# GCN_circulars

GRB_name: GRB160504A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19390
SUBJECT: GRB 160504A: Swift/UVOT Upper Limits
DATE:    16/05/05 18:34:55 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU) and D. Malesani (DARK/NBI)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 160504A
99 s after the BAT trigger (Malesani et al., GCN Circ. 19382).
No optical afterglow consistent with the XRT position
(Goad et al. GCN Circ. 19386)
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)             99          249          147         >20.8
white               99        11822         1316         >21.7
v                  587        16542         1317         >20.2
b                  513        10910         1145         >21.5
u (fc)                257          507          246         >20.4
u                  257         6616          678         >21.2
w1                 636         6411          432         >20.4
m2                4571        17443         1275         >21.0
w2                 735        12387          963         >21.7

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: GRB160504A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19391
SUBJECT: GRB 160504A: RATIR Optical and NIR Observations
DATE:    16/05/05 19:17:33 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), Ori Fox (STScI), J. Xavier
Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (GSFC/STScI),
Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC),
JosÃ© A. de Diego (UNAM), Leonid Georgiev (UNAM), JesÃºs GonzÃ¡lez (UNAM),
Carlos RomÃ¡n-ZÃºÃ±iga (UNAM), Neil Gehrels (GSFC), Harvey Moseley (GSFC),
John Capone (UMD), V. Zach Golkhou (ASU), and Vicki Toy (UMD) report:

We observed the field of GRB 160504A (Malesani, et al., GCN 19382) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio AstronÃ³mico Nacional on
Sierra San Pedro MÃ¡rtir from 2016/05 5.21 to 2016/05 5.36 UTC (19.64 to
23.11 hours after the BAT trigger), obtaining a total of 2.49 hours
exposure in the r and i bands and 1.04 hours exposure in the Z, Y, J, and H
bands.

For a source within the Swift-XRT error circle (Goad, et al., GCN 19386),
in comparison with the SDSS DR9 and 2MASS catalogs, we obtain the following
detection and upper limits (3-sigma):

 r > 23.70
 i = 23.62 +/- 0.36
 Z > 22.38
 Y > 22.08
 J > 21.73
 H > 21.35

These magnitudes, which appear to be consistent with those reported by
Cenko et al., (GCN 19389), are in the AB system and are not corrected for
Galactic extinction in the direction of the GRB.

We thank the staff of the Observatorio AstronÃ³mico Nacional in San Pedro
MÃ¡rtir.


GRB_name: GRB160504A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19393
SUBJECT: GRB 160504A: Swift-BAT refined analysis
DATE:    16/05/06 03:20:07 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (GSFC/UMBC),
D. Malesani (DARK/NBI), C. B. Markwardt (GSFC), T. Sakamoto (AGU),
M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team):

Using the data set from T-240 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 160504A (trigger #685124)
(Malesani, et al., GCN Circ. 19382).  The BAT ground-calculated position is
RA, Dec = 170.073, 56.002 deg which is
RA(J2000) = 11h 20m 17.5s
Dec(J2000) = +56d 00' 05.7"
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 88%.

The mask-weighted light curve shows that the main emission starts at T-40 sec, 
has a very broad profile, peaks near T+0 sec and ends by T+30 sec. T90 (15-350 
keV) is 53.9 +- 6.0 sec (estimated error including systematics). We have 
concluded that a soft spike in the light curve of ~10 msec duration at T-135.5 
sec is of instrumental and not astrophysical origin.  Our analysis therefore 
excludes the time before T-135 sec.

The time-averaged spectrum from T-42.3 to T+16.2 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.88 +- 0.20. The fluence in the 15-150 keV band is 7.3 +- 0.9 x 10^-7erg/cm2.
The 1-sec peak photon flux measured from T+0.51 sec in the 15-150 keV band
is 0.7 +- 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/685124/BA/


GRB_name: GRB160506A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19394
SUBJECT: GRB 160506A: Swift detection of a burst
DATE:    16/05/06 03:50:19 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

L. M. Z. Hagen (PSU), S. D. Barthelmy (GSFC),
H. A. Krimm (CRESST/GSFC/USRA), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL) and M. H. Siegel (PSU) report on behalf of the
Swift Team:

At 03:29:15 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 160506A (trigger=685245).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 265.774, -46.117 which is 
   RA(J2000)  =  17h 43m 06s
   Dec(J2000) = -46d 07' 00"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows broad peak
with a total duration of about 50 sec.  The peak count rate
was ~1200 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 03:30:50.6 UT, 94.8 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
265.8484, -46.1340 which is equivalent to:
   RA(J2000)  = 17h 43m 23.60s
   Dec(J2000) = -46d 08' 02.3"
with an uncertainty of 2.0 arcseconds (radius, 90% containment). This
location is 195 arcseconds from the BAT onboard position, outside 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 (2.67 x
10^21 cm^-2, Willingale et al. 2013), with an excess column of 4.8
(+2.85/-2.47) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 2.68e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
101 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 upper limit has been 19.6 mag. The
8'x8' region for the list of sources generated on-board covers 100% of the XRT
error circle. The typical upper limit has been 18.0 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.26. 

Burst Advocate for this burst is L. M. Z. Hagen (lea.zernow.hagen 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: GRB160506A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19395
SUBJECT: GRB 160506A: Enhanced Swift-XRT position
DATE:    16/05/06 07:28:32 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 1815 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 160506A, 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 = 265.84841, -46.13410 which is equivalent
to:

RA (J2000): 17h 43m 23.62s
Dec (J2000): -46d 08' 02.8"

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: GRB160506A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19396
SUBJECT: GRB 160506A: GROND upper limits
DATE:    16/05/06 09:12:52 GMT
FROM:    Fabian Knust at MPE/GROND  <fknust@mpe.mpg.de>

F. Knust, C. Delvaux, J. Greiner (all MPE Garching) report on behalf of
the GROND team:

We observed the field of GRB 160506A (Swift trigger 685245; Hagen et al.,
GCN #19394) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La Silla
Observatory (Chile).

Observations started at  06:45 UT on 2016-05-06, 3.25 hrs after the GRB
trigger. They were performed through substantial cirrus at an average
seeing of 2.1" and at an average airmass of 1.1.

We do not detect any source within the Swift-XRT error circle reported by
Osborne et al. (GCN #19395) down to

g' > 20.9 mag,
r' > 22.1 mag,
i' > 21.5 mag,
z' > 21.7 mag,
J > 19.4 mag,
H > 19.1 mag, and
K > 17.2 mag.
(all in AB),

but we see two faint sources north-east and sout-west of the XRT error
circle, each about 4 arcsec away from the XRT centroid.

Given magnitudes are calibrated against USNO as well as 2MASS field stars
and are not corrected for the expected Galactic foreground extinction
corresponding to a reddening of E_(B-V)=0.26 mag in the direction of the
burst (Schlegel et al. 1998).


GRB_name: GRB160506A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19397
SUBJECT: GRB 160506A: Swift-BAT refined analysis
DATE:    16/05/06 14:29:56 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

T. Sakamoto (AGU), S. D. Barthelmy (GSFC),  J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), L. M. Z. Hagen (PSU), H. A. Krimm (GSFC/USRA),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
M. Stamatikos (OSU), T. N. Ukwatta (LANL) (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 160506A (trigger #685245)
(Hagen, et al., GCN Circ. 19394).  The BAT ground-calculated position is
RA, Dec = 265.857, -46.127 deg which is
    RA(J2000)  =  17h 43m 25.6s
    Dec(J2000) = -46d 07' 36.1"
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The mask-weighted light curve shows a long and complex structure.  The emission 
starts at T-10 sec, and continues with multiple peaks out to about T+275 sec.
The highest count rate is at T+100 sec.  The peaks after the slew ended at 
T+94.8 sec are also seen as flares in the XRT.  T90 (15-350 keV) is 254.5 +- 
24.9 sec (estimated error including systematics).

The time-averaged spectrum from T-8.33 to T+267.03 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.09 +- 0.21.  The fluence in the 15-150 keV band is 1.5 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+98.80 sec in the 15-150 keV band
is 0.4 +- 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/685245/BA/


GRB_name: GRB160506A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19398
SUBJECT: GRB 160506A: Swift/UVOT Upper Limits
DATE:    16/05/06 15:13:11 GMT
FROM:    Lea Hagen at PSU  <lea.zernow.hagen@gmail.com>

L. M. Z. Hagen (PSU) reports on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 160506A
102 s after the BAT trigger (Hagen et al., GCN Circ. 19394). No optical
afterglow consistent with the XRT position (Osborne et al. GCN Circ.
19395) 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

v                  407         2279          233        >19.36
b                  357         2229          252        >20.37
u_FC               101          351          245        >20.13
u                  101         2353          626        >20.58
uvw1               457         2329          233        >19.75
uvm2               432         2304          233        >19.52
uvw2               383         2255          252        >19.86


The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.26 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB160506A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19399
SUBJECT: GRB 160506A: Swift-XRT refined Analysis
DATE:    16/05/06 16:50:41 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.A. Kennea (PSU), P.A. Evans (U. Leicester), S.L. Gibson (U.
Leicester), J.P. Osborne (U. Leicester), A. D'Ai (INAF-IASFPA), A.
Maselli  (INAF-IASFPA), A. Melandri (INAF-OAB), B. Sbarufatti
(INAF-OAB/PSU), D.N. Burrows (PSU) and L.M.Z. Hagen report on behalf of
the Swift-XRT team:

We have analysed 7.4 ks of XRT data for GRB 160506A (Hagen et al. GCN
Circ. 19394), from 86 s to 36.2 ks after the  BAT trigger. The data
comprise 422 s in Windowed Timing (WT) mode (the first 7 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. 19395).

The late-time light curve (from T0+5.6 ks) can be modelled with a
power-law decay with a decay index of alpha=0.54 (+0.22, -0.21).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.65 (+/-0.05). The
best-fitting absorption column is  7.1 (+/-0.5) x 10^21 cm^-2, in
excess of the Galactic value of 2.7 x 10^21 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.11 (+0.21, -0.20)
and a best-fitting absorption column of 7.9 (+1.7, -1.5) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 4.3 x 10^-11 (8.2 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      7.9 (+1.7, -1.5) x 10^21 cm^-2
Galactic foreground: 2.7 x 10^21 cm^-2
Excess significance: 5.9 sigma
Photon index:      2.11 (+0.21, -0.20)

If the light curve continues to decay with a power-law decay index of
0.54, 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 5.4 x
10^-13 (1.0 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/00685245.

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


GRB_name: GRB160506A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19400
SUBJECT: GRB 160506A: IRSF upper limits
DATE:    16/05/07 01:59:55 GMT
FROM:    Katsuhiro L. Murata at Nagoya U  <murata@u.phys.nagoya-u.ac.jp>

K. L. Murata (Nagoya U.), Y.-H. Lee, B.-C. Koo (Seoul National U.), and T.
Nagayama (Kagoshima U.)

We observed the field of GRB 160506A ( Hagen et al., GCN Circular #19394)
with the near-infrared (J, H, Ks) simultaneous imaging camera SIRIUS
attached to 1.4 m telescope IRSF ( InfraRed Survey Facility) in Sutherland
observatory, South Africa. We observed with a narrow band filter with
double transmissions at 1.189 um and 1.644 um.

The observations started on 2016-05-06 04:18:47 UT (~ 49 min. after the
burst). We could not detect the afterglow within the XRT error circle
reported in the GCN circular. We have obtained the following preliminary
upper limits (Vega magnitude system):
 M_1.189um > 17.3 mag
 M_1.644um > 16.6 mag

Given magnitudes of M_1.189um and M_1.644um were calibrated against J band
and H band of 2MASS point sources in this field, respectively. The upper
limits were determined as the magnitudes of the faintest star within 1
arcmin from the XRT position.

This observation was carried out by IRSF and OISTER collaboration.


GRB_name: GRB160506A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19402
SUBJECT: GRB 160506A: TAROT La Silla observatory optical observations
DATE:    16/05/08 19:46:54 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

Klotz A., Turpin D., Atteia J.L. (CNRS-OMP-IRAP),
Boer, M., Laugier, R. (CNRS-ARTEMIS),
Gendre B. (UVI - Etelman Obs.) report:

We imaged the field of GRB 160506A detected by SWIFT
(trigger 685245) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 62.1s after the GRB trigger
(14.0s after the notice). The elevation of the field increased from
41 degrees above horizon but clouds were presents in the sky.

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 any OT with a limiting magnitude of:
t0+62.1s to t0+122.1s : Rlim = 12.7

Then the observations were stopped due to the bad weather
and start again 39 minutes later. We co-added a series
of exposures:
t0+2366s to t0+3314s : Rlim = 16.7

Magnitudes were estimated with the nearby NOMAD1 stars
and are not corrected for galactic dust extinction.


GRB_name: GRB160509A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19403
SUBJECT: GRB 160509A: Fermi-LAT prompt detection of a very bright burst
DATE:    16/05/09 09:42:59 GMT
FROM:    Elisabetta Bissaldi at U.Innsbruk/IAPP  <Elisabetta.Bissaldi@uibk.ac.at>

F.Longo (University and INFN, Trieste), E.Bissaldi (Politecnico and INFN, Bari),
J. Bregeon (CNRS/IN2P3/LUPM), J. McEnery (NASA/GSFC), M. Ohno (Hiroshima U),
S. Zhu (AEI Potsdam-Golm/AEI Hannover) report on behalf of the Fermi-LAT team:


At 08:59:04.36 UTC on May 09, 2016, Fermi-LAT triggered on
high-energy emission from GRB 160509A,
also detected by GBM (trigger 484477130/160509374).

The onboard location is

RA, Dec 310.1, 76.0 (J2000)

with an estimated error radius of 0.50 deg
(90% containment, systematic error only).
This was 31.8 deg from the LAT boresight at the time of the trigger.

We anticipate providing a refined location within the next 12 hours
when the LAT science data for this burst is downlinked and processed.

We note that this is an extraordinarily bright GRB,
and strongly encourage additional observations.

The Fermi-LAT point of contact for this burst
is Francesco Longo (francesco.longo@ts.infn.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: GRB160227A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19404
SUBJECT: GRB 160227A: MAXI/GSC detection
DATE:    16/05/09 10:09:49 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

Y.Ono (Tokyo Tech), S. Ueno, H. Tomida, S. Nakahira, M. Ishikawa, Y. E. Nakagawa, Y. Sugawara (JAXA), 
T. Mihara, M. Sugizaki, M. Serino, W. Iwakiri, M. Shidatsu, J. Sugimoto, T. Takagi, M. Matsuoka (RIKEN), 
N. Kawai, N.Isobe, S.Sugita, T. Yoshii, Y. Tachibana, T. Fujiwara (Tokyo Tech), 
A. Yoshida, T. Sakamoto, Y. Kawakubo, Y. Kitaoka (AGU), 
H. Tsunemi, R.Imatani (Osaka U.), 
H. Negoro, M. Nakajima, K. Tanaka, T. Masumitsu, T. Kawase (Nihon U.), 
Y. Ueda, T. Kawamuro, T. Hori, A. Tanimoto (Kyoto U.), 
Y. Tsuboi, Y. Nakamura, R. Sasaki (Chuo U.), 
M. Yamauchi, K. Furuya (Miyazaki U.), 
K. Yamaoka (Nagoya U.)
report on behalf of the MAXI team:

The MAXI/GSC nova alert system triggered a bright uncatalogued X-ray transient source at UT 2016-05-09T09:04:16.

Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (312.131 deg, 75.810 deg) = (20 48 31, +75 48 36) (J2000)
with a 90% C.L. statistical error of 0.06 deg and an additional systematic uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 1307 +- 69 mCrab
(4-10keV, 1 sigma error).
Without assumptions on the source constancy,we obtain a rectangular error
box for the transient source with the following corners:
(310.897 deg, 75.728 deg) = (20 43 35, +75 43 40) (J2000)
(311.105 deg, 75.626 deg) = (20 44 25, +75 37 34) (J2000)
(313.379 deg, 75.887 deg) = (20 53 30, +75 53 14) (J2000)
(313.181 deg, 75.991 deg) = (20 52 43, +75 59 27) (J2000)

There was no significant excess flux in the previous transit at UT 2016-0509T07:32
with an upper limit of 20 mCrab.


GRB_name: GRB160509A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19405
SUBJECT: Correction to GCN 19404; GRB 160509A: MAXI/GSC detection  
DATE:    16/05/09 10:20:07 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

Y.Ono (Tokyo Tech), S. Ueno, H. Tomida, S. Nakahira, M. Ishikawa, Y. E. Nakagawa, Y. Sugawara (JAXA), 
T. Mihara, M. Sugizaki, M. Serino, W. Iwakiri, M. Shidatsu, J. Sugimoto, T. Takagi, M. Matsuoka (RIKEN), 
N. Kawai, N.Isobe, S.Sugita, T. Yoshii, Y. Tachibana, T. Fujiwara (Tokyo Tech), 
A. Yoshida, T. Sakamoto, Y. Kawakubo, Y. Kitaoka (AGU), 
H. Tsunemi, R.Imatani (Osaka U.), 
H. Negoro, M. Nakajima, K. Tanaka, T. Masumitsu, T. Kawase (Nihon U.), 
Y. Ueda, T. Kawamuro, T. Hori, A. Tanimoto (Kyoto U.), 
Y. Tsuboi, Y. Nakamura, R. Sasaki (Chuo U.), 
M. Yamauchi, K. Furuya (Miyazaki U.), 
K. Yamaoka (Nagoya U.)
report on behalf of the MAXI team:

The MAXI/GSC nova alert system triggered a bright uncatalogued X-ray transient source at UT 2016-05-09T09:04:16.

Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (312.131 deg, 75.810 deg) = (20 48 31, +75 48 36) (J2000)
with a 90% C.L. statistical error of 0.06 deg and an additional systematic uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 1307 +- 69 mCrab
(4-10keV, 1 sigma error).
Without assumptions on the source constancy,we obtain a rectangular error
box for the transient source with the following corners:
(310.897 deg, 75.728 deg) = (20 43 35, +75 43 40) (J2000)
(311.105 deg, 75.626 deg) = (20 44 25, +75 37 34) (J2000)
(313.379 deg, 75.887 deg) = (20 53 30, +75 53 14) (J2000)
(313.181 deg, 75.991 deg) = (20 52 43, +75 59 27) (J2000)

There was no significant excess flux in the previous transit at UT 2016-0509T07:32
with an upper limit of 20 mCrab.


GRB_name: GRB160509A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19406
SUBJECT: GRB 160509A: Tiled Swift observations
DATE:    16/05/09 10:55:20 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a series of observations, tiled on the sky, of the
Fermi/LAT GRB 160509A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00054

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the Fermi/LAT event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).

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


GRB_name: GRB160509A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19407
SUBJECT: GRB 160509A: Preliminary XRT positon
DATE:    16/05/09 14:20:01 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@swift.psu.edu>

J. A. Kennea (PSU) reports on behalf of the Swift team:

Swift performed a target of opportunity observation of the Fermi/LAT 
detected GRB 160509A (GCN 19403). In rapid analysis of XRT downlinked data 
we find a bright uncatalogued point source at the following location: 
RA/Dec (J2000) = 311.74406, 76.10634, which is equivalent to:

RA(J2000) = 20h 46m 58.6s
Dec(J2000) = +76d 06m 22.8s

with an estimated uncertainty of 8 arcseconds (90% confidence). This 
position lies 24.6' away from the LAT onboard position, and 8 arcminutes 
from a LAT ground refined position (Racusin, private communication), so 
we suggest this is likely the afterglow of GRB 160509A. A refined position 
will be issued soon. Swift observations of this burst are on-going.


GRB_name: GRB160509A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19408
SUBJECT: GRB 160509A: Swift-XRT afterglow detection
DATE:    16/05/09 15:04:24 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@swift.psu.edu>

J. A. Kennea (PSU), T.G.R. Roegiers (PSU), J.P. Osborne (U. Leicester),
K.L. Page (U. Leicester), A. Melandri (INAF-OAB), P. D'Avanzo
(INAF-OAB), V. D'Elia (ASDC), D.N. Burrows (PSU), L.M. McCauley (PSU),
C. Pagani (U. Leicester) and P.A. Evans (U. Leicester) report on behalf
of the Swift-XRT team:

Swift-XRT has performed follow-up observations of the
Fermi/LAT-detected burst GRB 160509A (Longo et al. GCN Circ. 19403) in
a series of observations tiled on the sky. The total exposure time is
1.7 ks, distributed over 7 tiles; the maximum exposure at a single sky
location was 560 s. The data were collected between T0+7.3 ks and
T0+7.5 ks, and are entirely in Photon Counting (PC) mode. 

Using 250 s of XRT Photon Counting mode data and 1 UVOT images, 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 = 311.75375, 76.10837 which is equivalent to:

RA (J2000):  20 47 00.90
Dec (J2000): +76 06 30.1

with an uncertainty of 2.3 arcsec (radius, 90% confidence). This
position is 24.8 arcmin from the Fermi/LAT position, and 11 arcseconds
from the preliminary XRT position (GCN 19407). The light curve is
consistent with a constant source of mean count rate 1.4 ct/sec. We
cannot determine fading at this time.

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.7 (+/-0.3). The
best-fitting absorption column is  4.6 (+2.3, -1.8) x 10^21 cm^-2, in
excess of the Galactic value of 2.1 x 10^21 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.9 x 10^-11 (6.6 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.6 (+2.3, -1.8) x 10^21 cm^-2
Galactic foreground: 2.1 x 10^21 cm^-2
Excess significance: 2.2 sigma
Photon index:      1.7 (+/-0.3)

The results of the XRT-team automatic analysis of the likely afterglow
are at http://www.swift.ac.uk/xrt_products/TILED_GRB00054/index_2.php.
The results of the full analysis of the tiled XRT observations are
available at http://www.swift.ac.uk/xrt_products/TILED_GRB00054.

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


GRB_name: GRB160509A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19409
SUBJECT: GRB 160509A: optical observations
DATE:    16/05/09 16:52:26 GMT
FROM:    Luca Izzo at IAA-CSIC  <izzo@iaa.es>

L.Izzo (IAA-CSIC), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), C. Thoene
(IAA-CSIC) report:

We observed the field of GRB 160509A (Longo et al., GCN 19403; Ono et al.,
GCN 19404) with the iTelescope.Net <http://itelescope.net> (
http://www.itelescope.net)
T11 (Planewave CDK 0.51m) telescope located at the Mayhill observatory
(NM).
A single image of 300 s was obtained in the R filter, starting at 10:32:32
UT, 1.56 hr
after the GRB trigger. We do not detect any optical afterglow candidate at
the refined Swift-XRT position (Kennea et al. GCN 19408). We estimate an
upper limit magnitude of R = 19.5 mag (3-sigma), using the USNO-B1 catalog
as reference. We note that our image covers also the complete error box of
the MAXI (Ono et al., GCN 19404). Data are available on request.

An image of the field of view can be seen at http://goo.gl/dKTki3

[GCN OPS NOTE(09may16):  Per author's request, The affiiation and reply-to
email address of LI was changed.]


GRB_name: GRB160509A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19410
SUBJECT: GRB 160509A Gemini North candidate afterglow
DATE:    16/05/09 17:08:50 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

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

We observed the field of Fermi/LAT GRB 160509A
(Longo et al. GCN 19403) with the Gemini North telescope
on Mauna Kea, beginning at 14:45 UT during morning twilight,
approximately 5.75 hr post-burst.  Consistent with the
refined X-ray afterglow position reported by Kennea et al.
(GCN 19408) we detect a faint source with preliminary
magnitudes of r=23.52+/-0.15, z=21.35+/-0.30 (calibrated
via SDSS stars in the field).  We cannot make any statement
about the variability of this source at the present time.

The position of the source is 20:47:00.93 +76:06:29.2 (J2000),
accurate to about 0.5" in each coordinate.

The fairly red r-z colour could be explained if the burst
was at a high redshift of z=5-6, or alternatively at a 
more moderate redshift with some extinction in the host
galaxy.

We acknowledge the rapid response of the Gemini staff, in
obtaining these observations.


GRB_name: GRB160509A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19411
SUBJECT: GRB 160509A: Fermi GBM Detection
DATE:    16/05/09 17:47:13 GMT
FROM:    Oliver Roberts at UCD/Fermi  <oliver.roberts@ucd.ie>

O.J. Roberts (UCD), G. Fitzpatrick (UCD) and
P. Veres (UAH) report on behalf of the Fermi GBM Team:

"At 08:59:04.36 UT on 09 May 2016, the Fermi Gamma-Ray
Burst Monitor triggered and located GRB 160509A
(trigger 484477148/160509374). The trigger resulted in
an Autonomous Repoint Request (ARR) by the GBM Flight
Software owing to the high peak flux of the GRB. This
ARR was accepted and the spacecraft slewed to the GBM
in-flight location. The GRB was also detected by the
LAT (F. Longo et al. 2016, GCN 19403), MAXI/GSC
(Y. Ono et al. 2016, GCN 19404) and Swift XRT
(J.A. Kennea et al. 2016, GCN 19408). The GBM on-ground
location is consistent with these positions.

The angle from the Fermi LAT boresight at the GBM
trigger time using the LAT position, is 32 degrees.

The GBM light curve consists of multiple peaks
with a duration (T90) of about 371 s (50-300 keV).
The time-averaged spectrum from T0-1.5 s to T0+39.4 s is
best fit by a BAND function, with Epeak = 370 +/- 7 keV,
alpha = -0.89 +/- 0.01, and beta = -2.11 +/- 0.02.

The event fluence (10-1000 keV) in this time interval is
(1.51 +/- 0.01)E-04 erg/cm^2. The 1-sec peak photon flux
measured starting from T0+16.6 s in the 8-1000 keV band
is 75.5 +/- 0.6 ph/s/cm^2.

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


GRB_name: GRB160509A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19412
SUBJECT: GRB 160509A: Swift/UVOT Upper Limit
DATE:    16/05/09 17:54:45 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and T.G.R. Roegiers (PSU) report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the Swift-XRT afterglow
(Kennea et al., GCN Circ. 19408) 7259 s after the LAT trigger 
(Longo et al., GCN Circ. 19403). No UVOT source consistent with the position 
of Swift-XRT afterglow or the position of the optical afterglow
candidate (Levan et al., GCN Circ. 19410) is found in the initial exposure.
The preliminary upper limit using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) is:

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

u                7259         7531          268          >20.5 

The magnitude in the table is not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.31 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB160509A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19413
SUBJECT: GRB 160509A: Fermi-LAT refined analysis
DATE:    16/05/09 18:09:47 GMT
FROM:    Elisabetta Bissaldi at U.Innsbruk/IAPP  <Elisabetta.Bissaldi@uibk.ac.at>

F. Longo (University and INFN, Trieste), E. Bissaldi (Politecnico and INFN, Bari),
G. Vianello (Stanford U.), E. Moretti (MPI, Munich), N. Omodei (Stanford U.),
J. Bregeon (CNRS/IN2P3/LUPM), F. Dirirsa (Johannesburg U.),  M. Yassine (LUPM, Montpellier),
D. Kocevski, J. Racusin, J. McEnery (all NASA/GSFC), M. Ohno (Hiroshima U.) and
S. Zhu (AEI Potsdam-Golm / AEI Hannover) report on behalf of the Fermi-LAT Team:


Using LAT source class events >100 MeV from 0 until 2660 seconds after the LAT trigger,
we find a LAT localization of

RA, Dec = 311.3, 76.1 (J2000 deg)

with a 90% containment radius of 0.12 degrees (statistical only).
The LAT executed an autonomous repoint 2 minutes after the trigger to follow
the burst for 2.5 hours. A Fermi ToO for the next 36 hours has been issued.

Following our detection, Swift followed the GRB and detected the X-ray afterglow
with the Swift/XRT (Kennea et al. GCN 19408).

The highest-energy photon is a 52 GeV event, which is observed
77 seconds after the GBM trigger.

The LAT Low Energy (LLE) emission consists of two bright structured
peaks (around T0+12 and T0+18 s), in coincidence with the main GBM emission episode.

The >100 MeV emission spectrum during the main GBM emission episode
(from T0 to T0+40 s, see Roberts et al. GCN 19411) is fit by a
soft power-law with index -3.4 +/- 0.2,
resulting in a flux of (0.56 +/- 0.06)E-4 ph cm^-2 s^-1.

The >100 MeV emission spectrum after 40 s and up to the currently
available data (up to 2660 s) is fit by a power-law with index -2.0 +/- 0.1.


The Fermi LAT point of contact for this burst is
Francesco Longo (francesco.longo@ts.infn.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: GRB160509A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19414
SUBJECT: GRB 160509A: VLA Detection
DATE:    16/05/09 22:29:25 GMT
FROM:    Kate Alexander at Harvard  <kalexander@cfa.harvard.edu>

K. D. Alexander (Harvard), T. Laskar (NRAO / UC Berkeley), and E. Berger
(Harvard) report on behalf of a larger collaboration:

We observed the Fermi/LAT GRB 160509A (Longo et al. GCN 19403) at multiple
frequencies with the Karl G. Jansky Very Large Array (VLA) beginning 2016
May 9.72 UT (8.33 hours after the burst). At a mean frequency of 6.0 GHz,
we detect a radio source with a preliminary flux density of ~80 uJy at

RA (J2000) = 20:47:00.89 +/- 0.11
Dec (J2000) = +76:06:28.92 +/- 1.2

consistent with the position of the candidate optical afterglow reported by
Levan et al. (GCN 19410) and the refined Swift/XRT position (Kennea et al.
GCN 19408). Follow-up observations are planned.

We thank the VLA staff for rapidly executing these observations.


GRB_name: GRB160509A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19415
SUBJECT: GRB 160509A: MAXI/GSC refined analysis
DATE:    16/05/10 04:13:32 GMT
FROM:    H. Negoro at Nihon U.  <negoro@phys.cst.nihon-u.ac.jp>

H. Negoro (Nihon U.), S. Nakahira (JAXA),  T. Mihara (RIKEN),
S. Ueno, H. Tomida, M. Ishikawa, Y. E. Nakagawa, Y. Sugawara (JAXA), 
M. Sugizaki, M. Serino, W. Iwakiri, M. Shidatsu, J. Sugimoto, T. Takagi, M. Matsuoka (RIKEN), 
N. Kawai, N. Isobe, S. Sugita, T. Yoshii, Y. Tachibana, Y. Ono, T. Fujiwara (Tokyo Tech), 
A. Yoshida, T. Sakamoto, Y. Kawakubo, Y. Kitaoka (AGU), 
H. Tsunemi, R.Imatani (Osaka U.), M. Nakajima, K. Tanaka, T. Masumitsu, 
T. Kawase (Nihon U.), Y. Ueda, T. Kawamuro, T. Hori, A. Tanimoto (Kyoto U.), 
Y. Tsuboi, Y. Nakamura, R. Sasaki (Chuo U.), M. Yamauchi, K. Furuya (Miyazaki U.),  
K. Yamaoka (Nagoya U.) report on behalf of the MAXI team:

We reexamined the localization of GRB 160509A (Longo et al. GCN 19403; 
Ono et al. GCN 19404,19405) only using the GSC camera 7 (Bcam1), and
not using an uncalibrated GSC camera 0 (Acam0) which was also used in 
the previous analysis (GCN 19404, 19405).

We obtain the source position for a constant flux source at
(R.A., Dec) = (311.521 deg, 76.057 deg) = (20 46 05, +76 03 24) (J2000)
with a 90% C.L. statistical error of 0.12 deg and an additional systematic 
uncertainty of 0.1 deg (90% containment radius),
and a rectangular error box for a variable flux source with the following corners:
(R.A., Dec) = (310.806 deg, 76.105 deg) = (20 43 13, +76 06 16) (J2000)
(R.A., Dec) = (311.249 deg, 75.892 deg) = (20 44 59, +75 53 32) (J2000)
(R.A., Dec) = (312.671 deg, 76.056 deg) = (20 50 41, +76 03 21) (J2000)
(R.A., Dec) = (312.242 deg, 76.270 deg) = (20 48 57, +76 16 13) (J2000)

The Swift/XRT source position (Kennea et al. GCN 19408; Levan et al. GCN 19410;  
Alexander et al. GCN 19414) is 0.076 arc-degree from the refined best position, 
and also within the rectangular region.

A GSC spectrum is roughly represented by an absorbed power-law 
with a photon spectral index of 1.26 +/- 0.16, and the resultant 2-10 keV flux 
is 2.78e-08 ergs/cm^2/s. The absorption column is fixed to 4.6 x 10^21 cm^-2 
in the fit (Kennea et al. GCN 19408).

We also note that there was no significant excess flux in the next transit at 
10:37 UT on 2016 May 9 with an upper limit of 20 mCrab.
~                         


GRB_name: GRB160509A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19416
SUBJECT: GRB 160509A: DCT Imaging / Afterglow Confirmation
DATE:    16/05/10 12:17:04 GMT
FROM:    S. Bradley Cenko at NASA/GSFC  <brad.cenko@nasa.gov>

S. B. Cenko (NASA GSFC), E. Troja (NASA GSFC), and S. Tegler (NAU) report on behalf of a larger collaboration:

We imaged the location of the Fermi GBM (Roberts et al., GCN 19411), Fermi LAT (Longo et al., GCN 19403), and MAXI GSC (Ono et al, GCN 19405) GRB160509A with the Large Monolithic Imager on the 4.3 m Discovery Channel Telescope in Happy Jack, AZ.  Observations were obtained in the g, r, i, and z filters beginning at 9:40 UT on 10 May 2016 (~ 1.03 d after the trigger).

