT counterpart. No prompt event mode data were available as Swift entered
the SAA shortly after the burst was detected. 

UVOT took a finding chart exposure of 107 seconds with the White filter
starting 95 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 25% of
the BAT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
BAT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.36. 

Burst Advocate for this burst is S. T. Holland (sholland AT stsci.edu). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB130605A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14774
SUBJECT: GRB 130605A: GROND afterglow candidate
DATE:    13/06/06 00:28:23 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

Nicuesa Guelbenzu, A. (TLS Tautenburg), J. Greiner, Varela, K. (MPE 
Garching), S. Klose, D. A. Kann (TLS Tautenburg) report on behalf of the 
GROND team:

We observed the field of GRB 130605A (Swift trigger 557508; Holland et 
al., GCN 14773) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 
2008, PASP 120, 405) mounted at the 2.2m MPG/ESO telescope at La Silla 
Observatory (Chile).

Observations started at 23:44:36 UT on June 6, about 3 min after the GRB 
trigger. Inside the BAT error circle (Holland et al., GCN 14773) we find a 
source at coordinates RA, DEC (J2000) = 08:58:08.6, -33:27:40.3 which has 
no counterpart on the DSS2 red. We measure the following preliminary AB 
magnitude (mean time 23:47:39)

r' = 15.8 +/- 0.1,

calibrated against GROND zeropoints and 2MASS stars. We suggest that this 
is the GRB afterglow.


GRB_name: GRB130605A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14775
SUBJECT: GRB 130605A: TAROT La Silla observatory optical detection of the afterglow
DATE:    13/06/06 00:39:55 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (IRAP-CNRS-OMP),
Boer M., Siellez K., Dereli H., Bardho O. (UNS-CNRS-OCA),
Atteia J.L. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 130605A detected by SWIFT
(trigger 557508) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 32.7s after the GRB trigger
(12.8s after the notice). The elevation of the field decreased from
51 degrees above horizon and weather conditions
were excellents.

We detect a new fading source in the error box given by SWIFT
at the following position (+/- 3 arcsec):

RA(J2000)  = 08h 58m 08.53s
DEC(J2000) = +33d 27' 40.1"

OT was R = 15.1 at  121s after GRB.
OT was R = 18.4 at 1705s after GRB.

The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
The afterglow is seen but the trail is overlaped
by another star and will be analyzed in details
later.

Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.

N.B. Galactic coordinates are lon=257.1493 lat= +7.9340
and the galactic extinction in R band is about 0.9 magnitude
estimated from D. Schlegel et al. 1998ApJ...500..525S.


GRB_name: GRB130605A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14776
SUBJECT: GRB 130605A: Skynet/PROMPT detection of a fading afterglow
DATE:    13/06/06 00:50:18 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, A. Lacluyze, D. Reichart, J. Haislip, T. Berger, M. Carroll, 
H. T. Cromartie, R. Egger, A. Foster, C. Foster, N. Frank, K. Ivarsen, 
D. James, M. Maples, J. Moore, M. Nysewander, E. Speckhard, P. Taylor 
and J. A. Crain report

Skynet observed the Swift/BAT localization of GRB 130605A (Holland et 
al., GCN 14773, Swift trigger #557508) with three 16" telescopes of the 
PROMPT array at CTIO, Chile.  Starting at 2013-06-05, 23:43:23 UT 
(t=101s post-trigger)

We detect a fading afterglow in B, V and I bands at the position 
reported by Guelbenzu et al. (GCN 14774).  Preliminary magnitudes at 
t=10.4m are
B = 17.9
V = 17.1
I = 15.7
Magnitudes are in the Vega system, calibrated to 3 APASS stars in the 
field, and are not corrected for Milky Way extinction.

Skynet observations are ongoing.


GRB_name: GRB130605A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14777
SUBJECT: GRB 130605A: TAROT La Silla observatory optical decay
DATE:    13/06/06 03:01:51 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (IRAP-CNRS-OMP),
Boer M., Siellez K., Dereli H., Bardho O. (UNS-CNRS-OCA),
Atteia J.L. (IRAP-CNRS-OMP) report:

We analyzed TAROT La Silla images taken during the first hours
after the GRB 130605A (Holland et al. GCNC 14773).
We have a photometric follow-up of the afterglow
detected by Nicuesa Guelbenzu et al. (GCNC 14774).

All TAROT magnitudes are computed using the reference star
NOMAD-1 0565-0204137 (RA = 134.5240528 Dec. = -33.4675072 R=12.50).

The first TAROT image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
After substraction of an overlaped star we can mesure the
continuous photometry between 32.7 and 92.7s:

 From 32.7s to 58.5s the magnitude rises steeply until R = 14.85
 From 58.5s to 92.7s the magnitude stays at about the level R = 14.9

Then the decay is recorded using the later images:

  Tstart  Tstop  Rmag  1sig
  (sec)   (sec)
   106.3  136.3  15.20 0.02
   146.8  176.8  15.43 0.02
   187.4  217.4  15.56 0.02
   227.7  257.7  15.70 0.03
   268.5  298.5  16.10 0.02
   308.8  398.8  16.17 0.02
   409.4  499.4  16.45 0.04
   509.9  599.9  16.71 0.08
   610.5  700.5  16.98 0.04
   711.3 1161.3  17.88 0.07
  1113.3 1203.3  18.36 0.29
  1414.9 1684.9 >18.57
  1515.5 4845.5 >19.41

The light curve can be fitted in three parts implying
two breaks at 284s and 656s:

 From  76s to 284s alpha=0.65
 From 284s to 656s alpha=1.3
Beyond 656s       alpha=2.2

This message can be cited.


GRB_name: GRB130605A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14778
SUBJECT: GRB 130605A: Continued Skynet/PROMPT observations
DATE:    13/06/06 03:45:50 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, A. Lacluyze, D. Reichart, J. Haislip, T. Berger, M. Carroll, 
H. T. Cromartie, R. Egger, A. Foster, C. Foster, N. Frank, K. Ivarsen, 
D. James, M. Maples, J. Moore, M. Nysewander, E. Speckhard, P. Taylor 
and J. A. Crain report

Skynet observed the Swift/BAT localization of GRB 130605A (Holland et 
al., GCN 14773, Swift trigger #557508) with three 16" telescopes of the 
PROMPT array at CTIO, Chile,  starting at 2013-06-05, 23:43:23 UT 
(t=101s post-trigger), and continuing until t=3h. Exposure lengths range 
from 10s at early times to 160s at later times.  Multiple 160s exposures 
were stacked at later times to increase sensitivity.

We detect a fading afterglow in B, V and I bands at the position 
reported by Nicuesa Guelbenzu et al. (GCN 14774), at:
RA   08:50:08.6
Dec -33:27:40.3

 From t=1.7m to t=9m, the afterglow fades with an approximate temporal 
index alpha~-0.7, after which it steepens to alpha~-1.4.  A preliminary 
light curve is at:
http://www.skynet.unc.edu/grb/grb130605a.png

Magnitudes are in the Vega system, calibrated to 3 APASS stars in the 
field, and are not corrected for the expected Milky Way extinction of 
E(B-V)=1.12 (Schlegel et al. 1998), which, assuming R_V=3.1, corresponds to:
band      B       V       I
A_lambda  1.57    1.17    0.71

No further Skynet observations are scheduled.


GRB_name: GRB130604A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14779
SUBJECT: GRB 130604A: Swift-BAT refined analysis
DATE:    13/06/06 12:26:59 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU),
C. B. Markwardt (GSFC), A. Melandri (INAF-OAB), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+962 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 130604A (trigger #557354)
(Melandri, et al., GCN Circ. 14752).  The BAT ground-calculated position is
RA, Dec = 250.166, 68.225 deg, which is 
   RA(J2000)  =  16h 40m 39.9s 
   Dec(J2000) = +68d 13' 28.4" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 81%.
 
The mask-weighted light curve shows a FRED-like peak starting at ~T-1 sec,
peaking at ~T+10 sec, and ending at ~T+90 sec.
T90 (15-350 keV) is 37.7 +- 4.6 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.44 to T+43.58 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.51 +- 0.12.  The fluence in the 15-150 keV band is 1.4 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+14.39 sec in the 15-150 keV band
is 0.8 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/557354/BA/


GRB_name: GRB130605A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14780
SUBJECT: GRB 130605A: Swift/UVOT Detection
DATE:    13/06/06 19:00:31 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

B. Porterfield (PSU) and S. T. Holland (STScI)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 
130605A 96 s after the BAT trigger (Holland et al., GCN Circ. 14773).
A source consistent with the optical position(Guelbenzu et al. GCN
Circ. 14774) is detected in the initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) = 08:58:08.61 = 134.53587 (deg.)
    Dec (J2000) = -33:27:40.2 = -33.46118 (deg.)
with an estimated uncertainty of 0.50 arc sec. (radius, 90% confidence).

Preliminary detections and 3-sigma upper limits using the
UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc.
1358, 373) for the early exposures are: 

Filter     T_start(s)   T_stop(s)     Exp(s)      Mag

white fc       95          202         105     16.40+-0.07
wh           5498         5698         196     21.04+-0.29
v            4474         6109         393     19.90+-0.36
b            5294        30053        1355    >21.70
u            5089        35820        3306    >21.45
w1           4884        35150        3778    >21.57
m2           4679        34243        2860    >21.02
w2           5705        39258         421    >20.27

The magnitudes in the table are not corrected for the Galactic
extinction due to the reddening of E(B-V) = 0.36 in the direction
of the burst (Schlegel et al. 1998).


GRB_name: GRB130606A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14781
SUBJECT: GRB 130606A: Swift detection of a burst
DATE:    13/06/06 21:25:59 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

T. N. Ukwatta (MSU), S. D. Barthelmy (GSFC), N. Gehrels (NASA/GSFC),
H. A. Krimm (CRESST/GSFC/USRA), D. Malesani (DARK/NBI),
F. E. Marshall (NASA/GSFC), A. Maselli (INAF-IASFPA),
A. Melandri (INAF-OAB), D. M. Palmer (LANL) and
M. Stamatikos (OSU/NASA/GSFC) report on behalf of the Swift Team:

At 21:04:39 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130606A (trigger=557589).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 249.403, +29.791 which is 
   RA(J2000) = 16h 37m 37s
   Dec(J2000) = +29d 47' 27"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked
structure.  The initial peak is about 10 sec long from T-5 to T+5 sec. 
Then at T+150 sec, there is a second, brighter peak of about 20 sec
duration. The peak count rate was ~2300 counts/sec (15-350 keV), 
at ~155 sec after the trigger. 

The XRT began observing the field at 21:05:51.4 UT, 72.4 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 249.39916,
29.79428 which is equivalent to:
   RA(J2000)  = 16h 37m 35.80s
   Dec(J2000) = +29d 47' 39.4"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 16 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (1.98 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 3.3
(+1.76/-1.58) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 1.64e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 80 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 
100% of the XRT error circle. The typical 3-sigma upper limit has been 
about 19.6 mag, but the trailed images will reduce the sensitivity slightly. 
No correction has been made for the expected extinction corresponding 
to E(B-V) of 0.02. 

The UVOT data shows stars trailing by about 10 arcseconds, which
may indicate pointing instability at this level.  Therefore
this uncertainty should be added to the nominal XRT location
for follow-up searches.  A refined aspect solution will be
generated from the full downlinked data. 

Burst Advocate for this burst is T. N. Ukwatta (tilan.ukwatta AT gmail.com). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB130606A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14782
SUBJECT: GRB 130606A: optical afterglow with BOOTES-2/TELMA and 1.23m CAHA
DATE:    13/06/06 22:10:41 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

M. Jelinek (IAA-CSIC), J. Gorosabel (UPV-EY, IAA-CSIC), A. J.
Castro-Tirado (IAA-CSIC),  S. Mottola (DLR), S. Hellmich (DLR), R.
Fernndez-Muoz (EELM-CSIC) and V. F. Muoz-Martnez (UMA), on behalf of a
larger collaboration, report:

"Following the detection of GRB 130606 by Swift (Ukwatta et al. GCNC
14781), follow-up observation were taken with the 0.6m TELMA telescope at
the BOOTES-2 station (Mlaga) and with the 1.23m CAHA telescope at the
German-Spanish Calar Alto Observatory, starting 21m postburst. At the edge
of the Swift/XRT error box we identify an optical source not present in
the DSS-2 with a magnitude of R about 18.5 which we identify as the
optical afterglow."

[GCN OPS NOTE(06jun13): Per author's request, the GRB name in the Title was corrected.]


GRB_name: GRB130606A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14783
SUBJECT: GRB 130606A: NOT afterglow detection
DATE:    13/06/06 22:29:03 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), D. Malesani (DARK/NBI), S. Schulze (PUC and MCSS),
N. R Tanvir (U. Leicester), D. J. Watson (DARK/NBI), J. Hjorth
(DARK/NBI), J. Datson (Tuorla Observatory, U. Turku), R. Salinas
(FINCA) report on behalf of a larger collaboration:

We observed the field of GRB 130606A (Ukwatta et al., GCN 14781) using
the 2.5m Nordic Optical Telescope (NOT) equipped with the MOSCA
imager. Observations started at 21:35 UT on 2013-06-06 (i.e., 0.5 hr
after the burst) and 2x300 s frames were obtained in the Sloan
r-filter.

Close to the refined XRT position, we detect an object not visible in
the DSS and SDSS images of the field, at the following coordinates:

RA (J2000) = 16:37:35.188
Dec(J2000) = +29:47:47.03

These coordinates are formally outside the XRT error circle, which is
however affected by extra systematic uncertainties due to the problems
in the satellite attitude (Ukwatta et al., GCN 14781). The object has
m(r) = 20.8, calibrated against the SDSS.

We suggest this object is the afterglow of GRB 130606A. It is probably
the same object reported by Jelinek et al. (GCN 14782).


GRB_name: GRB130606A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14784
SUBJECT: GRB 130606A: IRSF NIR Observation
DATE:    13/06/06 22:51:42 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

Takahiro Nagayama (Nagoya Univ) on behalf of OISTER collaboration.

We observed the field of GRB 130606A (Ukwatta et al, GCN Circular
14781) with the Infrared Survey Facility 1.4m telescope and
NIR camera SIRIUS at Sutherland Observatory in South Africa.

The observation was started with the JHKs bands simultaneously
from 2013-06-06 21:38 (UT).

We have detected a bright source not detected in 2MASS ALL SKY survey
at RA=16:37:35.14 DEC=+29:47:46.4 (J2000) from the first 300sec
exposure image.

Preliminary photometry results are as follows
J=13.1
H=13.9
Ks=14.7

These magnitudes are in the Vega system and not corrected for
Galactic extinction in the direction of the GRB.


GRB_name: GRB130606A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14785
SUBJECT: GRB 130606A - Liverpool Telescope Optical Afterglow Confirmation
DATE:    13/06/06 23:05:39 GMT
FROM:    Francisco Virgili at Liverpool John Moores U  <fjv@astro.livjm.ac.uk>

F.J. Virgili, C.G. Mundell (LJMU), A. Melandri (INAF-OAB), and A. Gomboc (U. Ljubljana)
report:

"The 2-m Liverpool Telescope robotically followed up GRB 130606A
(SWIFT trigger 557589; Ukwatta et al., GCN 14781) 38.52 min after the 
GRB trigger time.
We detect a fading source in i' and z' bands consistent with the 
position reported by Xu et al. (GCN 14783) with magnitudes

Filter        Magnitude                t since trigger (min)
i'            18.60 +/- 0.02            45.02
i'            18.67 +/- 0.02            55.48
i'            18.89 +/- 0.03             83.00

z'            16.65 +/- 0.02                47.74
z'            16.80 +/- 0.03                61.47

Magnitudes are calibrate against SDSS catalogued field stars.
Observations and analysis are ongoing.

[GCN OPS NOTE(10jun13): Per author's request, AG was added to the author list.]


GRB_name: GRB130605A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14787
SUBJECT: GRB 130605A: Swift-BAT refined analysis
DATE:    13/06/06 23:31:02 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), S. T. Holland (STScI), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-61 to T+242 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 130605A (trigger #557508)
(Holland, et al., GCN Circ. 14773).  The BAT ground-calculated position is
RA, Dec = 134.536, -33.477 deg, which is 
   RA(J2000)  =  08h 58m 08.7s 
   Dec(J2000) = -33d 28' 36.5" 
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 5%.
 
The mask-weighted light curve shows a single peak starting at ~T-5 sec,
peaking at ~T+2 sec, and ending at ~T+45 sec.  T90 (15-350 keV)
is 12.6 +- 3.1 sec (estimated error including systematics).
 
The time-averaged spectrum from T-6.48 to T+9.18 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.58 +- 0.17.  The fluence in the 15-150 keV band is 2.6 +- 0.3 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-0.14 sec in the 15-150 keV band
is 4.1 +- 0.9 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/557508/BA/


GRB_name: GRB130605A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14788
SUBJECT: GRB 130605A: Swift-XRT refined Analysis
DATE:    13/06/06 23:36:06 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

A. Melandri (INAF/OAB) and S. T. Holland (STScI) report on behalf of
the Swift-XRT team:

We have analysed 15 ks of XRT data for GRB 130605A (Holland  et al. GCN
Circ. 14773),  from 78 s to 58.5 ks after the  BAT trigger. The data
comprise 385 s in Windowed Timing (WT) mode (the first 8 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. Using 6133 s of PC mode data and 5 UVOT images, we find an
enhanced XRT position (using the XRT-UVOT alignment and matching UVOT
field sources to the USNO-B1 catalogue): RA, Dec = 134.53571, -33.46152
which is equivalent to:

RA (J2000): 08h 58m 08.57s
Dec(J2000): -33d 27' 41.5"

with an uncertainty of 1.8 arcsec (radius, 90% confidence).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.23 (+/-0.05).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.3 (+0.5, -0.3). The
best-fitting absorption column is  2.35 (+1.96, -0.16) x 10^21 cm^-2,
consistent with the Galactic value of 2.2 x 10^21 cm^-2 (Kalberla et
al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 2.7 x 10^-11 (5.0 x
10^-11) erg cm^-2 count^-1. 

A summary of the WT-mode spectrum is thus:
Total column:      2.35 (+1.96, -0.16) x 10^21 cm^-2
Galactic foreground: 2.2 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.3 (+0.5, -0.3)

If the light curve continues to decay with a power-law decay index of
1.23, the count rate at T+24 hours will be 9.4 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.6 x
10^-14 (4.7 x 10^-14) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00557508.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB130606A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14789
SUBJECT: Virtual Telescope  observations of GRB 130606A
DATE:    13/06/06 23:45:11 GMT
FROM:    Gianluca Masi at Bellatrix Astronomical Obs  <gianluca@bellatrixobservatory.org>

G. Masi (Ceccano, Italy) and F. Nocentini (Frosinone, Italy) report:

On June 6.96456 2013 UT, we imaged the field around GRB 130606A (Ukwatta et al. 
(GCN 14781) remotely using the the 0.43m-f/6.8 robotic unit part of the Virtual 
Telescope robotic facility in Italy, 124 minutes after the burst.

4, 300 seconds unfiltered CCD images were coadded and show an object at the 
following coordinates (J2000):

R.A. = 16 37 35.13
Decl. +29 47 46.7

We also performed photometry, assuming R-mags from UCAC-4 for the stars in the 
field, getting an estimate for the magnitude of 19.6 (CR).


GRB_name: GRB130606A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14790
SUBJECT: GRB 130606A: 10.4m GTC spectroscopy indicates z = 6.1
DATE:    13/06/07 00:06:12 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

A. J. Castro-Tirado, R. Snchez-Ramrez, M. Jelinek (IAA-CSIC), J.
Gorosabel (EHU-UPV), J. C. Tello, P. Ferrero, O. Lara-Gil, R. Cunniffe
(IAA-CSIC), D. Prez-Ramrez (U. Jan), P. Kubanek (FZU), J. M. Castro
Cern (ESAC), A. Fernndez-Soto (UV), S. Mottola (DLR), S. Hellmich (DLR),
R. Fernndez-Muoz (EELM-CSIC), V. F. Muoz-Martnez (UMA), J. Cepa (IAC)
and C. lvarez-Iglesias (GTC), on behalf of a larger collaboration,
report:

Following the detection of the optical afterglow (Jelinek et al. GCNC
14782, Xu et al. GCNC 14783) to GRB 130606A ((Ukwatta et al. GCNC
14781), we have obtained an optical spectrum with the 10.4 m GTC (+OSIRIS)
starting aprox. 1.5 hr postburst, covering the 4000-10000 wavelength
range. The continuum is detected only redwards of aprox. 6500 A, with
multiple absorption lines which are indicative of the Lyman forest.
Therefore we infer a (preliminary) redshift of z = 6.1 (to be refined).
This is consistent with the dropout in the optical band (Virgili et al.
GCNC 14785) and the bright nIR afterglow (Nagayama et al. GCNC 14784).
Observations at all wavelengths are encouraged.


GRB_name: GRB130606A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14791
SUBJECT: GRB130606A: Montarrenti Observatory afterglow detection
DATE:    13/06/07 00:14:01 GMT
FROM:    Simone Leonini at Monarrenti Obs  <s.leonini@iol.it>

Simone Leonini, G. Guerrini, P. Rosi and L.M. Tinjaca Ramirez (Montarrenti 
Observatory, Siena, Italy) report:

We observed the field of GRB 130606A (Swift trigger 557589, Ukwatta et al., 
GCN 14781) with the automatic 0.53m RC telescope + U47 detector 
at Montarrenti Observatory (Siena, Italy, IAU code C88).

The observations was started at 2013-06-06 22:57:50 UT (~117 minutes after the 
trigger) and we co-added 4 unfiltered CCD exposures of 60s each.

We detect a new source of mag. R=18.9 +/-0.16 (USNO-B1 catalogue, not 
corrected for galactic dust extinction) at the following position:

RA    (J2000)  16h 37m 35.13s +/-0.19
Decl. (J2000) +29Â° 47' 46.9"  +/-0.18

The message may be cited.


GRB_name: GRB130606A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14792
SUBJECT: GRB 130606A: Errata of J and Ks magnitudes in GCN 14784
DATE:    13/06/07 00:24:12 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

Takahiro Nagayama (Nagoya Univ) on behalf of OISTER collaboration.

In the circular 14784, submited by us, the J and Ks magnitudes
are swapped by mistake.

J=14.7
H=13.9
Ks=14.7
are correct.


GRB_name: GRB130606A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14793
SUBJECT: GRB 130606A: Errata of J and Ks magnitudes in GCN 14784
DATE:    13/06/07 00:25:50 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

Takahiro Nagayama (Nagoya Univ) on behalf of OISTER collaboration.

In the circular 14784, submited by us, the J and Ks magnitudes
are swapped by mistake.

J=14.7
H=13.9
Ks=13.1
are correct.


GRB_name: GRB130606A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14794
SUBJECT: GRB 130606A: Errata Ks magnutide in GCN 14792
DATE:    13/06/07 00:37:22 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

Takahiro Nagayama (Nagoya Univ) on behalf of OISTER collaboration.

In the circular 14792, submited by us, the Ks magnitude is correct.
The circular 14793 are correct.

We apologize for the possible inconvenience.


GRB_name: GRB130606B
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14795
SUBJECT: GRB 130606B: Fermi-LAT detection of a bright hard burst
DATE:    13/06/07 01:20:12 GMT
FROM:    Giacomo Vianello at SLAC  <giacomov@slac.stanford.edu>

G. Vianello (Stanford University), J. Racusin (NASA/GSFC), Nicola Omodei
(Stanford University) and M. Ohno (Hiroshima U.) report on behalf of the
Fermi-LAT team:

At 11:55:33 UT on 06 June 2013, Fermi LAT detected high energy emission
from GRB 130606B, which was also detected by Fermi-GBM (trigger 392212536 /
130606497). The brightness of the event in GBM triggered an autonomous
repoint of the spacecraft. Unfortunately, the GBM flight software
determined an unreliable position and the spacecraft slewed to that
position.

We were nevertheless able to detect a very clear excess at the position:

(RA, Dec) = 218.574, -22.131 (J2000) with an error radius of 0.1 deg (68%
containment radius, statistical errors only)

which was within the LAT field of view between T0 + 180 s and T0 + 1000 s.
Using SOURCE class we detected > 10 events, with 4 events above 1 GeV,
compatible with the position of the source during this time interval.

This source was about 91 deg from the LAT boresight at the time of the
trigger and during the whole prompt emission (~100 s long), well outside
the nominal field of view for the standard data analysis. However, we
detected a strong signal using the non-standard LLE selection, most
sensitive in the 10 MeV - 100 MeV energy range and featuring a broader
acceptance. We detected an excess of more than 17 sigma in a time interval
from 5 to 30 s after the trigger, composed of few hundreds events above the
background level. The effective area of the LLE class is small at such high
off-axis angle, therefore the strong excess indicates that this burst was
exceptionally bright and hard.

A Swift TOO request has been submitted.

A GBM circular is forthcoming.

The Fermi LAT point of contact for this burst is Giacomo Vianello (
giacomov@stanford.edu).

The Fermi LAT is a pair conversion telescope designed to cover the energy
band from 20 MeV to greater than 300 GeV. It is the product of an
international collaboration between NASA and DOE in the U.S. and many
scientific institutions across France, Italy, Japan and Sweden.