At the location of the candidate optical afterglow (Levan et al., GCN 19410), we detect a source in all four filters.  We report the following preliminary photometry (using nearby point sources from SDSS for calibration):

g = 25.03 +/- 0.15
r = 24.05 +/- 0.14

The source has faded since the Gemini observations reported by Levan et al. (GCN 19410), indicating that it is indeed the afterglow of GRB160509A.  However, the detection in g limits the host redshift to be z <~ 3.5, requiring significant dust extinction along the line of sight.


GRB_name: GRB160509A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19417
SUBJECT: Konus-Wind observation of GRB 160509A
DATE:    16/05/10 12:44:04 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

D. Frederiks, S. Golenetskii, R.Aptekar, P. Oleynik, M. Ulanov,
D. Svinkin, A. Tsvetkova, A.Lysenko, A. Kozlova, and T. Cline,
on behalf of the Konus-Wind team, report:

The very bright, long-duration GRB 160509A
(Fermi-LAT detection: Longo et al., GCN 19403;
MAXI/GSC detection: Ono et al., GCNs 19404;
Fermi-GBM detection: Roberts, Fitzpatrick & Veres, GCN 19411)
triggered Konus-Wind at T0=32326.696 s UT (08:58:46.696).

The light curve shows a broad, multi-peaked pulse in the interval
from ~T0-10 s to ~T0+30 s, followed by several weaker emission
episodes until ~T0+380 s.
The emission is seen up to ~15 MeV.

As observed by Konus-Wind, the burst had a fluence
of 2.90(-0.35,+0.35)x10^-4 erg/cm2, and a 64-ms peak flux,
measured from T0+12.096 s, of 2.8(-0.2,+0.2)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+370.944 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 = -0.99 (-0.08,+0.10),
the high energy photon index beta = -2.08 (-0.17,+0.12),
the peak energy Ep = 288 (-45,+48) keV,
chi2 = 51.3/97 dof.

The spectrum near the peak count rate (measured from T0+11.264
to T0+12.800 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 = -0.71 (-0.07,+0.07),
the high energy photon index beta = -2.27 (-0.14,+0.11),
the peak energy Ep = 311 (-32,+35) keV,
chi2 = 96.7/77 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB160509_T32326/

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


GRB_name: GRB160509A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19419
SUBJECT: GRB 160509A Gemini North redshift
DATE:    16/05/10 16:43:15 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir (U. Leicester), A. J. Levan (U. Warwick),
S. B. Cenko (NASA/GSFC), D. Perley (DARK), A. Cucchiara (GSFC/STScI),
K. Roth (Gemini), K. Wiersema (U. Leicester), A. Fruchter (STScI), 
T. Laskar (NRAO/U.C. Berkeley) report on behalf of a larger collaboration:

We observed the optical counterpart of Fermi/LAT GRB 160509A
(Levan et al. GCN 19410) with the Gemini North telescope
on Mauna Kea, beginning at 2016-05-10 13:15 UT obtaining
both optical spectroscopy with GMOS-N and near-IR imaging
with NIRI.

Our spectroscopy covers a wavelength range of about 5900 AA
to 10100 AA, and reveals a single, well detected emission line
which we interpret as [OII] 3727 AA at a redshift of z=1.17 
(provisional analysis).  Alternative possible identifications for this 
line are ruled out by the absence of other lines in the spectrum.

Our infrared imaging shows the source, presumably some
combination of host and afterglow, to be very red with
K(Vega)~16.6 and J(Vega)~19.7 calibrated via 2MASS stars
in the field.  This would be consistent with a heavily dust
extinguished event. We also note that the source is apparently
unresolved in K-band seeing of 0.55 arcsec.

We acknowledge the excellent support of the Gemini staff,
in particular Michael Hoenig, and kind cooperation of the
visiting observers, in expediting these observations.  We also
thank Gemini Head of Science, Nancy Levenson, for approving 
this request.


GRB_name: GRB160509A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19420
SUBJECT: GRB 160509A: Further Swift/UVOT Observations
DATE:    16/05/10 21:30:27 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and T.G.R. Roegiers (PSU) report on behalf of the Swift/UVOT team:

The afterglow of the LAT-triggered GRB 160509A (Longo et al., GCN Circ. 19403)
has been detected in the X-ray (Kennea et al., GCN Circ. 19408),
optical (Levan et al., GCN Circ. 19410; Cenko et al., GCN Circ. 19416),
near-IR (Tanvir et al., GCN Circ. 19419), and radio (Alexander et al. GCN Circ. 19414) bands.
No afterglow was seen in the initial UVOT observation in the u filter
(Marshall and Roegiers, GCN Circ. 19412). As detailed in the table below,
additional UVOT observations also show no detections.
All the upper limits are at 2-sigma confidence.

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

u                7259        19794          626          >21.6
u               24201        36310         1802          >22.2
v               25452        36990         1257          >21.4
white           24826        36919         1802          >23.2

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.31 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB160509A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19421
SUBJECT: GRB 160509A: TLS Tautenburg Afterglow Detection
DATE:    16/05/10 21:32:49 GMT
FROM:    Sebastian Schmidl at TLS Tautenburg  <schmidl@tls-tautenburg.de>

S. Schmidl, D. A. Kann, U. Laux (all TLS Tautenburg), S. Schulze (PUC), S.
Klose, and A. Nicuesa Guelbenzu (both TLS Tautenburg) report:

We observed the location of the afterglow of the bright Fermi LAT/GBM
(Longo et al., GCN 19403, Roberts et al., GCN 19411) GRB 160509A,
localized in the X-rays by Kennea (GCN 19407) and Kennea et al. (GCN
19408), in the optical/NIR by Levan et al. (GCN 19411) and Cenko et al.
(GCN 19416), as well as in the radio band by Alexander et al. (GCN 19414),
with the 1.34m Schmidt telescope of the Thueringer Landessternwarte
Tautenburg, in good conditions.

We obtained a total of 26 x 600 s images in the Rc band, starting at
20:46:04 UT, 11.78 hrs after the GRB. The total stack has an integration
time of 15600 s, centered 0.583 days after the GRB.

At the afterglow position, we detect an extended source. Comparing to the
higher resolution DCT image (Cenko & Tanvir, priv. comm.), there is a
nearby source which is somewhat blended with the afterglow in our image.
Therefore, we use a small aperature to measure the afterglow magnitude. 
Using four comparison stars in the surroundings, whose SDSS magnitudes
were transformed to the Rc band using the transformation equations of
Lupton (2005), we obtained a magnitude of:

Rc = 23.6 +/- 0.3 mag.

This is in good agreement with the detections derived by Levan et al. and
Cenko et al. after transforming their results from AB to Vega mags.

The magnitude is not corrected for the Galactic extinction along the line
of sight of E(B-V) = 0.25 mag (Schlafly & Finkbeiner 2011).

Using the prompt emission results of Konus-Wind (Frederiks et al., GCN
19417) and the redshift z = 1.17 (Tanvir et al., GCN 19419), we derive a
bolometric (1 keV - 10 MeV in the source frame) isotropic energy release
of (8.56 +/- 1.1)E53 erg, and a E_peak,rest = 625 keV. The isotropic
energy release is very similar to that of GRB 130427A, and we note the
light curve also shows similarities.

PS.: We also wish to point out that this GRB occurred on the 11th
anniversary of the first ever detected short-GRB X-ray afterglow, that of
GRB 050509B (Gehrels et al. 2005).

[GCN OPS NOTE(10may16):  Per author's request, In the last paragraph,
"050509A" was corrected to "050509B".]


GRB_name: GRB160508A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19422
SUBJECT: GRB 160508A: CALET Gamma-Ray Burst Monitor detection
DATE:    16/05/11 01:54:08 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

P. S. Marrocchesi (U of Siena), A. Yoshida, T. Sakamoto, Y. Kawakubo, M. Moriyama,
Y. Yamada (AGU), K. Yamaoka (Nagoya U), S. Nakahira (JAXA), I. Takahashi (IPMU),
Y. Asaoka, S. Ozawa, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U),
W. Ishizaki (ICRR), M. L. Cherry (LSU), S. Ricciarini (U of Florence)
and the CALET collaboration:

The long-duration GRB 160508A (INTEGRAL-ACS trigger #7459; Konus-Wind trigger time on
14:32:38.795 UT) triggered the CALET Gamma-Ray Burst Monitor (CGBM) at 14:32:31.73 on
8 May 2016.  The burst signal was seen by all CGBM instruments.

The light curve of the SGM shows a single spike starting at T0, peaking at T0+6 sec,
and ending at T0+35 sec.  A hint of the emission is seen up to T0+~150 sec.
The T90 duration measured by the SGM data is 20.0 +- 1.6 sec (40-450 keV).

The CGBM data used in this analysis are provided by the Waseda CALET Operation Center
located at the Waseda University. 


GRB_name: GRB160509A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19423
SUBJECT: GRB 160509A: non-observation of VHE emission with HAWC
DATE:    16/05/11 17:27:37 GMT
FROM:    Dirk Lennarz at HAWC  <dirk.lennarz@gatech.edu>

D. Lennarz (Michigan State University), I. Taboada (Georgia Tech) report
on behalf of the HAWC collaboration
(http://www.hawc-observatory.org/collaboration/):

We used data from the HAWC detector to perform a search for VHE emission
in temporal coincidence with GRB 160509A (F.Longo et al., GCN 19403). At
the time of the LAT trigger, the elevation of the burst in HAWC's field
of view was only 27.98 degrees (it was rising, but culminated at an
elevation of 33 degrees). The sensitivity of HAWC at this elevation is
more than 2 orders of magnitude poorer than near the zenith.
Furthermore, the energy threshold towards the horizon is much higher.
Combined with the moderate redshift of z=1.17 (N. R. Tanvir et al., GCN
19419) it makes a detection by HAWC unlikely.

We used four search windows with respect to the LAT trigger time: one in
the range -5 s to 45 s, which covers the main GBM emission episode (O.J.
Roberts et al., GCN 19411) and appears to be correlated with the >100
MeV soft emission observed by the LAT (F.Longo et al., GCN 19413), a
window from -5 s to 375 s, which extends slightly beyond the T90
observed by GBM and a time window from 45 s to 375 s, where the LAT data
is fit with a power-law of index -2.0 +/- 0.1. We also searched -20 s to
20 s around the time of the highest-energy LAT photon (52 GeV) 77
seconds after the GBM trigger. A 2 degree angular bin is defined around
the position of the Swift-XRT afterglow position (J. A. Kennea et al.,
GCN 19408) and the number of background events is estimated using an
ON/OFF method. We find the counts in the search bin to deviate by 1.9 /
0.9 / 0.2 / -1.4 sigma from the background expectation. Our observations
are consistent with background only.

The search was conducted using the main data acquisition that
reconstructs the incident direction of showers. It uses data
reconstructed at the HAWC site, not applying gamma-hadron separation.
The implications of this non-detection with respect to the VHE fluence
of this GRB will be reported elsewhere.

HAWC is a very-high-energy gamma-ray observatory operating in Central
Mexico at a latitude of 19 deg north. HAWC has an instantaneous field of
view of 2 sr and surveys 2/3 of the sky every day. A detailed
description of the sensitivity of HAWC to GRBs can be found in A.U.
Abeysekara et al., Astroparticle Physics 35, 641-650 (2012).


GRB_name: GRB160509A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19424
SUBJECT: GRB 160509A: CALET Gamma-Ray Burst Monitor detection
DATE:    16/05/12 06:41:12 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

A. Yoshida, T. Sakamoto, Y. Kawakubo, M. Moriyama, Y. Yamada (AGU), 
K. Yamaoka (Nagoya U), S. Nakahira (JAXA), I. Takahashi (IPMU), Y. Asaoka, 
S. Ozawa, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), W. Ishizaki (ICRR), 
M. L. Cherry (LSU), S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena) 
and the CALET collaboration:

The long-duration GRB 160509A (Longo et al., GCN circ. 19403; Ono et al., 
GCN circ. 19404; Roberts et al., GCN circ. 19411; Frederiks et al., GCN circ. 19417) 
triggered the CALET Gamma-Ray Burst Monitor (CGBM) at 08:58:51.21 on 9 May 2016.  
The burst signal was seen by all CGBM instruments.  The angular separations between 
the GRB position (Kennea et al., GCN 19408) and the boresignt of the HXM and 
the SGM instrument at the trigger time were 108 deg. and 104 deg., respectively.  
Therefore, the GRB was outside the field of view of the CAL instrument.

The light curve of the SGM shows multiple overlapping pulses with a broad structure 
starting from T0-5 sec, peaking at T0+9 sec and ending at T0+30 sec.  A hint of the 
emission is seen at T0+~370 sec.  The T90 duration measured by the SGM data is 
14.6 +- 0.6 sec (40-1000 keV).

The CGBM data used in this analysis are provided by the Waseda CALET Operation Center
located at the Waseda University. 


GRB_name: GRB160509A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19425
SUBJECT: GRB 160509A MASTER-NET observations
DATE:    16/05/12 10:27:08 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

V. Lipunov, E. Gorbovskoy,   N.Tyurina, V.Kornilov, P.Balanutsa,
A.Kuznetsov, D.Kuvshinov,
Lomonosov Moscow State University, Sternberg Astronomical Institute

D.Buckley, S. Potter, A.Kniazev, M.Kotze
South African Astronomical Observatory

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

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)

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
The Instituto de Astrofisica de Canarias

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Blagoveschensk was pointed to the  GRB160509A (Longo et al GCN 
19403)  15306 sec after trigger time at 2016-05-09 13:14:10 UT directly 
after sunset. On our first (180s exposure)  set we not found optical 
transient brighter then 18.5m  on single (180 s) and 20.0m on coadd  (total 
exposure 1800 s) images at x-ray (Kennea et al GCN 19408) and optical 
(Levan et al 19410, Alexander et al GCN  19414, Cenko et al GCN  19416, 
Schmidl et al GCN  19421) position.

The message may be cited.


GRB_name: GRB160509A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19428
SUBJECT: GRB 160509A: Further VLA Observations
DATE:    16/05/13 15:48:05 GMT
FROM:    S. Bradley Cenko at NASA/GSFC  <brad.cenko@nasa.gov>

S. B. Cenko (NASA GSFC), S. Vogel (U. Maryland), D. A. Perley (DARK), and A. Fruchter (STScI) report on behalf of a larger collaboration:

We have imaged the location of the radio afterglow (Alexander et al., GCN 19414) of GRB 160509A (Longo et al., GCN 19403; Roberts et al., GCN 19411; Ono et al, GCN 19405) with the Very Large Array beginning at 10:11 UT on 2016 May 11 (2.0 d after the Fermi-GBM trigger time) in both C and X bands.  The radio counterpart has brightened significantly since the early observations reported in Alexander et al., GCN 19414.  We measure a preliminary flux density of ~ 0.7 mJy in X-band (9.0 GHz) and ~ 0.5 mJy in C-band (6.0 GHz), corresponding to a spectral index beta ~ 0.8 (fnu ~ nu^beta).

Further observations are planned.


GRB_name: GRB160519A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19436
SUBJECT: GRB 160519A: Swift detection of a burst
DATE:    16/05/19 00:29:48 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

P. D'Avanzo (INAF-OAB), S. D. Barthelmy (GSFC) and J. A. Kennea (PSU)
report on behalf of the Swift Team:

At 00:17:33 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 160519A (trigger=686818).  Swift did not slew due to Sun constraint. 
The BAT on-board calculated location is 
RA, Dec 71.113, +31.197, which is 
   RA(J2000)  =  04h 44m 27s
   Dec(J2000) = +31d 11' 48"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single, possibly multiple,
peaks with a duration of about 6 sec.  The peak count rate
was ~1500 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 11:24 UT on 2016 July 22. There will thus be no XRT or
UVOT data for this trigger before this time. 

Burst Advocate for this burst is P. D'Avanzo (paolo.davanzo 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: GRB160519A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19439
SUBJECT: GRB 160519A: Fermi GBM detection
DATE:    16/05/19 18:27:43 GMT
FROM:    Peter Veres at UAH  <veresp@gmail.com>

P Veres (UAH) and C Meegan (UAH)
report on behalf of the Fermi GBM Team:

"At 2016-05-19 00:17:33.55 UT on 19 May 2016, the Fermi Gamma-Ray
Burst Monitor triggered and located GRB 160519A (trigger 485309857 /
160519012), which was also detected by Swift (D'Avanzo et al., GCN
19436). The GBM on-ground location is consistent with the Swift
position.

The angle from the Fermi LAT boresight to the best location is 52 degrees.

The GBM light curve consists of multiple, weak emission episodes
with a duration (T90) of about 97 s (50-300 keV).
The time-averaged spectrum from T0-3.6 s to T0+40.4 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.97 +/- 0.25 and
the cutoff energy, parameterized as Epeak, is 61.7 +/- 7.3 keV.

The event fluence (10-1000 keV) in this time interval is
(1.4 +/- 0.1)E-6 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-0.2 s in the 10-1000 keV band
is 3.3 +/- 0.2 ph/s/cm^2.

A Band function fits the spectrum equally well
with Epeak = 51 +/- 11 keV, alpha = -0.67 +/- 0.51 and beta = -2.51 +/- 0.36.

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


GRB_name: GRB160519A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19441
SUBJECT: GRB 160519A: Swift-BAT refined analysis
DATE:    16/05/20 22:51:21 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
P. D'Avanzo (INAF-OAB), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), T. N. Ukwatta (LANL) (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 160519A (trigger #686818)
(D'Avanzo, et al., GCN Circ. 19436).  The BAT ground-calculated position is
RA, Dec = 71.122, 31.246 deg which is
  RA(J2000)  =  04h 44m 29.2s
  Dec(J2000) = +31d 14' 46.1"
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 19%.

The mask-weighted light curve shows a single-pulse structure that starts
at ~ T-1 s, peaks at ~T0, and ends at ~T+3 s. There are some weak emissions
extend till ~T+40 s. T90 (15-350 keV) is 35.57 +- 6.11 sec (estimated error
including systematics).

The time-averaged spectrum from T-0.99 to T+41.12 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.95 +- 0.25.  The fluence in the 15-150 keV band is 1.2 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-0.16 sec in the 15-150 keV band
is 2.4 +- 0.5 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/686818/BA/


GRB_name: GRB160521A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19442
SUBJECT: GRB 160521A: a long GRB detected by INTEGRAL
DATE:    16/05/21 04:45:52 GMT
FROM:    Sandro Mereghetti at IASF-Milano/INAF  <sandro@iasf-milano.inaf.it>

S.Mereghetti (IASF-Milano), D.Gotz (CEA, Saclay), C.Ferrigno, E.Bozzo, 
L.Di Gesu' (ISDC, Versoix), and J.Borkowski (CAMK, Torun) on behalf of the 
IBAS Localization Team report:

a gamma ray burst lasting about 160 s has been detected by IBAS in the 
IBIS/ISGRI data at 03:37:20 UT of May 21, 2016.

The refined coordinates (J2000) are:
R.A.=  129.7108
DEC.=    46.9142
with an uncertainty of    1.5 arcmin (90% c.l.).

The burst had a peak flux of 0.8 counts/cm2/s (20-200 keV, 1-s integration 
time) and a fluence in the same energy range of about 1.2e-6 erg/cmq.

A plot of the light curve will  be posted at
http://ibas.iasf-milano.inaf.it/IBAS_Results.html


GRB_name: GRB160521B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19443
SUBJECT: GRB 160521B: Fermi GBM detection
DATE:    16/05/21 18:49:44 GMT
FROM:    Hoi-Fung Yu at MPE  <sptfung@mpe.mpg.de>

H.-F. Yu (MPE) and P. Veres (UAH) report on behalf of the Fermi GBM Team:

"At 09:13:58.03 UT on 21 May 2016, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 160521B (trigger 485514842 / 160521385).

The on-ground calculated location, using the GBM trigger
data, is RA = 156, Dec = 76 (J2000 degrees, equivalent 
to 15h 25m, 76d 17'), with an uncertainty of 1 degree 
(radius, 1-sigma containment, statistical only; there is 
additionally a systematic error which we have characterized 
as a core-plus-tail model, with 90% of GRBs having a 3.7 deg 
error and a small tail suffering a larger than 10 deg
systematic error. [Connaughton et al. 2015, ApJS, 216, 32] ).

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

The trigger resulted in an Autonomous Repoint Request (ARR)
by the GBM Flight Software owing to the high peak flux of the GRB. 
This ARR was accepted and the spacecraft slewed to the GBM in-flight
location. The initial angle from the Fermi LAT boresight to
the GBM ground location is 47 degree.

The GBM light curve shows a single pulse with sub-structures
with a duration (T90) of about 2.8 s (50-300 keV).
The time-averaged spectrum from T0+0.002 s to T0+3.520 s is
best fit by a Band function with Epeak = 155 +/- 5 keV,
alpha = -0.45 +/- 0.03, and beta = -2.54 +/- 0.07.

The event fluence (10-1000 keV) in this time interval is
(1.25 +/- 0.02)E-05 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+0.960 s in the 10-1000 keV band
is 42.4 +/- 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: GRB160521B
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19444
SUBJECT: GRB 160521B: Fermi-LAT detection
DATE:    16/05/21 18:59:10 GMT
FROM:    Magnus Axelsson at Stockholm U.  <magaxe@kth.se>

M. Axelsson (KTH Stockholm), E. Bissaldi (Politecnico and INFN Bari), J. McEnery
(NASA/GSFC), F. Dirirsa (Univ. of Johannesburg) and J.M. Burgess (KTH Stockholm)
report on behalf of the Fermi-LAT team:

At UT 09:13:58.03 on May 21, 2016, Fermi-LAT detected high-energy emission
from GRB 160521B, which was also detected by Fermi-GBM
(trigger 485514841/160521385).

The best LAT on-ground location is found to be

RA, Dec = 148.17, 79.01 (degrees, J2000)

with an error radius of 0.17 deg (90% containment, statistical error only).
This was 47 deg from the LAT boresight at the time of the trigger and triggered
an autonomous repoint of the spacecraft.

The data from the Fermi-LAT show a significant increase in the event rate that
is spatially and temporally correlated with the trigger with high significance.
More than 10 photons above 100 MeV are observed within 3000 seconds, with
the highest-energy photon being a 12 GeV event observed 420 seconds after
the GBM trigger.

A Swift ToO has been approved for this burst.

The Fermi-LAT point of contact for this burst is Magnus Axelsson (magaxe@kth.se<mailto:magaxe@kth.se>).

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: GRB160521B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19445
SUBJECT: GRB 160521B: Swift ToO observations
DATE:    16/05/21 20:01:16 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a ToO observation of the Fermi/LAT GRB 160521B. 
Automated analysis of the XRT data will be presented online at
http://www.swift.ac.uk/ToO_GRBs/00020615

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. These are
not necessarily related to the Fermi/LAT event. Any X-ray source
considered to be a probable afterglow candidate will be reported via a 
GCN Circular after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).

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


GRB_name: GRB160521B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19448
SUBJECT: GRB 160521B: Swift-XRT observations
DATE:    16/05/22 03:38:23 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@swift.psu.edu>

K.L. Page (U. Leicester), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), A.
D'Ai (INAF-IASFPA), T.G.R. Roegiers (PSU), L.M. McCauley (PSU), J.A.
Kennea (PSU), C. Pagani (U. Leicester), A.P. Beardmore (U. Leicester)
and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team:

Swift-XRT has performed follow-up observations of the
Fermi/LAT-detected burst GRB 160521B (Axelsson et al. GCN Circ. 19444),
collecting 2.0 ks of Photon Counting (PC) mode data between T0+41.9 ks
and T0+47.7 ks. 

One uncatalogued X-ray source has been detected, it is below the RASS
limit and shows no definitive signs of fading. Therefore, at the
present time we cannot confirm this as the afterglow. Details of this
source are given below:

Source 1:
  RA (J2000):  147.6669  =  09:50:40.06
  Dec (J2000): +79.0302  =  +79:01:48.9
  Error: 4.6 arcsec (radius, 90% conf.)
  Count-rate: 0.0122 +/- 0.0028 ct s^-1
  Flux: (5.3 +/- 1.2)e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

The results of the XRT-team automatic analysis of the XRT observations,
including a position-specific upper limit calculator, are available at
http://www.swift.ac.uk/ToO_GRBs/00020615.

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


GRB_name: GRB160521B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19449
SUBJECT: GRB 160521B: Swift/UVOT Upper Limits
DATE:    16/05/22 17:23:14 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) reports on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of GRB 160521B centered on
the LAT position (Axelsson et al., GCN Circ. 19444) 41882 seconds after
the trigger. The exposures for the optical filters (white, b, and u)
cover about 20% of the LAT statistical error circle, and
the uv filters (uvw1 and uvm2) cover about 44%.
Only the exposures with the uv filters cover
the possible XRT counterpart (Page et al., GCN Circ. 19448).
The preliminary upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) are:

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

white           42794        43127          324          >20.8
b               41882        49001         1180          >20.7
u               47789        48695          885          >20.2
uvw1            46882        54226         1578          >20.1
uvw2            52616        53065          886          >20.4

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: GRB160313A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19450
SUBJECT: GRB 160313A: 15 GHz upper limits from AMI
DATE:    16/05/23 18:50:48 GMT
FROM:    Kunal Mooley at Oxford U  <kunal.mooley@physics.ox.ac.uk>

K. P. Mooley, T. D. Staley, R. P. Fender (Oxford), G. E. Anderson 
(Curtin), C. Rumsey, D. Titterington, S. Carey, J. Hickish, Y. C. 
Perrott, N. Razavi-Ghods, P. Scott (Cambridge), K. Grainge, A. Scaife 
(Manchester)

The AMI Large Array robotically triggered on the Swift alert for GRB 
160313A (D'Ai et al., GCN 19171) as part of the 4pisky program, and 
subsequent follow up observations were obtained up to 10 days 
post-burst. Our observations at 15 GHz on 2016 Mar 13.15, Mar 13.97, Mar 
16.00, Mar 20.11, and Mar 23.02 (UT) do not reveal any radio source at 
the XRT location (Goad et al., GCN 19174), with 3sigma upper limits of 
130 uJy, 60 uJy, 100 uJy, 170 uJy, and 70 uJy respectively.

We thank the AMI staff for scheduling these observations. The AMI-GRB 
database is a log of all GRB follow up observations with the AMI, and is 
available at http://4pisky.org/ami-grb/.


GRB_name: GRB160314A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19451
SUBJECT: GRB 160314A: 15 GHz upper limits from AMI
DATE:    16/05/23 18:53:30 GMT
FROM:    Kunal Mooley at Oxford U  <kunal.mooley@physics.ox.ac.uk>

K. P. Mooley, T. D. Staley, R. P. Fender (Oxford), G. E. Anderson 
(Curtin), C. Rumsey, D. Titterington, S. Carey, J. Hickish, Y. C. 
Perrott, N. Razavi-Ghods, P. Scott (Cambridge), K. Grainge, A. Scaife 
(Manchester)

The AMI Large Array robotically triggered on the Swift alert for GRB 
160314A (D'Elia et al., GCN 19182) as part of the 4pisky program, and 
subsequent follow up observations were obtained up to 10 days 
post-burst. Our observations at 15 GHz on 2016 Mar 14.65, Mar 15.81, Mar 
17.73, Mar 21.82, and Mar 24.91 (UT) do not reveal any radio source at 
the XRT location (Osborne et al., GCN 19185), with 3sigma upper limits 
of 280 uJy, 100 uJy, 270 uJy, 100 uJy, and 320 uJy respectively.

We thank the AMI staff for scheduling these observations. The AMI-GRB 
database is a log of all GRB follow up observations with the AMI, and is 
available at http://4pisky.org/ami-grb/.


GRB_name: GRB160321A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19452
SUBJECT: GRB 160321A: 15 GHz upper limits from AMI
DATE:    16/05/24 14:54:40 GMT
FROM:    Kunal Mooley at Oxford U  <kunal.mooley@physics.ox.ac.uk>

K. P. Mooley, T. D. Staley, R. P. Fender (Oxford), G. E. Anderson 
(Curtin), C. Rumsey, D. Titterington, S. Carey, J. Hickish, Y. C. 
Perrott, N. Razavi-Ghods, P. Scott (Cambridge), K. Grainge, A. Scaife 
(Manchester)

The AMI Large Array robotically triggered on the Swift alert for GRB 
160321A (Stamatikos et al., GCN 19211) as part of the 4pisky program, 
and subsequent follow up observations were obtained up to 10 days 
post-burst. Our observations at 15 GHz on 2016 Mar 21.70, Mar 22.85, Mar 
24.74, Mar 29.66, and Mar 31.68 (UT) do not reveal any radio source at 
the XRT location (Beardmore et al., GCN 19213), with 3sigma upper limits 
of 195 uJy, 261 uJy, 162 uJy, 207 uJy, and 189 uJy respectively.

We thank the AMI staff for scheduling these observations. The AMI-GRB 
database is a log of all GRB follow up observations with the AMI, and is 
available at http://4pisky.org/ami-grb/.


GRB_name: GRB160327A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19453
SUBJECT: GRB 160327A: 15 GHz upper limits from AMI
DATE:    16/05/24 15:04:33 GMT
FROM:    Kunal Mooley at Oxford U  <kunal.mooley@physics.ox.ac.uk>

K. P. Mooley, T. D. Staley, R. P. Fender (Oxford), G. E. Anderson 
(Curtin), C. Rumsey, D. Titterington, S. Carey, J. Hickish, Y. C. 
Perrott, N. Razavi-Ghods, P. Scott (Cambridge), K. Grainge, A. Scaife 
(Manchester)

The AMI Large Array robotically triggered on the Swift alert for GRB 
160327A (Racusin et al., GCN 19235) as part of the 4pisky program, and 
subsequent follow up observations were obtained up to 10 days 
post-burst. Our observations at 15 GHz on 2016 Mar 27.75, Mar 28.94, Mar 
30.94, Apr 04.79, and Apr 06.83 (UT) do not reveal any radio source at 
the XRT location (Goad et al., GCN 19237), with 3sigma upper limits of 
84 uJy, 69 uJy, 96 uJy, 102 uJy, and 93 uJy respectively.

We thank the AMI staff for scheduling these observations. The AMI-GRB 
database is a log of all GRB follow up observations with the AMI, and is 
available at http://4pisky.org/ami-grb/.


GRB_name: GRB160425A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19454
SUBJECT: GRB 160425A: SMARTS late-time observations
DATE:    16/05/24 18:35:05 GMT
FROM:    Bethany Cobb at GWU  <bcobb@gwu.edu>

B. E. Cobb (GWU), reports:

Using the ANDICAM instrument on the 1.3m telescope at CTIO, we obtained
additional optical/IR imaging of the error region of GRB 160425A
(GCN 19343, Krimm et al.) at 7.3, 18.4 and 26.4 days post-burst.
For each epoch, total summed exposure times amounted to 36 minutes in
I and 30 minutes in J.

The possible host of GRB 160425A (GCN 19350, Tanvir et al.,
GCN 19351, Balanutsa et al.) is observed in these images. This object
appears as two separate knots and, therefore, may be a merging pair
of galaxies (GCN 19350, Tanvir et al.). The object, with a magnitude
of I~20.1 (calibrated using USNO-B1.0 stars), exhibits no significant
changes in brightness between 7 and 26 days post-burst, though changes
in brightness of less than 0.05 magnitudes cannot be ruled out by the
data. In this type of host, at a redshift of z=0.555 (GCN 19350,
Tanvir et al.), a 1998bw-like supernova would be expected to increase
the brightness of the host by approximately 0.1 magnitudes, and can
therefore be excluded. If this unusual burst (GRB GCN 19343, Krimm
et al.) is actually a long-duration GRB, than any associated supernova
must be dimmer at peak than SN 1998bw.


GRB_name: GRB160521B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19456
SUBJECT: GRB 160521B: Theoretical estimate of the redshift and urgent need for further x-ray observations
DATE:    16/05/24 19:29:15 GMT
FROM:    Remo Rufinni at ICRA  <ruffini@icra.it>

R. Ruffini, Y. Aimuratov, L. Becerra, C.L. Bianco, M. Kovacevic, R.
Moradi, M. Muccino, A.V. Penacchioni, G.B. Pisani, D. Primorac, J.
Rueda, Y. Wang report:


From preliminary data of GRB 160521B detected by the Fermi satellite (Yu
& Veres, GCN 19443) and from the presence of both gamma-ray (Fermi-GBM,
8 keV - 40 MeV) and GeV emission (Fermi-LAT, 0.1-100 GeV, see Axelsson
et al., GCN 19444) it is likely that this source is a Binary driven
Hypernova (BdHN) at very high redshift.

Following Ruffini et al. 2016 (arXiv:1602.02732), it lies in the BdHN
region of the Ep-Eiso plane for selected values of the redshift above
0.5 (see purple filled circles in Fig.[1]). The observed GeV emission
implies that the source cannot be a XRF.

The current paucity of data of the X-ray afterglow (Page et al., GCN
19448) is surprising and should be further examined up to late times
taking as an example GRB 090423 at z = 8.

Assuming that GRB 160521B is actually a BdHN, we can test the overlap of
its X-ray flux with the prototypical BdHN sources (see Pisani et al.
2013, A&A, 552, L5). In Fig.[2] it is plotted the single available data
point (Page et al., GCN 19448), not yet observed dimming, of GRB 160521B
X-ray luminosity, assuming 20 different values of the redshift from 0.5
(the lowest blue point) to 10 (the highest one) in steps of 0.5.

From these preliminary data, GRB 160521B is a BdHN with possible
redshift z > 2.5 all the way up to z ~ 10, assuming that the single
observed X-ray data point belongs to the afterglow. A deep search for
the afterglow in the X-ray band is indeed crucial to define the nature
of this source.


[1] http://www.icranet.org/documents/GRB160521b_Fig1.pdf
[2] http://www.icranet.org/documents/GRB160521b_Fig2.pdf


GRB_name: GRB160525A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19458
SUBJECT: GRB 160525A: Swift detection of a probable burst
DATE:    16/05/25 01:47:52 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. Stamatikos (OSU/NASA/GSFC), A. D'Ai (INAF-IASFPA),
C. Gronwall (PSU), A. Maselli (INAF-IASFPA) and D. M. Palmer (LANL)
report on behalf of the Swift Team:

At 01:33:59 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 160525A (trigger=687492).  Swift could not slew to the 
burst due to an observing constraint. 
The BAT on-board calculated location is 
RA, Dec 103.530, -0.173 which is 
   RA(J2000) = 06h 54m 07s
   Dec(J2000) = -00d 10' 24"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As is typical for an image trigger, there
is no obvious variation in the immediately available lightcurve. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 12:15 UT on 2016 August 19. There will thus be no XRT or
UVOT data for this trigger before this time. 

Although the observing constraint prevents a confirmation of
this untriggered event, its significance (7.2 sigma) makes
it most likely to be a real astrophysical event.  A more
definite determination will require the full downlinked dataset. 

Burst Advocate for this burst is M. Stamatikos (Michael.Stamatikos-1 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: GRB160525B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19459
SUBJECT: GRB 160525B: Swift detection of a burst
DATE:    16/05/25 09:34:47 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

H. A. Krimm (CRESST/GSFC/USRA), S. D. Barthelmy (GSFC),
A. D'Ai (INAF-IASFPA), P.A. Evans (U Leicester), C. Gronwall (PSU),
F. E. Marshall (NASA/GSFC), A. Maselli (INAF-IASFPA),
K. L. Page (U Leicester) and D. M. Palmer (LANL) report on behalf of
the Swift Team:

At 09:25:07 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 160525B (trigger=687522).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 149.443, +51.180 which is 
   RA(J2000)  =  09h 57m 46s
   Dec(J2000) = +51d 10' 49"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single peak
structure with a duration of about 10 sec.  The peak count rate
was ~1500 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 09:26:31.0 UT, 83.4 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 149.38688, 51.20658 which is equivalent
to:
   RA(J2000)  = 09h 57m 32.85s
   Dec(J2000) = +51d 12' 23.7"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 158 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. No spectrum from the promptly downlinked
event data is yet available to determine the column density. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 88 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 0.01. 

Burst Advocate for this burst is H. A. Krimm (hans.krimm 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: GRB160525B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19460
SUBJECT: GRB 160525B: Prompt enhanced Swift-XRT position
DATE:    16/05/25 10:50:45 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 1.9 ks of promptly downlinked XRT event data for GRB 160525B, we
find an enhanced XRT position of the afterglow: RA, Dec: 149.3845,
51.2064 which is equivalent to:
   RA (J2000)  = 09 57 32.28
   Dec (J2000) = +51 12 23.0
with an uncertainty of 2.1 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/687522.

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: GRB160525A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19461
SUBJECT: GRB 160525A: Swift-BAT refined analysis
DATE:    16/05/25 12:09:38 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. N. Ukwatta (LANL), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU),
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+903 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 160525A (trigger #687492)
(Stamatikos, et al., GCN Circ. 19458).  The BAT ground-calculated position is
RA, Dec = 103.575, -0.199 deg, which is 
   RA(J2000)  =  06h 54m 17.9s 
   Dec(J2000) = -00d 11' 55.6" 
with an uncertainty of 3.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 98%.
 
The mask-weighted light curve shows a weak peak starting at ~T+5 sec and
ending at ~T+65 sec.
 
The time-averaged spectrum from T+0.00 to T+64.00 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.58 +- 0.54.  The fluence in the 15-150 keV band is 1.9 +- 0.7 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.00 sec in the 15-150 keV band
is 0.06 +- 0.02 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 

Given the low significance of the peak in the image domain (5.2 sigma)
in the ground analysis and the lack of XRT data (Sun constrained),
it is not possible to know with certainty if this is a GRB, but it seems likely.
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/687492/BA/


GRB_name: GRB160521B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19462
SUBJECT: Konus-Wind observation of GRB 160521B
DATE:    16/05/25 12:53:34 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks, P. Oleynik,
M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration GRB 160521B
(Fermi-GBM detection: Yu and Veres, GCN 19443;
Fermi-LAT detection: Axelsson et al., GCN 19444)
triggered Konus-Wind at T0=33237.337 s UT (09:13:57.337).

The burst light curve shows a broad, multi-peaked pulse
started at ~T0-0.3 s with a total duration of ~6.4 s.
The emission is seen up to ~2 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB160521_T33237/

As observed by Konus-Wind, the burst
had a fluence of 1.32(-0.15,+0.17)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+1.504 s,
of 1.01(-0.14,+0.14)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+9.984 s)
is best fit in the 20 keV - 2 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.65(-0.14,+0.16),
the high energy photon index beta = -2.72(-0.49,+0.26),
the peak energy Ep = 165(-16,+17) keV
(chi2 = 49/61 dof)

The spectrum near the maximum count rate
(measured from T0+0.256 to T0+1.792 s)
is best fit in the 20 keV - 2 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.43(-0.12,+0.14),
the high energy photon index beta = -3.62(-6.38,+0.62),
the peak energy Ep = 190(-15,+15) keV
(chi2 = 56/50 dof)

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


GRB_name: GRB160525B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19463
SUBJECT: GRB 160525B: Enhanced Swift-XRT position
DATE:    16/05/25 15:29:40 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 1923 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 160525B, 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 = 149.38464, +51.20657 which is equivalent
to:

RA (J2000): 09h 57m 32.31s
Dec (J2000): +51d 12' 23.7"

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: GRB160521B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19464
SUBJECT: GRB 160521B: Swift-XRT afterglow detection
DATE:    16/05/25 19:12:11 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

K.L. Page (U. Leicester), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), A.
D'Ai (INAF-IASFPA), T.G.R. Roegiers (PSU), L.M. McCauley (PSU), J.A.
Kennea (PSU), C. Pagani (U. Leicester), A.P. Beardmore (U. Leicester)
and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team:

Swift-XRT has conducted further observations of the field of the
Fermi/LAT-detected burst GRB 160521B (Axelsson et al. GCN Circ. 19444).
The observations now extend from T0+41.9 ks to T0+346.3 ks. The source
previously reported by Page et al. (GCN Circ. 19448), "Source 1", is
fading with 3-sigma significance, and is therefore likely the GRB
afterglow.  The position of this source is RA, Dec=147.6665, +79.0305
which is equivalent to:

RA (J2000): 09:50:39.96
Dec(J2000): +79:01:49.7

with an uncertainty of 4.2 arcsec (radius, 90% confidence).  This
position is 5.9 arcmin from the Fermi/LAT position. 

The light curve can be modelled with a power-law decay with a decay
index of alpha=0.7 (+0.7, -0.4).

The results of the XRT-team automatic analysis of the likely afterglow
are at http://www.swift.ac.uk/ToO_GRBs/00020615/index_1.php.
The results of the full analysis of the XRT observations are available
at http://www.swift.ac.uk/ToO_GRBs/00020615.

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


GRB_name: GRB160525B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19465
SUBJECT: GRB 160525B: Swift/UVOT Detection
DATE:    16/05/25 20:09:20 GMT
FROM:    Massimiliano de Pasquale at IASF-Palermo  <m.depasquale@ucl.ac.uk>

M. De Pasquale, N.P. Kuin (UCL-MSSL) 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 160525B
88 s after the BAT trigger (Krimm et al., GCN Circ. 19459).
A source consistent with the XRT position (Evans GCN Circ. 19460)
is detected in the initial UVOT white filter exposure.

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               88          238          147         19.8 +/- 0.3
white              581         1894          284        >20.9
v                  631         1945          156        >18.9
b                  556         1870          136        >19.8
u                  300         2018          379        >20.0
w1                 680         1996          156        >19.5
m2                1603         1795           39        >18.2
w2                 606         1573           58        >18.9

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).

-- 

Dr. Massimiliano De Pasquale
Research associate - Swift UVOT scientist
Mullard Space Science Laboratory, University College London


GRB_name: GRB160525B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19466
SUBJECT: GRB 160525B: Nanshan optical upper limit
DATE:    16/05/25 21:32:53 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

D. Xu, Y.-H. Han (both NAOC/CAS), S.-G. Ma, A. Esamdin, J.-Z. Liu, L. Ma 
(all XAO) report:

We observed the field of GRB 160525B (Krimm et al., GCN 19459) using the 
1m telescope located at Nanshan, Xinjiang, China. We obtained 5x300s 
R-band frames, starting at 15:26:24 UT on 2016-05-25, i.e., 6.02 hr 
after the burst.

No optical source is detected at the XRT position (Beardmore et al., GCN 
19463) in the stacked image, down to a limiting magnitude of m(R)>21.5, 
calibrated with the nearby SDSS field.


GRB_name: GRB160525B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19467
SUBJECT: GRB 160525B: Swift-XRT refined Analysis
DATE:    16/05/25 21:57:33 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), A. Maselli  (INAF-IASFPA),
L.M. McCauley (PSU), J.A. Kennea (PSU), B. Sbarufatti (INAF-OAB/PSU),
C. Pagani (U. Leicester), 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 6.3 ks of XRT data for GRB 160525B (Krimm et al. GCN
Circ. 19459), from 91 s to 18.0 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. 19460).

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.27 (+/-0.10).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.91 (+0.26, -0.24). The
best-fitting absorption column is  6.0 (+6.5, -5.1) x 10^20 cm^-2,
consistent with the Galactic value of 8.3 x 10^19 cm^-2 (Willingale et
al. 2013). 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:
Total column:      6.0 (+6.5, -5.1) x 10^20 cm^-2
Galactic foreground: 8.3 x 10^19 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.91 (+0.26, -0.24)

If the light curve continues to decay with a power-law decay index of
1.27, the count rate at T+24 hours will be 2.6 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 8.8 x
10^-15 (10.0 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/00687522.

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


GRB_name: GRB160525B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19468
SUBJECT: GRB 160525B: Swift-BAT refined analysis
DATE:    16/05/26 04:07:57 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL)
(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 160525B (trigger #687522)
(Krimm, et al., GCN Circ. 19459).  The BAT ground-calculated position is
RA, Dec = 149.438, 51.197 deg, which is 
   RA(J2000)  =  09h 57m 45.2s 
   Dec(J2000) = +51d 11' 48.9" 
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 81%.
 
The mask-weighted light curve shows weak emission starting at ~T-1 sec,
the main emission from ~T0 to ~T+0.3 sec, and weak emission out to ~T+0.6 sec.
T90 (15-350 keV) is 0.29 +- 0.05 sec (estimated error including systematics).
 
The time-averaged spectrum from T+0.02 to T+0.33 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.89 +- 0.35.  The fluence in the 15-150 keV band is 3.2 +- 0.8 x 10^-8 erg/cm2.
The 1-sec peak photon flux measured from T-0.32 sec in the 15-150 keV band
is 0.9 +- 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/687522/BA/


GRB_name: GRB160525B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19469
SUBJECT: GRB 160525B: Khureltogot optical upper limit
DATE:    16/05/26 18:06:16 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), S. Schmalz (ISON), A. Volnova (IKI),  N. Tungalag 
(Research Center of Astronomy and Geophysics MAS),   I. Molotov (KIAM),
A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration:

We observed the field of the GRB 160525B (Krimm et al., GCN  19459) with 
  ORI-40 telescope of Khureltogot observatory starting on May, 25 (UT) 
15:51:26.  We do not detect any source within enhanced Swift-XRT 
position (Beardmore et al., GCN 19463). Preliminary photometry  of  the 
combined image is following

Date        UT start   t-T0    Filter  Exp.    UpperLimit (3 sigma)
                       (mid, days)      (s)

2016-05-25  15:51:26   0.29070  clear  60*60  21.0

Photometry is based on nearby SDSS-DR9 stars, Lupton transformations into R:
SDSS-DR9_id            R(Lupton)
J095742.79+511301.4    16.17
J095737.78+511402.4    16.43
J095736.76+511019.5    14.87
J095730.61+510914.1    17.74
J095737.35+510856.0    15.01


GRB_name: GRB160525B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19470
SUBJECT: GRB 160525B: Mondy optical upper limit
DATE:    16/05/26 18:08:31 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI),  E. Klunko (ISTP), A. Volnova (IKI),   I. Korobtsev 
(ISTP),  A. Pozanenko (IKI) report on behalf of larger GRB follow-up 
collaboration:

We observed the field of the GRB 160525B (Krimm et al., GCN  19459) with 
AZT-33IK telescope of Sayan observatory (Mondy)  starting on May, 25 
(UT) 15:54:47.  We do not detect any source within enhanced Swift-XRT 
position (Beardmore et al., GCN 19463). Preliminary photometry  of  the 
combined image is following

Date        UT start   t-T0    Filter  Exp.    UpperLimit (3 sigma)
                       (mid, days)      (s)

2016-05-25  15:54:47   0.29111  R       30*120  22.6

Photometry is based on nearby SDSS-DR9 stars, Lupton transformations into R:
SDSS-DR9_id            R(Lupton)
J095742.79+511301.4    16.17
J095737.78+511402.4    16.43
J095736.76+511019.5    14.87
J095730.61+510914.1    17.74
J095737.35+510856.0    15.01


GRB_name: GRB160525C
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19471
SUBJECT: GRB 160525C: CALET Gamma-Ray Burst Monitor detection
DATE:    16/05/28 23:39:39 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

T. Sakamoto, A. Yoshida, Y. Kawakubo, M. Moriyama, Y. Yamada (AGU), K. Yamaoka (Nagoya U), 
S. Nakahira (JAXA), I. Takahashi (IPMU), Y. Asaoka, S. Ozawa, S. Torii (Waseda U), Y. Shimizu, 
T. Tamura (Kanagawa U), W. Ishizaki (ICRR), M. L. Cherry (LSU), S. Ricciarini (U of Florence) 
P. S. Marrocchesi (U of Siena) and the CALET collaboration:

GRB 160525C (Konus-Wind trigger time on 10:54:28.0 UT) triggered the CALET Gamma-Ray 
Burst Monitor (CGBM) at 10:54:20.25 on 25 May 2016.  The burst signal was seen by all 
CGBM instruments.

The light curve of the SGM shows a double peak structure starting at T0+4 sec, peaking 
at T0+5 sec, and ending at T0+6.5 sec sec.  The T90 duration measured by the SGM data 
is 2.4 +- 0.3 sec (40-230 keV).  The light curve is available at

http://cgbm.calet.jp/cgbm_trigger/flight/1148208864/index.html

The CGBM data used in this analysis are provided by the Waseda CALET Operation Center
located at the Waseda University. 


GRB_name: GRB160530A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19472
SUBJECT: GRB 160530A: Tiled Swift observations
DATE:    16/05/30 12:32:19 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a series of observations, tiled on the sky, of the
COSI GRB 160530A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00055

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the COSI event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).

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


GRB_name: GRB160530A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19473
SUBJECT: GRB 160530A: discovery with the Compton Spectrometer and Imager
DATE:    16/05/30 22:47:40 GMT
FROM:    John Tomsick at SSL at UCB  <jtomsick@ssl.berkeley.edu>

John A. Tomsick (UC Berkeley/Space Sciences Laboratory) reports on behalf 
of the Compton Spectrometer and Imager (COSI) team:

COSI is a large field of view (1/4-sky) gamma-ray (0.1-10 MeV) instrument on 
a Superpressure Balloon flight that began on May 16.  

A likely Gamma-ray Burst (GRB 160530A) was detected by COSI in both the 
cesium iodide shields and the germanium strip detectors (GeDs).  The GRB 
started at 2016 May 30, 07:03:46 UT and lasted until 07:04:23 UT (based on 
the shield rates).  During the burst, the light curve shows several large amplitude 
fluctuations.

Based on the GeD rates and assuming a Band function with alpha=1.0, 
beta=2.5, and E_break = 150 keV, we calculated a preliminary burst fluence of 
1.3E-5 erg/cm2.  This value may be revised in the future using the spectral 
capabilities of the GeDs.

The position of the GRB is R.A. = 120.2 deg, Decl. = -26.2 deg (J2000, 90% 
confidence error radius = 1.5 degrees), which corresponds to Galactic coordinates 
of l = 243.9 deg, b = 2.1 deg.  Due to the proximity to the Galactic plane, a Galactic 
origin cannot be ruled out.

We searched the SIMBAD database for possible counterparts, and three known 
gamma-ray sources are present in the COSI error region:  GRB 080516, 
2FGL J0758.0-2615c, and 3FGL J0755.2-2633 are, respectively, 0.4, 0.6, and 
1.3 degrees from the center of the COSI error circle. 

Follow-up observations with Swift/XRT are underway (see P.A. Evans et al., GCN 
Circ. 19472) to search for an afterglow that may allow us to improve the position 
and provide a definitive classification of the COSI burst.


GRB_name: GRB160530B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19474
SUBJECT: GRB 160530B: Fermi GBM Detection
DATE:    16/05/31 00:38:22 GMT
FROM:    Bagrat Mailyan at UAH  <bm0054@uah.edu>

B. Mailyan (UAH) and C. Meegan (UAH) report on behalf of the Fermi GBM Team:

"At 16:01:11.83 UT on 30 May 2016, the Fermi Gamma-Ray
Burst Monitor triggered and located GRB 160530B
(trigger 486316875/160530667). The on-ground calculated location,
using the GBM trigger data, is RA =  133.48, DEC = 43.48, with an
uncertainty of 1.0 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which we have characterized as a core-plus-tail model, with 90% of
GRBs having a 3.7 deg error and a small tail suffering a larger than 10 deg
systematic error. [Connaughton et al. 2015, ApJS, 216, 32] ).

The trigger resulted in an Autonomous Repoint Request
(ARR) by the GBM Flight Software owing to the high peak
flux of the GRB. This ARR was accepted and the spacecraft
slewed to the GBM in-flight location.

The angle from the Fermi LAT boresight at the GBM
trigger time is 78 degrees.

The GBM light curve consists of a single peak
with a duration (T90) of about 9 s (50-300 keV).
The time-averaged spectrum from T0+2.8 s to T0+12.0 s is
best fit by a BAND function, with Epeak = 188.40 +/- 2.23  keV,
alpha = -0.56 +/- 0.01, and beta = -2.53 +/- 0.04.

The event fluence (10-1000 keV) in this time interval is
 (8.898 +/- 0.055)E-05 erg/cm^2. The 1-sec peak photon flux
measured starting from T0+5.6 s in the 10-1000 keV band
is 107.7 +/- 0.7 ph/s/cm^2.

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


GRB_name: GRB160525B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19475
SUBJECT: GRB 160525B: MITSuME Akeno optical upper limits 
DATE:    16/05/31 10:05:57 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

K. Saisho, Y. Muraki, Y. Ono, T. Fujiwara, T. Yoshii, Y. Saito, Y. Tachibana,
H. Ohuchi, Y. Yano, S. Harita, Y. Yatsu, and N. Kawai (Tokyo Tech)
report on behalf of the MITSuME collaboration:

We searched for the optical counterpart of GRB 160525B (H. A. Krimm et al., GCN Circular #19459) 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 2016-05-25 10:03:51 UT (~0.65 h after the burst).
We did not find any new point source within XRT circle in all three bands.

We obtained following limits for the magnitudes.

T0+[hour]    MID-UT     T-EXP[sec]      g'         Rc          Ic
----------------------------------------------------------------------------
   0.65        15:58:53         1140       >18.6     >18.2    >17.6
----------------------------------------------------------------------------
T0+ : Elapsed time after the burst 
T-EXP: Total Exposure time 
We used GSC2.3 catalog for flux calibration.


GRB_name: GRB160530A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19476
SUBJECT: IPN Triangulation of GRB 160530A
DATE:    16/05/31 15:21:11 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, A. Kozlova,
and T. Cline on behalf of the Konus-Wind team,

K. Hurley, on behalf of the IPN,

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, very bright GRB 160530A (COSI detection Tomsick GCN 
Circ. 19473) has been detected by Konus-Wind and INTEGRAL (SPI-ACS), so 
far, at about 25426 s UT (07:03:46).

We have triangulated it to a Konus-SPI-ACS annulus centered at 
RA(2000)=50.332 deg (03h 21m 20s)  Dec(2000)=+12.855 deg (+12d 51' 19"), 
whose radius is 77.066 +/- 0.305 deg (3 sigma).

The COSI position reported by Tomsick (GCN Circ. 19473) is
consistent with the annulus. The annulus combined with the COSI
(90% confidence) error circle produces the following preliminary error
box:
----------------------------------
RA(2000), deg   Dec(2000), deg
----------------------------------
Center:
118.942        -25.764
Corners:
118.644        -25.659
118.758        -26.966
119.239        -25.868
119.707        -24.768
----------------------------------
The error box area is 3404.3 sq. arcmin, and its maximum
dimension is 2.36 deg (the minimum one is 18 arcmin).
The Sun distance was about 67 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB160530_T25426/IPN/

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


GRB_name: GRB160530A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19477
SUBJECT: Konus-Wind observation of GRB 160530A
DATE:    16/05/31 16:16:26 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, P. Oleynik,
M. Ulanov, A. Tsvetkova, A. Lysenko, A. Kozlova, and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration, very intense GRB 160530A
(COSI detection: Tomsick, GCN Circ. 19473;
IPN triangulation: Svinkin et al., GCN circ. 19476)
triggered Konus-Wind at T0=25426.549 s UT (07:03:46.549).

The burst light curve shows a multipeaked structure
started at ~T0-0.1 s with a total duration of ~37 s.
The emission is seen up to ~5 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB160530_T25426/

As observed by Konus-Wind, the burst
had a fluence of 1.30(-0.04,+0.04)x10^-4 erg/cm2,
and a 64-ms peak flux, measured from T0+2.416 s,
of 3.70(-0.38,+0.38)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+38.912 s)
is best fit in the 20 keV - 5 MeV range
by a power law with exponential cutoff (CPL) model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -0.93(-0.03,+0.03)
and Ep = 638(-33,+36) keV (chi2 = 73/73 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -3.5
(chi2 = 73/72 dof)

The spectrum near the maximum count rate
(measured from T0+1.792 to T0+2.560 s)
is best fit in the 20 keV - 7 MeV range
by the CPL model
with alpha = -0.23(-0.09,+0.10)
and Ep = 714(-50,+55) keV (chi2 = 53/62 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.9
(chi2 = 50/61 dof)

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


GRB_name: GRB160601A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19478
SUBJECT: GRB 160601A: Swift detection of a short hard burst
DATE:    16/06/01 15:00:57 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

D. Kocevski (NASA/GSFC/ORAU), P.A. Evans (U Leicester),
N. Gehrels (NASA/GSFC), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), B. Mingo (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL), T. G. R. Roegiers (PSU)
and M. H. Siegel (PSU) report on behalf of the Swift Team:

At 14:43:02 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 160601A (trigger=688452).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 235.034, +64.495 which is 
   RA(J2000) = 15h 40m 08s
   Dec(J2000) = +64d 29' 41"
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 0.2 sec.  The peak count rate
was ~7000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 14:44:16.3 UT, 74.0 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 234.9351, 64.5401 which
is equivalent to:
   RA(J2000)  = 15h 39m 44.43s
   Dec(J2000) = +64d 32' 24.2"
with an uncertainty of 3.3 arcseconds (radius, 90% containment). This
location is 223 arcseconds from the BAT onboard position. 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. This position is more than
2-sigma away from the BAT position, and so possibly unrelated to the
trigger. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 2.04
x 10^20 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 250 seconds with the U filter
starting 78 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. 

Burst Advocate for this burst is D. Kocevski (dankocevski 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: GRB160601A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19479
SUBJECT: GRB 160601A: MASTER-Net observations
DATE:    16/06/01 15:19:26 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

A.Gabovich, V.Yurkov, Yu.Sergienko
Blagoveschensk Educational State University, Blagoveschensk

V. Lipunov, E.Gorbovskoy,  N.Tyurina, P.Balanutsa, A.Kuznetsov, 
V.Kornilov, D.Kuvshinov, V.V.Chazov, E.Popova,
Lomonosov Moscow State University,
Sternberg Astronomical Institute, Moscow State University

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

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

D.Buckley, S. Potter, A.Kniazev
South African Astronomical Observatory

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
The Instituto de Astrofisica de Canarias

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

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


MASTER-Amur  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
was pointed to the  GRB160601A (Kocevski et al., GCN19478) 67 sec after 
notice time and 81 sec after trigger time at 2016-06-01 14:44:23 UT.
On our first (20s  and 70s exposures)  set we haven't found optical 
transient  within SWIFT error-box (ra=15h 39m 44.43s dec=+64d 32' 24.2" 
r=3.3 arcsec) The 5-sigma upper limit is 17.5mag.

MASTER-Tunka  robotic telescope was pointed to the  GRB160601.61 55 sec 
after notice time and 73 sec after trigger time at 2016-06-01 14:44:16 UT, 
on the first images (20s) there is also no OT .

The message may be cited.


GRB_name: GRB160601A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19480
SUBJECT: GRB 160601A: MITSuME Okayama upper limits
DATE:    16/06/01 15:56:56 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 160601A (Kocevski et al., GCNC 19478)
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 2016-06-01 14:43:48 UT (~46 sec after
the burst). We did not find any new point source within the XRT
circle (Kocevski et al., GCNC 19478) in all the three bands.

Three sigma upper limits of the OT are listed below.
We used SDSS-DR8 catalog for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'    Rc     Ic
-----------------------------------------------------
0.01716    15:07:45    2460.0   >20.5  >20.3  >19.3
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB160530A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19481
SUBJECT: GRB 160530A: Swift follow-up and X-ray afterglow candidate
DATE:    16/06/01 16:58:01 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. Dâ€™Elia (ASDC), L. Izzo (IAA-CSIC), P. A. Evans (U. Leicester), A.  
A. Breeveld (UCL-MSSL), J.A. Kennea (PSU), D. Malesani (DARK/NBI), C.  
B. Markwardt (NASA/GSFC) report on behalf of the Swift team:

Swift has performed follow-up observations of the COSI-detected burst  
GRB 160530A (Tomsick, GCN Circ. 19473) in a series of observations  
tiled on the sky. The total exposure time is 24 ks, distributed over  
46 tiles; the maximum exposure at a single sky location was 1.4 ks.  
The data were collected between T0+19.0 ks and T0+158 ks, and are  
entirely in Photon Counting (PC) mode.

One uncatalogued X-ray source has been detected by XRT in the  
intersection of the COSI and the IPN error regions (Svinkin et al.,  
GCN Circ. 19476), however, this source is below the RASS limit at its  
location, and we cannot currently determine whether it is fading.  
Therefore, at the present time we cannot state if it is the afterglow.  
The source was imaged and detected in the time interval T0+145 ks to  
T0+158 ks and comprises 920 s of exposure time. More XRT data are  
expected in the forthcoming days. Further details of this source are  
given below:

RA (J2000):  118.9741  =  07:55:53.77
Dec (J2000): -25.4638  =  -25:27:49.7
Error: 6.6 arcsec (radius, 90% conf.)
Count-rate: 0.0222 +/- 0.0070 ct s^-1
Flux: (6.3 +/- 2.0)e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

No optical afterglow consistent with the XRT source position is  
detected in the initial UVOT exposures. The preliminary 3-sigma upper  
limit for the summed U-band exposures (926 s) is 20.8 mag.


GRB_name: GRB160601A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19482
SUBJECT: GRB 160601A: MITSuME Okayama Ks-band upper-limit
DATE:    16/06/01 17:09:41 GMT
FROM:    Kenshi Yanagisawa at OAO/NAOJ  <yanagi@oao.nao.ac.jp>

K. Yanagisawa, D. Kuroda, Y. Shimizu, H. Izumiura(OAO/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 160601A (Kocevski et al., GCN 19478)
in Ks-band with a wide-field near infrared imager at Okayama
Astrophysical Observatory (Japan).  The imager has effective
aperture of 0.91 m.

Observations started from 14:57 UT on 1st June, 14 min after
the BAT trigger, to 15:22 UT. The total exposure of 10.0 min
was successfully obtained.

In our co-add image, we did not find any new point source within
the XRT error circle down to the limiting magnitude of
Ks=16.1 (Vega, S/N=3). The photometric calibration was made
against 2MASS field stars.

T0+[sec]    MID-UT     T-EXP[sec]      Ks
---------------------------------------------------
   +1,560    15:09      600.0          >16.1
---------------------------------------------------
T0+ : Elapsed time after the burt [sec]
T-EXP: Total Exposure time [sec]


GRB_name: GRB160601A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19483
SUBJECT: GRB 160601A: Mondy optical observations
DATE:    16/06/01 19:54:08 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI),  E. Klunko (ISTP), A. Volnova (IKI),   I. Korobtsev 
(ISTP),  A. Pozanenko (IKI) report on behalf of larger GRB follow-up 
collaboration:

We observed the field of the Swift  GRB 160601A (Kocevski et al., GCN 
19478) with AZT-33IK telescope of Sayan observatory (Mondy)  starting on 
June, 01 (UT) 15:00:41.  We obtained several images in R-filter under 
good weather conditions and FWHM of 1.5 arcsec. Using only part of 
images available we marginally detect (S/N ~2) a source at the edge of 
Swift-XRT position (Kocevski et al., GCN  19478).   Coordinates of the 
source are (J2000) 15:39:44.43 +64:32:19.3 with uncertainty of 1 arcsec. 
Preliminary photometry  of  the source is R~22.3, and details of 
observations are   following

Date        UT start   t-T0    Filter  Exp.   OT(?)  UpperLimit (3 sigma)
                       (mid, days)      (s)

2016-06-01  15:00:41   0.03026  R      16*60  22.3   21.8

Photometry is based on nearby SDSS-DR9 stars, Lupton transformations into R:
SDSS-DR9_id            R(Lupton)
J153959.67+643325.7    16.72
J153956.37+643102.2    17.00
J153931.88+643247.0    17.02
J153927.50+643304.3    19.23
J153942.70+643016.4    16.27

We will update the results after all the data will be available.


GRB_name: GRB160601A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19484
SUBJECT: GRB 160601A: Enhanced Swift-XRT position
DATE:    16/06/01 20:45:22 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 609 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 160601A, 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 = 234.93505, +64.54133 which is equivalent
to:

RA (J2000): 15h 39m 44.41s
Dec (J2000): +64d 32' 28.8"

with an uncertainty of 3.3 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: GRB160601A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19485
SUBJECT: GRB160601A: NOT detection of an afterglow candidate
DATE:    16/06/01 22:49:29 GMT
FROM:    Steve Schulze at U of Iceland  <sts30@hi.is>

D. Malesani (DARK/NBI), S. Schulze (PUC, MAS), N. R. Tanvir (U Leicester), D. Xu (NAOC/CAS), A. A. Djupvik (NOT) and P. Jakobsson (U Iceland) report on behalf a larger collaboration:

We observed the field of the short GRB 160601A (Kocevski et al., GCN 19478) with the Nordic Optical Telescope (NOT) equipped with the AlFOSC imager. Our first 900-s exposure in the r band started on Jun 1.885 UT (6.5 hr after the GRB).

Close to the UVOT-enhanced XRT position (Evans et al., GCN 19484), we detect two sources, at coordinates:

(1)
RA = 15:39:43.97
Dec = +64:32:30.5
r mag = 22.85 +/- 0.10 (AB)

(2)
RA = 15:39:44.91
Dec = +64:32:32.1
r mag = 23.04 +/- 0.09 (AB)

Visual inspection of the SDSS at the above locations shows a faint, marginally detected object coincident with source (2), but no object at the position of source (1). We thus consider source (1) to be a potential afterglow candidate, though further observations are needed to test its variability.


GRB_name: GRB160601A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19486
SUBJECT: GRB 160601A: Swift-XRT refined Analysis
DATE:    16/06/02 00:29:54 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A. Maselli  (INAF-IASFPA), B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows
(PSU), T.G.R. Roegiers (PSU), P.A. Evans (U. Leicester), S.L. Gibson
(U. Leicester), J.P. Osborne (U. Leicester), A. Melandri (INAF-OAB), P.
D'Avanzo (INAF-OAB) and D. Kocevski report on behalf of the Swift-XRT
team:

We have analysed 7.9 ks of XRT data for GRB 160601A (Kocevski et al.
GCN Circ. 19478), from 94 s to 23.6 ks after the  BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Evans et al. (GCN Circ. 19484).

The light curve can be modelled with a power-law decay with a decay
index of alpha=0.49 (+0.14, -0.15).

If the light curve continues to decay with a power-law decay index of
0.49, the count rate at T+24 hours will be 2.0 x 10^-3 count s^-1

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00688452.