-- 
-----------------------------------------------------------
Giacomo Vianello

Stanford University,
Hansen Experimental Physics Lab,
452 Lomita Mall,
Stanford, CA 94305-4085

"A few observation and much reasoning lead
to error; many observations and a little
reasoning to truth." (A.Carrell)

ICQ: 566213964
-----------------------------------------------------------


GRB_name: GRB130606A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14796
SUBJECT: GRB 130606A: 10.4m GTC refined redshift z = 5.91
DATE:    13/06/07 01:59:16 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

A. J. Castro-Tirado, R. Snchez-Ramrez (IAA-CSIC), J. Gorosabel (EHU-UPV,
IAA-CSIC), M. Jelinek, J. C. Tello, P. Ferrero, O. Lara-Gil, R. Cunniffe
(IAA-CSIC), D. Prez-Ramrez (U. Jan), S. Guziy (Nikolaev Univ.), P. Kubanek (FZU),
J. M. Castro Cern (ESAC), A. Fernndez-Soto (UV), S. Mottola (DLR), S. Hellmich (DLR),
R. Fernndez-Muoz (EELM-CSIC), V. F. Muoz-Martnez (UMA), L.
Sabau-Graziati (INTA), A. Martn-Carrillo (UCD), J. Cepa (IAC), A. Tejero
and C. lvarez-Iglesias (GTC), on behalf of a larger collaboration,
report:

A detailed analysis of our 10.4m GTC spectrum reported on GCNC 14790
reveals several absorption metallic lines (N V, Si II and Si IV amongst
others) at a common redshift of z = 5.91 which we propose to be the
redshift of GRB 130606A.

[GCN OPS NOTE(10jun13): Per author's request, SG was added to the author list.]


GRB_name: GRB130606A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14797
SUBJECT: GRB 130606A:T100 observations
DATE:    13/06/07 05:13:14 GMT
FROM:    Eda Sonbas at NASA/GSFC  <edasonbas@gmail.com>

E. Sonbas (Adiyaman Univ.), H. Avdan (Cukurova Univ.), T. Guver (Sabanci
Univ.), M. Kaplan (Akdeniz Univ.), M. Kocak (TUG), E. Gogus (Sabanci
Univ.),
H. Kirbiyik (TUG) report on behalf of a larger collaboration

We observed the field of Swift  GRB 130606A (Ukwatta et al. GCN#14781)
with  the  1.0 meter  T100  telescope  (TUBITAK National  Observatory,
Antalya - Turkey),  starting June, 6,  22:43:53 UT (~ 1.6 hours after
the trigger). Observations were carried out in the R filter under moderate
weather conditions. We detected a new source in 300 s R band
image at a position that is consistent with Xu et al. GCN#14783
Using USNO-B1 star USNO-B1 1198-0251348  (RA=  16:37:32.14 , Dec=
+29:51:58.15 ) in the field, the magnitude of the OT were estimated as 20.6
+/-0.2.

Further observations using the same filter are ongoing.

We are grateful to the TUBITAK National Observatory staff for promptly
scheduling the observations and their technical support.


GRB_name: GRB130606A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14798
SUBJECT: GRB 130606A: MMT Spectroscopy
DATE:    13/06/07 05:16:26 GMT
FROM:    Ryan Chornock at Harvard  <rchornock@cfa.harvard.edu>

R. Lunnan, M. Drout, R. Chornock, and E. Berger (Harvard) report:

We observed the optical afterglow (Jelinek et al., GNC 14782; Xu et al., GCN 
14783; Nagayama et al., GCN 14784; Virgili et al., 14785; Masi et al., GCN 
14789; Leonini et al., GCN 14791; Sonbas et al., GCN 14797) of GRB 130606A 
(Ukwatta et al., GCN 14781) using the Blue Channel spectrograph on the 6.5-m MMT 
starting at 04:04 UT on 7 June (7.0 hours after the BAT trigger).  We obtained 
4x1200s of spectroscopy spanning the wavelength range 7450-9350 Angs with a 
resolution of 2.1 Angstroms.

We detect a sharp cutoff in flux blueward of ~8425 Angs, consistent with 
Lyman-alpha at a redshift of z=5.9, with very little transmission between 7850 
and 8400 Angs, although some flux is present blueward of that.  Several metal 
absorption lines are present to the red, including NV, Si II, C II, and O I at 
redshift z=5.913, confirming the GTC redshift of Castro-Tirado et al. (GCN 
14790, GCN 14796).


GRB_name: GRB130606A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14799
SUBJECT: GRB 130606A: RATIR r'-band Dropout
DATE:    13/06/07 05:46:43 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB)
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC),
Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC),
Jos A. de Diego (UNAM), Leonid Georgiev (UNAM), Jess Gonzlez (UNAM),
Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC), and Harvey Moseley (GSFC)
report:

We observed the field of GRB 130606A (Ukwatta, et al., GCN 14781) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional on
Sierra San Pedro Mrtir from 2013/06 7.19 to 2013/06 7.20 UTC (7.38 to 7.79
hours after the BAT trigger), obtaining a total of 0.36 hours exposure in
the r' and i' bands and 0.15 hours exposure in the Z, Y, J, and H bands.

The optical/NIR afterglow (Jelinek, et al., GCN 14782; Xu et al., GCN
14783) is quite red and clearly detected in all bands but r'.  In
comparison with SDSS DR9 and 2MASS, we obtain the following detections and
3-sigma upper limit:

r' > 23.02
i' 21.16 +/- 0.06
Z  18.79 +/- 0.03
Y  18.40 +/- 0.03
J  18.32 +/- 0.03
H  17.92 +/- 0.03

These magnitudes are in the AB system and not corrected for Galactic
extinction in the direction of the GRB.  The lack of detection in r' and
relatively faint flux level in i' are consistent with the high-redshift
determined from spectroscopy (Castro-Tirado, et al., GCN 14790, 14796;
Lunnan, et al., GCN 14798).

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.  Further observations are planned.


GRB_name: GRB130606A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14800
SUBJECT: GRB 130606A: LOAO IZY Observation
DATE:    13/06/07 08:34:27 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

M. Im (CEOU/SNU), H.-I. Sung(KASI), and Y. Urata (NCU) 
on behalf of EAFON

We observed the afterglow of GRB 130606A (Ukwatta et al. GCN 14781),
using a 1-m telescope at Mt. Lemmon Optical Observatory (LOAO) in
Arizona, US. The observation started at 2013-06-07 03:50:26 UT,
about 6.75 hrs after the burst alert, and a series of images were 
taken in I, Z, and Y-bands for about 1 hr.

We identify the afterglow, in all the three bands,
with approximate magnitudes of I = 20.8 +- 0.1, Z=18.70 +- 0.11,
and Y=18.49 +- 0.29, all in AB magnitude, calibrated against a star
in vicinity using SDSS and 2MASS photometry. This confirms 
earlier reports of the afterglow detection and its sharp drop in
SED between I-band and Z-band that is expected at z=5.91 
(Jelinek et al. GNC 14782; Xu et al.GCN 14783; Nagayama et al. GCN 14784; 
Virgili et al. 14785; Masi et al. GCN 14789; Leonini et al. GCN 14791; 
Sonbas et al., GCN 14797; Lunnan et al. GCN 14798; Castro-Tirado et al. 
GCN 14790; Butler et al. GCN 14799).

We thank the LOAO operator, Jae-Hyuk Yoon for performing 
the observation.


GRB_name: GRB130606B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14801
SUBJECT: GRB 130606B; Fermi GBM observation
DATE:    13/06/07 09:31:21 GMT
FROM:    Hoi-Fung Yu at MPE  <sptfung@mpe.mpg.de>

Subject: GRB 130606B: Fermi GBM observation

Hoi-Fung Yu (MPE)
reports on behalf of the Fermi GBM Team:

"At 11:55:33.63 UT on 6 June 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130606B (trigger 392212536 / 130606497).
The GBM on-ground location is consistent with the LAT position
(Vianello et al., GCN 14795). The angle from the Fermi LAT boresight
is 93 degrees.

The high peak flux from the GRB caused GBM to issue an autonomous
rapid repoint (ARR) maneuver but to an unreliable sky position 
according to the flight software calculation. 

This burst was also independently detected by INTEGRAL SPI-ACS.

The GBM light curve shows a multi-peaked feature with a duration (T90)
of about 52 s (50-300 keV). The time-averaged spectrum from T0+0.003 s
to T0+65.537 s is well fit by a Band function with
Epeak = 435 +/- 11 keV, alpha = -1.14 +/- 0.01, and
beta = -2.05 +/- 0.02.

The event fluence (10-1000 keV) in this time interval is
(2.034 +/- 0.007)E-04 erg/cm^2. The 1.024 s peak photon flux measured
starting from T0+9.15 s in the 10-1000 keV band
is 62.14 +/- 0.58 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB130606A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14802
SUBJECT: GRB 130606A: PAIRITEL NIR Afterglow Observations
DATE:    13/06/07 09:49:51 GMT
FROM:    Adam Morgan at U.C. Berkeley  <qmorgan@gmail.com>

A. N. Morgan (UC Berkeley) reports:

We observed the field of GRB 130606A (Ukwatta, et al., GCN 14781) with the
1.3m PAIRITEL located at Mt. Hopkins, Arizona. Observations began at
2013-Jun-07 06h01m22s UT, ~8.9 hours after the Swift Trigger.  In  mosaics
(effective exposure time of ~36.3 minutes) taken simultaneously in the J,
H, and Ks filters, we detect the optical afterglow (e.g. Jelinek, et al.,
GCN 14782; Xu et al., GCN 14783; Nagayama et al., GCN 14784).

The preliminary photometry yields:

post burst
t_mid (hr) exp.(m)  filt  mag   m_err
9.44       36.3     J     17.83  0.06
9.44       36.3     H     17.06  0.07
9.44       36.3     Ks    16.4   0.1

Observations are ongoing. All magnitudes are given in the Vega system,
calibrated to 2MASS. No correction for Galactic extinction has been made to
the above reported values.


GRB_name: GRB130606B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14803
SUBJECT: Konus-Wind observation of GRB 130606B
DATE:    13/06/07 11:35:33 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf
of the Konus-Wind team, report:

The long-duration intense hard-spectrum GRB 130606B
(Fermi-LAT detection: Vianello et al., GCN 14795;
Fermi-GBM detection: Yu, GCN 14801)
triggered Konus-Wind at T0=42940.544s UT (11:55:40.544).

The light curve shows a bright hard pulse complex from ~T0 to ~T0+70 s,
followed by a weak soft tail of emission out to ~T0+100s.
The emission at the main phase is seen up to ~17 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130606_T42940/
Periodic 'dips' visible in the 64-ms light curve are
due to the source occultation by the spacecraft.

As observed by Konus-Wind, the burst
had a fluence of (4.3  0.1)x10-4 erg/cm2,
and a 64-ms peak flux, measured from T0+8.064s,
of (5.7  0.3)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+67.328 s)
is best fit in the 100 keV - 18 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.25  0.15,
the high energy photon index beta = -1.92  0.02,
the peak energy Ep = 337  59 keV,
chi2 = 120/81 dof.

The spectrum at the maximum count rate
(measured from T0+7.680 to T0+8.704 s)
is best fit in the 50 keV - 18 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.92  0.18,
the high energy photon index beta = -1.87  0.10,
the peak energy Ep = 690  240 keV,
chi2 = 96/90 dof.

All the quoted results are preliminary.


GRB_name: GRB130606A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14804
SUBJECT: GRB 130606A: P60 Observations
DATE:    13/06/07 11:48:56 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) and S. B. Cenko (GSFC) report on behalf of a 
larger collaboration:

We imaged the field of GRB 130606A (Ukwatta et al., GCN 14781) with the 
robotic Palomar 60-inch telescope throughout the night of 2013-06-07 UT, 
beginning at 04:01 UT and continuing until morning twilight at 11:39 UT. 
  Initial observations consisted of a series of r, i, and z-band frames; 
later in the night we switched to exclusively z-band observations. 
Transparency and seeing conditions were good throughout.

The GRB afterglow (Jelinek et al., GCN 14782; Xu et al., GCN 14783; 
Nagayama et al., GCN 14784) is well-detected in the z-band exposures and 
marginally detected in the other filters.  Preliminary (not 
fringe-corrected) aperture photometry of a few select points yields:

t_start(d)  t_exp(s) filter  magnitude
  0.30679     180     z = 18.62 +/- 0.08
  0.42224     180     z = 19.22 +/- 0.09
  0.50888     180     z = 19.59 +/- 0.11
  0.58040     180     z = 19.73 +/- 0.22

The afterglow decays as a power-law with an index of approximately 
alpha=1.6-1.7 over the course of the observations.

Given the redshift (Castro-Tirado et al., GCN 14796; Lunnan et al., GCN 
14798) these relatively bright fluxes indicate an extremely luminous 
afterglow, especially at early times; similar to the luminous 
high-redshift GRB 050904 (e.g. Kann, Masetti, & Klose 2007; AJ 133:1187).


GRB_name: GRB130606A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14806
SUBJECT: GRB 130606A: AAO optical observations
DATE:    13/06/07 13:22:00 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), R.Inasaridze (AAO), O. Kvaratskhelia (AAO), V. 
Ayvazian(AAO), Yu. Krugly (IA KhNU),  I. Molotov (KIAM), A. Pozanenko 
(IKI)  report on behalf of  larger GRB follow-up collaboration:

We observed the field of the Swift Swift GRB 130606A (Ukwatta et al., 
GCN 14781)with AS-32 (0.7m) telescope of Abastumani Observatory, 
starting on Jun. 06 (UT) 21:47:43. We obtained several unfiltered images 
of 180 s exposure. The afterglow (Jelinek et al., GCN 14782; Xu et al., 
GCN 14783; Nagayama et al., GCN 14784) is well detected in  separate 
images. Preliminary photometry

T_start,   Exp,  T-t0, d    OT +/- err
  UT        s     mid, days
21:47:43   180   0.03095    18.84 +/- 0.05
21:51:24   180   0.03351    18.86 +/- 0.04
21:55:04   180   0.03605    18.95 +/- 0.05
21:58:45 2x180   0.03988    19.16 +/- 0.06

is based on SDSS stars R mag, where R mag obtained via transformations 
ugriz in BVRI (Lupton, 2005):

SDSS                 u     g       r     i      z       R
J163722.96+294541.6 16.747 15.352 14.827 14.598 14.568  14.625
J163734.99+294356.8 18.166 17.023 16.665 16.540 16.503  16.493


GRB_name: GRB130606A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14807
SUBJECT: GRB 130606A: GROND Detection of the Optical/NIR Afterglow
DATE:    13/06/07 13:29:05 GMT
FROM:    Jonny Elliott at MPE/GROND  <jonnyelliott@mpe.mpg.de>

P. Afonso (American River College), D. A. Kann, A. Nicuesa Guelbenzu (both
TLS Tautenburg), T. Kruehler (DARK), J. Elliott, and J. Greiner (both MPE
Garching) report on behalf of the GROND team:

We observed the field of GRB 130606A (Swift trigger 557589; Ukwatta et
al., GCN #14781) simultaneously in g'r'i'z'JHK with GROND (Greiner et al.
2008, PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La Silla
Observatory (Chile).

Observations started at 03:30 UT on 7th June 2013, 6.4 hours after the GRB
trigger. They were performed at an average seeing of 1.1" and at an
average airmass of 2.0.

We detect the afterglow (Jelinek et al.; GCN #14782) at the position of Xu
et al. (GCN #14783), and based on images taken at a mid-time of 05:00 UT,
with total exposures of 7.66 minutes in g'r'i'z' and 8 minutes in JHK, we
estimate preliminary magnitudes (all in AB) of

g' > 24.3 mag,
r' = 23.4 +/- 0.2 mag,
i' = 21.4 +/- 0.1 mag,
z' = 18.8 +/- 0.1 mag,
J = 18.4 +/- 0.1 mag,
H = 18.1 +/- 0.1 mag, and
K = 17.8 +/- 0.2 mag.

The spectral energy distribution is best fit with a small amount of
LMC-like dust and a spectral slope of beta ~ 0.7.

Given magnitudes are calibrated against GROND zeropoints as well as 2MASS
field stars and are not corrected for the expected Galactic foreground
extinction corresponding to a reddening of E_(B-V)=0.024 mag in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB130606A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14808
SUBJECT: Konus-Wind observation of GRB 130606A
DATE:    13/06/07 14:09:41 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P.
Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind
team report:

The long GRB 130606A (Swift-BAT trigger #557589: Ukwatta et al., GCN
14781) was detected by Konus-Wind in the waiting mode.

The burst light curve shows a weak initial pulse followed in ~150 s by a 
much brighter peak.

As observed by Konus-Wind, the burst had a fluence of (4.4 +/- 
0.8)x10^-6 erg/cm2 (in the 20 - 1300 keV energy range).

Modeling the K-W 3-channel time-integrated spectrum (from T0(BAT)+153 s 
to T0(BAT)+165 s) by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -1.14 +/- 0.15, and Ep = 294(-50,+90) keV.

Assuming z = 5.91 (Castro-Tirado et al., GCN 14796; Chornock et al. GCN 
14798) and a standard cosmology model with H_0 = 71 km/s/Mpc, Omega_M = 
0.27, Omega_Lambda = 0.73, the isotropic energy release is E_iso =
(2.83 +/- 0.52)x10^53 erg in 1 keV to 10 MeV at the GRB rest frame
extrapolating the best exponential cutoff function fit.

All the quoted errors are estimated at the 1 sigma confidence level.

The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB130606A/


GRB_name: GRB130605A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14809
SUBJECT: Konus-Wind observation of GRB 130605A
DATE:    13/06/07 14:16:21 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf
of the Konus-Wind team, report:

The long-duration GRB 130605A
(Swift-BAT trigger 557508: Holland, et al., GCN 14773;
Barthelmy, et al., GCN 14787)
triggered Konus-Wind at T0=85303.441s UT (23:41:43.441)

The burst light curve shows a single pulse from ~T0-1 s to ~T0+5 s.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130606_T85303/

As observed by Konus-Wind, the burst
had a fluence of (3.4  0.4)x10-6 erg/cm2,
and a 64-ms peak flux, measured from T0+0.320 s,
of (2.5  0.3)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The spectrum of the burst (measured from T0 to T0+0.128 s)
is best fit in the 20 keV - 5 MeV range by a simple power-law
model with the photon index 2.19  0.07, chi2 = 80/69 dof.

All the quoted results are preliminary.


GRB_name: GRB130605A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14810
SUBJECT: Konus-Wind observation of GRB 130605A: correction to GCN 14809 
DATE:    13/06/07 14:55:17 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

D. Frederiks, on behalf of the Konus-Wind team:

The correct URL for the Konus-Wind light curve of GRB 130605A is:
http://www.ioffe.ru/LEA/GRBs/GRB130605_T85303/

We are sorry for the inconvenience.


GRB_name: GRB130606A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14811
SUBJECT: GRB 130606A: Enhanced Swift-XRT position
DATE:    13/06/07 15:17:53 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 3364 s of XRT Photon Counting mode data and 8 UVOT
images for GRB 130606A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 249.39633, +29.79622 which is equivalent
to:

RA (J2000): 16h 37m 35.12s
Dec (J2000): +29d 47' 46.4"

with an uncertainty of 1.5 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB130606A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14812
SUBJECT: GRB 130606A: Swift-XRT refined Analysis
DATE:    13/06/07 16:26:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

D.N. Burrows (PSU), B.P. Gompertz (U. Leicester), J.P. Osborne (U.
Leicester), K.L. Page (U. Leicester), V. D'Elia (ASDC), A. Maselli 
(INAF-IASFPA), V. Mangano (INAF-IASFPA), J.A. Kennea (PSU), M.C. Stroh
(PSU) and T.N. Ukwatta report on behalf of the Swift-XRT team:

We have analysed 7.6 ks of XRT data for GRB 130606A (Ukwatta  et al.
GCN Circ. 14781),  from 62 s to 58.7 ks after the  BAT trigger. The
data comprise 499 s in Windowed Timing (WT) mode (the first 9 s were
taken while Swift was slewing) with the remainder in Photon Counting
(PC) mode. The enhanced XRT position for this burst was given by
Osborne et al. (GCN. Circ 14811).

The late-time light curve (from T0+5.3 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.13 (+0.10, -0.09).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.55 (+/-0.04). The
best-fitting absorption column is  8.4 (+/-1.0) x 10^20 cm^-2, in
excess of the Galactic value of 2.0 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.84 (+0.15, -0.14)
and a best-fitting absorption column of 4.5 (+3.1, -2.5) x 10^20 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.8 x 10^-11 (4.2 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.5 (+3.1, -2.5) x 10^20 cm^-2
Galactic foreground: 2.0 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.84 (+0.15, -0.14)

If the light curve continues to decay with a power-law decay index of
1.13, the count rate at T+24 hours will be 0.011 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.3 x
10^-13 (4.8 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00557589.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB130603A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14813
SUBJECT: GRB 130603A: AAO optical observations
DATE:    13/06/07 18:24:37 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), R.Inasaridze (AAO), O. Kvaratskhelia (AAO), V. 
Ayvazian(AAO), Yu. Krugly (IA KhNU),  I. Molotov (KIAM), A. Pozanenko 
(IKI)  report on behalf of  larger GRB follow-up collaboration:

We observed the field of the Swift Swift GRB 130603A (Melandri et al., 
GCN 14731)with AS-32 (0.7m) telescope of Abastumani Observatory  on Jun. 
03 and Jun. 04. We obtained several unfiltered images of 300 s and 180 s 
exposures. The afterglow (Melandri  et al., GCN 14732) is well detected 
in  combined images in both epochs. Preliminary photometry

Date        T_start    t-t0,      exp,    OT
             (UT)       mid, d     s
2013-06-03  22:19:06   0.69976    9x300   20.30 +/- 0.09
2013-06-04  20:28:49   1.62003   13x180   21.60 +/- 0.19

is based on SDSS stars R mag, where R mag obtained via transformations 
ugriz in BVRI (Lupton, 2005):

n SDSS                  R     errR
1 J054806.91+825053.0  17.648 0.015
2 J054805.54+825456.1  16.750 0.013
3 J054706.99+825234.5  15.573 0.012


GRB_name: GRB130606A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14814
SUBJECT: GRB 130606A: Swift/UVOT Upper Limits
DATE:    13/06/07 20:02:03 GMT
FROM:    Tyler Pritchard at PSU  <tapritchard@astro.psu.edu>

T. A. Pritchard (PSU) and T. N. Ukwatta (MSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130606A
84 s after the BAT trigger (Ukwatta et al., GCN Circ. 14781).
No optical afterglow consistent with the optical position
(Xu et al., GCN Circ 15783) is detected in the initial UVOT exposures.
Aspect correction was lost in a number of sub-exposures resulting in
image streaks, rough aspect corrections and larger apertures have been
used to calibrate the field, although with a lower sensitivity.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white_FC            84          231          144         >21.1
u_FC               293          543          246         >20.3
white               84         6539          361         >22.1
v                 5314        12245         1148         >20.6
b                  549         6334          236         >20.7
u                  293        18354          561         >20.4
w1                 672        18247         1102         >21.1
m2                5519        15930          625         >20.5
w2                1028         6744          216         >20.1

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.02 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB130606A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14815
SUBJECT: GRB 130606A: Skynet/PROMPT detection of the optical afterglow
DATE:    13/06/07 20:46:16 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, A. LaCluyze, D. Reichart, J. Haislip, T. Berger, M. Carroll,
H. T. Cromartie, R. Egger, A. Foster, C. Foster, N. Frank, K. Ivarsen,
D. James, M. Maples, J. Moore, M. Nysewander, E. Speckhard, P. Taylor
and J. A. Crain report:

Skynet observed field of GRB 130606A (Ukwatta et al., GCN 14781, Swift
trigger #557589), using the optical localization of Xu et al. (GCN
14783).  It took ~150 160-second exposures in each of the g', R and z'
bands with three 16" telescopes of the PROMPT array at CTIO, Chile,
starting at 2013-06-07, 00:47 UT (t=3.75h post-trigger), and continuing
until t=9.7h.

We detect a fading afterglow in the z' band in most individual
exposures, with z~18.5 at t~6.3h, and an approximate temporal index
alpha~-1.4.   We do not detect the afterglow in the R or g' bands in
individual exposures, consistent with the spectroscopic redshift z=5.91
reported by Castro-Tirado et al. (GCN 14796).  Stacks of ~70 160-second
exposures at a mean time t~5.7h yield a questionable R~21.9 detection
and a 3-sigma upper limit g'>23.7.  Similar stacks at t~8.5h yield
3-sigma upper limits R>22.7 and g'>23.6.  A preliminary light curve is at:

http://www.skynet.unc.edu/grb/grb130606a.png

Photometry is calibrated to 10 SDSS stars in the field; g' and z'  
magnitudes are in the AB system; R-band magnitudes are in the Vega
system, with the SDSS calibration stars transformed according to Jester
(2005).  No correction has been applied for the expected line-of-sight
Milky Way extinction of E(B-V)=0.02 (Schlegel et al. 1998).

Further Skynet observations are scheduled.