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


GRB_name: GRB160530B
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19487
SUBJECT: GRB 160530B CALET Gamma-Ray Burst Monitor detection
DATE:    16/06/02 03:38:23 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

Y. Kawakubo, A. Yoshida, T. Sakamoto, M. Moriyama, Y. Yamada (AGU), 
K. Yamaoka (Nagoya U), S. Nakahira (JAXA), I. Takahashi (IPMU), 
Y. Asaoka, S. Ozawa, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), 
W. Ishizaki (ICRR), M. L. Cherry (LSU), S. Ricciarini (U of Florence) 
P. S. Marrocchesi (U of Siena) and the CALET collaboration:

The long-duration GRB 160530B (Fermi-GBM trigger #486316875; Konus-Wind trigger time on 
16:01:13.14 UT) triggered the CALET Gamma-Ray Burst Monitor (CGBM) at 16:01:14.40 on 
30 May 2016.  No real time CGBM GCN notice was distributed about this trigger because 
the real time communication from the ISS was off (loss of signal) between 15:48 and 16:04.  
The burst signal was seen by all CGBM instruments.  

The light curve of the SGM shows bright structure overlaid with multiple spikes.  The emission 
starts at T0-4 sec and ends at T0+16 sec.  The multiple spikes peak at T0+2 sec, T0+3 sec 
and T0+5 sec.  The T90 duration measured by the SGM data is 7.6 +- 0.3 sec (40-450 keV).  
The light curve is available at 

http://cgbm.calet.jp/cgbm_trigger/flight/1148659270/

The CGBM data used in this analysis are provided by the Waseda CALET Operation Center 
located at the Waseda University.


GRB_name: GRB160601A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19488
SUBJECT: GRB160601A: NOT afterglow confirmation
DATE:    16/06/02 05:43:55 GMT
FROM:    Steve Schulze at U of Iceland  <sts30@hi.is>

S. Schulze (PUC, MAS), D. Malesani (DARK/NBI), A. A. Djupvik (NOT) and P. Jakobsson (U Iceland) report on behalf a larger collaboration:

We re-observed the field of the short GRB 160601A (Kocevski et al., GCN 19478) with the Nordic Optical Telescope (NOT) equipped with the AlFOSC imager. Our first 600-s exposure in the r band started on June 1 at 21:14:48 UT (13.5 hr after the GRB).

We cleanly detect the two objects reported in Malesani et al. (GCN 19485).

Object (1) (RA, Dec. = 15:39:43.97, +64:32:30.5) faded from 22.85 +- 0.10 to 23.36 +- 0.10 mag. The fading corresponds to a decay slope of 0.64 +- 0.25.

Object (2) (RA, Dec. = 15:39:44.91, +64:32:32.1) exhibits no variability beyond the 1.7 sigma confidence level.

These properties let us conclude that object (1) is the afterglow of the short GRB.

[GCN OPS NOTE(02jun16): Per author's request, the start time in the first sentence
was corrected from "21:14:48" to "04:15:44".]


GRB_name: GRB160601A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19489
SUBJECT: GRB160601A: Kanata Telescope I- and Ks-bands upper limits
DATE:    16/06/02 13:51:17 GMT
FROM:    Michitoshi Yoshida at HASC,Hiroshima U  <yoshidam@hiroshima-u.ac.jp>

T. Nakaoka, Hirochi, J., Yoshida, M. and Kawabata, K. S. (Hiroshima
Univ.) report on behalf of the OISTER collaboration

We performed I and Ks bands imaging observations around the error
circle of GRB 160601A (Kocevski et al., GCNC 19478) with the optical
infrared simultaneous camera HONIR attached to Kanata telescope of
Hiroshima University. We started the observations at 2016-06-01 16:42
UT. We did not find any optical-infrared counterpart of the burst. Five
sigma upper limits (Vega magnitude) are listed below.

# T0+[day]  MID-UT    T-EXP(I)   T-EXP(Ks)     I      Ks
-----------------------------------------------------------
0.08249     17:25:14    4025s      3500s     >20.6   >17.0
-----------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB160601A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19490
SUBJECT: GRB 160601A: Mondy optical observations, photometry of NOT sources
DATE:    16/06/02 14:35:18 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI),  E. Klunko (ISTP), A. Volnova (IKI),   I. Korobtsev
(ISTP),  A. Pozanenko (IKI) report on behalf of larger GRB follow-up
collaboration:

We observed the field of the Swift  GRB 160601A (Kocevski et al., GCN
19478) with AZT-33IK telescope of Sayan observatory (Mondy)  starting on 
June, 01 (UT) 15:00:41, i.e. 17 minutes after GRB trigger (GCN 19483). 
In a combined image we detected both NOT sources (Malesani et al., GCN 
19485) near enhanced XRT error circle (Evans et al., GCN 19484). 
Preliminary photometry (Vega) of the sources are following

Date        UT start   t-T0    Filter Exp.  NOT1          NOT2
                       (mid, days)     (s)

2016-06-01  15:00:41   0.04181  R    85*60  22.40+/-0.25  22.10+/-0.20

Photometry is based on nearby SDSS-DR9 stars, Lupton transformations into R:
SDSS-DR9_id            R(Lupton)
J153959.67+643325.7    16.72
J153956.37+643102.2    17.00
J153931.88+643247.0    17.02
J153927.50+643304.3    19.23
J153942.70+643016.4    16.27

A finding chart can be found at 
http://grb.rssi.ru/GRB160601A/GRB160601A_Mondy_160601_NOT_1_2.png


GRB_name: GRB160601A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19491
SUBJECT: GRB 160601A: GTC observations confirming transient source decay
DATE:    16/06/02 15:00:10 GMT
FROM:    Juan Carlos Tello at IAA-CSIC  <jtello@iaa.es>

J. C. Tello, Y. Hu (IAA-CSIC), A.J. Castro-Tirado (IAA-CSIC, ISA-UMA),
S. Oates (Warwick U.), A. Perez-Romero and D. Garcia-Alvarez (GTC-IAC)
on behalf of a larger collaboration, report:

We observed the field of GRB 160601A (Kocevski et al., GCN 19478) with the
Gran Telescopio Canarias (GTC) with the OSIRIS instrument and acquired
6x100s images starting 01:37:31 UT and ending 01:49:29 UT on July 2nd
(10h54m-11h06m after the Swift trigger) and we detect the afterglow
candidates reported by Malesani et al. (GCN 19485).

We also find like Schulze (GCN 19488) that Object 1 is fading and at the
time of our observations was at a magntude of ~ 23.5 in the Sloan_r filter
and calibrated to SDSS Release 6.

We note that our observations precede Schulze's by 2.5 hours and are
slightly fainter but not much more than the uncertainty of these
preliminary results, implying either a rebrightening event or a plateau due
to either afterglow behaviour or host galaxy.

[GCN OPS NOTE903jun16): Per author's request, AP-R and DG-A were added
to the author list.]


GRB_name: GRB160601A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19492
SUBJECT: GRB160601A: Gemini Imaging
DATE:    16/06/02 15:06:54 GMT
FROM:    S. Bradley Cenko at NASA/GSFC  <brad.cenko@nasa.gov>

S. B. Cenko (NASA/GSFC), W.-F. Fong (Arizona), A. J. Levan (Warwick), A. Cucchiara (STScI), E. Berger (Harvard), and D. A Perley (DARK) report on behalf of a larger collaboration:

We imaged the location of GRB160601A (Kocevski et al., GCN 19478) with the Gemini Multi-Object Spectrograph (GMOS) mounted on the 8m Gemini North telescope.  We obtained a series of 5 x 180 s r-band images beginning at 6:02 UT on 2016 June 2 (~ 15.3 hr after the BAT trigger).  The candidate optical afterglow proposed by Malesani et al (GCN 19485; their Source 1) is confirmed to be fading (see also Schulze et al., GCN 19488, Tello et al., GCN 19491).  Using nearby point sources from SDSS for calibration, we measure a magnitude of r = 23.69 +/- 0.05 at this time.  

We note that the source appears to be (marginally) extended in our GMOS images, and therefore host contamination may to be present in the above magnitude estimate.


GRB_name: GRB160601A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19494
SUBJECT: GRB 160601A: Swift-BAT refined analysis
DATE:    16/06/02 17:50:25 GMT
FROM:    Tilan Ukwatta at LANL  <tilan.ukwatta@gmail.com>

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

Using the data set from T-240 to T+500 sec from the recent
telemetry downlink, we report further analysis of BAT
GRB 160601A (trigger #688452) (Kocevski, et al., GCN Circ.
19478).  The BAT ground-calculated position is
RA, Dec = 234.923, 64.532 deg which is
   RA(J2000)  =  15h 39m 41.6s
   Dec(J2000) = +64d 31' 53.5"
with an uncertainty of 1.9 arcmin, (radius, sys+stat,
90% containment). The partial coding was 66%.

The mask-weighted light curve shows a single pluse
starting ~T-0.1 sec, and ending around ~T+0.15 sec.
T90 (15-350 keV) is 0.12 +- 0.02 sec (estimated error
including systematics).

The time-averaged spectrum from T-0.02 to T+0.12 sec is
best fit by a simple power-law model.  The power law
index of the time-averaged spectrum is 1.04 +- 0.24.
The fluence in the 15-150 keV band is 6.6 +- 1.1 x 10^-08
erg/cm2. The 1-sec peak photon flux measured from T-0.45
sec in the 15-150 keV band is 0.9 +- 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/688452/BA/


GRB_name: GRB160601A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19495
SUBJECT: GRB 160601A: MITSuME Akeno optical upper limits 
DATE:    16/06/03 06:44:27 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

Y. Saito, Y. Tachibana, T. Yoshii, T. Fujiwara, Y. Ono, Y. Muraki, S. Harita, 
T, Ozawa, K. Saisho, Y. Yatsu, and N. Kawai (Tokyo Tech) 
report on behalf of the MITSuME collaboration:

We searched for the optical counterpart of GRB 160601A (D. Kocevski et al., GCN Circular #19478) 
with theoptical three color (g', Rc, and Ic) CCD cameras attached to the 
MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan.

The observation started on 2016-06-01 23:43:35 UT (33 sec after the burst).
We did not find any new point source within XRT circle in all three bands.

We obtained following limits for the magnitudes.


T0+[day]     MID-UT      T-EXP[sec]          g'           Rc            Ic 
------------------------------------------------------------------------------------------
0.078          16:35:35        12060        >21.7         >21.1         >19.9    
------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst.
T-EXP: Total Exposure time.
We used GSC2.3 catalog for flux calibration.


GRB_name: GRB160601A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19496
SUBJECT: GRB 160601A: Swift/UVOT Upper Limits
DATE:    16/06/03 15:28:24 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

S. Sebzda (Penn State/Swift) 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 160601A
78 s after the BAT trigger (Kocevski et al., GCN Circ. 19478).
No optical afterglow consistent with the XRT position
(Evans et al. GCN Circ. 19484) 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)       78             227          147      >21.00
white            78       589          166      >20.90
v               619             639           19      >17.30
b               544             564           19      >18.32
u (fc)          289             539          491      >20.19
uvw1            668             688           19      >17.72
uvm2            643             663           19      >17.46
uvw2            595             615           19      >17.87

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: GRB160601A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19497
SUBJECT: GRB 160601A: Discovery Channel Telescope Limits
DATE:    16/06/03 17:32:35 GMT
FROM:    S. Bradley Cenko at NASA/GSFC  <brad.cenko@nasa.gov>

S. B. Cenko and E. Troja (NASA/GSFC) report on behalf of a larger collaboration:

We imaged the location of the optical afterglow (Malesani et al., GCN 19485) of the short GRB 160601A (Kocevski et al., GCN 19478) with the Large Monolithic Imager on the 4.3-m Discovery Channel Telescope in Happy Jack, AZ.  We obtained a series of 180 s exposures in the r-band filter beginning at 5:00 UT on 2016 June 3 (~ 1.6 d after the Swift trigger).  We do not detect any significant emission at the location of the optical afterglow to a limiting magnitude of r > 25.0 (calculated with respect to nearby point sources from SDSS).  Compared to the most recent detection with Gemini (Cenko et al, GCN 19492), our limits imply a significant steepening of the afterglow decay, with a lower limit on the power-law index of alpha > 1.3 (compared to alpha ~ 0.6 at earlier times; Schulze et al. 19488).

We thank the observers (T. Farnham, M. Knight, and L. Feagan) and the DCT staff for their assistance with these observations.


GRB_name: GRB160601A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19498
SUBJECT: GRB 160601A: AbAO optical observations
DATE:    16/06/03 18:19:24 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), A. Volnova  (IKI), R. Inasaridze (AbAO), V. Ayvazian 
(AbAO), I. Molotov (KIAM), A. Pozanenko (IKI) report on behalf of larger
GRB follow-up collaboration:

We observed the field of of the Swift  GRB 160601A (Kocevski et al., GCN 
19478) with AS-32 (0.7m) telescope of Abastumani Observatory starting on 
June, 01 (UT) 19:07:28. We obtained several unfiltered images of the 
field. In a combined image we detected both NOT sources (Malesani et 
al., GCN 19485). Preliminary photometry  of the optical afterglow (NOT 
source #1,  Schulze et al., GCN 19488) are following

Date        UT start   t-T0    Filter Exp.    OT         UpLim (3 sigma)
                        (mid, days)     (s)

2016-06-01  19:07:28   0.20169 CR     26*120  22.9+/-0.3 23.0


Photometry is based on nearby SDSS-DR9 stars, Lupton transformations 
into R:
SDSS-DR9_id            R(Lupton)
J153959.67+643325.7    16.72
J153956.37+643102.2    17.00
J153931.88+643247.0    17.02
J153927.50+643304.3    19.23
J153942.70+643016.4    16.27
J153948.64+643150.1    19.27
J153948.72+643220.0    19.86


GRB_name: GRB160530A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19501
SUBJECT: GRB 160530A: further Swift-XRT follow-up observations
DATE:    16/06/06 16:05:27 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. Dâ€™Elia (ASDC), L. Izzo (IAA-CSIC), A. A. Breeveld (UCL-MSSL), C. B.  
Markwardt (NASA/GSFC) report on behalf of the Swift team:

The source reported in Dâ€™Elia et al. (GCN Circ. 19481) as an X-ray  
afterglow candidate for GRB 160530A (Tomsick, GCN Circ. 19473; Svinkin  
et al., GCN Circ. 19476) does not show any sign of fading during the  
Swift-XRT observations. Several X-ray sources have been detected  
during the XRT follow-up campaign, but again, none of them show  
evidence of fading. We thus conclude that the X-ray afterglow  
associated with GRB 160530A was not identified by our observations.

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


GRB_name: GRB160607A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19502
SUBJECT: GRB 160607A: Swift detection of a bright burst
DATE:    16/06/07 11:24:20 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

T. N. Ukwatta (LANL), A. P. Beardmore (U Leicester),
P.A. Evans (U Leicester), N. Gehrels (NASA/GSFC), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), K. L. Page (U Leicester) and
D. M. Palmer (LANL) report on behalf of the Swift Team:

At 11:14:00 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 160607A (trigger=689597).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 13.663, -4.948 which is 
   RA(J2000) = 00h 54m 39s
   Dec(J2000) = -04d 56' 52"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with a duration of about 70 sec.  The peak count rate
was ~33000 counts/sec (15-350 keV), at ~12 sec after the trigger. 

The XRT began observing the field at 11:15:16.3 UT, 75.5 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 13.6655, -4.9481 which is equivalent to:
   RA(J2000)  = +00h 54m 39.72s
   Dec(J2000) = -04d 56' 53.2"
with an uncertainty of 5.2 arcseconds (radius, 90% containment). This
location is 9.0 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 1.72e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 83 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
0.05. 

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: GRB160607A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19503
SUBJECT: GRB 160607A: Enhanced Swift-XRT position
DATE:    16/06/07 18:42:30 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 616 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 160607A, 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 = 13.66744, -4.94858 which is equivalent
to:

RA (J2000): 00h 54m 40.19s
Dec (J2000): -04d 56' 54.9"

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: GRB160607A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19504
SUBJECT: GRB 160607A: Swift-XRT refined Analysis
DATE:    16/06/07 21:22:53 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

D.N. Burrows (PSU), T.G.R. Roegiers (PSU), L.M. McCauley (PSU), S.L.
Gibson (U. Leicester), J.P. Osborne (U. Leicester), K.L. Page (U.
Leicester), A. Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB), V. D'Elia
(ASDC) and T.N. Ukwatta report on behalf of the Swift-XRT team:

We have analysed 7.1 ks of XRT data for GRB 160607A (Ukwatta et al. GCN
Circ. 19502), from 65 s to 24.3 ks after the  BAT trigger. The data
comprise 935 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 Goad et al.
(GCN Circ. 19503).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=1.38 (+0.38, -0.21). At T+125 s  the decay
flattens to an alpha of 0.66 (+/-0.04) before breaking again at T+2142
s to a final decay with index alpha=1.25 (+0.08, -0.07).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.85 (+0.06, -0.05). The
best-fitting absorption column is  1.87 (+0.23, -0.22) x 10^21 cm^-2,
in excess of the Galactic value of 5.1 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.98 (+/-0.09) and a
best-fitting absorption column of 2.3 (+/-0.3) 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 (5.1 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.3 (+/-0.3) x 10^21 cm^-2
Galactic foreground: 5.1 x 10^20 cm^-2
Excess significance: 9.0 sigma
Photon index:      1.98 (+/-0.09)

If the light curve continues to decay with a power-law decay index of
1.25, the count rate at T+24 hours will be 0.048 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.7 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/00689597.

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


GRB_name: GRB160607A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19506
SUBJECT: GRB 160607A: Swift-BAT refined analysis
DATE:    16/06/07 21:41:17 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC),  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),
T. N. Ukwatta (LANL) (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 160607A (trigger #689597)
(Ukwatta, et al., GCN Circ. 19502).  The BAT ground-calculated position is
RA, Dec = 13.661, -4.952 deg which is
    RA(J2000)  =  00h 54m 38.8s
    Dec(J2000) = -04d 57' 08.0"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 84%.

The mask-weighted light curve shows a complex structure of multiple peaks.  The 
first complex begins at T-3 sec, peaks at T+12 and decays to baseline by T+24 
sec.  This is followed by another weaker peak from T+30 to T+36 sec and then 
very weak emission out to T+80 sec. T90 (15-350 keV) is 33.4 +- 0.45 sec 
(estimated error including systematics).

The time-averaged spectrum from T-13.89 to T+44.08 sec is best fit by a power 
law with an exponential cutoff.  This fit gives a photon index 1.15 +- 0.10,
and Epeak of 245.1 +- 92.7 keV (chi squared 28.56 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 2.1 +- 0.0 x 10^-5 erg/cm2
and the 1-sec peak flux measured from T+11.65 sec in the 15-150 keV band is
21.8 +- 0.5 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.37 +- 0.02 (chi squared 44.40 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/689597/BA/


GRB_name: GRB160607A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19507
SUBJECT: GRB 160607A: candidate optical afterglow from the NOT
DATE:    16/06/08 07:12:12 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Malesani (DARK/NBI), D. Xu (NAOC/CAS), H. Jonsson (Lund Univ.), and 
P. Jakobsson (Univ. Iceland) report on behalf of a larger collaboration:

We observed the field of GRB 160607A (Ukwatta et al., GCN 19502) with 
the Nordic Optical Telescope (NOT), located in La Palma (Canary 
Islands). Observations were carried out at large airmass (~3) in the 
SDSS i filter, for a total of 20 min on source, at a mean epoch 2016 
June 8.19 UT (0.725 days after the BAT trigger).

Within the refined XRT position (Goad et al., GCN 19503), we detect a 
single, faint source at coordinates (J2000):

RA = 00:54:40.14
Dec = -04:56:53.3

Carrying out photometry against the SDSS catalog, we derive a magnitude 
i = 23.45 +- 0.20 AB. As this value is fainter than the SDSS limit, and 
as we lack variability information, we cannot presently conclude whether 
this source is the afterglow of GRB 160607A. Further observations are 
planned, but will be probably delayed until the field has a better 
visibility from La Palma.


GRB_name: GRB160408A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19508
SUBJECT: GRB 160408A: 15 GHz upper limits from AMI
DATE:    16/06/08 15:12:47 GMT
FROM:    Kunal Mooley at Oxford U  <kunal.mooley@physics.ox.ac.uk>

K. P. Mooley, T. D. Staley, R. P. Fender (Oxford), G. E. Anderson 
(Curtin), T. Cantwell (Manchester), C. Rumsey, D. Titterington, S. 
Carey, J. Hickish, Y. C. Perrott, N. Razavi-Ghods, P. Scott (Cambridge), 
K. Grainge, A. Scaife (Manchester)

The AMI Large Array robotically triggered on the Swift alert for GRB 
160408A (Evans et al., GCN 19260) as part of the 4pisky program, and 
subsequent follow up observations were obtained up to 10 days 
post-burst. Our observations at 15 GHz on 2016 Apr 08.61, Apr 09.77, Apr 
13.87, Apr 15.74, and Apr 19.78 (UT) do not reveal any radio source at 
the XRT location (Osborne et al., GCN 19261), with 3sigma upper limits 
of 117 uJy, 144 uJy, 102 uJy, 204 uJy, and 145 uJy respectively.

We thank the AMI staff for scheduling these observations. The AMI-GRB 
database is a log of all GRB follow up observations with the AMI, and is 
available at http://4pisky.org/ami-grb/.


GRB_name: GRB160417A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19509
SUBJECT: GRB 160417A: 15 GHz upper limits from AMI
DATE:    16/06/08 15:16:24 GMT
FROM:    Kunal Mooley at Oxford U  <kunal.mooley@physics.ox.ac.uk>

K. P. Mooley, T. D. Staley, R. P. Fender (Oxford), G. E. Anderson 
(Curtin), T. Cantwell (Manchester), C. Rumsey, D. Titterington, S. 
Carey, J. Hickish, Y. C. Perrott, N. Razavi-Ghods, P. Scott (Cambridge), 
K. Grainge, A. Scaife (Manchester)

The AMI Large Array robotically triggered on the Swift alert for GRB 
160417A (D'Avanzo et al., GCN 19316) as part of the 4pisky program, and 
subsequent follow up observations were obtained up to 10 days 
post-burst. Our observations at 15 GHz on 2016 Apr 17.58, Apr 18.81, Apr 
20.66, Apr 24.68, and Apr 28.77 (UT) do not reveal any radio source at 
the XRT location (Osborne et al., GCN 19318), with 3sigma upper limits 
of 225 uJy, 105 uJy, 123 uJy, 72 uJy, and 96 uJy respectively.

We thank the AMI staff for scheduling these observations. The AMI-GRB 
database is a log of all GRB follow up observations with the AMI, and is 
available at http://4pisky.org/ami-grb/.


GRB_name: GRB160504A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19510
SUBJECT: GRB 160504A: 15 GHz upper limits from AMI
DATE:    16/06/08 15:19:48 GMT
FROM:    Kunal Mooley at Oxford U  <kunal.mooley@physics.ox.ac.uk>

K. P. Mooley, T. D. Staley, R. P. Fender (Oxford), G. E. Anderson 
(Curtin), T. Cantwell (Manchester), C. Rumsey, D. Titterington, S. 
Carey, J. Hickish, Y. C. Perrott, N. Razavi-Ghods, P. Scott (Cambridge), 
K. Grainge, A. Scaife (Manchester)

The AMI Large Array robotically triggered on the Swift alert for GRB 
160504A (Malesani et al., GCN 19382) as part of the 4pisky program, and 
subsequent follow up observations were obtained up to 10 days 
post-burst. Our observations at 15 GHz on 2016 May 04.85, May 05.88, May 
07.82, May 11.90, and May 14.90 (UT) do not reveal any radio source at 
the XRT location (Goad et al., GCN 19386), with 3sigma upper limits of 
93 uJy, 72 uJy, 129 uJy, 123 uJy, and 120 uJy respectively.

We thank the AMI staff for scheduling these observations. The AMI-GRB 
database is a log of all GRB follow up observations with the AMI, and is 
available at http://4pisky.org/ami-grb/.


GRB_name: GRB160607A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19511
SUBJECT: Konus-Wind observation of GRB 160607A
DATE:    16/06/08 15:25:14 GMT
FROM:    Anastasia Tsvetkova at Ioffe Institute  <tsvetkova@mail.ioffe.ru>

A. Tsvetkova, S. Golenetskii, R.Aptekar, D. Frederiks, P. Oleynik,
M. Ulanov, D. Svinkin, A. Lysenko, A. Kozlova and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration 160607A (Swift-BAT trigger #689597:
Ukwatta et al., GCN 19502; Lien et al., GCN 19506)
triggered Konus-Wind at T0=40436.923 s UT (11:13:56.923).

The burst light curve shows a complex structure of multiple peaks
with a total duration of ~38 s.
The emission is seen up to ~15 MeV.

As observed by Konus-Wind, the burst
had a fluence of 4.12(-0.51,+0.64)x10^-5 erg/cm2,
and a 64-ms peak energy flux, measured from T0+11.952 s,
of 8.13(-1.59,+1.64)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+38.912 s)
is best fit in the 70 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.68(-0.43,+1.47),
the high energy photon index beta = -2.51(-0.35,+0.26),
the peak energy Ep = 176(-42,+25) keV,
chi2 = 84/76 dof.

The spectrum near the peak count rate
(measured from T0+8.448 to T0+14.336 s)
is best fit in the 70 keV - 15 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.68(-0.31,+0.39),
the high energy photon index beta = -2.76(-0.37,+0.23),
the peak energy Ep = 188(-17,+17) keV,
chi2 = 56/74 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB160607_T40436/

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


GRB_name: GRB160607A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19512
SUBJECT: GRB 160607A: GROND confirmation of the afterglow
DATE:    16/06/08 17:51:04 GMT
FROM:    Ting-Wan Chen at MPE  <jchen@mpe.mpg.de>

T.-W. Chen, F. Knust, J. Greiner (all MPE Garching), and D. A. Kann (TLS) report on behalf of the GROND team:

We observed the field of GRB 160607A (Swift trigger 689597; Ukwatta et al., GCN #19502) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La Silla Observatory (Chile).

At the enhanced XRT position (Goad et al., GCN #19503), an afterglow candidate was discovered by NOT (Malesani et al., GCN #19507) at i' = 23.45 +/- 0.20 (AB mag), 0.725 days after the BAT trigger.

GROND observations started at 08:48 UT on 2016 June 8, 0.899 days after the GRB trigger, and are continuing. They were performed at an average seeing of 1.5" and at an average airmass of 1.48.

We found a single point source at the edge of the 1.5" Swift-XRT error circle at

RA (J2000) = 00 h 54 m 40.164 s

DEC (J2000) = -04d 56' 53.23"

with an uncertainty of 0.13" in each coordinate.

The position is consistent with the NOT position, we find that the source has faded significantly.

Based on the 100.83 min of total exposures in g'r'i'z' and 38.00 min in JHK, we estimate preliminary magnitudes for detections and the detection limits (all in AB system) of:

g' > 25.4 mag,
r' = 24.49 +/- 0.19 mag,
i' = 24.51 +/- 0.46 mag,
z' > 24.0 mag,
J = 22.34 +/- 0.34 mag,
H = 21.29 +/- 0.21 mag, and
K > 21.3 mag.

Given magnitudes are calibrated against SDSS field stars as well as 2MASS field stars and are not corrected for the expected Galactic foreground extinction corresponding to a reddening of E_(B-V)=0.05 mag in the direction of the burst (Schlafly & Finkbeiner 2011).


GRB_name: GRB160607A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19513
SUBJECT: GRB 160607A: Swift/UVOT Upper Limits
DATE:    16/06/08 18:45:54 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

S. J. LaPorte (PSU) and T. N. Ukwatta (LANL)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 160607A
84 s after the BAT trigger (Ukwatta et al., GCN Circ. 19502).
No optical afterglow consistent with the enhanced XRT position
(Goad et al., GCN Circ. 19503) nor at the position of the NOT source
(Malesani et al., GCN 19507), 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            84          233          147         >20.4
u_FC               296          546          246         >19.9
white               84         1658          299         >20.6
v                  626         1707          117         >18.7
b                  552         1633          115         >19.5
u                  296         1088          393         >19.9
w1                 849         1237           39         >19.0

The magnitudes in the table are 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).


GRB_name: GRB160607A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19517
SUBJECT: GRB 160607A CALET Gamma-Ray Burst Monitor detection
DATE:    16/06/10 01:52:00 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

M. Moriyama, A. Yoshida, T. Sakamoto, Y. Kawakubo, Y. Yamada (AGU),
K. Yamaoka (Nagoya U), S. Nakahira (JAXA), I. Takahashi (IPMU), Y. Asaoka,
S. Ozawa, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), W. Ishizaki (ICRR),
M. L. Cherry (LSU), S. Ricciarini (U of Florence) P. S. Marrocchesi (U of Siena)
and the CALET collaboration:

The long-duration GRB 160607A (Swift, Ukwatta et al. GCN Circ. 19502; Konus-Wind
trigger time on 11:13:56.92 UT; INTEGRAL-ACS trigger #7487) triggered the CALET
Gamma-Ray Burst Monitor (CGBM) at 11:13:57.49 on 7 June 2016.   The burst signal
was seen by all CGBM instruments.

The light curve of the SGM shows a complex structure with multiple spikes.
The emission starts at T0 and ends at T0+30 sec.  The multiple spikes peak
at T0+2 sec, T0+4 sec, T0+7 sec, T0+11 sec,  T0+14 sec, T0+15 sec and T0+21 sec.
The T90 duration measured by the SGM data is 18.9 +- 2.9 sec (40-1000 keV).
The light curve is available at

http://cgbm.calet.jp/cgbm_trigger/flight/1149333220/

The CGBM data used in this analysis are provided by the Waseda CALET Operation Center
located at the Waseda University.


GRB_name: GRB160508A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19519
SUBJECT: GRB 160508A: Astrosat CZTI detection
DATE:    16/06/10 11:22:12 GMT
FROM:    Varun Bhalerao at IUCAA  <varunb@iucaa.in>

V. Bhalerao (IUCAA), V. Kumar (IUCAA), D. Bhattacharya (IUCAA), A. R. Rao (TIFR), S. Vadawale (PRL) report on behalf of the Astrosat CZTI collaboration:

Analysis of Astrosat data showed the detection of GRB 160508A
(Marrocchesi et al., GCN 19422; INTEGRAL-ACS trigger #7459; Konus-Wind
trigger time on 14:32:38.795 UT) in CZTI data. The source was clearly
detected in the 40-240 keV energy range. The light curve shows a single
peak at UT 14:32:37.7 and a peak count rate of 416.6 counts/sec above
the background (four quadrants summed together), with a total of 3373
counts. The local mean background count rate was 84.0 counts/sec.  Using
cumulative rates, we measure a T90 of 25.0 secs.

CZTI GRB detections are reported regularly on the payload site at
http://astrosat.iucaa.in/czti/?q=node/9. CZTI is built by a TIFR-led
consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC
and PRL.The Indian Space Research Organisation funded, managed and
facilitated the project.


GRB_name: GRB160525C
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19520
SUBJECT: GRB 160525C: Astrosat CZTI detection
DATE:    16/06/10 11:22:33 GMT
FROM:    Varun Bhalerao at IUCAA  <varunb@iucaa.in>

V. Bhalerao (IUCAA), V. Kumar (IUCAA), D. Bhattacharya (IUCAA), A. R. Rao (TIFR), S. Vadawale (PRL)  report on behalf of the Astrosat CZTI collaboration:

Analysis of Astrosat data showed the detection of GRB 160525C (Sakamoto
et al., GCN 19471; Konus Wind trigger time 10:54:28.0 UT) in CZTI data.
The source was clearly detected in the 40-240 keV energy range. The
light curve shows a complex structure, with the strongest peak at UT
10:54:23 and a peak count rate of 640 counts/sec above the background
(four quadrants summed together), with a total of 2796 counts. The local
mean background count rate of 86.2 is counts/sec. Using cumulative
rates, we measure a T90 of 5.1 sec.

CZTI GRB detections are reported regularly on the payload site at
http://astrosat.iucaa.in/czti/?q=node/9 . CZTI is built by a TIFR-led
consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC
and PRL. The Indian Space Research Organisation funded, managed and
facilitated the project.


GRB_name: GRB160611A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19522
SUBJECT: GRB 160611A: Swift detection of a burst
DATE:    16/06/11 21:49:29 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

D. Malesani (DARK/NBI), S. D. Barthelmy (GSFC), D. M. Palmer (LANL)
and M. H. Siegel (PSU) report on behalf of the Swift Team:

At 21:40:34 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 160611A (trigger=690598).  Swift did not slew due to an observing
constraint.  The BAT on-board calculated location is 
RA, Dec 164.438, -70.395, which is 
   RA(J2000)  =  10h 57m 45s
   Dec(J2000) = -70d 23' 40"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows multiple peaks
with a duration of about 30 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~4 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+43.3
minutes. There will be no XRT or UVOT data until this time. 

Burst Advocate for this burst is D. Malesani (malesani AT dark-cosmology.dk). 
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: GRB160611A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19523
SUBJECT: GRB 160611A: Swift-XRT observations
DATE:    16/06/11 23:00:57 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

The XRT began observing the field of GRB 160611A at 22:25:16.5 UT,
2682.1 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source located at RA, Dec 164.42342,
-70.39301 which is equivalent to:
   RA(J2000)  = 10h 57m 41.62s
   Dec(J2000) = -70d 23' 34.8"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 19 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 (1.70 x
10^21 cm^-2, Willingale et al. 2013), with an excess column of 7.6
(+2.39/-2.15) x 10^21 cm^-2 (90% confidence). 


GRB_name: GRB160611A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19524
SUBJECT: GRB 160611A: Enhanced Swift-XRT position
DATE:    16/06/12 05:32:33 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 4788 s of XRT Photon Counting mode data and 10 UVOT
images for GRB 160611A, 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 = 164.42229, -70.39243 which is equivalent
to:

RA (J2000): 10h 57m 41.35s
Dec (J2000): -70d 23' 32.7"

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: GRB160611A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19526
SUBJECT: GRB 160611A: GCN19525 OT is known star
DATE:    16/06/12 08:33:51 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov (MASTER, LMSU)


The OT wich published in GCN 19525 is the result
  of the false identification.
I am sorry for my mistake.

The message may be cited.


GRB_name: GRB160611A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19527
SUBJECT: GRB 160611A: Swift-XRT refined Analysis
DATE:    16/06/12 12:58:59 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

T.G.R. Roegiers (PSU), L.M. McCauley (PSU), J.P. Osborne (U.
Leicester), K.L. Page (U. Leicester), B. Mingo (U. Leicester), P.
D'Avanzo (INAF-OAB), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), J.A.
Kennea (PSU) and D. Malesani report on behalf of the Swift-XRT team:

We have analysed 7.9 ks of XRT data for GRB 160611A (Malesani et al.
GCN Circ. 19522), from 2.7 ks to 44.8 ks after the  BAT trigger. The
data comprise 50 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. 19524).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=1.54 (+0.48, -0.21). At T+5128 s  the
decay flattens to an alpha of -0.7 (+1.3, -0.8) before breaking again
at T+7161 s to a final decay with index alpha=1.28 (+0.10, -0.09).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.01 (+0.12, -0.11). The
best-fitting absorption column is  5.0 (+0.7, -0.6) x 10^21 cm^-2, in
excess of the Galactic value of 1.7 x 10^21 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.0 x 10^-11 (6.6 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.0 (+0.7, -0.6) x 10^21 cm^-2
Galactic foreground: 1.7 x 10^21 cm^-2
Excess significance: 8.5 sigma
Photon index:      2.01 (+0.12, -0.11)

If the light curve continues to decay with a power-law decay index of
1.28, the count rate at T+24 hours will be 0.021 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 8.4 x
10^-13 (1.4 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/00690598.

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


GRB_name: GRB160611A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19529
SUBJECT: GRB 160611A: Swift-BAT refined analysis
DATE:    16/06/12 18:47:00 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

T. Sakamoto (AGU), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (GSFC/UMBC),
D. Malesani (DARK/NBI), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL)
(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 160611A (trigger #690598)
(Malesani, et al., GCN Circ. 19522).  The BAT ground-calculated position is
RA, Dec = 164.417, -70.396 deg which is
    RA(J2000)  =  10h 57m 40.0s
    Dec(J2000) = -70d 23' 45.8"
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 45%.
  
The mask-weighted light curve shows a single episode with several overlapping
pulses.  The emission starts at T-15 sec, peaks at T+3 sec and ends at T+20 sec.
T90 (15-350 keV) is 34.1 +- 5.6 sec (estimated error including systematics).
A pre-planned spacecraft slew moved the source out of the field of view at
about T+165 sec.
  
The time-averaged spectrum from T-31.38 to T+10.37 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.67 +- 0.12.  The fluence in the 15-150 keV band is 1.7 +- 0.1 x 10^-6  erg/cm2.
The 1-sec peak photon flux measured from T+2.84 sec in the 15-150 keV band
is 2.0 +- 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/690598/BA/


GRB_name: GRB160611A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19530
SUBJECT: GRB 160611A: Swift/UVOT observations
DATE:    16/06/12 18:52:25 GMT
FROM:    Massimiliano de Pasquale at IASF-Palermo  <m.depasquale@ucl.ac.uk>

M. De Pasquale (UCL-MSSL) and D. Malesani (DARK/NBI)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 160611A
2687 s after the BAT trigger (Malesani et al., GCN Circ. 19522).

Very close to the XRT error circle (Osborne et al. GCN Circ. 19523), two
sources are detected in the UVOT images. These sources are also detected
in the Digitized Sky Survey (DSS) and are listed in the USNO catalog.
Their light would blend with any new source at the XRT position, making
the analysis more delicate.

None of the two sources shows any significant flux decrease in the white
filter between the first two white exposures (mid-time: 3071 s after
the trigger) and the last three white exposures (mid-time: 10030 s after
the trigger). Similarly, we find no significant decrease of the flux
of the two sources in the u filter between the first u filter exposure
(mid-time: 2946 s) and the last one (mid-time: 8560 s).
We conclude that no optical afterglow consistent with the XRT position
is detected in the UVOT exposures.

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

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

white             2687         3456          344         >19.6
white             9578        10478          880         >19.8
v                 3668         3867          197         >18.1
b                 3051         9573         1082         >18.9
u                 2846         8660          393         >19.6
w1                4078         5167          191         >19.7
m2                3873         4072          197         >19.4
w2                3463        10905          611         >20.6

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: GRB160612A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19531
SUBJECT: GRB 160612A: Fermi GBM detection
DATE:    16/06/13 02:29:47 GMT
FROM:    Eric Burns at U of Alabama  <eb0016@uah.edu>

E. Burns (UAH), C. Meegan (UAH), and P. Jenke (UAH)
report on behalf of the Fermi GBM Team:

"At 20:12:47.55 UT on 12 June 2016, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 160612A (trigger 487455171 / 160612842).

The on-ground calculated location, using the GBM trigger
data, is RA = 350, DEC = -37 with an uncertainty
of 3 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which we have characterized as a core-plus-tail model, with 90% of
GRBs having a 3.7 deg error and a small tail suffering a larger than 10 deg
systematic error. [Connaughton et al. 2015, ApJS, 216, 32] ).

The trigger resulted in an Autonomous Repoint Request (ARR)
by the GBM Flight Software owing to the high peak flux
of the GRB. This ARR was accepted and the spacecraft slewed to the GBM
in-flight
location. The initial angle from the Fermi LAT boresight to
the GBM ground location is 26 degrees.

The GBM light curve consists of a single peak
with a duration (T90) of about 0.4 s (50-300 keV).
The time-averaged spectrum from T0-0.256 s to T0+0.192 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.7 +/- 0.1 and
the cutoff energy, parameterized as Epeak, is 1148 +/- 291 keV

The event fluence (10-1000 keV) in this time interval is
(9.8 +/- 0.7)E-07 erg/cm^2. The 0.256-sec peak photon flux measured
starting from T0-0.064 s in the 10-1000 keV band
is 8.6 +/- 0.5 ph/s/cm^2.

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


GRB_name: GRB160509A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19532
SUBJECT: GRB 160509A: 15 GHz upper limits from AMI
DATE:    16/06/14 16:18:03 GMT
FROM:    Kunal Mooley at Oxford U  <kunal.mooley@physics.ox.ac.uk>

K. P. Mooley, T. D. Staley, R. P. Fender (Oxford), G. E. Anderson 
(Curtin), T. Cantwell (Manchester), C. Rumsey, D. Titterington, S. H. 
Carey, J. Hickish, Y. C. Perrott, N. Razavi-Ghods, P. Scott (Cambridge), 
K. Grainge, A. Scaife (Manchester)

We observed the Fermi/LAT GRB 160509A (Longo et al., GCN 19403) with the 
AMI Large Array at 15 GHz on 2016 May 23.25 and May 26.21 (UT) as part 
of the 4pisky program. We do not detect any source at the VLA location 
(Alexander et al., GCN 19414), with 3sigma upper limits of 137 uJy and 
152 uJy respectively.

We thank the AMI staff for scheduling these observations. The AMI-GRB 
database is a log of all GRB follow up observations with the AMI, and is 
available at http://4pisky.org/ami-grb/.


GRB_name: GRB160519A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19533
SUBJECT: GRB 160519A: 15 GHz upper limits from AMI
DATE:    16/06/14 16:18:09 GMT
FROM:    Kunal Mooley at Oxford U  <kunal.mooley@physics.ox.ac.uk>

K. P. Mooley, T. D. Staley, R. P. Fender (Oxford), G. E. Anderson 
(Curtin), T. Cantwell (Manchester), C. Rumsey, D. Titterington, S. H. 
Carey, J. Hickish, Y. C. Perrott, N. Razavi-Ghods, P. Scott (Cambridge), 
K. Grainge, A. Scaife (Manchester)

The AMI Large Array robotically triggered on the Swift alert for GRB 
160519A (D'Avanzo et al., GCN 19436) as part of the 4pisky program, and 
subsequent follow up observations were obtained up to 10 days 
post-burst. Our observations at 15 GHz on 2016 May 19.35, May 20.50, May 
22.61, May 26.50, and May 29.49 (UT) do not reveal any variable radio 
source within the BAT error circle (Stamatikos et al., GCN 19441), with 
3sigma upper limits of 202 uJy, 72 uJy, 84 uJy, 87 uJy, and 87 uJy 
respectively.

We thank the AMI staff for scheduling these observations. The AMI-GRB 
database is a log of all GRB follow up observations with the AMI, and is 
available at http://4pisky.org/ami-grb/.


GRB_name: GRB160521A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19534
SUBJECT: GRB 160521A: 15 GHz detections and upper limit from AMI
DATE:    16/06/14 16:24:06 GMT
FROM:    Kunal Mooley at Oxford U  <kunal.mooley@physics.ox.ac.uk>

K. P. Mooley, T. D. Staley, R. P. Fender (Oxford), G. E. Anderson 
(Curtin), T. Cantwell (Manchester), C. Rumsey, D. Titterington, S. H. 
Carey, J. Hickish, Y. C. Perrott, N. Razavi-Ghods, P. Scott (Cambridge), 
K. Grainge, A. Scaife (Manchester)

We observed the INTEGRAL/IBIS GRB 160521A (Mereghetti et al., GCN 19442) 
with the AMI Large Array at 15 GHz on 2016 May 24.62, May 27.52, and Jun 
03.61 (UT) as part of the 4pisky program. We detect a transient radio 
source (RA=08:38:51.3 +/-6 arcsec, Dec=+46:54:21 +/-24 arcsec) within 
the INTEGRAL error circle at 266+/-36 uJy and 133+/-29 uJy in the first 
two epochs, and obtain a 3sigma upper limit of 93 uJy in the third epoch.

We thank the AMI staff for scheduling these observations. The AMI-GRB 
database is a log of all GRB follow up observations with the AMI, and is 
available at http://4pisky.org/ami-grb/.


GRB_name: GRB160612A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19535
SUBJECT: IPN Triangulation of GRB 160612A (short/hard)
DATE:    16/06/14 16:35:30 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks, D. Svinkin,
and T. Cline on behalf of the Konus-Wind team,

K. Hurley, on behalf of the IPN,

V. Connaughton, M. S. Briggs, C. Meegan, V. Pelassa,
and A. Goldstein, on behalf of the Fermi GBM team,

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, and

S. Barthelmy, J. Cummings, N. Gehrels, H. Krimm, and D. Palmer,
on behalf of the Swift-BAT team, report:

The short-duration GRB 160612A (Burns et al., GCN Circ. 19531) has been
detected by Fermi (GBM), Konus-Wind, INTEGRAL (SPI-ACS), and Swift (BAT),
so far, at about 72768 s UT (20:12:48). The burst was outside the coded
field of view of the BAT.

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
 ---------------------------------------------
  RA(2000), deg                 Dec(2000), deg
 ---------------------------------------------
 Center:
  348.342 (23h 13m 22s) -25.181 (-25d 10' 51")
 Corners:
  348.982 (23h 15m 56s) -27.398 (-27d 23' 52")
  349.501 (23h 18m 00s) -27.279 (-27d 16' 45")
  347.719 (23h 10m 52s) -22.963 (-22d 57' 45")
  347.216 (23h 08m 52s) -23.074 (-23d 04' 27")
 ---------------------------------------------
The error box area is 2.18 sq. deg, and its maximum
dimension is 4.7 deg (the minimum one is 28 arcmin).
The Sun distance was about 102 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB160612_T72767/IPN/

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


GRB_name: GRB160612A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19536
SUBJECT: GRB 160612A: Swift ToO observations
DATE:    16/06/14 21:57:18 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a ToO observation of the Swift/BAT GRB 160612A. 
Automated analysis of the XRT data will be presented online at
http://www.swift.ac.uk/ToO_GRBs/00020665

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. These are
not necessarily related to the Swift/BAT event. Any X-ray source
considered to be a probable afterglow candidate will be reported via a 
GCN Circular after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).

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


GRB_name: GRB160612A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19537
SUBJECT: BAT detection and localization of GRB 160612A
DATE:    16/06/14 23:22:57 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. Y. Lien (GSFC/UMBC) and D. M. Palmer (LANL) 
report on behalf of the Swift Team:

At 20:12:48 UT on 2016-06-12, a number of gamma ray instruments, including
Swift-BAT, detected the short-hard GRB 160612A (Burns et al., GCN Circ. 19531).
BAT was slewing to a pre-planned target at that time, so it did not immediately
trigger.  However, ground analysis of the slew data reveals the GRB location
of RA, dec = 348.364, -25.375 which is
 RA(J2000) = 23h 13m 27s
 dec(J2000) = -25d 22' 30"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  This position is consistent with the IPN error box 
(Kozlova, GCN Circ 19535).  The lightcurve shows a short, complex peak
with a duration of T90 = 0.25 seconds and a peak count rate of 
~18,000 counts/s (15-350 keV)..

The time-averaged spectrum over the T90 interval is best fit by a
simple power-law model, with a photon index of 0.74+/-0.17
and a fluence in the 15-150 keV band of 1.16 +/- 0.12 x 10^-7
erg/cm^2.  All quoted errors are at the 90% confidence level

Swift ToO observations are underway (GCN 19536).


GRB_name: GRB160612A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19538
SUBJECT: GRB 160612A: Swift-XRT observations
DATE:    16/06/15 12:24:55 GMT
FROM:    Beatriz Mingo at U of Leicester,XRT  <bm188@le.ac.uk>

L.M. McCauley (PSU), K.L. Page (U. Leicester), B. Mingo (U. Leicester),
A.P. Beardmore (U. Leicester), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA),
A. Maselli  (INAF-IASFPA), J.A. Kennea (PSU), B. Sbarufatti
(INAF-OAB/PSU) and P.A. Evans (U. Leicester), S. R. Oates (U. Warwick)
report on behalf of the Swift-XRT and UVOT teams:

Swift-XRT has performed follow-up observations of the
Swift/BAT-detected burst GRB 160612A (Lien et al. GCN Circ. 19537),
collecting 985 s of Photon Counting (PC) mode data between T0+178.4 ks
and T0+179.4 ks. 

No X-ray sources have been detected inside or close to the Swift/BAT
error region. The 3-sigma upper limit in the field is 0.008 ct s^-1,
corresponding to a 0.3-10 keV observed flux of 3.1e-13 erg cm^-2 s^-1
(assuming a typical GRB spectrum).

The results of the XRT-team automatic analysis of the XRT observations,
including a position-specific upper limit calculator, are available at
http://www.swift.ac.uk/ToO_GRBs/00020665.

The UVOT did not detect an afterglow within the BAT error circle, down
to a magnitude of > 20.87 with an exposure of 978s in the w2 filter.

This circular is an official product of the Swift-XRT and UVOT teams.


GRB_name: GRB160612A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19539
SUBJECT: Konus-Wind observation of GRB 160612A
DATE:    16/06/15 13:59:33 GMT
FROM:    Anastasia Tsvetkova at Ioffe Institute  <tsvetkova@mail.ioffe.ru>

A. Tsvetkova, S. Golenetskii, R.Aptekar, D. Frederiks, P. Oleynik,
M. Ulanov, D. Svinkin, A. Lysenko, A. Kozlova and T. Cline
on behalf of the Konus-Wind team, report:

The short-duration, hard-spectrum GRB 160612A
(Fermi GBM detection: Burns, Meegan & Jenke, GCN 19531;
IPN triangulation: Kozlova et al., GCN 19535;
BAT detection and localization:  Lien & Palmer, GCN 19537)
triggered Konus-Wind at T0=72767.893 s UT (20:12:47.893).

The burst light curve shows a single pulse with a total duration of ~0.2 s.

As observed by Konus-Wind, the burst
had a fluence of 1.02(-0.13,+0.12)x10^-6 erg/cm2
and a 16-ms peak flux, measured from T0-0.074 s,
of 1.16(-0.26,+0.26)x10^-5 erg/cm2/s
(both in the 20 - 1000 keV energy range).

Since a major fraction of the burst counts was accumulated
before the trigger, the spectral analysis was performed using
the KW 3-channel light curve data.
Modeling the 3-channel time-integrated spectrum
(measured from T0-0.128 s to T0+0.064 s)
by the cutoff power law yields the following model parameters:
the photon index alpha=-0.54(-0.38,+0.53),
and the peak energy Ep=1.46(-0.62,+8.00) MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB160612_T72767/

All the quoted errors are at the 68% confidence level.
All the quoted values are preliminary.


GRB_name: GRB160622A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19547
SUBJECT: GRB 160622A: Swift detection of a possible short GRB or a new SGR
DATE:    16/06/22 02:38:47 GMT
FROM:    Caryl Gronwall at PSU/Swift-UVOT  <caryl@swift.psu.edu>

A. D'Ai (INAF-IASFPA), N. Gehrels (NASA/GSFC), C. Gronwall (PSU),
J. A. Kennea (PSU), A. Y. Lien (GSFC/UMBC),
F. E. Marshall (NASA/GSFC), A. Maselli (INAF-IASFPA),
T. Sakamoto (AGU) and M. H. Siegel (PSU) report on behalf of the Swift
Team:

At 02:03:13 UT, the Swift Burst Alert Telescope (BAT) triggered and
located possible GRB 160622A (trigger=700791).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 244.373, -51.045 which is 
   RA(J2000) = 16h 17m 30s
   Dec(J2000) = -51d 02' 41"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a short pulse
with a duration of about 0.1 sec.  The peak count rate
was ~4000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 02:04:44.8 UT, 91.1 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. 

UVOT took a finding chart exposure of 3 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. Because of the density of catalogued stars, further
analysis is required to report an upper limit for any afterglow in the
sub-image. Results from the list of sources generated on-board are not
available at this time. No correction has been made for the large, but
uncertain extinction expected. 

This source is at a low galactic latitude of -0.37 degrees and may be 
an SGR.  While the BAT lightcurve looks like a short GRB, it is not
dissimilar from an SGR.  We need the full  dataset to determine the
nature of this trigger. 

Burst Advocate for this burst is A. D'Ai (antonino.dai AT ifc.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: GRB160622A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19548
SUBJECT: BAT trigger 700791 (possible GRB 160622A) is SNR RCW 103
DATE:    16/06/22 14:20:36 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A. D'Ai(INAF-IASFPA), P.Evans (U. Leicester), N. Gehrels (NASA/GSFC), C. 
Gronwall (PSU), J. A. Kennea (PSU), A. Y. Lien (GSFC/UMBC), F. E. 
Marshall (NASA/GSFC), A. Maselli (INAF-IASFPA), T. Sakamoto (AGU) and M. 
H. Siegel (PSU) report on behalf of the Swift Team:

Swift has gathered 5.8 ks of WT mode data and 463 s of PC mode data on 
the field of the BAT trigger 700791 (= possible GRB 160622A, GCN 19547).

The XRT image is dominated by diffuse emission from the supernova 
remnant RCW 103 (Frank et al., ApJ, 2015, 810,113), with a bright 
central source at RA,Dec. = 244.40282,  -51.03916,  which is equivalent to:

RA (J2000) = 16h 17m 36.68s
Dec (J2000) = -51d 02' 21.0"

with an uncertainty of 3.5" (radius, 90% confidence). This is consistent 
with the catalogued X-ray source 3XMM J161736.1-510224. Analysis is 
complicated by the presence of the diffuse emission from the SNR, 
however the source count rate is ~2 ct/sec, with a flux of approximately 
9.1 (+2.0, -1.6) Ã— 10^-11 erg cm^-2 s^-1 (derived from a power-law 
spectrum with NH=7.0 (+3.6, -2.5)e21 cm^-2, and a photon index of 2.2 
(+/- 0.4). This is substantially above the 3XMM count rate of 2.567 (+/- 
0.020)e-12 erg cm^-2 s^-1.

Observations and analysis are ongoing.

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

[GCN OPS NOTE(22jun16): Per author's request, A.D'A's name was corrected,
and the missing minus sign for the sexagesimal form of the Dec value
was added.]


GRB_name: GRB160623A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19552
SUBJECT: GRB 160623A: Swift ToO observations
DATE:    16/06/23 16:11:17 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a ToO observation of the Fermi/LAT GRB 160623A. 
Automated analysis of the XRT data will be presented online at
http://www.swift.ac.uk/ToO_GRBs/00020666

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. These are
not necessarily related to the Fermi/LAT event. Any X-ray source
considered to be a probable afterglow candidate will be reported via a 
GCN Circular after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).

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


GRB_name: GRB160623A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19553
SUBJECT: GRB 160623A / Galactic transient: Fermi-LAT detection
DATE:    16/06/23 16:18:15 GMT
FROM:    Giacomo Vianello at SLAC  <giacomov@slac.stanford.edu>

G. Vianello (Stanford), F. Dirirsa (UJ), N. Omodei (Stanford), J. L.
Racusin (NASA/GSFC), M. Axelsson (KTH Stockholm), D.Kocevski
(NASA/GSFC)

report on behalf of the Fermi-LAT team:

At 05:00:34.23 UT on June, 23, 2016 Fermi-GBM triggered on GRB 160623A
(trigger 488350837 / 160623209).  This burst is also visible in the
Swift/BAT raw count rate light curve, during a slew with no event
capture (D. Palmer/Swift private communication).

As the source came into the field of view of Fermi-LAT 400 s later,
high-energy emission was detected at a position compatible with GRB
160623A.

The best LAT on-ground location is found to be

RA, Dec = 315.24, 42.27 deg (J2000)

with an error radius of 0.1 deg (90 % containment, statistical error only).

The source is very bright in the LAT, with a fading high-energy
emission detected up to approximately 12 ks after the trigger time. We
detect more than 15 photons above 1 GeV.

We note that the LAT position is close to the Galactic plane,
corresponding to (L,B) = (84.17, -2.69) deg. Given the large
uncertainty in the GBM localization, we cannot exclude at this stage
the possibility that the LAT transient is a Galactic transient
unrelated to the GBM GRB. However, as seen by the LAT, the transient
has spectral and temporal properties typical of a long GRB.

A Swift ToO has been requested for this burst.

The Fermi-LAT point of contact for this burst is Feraol Dirirsa
(fdirirsa@uj.ac.za)

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: GRB160623A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19554
SUBJECT: Konus-Wind observation of GRB 160623A
DATE:    16/06/23 17:25:59 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

D. Frederiks, S. Golenetskii, R.Aptekar, P. Oleynik, M. Ulanov,
D. Svinkin, A. Tsvetkova, A.Lysenko, A. Kozlova, and T. Cline,
on behalf of the Konus-Wind team, report:

The very bright, long-duration GRB 160623A
(Fermi-LAT detection: Vianello et al., GCN 19553)
triggered Konus-Wind at T0=17977.594 s UT (04:59:37.594).

The light curve shows a broad pulse in the interval
from ~T0-25 s to ~T0+30 s, followed by a weaker emission
lasting until ~T0+200 s.
The emission is seen up to ~15 MeV.

As observed by Konus-Wind, the burst had a fluence
of 6.6(-0.1,+0.1)x10^-4 erg/cm2, and a 64-ms peak flux,
measured from T0+9.920 s, of 1.27(-0.03,+0.03)x10^-4 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+38.912 s)
is best fit in the 50 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.05 (-0.03,+0.03),
the high energy photon index beta = -2.67 (-0.10,+0.08),
the peak energy Ep = 562 (-23,+23) keV,
chi2 = 107/88 dof.

The spectrum near the peak count rate (measured from T0+7.936
to T0+11.776 s) is best fit in the 50 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.88 (-0.05,+0.05),
the high energy photon index beta = -2.95 (-0.14,+0.11),
the peak energy Ep = 648 (-32,+33) keV,
chi2 = 104/88 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB160623_T11977/

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


GRB_name: GRB160623A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19555
SUBJECT: GRB 160623A: Fermi GBM detection/observation
DATE:    16/06/23 19:10:15 GMT
FROM:    Bagrat Mailyan at UAH  <bm0054@uah.edu>

B. Mailyan (UAH), K. Toelge (MPE) and O. Roberts (UCD)
report on behalf of the Fermi GBM Team:

"At 05:00:34.23 UT on 23 June 2016, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 160623A (trigger 488350838 / 160623209 ),
which was also detected by the LAT (G. Vianello et al. 2016, GCN 19553)
and Konus-Wind (D. Frederiks et al. 2016, GCN 19554).
The GBM on-ground location is consistent with the LAT position.

The angle from the Fermi LAT boresight at the GBM trigger time is 83
degrees.

The GRB was occulted by the Earth for a large part of its duration, and
the GBM trigger occurred ~50 s after the start of the GRB based on
the Konus-Wind lightcurve.
The GBM light curve consists of a single peak with a duration of about 50 s.
The time-averaged spectrum from T0-4.9 s to T0+32.8 s is
best fit by a power law function.  The power law index is -1.60 +/- 0.04.

The event fluence (10-1000 keV) in this time interval is
(5.598 +/- 0.369)E-06 erg/cm^2.

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


GRB_name: GRB160623A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19558
SUBJECT: GRB 160623A: Swift-XRT afterglow detection
DATE:    16/06/23 21:03:42 GMT
FROM:    Alessandro Maselli at INAF/IASF Palermo  <maselli@ifc.inaf.it>

B. Mingo (U. Leicester), A.P. Beardmore (U. Leicester), A. D'Ai
(INAF-IASFPA), A. Maselli  (INAF-IASFPA), A. Melandri (INAF-OAB), J.A.
Kennea (PSU), B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU) and P.A.
Evans (U. Leicester) report on behalf of the Swift-XRT team:

Swift-XRT has performed follow-up observations of the
Fermi/LAT-detected burst GRB 160623A (Vianello et al. GCN Circ. 19553),
collecting 1.9 ks of Photon Counting (PC) mode data between T0+40.3 ks
and T0+45.4 ks. 

Three uncatalogued X-ray sources are detected, of which one ("Source
1") is above the RASS limit, and is therefore likely the GRB afterglow.
 The position of this source is RA, Dec=315.2967, +42.2205 which is
equivalent to:

RA (J2000): 21:01:11.22
Dec(J2000): +42:13:13.7

with an uncertainty of 3.5 arcsec (radius, 90% confidence).  This
position is 2.5 arcmin from the Fermi/LAT position. 

The light curve can be modelled with a power-law decay with a decay
index of alpha=2.3 (+0.5, -1.4).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.79 (+0.21, -0.20). The
best-fitting absorption column is  1.69 (+0.32, -0.29) x 10^22 cm^-2,
in excess of the Galactic value of 7.2 x 10^21 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 6.3 x 10^-11 (1.1 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.69 (+0.32, -0.29) x 10^22 cm^-2
Galactic foreground: 7.2 x 10^21 cm^-2
Excess significance: 5.5 sigma
Photon index:      1.79 (+0.21, -0.20)

If the light curve continues to decay with a power-law decay index of
2.3, the count rate at T+24 hours will be 0.12 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 7.6 x
10^-12 (1.4 x 10^-11) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis of the likely afterglow
are at http://www.swift.ac.uk/ToO_GRBs/00020666/index_1.php.
The results of the full analysis of the XRT observations are available
at http://www.swift.ac.uk/ToO_GRBs/00020666.

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


GRB_name: GRB160623A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19559
SUBJECT: Swift detection of a dust-scattered halo around GRB 160623A
DATE:    16/06/23 23:43:24 GMT
FROM:    Giacomo Vianello at SLAC  <giacomov@slac.stanford.edu>

A. Tiengo (IUSS Pavia), G. Vianello (Stanford), P. Esposito (API/UVA),
R. Salvaterra (INAF/IASF Milano)

report on behalf of a larger collaboration:

GRB 160623A was detected by Fermi/LAT on 2016 June 23 (Vianello et al.
GCN Circ. 19553) and its X-ray afterglow was identified by Swift/XRT
(Maselli et al. GCN Circ. 19558).

The XRT observation started on 2016 June 23 at 16:11:43 UT (40.3 ks
after the Fermi trigger) and lasted until 17:37:24, collecting data in
PC mode for a net exposure time of approximately 1.9 ks.

This burst was exceptionally bright and located at low Galactic
latitude (b=-2.6). The total Galactic extinction towards the GRB is Av
= 4.1 according to Schlafly & Finkbeiner 2011, ApJ 737, 103, or 4.8
according to Schlegel et al. 1998, ApJ 500, 525.

A bright X-ray halo with radius of approximately 3.5 arcmin  is
clearly visible around the GRB. This halo is possibly composed by
multiple rings produced by dust clouds in our Galaxy that scatter the
GRB X-ray emission.

The observation is too short to detect confidently the expansion of
the halo. From the size of the halo and the time of the GRB, we derive
a distance of about 800 pc for the closest dust structure responsible
for the scattering.


GRB_name: GRB160624A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19560
SUBJECT: GRB 160624A: Swift detection of a short burst
DATE:    16/06/24 11:41:14 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

A. D'Ai (INAF-IASFPA), S. D. Barthelmy (GSFC), N. Gehrels (NASA/GSFC),
C. Gronwall (PSU), H. A. Krimm (CRESST/GSFC/USRA),
A. Y. Lien (GSFC/UMBC), F. E. Marshall (NASA/GSFC),
A. Maselli (INAF-IASFPA) and E. Troja (NASA/GSFC/UMCP) report on
behalf of the Swift Team:

At 11:27:01 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 160624A (trigger=701288).  Swift slewed immediately to the short burst. 
The BAT on-board calculated location is 
RA, Dec 330.203, +29.634 which is 
   RA(J2000)  =  22h 00m 49s
   Dec(J2000) = +29d 38' 02"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single spike
structure with a duration of about 0.25 sec.  The peak count rate
was ~7000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 11:28:15.0 UT, 73.7 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 330.19123, 29.64388 which is equivalent
to:
   RA(J2000)  = 22h 00m 45.90s
   Dec(J2000) = +29d 38' 38.0"
with an uncertainty of 3.9 arcseconds (radius, 90% containment). This
location is 51 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. No
spectrum from the promptly downlinked event data is yet available to
determine the column density. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 76 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
0.07. 

Burst Advocate for this burst is A. D'Ai (antonino.dai AT ifc.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: GRB160623A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19561
SUBJECT: GRB 160623A: Mondy optical observations
DATE:    16/06/24 11:59:19 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI), E. Mazaeva (IKI),  P. Minaev (IKI), E. Klunko 
(ISTP), A. Volnova (IKI),  I. Korobtsev (ISTP),  report on behalf of 
larger GRB follow-up collaboration:

We observed the field of the bright hard GRB 160623A initially reported 
by GBM and LAT (Vianello et al., GCN 19553; Mailyan et al., GCN 19555) 
and also observed by  Konus-Wind (Frederiks  et al., GCN 19554) and 
SPI-ACS/INTEGRAL  with AZT-33IK telescope of Sayan observatory (Mondy) 
starting on June, 23 (UT) 18:21:25.  We obtained several images in 
R-filter under good weather conditions and FWHM of about 1.6 arcsec.  At 
the edge of XRT error circle  (Mingo et al., GCN 19558) we detect a 
source which is not presented in USNO-B1.0 and not visible in  POSS2 
(any filter).  Coordinates of the source are (J2000) 21:01:11.57 
+42:13:15.8 with uncertainty of 0.7 arcsec. Preliminary photometry   is 
following

t-T0    Filter  Exp.   OT(?) Err
(mid, days)     (s)

0.56330  R      20*60  19.94 0.07
0.57720  R      20*60  19.94 0.07
0.59112  R      20*60  20.32 0.13

Photometry is based on nearby USNO-B1.0 star
USNO-B.1_id  R2
1322-0479855 15.22

Despite a hint of some decaying of the source it is unclear whether 
source is an afterglow of GRB 160623A.

A finding chart can be found in 
http://grb.rssi.ru/GRB160623A/GRB160623A_160623_Mondy.png
A light curve of SPI-ACS/INTEGRAL  can be found in 
http://grb.rssi.ru/GRB160623A/GRB160623A_spi-acs.png


GRB_name: GRB160624A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19562
SUBJECT: GRB 160624A: Prompt enhanced Swift-XRT position
DATE:    16/06/24 12:05:29 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 160624A, we find an
enhanced XRT position of the afterglow: RA, Dec: 330.1928, 29.6443
which is equivalent to:
   RA (J2000)  = 22 00 46.27
   Dec (J2000) = +29 38 39.4
with an uncertainty of 2.3 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/701288.

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: GRB160521B
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19563
SUBJECT: GRB 160521B: 15 GHz upper limits from AMI
DATE:    16/06/24 12:49:41 GMT
FROM:    Kunal Mooley at Oxford U  <kunal.mooley@physics.ox.ac.uk>

K. P. Mooley, T. D. Staley, R. P. Fender (Oxford), G. E. Anderson 
(Curtin), T. Cantwell (Manchester), C. Rumsey, D. Titterington, S. 
Carey, J. Hickish, Y. C. Perrott, N. Razavi-Ghods, P. Scott (Cambridge), 
K. Grainge, A. Scaife (Manchester)

We observed the Fermi/LAT GRB 160521B (Veres et al., GCN 19434) with the 
AMI Large Array at 15 GHz on 2016 May 24.75, May 27.65, and Jun 03.73 
(UT) as part of the 4pisky program. We do not detect any source at the 
XRT location (Page et al., GCN 19448), with 3sigma upper limits of 108 
uJy, 108 uJy, and 117 uJy respectively.