GRB_name: GRB130606A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14816
SUBJECT: GRB 130606A: VLT/X-shooter redshift confirmation
DATE:    13/06/07 21:11:06 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), D. Malesani (DARK/NBI), S. Schulze (PUC and MCSS),
J. P. U. Fynbo (DARK/NBI), Valerio D'Elia (ASI-SDC, INAF OAR), P.
Goldoni (APC/Univ. Paris 7 and SAp/CEA), O. Hartoog (Amsterdam), J.
Hjorth (DARK/NBI), L. Kaper (Amsterdam), T. Kruehler (DARK/NBI), A. J.
Levan (U. Warwick), B. Milvang-Jensen (DARK/NBI), N. R. Tanvir (U.
Leicester), K. Wiersema (U. Leicester) report on behalf of the
X-shooter GRB GTO collaboration:

We observed the optical afterglow of GRB 130606A (Ukwatta et al., GCN
14781; Jelinek et al., GCN 14782; Xu et al., GCN 14783) using the ESO
VLT equipped with the X-shooter spectrograph. The observations started
on 2013-06-07 at 04:09 UT (i.e., 7.08 hr after the burst). A total
exposure of 6x600 s was obtained, covering the spectral range from
~3000 to ~21000 A.

A continuum is detected redward of ~8410 A in the VIS/NIR arms of the
spectra, consistent with a Lyman alpha dropout at z~5.9, while
discrete transmission is present blueward down to ~6505 A. In the
spectra prominent absorption lines are detected, such as NV, C II, O
I, Si IV, C IV, and Si II, all at a common redshift of z=5.913, fully
consistent with the measurements in Castro-Tirado et al. (GCN 14796)
and Lunnan et al. (GCN 14798). We also identified at least two
intervening absorbers at z=3.451 and at z=2.310 through Mg II and Fe
II, respectively.

We thank the Paranal staff for enthusiastic support, in particular
Cedric Ledoux and Felipe Gaete.


GRB_name: GRB130606A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14817
SUBJECT: GRB 130606A: EVLA detection
DATE:    13/06/07 22:41:49 GMT
FROM:    Tanmoy Laskar at Harvard U  <tanmoylaskar@gmail.com>

T. Laskar, A. Zauderer, and E. Berger (Harvard) report:

"We observed the position of GRB 130606A (Ukwatta et al; GCN 14781) with
the EVLA beginning on 2013 June 07.30 UT (0.59 days after the burst). At a
mean frequency of 21.8 GHz, we detect a radio source with a preliminary
flux density of ~ 0.1 mJy at

RA = 16:37:35.134 +/- 0.004
Dec = 29:47:46.47 +/- 0.06,

consistent with the enhanced Swft/XRT position (Burrows et al.; GCN 14812),
the NIR position (Xu et al.; GCN 14783, Nagayama et al.; GCN 14784), and
the optical position (Masi and Nocentini; GCN 13891, Leonini et al.; GCN
14791). Follow-up observations are planned."


GRB_name: GRB130606A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14818
SUBJECT: GRB 130606A: TAROT Calern observatory early optical observations
DATE:    13/06/07 23:34:40 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (IRAP-CNRS-OMP),
Boer M., Siellez K., Dereli H., Bardho O. (UNS-CNRS-OCA),
Atteia J.L. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 130606A detected by SWIFT
(trigger 557589) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 7.1 min after the GRB trigger
The elevation of the field increased from
63 degrees above horizon and weather conditions
were good.

We detect the optical transient (OT) discovered by
Jelinek et al. (GCNC 14782). TAROT images are unfiltered.
The redshift 5.9 means the OT should emit mainly in the I band.
At the present level of analysis we can not give the
flux of the OT refered in the I band.

We choose the zero point of magnitudes using
the star NOMAD-1 1197-0254828 (R=16.43). We refer the TAROT
magnitudes to the R magnitude of the reference star
(we use CR as the symbol of the clear filtered image
calibrated with the R magnitude of the reference star).

At 7.85 minutes after the GRB, CR=17.1

The OT is measured continuously until 141 minutes
with a mean decay of 0.9.

This message may be cited.


GRB_name: GRB130606A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14819
SUBJECT: GRB 130606A, Swift-BAT refined analysis
DATE:    13/06/07 23:39:13 GMT
FROM:    Tilan Ukwatta at MSU  <tilan.ukwatta@gmail.com>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):

Using the data set from T-240 to T+962 sec from the recent telemetry
downlink,
we report further analysis of BAT GRB 130606A (trigger #557589)
(Ukwatta, et al., GCN Circ. 14781).  The BAT ground-calculated position is
RA, Dec = 249.390, 29.796 deg which is
   RA(J2000)  =  16h 37m 33.6s
   Dec(J2000) = +29d 47' 44.5"
with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 96%.

The mask-weighted light curve shows multiple peaks. The first peak starts
around T-5 secs and last for 15 seconds, a cluster of weak peaks can be seen
from T+80 sec to T+110 sec, bright two peak structure is seen from T+150 sec
to T+ 170 sec, finally very weak extended multi-peak structure is observed
beyond
T+200 sec up to T+500 sec. T90 (15-350 keV) is 276.58 +- 19.31 sec
(estimated error including systematics).

The time-averaged spectrum from T-1.34 to T+297 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.52 +- 0.12.  The fluence in the 15-150 keV band is 2.9 +- 0.2 x 10^-6
erg/cm2.
The 1-sec peak photon flux measured from T+160.36 sec in the 15-150 keV band
is 2.6 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/557589/BA/


GRB_name: GRB130606B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14820
SUBJECT: GRB 130606B: Swift-XRT observations
DATE:    13/06/08 00:26:50 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@swift.psu.edu>

J. A. Kennea (PSU)  reports on behalf of the Swift-XRT team:

We have analysed 3.1 ks of XRT data for the Fermi/LAT-detected burst:
GRB 130606B,  from 106.6 ks to 114.1 ks after the  Fermi/LAT trigger.
The data are entirely in Photon Counting (PC) mode.  An X-ray source is
detected within the Fermi/LAT error circle. Using 2899 s of PC mode
data and 4 UVOT images, we find an enhanced XRT position (using the
XRT-UVOT alignment and matching UVOT field sources to the USNO-B1
catalogue): RA, Dec = 218.52931, -22.10229 which is equivalent to:

RA (J2000): 14h 34m 07.04s
Dec(J2000): -22d 06' 08.2"

with an uncertainty of 1.8 arcsec (radius, 90% confidence). This
position is 181 arcsec from the Fermi/LAT position.  the light curve is
consistent with a constant source of mean count rate 8.0e-02 ct/sec. 

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.3 (+/-0.4). The
best-fitting absorption column is  2.0 (+1.0, -0.9) x 10^21 cm^-2, in
excess of the Galactic value of 6.7 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.3 x 10^-11 (5.6 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.0 (+1.0, -0.9) x 10^21 cm^-2
Galactic foreground: 6.7 x 10^20 cm^-2
Excess significance: 2.5 sigma
Photon index:      2.3 (+/-0.4)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020283.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB130606B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14822
SUBJECT: GRB 130606B: RATIR Optical and NIR Observations 
DATE:    13/06/08 02:46:15 GMT
FROM:    Alan M. Watson at Instituto de Astronomia UNAM  <alan@astro.unam.mx>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC),
William H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB),
Ori Fox (UCB) J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino
Cucchiara (UCSC), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), Jos A. de Diego (UNAM), Leonid Georgiev (UNAM),
Jess Gonzlez (UNAM), Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC),
and Harvey Moseley (GSFC) report:

We observed the field of GRB 130606B (Vianello et al., GCN Circular
14795) with the Reionization and Transients Infrared Camera (RATIR;
www.ratir.org) on the 1.5m Harold Johnson Telescope at the Observatorio
Astronmico Nacional on Sierra San Pedro Mrtir from 2013/06 7.16 to
2013/06 7.25 UTC (15.97 to 18.08 hours after the BAT trigger), obtaining
a total of 0.36 hours exposure in the r' and i' bands and 0.30 hours
exposure in the Y and H bands.

For a source within the XRT error circle (Kennea et al., GCN Circular
14820), in comparison with USNO-B1 and 2MASS, we obtain the following
3-sigma upper limits:

r'    > 23.59
i'    > 23.61
Y     > 21.52
H     > 20.73

These magnitudes are in the AB system and not corrected for Galactic
extinction in the direction of the GRB.

No further observations are planned.

We thank the staff of the Observatorio Astronmico Nacional in San Pedro 
Mrtir.


GRB_name: GRB130606B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14823
SUBJECT: GRB 130606B: AGILE-MCAL observation
DATE:    13/06/08 07:52:59 GMT
FROM:    Martino Marisaldi at INAF-IASF  <marisaldi@iasfbo.inaf.it>

M. Marisaldi, F. Fuschino (INAF/IASF-Bo), F. Verrecchia, C. Pittori (ASDC and INAF/OAR), A. Giuliani (INAF/IASF-Mi), F. Longo (University of Trieste and INFN Trieste), F. Lucarelli (ASDC and INAF/OAR), E. Del Monte, F. Lazzarotto, I. Donnarumma, Y. Evangelista, M. Feroci, L. Pacciani, P. Soffitta, E. Costa, I. Lapshov, M. Rapisarda (INAF/IAPS Rome), G. Barbiellini, (INFN Trieste), A. Bulgarelli, F. Gianotti, M. Trifoglio, G. Di Cocco, C. Labanti, V. Fioretti, M. Galli (INAF/IASF-Bo), A. Chen, S. Mereghetti, F. Perotti, P. Caraveo (INAF/IASF-Mi), M. Cardillo, E. Striani, M. Tavani (INAF/IAPS Rome, and Univ. Roma Tor Vergata), A. Argan, G. Piano, S.
Sabatini, V. Vittorini (INAF/IAPS Rome), G. Pucella (ENEA Frascati), A. Pellizzoni, A. Trois (INAF/OA Cagliari), M. Pilia (ASTRON), S. Vercellone (INAF/IASF-Pa), P. W. Cattaneo, A. Rappoldi (INFN Pavia), A. Morselli, P. Picozza (INFN Roma-2), M. Prest, E. Vallazza (Universita' 
dell'Insubria), S. Colafrancesco (INAF/OAR and WITS), P. Lipari, D. Zanello (INFN Roma-1), P. Giommi (ASI), and G. Valentini (ASI),
on behalf of the AGILE Team, report:

"The long hard bright GRB 130606B, observed in gamma-rays by Fermi-LAT (Vianello et al., GCN 14795), Fermi-GBM (Yu et al., GCN 14801) and Konus-Wind (Golenetskii et al., GCN 14803), triggered AGILE-MCAL, sensitive in the range 0.4 - 100 MeV, at 11:55:33 UT (T0).

The light curve above 400 keV shows three main peaks between T0 and T0 + 20 s, followed by two less bright peaks at T0 + 40 s and T0 + 50 s.
The time-integrated spectrum measured between T0 and T0 + 20 s can be fit in the energy range 0.5 - 20 MeV with a simple power law with photon index -2.15 +/- 0.03 and reduced chi-squared 1.67 (46 d.o.f). As observed by MCAL the burst fluence in the same energy range and time interval is (1.62 +/- 0.05)E-04 erg/cm^2. All quoted errors are at 90% confidence levels.

The burst was 118 degrees off-axis with respect to the AGILE GRID pointing direction at T0, from a sky region not accessible to the GRID.
This measurement was obtained with AGILE observing a large portion of the sky in spinning mode."


GRB_name: GRB130606A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14824
SUBJECT: GRB 130606A: Continued RATIR Optical and NIR Monitoring
DATE:    13/06/08 13:54:51 GMT
FROM:    Nat Butler at UC berkeley  <natxbutler@gmail.com>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB)
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC),
Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC),
Jos A. de Diego (UNAM), Leonid Georgiev (UNAM), Jess Gonzlez (UNAM),
Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC), and Harvey Moseley (GSFC)
report:

We observed the field of GRB 130606A (Ukwatta, et al., GCN 14781) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional on
Sierra San Pedro Mrtir from 2013/06 8.18 to 2013/06 8.46 UTC (31.14 to
37.86 hours after the BAT trigger), obtaining a total of 4.96 hours
exposure in the r' and i' bands and 2.07 hours exposure in the Z, Y, J, and
H bands.

The optical/NIR afterglow (Jelinek, et al., GCN 14782; Xu et al., GCN
14783) is well detected.   In comparison with SDSS DR9 and 2MASS, we obtain
the following detections and 3-sigma upper limit:

 r'  >24.06
 i'  24.06 +/- 0.27
 Z   21.50 +/- 0.09
 Y   21.41 +/- 0.12
 J   21.16 +/- 0.12
 H   20.78 +/- 0.12

These magnitudes are in the AB system and not corrected for Galactic
extinction in the direction of the GRB.  In comparison to our observations
on the previous night (2013/06/07; Butler, et al., GCN 14799), the
afterglow has faded by about 3 magnitudes in all bands.

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB130606A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14826
SUBJECT: GRB 130606A: Continued Skynet/PROMPT observations
DATE:    13/06/08 18:21:21 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, A. LaCluyze, D. Reichart, J. Haislip, T. Berger, M. Carroll, 
H. T. Cromartie, R. Egger, A. Foster, C. Foster, N. Frank, K. Ivarsen, 
D. James, M. Maples, J. Moore, M. Nysewander, E. Speckhard, P. Taylor 
and J. A. Crain report:

Skynet continued observing the field of GRB 130606A (Ukwatta et al., GCN 
14781, Swift trigger #557589), using the optical localization of Xu et 
al. (GCN 14783).  It took 109 160-second exposures in the z' band with 
one of the 16" telescopes of the PROMPT array at CTIO, Chile, with a 
mean time t=1.3d post-trigger.

In a stack of all 109 exposures, we detect the afterglow at the 5-sigma 
level, with z'~20.5 at t=1.3d.  Together with the z' detections we 
reported in Trotter et al. (GCN 14815), this implies an approximate 
temporal index alpha~-1.2.   A preliminary light curve of both nights' 
data is at:
http://www.skynet.unc.edu/grb/grb130606a_2.png

Photometry is calibrated to 10 SDSS stars in the field; g' and z' 
magnitudes are in the AB system; R-band magnitudes are in the Vega 
system, with the SDSS calibration stars transformed according to Jester 
(2005).  No correction has been applied for the expected line-of-sight 
Milky Way extinction of E(B-V)=0.02 (Schlegel et al. 1998).

No further Skynet observations are scheduled.


GRB_name: GRB130608A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14827
SUBJECT: GRB 130608A: Swift detection of a burst
DATE:    13/06/08 23:27:48 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

H. A. Krimm (CRESST/GSFC/USRA), D. N. Burrows (PSU),
J. R. Cummings (NASA/UMBC), N. Gehrels (NASA/GSFC),
D. Malesani (DARK/NBI), F. E. Marshall (NASA/GSFC),
A. Maselli (INAF-IASFPA), A. Melandri (INAF-OAB), D. M. Palmer (LANL)
and T. N. Ukwatta (MSU) report on behalf of the Swift Team:

At 23:14:21 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130608A (trigger=557771).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 24.580, +41.494 which is 
   RA(J2000) = 01h 38m 19s
   Dec(J2000) = +41d 29' 38"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve suggests a broad weak peak
from T-20 to T+40 s.  The maximum count rate was ~500 counts/sec 
(15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 23:17:02.9 UT, 161.6 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source with an enhanced position: RA, Dec 24.6087,
41.5027 which is equivalent to:
   RA(J2000)  = 01h 38m 26.08s
   Dec(J2000) = +41d 30' 09.7"
with an uncertainty of 2.7 arcseconds (radius, 90% containment). This
location is 83 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (6.62 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 6.2
(+5.87/-4.48) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 4.77e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 168 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.06. 

Burst Advocate for this burst is H. A. Krimm (krimm AT milkyway.gsfc.nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB130609A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14828
SUBJECT: GRB 130609A: Swift detection of a burst
DATE:    13/06/09 03:14:55 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

J. R. Cummings (NASA/UMBC), W. H. Baumgartner (GSFC/UMBC),
N. Gehrels (NASA/GSFC), H. A. Krimm (CRESST/GSFC/USRA),
D. Malesani (DARK/NBI), F. E. Marshall (NASA/GSFC),
A. Maselli (INAF-IASFPA), D. M. Palmer (LANL), M. H. Siegel (PSU) and
C. A. Swenson (PSU) report on behalf of the Swift Team:

At 03:05:08 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130609A (trigger=557782).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 152.676, +24.101 which is 
   RA(J2000) = 10h 10m 42s
   Dec(J2000) = +24d 06' 05"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 10 sec.  The peak count rate
was ~2500 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 03:06:15.4 UT, 66.8 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 152.67159, 24.13359 which is equivalent
to:
   RA(J2000)  = 10h 10m 41.18s
   Dec(J2000) = +24d 08' 00.9"
with an uncertainty of 3.9 arcseconds (radius, 90% containment). This
location is 118 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper.  We cannot determine whether the source is
fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (2.67 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 2.4
(+2.79/-2.37) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 70 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers none of
the XRT error circle. The 8'x8' region for the list of sources generated
on-board covers 100% of the XRT error circle. The list of sources is typically
complete to about 18 mag. No correction has been made for the expected
extinction corresponding to E(B-V) of 0.03. 

Burst Advocate for this burst is J. R. Cummings (jayc AT milkyway.gsfc.nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB130608A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14829
SUBJECT: GRB130608A: BOOTES-2/TELMA upper limits
DATE:    13/06/09 04:16:18 GMT
FROM:    Juan Carlos Tello at IAA-CSIC  <jtello@iaa.es>

J.C.Tello, M.Jelinek, (IAA-CSIC) J.Gorosabel (UPV-EY, IAA-CSIC),
A.J.Castro-Tirado, R. Sanchez-Ramirez (IAA-CSIC), on behalf of a larger
collaboration report:

We observed the field of GRB130608A (Krimm et al. GCNC 14827) with the
BOOTES-2/TELMA telescope located in Malaga, Spain, starting at 02h31m UT
(136 minutes after the burst, when the source rose above the local
horizon). No new source is visible within the XRT error circle.

During a first epoch we combined 11 images with an unfiltered exposure of
60 seconds each that begun at 02h31m45s (136 minutes after the burst) and
ended at 02h44m21s (mean time 142 minutes after the burst), and a limiting
magnitude of 18.8 was obtained when compared to the values of R2Mag of the
field stars as stated in the USNO-B1 catalog.

During a 2nd epoch we combined 22 images with an unfiltered exposure of 60
seconds each that begun at 3h00m11s (165 minutes after the burst) and ended
at 3h22m08s (mean time 176 minutes after the burst), and we obtained a
limiting magnitude of 19.5 when compared to the values of R2Mag of the
field stars as stated in the USNO-B1 catalog.


GRB_name: GRB130609A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14830
SUBJECT: GRB 130609A: P60 nondetection
DATE:    13/06/09 05:28:54 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) and S. B. Cenko (GSFC) report:

The Palomar 60-inch telescope automatically responded to GRB 130609A 
(Cummings et al., GCN 14828) and began taking observations at 04:03:23 
UT (58.25 minutes after the BAT trigger) as soon as the sky became dark. 
  A sequence of cycled 60-second r, i, and z images was acquired.  We 
detect no source consistent with the XRT localization in either 
individual images or in combined stacks of the first 6 images in each 
filter.  Approximate 5-sigma limiting magnitudes from the combined 
images at an approximate mean time of 4:20 UT (75 minutes after the GRB 
trigger) are:

r > 22.5
i > 21.5
z > 20.9

These limits are suggestive of a dark GRB.  Cummings et al. report a 
detection of significant excess absorption in the XRT spectrum, which 
may indicate a dust-extinguished (as opposed to high-redshift) event, 
although given the quoted errors there the excess may be only marginal.

NIR follow-up is highly encouraged.


GRB_name: GRB130609A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14831
SUBJECT: GRB 130609A: RATIR Optical and NIR Observations
DATE:    13/06/09 06:33:31 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB)
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC),
Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC),
Jos A. de Diego (UNAM), Leonid Georgiev (UNAM), Jess Gonzlez (UNAM),
Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC), and Harvey Moseley (GSFC)
report:

We observed the field of GRB 130609A (Cummings, et al., GCN 14828) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional on
Sierra San Pedro Mrtir from 2013/06 9.15 to 2013/06 9.23 UTC (0.56 to 2.52
hours after the BAT trigger), obtaining a total of 1.24 hours exposure in
the r' and i' bands and 0.60 hours exposure in the Z, Y, J, and H bands.

For a source within the Swift-XRT error circle, in comparison with SDSS DR9
and 2MASS, we obtain the following upper limits (3-sigma):

  r'    > 23.34
  i'    > 23.27
  Z     > 22.39
  Y     > 21.91
  J     > 21.72
  H     > 21.06

These magnitudes are in the AB system and not corrected for Galactic
extinction in the direction of the GRB.

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB130608A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14832
SUBJECT: GRB 130608A: Enhanced Swift-XRT position
DATE:    13/06/09 11:20:08 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 952 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 130608A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 24.61111, +41.50289 which is equivalent
to:

RA (J2000): 01h 38m 26.67s
Dec (J2000): +41d 30' 10.4"

with an uncertainty of 1.7 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB130608A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14833
SUBJECT: GRB 130608A: Swift-BAT refined analysis
DATE:    13/06/09 12:34:01 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), A. Y. Lien (NASA/GSFC/ORAU),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 130608A (trigger #557771)
(Krimm, et al., GCN Circ. 14827).  The BAT ground-calculated position is
RA, Dec = 24.594, 41.485 deg, which is 
   RA(J2000)  =  01h 38m 22.5s 
   Dec(J2000) = +41d 29' 05.0" 
with an uncertainty of 2.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 45%.
 
The mask-weighted light curve shows a broad peak starting at ~T-25 sec,
peaking at ~T+5 sec, and ending at ~T+50 sec.  T90 (15-350 keV) is
44.4 +- 8.0 sec (estimated error including systematics).
 
The time-averaged spectrum from T-25.56 to T+24.18 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
3.21 +- 0.34.  The fluence in the 15-150 keV band is 6.4 +- 1.0 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+19.06 sec in the 15-150 keV band
is 0.6 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/557771/BA/


GRB_name: GRB130609A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14834
SUBJECT: GRB 130609A, Swift-BAT refined analysis
DATE:    13/06/09 13:43:19 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC),
T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
  
Using the data set from T-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 130609A (trigger #557782)
(Cummings, et al., GCN Circ. 14828).  The BAT ground-calculated position is
RA, Dec = 152.680, 24.124 deg which is
    RA(J2000)  =  10h 10m 43.2s
    Dec(J2000) = +24d 07' 27.1"
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 87%.
  
The mask-weighted light curve shows a single FRED peak.  T90 (15-350 keV) is
7.0 +- 0.8 sec (estimated error including systematics).
  
The time-averaged spectrum from T-1.19 to T+7.28 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.88 +- 0.11.  The fluence in the 15-150 keV band is 5.7 +- 0.4 x 10^-07 erg/cm2.
The 1-sec peak photon flux measured from T+0.52 sec in the 15-150 keV band
is 1.8 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.
  
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/557782/BA/


GRB_name: GRB130609A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14835
SUBJECT: GRB 130609A: Enhanced Swift-XRT position
DATE:    13/06/09 15:17:08 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 3372 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 130609A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 152.66941, +24.13195 which is equivalent
to:

RA (J2000): 10h 10m 40.66s
Dec (J2000): +24d 07' 55.0"

with an uncertainty of 2.3 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB130608A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14836
SUBJECT: GRB 130608A: RATIR Optical and NIR Observations
DATE:    13/06/09 16:26:17 GMT
FROM:    Alan M. Watson at Instituto de Astronomia UNAM  <alan@astro.unam.mx>

Alan M. Watson (UNAM), Nat Butler (ASU), Alexander Kutyrev (GSFC),
William H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori
Fox (UCB) J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino
Cucchiara (UCSC), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), Jos A. de Diego (UNAM), Leonid Georgiev (UNAM),
Jess Gonzlez (UNAM), Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC),
and Harvey Moseley (GSFC) report:

We observed the field of GRB 130608A (Krimm, et al., GCN 14827) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on
the 1.5m Harold Johnson Telescope at the Observatorio Astronmico
Nacional on Sierra San Pedro Mrtir in morning twilight from 2013/06
9.46 to 2013/06 9.47 UTC (11.70 to 12.00 hours after the BAT trigger),
obtaining a total of 0.20 hours exposure in the r' and i' bands and 0.08
hours exposure in the Z, Y, J, and H bands.

For a source within the Swift-XRT error circle (Beardmore, et al., GCN
14832), in comparison with the RATIR zero points and 2MASS, we obtain
the following upper limits (3-sigma):

 r'    > 21.90
 i'    > 22.27
 Z     > 21.21
 Y     > 20.64
 J     > 20.12
 H     > 19.80

These magnitudes are in the AB system and not corrected for Galactic
extinction in the direction of the GRB.