We thank the AMI staff for scheduling these observations. The AMI-GRB 
database is a log of all GRB follow up observations with the AMI, and is 
available at http://4pisky.org/ami-grb/.


GRB_name: GRB160525B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19564
SUBJECT: GRB 160525B: 15 GHz upper limits from AMI
DATE:    16/06/24 12:53:04 GMT
FROM:    Kunal Mooley at Oxford U  <kunal.mooley@physics.ox.ac.uk>

K. P. Mooley, T. D. Staley, R. P. Fender (Oxford), G. E. Anderson 
(Curtin), T. Cantwell (Manchester), C. Rumsey, D. Titterington, S. 
Carey, J. Hickish, Y. C. Perrott, N. Razavi-Ghods, P. Scott (Cambridge), 
K. Grainge, A. Scaife (Manchester)

The AMI Large Array robotically triggered on the Swift alert for GRB 
160525B (Krimm et al., GCN 19459) as part of the 4pisky program, and 
subsequent follow up observations were obtained up to 10 days 
post-burst. Our observations at 15 GHz on 2016 May 25.55, May 26.66, May 
28.66, and May 31.68 (UT) do not reveal any radio source at the XRT 
location (Beardmore et al., GCN 19463), with 3sigma upper limits of 99 
uJy, 63 uJy, 66 uJy, and 96 uJy respectively.

We thank the AMI staff for scheduling these observations. The AMI-GRB 
database is a log of all GRB follow up observations with the AMI, and is 
available at http://4pisky.org/ami-grb/.


GRB_name: GRB160624A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19565
SUBJECT: GRB160624A:possible GRB host redshift
DATE:    16/06/24 13:38:07 GMT
FROM:    Antonino Cucchiara at NASA/GSFC  <antonino.cucchiara@nasa.gov>

A. Cucchiara (STScI/GSFC) and A. J. Levan (U. Warwick)
report on behalf of a larger collaboration:

On June 24, 12:12:58 UT (~T+46min after the burst) we observed
the field of the Swift short GRB160624A (Dâ€™Ai  et al. GCN 19560, 
Evans et al. GCN 19562) with the GMOS-N camera mounted on the
Gemini North telescope.

In a 180s râ€™-band acquisition image a galaxy is identified 
within the enhanced XRT error circle. The galaxy is also visible 
in SDSS. We performed a 900s spectroscopic observation with the 
R400 grating covering the 3800-8100 Angstrom wavelength range.

The galaxy spectrum reveals emission features of [OIII]5007, 
H-beta and [OII]3727 at the common redshift of z=0.483.

We also obtained deeper râ€™ band imaging with the GMOS camera: no
other source is detected in the enhanced error circle down to 
a limiting magnitude of râ€™~25.5, although we are not sensitive to
possible faint point source superposed on the galaxy light.

We thank the Gemini staff for their extremely rapid
response, in particular Andrew Stephens.


GRB_name: GRB160624A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19566
SUBJECT: GRB 160624A: Enhanced Swift-XRT position
DATE:    16/06/24 15:42:50 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 371 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 160624A, 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 = 330.19271, +29.64373 which is equivalent
to:

RA (J2000): 22h 00m 46.25s
Dec (J2000): +29d 38' 37.4"

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: GRB160623A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19567
SUBJECT: GRB 160623A: RATIR Optical and NIR Observations, Afterglow Confirmation
DATE:    16/06/24 16:48:40 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), Ori Fox (STScI), J. Xavier
Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (GSFC/STScI),
Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC),
JosÃ© A. de Diego (UNAM), Leonid Georgiev (UNAM), JesÃºs GonzÃ¡lez (UNAM),
Carlos RomÃ¡n-ZÃºÃ±iga (UNAM), Neil Gehrels (GSFC), Harvey Moseley (GSFC),
John Capone (UMD), V. Zach Golkhou (ASU), and Vicki Toy (UMD) report:

We observed the field of GRB 160623A (Vianello, et al., GCN 19553) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio AstronÃ³mico Nacional on
Sierra San Pedro MÃ¡rtir from 2016/06 24.44 to 2016/06 24.47 UTC (29.48 to
30.31 hours after the BAT trigger), obtaining a total of 0.56 hours
exposure in the r and i bands and 0.23 hours exposure in the Z, Y, J, and H
bands.

For a source on the edge of the Swift-XRT error circle (Mingo, et al., GCN
19558), in comparison with the USNO-B1 and 2MASS catalogs, we obtain the
following detections:

  r = 21.12 +/- 0.05
  i = 19.77 +/- 0.02
  Z = 18.73 +/- 0.02
  Y = 18.41 +/- 0.02
  J = 17.46 +/- 0.01
  H = 16.93 +/- 0.01

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.  Comparing our images to the finder
chart reported by Pozanenko, et al. (GCN 19561), we believe this to be the
same optical source.  It has apparently faded by about 1 mag in r over the
~16 hours separating our observations.

The source is located at RA, Dec = 21:1:11.48, +42:13:14.6 (J2000,
+/-0.5").  Further observations are planned.

We thank the staff of the Observatorio AstronÃ³mico Nacional in San Pedro
MÃ¡rtir.


GRB_name: GRB160623A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19568
SUBJECT: GRB 160623A: Swift/UVOT Upper Limits
DATE:    16/06/24 19:31:52 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 160623A
40254 s after the LAT trigger (Vianello et al., GCN Circ. 19553).
No optical afterglow consistent with the XRT position (Mingo et al. GCN 
Circ. 19558) or the Mondy and RATIR position (Pozanenko et al. GCN Circ. 
19561; Butler et al. GCN Circ. 19567) 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 initial 
exposures are:

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

v                40657        51652         2859         >21.1
u                40254        51253         2008         >21.5

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 1.35 in the direction of the 
burst (Schlegel et al. 1998).


GRB_name: GRB160624A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19569
SUBJECT: GRB 160624A, Swift-BAT refined analysis
DATE:    16/06/24 19:38:17 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

T. N. Ukwatta (LANL), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
A. D'Ai (INAF-IASFPA), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU) (i.e. the Swift-BAT team):

Using the data set from T-240 to T+581 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 160624A (trigger #701288)
(D'Ai et al., GCN Circ. 19560).  The BAT ground-calculated position is
RA, Dec = 330.210, 29.667 deg which is
  RA(J2000)  =  22h 00m 50.5s
  Dec(J2000) = +29d 40' 02.4"
with an uncertainty of 2.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The mask-weighted light curve shows a single pulse that starts at ~T0,
peaks at ~T+0.1 s, and ends at ~T+0.3. T90 (15-350 keV) is 0.2 +- 0.1 sec
(estimated error including systematics).

The time-averaged spectrum from T+0.0 to T+0.3 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
0.57 +- 0.45.  The fluence in the 15-150 keV band is 4.0 +- 0.9 x 10^-8 erg/cm2.
The 1-sec peak photon flux measured from T-0.29 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/701288/BA/


GRB_name: GRB160624A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19570
SUBJECT: GRB 160624A: Fermi GBM observation
DATE:    16/06/24 20:19:03 GMT
FROM:    Eric Burns at U of Alabama  <eb0016@uah.edu>

R. Hamburg (UAH) and A. von Kienlin (MPE)
report on behalf of the Fermi GBM Team:

"At 11:27:01.35 UT on 24 June 2016, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 160624A (trigger 488460425 / 160624477),
which was also detected by the Swift (D'Ai et al. 2016, GCN 19560)
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 76
degrees.

The GBM light curve consists of a single peak
with a duration (T90) of about 0.4 s (50-300 keV).
The time-averaged spectrum from T0-0.064 s to T0+0.192 s is
well fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.40 +/- 0.28 and
the cutoff energy, parameterized as Epeak, is 841 +/- 358 keV.

The event fluence (10-1000 keV) in this time interval is
(5.2 +/- 0.5)E-07 erg/cm^2. The 0.064-sec peak photon flux measured
starting from T0+0.00 s in the 10-1000 keV band
is 6.4 +/- 1.3 ph/s/cm^2.

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


GRB_name: GRB160624A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19571
SUBJECT: GRB 160624A: MITSuME Ishigakijima upper limits
DATE:    16/06/25 01:40:48 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda (OAO, NAOJ),  H. Hanayama, T. Miyaji, J. Watanabe (IAO, NAOJ),
K. Yanagisawa (OAO, NAOJ), S.Nagayama (NAOJ), M. Yoshida (Hiroshima),
K. Ohta (Kyoto) and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME and OISTER collaboration:

We observed the field of GRB 151029A (D'Ai et al., GCNC 19560)
with the optical three color (g', Rc and Ic) CCD camera attached
to the Murikabushi 1m telescope of Ishigakijima Astronomical
Observatory.

The observation started on 2016-06-24 15:22:38 UT (~3.9h after
the burst). We did not find any new point source within the
enhanced XRT circle (Beardmore et al., GCNC 19566) in all the
three bands.

Three sigma upper limits of the OT are listed below.
We used GSC2.3 catalog for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'     Rc     Ic
-----------------------------------------------------
0.17131    15:33:41    1740.0   >20.5  >20.1  >19.3
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB160623A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19572
SUBJECT: GRB 160623A: MITSuME Ishigakijima Optical Observation
DATE:    16/06/25 02:37:27 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda (OAO, NAOJ),  H. Hanayama, T. Miyaji, J. Watanabe (IAO, NAOJ),
K. Yanagisawa (OAO, NAOJ), S.Nagayama (NAOJ), M. Yoshida (Hiroshima),
K. Ohta (Kyoto) and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME and OISTER collaboration:

We observed the field of GRB 160623A (Vianello et al., GCNC 19553;
Tiengo et al., GCNC 19559) with the optical three color
(g', Rc and Ic) CCD camera attached to the Murikabushi 1m telescope
of Ishigakijima Astronomical Observatory.

The observation started on 2016-06-23 15:14:25 UT (~10.2 h after
the burst). We detected the previously reported afterglow
(Pozanenko et al., GCNC 19561; Butler et al., GCNC 19567) in
Rc and Ic bands.

Three sigma upper limit and photometric results of the OT are
listed below. We used GSC2.3 catalog for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'    Rc   Rc_err  Ic   Ic_err
------------------------------------------------------------------
0.42989    15:19:37     540.0    >20.4  18.63 0.06   17.19 0.06
0.45924    16:01:53     480.0    >20.4  18.86 0.09   17.63 0.11
------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB160624A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19573
SUBJECT: GRB 160624A: Swift-XRT refined Analysis
DATE:    16/06/25 03:45:51 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), A. Maselli 
(INAF-IASFPA), A. Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB), B.
Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), T.G.R. Roegiers (PSU),
S.L. Gibson (U. Leicester) and A. D'Ai report on behalf of the
Swift-XRT team:

We have analysed 6.2 ks of XRT data for GRB 160624A (D'Ai et al. GCN
Circ. 19560), from 58 s to 45.7 ks after the  BAT trigger. The data
comprise 72 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. 19562).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=0.8 (+0.4, -0.5). At T+126 s  the decay
steepens to an alpha of 3.0 (+1.1, -0.8) before breaking again at T+217
s to a final decay with index alpha=6.7 (+1.3, -0.7).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.73 (+0.31, -0.29). The
best-fitting absorption column is  5.5 (+2.6, -2.2) x 10^21 cm^-2, in
excess of the Galactic value of 9.1 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.6 x 10^-11 (6.5 x 10^-11) erg
cm^-2 count^-1. 

A summary of the WT-mode spectrum is thus:
Total column:      5.5 (+2.6, -2.2) x 10^21 cm^-2
Galactic foreground: 9.1 x 10^20 cm^-2
Excess significance: 3.4 sigma
Photon index:      1.73 (+0.31, -0.29)

If the light curve continues to decay with a power-law decay index of
6.7, the count rate at T+24 hours will be 3.8 x 10^-18 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.7 x
10^-28 (2.4 x 10^-28) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00701288.

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


GRB_name: GRB160623A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19574
SUBJECT: GRB 160623A: TSHAO optical observations
DATE:    16/06/25 10:07:47 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), A. Kusakin (Fesenkov Astrophysical Institute), I. Reva 
(Fesenkov Astrophysical Institute), A. Volnova (IKI), A. Pozanenko (IKI) 
report on behalf of larger GRB follow-up collaboration:

We observed GRB 160623A  (Vianello et al., GCN 19553; Mailyan et al., 
GCN 19555; Frederiks  et al., GCN 19554) with Zeiss-1000 (East) 1-m 
telescopes of Tien Shan Astronomical Observatory. We obtained several 
images in R filter starting on June 24 (UT) 19:19:17. We detect optical 
transient associated with GRB 160623A (Pozanenko et al., GCN 19561; 
Butler  et al., GCN 19567).   Preliminary photometry of combined image 
is following

Date       UT start   t-T0    Filter  Exp.   OT     Err.  UL
                       (mid, days)     (s)

2016-06-24 19:19:17   1.62157 R       40*90 20.57   0.10  22.0

Photometry is based on nearby USNO-B1.0 star

USNO-B.1_id     R2
1322-0479881    15.12
1322-0479687    15.57
1322-0479855    15.22
1322-0479927    17.43
1322-0479987    17.39


GRB_name: GRB160624A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19575
SUBJECT: GRB 160624A: Lulin observation
DATE:    16/06/25 15:01:46 GMT
FROM:    Albert Kong at NTHU  <akhkong@gmail.com>

A.K.H. Kong (NTHU), M.Y. Lee, Y.-M. Lin (TFGHS), X. Hou (NTHU/YAO),
C.Y. Liu (NTHU)

We observed the field of GRB 160624A (D'Ai et al. GCN #19560) with the
1m telescope at the Lulin Observatory in Taiwan. We obtained a 600-s
image with the SDSS r-band filter on 2016 June 24, 17:32 UT (~ 6 hours
after the burst). Apart from the possible host galaxy that is also
seen in SDSS (Cucchiara et al. GCN #19565), no new point source was
detected at the enhanced XRT position (Beardmore et al. GCN #19566)
with r > 22.2 mag.


GRB_name: GRB160624A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19576
SUBJECT: GRB 160624A: Swift/UVOT Upper Limits
DATE:    16/06/25 16:26:56 GMT
FROM:    Massimiliano de Pasquale at IASF-Palermo  <m.depasquale@ucl.ac.uk>

M. De Pasquale (UCL-MSSL) and A. D'Ai (INAF-IASFPA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 160624A
77 s after the BAT trigger (D'Ai et al., GCN Circ. 19560).
No optical afterglow consistent with the XRT position
(Beardmore et al. GCN Circ. 19566) is detected in the initial
and summed UVOT exposures, nor at the position of the SDSS
galaxy mentioned by Cucchiara et al. (GCN Circ. 19565).
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            77          227          147         >20.8
u_FC               289          527          234         >20.0
white               77         6288          541         >21.5
v                 5060         6657          352         >19.5
b                 4445         6082          393         >20.7
u                  289        12622         1073         >20.7
w1                5471        11954         1082         >20.8
m2                5266        11048         1082         >20.7
w2                4855         6494          393         >20.3

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.07 in the direction of the burst
(Schlegel et al. 1998).

-- 

Dr. Massimiliano De Pasquale
Research associate - Swift UVOT scientist
Mullard Space Science Laboratory, University College London


GRB_name: GRB160625A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19577
SUBJECT: GRB 160625A: Swift detection of a burst
DATE:    16/06/25 22:56:43 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

A. Maselli (INAF-IASFPA), S. D. Barthelmy (GSFC),
A. D'Ai (INAF-IASFPA), N. Gehrels (NASA/GSFC), C. Gronwall (PSU),
A. Y. Lien (GSFC/UMBC), D. M. Palmer (LANL), J. L. Racusin (NASA/GSFC)
and T. N. Ukwatta (LANL) report on behalf of the Swift Team:

At 22:40:31 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 160625A (trigger=701503).  Swift did not slew to the burst due to
an observing constraint.  The BAT on-board calculated location is 
RA, Dec 176.937, -65.114, which is 
   RA(J2000)  =  11h 47m 45s
   Dec(J2000) = -65d 06' 49"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows several peaks in the first 
40 sec and then a large peak at T+170 sec
structure with a duration of at least 180 sec.  The peak count rate
was ~14000 counts/sec (15-350 keV), at ~175 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+20.3
minutes. There will be no XRT or UVOT data until this time. 

Burst Advocate for this burst is A. Maselli (maselli AT ifc.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: GRB160625A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19578
SUBJECT: GRB 160625A: Swift-XRT observations
DATE:    16/06/25 23:51:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

D.N. Burrows (PSU), J.A. Kennea (PSU), S. Campana (INAF-OAB), G.
Cusumano (INAF-IASF PA), 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 160625A at 23:02:36.8 UT,
1325.3 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source located at RA, Dec 176.91418,
-65.14362 which is equivalent to:
   RA(J2000)  = 11h 47m 39.40s
   Dec(J2000) = -65d 08' 37.0"
with an uncertainty of 5.8 arcseconds (radius, 90% containment). This
location is 112 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. No spectrum from the promptly downlinked
event data is yet available to determine the column density.


GRB_name: GRB160625A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19579
SUBJECT: GRB 160625A - two different events?
DATE:    16/06/26 00:01:31 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

D. A. Kann (TLS Tautenburg) speculates:

Swift just triggered on GRB 160625A (Swift Trigger 701503, Maselli et al.,
GCN #19577). They reported several rather small peaks followed by very
strong emission ca. three minutes later.

This burst is seen to be extremely powerful in INTEGRAL SPI ACS and CALET
GBM. It seems to have begun with a short spike at about the same time as
the Swift BAT trigger (Fermi GBM trigger 488587220).

Three minutes later, Fermi LAT sent out a flight position at:

RA = 308.267
Dec. = +6.900

with an error of 0.5 degrees.

This position differs very strongly from the Swift BAT position. (Dec. of
-65!)

Additionally, Swift BAT has recently slewed to the BAT position and found
a faint X-ray afterglow (Burrows et al., GCN 19578), which is in contrast
to the very bright one one would expect from the extreme burst seen by
INTEGRAL and CALET.

I suggest that these are two different events, with the bright GRB seen
through side of the Swift spacecraft.

The Fermi LAT position is affected by a relatively low amount of
extinction (E_(B-V)=0.1), in contrast to the Swift position (E_(B-V)=1.3).

I strongly urge observations of the LAT position by Swift to determine an
XRT position, and by optical observatories as well. Judging from the
INTEGRAL SPI ACS light curve, this GRB is of similar intensity to GRB
160623A.


GRB_name: GRB160625B
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19580
SUBJECT: GRB 160625B: Fermi-LAT detection of a bright burst 
DATE:    16/06/26 00:23:32 GMT
FROM:    Judith Racusin at GSFC  <judith.racusin@nasa.gov>

F. Dirirsa (U. Johannesburg), J. Racusin (NASA/GSFC), J. McEnery (NASA/GSFC), 
and R. Desiante (INFN Torino) report on behalf of the Fermi-LAT team:

At 22:43:24 on June 25, 2016, Fermi/LAT detected a sharp increase in the rate of 
high-energy photons, resulting in an onboard trigger on GRB 160625B.  Fermi/GBM 
triggered on this object two separate times (160625945/488587220, 
160625952/488587880), with emission evident between triggers, including the time 
at which LAT triggered.

Note that all of these triggers are distinct from the Swift/BAT trigger on GRB160625A 
(Maselli et al., GCN 19577) that occurred 15 seconds after the first GBM trigger, and 
was occulted by the Earth to Fermi at the time, and >100 degrees away on the sky.

The onboard location is:
RA, Dec = 308.3, +6.9  (J2000)

with an error radius of 0.5 deg (90% containment, systematic error only). 

This was 12.3 deg from the LAT boresight at the time of the LAT trigger. 

We anticipate providing a refined location within the next 8 hours when the LAT 
science data for this burst is downlinked and processed.

A Swift TOO request has been approved, and given the unusual nature of this trigger, 
a Fermi TOO will extended the pointed-mode observations to T0+24 hours beyond the 
initial autonomous repoint.

The Fermi-LAT point of contact for this burst is Feraol Dirirsa (fdirirsa@uj.ac.za).

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: GRB160625B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19581
SUBJECT: GRB 160625B: Fermi GBM initial observations
DATE:    16/06/26 00:53:38 GMT
FROM:    Eric Burns at U of Alabama  <eb0016@uah.edu>

E. Burns (UAH) reports on behalf of the Fermi GBM Team:

"At 22:40:16.28 UT on 25 June 2016, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 160625B for the first time
(trigger 488587220 / 160625945).

The trigger resulted in an Autonomous Repoint Request (ARR)
by the GBM Flight Software owing to the high peak flux of the GRB.
This ARR was accepted and the spacecraft slewed to the GBM in-flight
location. The initial angle from the Fermi LAT boresight to
the GBM ground location is 40 degrees.

At 22:43:24.82 the Fermi LAT triggered on a bright
pulse from the same GRB (Dirirsa et al. 2016, GCN 19580). Owing to
the ARR the initial angle from the Fermi LAT boresight to the
LAT position at LAT trigger time was 12 degrees.

At 22:51:16.03 GBM triggered again on GRB 160625B
(trigger 488587880 / 160625952).

GRB 160625B is distinct from the Swift BAT GRB 160625A
(Maselli et al. 2016, GCN 19577).

The GBM light curve consists of multiple peaks over
approximately 700 seconds. The first peak is soft with a
duration of about 1 second. The main peak, corresponding
to the LAT trigger, is about 25 seconds long and is very
hard. The peak that triggered GBM for the second time is
about 30 seconds long and soft.

Standard GBM temporal and spectral analysis is awaiting
downlink of the full dataset and will be reported when
available."


GRB_name: GRB160625B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19582
SUBJECT: GRB 160625B: Tiled Swift observations
DATE:    16/06/26 01:18:16 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a series of observations, tiled on the sky, of the
Fermi/LAT GRB 160625B. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00056

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the Fermi/LAT event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).

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


GRB_name: GRB160625A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19583
SUBJECT: GRB 160625A: Enhanced Swift-XRT position
DATE:    16/06/26 04:35:51 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 830 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 160625A, 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 = 176.91548, -65.14460 which is equivalent
to:

RA (J2000): 11h 47m 39.72s
Dec (J2000): -65d 08' 40.6"

with an uncertainty of 2.5 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: GRB160623A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19584
SUBJECT: GRB 160623A: SMA submm afterglow observations
DATE:    16/06/26 05:02:28 GMT
FROM:    Yuji Urata at Nat. Central U.  <urata@astro.ncu.edu.tw>

Yuji Urata (NCU/ASIAA), Kuiyun Huang (NTNU), and Glen Petitpas (SMA/SAO)
report:

We observed the GRB 160623A afterglow (Mingo et al. GCN 19558, Butler
et al. 19567) with Submillimeter Array (SMA) on 2016/06/24 (1.1 day
after the Fermi-GBM trigger) and 2016/06/25 (2.2 day).  The quick look
image at the 1st epoch shows the bright (~15 mJy) submm afterglow. The
source also shows a gradual fading at the 2nd epoch (corresponding
decay index of ~-0.4).

Further observation is ongoing.

We thank the staff of SMA.


GRB_name: GRB160625B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19585
SUBJECT: GRB 160625B: Swift-XRT afterglow detection
DATE:    16/06/26 06:54:13 GMT
FROM:    Antonino D'Ai at IASF-PA  <antonino.dai@ifc.inaf.it>

A. Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), D.N.
Burrows (PSU), T.G.R. Roegiers (PSU), L.M. McCauley (PSU), S.L. Gibson
(U. Leicester), J.P. Osborne (U. Leicester) and P.A. Evans (U.
Leicester) report on behalf of the Swift-XRT team:

Swift-XRT has performed follow-up observations of the
Fermi/LAT-detected burst GRB 160625B (Dirirsa et al. GCN Circ. 19580)
in a series of observations tiled on the sky. The total exposure time
is 2.7 ks, distributed over 8 tiles; the maximum exposure at a single
sky location was 1.1 ks. The data were collected between T0+9.6 ks and
T0+10.0 ks, and are entirely in Photon Counting (PC) mode. 

An uncatalogued X-ray source is detected and is above the RASS limit,
and is therefore likely the GRB afterglow.  The position of this source
is RA, Dec=308.5969, +6.9196 which is equivalent to:

RA (J2000): 20:34:23.25
Dec(J2000): +06:55:10.5

with an uncertainty of 3.8 arcsec (radius, 90% confidence).  This
position is 19.7 arcmin from the Fermi/LAT position. 

The light curve can be modelled with a power-law decay with a decay
index of alpha=3.156 (+0.011, -2.764).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.09 (+0.20, -0.19). The
best-fitting absorption column is  1.6 (+/-0.6) x 10^21 cm^-2, in
excess of the Galactic value of 9.8 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.1 x 10^-11 (4.3 x 10^-11) erg
cm^-2 count^-1. 

A summary of the WT-mode spectrum is thus:
Total column:      1.6 (+/-0.6) x 10^21 cm^-2
Galactic foreground: 9.8 x 10^20 cm^-2
Excess significance: 1.8 sigma
Photon index:      2.09 (+0.20, -0.19)

If the light curve continues to decay with a power-law decay index of
3.156, the count rate at T+24 hours will be 6.1 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.9 x
10^-13 (2.6 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis of the likely afterglow
are at http://www.swift.ac.uk/xrt_products/TILED_GRB00056/index_1.php.
The results of the full analysis of the tiled XRT observations are
available at http://www.swift.ac.uk/xrt_products/TILED_GRB00056.

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


GRB_name: GRB160625B
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19586
SUBJECT: GRB 160625B: Fermi-LAT refined analysis
DATE:    16/06/26 07:55:38 GMT
FROM:    Judith Racusin at GSFC  <judith.racusin@nasa.gov>

F. Dirirsa (U. Johannesburg), G. Vianello (Stanford), J. Racusin (NASA/GSFC), and
M. Axelsson (KTH Stockholm) report on behalf of the Fermi-LAT team:
We report the on-ground localization and analysis of GRB 160625B, which triggered 
the LAT onboard (Dirisa et al., GCN 19580).  All times are relative to the initial GBM 
trigger (Burns et al, GCN 19581).
The best LAT on-ground location is found to be:
RA, Dec = 308.56, 6.93 deg (J2000)
with an error radius of 0.06 deg (90 % containment, statistical error only). This is fully 
compatible with the position of the afterglow detected by Swift/XRT (Melandri et al., 
GCN 19585).
This was 42 deg from the LAT boresight at the time of the GBM trigger and triggered 
an autonomous repoint of the spacecraft.

More than 300 photons were detected above 100 MeV.  The LAT emission became 
detectable during the second bright pulse observed by GBM at ~T0+181 s.  The 
highest-energy photon is a 15 GeV event which is observed ~345 seconds after 
the GBM trigger.  The GRB was detectable by the LAT up to ~1 ks after the 
trigger.  Data are still being collected, and pointed mode observations are continuing 
to maximize exposure to the GRB location. 
The Fermi-LAT point of contact for this burst is Feraol Dirirsa (fdirirsa@uj.ac.za <mailto:fdirirsa@uj.ac.za>).
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: GRB160625B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19587
SUBJECT: GRB 160625B: Fermi GBM refined analysis
DATE:    16/06/26 08:01:15 GMT
FROM:    Eric Burns at U of Alabama  <eb0016@uah.edu>

E. Burns (UAH) reports on behalf of the Fermi GBM Team:

"We report temporal and spectral analysis on GRB 160625B, covering
all three Fermi trigger times (LAT trigger 488587408 / 160625947
GBM triggers 488587220 / 160625945 and 488587880 / 160625952).
All times are relative to the first GBM trigger time.

The GBM light curve consists of multiple peaks
with a total duration (T90) of about 460 s (50-300 keV).
The 1.024-sec peak photon flux of the main peak measured starting
from T0+188.707 s in the 10-1000 keV band is 167 +/- 1 ph/s/cm^2.

The soft peak that initially triggered GBM is about 1 second long.
The time-averaged spectrum from T0+0.002 s to T0+1.056 s is
well fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.2 +/- 0.1 and
the cutoff energy, parameterized as Epeak, is 68 +/- 1 keV.
The event fluence (10-1000 keV) in this time interval is
(1.65 +/- 0.03)E-06 erg/cm^2.

The main peak that triggered the LAT is about 25 seconds long.
The time-averaged spectrum from T0+187.427 s to T0+212.003 s is
well fit by a Band function with Epeak = 657 +/- 5 keV,
alpha = -0.74 +/- 0.00, and beta = 2.36 +/- 0.01.
The event fluence (10-1000 keV) in this time interval is
(5.00 +/- 0.01)E-04 erg/cm^2.

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


GRB_name: GRB160625B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19588
SUBJECT: GRB 160625B: RATIR Optical and NIR Afterglow Detection
DATE:    16/06/26 08:18:57 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),
Ori Fox (STScI), J. Xavier Prochaska (UCSC), Josh Bloom (UCB),
Antonino Cucchiara (GSFC/STScI), Owen Littlejohns (ASU),
Enrico Ramirez-Ruiz (UCSC), JosÃ© A. de Diego (UNAM), Leonid Georgiev
(UNAM), JesÃºs GonzÃ¡lez (UNAM), Carlos RomÃ¡n-ZÃºÃ±iga (UNAM), Neil
Gehrels (GSFC), Harvey Moseley (GSFC), John Capone (UMD), V. Zach
Golkhou (ASU), and Vicki Toy (UMD) report:

We observed the field of the Fermi LAT GRB 160625B (Dirirsa, et al., GCN 
19580)
with the Reionization and Transients Infrared Camera (RATIR; www.ratir.org)
on the 1.5m Harold Johnson Telescope at the Observatorio AstronÃ³mico 
Nacional
on Sierra San Pedro MÃ¡rtir from 2016/06 26.30 to 2016/06 26.32 UTC (8.53
to 9.02 hours after the LAT 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.

We detect a bright, fading and uncatalogued source at the edge of the 
Swift-XRT
error circle (Melandri, et al., GCN 19585), at a position RA, Dec = 
20:34:23.50,
+6:55:8.1 (J2000, +/-0.5"). In comparison with the USNO-B1 and 2MASS 
catalogs,
we obtain the following values:

   r    = 18.28 +/- 0.01
   i    = 18.08 +/- 0.01
   Z    = 17.95 +/- 0.01
   Y    = 17.78 +/- 0.01
   J    = 17.77 +/- 0.02
   H    = 17.65 +/- 0.02

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

Further observations are on-going.

We thank the staff of the Observatorio AstronÃ³mico Nacional in San Pedro
MÃ¡rtir.


GRB_name: GRB160625B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19589
SUBJECT: GRB 160625B: Swift/UVOT Detection
DATE:    16/06/26 11:15:45 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

GRB 160625B: Swift/UVOT Detection

S. R. Oates (U. Warwick) and A. D'A (INAF-IASFPA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 160625B
9616 s after the LAT trigger (Dirirsa et al., GCN Circ. 19580).
A source consistent with the RATIR position (Troja et al. GCN Circ. 19588)
and the edge of the XRT position (Melandri et al. GCN Circ. 19585)
is detected in the initial UVOT exposures.

Preliminary detections 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

u                 9616         9978          353         16.41 +/- 0.04

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: GRB160625A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19591
SUBJECT: GRB 160625A: Swift-XRT refined Analysis
DATE:    16/06/26 17:22:41 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), T.G.R.
Roegiers (PSU), L.M. McCauley (PSU), J.A. Kennea (PSU), S.L. Gibson (U.
Leicester), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester) and
A. Maselli report on behalf of the Swift-XRT team:

We have analysed 6.4 ks of XRT data for GRB 160625A (Maselli et al. GCN
Circ. 19577), from 1.3 ks to 48.7 ks after the BAT trigger. The data
comprise 1.7 ks 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. 19583).

The late-time light curve (from T0+7.4 ks) can be modelled with a
power-law decay with a decay index of alpha=0.71 (+0.31, -0.28).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.2 (+/-0.5). The
best-fitting absorption column is  2.2 (+0.9, -0.7) x 10^22 cm^-2, in
excess of the Galactic value of 1.0 x 10^22 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 5.8 x 10^-11 (1.6 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.2 (+0.9, -0.7) x 10^22 cm^-2
Galactic foreground: 1.0 x 10^22 cm^-2
Excess significance: 2.8 sigma
Photon index:      2.2 (+/-0.5)

If the light curve continues to decay with a power-law decay index of
0.71, the count rate at T+24 hours will be 9.8 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.7 x
10^-13 (1.6 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/00701503.

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


GRB_name: GRB160625A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19592
SUBJECT: GRB 160625A: Swift-BAT refined analysis
DATE:    16/06/26 17:23:45 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
A. Maselli (INAF-IASFPA), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+962 sec from the recent telemetry downlinks,
we report further analysis of BAT GRB 160625A (trigger #701503)
(Maselli, et al., GCN Circ. 19577).  The BAT ground-calculated position is
RA, Dec = 176.939, -65.142 deg, which is 
   RA(J2000)  =  11h 47m 45.3s 
   Dec(J2000) = -65d 08' 30.9" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 57%.
 
The mask-weighted light curve shows at least 7 peaks, the first starting
at ~T-35 sec, the brightest peak at ~T+36 sec, and the last peak ending at ~T+70 sec.
The peak mentioned in GCN Circ 19577 at T+170 sec is due to GRB 160625B (as suggested
by Kann, Circ 19579) and confirmed by our analysis.
T90 (15-350 keV) is 53.9 +- 3.1 sec (estimated error including systematics).
 
The time-averaged spectrum from T-15.04 to T+47.41 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.08 +- 0.07.  The fluence in the 15-150 keV band is 3.3 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+35.07 sec in the 15-150 keV band
is 3.0 +- 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/701503/BA/


GRB_name: GRB160625A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19593
SUBJECT: GRB 160625A: Swift/UVOT Upper Limits
DATE:    16/06/26 20:48:32 GMT
FROM:    Massimiliano de Pasquale at IASF-Palermo  <m.depasquale@ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 160625A
7183 s after the BAT trigger (Maselli et al., GCN Circ. 19577).
No optical afterglow consistent with the XRT position
(Burrows et al. GCN Circ. 19578) is detected in the UVOT exposures.
We note the presence of a source approximately 3'' from the
XRT position. This source is present in the USNO catalogue.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the
exposures are:

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

white             7183         7952          344         >20.8
v                 8163         8363          197         >19.0
b                 7548         7747          197         >19.9
u                 7342         7542          197         >19.4
m2                8368         8483          113         >18.9
w2                7958         8158          197         >19.6

The magnitudes in the table are not corrected for the substantial Galactic
extinction due to the reddening of E(B-V) = 1.51 in the direction of the
burst (Schlegel et al. 1998).

-- 

Dr. Massimiliano De Pasquale
Research associate - Swift UVOT scientist
Mullard Space Science Laboratory, University College London


GRB_name: GRB160620A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19594
SUBJECT: IPN Triangulation of GRB 160620A (short/hard)
DATE:    16/06/26 22:29:47 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

K. Hurley, on behalf of the IPN,

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

S. Golenetskii, R. Aptekar, D. Frederiks, D. Svinkin, A. Kozlova,
and T. Cline on behalf of the Konus-Wind team,

S. Barthelmy, J. Cummings, N. Gehrels, H. Krimm, and D. Palmer,
on behalf of the Swift-BAT team,

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, and

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

A short-duration GRB 160620A was detected by Konus-Wind, Swift (BAT), 
INTEGRAL (SPI-ACS), and Mars-Odyssey (HEND) at about 18373 s UT 
(05:06:13). The burst was outside the coded field of view of the BAT.

We have triangulated it to a preliminary, 3 sigma error box whose 
coordinates are:
   ---------------------------------------------
    RA(2000), deg                 Dec(2000), deg
   ---------------------------------------------
   Center:
    250.662 (16h 42m 39s) +30.321 (+30d 19' 15")
   Corners:
    251.505 (16h 46m 01s) +30.332 (+30d 19' 57")
    250.769 (16h 43m 04s) +30.603 (+30d 36' 11")
    249.821 (16h 39m 17s) +30.298 (+30d 17' 51")
    250.557 (16h 42m 14s) +30.038 (+30d 02' 18")
   ---------------------------------------------
The error box area is 1467 sq. arcmin, and its maximum
dimension is 1.454 deg (the minimum one is 28 arcmin).
The Sun distance was 123 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB160620_T18380/IPN/

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


GRB_name: GRB160623A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19597
SUBJECT: GRB 160623A CALET Gamma-Ray Burst Monitor detection
DATE:    16/06/27 01:26:43 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

K. Yamaoka (Nagoya U), A. Yoshida, T. Sakamoto, Y. Kawakubo, M. Moriyama, 
Y. Yamada (AGU), S. Nakahira (JAXA), I. Takahashi (IPMU), Y. Asaoka, S. Ozawa, 
S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), W. Ishizaki (ICRR), 
M. L. Cherry (LSU), S. Ricciarini (U of Florence) P. S. Marrocchesi (U of Siena) ,
and the CALET collaboration:

The long-duration GRB 160623A (Mailyan et al., GCN Circ. 19555; 
Vianello et al. GCN Circ. 19553; Mingo et al. GCN Circ. 19558; 
Frederiks et al. GCN Circ. 19554) triggered the CALET Gamma-ray 
Burst Monitor (CGBM) at 04:59:34.27 on 23 June 2016.   The burst signal 
was seen by all CGBM instruments.  

The light curve of the SGM shows a bright peak with several overlapping pulses.  
The emission starts at T0, peaks at T0+12 sec and ends at T0+40 sec.  
The T90 duration measured by the SGM data is 13.5 +- 0.6 sec (40-1000 keV).  
The light curve is available at 

http://cgbm.calet.jp/cgbm_trigger/flight/1150693129/

The CGBM data used in this analysis are provided by the Waseda CALET Operation Center 
located at the Waseda University.


GRB_name: GRB160625B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19599
SUBJECT: GRB 160625B: MITSuME Ishigakijima Optical Observation
DATE:    16/06/27 02:51:23 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda (OAO, NAOJ),  H. Hanayama, T. Miyaji, J. Watanabe (IAO, NAOJ),
K. Yanagisawa (OAO, NAOJ), S.Nagayama (NAOJ), M. Yoshida (Hiroshima),
K. Ohta (Kyoto) and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME and OISTER collaboration:

We observed the field of GRB 160625B (Dirirsa et al., GCNC 19580;
Melandri et al., GCNC 19585) with the optical three color (g', Rc
and Ic) CCD camera attached to the Murikabushi 1m telescope of
Ishigakijima Astronomical Observatory.

The observation started on 2016-06-26 14:03:44 UT (~15.3 h after
the burst). We detected the previously reported afterglow
(Troja et al., GCNC 19588) in in all the three bands.

The photometric results of the OT are listed below.
We used GSC2.3 catalog for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec] g'    g'_e  Rc    Rc_e  Ic    Ic_e
-------------------------------------------------------------------
0.64273    14:08:57     540.0   19.16 0.10  18.59 0.05  18.08 0.10
0.73075    16:15:41     540.0   19.27 0.08  18.78 0.06  18.28 0.08
-------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB160625B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19600
SUBJECT: GRB 160625B: VLT/X-shooter redshift
DATE:    16/06/27 09:50:38 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Xu (NAOC/CAS), D. Malesani (DARK/NBI), J. P. U. Fynbo (DARK/NBI), N. 
R. Tanvir (Univ. Leicester), A. J. Levan (Univ. Warwick), D. A. Perley 
(DARK/NBI), report on behalf of a larger collaboration:

We observed the optical afterglow of the Fermi GRB 160625B (Dirirsa et 
al., GCN 19580; Burns, GCN 19581; Troja et al., GCN 19588) with the ESO 
VLT UT2 (Kueyen) equipped with the X-shooter spectrograph. Observations 
started on 2016 June 27.19 UT (1.25 days after the Fermi trigger) and 
consisted of 4 spectra by 600 s each, covering the wavelength range 
3500-20000 AA.

The afterglow is well detected in the acquisition image with R ~ 19.1 +- 
0.3, where the large error is due to scatter in the USNO magnitudes used 
as reference, and the r versus R filter transformation.

The continuum trace is well detected in our exposures, down to ~3100 AA. 
The lack of any drop sets an upper limit to the redshift z < 1.55. A 
number of superimposed absorption features are visible; among others, we 
detect Mg I, Mg II, Fe II, C IV, Si IV, O I, Si II, Zn II, Al II, and Al 
III, all at a common redshift z = 1.406, which we conclude to be the 
redshift of GRB 160625B. We also detect an intervening Mg II absorption 
system at z = 1.319.

At z = 1.406, the fluence in the 10-1000 keV Fermi band (Burns, GCN 
19587) corresponds to an isotropic-equivalent energy of ~2.5*10^54 erg.

We acknowledge excellent support from the ESO observing staff in 
Paranal, in particular Juan Carlos Munoz, Elizabeth (Liz) Bartlett, 
Dimitri Gadotti and Francisco Caceres.


GRB_name: GRB160625B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19601
SUBJECT: GRB 160625B: TNG redshift confirmation
DATE:    16/06/27 09:51:06 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. DElia (INAF-OAR/ASI-ASDC), A. Melandri (INAF-OAB) and D. Malesani (DARK/NBI) report on behalf of the CIBO collaboration:

We observed the afterglow of GRB 160625B (Dirirsa et al., GCN 19580) with the TNG equipped with DOLORES and the LR-B grism. The spectrum was acquired on 2016-06-26 and covers the range between 3000 and 7800 AA. The observation consisted of 2400 s exposure, starting at 23:04:20.836 (24 hr after the trigger).

The optical counterpart is clearly detected in the acquisition images with a magnitude r = 19.0 +/- 0.3 at the position reported by Troja et al. (GCN 19588) and Oates and D'A (GCN 19589).

The spectrum shows a clear continuum. We detect absorption features consistent with Mg I, Mg II, Mn II and Fe II lines a redshift of z = 1.41 +/- 0.01, thus confirming the redshift reported by Xu et al. (GCN 19600).

We thanks the TNG staff for excellent support, in particular Luca di Fabrizio and Albar Garcia.


GRB_name: GRB160625B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19602
SUBJECT: GRB 160625B: RATIR Optical and NIR Observations 
DATE:    16/06/27 14:12:33 GMT
FROM:    Alan M. Watson at Instituto de Astronomia UNAM  <alan@astro.unam.mx>

Alan M. Watson (UNAM), Eleonora Troja (GSFC), Nat Butler (ASU),
Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer
(UNAM), Ori Fox (STScI), J. Xavier Prochaska (UCSC), Josh Bloom (UCB),
Antonino Cucchiara (GSFC/STScI), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), JosÃ© A. de Diego (UNAM), Leonid Georgiev (UNAM),
JesÃºs GonzÃ¡lez (UNAM), Carlos RomÃ¡n-ZÃºÃ±iga (UNAM), Neil Gehrels (GSFC),
Harvey Moseley (GSFC), John Capone (UMD), V. Zach Golkhou (ASU), and
Vicki Toy (UMD) report:

We observed the field of the Fermi LAT GRB 160625B (Dirirsa, et al., GCN
19580) with the Reionization and Transients Infrared Camera (RATIR;
www.ratir.org) on the 1.5m Harold Johnson Telescope at the Observatorio
AstronÃ³mico Nacional on Sierra San Pedro MÃ¡rtir from 2016/06 27.36 to
2016/06 27.47 UTC (33.89 to 36.56 hours after the BAT trigger),
obtaining a total of 1.73 hours exposure in the r and i bands and 0.73
hours exposure in the Z, Y, J, and H bands.

We detect the afterglow reported by Troja et al. (GCN Circ. 19588) and,
in comparison with the USNO-B1 and 2MASS catalogs, obtain the following
magnitudes:

  r = 19.63 +/- 0.01
  i = 19.52 +/- 0.01
  Z = 19.34 +/- 0.02
  Y = 19.17 +/- 0.02
  J = 19.11 +/- 0.02
  H = 18.98 +/- 0.03

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

The afterglow has faded by about 1.20 magnitude in all bands compared to
our earlier epoch, confirming the fading seen during the first epoch.
The fading is consistent with a temporal index of -0.90.

More observations are planned.

We thank the staff of the Observatorio AstronÃ³mico Nacional in San Pedro
MÃ¡rtir.

[GCN OPS NOTE(27jun16): Per author's request, the GRB name in the Title
was changed from "A" to "B".  The name in the text was/is correct.]


GRB_name: GRB160625B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19603
SUBJECT: GRB 160625B: Mini-MegaTORTORA detection of bright optical flash simultaneous with LAT event
DATE:    16/06/27 15:37:31 GMT
FROM:    Sergey Karpov at SAO RAS  <karpov@sao.ru>

S.Karpov, G.Beskin (SAO RAS and Kazan Federal University, Russia), S.Bondar,
E.Ivanov, E.Katkova, N.Orekhova, A.Perkov (OJS RPC PSI, Russia), A.Biryukov
(SAI MSU and Kazan Federal University, Russia), V.Sasyuk (Kazan Federal
University, Russia)

The on-sky position of GRB 160625B (Dirirsa et al., GCN Circ. 19580) has
been observed by Mini-MegaTORTORA nine-channel wide-field monitoring system
 with high temporal resolution (http://mmt.favor2.info) before, during and
just after the LAT trigger time (T0 = 2016-06-25 22:43:24).

Mini-MegaTORTORA reacted to Fermi GBM trigger 488587220 and started
observing its error box at 2016-06-25 22:41:07, 52 seconds after GBM
trigger and 136 seconds before LAT trigger. Due to large size of error box,
the observations have been performed in "widefield+deep" regime, with
channels simultaneously covering ~30x30 deg field of view with 30 s
exposures in white light to achieve deepest detection limit. The system
acquired 20 frames in such regime, covering time interval from T0-136 to
T0+466 s.

The system detected a bright optical flash on a frame coincident with LAT
trigger time (T0-15.9 - T0+14.1 s) at position reported by Troja et al.
(GCN Circ. 19588), with a magnitude of about V=8.8 mag. Next frame
displayed a slight rebrightening of about 0.1 mag, and then the light curve
followed nearly  smooth power-law decay  with slope of about -1.6, down to
V=12.2 at last acquired frame. The images acquired prior to LAT trigger do
not display any object at that position down to about V=13.5 mag.

The system also reacted to second GBM trigger 488587880 with slightly
different coordinates, and due to large field of view again covered the
position of a transient, acquiring 20 more frames from T0+1691 to T0+2264
s. No object is seen in these frames down to about V=13.5 mag.

Snapshots of a frames from first follow-up (20 arcmin fields around the
transient) is available at
http://vo.astronet.ru/~karpov/grb160625b_mosaic.png

Further analysis and calibration of the data is ongoing.

Mini-MegaTORTORA belongs to Kazan Federal University and is located at
Special Astrophysical Observatory near Russian 6-m telescope.


GRB_name: GRB160625B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19604
SUBJECT: Konus-Wind observation of GRB 160625B
DATE:    16/06/27 16:30:09 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, P. Oleynik,
M. Ulanov,  A. Tsvetkova, A. Lysenko, A. Kozlova, and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration, extremely bright GRB 160625B
(Fermi-LAT detection: Dirirsa et al., GCN Circ. 19580;
Fermi-GBM detection: Burns, GCN Circ. 19581)
triggered Konus-Wind at T0=81619.875 s UT (22:40:19.875).

The burst light curve starts, at ~T0-0.3 s, with a short soft
initial pulse (precursor) which had a duration of about 1 s.
The precursor is followed, starting at ~T0+180 s, by the main, extremely 
bright and spectrally-hard episode with a duration of
about 40 s. This episode evolves into a weak emission traceable
up to ~T0+680 s.
The emission in the main episode is seen up to ~20 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB160625_T81619/

As observed by Konus-Wind, the burst
had a fluence of 9.44(-0.16,+0.16)x10^-4 erg/cm2,
and a 256-ms peak flux, measured from T0+188.928 s,
of 1.26(-0.10,+0.10)x10^-4 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the initial pulse
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 1 MeV range
by a simple power law model with
the photon index alpha = -2.34(-0.22,+0.25)
(chi2 = 38/61 dof)

The time-averaged spectrum of the main episode
(measured from T0+180.480 to T0+229.632 s)
is best fit in the 20 keV - 20 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.79(-0.02,+0.02),
the high energy photon index beta = -2.25(-0.04,+0.04),
the peak energy Ep = 554(-19,+20) keV
(chi2 = 353/97 dof)

The spectrum near the maximum count rate
(measured from T0+188.928 to T0+189.184 s)
is best fit in the 20 keV - 20 MeV range
by the Band model with the following parameters:
the low-energy photon index alpha = -0.77(-0.08,+0.10),
the high energy photon index beta = -2.22(-0.25,+0.17),
the peak energy Ep = 937(-179,+195) keV
(chi2 = 62/67 dof)

Assuming the redshift z=1.406 (Xu, et al., GCN Circ. 19600)
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:
the isotropic energy release E_iso is ~5.0x10^54 erg,
the peak luminosity L_iso is ~1.6x10^54 erg/s,
and the rest-frame peak energy of the time-integrated spectrum,
Ep,i, is ~1.3 MeV.

This Eiso is the highest one measured by Konus-Wind for
more than 21 years of its GRB observations and, probably,
the highest Eiso recorded for a GRB ever.

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


GRB_name: GRB160625B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19605
SUBJECT: GRB 160625B: TSHAO optical observations
DATE:    16/06/27 19:59:50 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), A. Kusakin (Fesenkov Astrophysical Institute), P. 
Minaev (IKI), I. Reva (Fesenkov Astrophysical Institute), A. Volnova 
(IKI), A. Pozanenko (IKI) report on behalf of larger GRB follow-up 
collaboration:

We observed the field of GRB 160625B (Dirirsa et al., GCN 19580; Burns 
et al. GCN 19581) with Zeiss-1000 (East) 1-m telescopes of Tien Shan 
Astronomical Observatory. We obtained several images in R filter 
starting on June 26 (UT) 19:39:18. We detect optical afterglow of  GRB 
160625B (Troja et al., GCN 19588; Oates  et al., GCN  19589). 
Preliminary photometry of a combined image is following

Date       UT start   t-T0    Filter  Exp.   OT     Err.  UL
                       (mid, days)     (s)

2016-06-26 19:39:18   0.91784 R       50*120 19.07  0.05  22.0

Photometry is based on nearby USNO-B1.0 stars
USNO-B.1_id  R2
0969-0608423 16.38
0969-0608416 16.28
0969-0608335 15.00
0969-0608366 16.05
0969-0608449 17.38
0969-0608443 16.78
0969-0608456 16.79

The GRB 160625B triggered Fermi LAT and GBM (Dirirsa et al., GCN 19580; 
Burns et al. GCN 19581), Konus-Wind (Svinkin et al. GCN 19604) and  D. 
Kann (GCN 19579) reported about CALET and SPI-ACS/INTEGRAL trigger.

A light curve of SPI-ACS/INTEGRAL  can be found in
http://grb.rssi.ru/GRB160625B/GRB160625B_API-ACS.png

The SPI-ACS time profile of  GRB 160625B consists of 3 episodes of total 
duration about 750 seconds and compatible with time profiles reported by 
GBM (Burns, GCN 19581) and Konus-Wind (Svinkin et al. GCN 19604).


GRB_name: GRB160625B
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19606
SUBJECT: GRB 160625B: VLA Detection
DATE:    16/06/27 20:43:24 GMT
FROM:    Kate Alexander at Harvard  <kalexander@cfa.harvard.edu>

K. D. Alexander (Harvard), T. Laskar (NRAO / UC Berkeley), W. Fong
(University of Arizona) and E. Berger (Harvard) report on behalf of a
larger collaboration:

We observed the Fermi/LAT GRB 160625B (Diririsa et al., GCN 19580) at
multiple frequencies with the Karl G. Jansky Very Large Array (VLA)
beginning 2016 June 27.28 UT (1.34 days after the burst). At a mean
frequency of 9.8 GHz, we detect a radio source with a preliminary flux
density of ~400 uJy at

RA (J2000) = 20:34:23.507 +/- 0.003
Dec (J2000) = +06:55:07.89 +/- 0.03

consistent with the position of the optical afterglow (Troja et al., GCN
19588; Oates et al., GCN 19589) and the Swift/XRT position (Melandri et
al., GCN 19585). Follow-up observations are planned.

We thank the VLA staff for rapidly executing these observations.


GRB_name: GRB160601A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19608
SUBJECT: GRB 160601A: 15 GHz upper limits from AMI
DATE:    16/06/28 13:09:02 GMT
FROM:    Kunal Mooley at Oxford U  <kunal.mooley@physics.ox.ac.uk>

K. P. Mooley, T. D. Staley, R. P. Fender (Oxford), G. E. Anderson 
(Curtin), T. Cantwell (Manchester), C. Rumsey, D. Titterington, S. 
Carey, J. Hickish, Y. C. Perrott, N. Razavi-Ghods, P. Scott (Cambridge), 
K. Grainge, A. Scaife (Manchester)

The AMI Large Array robotically triggered on the Swift alert for GRB 
160601A (Kocevski et al., GCN 19478) as part of the 4pisky program, and 
subsequent follow up observations were obtained up to 10 days 
post-burst. Our observations at 15 GHz on 2016 Jun 01.78, Jun 02.95, Jun 
04.95, and Jun 11.95 (UT) do not reveal any radio source at the XRT 
location (Evans et al., GCN 19484), with 3sigma upper limits of 282 uJy, 
216 uJy, 108 uJy, and 132 uJy respectively.

We thank the AMI staff for scheduling these observations. The AMI-GRB 
database is a log of all GRB follow up observations with the AMI, and is 
available at http://4pisky.org/ami-grb/.


GRB_name: GRB160623A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19609
SUBJECT: GRB 160623A: Possible detection of a radio afterglow at 15 GHz with AMI
DATE:    16/06/28 13:14:00 GMT
FROM:    Kunal Mooley at Oxford U  <kunal.mooley@physics.ox.ac.uk>

K. P. Mooley, T. D. Staley, R. P. Fender (Oxford), G. E. Anderson 
(Curtin), T. Cantwell (Manchester), C. Rumsey, D. Titterington, S. H. 
Carey, J. Hickish, Y. C. Perrott, N. Razavi-Ghods, P. Scott (Cambridge), 
K. Grainge, A. Scaife (Manchester)

We observed the Fermi/LAT GRB 160623A (Vianello et al., GCN 19553) with 
the AMI Large Array at 15 GHz on 2016 Jun 25.15 and Jun 27.15 (UT), 2.0 
and 4.0 days post-burst, as part of the 4pisky program. We detect an 
uncataloged variable radio source at the XRT location (Mingo et al., GCN 
19558) at 5.0+/-0.1 mJy and 6.3+/-0.1 mJy (preliminary) respectively.

Monitoring of this source is underway. We thank the AMI staff for 
scheduling these observations. The AMI-GRB database is a log of all GRB 
follow up observations with the AMI, and is available at 
http://4pisky.org/ami-grb/.


GRB_name: GRB160625B
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19610
SUBJECT: GRB 160625B: 15 GHz detection from AMI
DATE:    16/06/28 13:15:59 GMT
FROM:    Kunal Mooley at Oxford U  <kunal.mooley@physics.ox.ac.uk>

K. P. Mooley, T. D. Staley, R. P. Fender (Oxford), G. E. Anderson 
(Curtin), T. Cantwell (Manchester), C. Rumsey, D. Titterington, S. H. 
Carey, J. Hickish, Y. C. Perrott, N. Razavi-Ghods, P. Scott (Cambridge), 
K. Grainge, A. Scaife (Manchester)

We observed the Fermi/LAT GRB 160625B (Dirirsa et al., GCN 19580) with 
the AMI Large Array at 15 GHz on 2016 Jun 28.06 (UT), 2.1 days 
post-burst, as part of the 4pisky program. We detect a radio source 
consistent with the VLA location (Alexander et al., GCN 19606) at 
640+/-40 uJy.

Monitoring of this source is underway. We thank the AMI staff for 
scheduling these observations. The AMI-GRB database is a log of all GRB 
follow up observations with the AMI, and is available at 
http://4pisky.org/ami-grb/.


GRB_name: GRB160625B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19611
SUBJECT: GRB 160625B: SAO RAS optical observations
DATE:    16/06/28 14:00:13 GMT
FROM:    Moskvitin Alexander at SAO RAS  <mosk@sao.ru>

A. Moskvitin (SAO RAS, Russia) report on behalf of the larger team.

After fruitful multiband observations of the GRB 160625B optical
counterpart by several telescopes including Mini-MegaTORTORA
system located at SAO RAS (Karpov et al. GCNC #19603)
we observed the GRB160625B field (Dirirsa et al. GCNC #19580)
with the 1-meter telescope Zeiss-1000 of SAO RAS on June, 27.923
(1.976 days after the trigger). 7 x 300 sec. images in Rc band
were obtained under good weather conditions.

The OT is clearly visible in separate frames and in the stacked frame.
It's position is perfectly consistent with the coordinates reported by
Troja et al. (GCNC #19588) and Alexander et al. (GCNC #19606).
During our observations the OT magnitude was R = 19.87 +/- 0.07.
This estimation is based on the R2 magnitudes of nearby USNO-B1 stars,
without any correction for the Galactic extinction in the GRB direction.
The finding chart can be found at
ftp://ftp.sao.ru/pub/grb/GRB160625B/GRB160625B_z1000.jpg


GRB_name: GRB160625B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19612
SUBJECT: GRB 160625B: Global MASTER-Net prompt optical emission detection  
DATE:    16/06/28 14:05:38 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

E. Gorbovskoy, V. Lipunov, N.Tyurina, V.Kornilov,
P.Balanutsa,  A.Kuznetsov, D.Kuvshinov,
Lomonosov Moscow State University, Sternberg Astronomical Institute

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
The Instituto de Astrofisica de Canarias

D.Buckley, S. Potter, A.Kniazev, M.Kotze
South African Astronomical Observatory

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

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

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

Ricardo Podesta, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)

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

MASTER-IAC  robotic telescope (MASTER-Net: http://observ.pereplet.ru)
was pointed to the  GRB 160625B (Burns et al., GCN19581) 31 sec after GBM
notice time   and  57 sec after GBM trigger (131 sec before LAT Trigger, 
Dirirsa et al., GCN 19580)    at 2016-06-25 22:41:13UT .

Starting from this time we continiously observed Swift X-ray 
error box (Melandri et al., GCN 19585) by MASTER-IAC wide field camera 
with 5 sec unfiltered exposition. We have several thousands frames.
The OT appears at 22 43 30 (+- 2.5 sec) UT and rised to  maximum ~8 mag 
after  ~5 sec  at RATIR position (Troja et al., GCN 19588).

The prompt optical emission strongly correlated with Konus Wind gamma ray 
light curve ( Svinkin et al., GCN 19604 ).

MASTER-IAC  robotic telescope  started OT error box observation 43 
sec after  LAT notice time and 95 sec after trigger time at 2016-06-25 22:44:59
in two polarisations. The OT was about ~ 9.7 mag at this moment ( 0.2B + 
0.8R with respect  to USNOB1.0 stars)

The delay with publication connected with installation new MASTER 
telescope at Argentina (http://master.sai.msu.ru/masternet/).


The message may be cited.


GRB_name: GRB160623A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19614
SUBJECT: GRB 160623A: SAO RAS optical observations
DATE:    16/06/28 17:39:34 GMT
FROM:    Moskvitin Alexander at SAO RAS  <mosk@sao.ru>

A. Moskvitin (SAO RAS, Russia) report on behalf of the larger team.

We observed the field of GRB160623A (Vianello et al., GCNC #19553;
Mailyan et al., GCNC #19555) with the 1-meter telescope Zeiss-1000
of SAO RAS on June, 27.884 (4.676 days after the trigger).
A set of 8 x 300 sec. frames in Rc band were obtained.

The OT (coordinates reported by Pozanenko et al., GCNC #19561)
is clearly visible in the stacked image as the object
with the brightness R = 21.7 +/- 0.2. This estimation is based
on the USNO-B1 stars described by Mazaeva et al. (GCNC #19574).
The finding chart can be found at
ftp://ftp.sao.ru/pub/grb/GRB160623A/GRB160623A_z1000.jpg


GRB_name: GRB160625B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19615
SUBJECT: Pi of the Sky detection of an optical flash accompanying GRB 160625B
DATE:    16/06/28 19:34:52 GMT
FROM:    Lech Wiktor Piotrowski at U Warsaw  <lewhoo@fuw.edu.pl>

T. Batsch, A.J. Castro-Tirado, R. Cunniffe, H. Czyrkowski, A. Ä†wiek, M. Ä†wiok, R. DÄ…browski,
M. JelÃ­nek, G. Kasprowicz, A.Majcher, K. MaÅ‚ek, L. Mankiewicz, K. Nawrocki, Å. Obara,
R. Opiela, M. Siudek, M. SokoÅ‚owski, L. W. Piotrowski, R. Wawrzaszek, G. Wrochna,
A ZadroÅ¼ny, M. Zaremba, A.F. Å»arnecki (Pi of the Sky Collaboration)

Following GCN 19603 we present the reconstructed light curve of GRB 160625B.
One of four Pi of the Sky North detectors located at INTA - El Arenosillo
observatory in MazagÃ³n near Huelva, Spain imaged the region of GRB 160625B
(Swift-XRT error circle (Melandri, et al., GCN 19585), at a position RA, Dec =
20:34:23.50, +6:55:8.1) before, during and after the GRB with 10s exposures
(the exposures were taken in white light, IR-cut and UV-cut filters only,
to achieve deepest detection limit).

Cameras of the Pi of the Sky North observatory were observing the position of the GRB160625B
48s after Fermi GBM trigger 488587220 time (Jun 25 22:40:16.28 UT) 140 seconds 
before the LAT 488587408 trigger (Jun 25 22:43:24.82 UT). We observed optical emission
at the position given by Swift XRT recording a bright light curve starting -5.9 s 
before the LAT trigger. The first 10 s exposure shows initial magnitude of ~9.18 (unfiltered)
brightening to ~8.04 on the second exposure, than becoming gradually dimmer. 
It is important to note that both cameras, 35 and 39, identified a new object
on exposures starting just  before the time of the trigger. Below we give the light curve of 
GRB 160625B separately for two cameras:

For camera id = 35

t - t0            MagV           ErrV
-5.90351900 9.17858000 0.01979590
7.30034010 8.04185240 0.00692530
20.50411000 8.85256720 0.01464740
33.70891000 9.16411390 0.01958250
46.91391000 9.35221170 0.02310580
60.12562000 9.48356820 0.02605830
73.33060000 9.76273220 0.03348310
86.53484000 9.88869010 0.03764580
110.75906000 10.36167800 0.05831040
123.96549000 10.36315500 0.05835510
137.17366000 10.65792100 0.07717340
150.37855000 10.78365300 0.08672800
163.58296000 10.90103300 0.09643880
176.79191000 11.10503700 0.11532510
190.00141000 11.27645400 0.13539200
203.20498000 11.43088800 0.15646540
216.40969000 11.52125300 0.16944510
229.59719000 11.66219300 0.19535900
242.80196000 11.97388500 0.26215110
255.98556000 11.44272600 0.15893520
269.18835000 12.22780400 0.33061590
282.39288000 11.70644300 0.20138410
295.59737000 12.10355100 0.29637090
308.80171000 12.01954200 0.27279960
348.41412000 12.14943500 0.30407830
388.02095000 12.20940300 0.32526530

For camera id = 39

t-t0               MagV            ErrV
-0.21738000 8.08332450 0.00848860
15.13208000 8.39624730 0.01125160
30.48032000 9.30388780 0.02600590
45.83497000 9.38090950 0.02766380
61.69324000 9.60060770 0.03356240
77.04026000 9.76118030 0.03894990
92.38808000 10.00068600 0.04923380
107.71683000 10.23761200 0.05958340
123.06963000 10.43917000 0.07335490
138.42439000 10.63567700 0.08856020
153.77331000 10.78614800 0.10097800
169.12145000 10.99128200 0.12175100
184.46995000 11.23445500 0.15126550
199.82483000 11.04686000 0.12786780
215.17292000 11.27135000 0.15866670
232.56505000 11.47398300 0.19109480
247.89472000 11.99905600 0.31466480
263.75136000 11.78799000 0.25153010
279.09823000 12.08530200 0.33607390
294.44611000 11.95412600 0.30025650
325.14680000 12.14188100 0.35312590
432.59537000 12.18551500 0.36922680

Indicated errors are statistical only. Estimated systematic uncertainty of the image calibration is around 0.06-0.08 mag.

T0 is the Fermi GBM trigger 488587408 time (Jun 25 22:43:24.82 UT) and t is the time of shutter oppening. Each image taken covers approximately 400 square degrees. The 
magnitudo limit was about 12.5 mag.

Pi of the Sky observations are performed in wide visible band, with IR-cut and UV-cut filters only. We calibrate our observations to the reference stars from Tycho 2 using 
the transformation from Tycho to Pi of the Sky system given by:

VPi =  VT + 0.235313 - 0.292266*(BT - VT)

Due to the proximity of the burst to the edge of our FoV, the transient was not detected automatically. However, this allowed us to record it with two cameras, with 
exposures slightly shifted in time.

The light curve is available at:  http://grb.fuw.edu.pl/results/gamma-ray-bursts/grb160625b/.
More information will be published at http://grb.fuw.edu.pl and  http://grb.fuw.edu.pl/results/gamma-ray-bursts/grb160625b/

[GCN OPS NOTE(04jul16): Per author's request, the GRB name in the 2nd paragraph was corrected,
and RC was added to the author list.]


GRB_name: GRB160625B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19616
SUBJECT: GRB 160625B: SMARTS optical/IR afterglow observations
DATE:    16/06/28 20:56:18 GMT
FROM:    Bethany Cobb at GWU  <bcobb@gwu.edu>

B. E. Cobb (GWU) reports:

Using the ANDICAM instrument on the 1.3m telescope at CTIO, we
obtained optical/IR imaging of the error region of GRB 160625B
(GCN 19580, Dirirsa et al.) with a mid-exposure time of about
32 hours post-burst (2016-06-27 06:51 UT). Total summed exposure
times amounted to 36 minutes in I and 30 minutes in J.

The afterglow of GRB 160625B (e.g. GCN 19585, Melandri et al.;
GCN 19588, Troja et al.; GCN 19589, Oates et al.) is detected
in our images. Preliminary comparison to USNO-B1.0 stars in I
and 2MASS stars in J indicates the following afterglow magnitudes:

mid-exposure
time post-burst       I mag           J mag
1.338 days            18.9+/-0.2      18.6+/-0.1


GRB_name: GRB160625B
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19617
SUBJECT: GRB 160625B CALET Gamma-Ray Burst Monitor detection
DATE:    16/06/29 08:09:50 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

S. Nakahira (JAXA), A. Yoshida, T. Sakamoto, Y. Kawakubo, M. Moriyama,
Y. Yamada (AGU), K. Yamaoka (Nagoya U), I. Takahashi (IPMU), Y. Asaoka,
S. Ozawa, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), W. Ishizaki (ICRR),
M. L. Cherry (LSU), S. Ricciarini (U of Florence) P. S. Marrocchesi (U of Siena)
and the CALET collaboration:

The long-duration GRB 160625B (Burns et al., GCN Circ. 19581;
Dirirsa et al. GCN Circ. 19586; INTEGRAL-ACS #7495) triggered the CALET Gamma-ray
Burst Monitor (CGBM) at 22:40:15.49 on 25 June 2016.  The burst signal
was seen by all CGBM instruments.