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB130609A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14837
SUBJECT: GRB 130609A: Swift-XRT refined Analysis
DATE:    13/06/09 17:15:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), C. Pagani (U.
Leicester), A. Maselli (INAF-IASFPA), V. Mangano (INAF-IASFPA), A.
Melandri (INAF-OAB), J.A. Kennea (PSU), M.C. Stroh (PSU), D.N. Burrows
(PSU) and J.R. Cummings report on behalf of the Swift-XRT team:

We have analysed 10 ks of XRT data for GRB 130609A (Cummings  et al.
GCN Circ. 14828),  from 52 s to 23.5 ks after the  BAT trigger. The
data comprise 8 s in Windowed Timing (WT) mode (taken while Swift was
slewing), with the remainder in Photon Counting (PC) mode. The enhanced
XRT position for this burst was given by Evans et al. (GCN. Circ
14835).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.79 (+/-0.06).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.6 (+0.4, -0.3). The
best-fitting absorption column is  3.3 (+1.0, -0.9) x 10^21 cm^-2, in
excess of the Galactic value of 2.7 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.2 x 10^-11 (7.9 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.3 (+1.0, -0.9) x 10^21 cm^-2
Galactic foreground: 2.7 x 10^20 cm^-2
Excess significance: 5.4 sigma
Photon index:      2.6 (+0.4, -0.3)

If the light curve continues to decay with a power-law decay index of
0.79, the count rate at T+24 hours will be 3.5 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x
10^-13 (2.8 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00557782.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB130608A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14838
SUBJECT: GRB 130608A: Swift-XRT refined Analysis
DATE:    13/06/09 17:28:07 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

K.L. Page (U. Leicester), C. Pagani (U. Leicester), V. Mangano
(INAF-IASFPA), A. Melandri (INAF-OAB), B. Sbarufatti (INAF-OAB/PSU),
M.C. Stroh (PSU), D.N. Burrows (PSU), J.A. Kennea (PSU), A.P. Beardmore
(U. Leicester) and H.A. Krimm report on behalf of the Swift-XRT team:

We have analysed 9.4 ks of XRT data for GRB 130608A (Krimm  et al. GCN
Circ. 14827),  from 147 s to 47.3 ks after the BAT trigger. The data
comprise 98 s in Windowed Timing (WT) mode (the first 10 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Beardmore
et al. (GCN. Circ 14832).

The light curve can be modelled with an initial power-law decay with an
index of alpha=4.33 (+0.26, -0.23), followed by a break at T+653 s to
an alpha of 0.40 (+0.11, -0.12).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 3.23 (+0.27, -0.25). The
best-fitting absorption column is  1.0 (+0.4, -0.3) x 10^21 cm^-2, in
excess of the Galactic value of 6.6 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.40 (+0.36, -0.11)
and a best-fitting absorption column consistent with the Galactic
value. The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.0 x 10^-11 (4.0 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      0 (+4.9, -0) x 10^20 cm^-2
Galactic foreground: 6.6 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.40 (+0.36, -0.11)

If the light curve continues to decay with a power-law decay index of
0.40, the count rate at T+24 hours will be 7.3 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.2 x
10^-13 (3.0 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00557771.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB130609A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14839
SUBJECT: GRB 130609A: Fermi GBM observation
DATE:    13/06/09 20:20:46 GMT
FROM:    Gerard Fitzpatrick at UCD  <gerard.fitzpatrick@ucdconnect.ie>

G. Fitzpatrick (UCD) and J. Michael Burgess (UAH) report
on behalf of the Fermi GBM Team:

At 03:05:10.69 UT on 09 June 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130609A (trigger 392439913 /130609129),
which was also detected by the Swift/BAT (Cummings et al., GCN Circ. 14828).
The GBM on-ground location is consistent with the Swift position.

The GBM light curve consists of a single peak
with a duration (T90) of about 5 s (50-300 keV).
The time-averaged spectrum from T0-2.6 s to T0+2.8 s is
adequately fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.2 +/- 0.2 and
the cutoff energy, parameterized as Epeak, is 59.5 +/- 7.3 keV.

The event fluence (10-1000 keV) in this time interval is
(7.7 +/- 0.6)E-07 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-1.6 s in the 8-1000 keV band is 3.2 +/- 0.3 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog.


GRB_name: GRB130606A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14840
SUBJECT: GRB 130606A - Liverpool Telescope and Faulkes Telescope North optical observations
DATE:    13/06/09 21:43:42 GMT
FROM:    Francisco Virgili at Liverpool John Moores U  <fjv@astro.livjm.ac.uk>

F.J. Virgili, C.G. Mundell (LJMU), A. Melandri (INAF-OAB), and A. Gomboc 
(U. Ljubljana) report:

Observations of GRB 130606A (Ukwatta et al., GCN 14781) with the 2-m 
robotic Liverpool Telescope automatically performed between 48 and 80 
minutes after the GRB trigger confirms a detection of the afterglow in 
the r'-band with magnitude

r' = 21.9  0.29 at 49.95 minutes

consistent with reported values at similar epochs (Xu et al. 14783) and 
dimmer than times around 100 minutes post trigger (Leonini et al., GCN 
14791; Masi et al., GCN 14789; Sonbas et al., GCN 14797), possibly 
indicating mild re-brightening.  This detection clarifies that the 
afterglow has not yet dropped out of the r'-band at the times coincident 
with our i' and z' band detections (Virgili et al., GCN 14785) and 
continues to be detected until at least 6.4 hrs after the initial 
trigger (Afonso et al., GCN 14807).

In addition, the 2-m Faulkes Telescope North and Liverpool Telescope 
performed late-time follow up observations, resulting in a 3-sigma 
upper-limit of

r' > 23.4 at 849.73 min (14.16 hr post-trigger; FTN)
r' > 24 at 1683.67 minutes (= 28.06 hr; LT)

and an additional i'-band detection of

i' = 23.76  0.22 @ 28.60 hr (= 1716.51 minutes; LT),

in a co-added series of 6x300s exposures, which are consistent with 
values reported by Trotter et al. (GCN 14815) and Butler et al. (GCN 
14824).  FTN images have been acquired with the R-Bessell filter and 
calibrated against nearby SDSS catalogue stars.


GRB_name: GRB130609B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14841
SUBJECT: GRB 130609B: Swift detection of a burst with an optical counterpart
DATE:    13/06/09 21:46:41 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

H. A. Krimm (CRESST/GSFC/USRA), S. D. Barthelmy (GSFC),
D. N. Burrows (PSU), J. A. Kennea (PSU), D. Malesani (DARK/NBI),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC) and
A. Maselli (INAF-IASFPA) report on behalf of the Swift Team:

At 21:38:40 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130609B (trigger=557828).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 53.754, -40.153 which is 
   RA(J2000) = 03h 35m 01s
   Dec(J2000) = -40d 09' 11"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows multiple peaks
with a total duration of at least 200 sec.  The peak count rate
was ~8500 counts/sec (15-350 keV), at ~2 sec after the trigger. 

The XRT began observing the field at 21:39:56.4 UT, 76.0 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 53.7695, -40.1747 which is equivalent to:
   RA(J2000)  = +03h 35m 4.68s
   Dec(J2000) = -40d 10' 28.9"
with an uncertainty of 4.9 arcseconds (radius, 90% containment). This
location is 89 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

UVOT took a finding chart exposure of nominal 150.000 seconds with the White
filter starting 84 seconds after the BAT trigger. There is a candidate
afterglow in the list of sources generated on-board at
  RA(J2000)  = 03:35:05.11 =  53.77128
  DEC(J2000) = -40:10:26.6  = -40.17406
with a 90%-confidence error radius of about 1.10 arc sec. This position is 5.4
arc sec. from the center of the XRT error circle. The estimated magnitude is
15.71. No correction has been made for the expected extinction corresponding to
E(B-V) of 0.01. 

Burst Advocate for this burst is H. A. Krimm (krimm AT milkyway.gsfc.nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB130610A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14842
SUBJECT: GRB 130610A: Swift detection of a burst with an optical counterpart
DATE:    13/06/10 03:21:59 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

J. R. Cummings (NASA/UMBC), D. N. Burrows (PSU),
N. Gehrels (NASA/GSFC), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), D. Malesani (DARK/NBI),
C. B. Markwardt (NASA/GSFC), A. Maselli (INAF-IASFPA),
A. Melandri (INAF-OAB), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. H. Siegel (PSU) and T. N. Ukwatta (MSU) report on behalf of the
Swift Team:

At 03:12:13 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130610A (trigger=557845).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 224.416, +28.191 which is 
   RA(J2000) = 14h 57m 40s
   Dec(J2000) = +28d 11' 28"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure with a total duration of about 30 sec.  The peak count rate
was ~2700 counts/sec (15-350 keV), at ~5 sec after the trigger. 

The XRT began observing the field at 03:14:26.3 UT, 133.0 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 224.4218, 28.2048 which is equivalent to:
   RA(J2000)  = +14h 57m 41.23s
   Dec(J2000) = +28d 12' 17.3"
with an uncertainty of 6.6 arcseconds (radius, 90% containment). This
location is 52 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 140 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 14:57:40.89 = 224.42037
  DEC(J2000) = +28:12:25.7  =  28.20715
with a 90%-confidence error radius of about 0.62 arc sec. This position is 9.6
arc sec. from the center of the XRT error circle. The estimated magnitude is
17.91 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.02. 

Burst Advocate for this burst is J. R. Cummings (jayc AT milkyway.gsfc.nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB130610A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14843
SUBJECT: GRB 130610A - Liverpool Telescope Optical Afterglow Confirmation
DATE:    13/06/10 03:52:01 GMT
FROM:    Francisco Virgili at Liverpool John Moores U  <fjv@astro.livjm.ac.uk>

A. Melandri (INAF-OAB), F.J. Virgili(LJMU), C.G. Mundell (LJMU) and A. 
Gomboc (U. Ljubljana) report:

The 2-m Liverpool Telescope robotically followed up GRB130610A (Swift 
trigger 557845, Cummings et al., GCN 14842) 15.5  min after the GRB 
trigger time observing with SLOAN-gri filters.

The automatic LT-TRAP procedure detected an uncatalogued fading source 
candidate at:

RA = 14:57:40.89
Dec = +28:12:25.5    (J2000)

with magnitude R~17.9 mag (vs USNOB1) ~16 min after the burst trigger.  
The object is clearly fading in all filters.

Observations and analysis are ongoing.

[GCN OPS NOTE(10jun13):  The GRB name in the firt sentence was changed
from "130410A" to "130610A".]


GRB_name: GRB130610A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14844
SUBJECT: GRB 130610A: Skynet/PROMPT detection of the optical afterglow
DATE:    13/06/10 03:57:35 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, J. Haislip, A. LaCluyze, D. Reichart, T. Berger, M. Carroll, 
H. T. Cromartie, R. Egger, A. Foster, C. Foster, N. Frank, K. Ivarsen, 
D. James, M. Maples, J. Moore, M. Nysewander, E. Speckhard, P. Taylor 
and J. A. Crain report

Skynet observed the Swift/XRT localization of GRB 130610A (Cummings et 
al., GCN 14842, Swift trigger #557845), starting at 2013-06-10, 03:14:05 
UT (t=2.03m post-trigger), with three 16" telescopes of the PROMPT array 
at CTIO, Chile.  We detect a fading afterglow in B, V and I bands at: RA 
= 14:57:40.9, Dec = 28:12:25.5 (J2000), consistent with the UVOT 
source position reported in GCN 14842.

The afterglow rises until t~3.4m, at which time the apparent magnitudes 
are B~18.1, V~17.1, I~16.6.  A preliminary light curve is at:
http://www.skynet.unc.edu/grb/grb130610a.png

Magnitudes are in the Vega system and photometry is calibrated to 4 SDSS 
stars in the field.

Skynet observations are ongoing.


GRB_name: GRB130610A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14845
SUBJECT: GRB 130610A: PAIRITEL NIR Afterglow Observations
DATE:    13/06/10 04:04:56 GMT
FROM:    Adam Morgan at U.C. Berkeley  <qmorgan@gmail.com>

A. N. Morgan & C. R. Klein (UC Berkeley) report:

We observed the field of GRB 130610A (Cummings et al., GCN 14842) with the
1.3m PAIRITEL located at Mt. Hopkins, Arizona. Observations began at
2013-Jun-07 03h35m37s UT, 0.39 hr after the Swift Trigger.  In  mosaics
(effective exposure time of ~5.85 minutes) taken simultaneously in the J,
H, and Ks filters, we detect the optical afterglow (Cummings et al., GCN
14842; Melandri et al., GCN 14843; Trotter et al. GCN 14844). The
preliminary K-band reduction is corrupted.

The preliminary photometry yields:

post burst
t_mid (hr) exp.(m)  filt  mag   m_err
0.47       5.85     J     17.49  0.16
0.47       5.85     H     16.95  0.20

Observations are ongoing. All magnitudes are given in the Vega system,
calibrated to 2MASS. No correction for Galactic extinction has been made to
the above reported values.


GRB_name: GRB130610A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14846
SUBJECT: GRB 130610A: P60 Observations
DATE:    13/06/10 05:19:12 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (NASA/GSFC) and D. A. Perley (Caltech) report on behalf of a
larger collaboration:

We have imaged the optical afterglow of the Swift GRB 130610A (Cummings et
al., GCN 14842) with the robotic Palomar 60 inch telescope.  A series of
90 s exposures in the g', r', i', and z' filters were begun starting at
04:23 UT on 2013 Jun 10 (1.18 hr after the Swift trigger).  We detect the
afterglow in individual exposures in all 4 filters.  Using nearby point
sources from SDSS for calibration, we measure a magnitude of r' = 19.8 in
our initial images.  Compared with earlier observations with the Liverpool
telescope (Melandri et al., GCN 14843), this suggests a power-law decay
index of ~ 1.2.


GRB_name: GRB130609B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14847
SUBJECT: GRB 130609B: Enhanced Swift-XRT position
DATE:    13/06/10 06:30:59 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 2407 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 130609B, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 53.77097, -40.17407 which is equivalent
to:

RA (J2000): 03h 35m 5.03s
Dec (J2000): -40d 10' 26.7"

with an uncertainty of 1.7 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB130610A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14848
SUBJECT: GRB 130610A: VLT/UVES redshift
DATE:    13/06/10 07:11:49 GMT
FROM:    Alain Smette at ESO/Chile  <asmette@eso.org>

A. Smette (ESO), C. Ledoux (ESO), P. Vreeswijk (Weizmann), A. De Cia 
(Weizmann)**,
P. Petitjean (IAP),  J. Fynbo (DARK/NBI), D. Malesani (DARK/NBI), A. Fox 
(STSCI) report:

  We have observed GRB 130610A  (Cummings et al., GCN 14842) with UVES
on the ESO-VLT, in Rapid Response Mode. Preliminary analysis of the 
automatically
reduced spectra reveals the presence of an absorption line system at z ~ 
2.092
including a damped Ly-alpha line, CIV 1548 &1550, SiIV 1393 & 1402, SiII 
1260 & 1526
FeII 1608, 2382, 2600, AlII1670, AlIII 1854 & 1862. This absorption line 
system
can be identified with the gamma-ray burst redshift.

We are grateful to the excellent support provided by Christophe Martayan
and Felipe Gaete.


GRB_name: GRB130610A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14849
SUBJECT: GRB 130610A, Swift-BAT refined analysis
DATE:    13/06/10 13:40:50 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC),  W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU), D. M. Palmer (LANL),
T. Sakamoto (AGU), G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC),
T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
  
Using the data set from T-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 130610A (trigger #557845)
(Cummings, et al., GCN Circ. 14842).  The BAT ground-calculated position is
RA, Dec = 224.414, 28.187 deg which is
    RA(J2000)  =  14h 57m 39.3s
    Dec(J2000) = +28d 11' 13.8"
with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 96%.
  
The mask-weighted light curve shows a single FRED peak.  T90 (15-350 keV) is
46.4 +- 11.2 sec (estimated error including systematics).
  
The time-averaged spectrum from T-7.04 to T+61.02 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.27 +- 0.08.  The fluence in the 15-150 keV band is 2.5 +- 0.1 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T+4.53 sec in the 15-150 keV band
is 1.7 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.
  
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/557845/BA/


GRB_name: GRB130608A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14850
SUBJECT: GRB 130608A: Further Swift-BAT analysis
DATE:    13/06/10 14:16:12 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

H. A. Krimm (GSFC/USRA)for the Swift-BAT team:

Using the full data set from T-239 to T+963 sec,we report further
analysis of BAT GRB 130608A (trigger #557771)(Krimm, et al.,
GCN Circ. 14827; Krimm, et al., GCN Circ. 14833). Information in
this Circular supersedes that presented in Krimm, et al., GCN Circ. 14833.

The BAT ground-calculated position isrefined to RA, Dec = 24.597,
41.492 deg which is
    RA(J2000)  =  01h 38m 23.3s
    Dec(J2000) = +41d 29' 30.5"
with an uncertainty of 2.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 45%.

The initial Swift-BAT circular reported a broad peak starting at
~T-25 sec, peaking at ~T+5 sec, and ending at ~T+50 sec. With further
data available we see that the mask-weighted light curve contains
precursor emission from~T-150 sec to ~T-90. BAT did not trigger on
this precursor because it occurred during a slew to the field containing
the burst.  T90 (15-350 keV) is 151.38 +- 10.84 sec (estimated error
including systematics).

The time-averaged spectrum from T-134.19 to T+22.20 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.71 +- 0.41.  The fluence in the 15-150 keV band is 9.0 +- 1.9 x 10^-07 erg/cm2.
The 1-sec peak photon flux measured from T+19.06 sec in the 15-150 keV band
is 0.6 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/557771/BA/


GRB_name: GRB130610A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14851
SUBJECT: GRB 130610A: Enhanced Swift-XRT position
DATE:    13/06/10 14:44:39 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 7625 s of XRT Photon Counting mode data and 8 UVOT
images for GRB 130610A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 224.42032, +28.20711 which is equivalent
to:

RA (J2000): 14h 57m 40.88s
Dec (J2000): +28d 12' 25.6"

with an uncertainty of 1.4 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB130609B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14852
SUBJECT: GRB 130609B: Swift-XRT refined Analysis
DATE:    13/06/10 14:46:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

C. Pagani (U. Leicester), A. Melandri (INAF-OAB), B. Sbarufatti
(INAF-OAB/PSU), G. Stratta (ASDC), D.N. Burrows (PSU), J.A. Kennea
(PSU), M.C. Stroh (PSU), A.P. Beardmore (U. Leicester), P.A. Evans (U.
Leicester) and H.A. Krimm report on behalf of the Swift-XRT team:

We have analysed 7.0 ks of XRT data for GRB 130609B (Krimm  et al. GCN
Circ. 14841),  from 66 s to 46.7 ks after the  BAT trigger. The data
comprise 1.4 ks in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Goad et al.
(GCN. Circ 14847).

The late-time light curve (from T0+5.4 ks) can be modelled with an
initial power-law decay with an index of alpha=1.42 (+0.14, -0.56),
followed by a break at T+13.6 ks to an alpha of 2.36 (+0.38, -0.22).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.840 (+/-0.029). The
best-fitting absorption column is  1.40 (+0.08, -0.07) x 10^21 cm^-2,
in excess of the Galactic value of 1.4 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.01 (+/-0.10) and a
best-fitting absorption column of 1.28 (+0.26, -0.24) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.7 x 10^-11 (5.0 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.28 (+0.26, -0.24) x 10^21 cm^-2
Galactic foreground: 1.4 x 10^20 cm^-2
Excess significance: 7.6 sigma
Photon index:      2.01 (+/-0.10)

If the light curve continues to decay with a power-law decay index of
2.36, the count rate at T+24 hours will be 8.4 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.1 x
10^-13 (4.1 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00557828.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB130610A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14853
SUBJECT: GRB 130610A: Swift-XRT refined Analysis
DATE:    13/06/10 15:22:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

B. Sbarufatti (INAF-OAB/PSU), G. Stratta (ASDC), P. D'Avanzo
(INAF-OAB), J.A. Kennea (PSU), M.C. Stroh (PSU), D.N. Burrows (PSU),
A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), B.P. Gompertz
(U. Leicester) and J.R. Cummings report on behalf of the Swift-XRT
team:

We have analysed 11 ks of XRT data for GRB 130610A (Cummings  et al.
GCN Circ. 14842),  from 139 s to 25.1 ks after the  BAT trigger. The
data comprise 116 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Osborne et al. (GCN. Circ 14851).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.17 (+/-0.03).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.04 (+/-0.15). The
best-fitting absorption column is  2.6 (+2.8, -2.6) x 10^21 cm^-2, at a
redshift of 2.092, in addition to the Galactic value of 1.9 x 10^20
cm^-2 (Kalberla et al. 2005). The counts to observed (unabsorbed)
0.3-10 keV flux conversion factor deduced from this spectrum  is 3.4 x
10^-11 (3.9 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 1.9 x 10^20 cm^-2
Intrinsic column:    2.6 (+2.8, -2.6) x 10^21 cm^-2 at z=2.092
Photon index:      2.04 (+/-0.15)

If the light curve continues to decay with a power-law decay index of
1.17, the count rate at T+24 hours will be 3.2 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x
10^-13 (1.3 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00557845.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB130610A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14854
SUBJECT: GRB 130610A: LOAO BVR Observation
DATE:    13/06/10 15:24:59 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

M. Im (CEOU/SNU), H.-I. Sung(KASI), and Y. Urata (NCU) 
on behalf of EAFON

We observed the field of GRB 130610A (Cummings et al. GCN 14842),
using a 1-m telescope at Mt. Lemmon Optical Observatory (LOAO) in
Arizona, US. The observation started at 2013-06-10 05:54:16 UT,
about 2.7 hrs after the burst alert, and a series of images were 
taken in B, R, and I-band for about 40 min.

We identify the afterglow (Melandri et al. GCN 14843), in all the 
three bands, with approximate magnitude of B = 21.35 +- 0.12, 
V=20.90 +- 0.26, and R=20.35 +- 0.18, all in Vega magnitude, calibrated 
against a star in the vicinity using SDSS photometry converted to BVR.

We thank the LOAO operator, In-Kyung Baek for performing 
the observation.


GRB_name: GRB130606B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14855
SUBJECT: GRB 130606B:  Swift/UVOT Upper Limit
DATE:    13/06/10 15:38:48 GMT
FROM:    Craig Swenson at PSU/Swift  <cswenson@astro.psu.edu>

C. A. Swenson (PSU) and D. Kocevski (NASA/GSFC/ORAU) report
on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of
GRB 130606B 106.6 ks after the Fermi/LAT trigger (Vianello
et al., GCN 14795).  No optical afterglow consistent with
the position of the potential X-ray candidate (Kennea, GCN
14820) is detected in the UVOT exposures.  A preliminary 3-
sigma upper limit using the UVOT photometric system (Breveld
et al., 2011, AIP Conf. Proc. 1358, 373) for the initial
exposures is:

Filter       T_start(s)     T_stop(s)       Exp(s)     Mag
------       ----------     ---------       ------     ---
White          106556        123017          4142     >22.6

The magnitudes in the table are not corrected for the Galactic
extinction due to the reddening of E(B-V) = 0.10 in the
direction of the burst (Schlegel et al. 1998)


GRB_name: GRB130609B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14856
SUBJECT: Konus-Wind observation of GRB 130609B
DATE:    13/06/10 16:22:33 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline,
on behalf of the Konus-Wind team, report:

The long-duration intense GRB 130609B
(Swift-BAT trigger 557828: Krimm, et al., GCN 14841)
triggered Konus-Wind at T0=77916.818 s UT (21:38:36.818)

The light curve consists of two major emission episodes:
the first one with a bright multi-peaked structure from ~T0-30 s to ~T0+55 s,
and the second, much weaker and softer episode, from ~T0+170 s to ~T0+210 s.
The emission is seen up to 7 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130609_T77916/

As observed by Konus-Wind, the burst
had a fluence of (9.4  0.7)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+3.712 s,
of (9.5  0.6)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the first emission episode
(measured from T0 to T0+54.528 s)
is best fit in the 20 keV - 18 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.84  0.05,
the high energy photon index beta = -2.39  0.15,
the peak energy Ep = 397  26 keV,
chi2 = 97/97 dof.

The time-averaged spectrum of the second emission episode
(measured from T0+169.216 to T0+210.176 s)
is best fit in the 20 keV - 18 MeV range
by the cutoff power law with the following model parameters:
the photon index alpha = -1.64  0.21,
the peak energy Ep = 198  105 keV,
chi2 = 93.7/98 dof.

The spectrum at the maximum count rate
(measured from T0 to T0+6.656 s)
is best fit in the 20 keV - 18 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.70  0.07,
the high energy photon index beta = -3.0  0.3,
the peak energy Ep = 740  90 keV,
chi2 = 105/97 dof.


All the quoted results are preliminary.


GRB_name: GRB130609B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14857
SUBJECT: GRB 130609B: Swift/UVOT Observations
DATE:    13/06/10 16:46:41 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU) and H. A. Krimm (CRESST/GSFC/USRA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130609B
85 s after the BAT trigger (Krimm et al., GCN Circ. 14841).
A fading source consistent with the XRT position (Goad et al. GCN Circ.
14847) is detected in the initial UVOT exposures.

The preliminary UVOT position is:
   RA  (J2000) =  03:35:05.11 =  53.77128 (deg.)
   Dec (J2000) = -40:10:26.7  = -40.17409 (deg.)
with an estimated uncertainty of 0.50 arc sec. (radius, 90% confidence).

Preliminary detections and 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first and second orbit
exposures are: 

Filter        T_start(s)   T_stop(s)    Exp(s)      Mag
white (fc)           84          234      147    15.47+-0.02
white               577         1891      283    17.36+-0.03
white              6046         7681      393    18.39+-0.05
v                   799         1941      136    16.89+-0.09
v                  6457         6657      196    18.00+-0.15
b                   552         1866      136    17.32+-0.06
b                  5841         7476      393    18.46+-0.09
u (fc)              297          546      245    16.31+-0.04
u                   700         1841      116    17.15+-0.08
u                  5636         7271      393    18.15+-0.09
uvw1                676         1816      136    17.61+-0.12
uvw1               5432         7067      393    18.75+-0.15
uvm2                823         1791      116    19.12+-0.35
uvm2               6662         6861      196    >19.66
uvw2                603         1916      116    >19.51
uvw2               6252         7855      362    >20.39

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.01 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB130610A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14858
SUBJECT: GRB 130610A: Fermi GBM Observation
DATE:    13/06/10 18:03:27 GMT
FROM:    Gerard Fitzpatrick at UCD  <gerard.fitzpatrick@ucdconnect.ie>

G. Fitzpatrick (UCD) and V. Pelassa (UAH)
report on behalf of the Fermi GBM Team:

At 03:12:10.50 UT on 10 June 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130610A (trigger 392526733 /130610133)
which was also detected by the Swift/BAT (Cummings et al., GCN Circ. 14842).
The GBM on-ground location is consistent with the Swift position.

The GBM light curve consists of a single peak
with a duration (T90) of about 28 s (50-300 keV).
The time-averaged spectrum from T0-2.6 s to T0+25.7 s is
adequately fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.0 +/- 0.1 and
the cutoff energy, parameterized as Epeak, is 294.9 +/- 42.9 keV

The event fluence (10-1000 keV) in this time interval is
(6.1 +/- 0.4)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+8.0 s in the 10-1000 keV band is 4.5 +/- 0.9 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog.


GRB_name: GRB130610A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14859
SUBJECT: GRB 130610A: Swift/UVOT Observations 
DATE:    13/06/10 18:12:42 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU) and J. R. Cummings (NASA/UMBC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130610A
140 s after the BAT trigger (Cummings et al., GCN Circ. 14842).
A fading source consistent with the XRT position (Cummings et al. GCN Circ. 14842)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
   RA  (J2000) =  14:57:40.88 = 224.42034 (deg.)
   Dec (J2000) = +28:12:25.8  =  28.20717 (deg.)
with an estimated uncertainty of 0.51 arc sec. (radius, 90% confidence).

Preliminary detections and 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are listed below.
The lack of detection in the NUV filters would be consistent with the z=2.1 redshift 
reported by Smette et al. (GCN Circ. 14848).

Filter     T_start(s)   T_stop(s)    Exp(s)       Mag

white (fc)       140         290        147     17.85+-0.04
white           1491        1857         58     19.56+-0.19
white           5267        6902        393     20.47+-0.15
v               1540        7312        451    >20.07
b               1467        2005         77     19.12+-0.20
b               6498       19320       1754     21.72+-0.38
u                298         441        140     17.67+-0.09
u               1614        1980         58     19.00+-0.30
uvw1            1589        1956         58    >19.05
uvm2            1911       23463       1298    >21.09
uvw2            1863        7108        412    >20.63

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.02 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB130610A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14860
SUBJECT: GRB 130610A: ISON-NM optical observations
DATE:    13/06/10 18:56:07 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

L. Elenin (KIAM),  V. Savanevych (KNURE),  A. Bryukhovetskiy (NSFCTC), 
I. Molotov (KIAM), A. Pozanenko (IKI) report on behalf of  larger GRB 
follow-up collaboration:

We observed of  the field of  the Swift GRB 130610A (Cummings et al., 
GCN 14842)  with 0.45-m telescope of ISON-NM observatory starting on 
June, 10 (UT) 03:53:49. Series of 30 s  exposures were obtained in clear 
filter. In the combined images we detect afterglow  (Cummings et al., 
GCN 14842; Melandri et al., GCN 14843; Trotter et al., GCN 14844). 
Preliminary photometry  is based  on the SDSS nearby  stars:


UT start,   T0+       Filter  Exposure,  OT,
             days              s
03:53:49    0.03531   none    25*30     19.33 Â± 0.07
04:12:33    0.04831   none    25*30     19.56 Â± 0.10


GRB_name: GRB130608A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14861
SUBJECT: GRB 130608A: ISON-Kislovodsk optical upper limit
DATE:    13/06/10 20:01:43 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), V. Linkov (ISON), M.Suvorov (ISON), V. Nevskiy (ISON), 
D. Ivanov (ISON),  I. Molotov (KIAM), A. Pozanenko (IKI),  report on 
behalf of larger collaboration:

We observed the field of  GRB 130608A (Krimm  et al., GCN 14827) with
SANTEL-400AN (0.4-m f/3)  telescope of ISON-Kislovodsk observatory.
Observations started on  Jun. 09 (UT) 00:01:42.   We obtained  several
unfiltered images  of 60 s exposure. We do not detect any source within 
enhanced XRT error circle (Beardmore et al., GCN 14832). Preliminary 
photometry of combined image is based on USNO-B1.0 (R2) nearby  stars:

T_start,             T0+,      Exp,   Filter,  UL (3 sigma)
(UT)                 mid (d)   (s)

2013-06-09T00:01:42  0.04170   960    none     >18.1


GRB_name: GRB130609B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14862
SUBJECT: GRB 130609B, Swift-BAT refined analysis
DATE:    13/06/10 21:39:05 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

A. Y. Lien (NASA/GSFC/ORAU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):

Using the data set from T-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 130609B (trigger #557828)
(Krimm, et al., GCN Circ. 13841).  The BAT ground-calculated position is
RA, Dec = 53.776, -40.168 deg which is
     RA(J2000)  =  03h 35m 06.2s
     Dec(J2000) = -40d 10' 04.0"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 43%.

The mask-weighted light curve shows an initial complex of two main
overlapping peaks with numerous subsidiary peaks, with strong emission
between T-10 and T+50 sec and low-level emission between T-30 and T+120 sec.
The highest points are at T+4 and T+18 sec.  Then there is a second, weaker
and softer pair of overlapping peaks between T+160 sec and T+220 sec.  This
second set of peaks is consistent with a flare seen in the Swift-XRT.
T90 (15-350 keV) is 191.98 +- 2.44 sec (estimated error including systematics)
We note that receipt of the full event data for GRB 130609B may reveal
further late-time peaks and require a revision of the T90 estimate.  We will
report on the full data set in a later Circular.

The time-averaged spectrum from T-7.84 to T+213.25 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.23 +- 0.04.  The fluence in the 15-150 keV band is 1.6 +- 0.0 x 10^-05
erg/cm2. The 1-sec peak photon flux measured from T+16.78 sec in the 15-150 keV
band is 8.5 +- 0.4 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/557828/BA/


GRB_name: GRB130609A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14863
SUBJECT: GRB 130609A: Radio Observations (5.8, 22 and 85 GHz)
DATE:    13/06/10 23:18:16 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

B. A. Zauderer, W. Fong, E. Berger and T. Laskar (Harvard) report
on behalf of the CARMA Key Project, "A Millimeter View of the
Transient Universe" and a larger collaboration:

"We observed the position of GRB 130609A (Cummings et al. GCN 14828;
also detected by Fitzpatrick et al. GCN 14839) beginning 2013 Jun 9.88 UT
(dt = 0.75 d) with the Very Large Array (VLA) and beginning  2013 Jun 10.05
UT (dt = 0.92 d) with the Combined Array for Research in Millimeter Astronomy
(CARMA).  For this dark burst with deep optical and NIR afterglow upper limits
(e.g. Perley et al. GCN 14830 and Butler et al. GCN 14831), we find no
significant radio emission at the enhanced Swift-XRT position (Evans et al.;
GCN 14835) with the following three-sigma upper limits:
 5.8  GHz  <35 uJy  (VLA)
21.8  GHz  <60 uJy  (VLA)
84.5  GHz   <0.36 mJy (CARMA).

We thank the VLA and CARMA staff and observers for their support of these
observations."


GRB_name: GRB130606A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14864
SUBJECT: GRB 130606A: CrAO optical upper limit
DATE:    13/06/11 00:18:42 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

V. Rumyantsev (CrAO), N.Pit' (CrAO), Ð. Volnova (IKI), A. Pozanenko (IKI) 
report on behalf of  larger GRB  follow-up collaboration:

We observed the field of  the Swift GRB 130606A (Ukwatta  et al., GCN 
14781) with  AZT-11 telescope of CrAO observatory  starting on  June 06
(UT) 21:59:60. We took  several images in R-filter of 180 s exposure. The 
afterglow (Jelinek et al., GCN 14782; Xu et al.,  GCN 14783; Nagayama et 
al., GCN 14784)   is not detected in a combined image.   A photometry  is 
based  on the same SDSS stars we used  in GCN 14806:

Start         T0+,        Filter   Exposure,   OT,        UL (3 sigma)
UT             mid, d                 (s)

21:59:60  0.0489    R        10x180      n/d         20.7


GRB_name: GRB130603B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14865
SUBJECT: GMRT radio observation of GRB 130603B
DATE:    13/06/11 07:16:47 GMT
FROM:    Poonam Chandra at TIFR  <poonam@ncra.tifr.res.in>

Poonam Chandra (NCRA-TIFR) reports:

We carried out Giant Metrewave Radio Telescope (GMRT) observations of
GRB 130427A at 1390 GHz band on 2013 June 07.38 UT. We don't detect the
GRB in our radio observations. The 3-sigma upper limit at the GRB afterglow
position (Levan et al., GCN 14742; de Ugarte Postigo et al., GCN 14743;
Foley et al., GCN 14745; Cucchiara et al., GCN 14748) is 273 uJy.

We thank GMRT staff for making these observations possible.

-- 

**********************************************************************
Poonam Chandra                          Phone: +91 20 2571 9290
Tata Institute of Fundamental Research  Email: poonam@ncra.tifr.res.in
National Center for Radio Astrophysics  Home: ncra.tifr.res.in/~poonam
Post Bag 3, Pune University campus
Ganeshkhind, Pune 411 008, INDIA


GRB_name: GRB130609B
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14866
SUBJECT: GRB 130609B: GROND observations
DATE:    13/06/11 13:16:42 GMT
FROM:    Andrea Rossi at TLS Tautenburg  <rossi@tls-tautenburg.de>

S. Schmidl, A. Rossi (both TLS Tautenburg), and J. Greiner (MPE
Garching) report on behalf of the GROND team:

We observed the field of GRB 130609B (Swift trigger 557828; Krimm et
al., GCN #14841) simultaneously in g'r'i'z'JHK with GROND (Greiner
et al. 2008, PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope
  at La Silla Observatory (Chile).

Observations started at 09:30 UT on 11th June 2013, 35.9 hours after
the GRB trigger. They were performed at an average seeing of 1.6"
and at an average airmass of 2.2.

We detect a source at the position of the UVOT afterglow (Siegel
et al.; GCN #14857), and based on images taken at a mid-time of
09:45 UT, with total exposures of 25 minutes in g'r'i'z' and 20
minutes in JHK, we estimate preliminary magnitudes (all in AB) of

g' = 22.2 +/- 0.1 mag,
r' = 21.7 +/- 0.1 mag,
i' = 21.1 +/- 0.2 mag,
z' = 20.9 +/- 0.2 mag,
J = 20.6 +/- 0.3 mag,
H = 19.8 +/- 0.4 mag, and
K = 19.4 +/- 0.4 mag.

The source is brighter than what one could expect extrapolating
the early UVOT data (Siegel et al.; GCN #14857) and could be either
a plateau/flare, or due to the contribution of the host galaxy.

Given magnitudes are calibrated against GROND zeropoints as well as
2MASS field stars and are not corrected for the expected Galactic
  foreground extinction corresponding to a reddening of E_(B-V)=0.01 mag
in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB130609B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14867
SUBJECT: GRB 130609B, Further Swift-BAT refined analysis
DATE:    13/06/11 13:22:03 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

H. A. Krimm (GSFC/USRA) and J. R. Cummings (GSFC/UMBC)
for the Swift-BAT team:

Using the full data set from T-239 to T+963 sec from the recent telemetry 
downlink, we report final analysis of BAT GRB 130609B (trigger #557828)
(Krimm, et al., GCN Circ. 14841; Lien at al., GCN Circ. 14862).

In addition to the peaks described in Lien at al., GCN Circ. 14862, we report
that there is a small peak in the BAT at around T+270 sec, coincident with a
second flare in the XRT.  T90 (15-350 keV) is 210.6 +- 15.1 sec (estimated
error including systematics).

The time-averaged spectrum from T-7.8 to T+307.6 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.32 +- 0.04.  The fluence and peak photon flux are as reported in GCN Circ. 
14862. The quoted error is at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/557828/BA/


GRB_name: GRB130610B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14868
SUBJECT: IPN Triangulation of GRB 130610B (long/multipeaked)
DATE:    13/06/11 14:51:30 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

K. Hurley and J. Goldsten, on behalf of MESSENGER GRNS GRB team,

S. Golenetskii, R. Aptekar, V. Pal'shin, D. Frederiks,
D. Svinkin, and T. Cline on behalf of the Konus-Wind team, and

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C.
Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, report:

The long-duration GRB 130610B has been observed by Konus-Wind, INTEGRAL 
(SPI-ACS), and MESSENGER (GRNS), so far, at about 76880 s UT (21:21:20).

We have triangulated it to a preliminary, 3 sigma error box whose 
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   176.359 (11h 45m 26s) -32.187 (-32d 11' 12")
  Corners:
   176.728 (11h 46m 55s) -31.962 (-31d 57' 43")
   176.012 (11h 44m 03s) -32.983 (-32d 58' 58")
   175.989 (11h 43m 57s) -32.409 (-32d 24' 33")
   176.709 (11h 46m 50s) -31.377 (-31d 22' 36")
  ---------------------------------------------
The error box area is 0.37 sq. deg, and its maximum dimension is
1.71 deg (the minimum one is 0.31 deg).

This box may be improved.

A triangulation map is posted at 
http://www.ioffe.ru/LEA/GRBs/GRB130610_T76879/IPN/

The time history and spectrum will be given in a forthcoming GCN Circular.


GRB_name: GRB130609B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14869
SUBJECT: GRB 130609B: Fermi GBM observation
DATE:    13/06/11 14:52:13 GMT
FROM:    Veronique Pelassa at UAH  <vero.pelassa@gmail.com>

V. Pelassa (UAH) reports on behalf of the Fermi GBM Team:

"At 21:38:35.61 UT on 09 June 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130609B (trigger 392506718 / 130609902),
which was also detected by the Swift/BAT (H.A. Krimm et al. 2013, GCN 14841).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 117 degrees.

The GBM light curve consists of two bright peaks within 30s of trigger
and a fainter bump at 170s after trigger with a duration (T90) of about
191 s (50-300 keV).

The time-averaged spectrum from T0+0.003s to T0+28.672s is well fit by
a power law function with an exponential high-energy cutoff.
The power law index is -0.70 +/- 0.02 and the cutoff energy,
parameterized as Epeak, is 536 +/- 18 keV
(Castor statistics 474 for 365 d.o.f.).

The event fluence (10-1000 keV) in this time interval is
(6.02 +/- 0.07)E-05 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+6.592 s in the 10-1000 keV band is 13.6 +/-0.4 ph/s/cm^2.

A Band function fits the spectrum equally well (Castor statistics 468
for 364 d.o.f.)
with Epeak= 491 +/- 20 keV, alpha = -0.66 +/- 0.02 and beta = -2.6 +/- 0.2.


The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB130608A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14870
SUBJECT: GRB 130608A: Swift/UVOT Upper Limits
DATE:    13/06/11 14:55:09 GMT
FROM:    Stephen Holland at STScI  <sholland@stsci.edu>

S. T. Holland (STScI) and Hans Krimm (CRESST/GSFC/USRA) report on
behalf of the Swift/UVOT team:

    The Swift/UVOT began settled observations of the field of GRB
130608A starting 168 s after the BAT trigger (Krimm et al. 2013, GCNC
14827).  We do not detect any new source consistent with the
UVOT-enhanced XRT position (Beardmore 2013, GCNC 14832) in any of the
UVOT exposures.  Preliminary 3-sigma upper limits using the UVOT
photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373)
for the finding chart (FC) exposures and initial summed exposures are
presented below.

Filter      TSTART      TSTOP   Exposure      Mag
-------------------------------------------------
white (FC)     169        318        147    >21.0
               607        626         19    >19.6
u (FC)         327        576        246    >20.1
               731        750         19    >18.4
-------------------------------------------------
v              657     12,041       1154    >20.6
b              583       6742        452    >20.8
u             4899       6536        393    >20.5
uvw1           706       6331        432    >20.6
uvm2           681     12,759       1134    >21.3
uvw2           632     11,127       1199    >21.5
white          858       6946        560    >21.5
-------------------------------------------------

    The quoted upper limits have not been corrected for the expected
extinction due to the Galactic reddening along the line of sight to
this burst of E(B-V) = 0.05 mag (Schlafly et al. 2011, ApJS, 737,
103).


GRB_name: GRB130609A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14871
SUBJECT: GRB 130609A: Swift/UVOT Upper Limits
DATE:    13/06/11 14:56:06 GMT
FROM:    Stephen Holland at STScI  <sholland@stsci.edu>

S. T. Holland (STScI) and J. R. Cummings (NASA/UMBC) report on behalf
of the Swift/UVOT team:

    The Swift/UVOT began settled observations of the field of GRB
130609A starting 70 s after the BAT trigger (Cummings et al. 2013,
GCNC 14828).  We do not detect any new source consistent with the
UVOT-enhanced XRT position (Evans 2013, GCNC 14835) in any of the UVOT
exposures.  Preliminary 3-sigma upper limits using the UVOT
photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373)
for the finding chart (FC) exposures and initial summed exposures are
presented below.

Filter      TSTART      TSTOP   Exposure      Mag
-------------------------------------------------
white (FC)      70        220        147    >21.0
               562        582         19    >19.8
u (FC)         282        532        246    >20.3
               686        706         19    >18.6
-------------------------------------------------
v              612       6212        413    >19.9
b              537     18,175       1773    >21.7
u             5191     23,545       2254    >21.4
uvw1          4987     23,257       2164    >21.5
uvm2          4782     22,351       1279    >21.3
uvw2          4372       6007        393    >20.8
white         4166     12,406       1022    >22.0
-------------------------------------------------

    The quoted upper limits have not been corrected for the expected
extinction due to the Galactic reddening along the line of sight to
this burst of E(B-V) = 0.03 mag (Schlafly et al. 2011, ApJS, 737,
103).


GRB_name: GRB130610B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14872
SUBJECT: Konus-Wind observation of GRB 130610B
DATE:    13/06/11 16:23:38 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline, on behalf
of the Konus-Wind team, report:

The long-duration GRB 130610B
(IPN triangulation: Hurley at al., GCN 14868)
triggered Konus-Wind at T0=76879.093 s UT (21:21:19.093).

The light curve  from ~T0-0.5 s to ~T0+16s shows multiple pulses
with decaying spectral hardness.
The pulses form a quasi-periodic structure with the period of ~1s
during first ~5 seconds of the burst, which is followed, after T0+7s,
by the three pulses separated by ~2.7s.

A weak count rate excess in the soft energy channel (20-80 keV)
is observed from ~T0-170 s to ~T0-100 s in the instrument
background mode; however, its attribution to GRB 130610B
is not yet confirmed.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130610_T76879/

As observed by Konus-Wind, the burst
had a fluence of (8.5  0.4)x10-6 erg/cm2,
and a 64-ms peak flux, measured from T0+0.256s,
of (6.0  0.5)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+16.640 s)
is best fit in the 20 keV - 15 MeV range
by the cutoff power law with the following model parameters:
the photon index alpha = -1.7  0.1,
the peak energy Ep = 62  9 keV,
chi2 = 99/98 dof.

The 3-channel spectrum at the maximum count rate
(measured from T0+0.256 to T0+0.384 s)
can be modeled, in the 20 keV - 1.35 MeV range,
by the cutoff power law with the following model parameters:
the photon index alpha = -0.52  0.08,
and the peak energy Ep = 444  30 keV.

All the quoted results are preliminary.


GRB_name: GRB130612A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14874
SUBJECT: GRB 130612A: Swift detection of a burst with an optical counterpart
DATE:    13/06/12 03:44:00 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

J. L. Racusin (NASA/GSFC), J. R. Cummings (NASA/UMBC),
N. Gehrels (NASA/GSFC), J. A. Kennea (PSU),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
C. Pagani (U Leicester), K. L. Page (U Leicester),
D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/PSU) and
M. H. Siegel (PSU) report on behalf of the Swift Team:

At 03:22:22 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130612A (trigger=557976).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 259.804, +16.706 which is 
   RA(J2000) = 17h 19m 13s
   Dec(J2000) = +16d 42' 21"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 5 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 03:23:49.1 UT, 87.0 seconds after
the BAT trigger. The position determined from promptly downlinked data
differs significantly from the on-board position, suggesting that the
XRT may have centroided on a cosmic ray; the initial XRT position
notice should be treated with caution. Using promptly downlinked data
we find an uncatalogued X-ray source with an enhanced position: RA, Dec
259.7940, 16.7205 which is equivalent to:
   RA(J2000)  = 17h 19m 10.55s
   Dec(J2000) = +16d 43' 13.9"
with an uncertainty of 2.7 arcseconds (radius, 90% containment). This
location is 62 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (5.96 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 7.8
(+9.63/-6.58) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of  91 seconds with the White filter
starting 94 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 17:19:10.59 = 259.79411
  DEC(J2000) = +16:43:11.7  =  16.71991
with a 90%-confidence error radius of about 0.64 arc sec. This position is 2.3
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.80 with a 1-sigma error of about  0.15. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.08. 

Burst Advocate for this burst is J. L. Racusin (judith.racusin AT nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB130612A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14875
SUBJECT: GRB 130612A: Liverpool Telescope Afterglow detection
DATE:    13/06/12 03:58:00 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

A. Melandri (INAF-OAB), C.G. Mundell (LJMU) and A. Gomboc (U.  
Ljubljana) )report:

The 2-m Liverpool Telescope robotically followed up GRB130612A (Swift  
trigger 557976, Racusin et al., GCN 14874) ~16  min after the GRB  
trigger time observing with SLOAN-gri filters.

The automatic LT-TRAP procedure detected an uncatalogued fading source  
candidate at:

RA = 17:19:10.57
Dec = +16:43:11.6    (J2000)

with magnitude R~18.9 mag (vs USNOB1) ~16 min after the burst  
trigger.  The object is clearly fading in all filters.

Observations and analysis are ongoing.


GRB_name: GRB130612A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14876
SUBJECT: GRB 130612A: PAIRITEL NIR Afterglow Observations
DATE:    13/06/12 04:07:12 GMT
FROM:    Adam Morgan at U.C. Berkeley  <qmorgan@gmail.com>

A. N. Morgan (UC Berkeley) reports:

We observed the field of GRB 130612A (Racusin et al., GCN 14874) with the
1.3m PAIRITEL located at Mt. Hopkins, Arizona. Observations began at
2013-Jun-12 03h29m25s UT, 6.65 minutes after the Swift Trigger.  In
 mosaics (consisting of 48 ~8 second images for a total effective exposure
time of 6.3 minutes) taken simultaneously in the J, H, and Ks filters, we
detect the optical afterglow (Racusin et al., GCN 14874; Melandri et al.,
GCN 14875). The preliminary K-band reduction is corrupted.  The
observations quoted below began at 3:32 UT, ~9.5 minutes after the Swift
trigger, after an automatic pointing reset by our telescope.

The preliminary photometry yields:

post burst
t_mid (m) exp.(m)  filt  mag   m_err
14.6      6.3     J     17.26  0.12
14.6      6.3     H     16.78  0.15

Observations are ongoing. All magnitudes are given in the Vega system,
calibrated to 2MASS. No correction for Galactic extinction has been made to
the above reported values.


GRB_name: GRB130612A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14877
SUBJECT: GRB 130612A: Skynet/PROMPT detection of the optical afterglow
DATE:    13/06/12 04:36:09 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, J. Haislip, D. Reichart, A. LaCluyze, T. Berger, M. 
Carroll, H. T. Cromartie, R. Egger, A. Foster, C. Foster, N. Frank, K. 
Ivarsen, D. James, M. Maples, J. Moore, M. Nysewander, E. Speckhard, P. 
Taylor and J. A. Crain report

Skynet observed the Swift XRT localization of the field of GRB 130612A 
(Racusin et al., GCN 14874, Swift trigger #557976), beginning at 
2013-06-12, 3:23:27 UT (t=70s post-trigger) using three 16" telescopes 
of the PROMPT array at Cerro Tololo, Chile.  We detect a fading 
afterglow in the B, V and I bands at a position (J2000)
RA: 17:19:10.6
Dec: 16:43:11.6,
consistent with the detections of Racusin et al. (GCN 14874), Melandri, 
Mundell & Gomboc (GCN 14875), and Morgan (GCN 14876).

A preliminary light curve is at:
http://www.skynet.unc.edu/grb/grb130612a.png

Preliminary photometry is calibrated to 5 NOMAD/USNO B1.0 stars in the 
field, and magnitudes are in the Vega system.

Skynet observations are ongoing.

[GCN OPS NOTE(12jun13): Per author's request, the typo in JH's name was corrected.]


GRB_name: GRB130612A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14878
SUBJECT: GRB 130612A: NOT optical observations
DATE:    13/06/12 04:50:12 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

P. Jakobsson (U. Iceland), D. Xu (DARK/NBI), D. Malesani (DARK/NBI),
K. Mikkelsen (U. Oslo), N. Aghanim (CNRS & Universite Paris-Sud Orsay)
report on behalf of a larger collaboration:

We observed the optical afterglow of GRB 130612A (Racusin et al., GCN
14874; Melandri et al., GCN 14875) using the 2.5-m Nordic Optical
Telescope (NOT) equipped with the ALFOSC camera. We obtained 4x300s
R-band images with a median time 04:06:09 UT on 12 June 2013 (i.e.
0.73 hr after the burst).

The optical afterglow was clearly detected with R ~ 20.3 mag
calibrated with nearby stars in the USNO B1 catalog.

[GCN OPS NOTE(12jun13): Per author's request, NA was added to the author list.]


GRB_name: GRB130612A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14879
SUBJECT: GRB 130612A: P60 Observations
DATE:    13/06/12 04:56:01 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko (NASA/GSFC) and D. A. Perley report on behalf of a larger
collaboration:

We have imaged the field of the Swift GRB 130612A (Racusin et al., GCN
14874) with the robotic Palomar 60 inch telescope.  Observations consist
of individual 120 s frames in the g', r', i', and z' filters beginning at
4:20 UT on 2013 June 12 (58 minutes after the Swift trigger).  The
optical afterglow is detected in individual frames in all four
filters.  Using several nearby point sources from the USNO-B1 catalog for
reference, we measure a magnitude of R = 20.8 at this time.


GRB_name: GRB130612A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14880
SUBJECT: GRB 130612A: RATIR Optical Observations
DATE:    13/06/12 05:11:03 GMT
FROM:    Alan M. Watson at Instituto de Astronomia UNAM  <alan@astro.unam.mx>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC),
William H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori
Fox (UCB) J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino
Cucchiara (UCSC), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), Jos A. de Diego (UNAM), Leonid Georgiev (UNAM),
Jess Gonzlez (UNAM), Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC),
and Harvey Moseley (GSFC) report:

We observed the field of GRB 130612A (Racusin, et al., GCN Circular
14874) with the Reionization and Transients Infrared Camera (RATIR;
www.ratir.org) on the 1.5m Harold Johnson Telescope at the Observatorio
Astronmico Nacional on Sierra San Pedro Mrtir from 2013/06 12.16 to
2013/06 12.20 UTC (0.40 to 1.31 hours after the BAT trigger), obtaining
a total of 0.71 hours exposure in the r' and i' bands.

For a source within the Swift-XRT error circle, in comparison with
USNO-B1 and 2MASS, we obtain the following detections:

r' 21.23  0.07
i' 21.05  0.06

These magnitudes are in the AB system and not corrected for Galactic
extinction in the direction of the GRB.

The position of the source is consistent with the UVOT afterglow
position Racusin, et al., GCN Circular 14874). The afterglow appears to
have faded considerably since the earlier observations reported by
Melandri et al. (GCN Circular 14875), and Jakobsson et al. (GCN Circular
14878).

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB130612A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14881
SUBJECT: GRB130612A OSN I-band observations
DATE:    13/06/12 05:40:32 GMT
FROM:    Juan Carlos Tello at IAA-CSIC  <jtello@iaa.es>

J.C.Tello, V. Casanova (IAA-CSIC), J. Gorosabel (UPV-EHU, IAA-CSIC),
A.J.Castro-Tirado, R. Sanchez-Ramirez, M. Jelinek (IAA-CSIC), on behalf of
a larger collaboration report:

We observed the field of GRB130612A (Racusin et al., GCNC 14874) in the
I-band with the 1.5m telescope in Sierra Nevada, Granada, Spain. Combining
33x10s images (for a total 330 seconds of exposure) spanning from 03h38m
(16 minutes after the burst) to 03h55m (with a mean time of 25 minutes
after the burst) we observe the reported afterglow (Melandri et al., GCNC
14875) with a magnitude of I(Vega) ~ 18.7 when compared to the USNO B1.0
catalog.


GRB_name: GRB130612A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14882
SUBJECT: GRB 130612A: VLT/X-shooter redshift
DATE:    13/06/12 06:18:45 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir (U. Leicester), K. Wiersema (U. Leicester), D. Xu
(DARK/NBI), J. P. U. Fynbo (DARK/NBI) report for a larger
collaboration:

We observed the afterglow of GRB 130612A (Racusin et al. GCN 14874)
with VLT/X-shooter, beginning at 2013-06-12 04:28 UT, about 66 mins
after the burst.

Preliminary analysis of the spectrum reveals absorption lines of FeII
2261, 2374, 2344, 2383, 2600, 2587, 2600, 2607, MnII 2577, MgII
2796/2803 and MgI 2852 at a common redshift of z=2.006.  This
is consistent with a break seen in the UVB arm spectrum due to a 
damped Lyman-alpha feature at ~3650 A. We therefore propose 
this to be the redshift of the GRB.

We thank the staff at Paranal, particularly Christophe Martayan, for
obtaining these observations.


GRB_name: GRB130612A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14883
SUBJECT: GRB 130612A: TAROT La Silla observatory optical observations
DATE:    13/06/12 08:53:25 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (IRAP-CNRS-OMP),
Boer M., Siellez K., Dereli H., Bardho O. (UNS-CNRS-OCA),
Atteia J.L. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 130612A detected by SWIFT
(trigger 557976) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 34.4s after the GRB trigger
(14.5s after the notice). The elevation of the field increased from
40 degrees above horizon and weather conditions
were excellents.

The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
We detect the OT detected by Racusin et al. (GCNC 14874),
Melandri et al. (GCNC 14875). Photometry is done using
NOMAD-1 1067-0303513 (R.A.=259.7905194 Dec=+16.7139250
R=16.9) as reference star.

At the start of the trail t0+34.4s R=16.9
At the end of the trail   t0+94.4s R=17.5

Next images are acquired in tracking mode.
The afterglow is visible more than 30
minutes after the burst. One of the last
measurement is:

 From t0+1466s to t0+2113s  R=19.9

Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.

This message may be cited.


GRB_name: GRB130612A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14884
SUBJECT: GRB 130612A: Enhanced Swift-XRT position
DATE:    13/06/12 11:57:53 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 501 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 130612A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 259.79393, +16.71971 which is equivalent
to:

RA (J2000): 17h 19m 10.54s
Dec (J2000): +16d 43' 11.0"

with an uncertainty of 1.9 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB130612A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14885
SUBJECT: GRB 130612A: Zadko observatory - Gingin optical observations
DATE:    13/06/12 13:55:06 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

A. Klotz (IRAP-CNRS-OMP), D. Macpherson (UWA/ICRAR), D. Coward (UWA),
B. Gendre (IRAP-CNRS-OMP), M. Boer, K. Siellez, H. Dereli ,
O. Bardho (UNS-CNRS-OCA), A. Williams (PO-UWA), R. Martin (PO-UWA)
report:

We imaged the field of GRB 130612A detected by SWIFT
(trigger 557976) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 9.3h after the GRB trigger.
The elevation of the field increased from
20 degrees above horizon and weather conditions
were good.

We have not detected the OT detected by Racusin et al.
(GCNC 14874), Melandri et al. (GCNC 14875):

 From t0+9.3h to t0+10.2h  Rlim = 21.2

Magnitudes are not corrected for galactic dust extinction.

This message may be cited.


GRB_name: GRB130612A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14886
SUBJECT: GRB 130612A: Swift-XRT refined Analysis
DATE:    13/06/12 15:44:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

G. Stratta (ASDC), P. D'Avanzo (INAF-OAB), M.C. Stroh (PSU), D.N.
Burrows (PSU), J.A. Kennea (PSU), P.A. Evans (U. Leicester), B.P.
Gompertz (U. Leicester), J.P. Osborne (U. Leicester), V. D'Elia (ASDC)
and J.L. Racusin report on behalf of the Swift-XRT team:

We have analysed 11 ks of XRT data for GRB 130612A (Racusin  et al. GCN
Circ. 14874),  from 74 s to 30.7 ks after the  BAT trigger. The data
comprise 233 s in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Beardmore
et al. (GCN. Circ 14884).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.96 (+0.09, -0.08).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.19 (+0.28, -0.26). The
best-fitting absorption column is  7.7 (+6.6, -5.5) x 10^21 cm^-2, at a
redshift of 2.006, in addition to the Galactic value of 6.0 x 10^20
cm^-2 (Kalberla et al. 2005). The counts to observed (unabsorbed)
0.3-10 keV flux conversion factor deduced from this spectrum  is 3.3 x
10^-11 (4.7 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 6.0 x 10^20 cm^-2
Intrinsic column:    7.7 (+6.6, -5.5) x 10^21 cm^-2 at z=2.006
Photon index:      2.19 (+0.28, -0.26)

If the light curve continues to decay with a power-law decay index of
0.96, the count rate at T+24 hours will be 1.8 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.1 x
10^-14 (8.7 x 10^-14) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00557976.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB130612A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14887
SUBJECT: GRB 130612A: Swift/UVOT Detection
DATE:    13/06/12 17:42:22 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (MSSL-UCL) and J. L. Racusin (NASA/GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130612A 94 
s after the BAT trigger (Racusin et al., GCN Circ. 14874).
A fading source consistent with the XRT position (Beardmore et al. GCN 
Circ. 14884) is detected in the initial UVOT exposures.

The preliminary UVOT position is:
     RA  (J2000) =  17:19:10.58 = 259.79408 (deg.)
     Dec (J2000) = +16:43:11.9  =  16.71996 (deg.)
with an estimated uncertainty of 0.53 arc sec. (radius, 90% confidence).

Preliminary detections and 3-sigma upper limits using the UVOT 
photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for 
the early exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)           Mag

white               94          185           89         18.97  0.07
v                  763         7763          549        >20.6
b                  688        13692         1307        >21.3
u                  664         1655          117         19.68  0.24
w1                 639        18651         2143        >21.6
m2                 614        17743         1406        >21.6
w2                 738         7559          549        >21.1

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 0.08 in the direction of the 
burst (Schlegel et al. 1998).


GRB_name: GRB130609B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14888
SUBJECT: GRB 130609B: Theoretical redshift estimation
DATE:    13/06/12 18:57:55 GMT
FROM:    Remo Rufinni at ICRA  <ruffini@icra.it>

R. Ruffini, C.L. Bianco, M. Enderli, M. Muccino, A.V. Penacchioni, G.B. Pisani, J.A. Rueda, N. Sahakyan, Y. Wang, L. Izzo report:

The late X-ray observations of GRB 130609B evidences a pattern typical of a family of GRBs associated to Supernovae following the Induced Gravitational Collapse (IGC) paradigm. We estimate a cosmological redshift for the GRB of approximately z=1.3. We encourage observations.


GRB_name: GRB130612A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14889
SUBJECT: GRB 130612A: MITSuME Okayama upper limits
DATE:    13/06/12 19:00:02 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ),
S. Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech)
report on behalf of MITSuME and OISTER collaboration:

We observed the field of GRB 130612A (Racusin et al., GCNC 14874)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.

The observation started on 2013-06-12 11:27:22 UT (~8.08 h after the burst).
We could not detect the previously reported afterglow
(Racusin et al., GCNC 14874; Melandri et al., GCNC 14875) in all the three bands.

Three sigma upper limits of the OT are listed below.
We used GSC 2.3 catalog for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'     Rc     Ic
-----------------------------------------------------
0.43348    13:46:34    7800.0   >20.2  >20.2  >19.4
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB130612A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14890
SUBJECT: GRB 130612A:  ISON-NM optical observations
DATE:    13/06/12 21:13:30 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

L. Elenin (KIAM), A. Volnova (IKI), V. Savanevych (KNURE), A. 
Bryukhovetskiy (NSFCTC), I. Molotov (KIAM), A. Pozanenko (IKI) report on 
behalf of  larger GRB follow-up collaboration:

We observed of  the field of  the Swift GRB 130612A (Racusin et al., GCN 
14874)  with 0.45-m telescope of ISON-NM observatory starting on June, 
12 (UT) 04:06:14. Series of 30 s exposures were obtained in clear 
filter. In the combined images we detected afterglow (Racusin et al., 
GCN 14874; Melandri et al., GCN14875) in coordinates (J2000) 17 19 10.63 
+16 43 12.0. Preliminary photometry  is based  on the USNO-B1.0 
1067-0299350 star assuming R=18.92.

UT start,           T0+    Filter Exposure, OT
                     mid,d         s

2013-06-12T04:06:14 0.0305 none  30*30      20.75 +/- 0.15
2013-06-12T04:29:28 0.0466 none  30*30      21.25 +/- 0.20


GRB_name: GRB130610A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14891
SUBJECT: GRB 130610A: iTelescope T21 optical observations
DATE:    13/06/13 05:26:42 GMT
FROM:    Veli-Pekka Hentunen at Taurus Hill Obs,A95  <veli-pekka.hentunen@kassiopeia.net>

Veli-Pekka Hentunen, Markku Nissinen and Tuomo Salmi (Taurus Hill
Observatory, Varkaus, Finland) report:

We have detected GRB 130610A optical afterglow at iTelescope observatory
T21 (Mayhill, New Mexico) 0.43m/6.8 astrograph and FLI-PL6303E CCD
camera. Three unfiltered images and three photometric R filter images with 
300 sec exposure time were made.

The afterglow was detected at following position RA 14:57:40.86 and 
DEC +28:12:26.0

The following magnitudes were obtained from the observations using 
NOMAD1 1182-0257977 (R=14.110) as the comparison:

Tmid(sec)+T0    Filter          Exp. time    Mag              Mag err. 
2442                  unfiltered      300            19.09CR     0.15
2759                  unfiltered      300            19.34CR     0.19
3076                  unfiltered      300            19.17CR     0.16
3717                  R                 300            19.58R        0.32
4034                  R                 300            19.93R        0.44
4351                  R                 300            19.93R        0.43


GRB_name: GRB130606B
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14892
SUBJECT: GRB 130606B: Suzaku WAM observation of the prompt emission
DATE:    13/06/13 11:04:12 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

Y. Ishida, M. Tashiro, Y. Terada, T. Yasuda, H. Ueno, S. Sugimoto
(Saitama U.), M. Ohno, K. Takaki, T. Kawano, R. Nakamura, S. Furui,
Y. Fukazawa (Hiroshima U.), M. Yamauchi, N. Ohmori, M. Akiyama
(Univ. of Miyazaki), K. Yamaoka (Nagoya U.),  S. Sugita (Ehime U.),
Y. E. Nakagawa, M. Kokubun, T. Takahashi (ISAS/JAXA), W. Iwakiri
(RIKEN), Y. Hanabata (ICRR), Y. Urata (NCU), K. Nakazawa,
K. Makishima (Univ. of Tokyo) on behalf of the Suzaku WAM team,
report:

The bright, long GRB 130606B (Fermi-LAT detection: G. Vianello, et al .
14795) triggered the Suzaku Wide-band  All-sky Monitor (WAM) which
covers an energy range of 50 keV - 5 MeV at  UT 11:55:35.360(=T0).

The observed light curve shows a multi-peaked structure starting at
T0-3.5 s, ending at T0+63 s with a duration (T90) of about 43.7 seconds.
The fluence in 100 - 1000 keV was 1.33 (-0.73, +0.02) *10^-4 erg/cm^2.
The 1-s peak flux measured from T0+11.5 s was
20.64 (-4.72, +0.51) photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-3 s to
T0+63 s is well fitted by a GRB Band model as follows.
the low-energy photon index alpha: -1.24 (-0.31, +0.79),
the high-energy photon index beta: -2.08 (-0.16, +0.11),
and the peak energy Epeak: 619 (-251, +396) keV,
(chi^2/d.o.f = 17.1/13).

Due to the brightness of this burst, a 3% systematic error was added for
low energy channels.
All the quoted errors are at statistical 90% confidence level.

The light curves for this burst are available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


GRB_name: GRB130603B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14893
SUBJECT: GRB 130603B: HST limits on an underlying supernova
DATE:    13/06/13 21:18:52 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir (U. Leicester), A. J. Levan (U. Warwick), A. S. Fruchter (STScI),
J. Hjorth (DARK/NBI) and K. Wiersema (U. Leicester) report:

We observed the location of GRB 130603B with HST/ACS and
WFC3/IR.  The host galaxy is clearly resolved as a disturbed spiral,
and it appears that the GRB occurred close to a spiral
arm that seems to have been tidally distorted or drawn out
by interaction with a smaller neighbour.

Our provisional analysis finds a point-source limit of F606W>27.6,
corresponding to M_V~-14.3, at the location of the GRB.  This is 
approaching a factor ~100 below what would be expected if there 
were a rising supernova comparable to SN1998bw, ruling out such an 
association for this burst.  It also rules out some part of the parameter
space of other radioactively-powered transients that have been
proposed may accompany short GRBs.

The position of the GRB lands on a region of extended emission in
the F160W (H') filter of WFC3/IR.    Another epoch scheduled for a
few weeks from now will allow a deeper search for a counterpart
through image subtraction.

We thank the STScI director and staff for rapidly expediting
these observations.


GRB_name: GRB130612A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14894
SUBJECT: GRB 130612A: iTelescope T21 optical observations
DATE:    13/06/14 02:27:46 GMT
FROM:    Veli-Pekka Hentunen at Taurus Hill Obs,A95  <veli-pekka.hentunen@kassiopeia.net>

Veli-Pekka Hentunen, Markku Nissinen and Tuomo Salmi (Taurus Hill
Observatory, Varkaus, Finland) report:

We have detected GRB 130612A optical afterglow at iTelescope observatory
T21 (Mayhill, New Mexico) 0.43m/6.8 astrograph and FLI-PL6303E 
CCD camera. One unfiltered image with 300 sec exposure time was made.

The afterglow was detected at following position RA 17:19:10.55
and DEC +16:43:11.9

The following magnitude was obtained from the observation using 
NOMAD1 1067-0303513 (R=16.900) as the comparison:

Tmid(sec)+T0    Filter          Exp. time    Mag              Mag err. 
1133                  unfiltered    300            19.19CR       0.39


GRB_name: GRB130603B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14895
SUBJECT: GRB 130603B: Detection of possible afterglow/kilonova in HST observations
DATE:    13/06/14 04:35:26 GMT
FROM:    Edo Berger at Harvard  <eberger@cfa.harvard.edu>

E. Berger and W. Fong (Harvard) report:

"We obtained the public Hubble Space Telescope ACS/F606W and WFC3/F160W
images of GRB 130603B (Tanvir et al. GCN #14893) from MAST and performed an
astrometric tie of these images relative to our afterglow images from
Magellan/IMACS (Foley et al. GCN #14745).  The resulting total rms of the
astrometic fit is 33 mas.  At the location of the optical afterglow we
identify an apparent point source in the WFC3/F160W image, with no
corresponding counterpart in the ACS/F606W image (the circles marking the
afterglow position have a radius of 10-sigma):

https://www.cfa.harvard.edu/~eberger/GRB130603B_HST.tif

PSF-matched photometry indicates m(F160W)=25.8+/-0.2 AB mag and
m(F606W)>27.5 mag (3-sigma; the limit is consistent with Tanvir et al. GCN
#14893).  At the redshift of GRB 130603B (z=0.356) these values correspond
to absolute magnitudes of M(F160W)=-15.2 mag and M(F606W)>-13.5 mag.

The red V-H>1.7 mag color is potentially in good agreement with the
afterglow g/r/i colors at early time (8.4 hr), which indicate a spectral
index of beta~-1.7 (Cucchiara et al. arXiv:1306.2028).  Based on this
spectral index and the g/r/i magnitudes from Cucchiara et al., the
interpolated/extrapolated magnitudes in the HST filters at 8.4 hr are
m(F160W)=20.0 mag and m(F606W)=21.9 mag, or V-H~1.9 mag.  Therefore, it is
possible that the source detected in WFC3/F160W is the fading afterglow,
indicating a decline rate of alpha_NIR~-1.6 between 8.4 hr and 9.4 days.
Incidentally, this decline rate is in good agreement with the Swift/XRT
decline rate of alpha_X~-1.6 at about 1 hr to 1 day (
http://www.swift.ac.uk/xrt_live_cat/00557310/)

Alternatively, the red V-H color and the absolute magnitude of
M(F160W)=-15.2 mag can be explained as emission from an r-process powered
"kilonova", along the recent models by Barnes & Kasen arXiv:1303.5787.  For
their fiducial model (with M_ej=0.01 Msun and v_ej=0.1c), the expected
absolute magnitude in the rest-frame J-band (corresponding to observed
H-band) at an observed time of 9.4 days is about -15 mag, while the
expected magnitude in the rest-frame B-band (corresponding to observed
V-band) is exceedingly low (about -3 mag).  Thus, it is possible that the
red source we detected in the WFC3/F160W image represents the first
detection of an r-process powered transient associated with a short GRB,
thereby strengthening their association with NS-NS/NS-BH mergers.

As noted by Tanvir et al. (GCN #14893) additional observations to determine
variability are essential."


GRB_name: GRB130612A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14896
SUBJECT: GRB 130612A: Fermi GBM observation
DATE:    13/06/14 18:06:06 GMT
FROM:    Gerard Fitzpatrick at UCD  <gerard.fitzpatrick@ucdconnect.ie>

G. Fitzpatrick (UCD) reports on behalf of the Fermi GBM Team:

At 03:22:23.36 UT on 12 June 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130612A (trigger 392700146/130612141)
which was also detected by the Swift/BAT (Racusin et al., GCN Circ. 14874).
The GBM on-ground location is consistent with the Swift position.

The GBM light curve consists of a single peak
with a duration (T90) of about 5.6 s (50-300 keV).
The time-averaged spectrum from T0-2.6 s to T0+2.3 s is
adequately fit by a power law function with an exponential
high-energy cutoff. The power law index is -1.3 +/- 0.3 and
the cutoff energy, parameterized as Epeak, is 61.9 +/- 10.5 keV.

The event fluence (10-1000 keV) in this time interval is
(5.7 +/- 0.6)E-07 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-1.8 s in the 10-1000 keV band is 4.1 +/- 0.2 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog.


GRB_name: GRB130615A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14897
SUBJECT: GRB 130615A: Swift detection of a burst
DATE:    13/06/15 10:00:09 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

E. Sonbas (NASA/GSFC/Adiyaman Univ.), S. D. Barthelmy (GSFC),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester),
D. M. Palmer (LANL) and B. Sbarufatti (INAF-OAB/PSU) report on behalf
of the Swift Team:

At 09:44:45 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130615A (trigger=558271).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 274.846, -68.166 which is 
   RA(J2000)  =  18h 19m 23s
   Dec(J2000) = -68d 09' 57"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As is typical for image triggers, there is nothing
obvious in the real-time TDRSS light curve. 

The XRT began observing the field at 09:47:39.3 UT, 174.1 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 274.82944, -68.16032 which
is equivalent to:
   RA(J2000)  = 18h 19m 19.07s
   Dec(J2000) = -68d 09' 37.2"
with an uncertainty of 3.8 arcseconds (radius, 90% containment). This
location is 30 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (8.27 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 3
(+2.62/-2.27) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 2.11e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
179 seconds after the BAT trigger. No credible afterglow candidate has been
found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the
XRT error circle. The typical 3-sigma upper limit has been about 19.2 mag. The
8'x8' region for the list of sources generated on-board covers 100% of the XRT
error circle. The list of sources is typically complete to about 18.0 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.12. 

Burst Advocate for this burst is E. Sonbas (edasonbas AT yahoo.com). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB130615A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14898
SUBJECT: GRB 130615A: GROND afterglow candidate
DATE:    13/06/15 12:44:37 GMT
FROM:    Sebastian Schmidl at TLS Tautenburg  <schmidl@tls-tautenburg.de>

J. Elliott (MPE Garching), S. Schmidl (TLS Tautenburg), J.Greiner
(MPE Garching), D. A. Kann (TLS Tautenburg), S. Ciceri and L. Mancini
(both MPIA) report on behalf of the GROND team:

We observed the field of GRB 130615A (Swift trigger 558271, Sonbas et al.,
GCN #14897) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La Silla
Observatory (Chile).

Observations started on June 15, 2013, at 10:17:21 UT, 0.54 hrs after the
GRB trigger. They were performed at an average seeing of 1".1 and at an
average airmass of 1.9.

We find a source inside the enhanced 2".1 SWIFT/XRT error circle
(http://www.swift.ac.uk/sper/558271/) at

RA (J2000) = 18:19:19.11

DEC (J2000) = -68:09:40.5

with an uncertainty of 0".5 in each coordinate.

Based on a total exposure time of 263 s in g'r'i'z' and 240 s in JHK, at a
midtime of 0.82 hrs after the burst, we measure the following preliminary
AB magnitudes:

g' = 21.3 +/- 0.1 mag,
r' = 20.7 +/- 0.1 mag,
i' = 20.6 +/- 0.1 mag,
z' = 20.5 +/- 0.1 mag,
J = 20.2 +/- 0.3 mag,
H = 19.8 +/- 0.3 mag and
K > 19.1 mag

Considering the galactic foreground extinction, the fit to the spectral
energy distribution indicates a redshift <~ 3.

Given magnitudes are calibrated against GROND zeropoints as well as
2MASS field stars and are not corrected for the expected Galactic
foreground extinction corresponding to a reddening of E_(B-V)=0.12 mag
in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB130615A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14899
SUBJECT: GRB 130615A: Swift-BAT refined analysis
DATE:    13/06/15 15:56:13 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), E. Sonbas (NASA/GSFC/Adiyaman Univ.), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 130615A (trigger #558271)
(Sonbas, et al., GCN Circ. 14897).  The BAT ground-calculated position is
RA, Dec = 274.963, -68.161 deg, which is 
   RA(J2000)  =  18h 19m 51.2s 
   Dec(J2000) = -68d 09' 39.7" 
with an uncertainty of 2.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 60%.
 
The mask-weighted light curve shows two peaks both of which are nearly smooth.
The first starts at ~T+10 sec and ends at ~T+150 se.  The second peak
goes from ~T+270 to T+450 sec.  T90 (15-350 keV) is 304 +- 30 sec
(estimated error including systematics).
 
The time-averaged spectrum from T+25.57 to T+386.86 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 0.87 +- 0.92, 
and Epeak of 33.2 +- 8.6 keV (chi squared 61.91 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 2.1 +- 0.3 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+31.84 sec in the 15-150 keV band is
0.7 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 2.18 +- 0.16 (chi squared 70.23 for 57 d.o.f.).  All the quoted errors
are at the 90% confidence level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/558271/BA/


GRB_name: GRB130615A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14900
SUBJECT: GRB 130615A: Enhanced Swift-XRT position
DATE:    13/06/15 16:33:43 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 1436 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 130615A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 274.82896, -68.16092 which is equivalent
to:

RA (J2000): 18h 19m 18.95s
Dec (J2000): -68d 09' 39.3"

with an uncertainty of 2.3 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB130615A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14901
SUBJECT: GRB 130615A: Skynet/PROMPT Observations
DATE:    13/06/15 17:58:55 GMT
FROM:    Nathan Frank at U.North Carolina  <nrfrank@live.unc.edu>

N. Frank, A. Trotter, J. Haislip, D. Reichart, A. LaCluyze, T. Berger, M. Carroll, H. T. Cromartie, R. Egger, A. Foster, C. Foster, K. Ivarsen, D. James, M. Maples, J. Moore, M. Nysewander, E. Speckhard, P. Taylor and J. A. Crain report

Skynet observed the Swift/XRT localization of the field of GRB 130615A (Sonbas et al., GCN 14897, Swift trigger #558271), starting at 2013-06-15, 09:46:37 UT (t=1.86m post-trigger), with four 16" telescopes of the PROMPT array at CTIO, Chile.  We detect an uncataloged optical source in B, V, R and I bands at: RA = 18:19:19.08, Dec = -68:09:41.02 (J2000), consistent with the GROND (Elliott et al., GCN 14898) and enhanced Swift/XRT positions (Evans et al., GCN 14900).

Calibrating to 6 APASS stars in the field we find an average magnitude of R~20.4 over the time period between t~8m and t~46m. The time range and sensitivity of these observations is not sufficient to determine if the source is fading with time. A preliminary light curve is at:
http://skynet.unc.edu/grb/grb130615a.png

Skynet observations are scheduled to determine if the source is indeed fading.


GRB_name: GRB130615A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14902
SUBJECT: GRB 130615A: Swift/UVOT Upper Limits
DATE:    13/06/15 19:21:11 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (MSSL-UCL) and E. Sonbas (NASA/GSFC/Adiyaman Univ.)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130615A
180 s after the BAT trigger (Sonbas et al., GCN Circ. 14897).
No optical afterglow consistent with the optical position
(Elliott et al. GCN Circ. 14898)
is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

u_FC               180          430          246         >20.1
v                  463         7314          580         >20.1
u                  180        12850         1827         >21.3
w1                 512        11936         1434         >20.9
m2                 488         7445          672         >20.3
w2                 439        13208          933         >20.8

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.12 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB130614A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14903
SUBJECT: GRB 130614A: Fermi GBM detection
DATE:    13/06/15 19:48:43 GMT
FROM:    Shaolin Xiong at UAH  <sx0002@uah.edu>

Shaolin Xiong (UAH) reports on behalf of the Fermi GBM Team:

"At 23:56:09.74 UT on 14 June 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130614A (trigger 392946972 / 130614997).

High peak flux from the GRB caused GBM to issue a repoint request
that reoriented the satellite to place the GRB near the LAT boresight
for 2.5 hours, subject to Earth limb contraints.

The on-ground calculated location, using the GBM trigger
data, is RA = 324.18, DEC = -33.89 (J2000 degrees,
equivalent to 21 h 36 m, -33 d 53 '), with an uncertainty
of 1.2 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).
The angle from the Fermi LAT boresight is 17 degrees.

The GBM light curve consists of a 'FRED' shape pulse
with a duration (T90) of about 9.3 s (50-300 keV).
The time-averaged spectrum from T0 s to T0+9.4 s is
well fit by a power law function with an exponential
high-energy cutoff. The power law index is -1.45 +/- 0.04 and
the cutoff energy, parameterized as Epeak, is 101 +/- 5 keV.

The event fluence (10-1000 keV) in this time interval is
(6.1 +/- 0.2)E-6 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+0.19 s in the 10-1000 keV band
is 20.7 +/- 0.4 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB130615A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14904
SUBJECT: GRB 130615A: Swift-XRT refined Analysis
DATE:    13/06/15 22:00:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. D'Avanzo (INAF-OAB), D.N. Burrows (PSU), J.A. Kennea (PSU), M.C.
Stroh (PSU), B.P. Gompertz (U. Leicester), J.P. Osborne (U. Leicester),
K.L. Page (U. Leicester), V. D'Elia (ASDC), A. Maselli  (INAF-IASFPA)
and E. Sonbas report on behalf of the Swift-XRT team:

We have analysed 10 ks of XRT data for GRB 130615A (Sonbas  et al. GCN
Circ. 14897),  from 180 s to 28.9 ks after the  BAT trigger. The data
comprise 459 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Evans et al. (GCN. Circ 14900).

The late-time light curve (from T0+5.3 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.5 (+/-0.3).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index  of 2.05 (+/-0.03). The
best-fitting absorption column is  1.93 (+/-0.09) x 10^21 cm^-2, in
excess of the Galactic value of 8.3 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.06 (+0.27, -0.09)
and a best-fitting absorption column consistent with the Galactic
value. The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.5 x 10^-11 (4.4 x 10^-11) erg
cm^-2 count^-1.

A summary of the PC-mode spectrum is thus:
Total column:        0 (+4.4, -0) x 10^20 cm^-2
Galactic foreground: 8.3 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:        2.06 (+0.27, -0.09)

If the light curve continues to decay with a power-law decay index of
0.5, the count rate at T+24 hours will be 4.9 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.7 x
10^-13 (2.2 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00558271.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB130615A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14905
SUBJECT: GRB 130615A: TAROT La Silla observatory optical observations
DATE:    13/06/15 22:01:29 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (IRAP-CNRS-OMP),
Boer M., Siellez K., Dereli H., Bardho O. (UNS-CNRS-OCA),
Atteia J.L. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 130615A detected by SWIFT
(trigger 558271) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 91.8s after the GRB trigger
(14.2s after the notice). The elevation of the field decreased from
36 degrees above horizon and weather conditions
were good.

The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
We do not detect the afterglow candidate mentioned by
Elliott et al. (GCNC 14898) with a limiting magnitude of:
t0+91.8s to t0+151.8s : Rlim = 16.4

The second image is 30.0s exposure in tracking mode,
the afterglow is not seen:
t0+165.4s to t0+195.4s : Rlim = 18.0

We co-added a series of exposures,
the afterglow is not seen:
t0+479s to t0+992s : Rlim = 19.3

Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.


GRB_name: GRB130615A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14906
SUBJECT: GRB 130615A: Zadko observatory - Gingin optical observations
DATE:    13/06/15 22:02:27 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

A. Klotz (IRAP-CNRS-OMP), D. Macpherson (UWA/ICRAR), D. Coward (UWA),
B. Gendre (IRAP-CNRS-OMP), M. Boer, K. Siellez, H. Dereli ,
O. Bardho (UNS-CNRS-OCA), A. Williams (PO-UWA), R. Martin (PO-UWA)
report:

We imaged the field of GRB 130615A detected by SWIFT
(trigger 558271) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 1.58h after the GRB trigger
just after the beginning of the night.
The elevation of the field increased from
30 degrees above horizon and weather conditions
were good.

We detect the afterglow candidate discovered
by Elliott et al. (GCNC 14898).

However, as mentioned by Frank et al. (GCNC 14901)
the stellar object stays at a constant magnitude
of R = 20.7 from 1.6h to 4.8h after the trigger.

Due to the absence of fading of its brightness,
we are not sure that the stellar object mentioned
by Elliott et al. (GCNC 14898) is the GRB afterglow.

Magnitudes were estimated with the nearby star
NOMAD-1 0218-0667138 (R.A.=274.8458361 Dec=-68.1621056
J2000) R=17.840. Magnitudes are not corrected for
galactic dust extinction.


GRB_name: GRB130610A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14907
SUBJECT: GRB 130610A: CrAO optical observations
DATE:    13/06/15 23:18:24 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

V. Rumyantsev (CrAO), A. Pozanenko (IKI) report on behalf of  larger GRB 
  follow-up collaboration:

We observed of  the field of  the Swift GRB 130610A (Cummings et al.,
GCN 14842) with Shajn telescope of CrAO starting on June, 10 (UT)
19:03:05. Several exposures of 120 s were obtained in R-filter. In the
combined image we clearly detected bright point-like source
superimposed on an extended object. Coordinates of the bright object
(J2000) 14 57 40.85 +28 12 25.5 (uncertainty of 0.2" in both
coordinates)  coincide with the afterglow coordinates (Cummings et al.,
GCN 14842; Melandri et al., GCN 14843). The extended object could be a
host galaxy with brightness of R ~ 23.8.

Preliminary photometry might be biasedby the extended object and  based 
  on the USNO B1.0 star 1182-0253576 14 57 45.41 +28 12 57.7 assuming 
R=18.98:


UT start,            T0+      Filter  Exposure, OT,             UL
                      mid,days          s
2013-06-10T19:03:05  0.6860   R       35*120    21.70 +/- 0.05  23.9


A finding chart can be found at
http://grb.rssi.ru/GRB130610A/GRB130610a_20130610_R_ZTSh.GIF


GRB_name: GRB130610A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14908
SUBJECT: GRB 130610A: TAROT La Silla observatory optical observations
DATE:    13/06/16 09:32:51 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

Klotz A. (IRAP-CNRS-OMP), Gendre B. (IRAP-CNRS-OMP),
Boer M., Siellez K., Dereli H., Bardho O. (UNS-CNRS-OCA),
Atteia J.L. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 130610A detected by SWIFT
(trigger 557845) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 91s after the GRB trigger
(17s after the notice). The elevation of the field
decreased from 31 degrees above horizon and weather conditions
were good.

The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
We recorded the rise of the afterglow discovered by
Melandri et al. (GCNC 14843).

We used the star NOMAD1 1182-0257977 R.A.=224.3892908
DEC=+28.2065917 R=14.11 to extract the light curve
of the rise of the afterglow:

start end     Rmag
(sec) (sec)
   91   97   > 17.8
   97  103   > 17.8
  103  109   > 17.8
  109  115   > 17.8
  115  121   > 17.8
  121  127     17.7
  127  133     16.9
  133  139     16.5
  139  145     16.6
  145  151     16.1

Magnitudes are not corrected for galactic dust extinction.

After the trailed image a technical problem prevented
to obtain next images.


GRB_name: GRB130615A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14909
SUBJECT: GRB 130615A: Continued Skynet/PROMPT Observations
DATE:    13/06/16 22:03:11 GMT
FROM:    Nathan Frank at U.North Carolina  <nrfrank@live.unc.edu>

N. Frank, A. Trotter, J. Haislip, D. Reichart, A. LaCluyze, T. Berger, M. Carroll, H. T. Cromartie, R. Egger, A. Foster, C. Foster, K. Ivarsen, D. James, M. Maples, J. Moore, M. Nysewander, E. Speckhard, P. Taylor and J. A. Crain report

Skynet continued observing the field of GRB 130615A (Sonbas et al., GCN 14897, Swift trigger #558271) with four 16" telescopes of the PROMPT array at CTIO, Chile, starting at 2013-06-16, 04:10 UT, and continuing until 10:11 UT (t=18.4h-24.4h post-trigger). In Frank et al. (GCN 14901) we reported detection of an uncatalogued optical source at the position reported by Elliott et al. (GCN 14898) and Evans et al. (GCN 14900).  We could not determine from our data whether the source was fading.

We took ~300 60s exposures in each of the B, V, R and I bands, with a mean time t~0.9d.  We do not detect the optical source in the B, R or I bands in stacks of all the exposures; there is a questionable (3-sigma) detection in the V-band stack. The 3-sigma limiting magnitudes of our stacked images are:
Filter       B       V       R       I
Mag       >21.83  >21.95  >22.09  >21.17

A light curve of both the first and second nights' data is at:
http://skynet.unc.edu/grb/grb130615a_2.png

Photometry is calibrated to 6 APASS stars in the field and magnitudes are in the Vega system. No correction has been applied for the expected line-of-sight Milky Way extinction of E(B-V)=0.12 (Schlegel et al. 1998). These observations are consistent with a fading afterglow with alpha <~ -0.4.

No further Skynet observations are scheduled.


GRB_name: GRB130603B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14913
SUBJECT: GRB 130603B: Analogy with GRB 090510A and possible connection with a supernova
DATE:    13/06/17 18:22:05 GMT
FROM:    Remo Rufinni at ICRA  <ruffini@icra.it>

R. Ruffini, C.L. Bianco, M. Enderli, M. Muccino, A.V. Penacchioni, G.B.
Pisani, J.A. Rueda, N. Sahakyan, Y. Wang report:

After a rest-frame time of 5000 sec from the BAT trigger (Melandri et
al., GCN 14735), the late X-ray rest-frame luminosity of GRB 130603B
overlaps the one of GRB 090510A (see the figure at:
<http://www.icra.it/temp/GCN/20130614.png>). This match occurs
irrespectively of their isotropic energies, which differ by a factor of
~50 (GRB 130603B: E_iso = 2.1 * 10^51 erg, Frederiks et al., GCN 14772;
GRB 090510A: E_iso = 1.1 * 10^53 erg, Muccino et al. 2013, ApJ, in
press, arXiv:1306.3467).

According to Muccino et al. 2013, GRB 090510A is a long GRB exploded in
a high density enviroment (10^3 particles/cm^3). The similarity shown
in the plot indicates that also GRB 130603B could be a long duration
GRB observed at closer distance (z~0.35). Therefore the detection (or
not detection) of a supernova associated to GRB 130603B between
20th-23rd of June, becomes a crucial test.

Observations are strongly encouraged.


GRB_name: GRB130612A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14914
SUBJECT: GRB 130612A: Continued Skynet/PROMPT/GORT/DSO observations
DATE:    13/06/17 23:14:09 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

M. Carroll, A. Trotter, J. Hailslip, D. Reichart, A. LaCluyze, K. McLin, 
L. Cominsky, A. Smith, D. Caton, L. Hawkins, T. Berger, H. T. Cromartie, 
R. Egger, A. Foster, C. Foster, N. Frank, K. Ivarsen, D. James, M. 
Maples, J. Moore, M. Nysewander, E. Speckhard, P. Taylor and J. A. Crain 
report

Skynet observed the Swift XRT localization of the field of GRB 130612A 
(Racusin et al., GCN 14874, Swift trigger #557976), beginning at 
2013-06-12, 3:23:27 UT (t=70s post-trigger), and continuing until t~5h, 
using three 16" telescopes of the PROMPT array at Cerro Tololo, Chile 
(BVI bands), the 14" GLAST Optical Robotic Telescope (GORT) at the Hume 
Observatory in California (RcIc bands), and the 14" telescope at the 
Appalachian State University Dark Sky Observatory (DSO-14) in Pisgah 
National Forest, North Carolina (RI bands). It took a total of ~500 
exposures ranging from 10s to 160s.

As we reported in Trotter et al. (GCN 14877), we detect a fading 
afterglow in the B, V and I bands out to t~1h at a position consistent 
with the detections of Racusin et al. (GCN 14874), Melandri, Mundell & 
Gomboc (GCN 14875), and Morgan (GCN 14876). In stacked images we obtain 
further detections in the V band at t=3.2h, and in the I band at t=1.5h 
and 1.9h.  The afterglow fades with an approximate temporal index 
alpha~-0.9.

A preliminary light curve is at:
http://skynet.unc.edu/grb/grb130612a_2.png

Magnitudes are in the Vega system, calibrated to 4 APASS stars in the 
field.  No correction has been applied for the expected line-of-sight 
Milky Way extinction E(B-V)=0.076 (Schlegel et al. 1998).

No further Skynet observations are scheduled.


GRB_name: GRB130609B
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14915
SUBJECT: GRB 130609B: Suzaku WAM observation of the prompt emission
DATE:    13/06/18 02:17:01 GMT
FROM:    Masanori Ohno at Hiroshima U  <ohno@hep01.hepl.hiroshima-u.ac.jp>

K. Takaki, M. Ohno, T. Kawano, R. Nakamura, S. Furui, Y. Fukazawa
(Hiroshima U.),
M. Tashiro, Y. Terada, T. Yasuda, Y. Ishida, H. Ueno, S. Sugimoto (Saitama
U.),
K. Yamaoka (Nagoya U.), M. Yamauchi, M. Akiyama, N. Ohmori (Univ. of
Miyazaki),
S. Sugita (Ehime U.), Y. E. Nakagawa, M. Kokubun, T. Takahashi (ISAS/JAXA),
W. Iwakiri(RIKEN), Y. Hanabata (ICRR), Y. Urata (NCU), K. Nakazawa,
K. Makishima (Univ. of Tokyo) on behalf of the Suzaku WAM team, report:

The long GRB 130609B (Krimm et al., GCN14841) triggered by the
Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of
50 keV - 5 MeV at 21:38:35 UT (=T0).

The observed light curve shows a multi-peaked structure starting at T0,
ending
at T0+30 s with a duration (T90) of about 19.6 seconds. The fluence in
100 - 1000 keV was 3.77 (+0.24/-0.70) x10^-5 erg/cm^2. The 1-s peak
flux measured
was 7.03 (+0.39/-2.80) photons/cm^2/s in the same  energy range.

Preliminary result shows that the time-averaged spectrum from
T0 to T0+30 s is well fitted by a power-law with exponential cutoff model:
 dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
 alpha      1.48 (+0.40/-0.41), and
 Epeak      845 (+179/-147) keV (chi^2/d.o.f. = 15.2/24).

Due to the brightness of this burst, a 5% systematic error was added
for low energy channels.

All the quoted errors are at statistical 90% confidence level.

The light curves for this burst will be available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


GRB_name: GRB130612A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14916
SUBJECT: GRB 130612A: Swift-BAT refined analysis
DATE:    13/06/19 22:01:54 GMT
FROM:    Craig Markwardt at NASA/GSFC  <craigm@milkyway.gsfc.nasa.gov>

C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC), T. Sakamoto (AGU),
on behalf of the Swift-BAT team:

Using the data set from T-25 to T+100 sec from the recent telemetry 
downlink, we report further analysis of BAT GRB 130612A (trigger 
#557976) (Racusin, et al., GCN Circ. 14874).  The BAT ground-calculated 
position is
RA, Dec = 259.771, 16.729 deg which is
    RA(J2000)  =  17h 19m 05.0s
    Dec(J2000) = +16d 43' 44.7"
with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 34%.

The mask weighted light curve shows a single FRED-like profile with a 
rise time of about 1 sec near T+0sec and a gradual decay time with 
e-folding time of about 3 sec.  This burst was detected as the Swift 
spacecraft was entering the South Atlantic Anomaly region, and the raw 
background counting rate was ramping upward.  The mask weighted light 
curve does not have a clean background level, so estimating the T90 is 
difficult.  If we restrict the analysis to the time range T-25 to T+100, 
we estimate T90 (15-350 keV) to be 4.0 +/- 1.4 sec.  However, we cannot 
rule out the possibility of a faint extended emission tail to 
approximately T+100 (in which case T90 is 110 +/- 60 sec).

The time-averaged spectrum from T-0.83 to T+3.17 sec is best fit by a 
power law with an exponential cutoff.  This fit gives a photon index 
-0.14 +- 1.71,  and Epeak of 36.4 +- 7.6 keV (chi squared 36 for 56 
d.o.f.).  For this model the total fluence in the 15-150 keV band is 2.3 
+- 0.5 x 10^-7 erg/cm2 and the 1-sec peak flux measured from T+0.17 sec 
in the 15-150 keV band is 1.7 +- 0.3 ph/cm2/sec.  A fit to a simple 
power law gives a photon index of 2.06 +- 0.25 (chi squared 44 for 57 
d.o.f.).  All the quoted errors are at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/557976/BA/


GRB_name: GRB130614A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14918
SUBJECT: GRB 130614A: Suzaku WAM observation of the prompt emission
DATE:    13/06/22 11:06:17 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

S. Sugimoto, M. Tashiro, Y. Terada, T. Yasuda, H. Ueno, Y. Ishida
(Saitama U.), M. Ohno, K. Takaki, T. Kawano, R. Nakamura, S. Furui,
Y. Fukazawa (Hiroshima U.), M. Yamauchi, N. Ohmori, M. Akiyama
(Univ. of Miyazaki), K. Yamaoka (Nagoya U.),  S. Sugita (Ehime U.),
Y. E. Nakagawa, M. Kokubun, T. Takahashi (ISAS/JAXA), W. Iwakiri
(RIKEN), Y. Hanabata (ICRR), Y. Urata (NCU), K. Nakazawa, K. Makishima
(Univ. of Tokyo) on behalf of the Suzaku WAM team, report:

The short GRB 130614A (Xiong, GCN 14903) was detected by the the Suzaku
Wide-band All-sky Monitor (WAM) which covers an energy range of
50 keV - 5 MeV at 23:56:9.064 UT (=T0).

The observed light curve shows a single FRED-like peak starting at
T0-1 s,ending at T0+9 s with a duration (T90) of about 4.9 seconds.
The fluence in 100 - 1000 keV was 3.08(+0.34/-0.31)*10^-6 erg/cm^2.
The 1-s peak flux measured from T0+1s was
2.41 (+0.35/-2.9) photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-1 s to
T0+9 s is well fitted by a single power-law with a photon index
of 2.42 (+0.28/-0.24) (chi^2/d.o.f = 17.6/17).

All the quoted errors are at statistical 90% confidence level,

The light curves for this burst are available at:

http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


GRB_name: GRB130623A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14921
SUBJECT: GRB 130623A detected in ground analysis of Swift-BAT data
DATE:    13/06/24 15:10:16 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings reports on behalf of the Swift-BAT team:

At 11:42:44.7 UTC, the time of Fermi-GBM trigger 393680570, Swift was executing a pre-
planned slew.  BAT photon detection event data was recorded during this slew.  In
ground analysis in a mosaic image, a significant source was found in found at RA, Dec
20.723, -77.784, which is:

RA (J2000)   01h 22m 53.5s
Dec (J2000) -77d 47m 04s

with an estimated 90% confidence radius of 4 arcmin.  The burst was a long GRB with 3
distinct peaks.  T90 was about 15 +/- 2 sec.

The spectrum from T0 to T0+15 sec is best fit by a simple powerlaw with a photon index
of 1.8 +/- 0.2.  The fluence from T0 to T+15 was (5.4 +/- 1.1) x 10^-0.7 ergs/cm^2.
The 1-second peak flux from T+0.6 sec was 1.4 +/- 0.3 photons/cm^2/sec.

A Swift TOO request has been approved.


GRB_name: GRB130603B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14922
SUBJECT: GRB 130603B: First epoch of XMM-Newton observations
DATE:    13/06/25 01:10:04 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

W. Fong, G. Migliori, R. Margutti, and E. Berger (Harvard) report:

"We observed the short-duration GRB 130603B (Melandri et al., GCN 14735)
with XMM-Newton + EPIC-pn starting on 2013 June 06.22 UT (2.57 d after the
burst) for a total of 24 ksec. We clearly detect the X-ray afterglow at the
position of the enhanced XRT error circle (Evans et al., GCN 14739) at a
significance level of about 6-sigma.

Taken together with the Swift/XRT afterglow light curve for t>4000 sec
(Kennea et al., GCN 14749), these observations indicate a single power-law
decline with index alpha_X=-1.83+/-0.15.  Therefore, the XMM observations
rule out the presence of a break at  t~4000 sec to 2.57 d, in contrast to
the suggested X-ray and optical break at ~8 hr (Tanvir et al., arXiv:
1306.4971)."


GRB_name: GRB130625A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14923
SUBJECT: GRB 130625A: Swift detection of a burst
DATE:    13/06/25 07:15:01 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <dxg35@psu.edu>

D. Grupe (PSU), V. D'Elia (ASDC), P. A. Evans (U Leicester),
A. Y. Lien (NASA/GSFC/ORAU) and K. L. Page (U Leicester) report on
behalf of the Swift Team:

At 07:00:39 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130625A (trigger=558982).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 343.268, +82.178 which is 
   RA(J2000) = 22h 53m 04s
   Dec(J2000) = +82d 10' 42"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peak
structure with a duration of about 30 sec.  The peak count rate
was ~1648 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 07:02:16.7 UT, 97.2 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 343.2798,
82.1734 which is equivalent to:
   RA(J2000)  = 22h 53m 07.15s
   Dec(J2000) = +82d 10' 24.1"
with an uncertainty of 2.6 arcseconds (radius, 90% containment). This
location is 17 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (1.06 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 2.8
(+2.84/-2.37) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 102 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.22. 

Burst Advocate for this burst is D. Grupe (dxg35 AT psu.edu). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB130625A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14924
SUBJECT: GRB 130625A: Enhanced Swift-XRT position
DATE:    13/06/25 11:44:13 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 1226 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 130625A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 343.27789, +82.17438 which is equivalent
to:

RA (J2000): 22h 53m 6.69s
Dec (J2000): +82d 10' 27.8"

with an uncertainty of 2.2 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB130625A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14925
SUBJECT: GRB 130625A: Swift-BAT refined analysis
DATE:    13/06/25 12:03:54 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), D. Grupe (PSU),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC),
T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC),
T. N. Ukwatta (MSU) (i.e. the Swift-BAT team):
 
Using the data set from T-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 130625A (trigger #558982)
(Grupe, et al., GCN Circ. 14923).  The BAT ground-calculated position is
RA, Dec = 343.336, 82.171 deg, which is 
   RA(J2000)  =  22h 53m 20.6s 
   Dec(J2000) = +82d 10' 17.1" 
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 75%.
 
The mask-weighted light curve shows two overlapping peaks starting at ~T-25sec,
peaking at ~T+3 sec, and ending at ~T+60 sec.  T90 (15-350 keV) is
38.1 +- 4.9 sec (estimated error including systematics).
 
The time-averaged spectrum from T-28.17 to T+18.50 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.37 +- 0.09.  The fluence in the 15-150 keV band is 1.8 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+2.54 sec in the 15-150 keV band
is 1.2 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/558982/BA/


GRB_name: GRB130623A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14926
SUBJECT: GRB 130623A: Swift-XRT and UVOT observations 
DATE:    13/06/25 14:35:13 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <dxg35@psu.edu>

Dirk Grupe (PSU), Phil Evans (Leicester), Jackie S. Linevsky (PSU/CBHS), 
and Mike Siegel (PSU)  report on behalf of the Swift team:

We have analyzed 5.0 ks of XRT data for the Swift/BAT-detected burst:
GRB 130623A (Cummings, GCN circ. 14921),  from 100.4 ks to 119.3 ks
after the  Swift/BAT trigger. The data are entirely in Photon Counting
(PC) mode.  An X-ray source is detected within the Swift/BAT error
circle. The refined XRT position is RA, Dec = 20.85346, -77.77338 which
is equivalent to:

RA (J2000): 01 23 24.83
Dec(J2000): -77 46 24.2

with an uncertainty of 4.5 arcsec (radius, 90% confidence). This
position is 106 arcsec from the Swift/BAT position. 
This source has a count rate in the XRT of (2.7+3.1-1.9)e-3 counts/s
which is equivalent of an X-ray flux of 1.4e-13 erg/s/cm2 assuming a 
standard X-ray afterglow spectrum.  We cannot
determine at the present time whether the source is fading.


The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020284.

Swift UVOT observed the field of GRB 130623A for 4611s. There is no 
source at the X-ray position in the white image. The 3sigma upper limit
is 22.6 mag in the Vega system. This magnitude is not corrected for 
the Galactic extinction due to the reddening of E(B-V) = 0.05 in the 
direction of the burst (Schlegel et al. 1998).



This circular is an official product of the Swift team.


GRB_name: GRB130625A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14927
SUBJECT: GRB 130625A: Nanshan optical upper limit
DATE:    13/06/25 18:36:32 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), A. Esamdin, L. Ma, C.-H. Bai, G.-J. Feng (XAO) report:

We observed the field of GRB 130625A (Grupe et al., GCN 14923) using
the 1m telescope located at Mt. Nanshan, Xinjiang Astronomical
Observatory, China. We obtained 6x300s R-band frames with a mean time
of 15:40:08 UT on 2013-06-25, (i.e., 8.658 hr after the burst).

No optical source is detected within the enhanced XRT error circle
(Goad et al., GCN 14924) in the stacked image, down to a limit
magnitude of R=21.0 mag, calibrated with the USNO B1 catalog.


GRB_name: GRB130625A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14928
SUBJECT: GRB 130625A: Swift/UVOT Upper Limits
DATE:    13/06/25 20:34:02 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

J. S. Linevsky (PSU/CBHS), M. H. Siegel (PSU), and
D. Grupe (PSU)  report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130625A
102 s after the BAT trigger (Grupe et al., GCN Circ. 14923).
No optical afterglow consistent with the enhanced XRT position
(Grupe et al. GCN Circ. 14924) is detected in the initial UVOT exposures.

Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

Filter  T_start(s)  T_stop(s)  Exp(s)  Mag 

white_FC    102      252       147    >20.96  
white       595     1890       283    >21.34 
v           644     1940       155    >19.34   
b           570     1866       136    >20.21  
u_FC        315      565       245    >20.26  
u           315     2003       617    >20.81 
uvw1        694     1989       136    >19.60     
uvm2        844     6816       332    >20.04  
uvw2        620     1916       155    >19.79   

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.22 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB130625A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14929
SUBJECT: GRB 130625A: MASTER afterglow limit
DATE:    13/06/26 06:31:35 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov, A.Gabovich
Blagoveschensk Educational State University, Blagoveschensk

  E. Gorbovskoy, V. Lipunov, D.Denisenko, V.Kornilov, 
D.Kuvshinov, N.Tyurina, N.Shatskiy, P.Balanutsa, D.Zimnukhov, A.Kuznetsov, 
V.V.Chazov
Sternberg Astronomical Institute, Lomonosov Moscow State University


K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk
Irkutsk State University, Irkutsk


A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Senik
Kislovodsk Solar Station of the Pulkovo Observatory

V.Krushinski, I.Zalozhnih,  A. Popov
Ural Federal University, Kourovka

Hugo Levato and Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

Claudio Mallamaci, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)



MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Blagoveschensk was pointed to the  GRB130625A 23177 sec s after 
notice time and 23214 sec after GRB time at 2013-06-25 13:27:34.231 UT. On 
our first (180s exposure) set we haven't found optical transient  within 
Swift error-box (D. Grupe et al. GCN 14923).
The 5-sigma upper limit has been about 17.5 mag

On coadd images  images we received the following limits


  T_start  T_finish  T_mid      t_mid-t_grb  Exptime   Filter   Limit  Coadd
---------------------------------------------------------------------------
13:27:34  14:17:44  13:52:39   24719 s      2700 s       R      19.0     15
13:31:38  14:17:44  13:54:41   24841 s      2520 s       W      19.5     14

The message may be cited.


GRB_name: GRB130625A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14930
SUBJECT: GRB 130625A: Swift-XRT refined Analysis
DATE:    13/06/26 07:15:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.A. Kennea (PSU), M.C. Stroh (PSU), D.N. Burrows (PSU), J.P. Osborne
(U. Leicester), K.L. Page (U. Leicester), C. Pagani (U. Leicester), V.
D'Elia (ASDC), A. Maselli  (INAF-IASFPA), V. Mangano (INAF-IASFPA) and
D. Grupe report on behalf of the Swift-XRT team:

We have analysed 2.8 ks of XRT data for GRB 130625A (Grupe  et al. GCN
Circ. 14923),  from 100 s to 25.1 ks after the BAT trigger. The data
comprise 34 s in Windowed Timing (WT) mode with the remainder in Photon
Counting (PC) mode. The enhanced XRT position for this burst was given
by Goad et al. (GCN. Circ 14924).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.70 (+0.21, -0.23).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.2 (+0.7, -0.6). The
best-fitting absorption column is  4.8 (+3.3, -2.3) x 10^21 cm^-2, in
excess of the Galactic value of 1.1 x 10^21 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.1 x 10^-11 (8.3 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.8 (+3.3, -2.3) x 10^21 cm^-2
Galactic foreground: 1.1 x 10^21 cm^-2
Excess significance: 2.6 sigma
Photon index:      2.2 (+0.7, -0.6)

If the light curve continues to decay with a power-law decay index of
1.70, the count rate at T+24 hours will be 5.3 x 10^-5 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.2 x
10^-15 (4.4 x 10^-15) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00558982.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB130626A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14931
SUBJECT: GRB 130626A: Swift detection of a short burst
DATE:    13/06/26 11:08:40 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

M. De Pasquale (UCL-MSSL), S. D. Barthelmy (GSFC),
D. N. Burrows (PSU), J. R. Cummings (NASA/UMBC), V. D'Elia (ASDC),
A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (NASA/GSFC),
F. E. Marshall (NASA/GSFC), S. R. Oates (UCL-MSSL) and
K. L. Page (U Leicester) report on behalf of the Swift Team:

At 10:51:03 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130626A (trigger=559075).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 273.130, -9.531 which is 
   RA(J2000)  =  18h 12m 31s
   Dec(J2000) = -09d 31' 50"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single spike
with a duration of about 0.2 sec.  The peak count rate
was ~5000 counts/sec (15-350 keV), at ~0.0 sec after the trigger. 

The XRT began observing the field at 10:52:02.1 UT, 58.6 seconds after
the BAT trigger, but centroided on a cosmic ray. Because of the short 
on-target time, we do not have enough data to identify an afterglow. 

UVOT took a finding chart exposure of  57 seconds with the White filter
starting 67 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers none of
the BAT error circle. The 8'x8' region for the list of sources
generated on-board covers 100% of the BAT error circle. No correction has
been made for the large, but uncertain extinction expected. 

Burst Advocate for this burst is M. De Pasquale (m.depasquale AT ucl.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB130627A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14933
SUBJECT: GRB 130627A: Swift detection of a burst
DATE:    13/06/27 09:07:45 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (UCL-MSSL), V. D'Elia (ASDC), P. A. Evans (U Leicester)
and A. Y. Lien (NASA/GSFC/ORAU) report on behalf of the Swift Team:

At 08:55:03 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130627A (trigger=559132).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 184.445, -37.086 which is 
   RA(J2000) = 12h 17m 47s
   Dec(J2000) = -37d 05' 09"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure with a duration of about 30 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~3 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+46.0
minutes. There will be no XRT or UVOT data until this time. 

Burst Advocate for this burst is S. R. Oates (samantha.oates AT ucl.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB130627A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14934
SUBJECT: GRB 130627A: Swift/UVOT Observation
DATE:    13/06/27 10:10:18 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates & M. De Pasquale (UCL-MSSL) report on behalf of the Swift/UVOT Team:

UVOT took a finding chart exposure of 150 seconds with the White filter of GRB 130627A (trigger= 559132)
starting 2979 seconds after the BAT trigger. No credible afterglow candidate
has been found in the initial data products. The 2.7'x2.7' sub-image covers 25%
of the BAT error circle. The typical 3-sigma upper limit has been about 19.6
mag. The 8'x8' region for the list of sources generated on-board covers 100% of
the BAT error circle. The list of sources is typically complete down to about 18
mag. No correction has been made for the expected extinction corresponding to
E(B-V) of 0.09. 


GRB_name: GRB130627A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14935
SUBJECT: GRB 130627A: Swift-XRT observations
DATE:    13/06/27 10:48:07 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.A. Kennea (PSU), G. Tagliaferri (INAF-OAB), S. Campana (INAF-OAB),
P.A. Evans (U. Leicester), J.P. Osborne (U. Leicester) and D.N. Burrows
(PSU) report on behalf of the Swift-XRT team:

The XRT began observing the field of GRB 130627A at 09:44:39.3 UT,
2975.9 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source located at RA, Dec 184.41689,
-37.08615 which is equivalent to:
   RA(J2000)  = 12h 17m 40.05s
   Dec(J2000) = -37d 05' 10.1"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 80 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (7.95 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 3.9
(+2.51/-2.13) x 10^21 cm^-2 (90% confidence). 


GRB_name: GRB130627B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14936
SUBJECT: GRB 130627B: Swift detection of a burst
DATE:    13/06/27 12:12:55 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

S. R. Oates (UCL-MSSL), S. D. Barthelmy (GSFC), D. N. Burrows (PSU),
V. D'Elia (ASDC), P. A. Evans (U Leicester), S. T. Holland (STScI),
A. Y. Lien (NASA/GSFC/ORAU), D. Malesani (DARK/NBI),
K. L. Page (U Leicester), D. M. Palmer (LANL) and M. H. Siegel (PSU)
report on behalf of the Swift Team:

At 12:00:50 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130627B (trigger=559139).  Due to an Earth limb constraint
Swift could not immediately slew to the burst. 
The BAT on-board calculated location is 
RA, Dec 181.932, -55.730 which is 
   RA(J2000) = 12h 07m 44s
   Dec(J2000) = -55d 43' 47"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 40 sec.  The peak count rate
was ~1300 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+48.4
minutes. There will be no XRT or UVOT data until this time. 

Burst Advocate for this burst is S. R. Oates (samantha.oates AT ucl.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB130626A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14937
SUBJECT: GRB 130626A: Swift-XRT possible detection and UVOT upper limits
DATE:    13/06/27 13:31:45 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page (U. Leicester), S.R. Oates (UCL-MSSL) and M. De Pasquale
(UCL-MSSL) report on behalf of the Swift-XRT and UVOT teams:

We have analysed 9.5 ks of Swift-XRT Photon Counting mode data collected
for GRB 130626A, starting 111 s after the trigger (De Pasquale et al., GCN
Circ. 14931). Of these data, only 10s were collected promptly following
the trigger before Swift had to slew away because of a pointing
constraint.

Within the onboard BAT error circle, there is a possible source detected,
with a count rate (averaged between 111 s and 34.7 ks after the trigger)
of (2.0 +0.5/-0.4) x 10^-3 count s^-1. The position of this source is RA,
Dec = 273.14043, -9.50093, which is equivalent to:

RA (J2000):   18h 12m 33.70s
Dec (J2000): -09d 30' 03.3"

with an uncertainty of 5.5 arcsec (radius, 90% confidence). It is not
possible to determine whether this candidate source is fading at present;
a follow-up observation will be performed at a later date.

We do note, however, that there are other possible sources detected at a
similar level in the XRT field of view, although outside the BAT error
circle.

The Swift-UVOT began settled observations of the field of GRB 130626A
67 s after the BAT trigger (De Pasquale et al., GCN Circ. 14931).
In the initial UVOT exposures, no optical afterglow is found within
the BAT error circle or consistent with the candidate XRT position.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial
exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white (FC)          67          124          57          >20.5
white               67         5608          597         >22.0
v                 4384         5892          269         >19.8
b                 3768         5403          393         >21.1
u                 3563         5198          393         >20.7
w1                4794         4993          197         >20.1

The magnitudes in the table are not corrected for the heavy, but
uncertain, Galactic extinction due to the reddening of E(B-V) = 1.45 in
the direction of the burst (Schlegel et al. 1998).

This circular is an official product of the Swift-XRT and UVOT teams.


GRB_name: GRB130627B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14938
SUBJECT: GRB 130627B: Swift-XRT observations
DATE:    13/06/27 13:53:24 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

S. Campana (INAF-OAB), G. Cusumano (INAF-IASF PA), P.A. Evans (U.
Leicester), J.P. Osborne (U. Leicester), D.N. Burrows (PSU) and J.A.
Kennea (PSU) report on behalf of the Swift-XRT team:

The XRT began observing the field of GRB 130627B at 12:50:47.2 UT,
2996.6 seconds after the BAT trigger. No source was detected in 1.8 ks
of promptly downlinked data, which covered 96% of the BAT error circle.
We are waiting for the full dataset to detect and localise the XRT
counterpart.


GRB_name: GRB130627B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14939
SUBJECT: GRB130627B: Swift/UVOT Observations
DATE:    13/06/27 13:53:30 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates & M. De Pasquale (UCL-MSSL) report on behalf of the Swift/UVOT Team:

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 3754 seconds after the BAT trigger. No credible afterglow candidate
has been found in the initial data products. The 2.7'x2.7' sub-image covers 25%
of the BAT error circle. The typical 3-sigma upper limit has been about 19.6
mag. The 8'x8' region for the list of sources generated on-board covers 100% of
the BAT error circle. The list of sources is typically complete down to about 18
mag. No correction has been made for the expected extinction corresponding to
E(B-V) of 0.40. 


GRB_name: GRB130623A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14940
SUBJECT: GRB 130623A: Fermi GBM detection
DATE:    13/06/27 17:07:07 GMT
FROM:    David Byrne at UCD  <david.byrne.2@ucdconnect.ie>

D. Byrne (UCD), A. von Kienlin (MPE) and W. Paciesas (UAH) report on the
behalf of the Fermi GBM Team:

"At 11:42:47.05 UT on 23 June 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130623A (trigger 393680570 / 130623488),
which was also detected by the Swift/BAT (J. R. Cummings 2013, GCN 14921).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 46 degrees.

The GBM light curve consists of four peaks within 30s of the trigger
time with a duration (T90) of about 21 s (50-300 keV).

The time-averaged spectrum from T0-6.144s to T0+24.576s is well fit by
a power law function with an exponential high-energy cutoff.
The power law index is -1.03 +/- 0.53 and the cutoff energy,
parameterized as Epeak, is 26.11 +/- 4.67 keV.

The event fluence (10-1000 keV) in this time interval is
(2.63 +/- 0.20)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+13.568 s in the 10-1000 keV band is 5.07 +/- 0.25 ph/s/cm^2.


The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."



-- 
David Byrne BSc.
School of Physics,
Science Center North,
University College Dublin,
Belfield, Dublin 4,
Ireland.


GRB_name: GRB130627A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14941
SUBJECT: GRB 130627A: Fermi GBM detection
DATE:    13/06/27 17:08:02 GMT
FROM:    David Byrne at UCD  <david.byrne.2@ucdconnect.ie>

D.Byrne (UCD) reports on behalf of the Fermi GBM Team:

"At 08:55:05.93 UT on 27 June 2013, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 130627A (trigger 394016108 / 130627372),
which was also detected by the Swift/BAT (Oates et al. 2013, GCN 14933).
The GBM on-ground location is consistent with the Swift position.

The GBM light curve shows/consists of a multiple pulses,
with a duration (T90) of about 28 s (50-300 keV).
The time-averaged spectrum from T0-13.31 s to T0+14.34 s is
adequately fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.4 +/- 0.2 and
the cutoff energy, parameterized as Epeak, is 86 +/- 25 keV.

The event fluence (10-1000 keV) in this time interval is
(1.334 +/- 0.185)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0-1.28 s in the 10-1000 keV band
is 2.17 +/- 0.25 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB130626A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14942
SUBJECT: GRB 130626A, Swift-BAT refined analysis
DATE:    13/06/27 20:18:56 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

T. Sakamoto (AGU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), M. De Pasquale (UCL-MSSL), E. E. Fenimore (LANL),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):

Using the data set from T-119 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 130626A (trigger #559075)
(De Pasquale, et al., GCN Circ. 14931).  The BAT ground-calculated position is
RA, Dec = 273.128, -9.525 deg which is
   RA(J2000)  =  18h 12m 30.6s
   Dec(J2000) = -09d 31' 29.9"
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The mask-weighted light curve shows a double short-peaked structure at T~ 0 sec.
The second peak is slightly weaker than the first peak, and starts immediately
at the end of the first peak. Each peak lasts ~ 0.08 sec.
T90 (15-350 keV) is 0.16 +- 0.03 sec (estimated error including systematics).

The time-averaged spectrum from T-0.0 to T+0.2 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index -0.53 +- 1.39,
and Epeak of 74.5 +- 25.6 keV (chi squared 54.40 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 5.2 +- 0.8 x 10^-08 erg/cm2
and the 1-sec peak flux measured from T-0.41 sec in the 15-150 keV band is
0.9 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.30 +- 0.21 (chi squared 62.40 for 57 d.o.f.).  All the quoted errors
are at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/559075/BA/


GRB_name: GRB130626A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14943
SUBJECT: GRB 130626A: RATIR Optical Observations
DATE:    13/06/27 21:36:50 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB)
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UCSC),
Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC),
Jos A. de Diego (UNAM), Leonid Georgiev (UNAM), Jess Gonzlez (UNAM),
Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC), and Harvey Moseley (GSFC)
report:

We observed the field of the short-duration GRB 130626A (De Pasquale, et
al., GCN 14931) with the Reionization and Transients Infrared Camera
(RATIR; www.ratir.org) on the 1.5m Harold Johnson Telescope at the
Observatorio Astronmico Nacional on Sierra San Pedro Mrtir beginning 200
seconds after the BAT trigger, obtaining simultaneous 80 second exposures
in the r' and i' bands.

We note that there is DSS source at the center of the corrected candidate
Swift-XRT error circle (Page, et al., GCN 14937).  In comparison with 2MASS
and the RATIR zero points, we measure for this source:

  r'    18.69 +/- 0.07
  i'    17.40 +/- 0.05

No uncatalogued sources are detected within the XRT error circle.   We
derive the following 3-sigma limits:

  r' > 20.8
  i' > 20.5

These magnitudes are in the AB system and not corrected for Galactic
extinction in the direction of the GRB.

We thank the staff of the Observatorio Astronmico Nacional in San
Pedro Mrtir.


GRB_name: GRB130626A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14944
SUBJECT: GRB 130626A: KAIT Optical Observations
DATE:    13/06/28 05:02:18 GMT
FROM:    Weikang Zheng at U.of Michigan  <zwk@umich.edu>

WeiKang Zheng, Alexei V. Filippenko, Adam Morgan (UC Berkeley), and
S. B. Cenko (NASA/Goddard Space Flight Center) report on behalf of the
KAIT GRB team:

The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, responded to the short-duration GRB 130626A
(De Pasquale et al., GCN 14931) starting at 10:52:40 UT, 97 s after
the burst. Observations were performed with an automatic sequence
in V, I, and clear filters (20 s exposure for each image). We detect
the DSS source mentioned by Butler et al. (GCN 14943) in the
corrected candidate XRT circle (Page et al., GCN 14937). We do not
detect any new source in the XRT error circle. The estimated limiting
magnitude in our first clear-band (close to R) image is about 18.7
(calibrated to USNO B1.0) at a midtime of 174 s after the burst.


GRB_name: GRB130627A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14945
SUBJECT: GRB 130627A: Enhanced Swift-XRT position
DATE:    13/06/28 05:51:02 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 4487 s of XRT Photon Counting mode data and 11 UVOT
images for GRB 130627A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 184.41524, -37.08699 which is equivalent
to:

RA (J2000): 12h 17m 39.66s
Dec (J2000): -37d 05' 13.2"

with an uncertainty of 1.6 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB130627B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14947
SUBJECT: GRB 130627B: Possible Swift-XRT afterglow detection
DATE:    13/06/28 08:03:34 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans (U. Leicester) & S.R. Oates (MSSL-UCL) report on behalf of
the Swift-XRT team:

In 3.3 ks of XRT data for GRB 130627B (Oates  et al. GCN Circ. 14936),
from 3.7 ks to 11.2 ks after the  BAT trigger we find an uncatalogued
X-ray sources at  RA, Dec = 181.91308, -55.7008 which is equivalent to:

RA (J2000): 12 07 39.14
Dec(J2000): -55 42 02.9

with an uncertainty of 4.2 arcsec (radius, 90% confidence). The mean
count rate in this interval is 8.8(+/-2.0) x 10^-3 ct/sec, and we cannot
determine at the present time whether the source is fading.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB130627A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14948
SUBJECT: GRB 130627A: Swift-XRT refined Analysis
DATE:    13/06/28 13:34:18 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

A. Amaral-Rogers (UoL) and S. R. Oates (UCL-MSSL) report on behalf of
the Swift-XRT team:

We have analysed 5.9 ks of XRT data for GRB 130627A (Oates  et al. GCN
Circ. 14933),  from 3.0 ks to 28.5 ks after the  BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Osborne et al. (GCN. Circ 14945).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.87 (+0.18, -0.16).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.4 (+/-0.3). The
best-fitting absorption column is  4.2 (+1.2, -1.1) x 10^21 cm^-2, in
excess of the Galactic value of 8.0 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.5 x 10^-11 (8.4 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.2 (+1.2, -1.1) x 10^21 cm^-2
Galactic foreground: 8.0 x 10^20 cm^-2
Excess significance: 5.3 sigma
Photon index:      2.4 (+/-0.3)

If the light curve continues to decay with a power-law decay index of
0.87, the count rate at T+24 hours will be 6.4 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.3 x
10^-13 (5.4 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00559132.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB130627A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  14949
SUBJECT: GRB 130627A: Swift/UVOT Upper Limits
DATE:    13/06/28 21:31:12 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin and S. R. Oates (UCL-MSSL) report on behalf of the
Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130627A
2979 s after the BAT trigger (Oates et al., GCN Circ. 14933, GCN Circ
14934).

No optical afterglow consistent with the (enhanced) XRT
position (Kennea et al. GCN Circ. 14935; Osborne et al. GCN Circ.
14945) is detected in the initial UVOT exposures.

Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white_FC          2979         3129          147         >20.5
white             2979        10701         1229         >22.1
v                 3136         4772          393         >19.7
b                 3956         9788         1125         >21.3
u                 3751         5386          393         >20.5
w1                3546         5182          393         >20.4
m2                3341         4976          393         >20.4
w2                4367        11202          684         >21.2

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.09 in the direction of the burst
(Schlegel et al. 1998).