The light curve of the SGM shows a precursor emission starting at T+0.5 sec,
peaking at T+1 sec and ending at T+2 sec.  Then, the bright main burst episode
follows starting from T+183 sec and ending at T+233 sec with overlapping
multiple pulses.  The T90 duration measured by the SGM data for the main
bright episode is 20.0 +- 0.4 sec (40-1000 keV).  The T90 duration of the precursor
emission measured by the SGM data is 0.8 +- 0.1 sec (40-1000 keV).
The light curve is available at

http://cgbm.calet.jp/cgbm_trigger/flight/1150929566/

Furthermore, the main pulse was also detected by Imaging Calorimeter (IMC;
plastic scintillating fibers) and Charge Detector (CHD; plastic scintillators),
which are subsystems of the CALET main instrument Calorimeter (CAL).  The
incident angles for this burst was 61 degrees and 67 degrees from the boresight
of CAL at the trigger time and at the main peak, respectively.
The CAL gamma-ray analysis (>1 GeV) is in progress.

The CALET data used in this analysis are provided by the Waseda CALET Operation
Center located at the Waseda University.


GRB_name: GRB160620A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19618
SUBJECT: Konus-Wind observation of GRB 160620A
DATE:    16/06/29 11:04:58 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

D. Frederiks, S. Golenetskii, R.Aptekar, P. Oleynik, M. Ulanov,
D. Svinkin, A. Tsvetkova, A.Lysenko, A. Kozlova, and T. Cline,
on behalf of the Konus-Wind team, report:

The short GRB 160620A (IPN triangulation: Hurley et al., GCN 19594)
triggered Konus-Wind at T0=18380.236 s UT (05:06:20.236).

The light curve shows a single pulse which starts at ~T0-0.256 s,
peaks at ~T0+0.608, and have a total duration of ~1.5 s.
The emission is seen up to ~3 MeV.

As observed by Konus-Wind, the burst had a fluence
of 4.8(-0.6,+1.1)x10^-6 erg/cm2, and a 16-ms peak flux,
measured from T0+0.608 s, of 9.4(-0.6,+1.0)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+8.448 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 = -0.63 (-0.23,+0.35),
the high energy photon index beta = -3.41 (-6.59,+0.91),
the peak energy Ep = 158 (-27,+23) keV,
chi2 = 106/97 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB160620_T18380/

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


GRB_name: GRB160625B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19619
SUBJECT: GRB 160625B: TSHAO optical observations
DATE:    16/06/29 15:18:38 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), A. Kusakin (Fesenkov Astrophysical Institute), P. 
Minaev (IKI), I. Reva (Fesenkov Astrophysical Institute), A. Volnova 
(IKI), A. Pozanenko (IKI) report on behalf of larger GRB follow-up 
collaboration:

We observed the field of GRB 160625B (Dirirsa et al., GCN 19580; Burns 
et al. GCN 19581) with Zeiss-1000 (East) 1-m telescopes of Tien Shan 
Astronomical Observatory. We obtained several images in R filter 
starting on June 27 (UT) 20:15:57. We detect optical afterglow of  GRB 
160625B (Troja et al., GCN 19588; Oates  et al., GCN  19589). 
Preliminary photometry of a combined image is following

Date       UT start   t-T0    Filter  Exp.   OT     Err.  UL
                       (mid, days)     (s)

2016-06-27 20:15:57   1.92994 R       54*60 19.56  0.06  22.0

Photometry is based on nearby USNO-B1.0 stars reported in GCN 19605 
(Mazaeva et. al).


GRB_name: GRB160625B
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19620
SUBJECT: GRB 160625B: TSHAO optical observations, correction GCN 19619
DATE:    16/06/29 15:45:03 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI) report on behalf of larger GRB follow-up  collaboration:


Corrected text of the GCN 19619 (Mazaeva et al.) should be as follows.

E. Mazaeva (IKI), A. Kusakin (Fesenkov Astrophysical Institute), P. 
Minaev (IKI), I. Reva (Fesenkov Astrophysical Institute), A. Volnova 
(IKI), A. Pozanenko (IKI) report on behalf of larger GRB follow-up 
collaboration:

We observed the field of GRB 160625B (Dirirsa et al., GCN 19580; Burns 
et al. GCN 19581) with Zeiss-1000 (East) 1-m telescopes of Tien Shan 
Astronomical Observatory. We obtained several images in R filter 
starting on June 28 (UT) 18:12:30. We detect optical afterglow of  GRB 
160625B (Troja et al., GCN 19588; Oates  et al., GCN  19589). 
Preliminary photometry of a combined image is following

Date       UT start   t-T0    Filter  Exp.   OT     Err.   UL
                       (mid, days)     (s)

2016-06-28 18:12:30   2.86135 R       63*120 20.32   0.06  22.7

Photometry is based on nearby USNO-B1.0 stars reported in GCN 19605 
(Mazaeva et. al).


I thank D. A. Kann who noticed the apparent error.


GRB_name: GRB160629A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19621
SUBJECT: GRB 160629A: a long GBB detected by INTEGRAL
DATE:    16/06/29 23:36:50 GMT
FROM:    Sandro Mereghetti at IASF-Milano/INAF  <sandro@iasf-milano.inaf.it>

D.Gotz (CEA, Saclay), S.Mereghetti (IASF-Milano), E.Bozzo, C.Ferrigno, 
L.Pavan (ISDC, Versoix), and J.Borkowski (CAMK, Torun) on behalf of the 
IBAS Localization Team report:

a gamma ray burst lasting about 100 s has been detected by IBAS in the 
IBIS/ISGRI data at 22:19:30 UT of 2016 June 29.

The refined coordinates (J2000) are:
R.A.=   4.7618  deg
DEC.=  76.9468 deg

with an uncertainty of  2 arcmin (90% c.l.).

The burst had a peak flux of 2.6 ph/cm2/s (20-200 keV, 1-s integration 
time) and a fluence in the same energy range of about 6.e-6 erg/cmq.

A plot of the light curve will  be posted at
http://ibas.iasf-milano.inaf.it/IBAS_Results.html


GRB_name: GRB160629A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19622
SUBJECT: GRB 160629A: TAROT Calern observatory optical detection
DATE:    16/06/30 02:56:57 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

Klotz A., Turpin D., Atteia J.L. (CNRS-OMP-IRAP),
Boer, M., Laugier, R. (CNRS-ARTEMIS),
Gendre B. (UVI - Etelman Obs.) report:

We imaged the field of GRB 160629A detected by INTEGRAL
(trigger 7498) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 21s after the GRB trigger
(19s after the notice). The elevation of the field increased from
39 degrees above horizon and weather conditions were good.

We detect a new fading source in the error box given by INTEGRAL
(Gotz et al. GCNC 19621) at the following position (+/- 2 arcsec):

  RA(J2000) = 00:19:27.42
DEC(J2000) = +76:58:00.7

t1(s) t2(s)  Rmag  Site
   98   128   16.4  TAROT Calern
  139   168   16.9  TAROT Calern
  407   497   17.1  TAROT Calern

The first image (t1=21s t2=81s) is trailed with a
duration of 60.0s (see the description in Klotz et al.,
2006, A&A 451, L39). It shows an increase of the
optical flux until R~16.4 at 81s. This image must
be analyzed more carefuly.

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

N.B. Galactic coordinates are lon=121.0706 lat=+14.2321
and the galactic extinction in R band is about 1.2 magnitude
estimated from D. Schlegel et al. 1998ApJ...500..525S.


GRB_name: GRB160629A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19623
SUBJECT: GRB 160629A: SAO RAS independent OT detection
DATE:    16/06/30 03:55:14 GMT
FROM:    Moskvitin Alexander at SAO RAS  <mosk@sao.ru>

V. Sokolov, A. Valeev, A. Moskvitin and V. Komarova (SAO RAS)
report on behalf of a larger team.

We observed the error box of INTEGRAL GRB 160629A (Gotz et al.
GCNC #19621) with the SAO RAS 6-meter telescope BTA + Scorpio.
The observations started since ~10 minutes after the trigger.
Several images in Rc band were obtained.

We find a fading source with the coordinates

R.A. =  00:19:27.1
Dec. = +76:58:00.7
error = 0".5

This object is consistent with the OT reported by Klotz et al.
(GCNC #19622).

We used USNO-B1 star 1669-0002297 (R.A = 00:19:31.12;
Dec. = +76:57:41.3) with R2 = 15.53 for the calibrations.
Preliminary magnitudes of OT are as following.

T-T0,s  exp,s  R_mag  err
==========================
 615     30    17.40  0.03
 688     60    17.55  0.03
 848    180    17.71  0.02
1039     60    17.85  0.05
1118     30    18.13  0.08
1393     80    18.21  0.09
1508     80    18.24  0.11
1648     80    18.41  0.10
1964    180    18.55  0.09
3859    180    19.25  0.07
4066    180    19.18  0.04
4262    180    19.25  0.04
4483    180    19.29  0.11
4725    180    19.24  0.05
4926    180    19.24  0.03
5132    180    19.33  0.04
5347    180    19.30  0.04
5585    180    19.43  0.05
5824    180    19.44  0.06

ftp://ftp.sao.ru/pub/grb/GRB160629A/GRB160629A_BTA.jpg


GRB_name: GRB160630A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19624
SUBJECT: GRB 160630A: Swift detection of a burst
DATE:    16/06/30 04:19:45 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

H. A. Krimm (CRESST/GSFC/USRA), P. D'Avanzo (INAF-OAB),
A. Y. Lien (GSFC/UMBC), F. E. Marshall (NASA/GSFC),
A. Melandri (INAF-OAB), B. Sbarufatti (INAF-OAB/PSU) and
M. H. Siegel (PSU) report on behalf of the Swift Team:

At 04:04:09 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 160630A (trigger=702252).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 198.239, -56.069 which is 
   RA(J2000) = 13h 12m 57s
   Dec(J2000) = -56d 04' 06"
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 160 sec.  The peak count rate
was ~3000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 04:05:33.0 UT, 83.1 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 198.2584, -56.0420
which is equivalent to:
   RA(J2000)  = 13h 13m 02.03s
   Dec(J2000) = -56d 02' 31.3"
with an uncertainty of 2.1 arcseconds (radius, 90% containment). This
location is 104 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 consistent with the Galactic value of 3.89
x 10^21 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 87 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 0.48. 

Burst Advocate for this burst is H. A. Krimm (hans.krimm 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: GRB160630A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19625
SUBJECT: GRB 160630A: GROND Afterglow Detection
DATE:    16/06/30 05:36:05 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

D. A. Kann (TLS Tautenburg), T. Kruehler (MPE Garching),  S. Schmidl (TLS
Tautenburg), J. Bolmer, and J. Greiner (both MPE Garching) report on
behalf of the GROND team.

We observed the field of GRB 160630A (Swift trigger 702252; Krimm et al.,
GCN #19624) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La Silla
Observatory (Chile).

Observations started at 04:10:58 UT, 6.8 minutes after the GRB trigger.
They were performed at an average seeing of 2".1 and at an average airmass
of 1.8.

In an image with exposure time 66 s in g'r'i'z' taken at a mid-time of 7.3
min after the trigger, we detect a source at the edge of the 1".8 XRT
error circle at position:

RA (J2000) = 13:13:02.04

Dec. (J2000) = -56:02:29.8

(with an error of 0".3) with (AB magnitudes):

g' > 21.0 mag,
r' = 20.4 +/- 0.1 mag,
i' = 19.5 +/- 0.1 mag,
z' = 18.7 +/- 0.1 mag.

The source faded by about 1.5 magnitudes within the next quarter hour. We
therefore propose this source to be the afterglow of GRB 160630A.

Given magnitudes are calibrated against GROND zeropoints as well as 2MASS
field stars and are not corrected for the expected Galactic foreground
extinction E_(B-V) = 0.43 mag in the direction of the burst (Schlafly &
Finkbeiner, 2011).


GRB_name: GRB160630A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19626
SUBJECT: GRB 160630A: Enhanced Swift-XRT position
DATE:    16/06/30 09:13:00 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 2865 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 160630A, 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 = 198.25909, -56.04183 which is equivalent
to:

RA (J2000): 13h 13m 2.18s
Dec (J2000): -56d 02' 30.6"

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: GRB160630A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19627
SUBJECT: GRB 160630A: REM NIR observations
DATE:    16/06/30 09:46:38 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

A. Melandri, D. Fugazza, P. D'Avanzo, S. Covino (INAF/OAB) report on behalf of the REM team:

We observed the field of GRB 160630A (Krimm et al., GCN 19624) with the 60-cm robotic telescope REM located at the La Silla Observatory (Chile). The observations started at 04:05:13 UT, ~65 seconds after the burst, and were carried out simultaneously in the g, r, i, z and H bands.

A preliminary photometry indicates that the optical afterglow (Kann et al., GCN 16625) is detected with a magnitude H = 14.9 +/- 0.2, about 100 sec after the burst.

Further analysis is in progress.


GRB_name: GRB160629A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19628
SUBJECT: GRB 160629A: Fermi GBM observation
DATE:    16/06/30 11:26:44 GMT
FROM:    Kilian Toelge at MPE  <tkili@mpe.mpg.de>

Kilian Toelge (MPE) reports on behalf of the Fermi GBM Team:

"At 22:19:38.28 UT on 26 June 2016, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 160629A (trigger 488931582 / 160629930),
which was also detected by the INTEGRAL/IBAS
(Gotz et al. 2016, GCN 19621)
The GBM on-ground location is consistent with the INTEGRAL position.

The GBM light curve consists of a long main peak and a short second peak 
after
around 65 seconds.
The duration (T90) is about 66.6 +/- 0.4 s (50-300 keV).
The time-averaged spectrum from T0-4.1 s to T0+70.7 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.05 +/- 0.03 and
the cutoff energy, parameterized as Epeak, is 295.50 +/- 19.30 keV

The event fluence (10-1000 keV) in this time interval is
(1.9 +/- 0.1)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+14.1 s in the 8-1000 keV band
is 5.6 ph/s/cm^2.

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


GRB_name: GRB160625A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19629
SUBJECT: GRB 160625A: GROND upper limits
DATE:    16/06/30 11:29:31 GMT
FROM:    Ting-Wan Chen at MPE  <jchen@mpe.mpg.de>

T. Schweyer, T.-W. Chen, and J. Greiner (all MPE Garching) report on behalf of the GROND team:

We observed the field of GRB 160625A (Swift trigger 701503; Maselli et al., GCN #19577) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La Silla Observatory (Chile).

Observations started at 22:55 UT on 2016-06-26, 24.24 hrs after the GRB trigger.
They were performed through cirrus at an average seeing of 1.4" and at an average airmass of 1.2.

We do not detect any source within the Swift-XRT error circle reported by Burrows et al. (GCN #19578) down to

g > 22.6 mag,
r > 23.9 mag,
i > 22.5 mag,
z > 22.6 mag,
J > 19.9 mag,
H > 19.4 mag,
K > 19.5 mag.

Given magnitudes are calibrated against USNO as well as 2MASS field stars and are not corrected for the expected Galactic foreground extinction corresponding to a reddening of E_(B-V)=1.2 mag in the direction of the burst (Schlafly and Finkbeiner 2011).


GRB_name: GRB160630A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19630
SUBJECT: GRB 160630A: Swift-XRT refined Analysis
DATE:    16/06/30 14:30:12 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), L.M. McCauley (PSU), J.A.
Kennea (PSU), B. Sbarufatti (INAF-OAB/PSU), J.P. Osborne (U.
Leicester), K.L. Page (U. Leicester), B. Mingo (U. Leicester), A.
Maselli  (INAF-IASFPA) and H.A. Krimm report on behalf of the Swift-XRT
team:

We have analysed 8.2 ks of XRT data for GRB 160630A (Krimm et al. GCN
Circ. 19624), from 69 s to 24.5 ks after the  BAT trigger. The data
comprise 7 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 Goad et al. (GCN Circ. 19626).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=3.3 (+4.7, -1.1). At T+110 s  the decay
flattens to an alpha of 0.20 (+/-0.14) before breaking again at T+2108
s to a final decay with index alpha=1.31 (+0.12, -0.11).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.74 (+0.13, -0.12). The
best-fitting absorption column is  4.5 (+0.8, -0.6) x 10^21 cm^-2,
consistent with the Galactic value of 3.9 x 10^21 cm^-2 (Willingale et
al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 4.6 x 10^-11 (6.4 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.5 (+0.8, -0.6) x 10^21 cm^-2
Galactic foreground: 3.9 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.74 (+0.13, -0.12)

If the light curve continues to decay with a power-law decay index of
1.31, the count rate at T+24 hours will be 8.6 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.0 x
10^-13 (5.6 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/00702252.

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


GRB_name: GRB160630A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19631
SUBJECT: GRB 160630A: Swift/UVOT Upper Limits
DATE:    16/06/30 15:22:22 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

S. J. LaPorte (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 160630A
87 s after the BAT trigger (Krimm et al., GCN Circ. 19624).
No optical afterglow consistent with the enhanced XRT position
(Goad et al., GCN Circ 19626) or the optical/IR position
(Kann et al. GCN Circ. 19625) 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            87          237          147         >20.6
u_FC               300          550          246         >19.9
white               87         6366          530         >21.7
v                  630         6777          439         >20.2
b                  555         6161          236         >20.5
u                  300         5956          462         >20.6
w1                 680         7042          290         >19.7
m2                 655         6982          432         >20.9
w2                 606         6572          255         >19.7

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.48 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB160629A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19632
SUBJECT: GRB 160629A: BTA and GTC redshift
DATE:    16/06/30 17:10:44 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

A. J. Castro-Tirado (IAA-CSIC Granada), T. A. Fatkhullin, A. S. Moskvitin,
A. F. Valeev, V. N. Komarova, V. V. Sokolov (SAO-RAS Zelenchuk), R.
Snchez-Ramrez, F. J. Aceituno, B.-B. Zhang, Y. Hu, J. C. Tello
(IAA-CSIC), S. B. Pandey (ARIES) and G. Lombardi (GTC La Palma), on behalf
of a larger collaboration, report:

Following the detection of GRB 160629A by INTEGRAL (Gotz et al. GCNC
19621), optical spectra of the optical counterpart (Klotz et al. GCNC
19622, Sokolov et al. GCNC 19623) were obtained at both the 6.0m BTA
telescope in Zelenchuk (Russia) and at the 10.4m GTC in La Palma (Spain)
starting at 22.57 (June 29) and 4:39 (June 30) UT (i.e. 0.6 and 8.3 hr
postburst) respectively. A preliminary analysis shows a deep Lyman-alpha
trough and several metal absorption lines (SiII, SiII*, CII, SiIV, CIV,
FeII, and AlII, amongst others) at a common redshift of z = 3.332, which
we propose to be the redshift of the GRB host galaxy."


GRB_name: GRB160630A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19633
SUBJECT: GRB 160630A: TAROT La Silla observatory optical observations
DATE:    16/06/30 17:51:08 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

Klotz A., Turpin D., Atteia J.L. (CNRS-OMP-IRAP),
Boer, M., Laugier, R. (CNRS-ARTEMIS),
Gendre B. (UVI - Etelman Obs.) report:

We imaged the field of GRB 160630A detected by SWIFT
(trigger 702252) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 33s after the GRB trigger
(15s after the notice). The elevation of the field decreased from
34 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 any OT with a limiting magnitude of:
t0+33s to t0+93s : Rlim = 16.4

The second image is 30.0s exposure in tracking mode:
t0+107s to t0+137s : Rlim = 17.5

We co-added a series of exposures:
t0+107s to t0+302s : Rlim = 18.0

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


GRB_name: GRB160630A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19634
SUBJECT: GRB 160630A: Zadko observatory - Gingin optical observations
DATE:    16/06/30 18:13:40 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

Klotz A., Turpin D., Atteia J.L. (CNRS-OMP-IRAP),
Boer, M., Laugier, R. (CNRS-ARTEMIS),
Gendre B. (UVI - Etelman Obs.),
Coward, D. McPherson, D. Williams A., Martin R.,
Moore J., Dodson R. (UWA) report:

We imaged the field of GRB 160630A detected by SWIFT
(trigger 702252) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 6.4h after the GRB trigger.
The elevation of the field increased from
64 degrees above horizon and weather conditions
were good.

We co-added a series of exposures:
t0+6.4h to t0+8.0h : Rlim = 21.0

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


GRB_name: GRB160629A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19635
SUBJECT: Konus-Wind observation of GRB 160629A
DATE:    16/06/30 18:37:43 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

D. Frederiks, S. Golenetskii, R.Aptekar, P. Oleynik, M. Ulanov,
D. Svinkin, A. Tsvetkova, A.Lysenko, A. Kozlova, and T. Cline,
on behalf of the Konus-Wind team, report:

The long GRB 160629A (INTEGRAL detection: Gotz et al., GCN 19621;
Fermi GBM observation: Toelge, GCN 19628)
triggered Konus-Wind at T0=80385.314 s UT (22:19:45.314).

The light curve shows a smooth pulse with a total duration of ~40 s.
The weaker subsequent emission is traceable up to ~T0+70 s.
The emission in the main pulse is seen up to ~4 MeV.

As observed by Konus-Wind, the burst had a fluence
of 1.5(-0.4,+0.6)x10^-5 erg/cm2, and a 64-ms peak flux,
measured from T0+10.560 s, of 1.4(-0.3,+0.3)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+24.832 s)
is best fit in the 20 keV - 5 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.79 (-0.17,+0.23),
the high energy photon index beta = -2.92 (-3.68,+0.50),
the peak energy Ep = 227 (-41,+41) keV,
chi2 = 76/76 dof.

Assuming the redshift z=3.332 (Castro-Tirado et al., GCN Circ. 19632)
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:
the isotropic energy release E_iso is ~3.7x10^53 erg,
the peak luminosity L_iso is ~1.5x10^53 erg/s,
and the rest-frame peak energy of the time-integrated spectrum,
Ep,i, is ~980 keV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB160629_T80385/

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


GRB_name: GRB160630A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19636
SUBJECT: GRB 160630A: Skynet PROMPT-CTIO observations of the optical afterglow
DATE:    16/06/30 18:42:41 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, D. Reichart, J. Haislip, J. Moore, N. Frank, M. Maples, D. Dutton, R. Gao, R. Joyner, J. Martin, M. Paggen, J. A. Crain, K. Ivarsen, A. LaCluyze, and M. Nysewander report:

Skynet observed the Swift BAT/XRT localization of GRB 160630A (Krimm et al., GCN 19624, Swift trigger=702252) with with two 16" telescopes (P5, P6), and two 24" telescopes (P1, P8) of the PROMPT array at CTIO, Chile. Starting at 2016-06-30 04:05 UT and continuing until 07:02 UT (t=60s-3h post-trigger), Skynet took a total of 452 2.5-160s exposures in the I band (P1, P5), V band (P6) and B band (P8).  

We detect a fading optical afterglow in stacked I-band images at the OT position reported by Kann et al. (GCN 19625) and Melandri et al. (GCN 19627), with I~17.4 at t=5m and I~18.6 at t=23m. 

A preliminary light curve is at:
http://www.skynet.unc.edu/grb/grb160630a.png

Preliminary magnitudes are in the Vega System, calibrated to 9 APASS DR9 stars in the field.  Magnitudes have not been corrected for line-of-sight Milky Way dust extinction, with expected E(B-V)=0.43 (Schlafly & Finkbeiner 2011).

No further Skynet observations are scheduled.


GRB_name: GRB160629A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19637
SUBJECT: GRB 160629A: Swift ToO observations
DATE:    16/06/30 19:51:17 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a ToO observation of the INTEGRAL GRB 160629A. 
Automated analysis of the XRT data will be presented online at
http://www.swift.ac.uk/ToO_GRBs/00020676

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. These are
not necessarily related to the INTEGRAL event. Any X-ray source
considered to be a probable afterglow candidate will be reported via a 
GCN Circular after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).

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


GRB_name: GRB160629A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19638
SUBJECT: GRB 160629A: Global MASTER Net Prompt OT observations
DATE:    16/07/01 11:58:48 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
The Instituto de Astrofisica de Canarias

V. Lipunov, P.Balanutsa, E. Gorbovskoy, N.Tyurina, V.Kornilov,
A.Kuznetsov, D.Kuvshinov,
Lomonosov Moscow State University, Sternberg Astronomical Institute

D.Buckley, S. Potter, A.Kniazev, M.Kotze
South African Astronomical Observatory

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

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

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

Ricardo Podesta, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)

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

MASTER-IAC  robotic telescope (MASTER-Net: http://observ.pereplet.ru)
was pointed to the  INTEGRAL GRB 160629A (Gotz et al., GCN19621) 41 sec 
after GBM trigger at 2016-06-29 22:20:10 UT   by two tubes during Gamma 
Ray active phase (see Gotz et al., GCN19621). We use trigger time 22 19 30 (Gotz et al., GCN19621). 
The OT magnitude is ~ 16.6

MASTER-Kislovodsk  robotic telescope (MASTER-Net: 
http://observ.pereplet.ru) 
located near Kislovodsk was pointed to the  GRB160629A 201 sec
trigger time at 2016-06-29 22:24:11 UT. On 
our first (20s exposure)  image  we  found 1 optical transient within 
INTEGRAL error-box (ra=00 20 16 dec=+77 04 43 r=0.051667) brighter then 
18.5.


  T-Tmid      Date      Time       Expt.      Mag
---------|---------------------|-------|-------
    134     2016-06-29 22:21:44      20       ~17.0


The OT found at  position:

00h 19m 27.21s (+-0.09 s =  +-1.4 arcsec ) +76d 58' 01".0 ( +-0.2 arcsec)

(Cf. with TAROT coordinates Klotz  et al., GCN 19622 and Sokolov et
al., GCN 19623).

The preliminary light curve is available at 
master.sai.msu.ru/static/OT/MASTERGRB160629A.png

The message may be cited.


GRB_name: GRB160630A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19639
SUBJECT: GRB 160630A: Swift-BAT refined analysis
DATE:    16/07/01 12:43:23 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), T. N. Ukwatta (LANL)
(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 160630A (trigger #702252)
(Krimm, et al., GCN Circ. 19624).  The BAT ground-calculated position is
RA, Dec = 198.238, -56.029 deg which is
  RA(J2000)  =  13h 12m 57.0s
  Dec(J2000) = -56d 01' 44.3"
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 51%.

The mask-weighted light curve shows a single-peaked structure that starts
at ~T-1 s, peaks at ~T0, and ends at ~T+35 s. T90 (15-350 keV)
is 29.50 +- 5.51 sec (estimated error including systematics).

The time-averaged spectrum from T-1.00 to T+34.89 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.32 +- 0.14.  The fluence in the 15-150 keV band is 1.2 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-0.42 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/702252/BA/


GRB_name: GRB160625B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19640
SUBJECT: GRB 160625B: LCOGT FTN observations
DATE:    16/07/01 16:43:58 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), S. Kobayashi (LJMU), C.G. Mundell (U. Bath), 
A. Gomboc (U. Nova Gorica), on behalf of a large collaboration report:

We observed Fermi GRB 160625B (Dirirsa et al. GCN 19580) with the 2-m 
LCOGT Faulkes Telescope North in Hawaii on July 01 from 11:12 UT to 
12:46 UT with the SDSS-r filter for a total exposure of 1500 s. We 
clearly detect the optical afterglow (Troja et al. GCN 19588; Oates et 
al. GCN 19589; Kuroda et al. GCN 19599; Xu et al. GCN 19600; D'Elia et 
al. GCN 19601; Karpov et al. GCN 19603; Mazaeva et al. GCN 19605; 
Moskvitin et al. GCN 19611; Gorbovskoy et al. GCN 19612; Batsch et al. 
GCN 19615; Cobb et al. GCN 19616) with a magnitude of r=21.15 +- 0.15 
mag at a mid epoch of 5.5 days post burst, as calibrated against nearby 
USNOB1 stars.


GRB_name: GRB160629A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19641
SUBJECT: GRB 160629A: Swift-XRT afterglow detection
DATE:    16/07/01 18:34:27 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

A. D'Ai (INAF-IASFPA), J.A. Kennea (PSU), B. Sbarufatti (INAF-OAB/PSU),
D.N. Burrows (PSU), K.L. Page (U. Leicester), B. Mingo (U. Leicester),
A.P. Beardmore (U. Leicester), A. Maselli  (INAF-IASFPA), A. Melandri
(INAF-OAB) and P.A. Evans (U. Leicester) report on behalf of the
Swift-XRT team:

Swift-XRT has performed follow-up observations of the INTEGRAL-detected
burst GRB 160629A (Gotz et al. GCN Circ. 19621), collecting 2.6 ks of
Photon Counting (PC) mode data between T0+77.1 ks and T0+89.3 ks. 

An uncatalogued X-ray source is detected within the 3-sigma INTEGRAL
error region and is  believed to be the afterglow. Using 1633 s of PC
mode data and 1 UVOT image, we find an enhanced XRT position (using the
XRT-UVOT alignment and matching UVOT field sources to the USNO-B1
catalogue): RA, Dec = 4.86537, +76.96703 which is equivalent to:

RA (J2000): 00h 19m 27.69s
Dec(J2000): +76d 58' 01.3"

with an uncertainty of 3.4 arcsec (radius, 90% confidence). This
position is 111 arcsec from the INTEGRAL position.  We cannot determine
at the present time whether the source is fading. 
Since this position is consistent with the one reported for the optical
afterglow (Klotz et al. GCN Circ 19622; Sokolov et al. GCN Circ 19623;
Rebolo et al. GCN Circ. 19638), we propose this source as the X-ray
afterglow of GRB 160629A. 

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020676.
The results of the full analysis of the XRT observations are available
at http://www.swift.ac.uk/ToO_GRBs/00020676.

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


GRB_name: GRB160625B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19642
SUBJECT: GRB 160625B: SAO RAS monitoring
DATE:    16/07/02 13:55:29 GMT
FROM:    Vladimir Sokolov at SAO RAS  <sokolov@sao.ru>

A. F. Valeev, A. S. Moskvitin, G. M. Beskin, V. V. Vlasyuk, V. V. Sokolov
(SAO RAS, Russia) report on behalf of the larger GRB follow-up team.

We observed the GRB160625B field (Dirirsa et al. GCNC #19580) with
two optical telescopes of SAO RAS: the 6-m BTA + Scorpio (B, V, Rc, Ic
bands),
and the 1-meter telescope Zeiss-1000 + CCD photometer (Rc band)
at the June 29/30 night.
We clearly detected an OT (Troja et al. ,GCNC #19588; Karpov et al GCNC
#19603;
Alexander et al. GCNC #19606) in our stacked frames.
Preliminary Rc band  results are shown in the following table.
These estimations are based on the R2 magnitudes of the same nearby
USNO-B1 stars as in our previous GCNC #19611.
Mid_date, UT   T-T0,d   exp,s    R_mag    err    Telescope
=================================================================
June, 29.827   3.880    3 x 200  20.53 +/- 0.07  BTA
June, 29.983   4.036    8 x 300  20.56 +/- 0.20  Zeiss-1000


GRB_name: GRB160629A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19643
SUBJECT: GRB 160629A: Swift/UVOT Upper Limits
DATE:    16/07/02 14:17:14 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

B. G. Balzer  (PSU) and C. B. Markwardt (GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 160629A
77035 s after the INTEGRAL trigger (Gotz et al., GCN Circ. 19621).
No optical afterglow consistent with the optical position
(Klotz et al., GCN Circ 19622, Sokolov, et al. GCN Circ 19623) or the
XRT position (DAi et al., GCN Circ. 19641) is detected.
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

u                77035        89233         2633         >21.4

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.40 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB160703A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19645
SUBJECT: GRB 160703A: Swift detection of a burst
DATE:    16/07/03 12:21:44 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

S. B. Cenko (GSFC), V. D'Elia (ASDC), N. Gehrels (NASA/GSFC),
L. Izzo (IAA-CSIC), J. A. Kennea (PSU), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL), T. Sakamoto (AGU),
B. Sbarufatti (INAF-OAB/PSU) and T. N. Ukwatta (LANL) report on behalf
of the Swift Team:

At 12:10:05 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 160703A (trigger=702699).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 287.392, +36.901 which is 
   RA(J2000) = 19h 09m 34s
   Dec(J2000) = +36d 54' 04"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with a duration of about 60 sec.  The peak count rate
was ~10000 counts/sec (15-350 keV), at ~22 sec after the trigger. 

XRT is temporarily offline, and so there will be no immediate data
from this GRB. 

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 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
0.14. 

Burst Advocate for this burst is S. B. Cenko (brad.cenko 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: GRB160629A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19646
SUBJECT: GRB 160629A: AbAO optical observations
DATE:    16/07/03 15:12:57 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), A. Pozanenko (IKI), A. Volnova  (IKI), R. Inasaridze 
(AbAO), V. Ayvazian  (AbAO), V. Zhuzhunadze,  (AbAO),  O.Kvaratskhelia 
(AbAO), G. Inasaridze (AbAO),  I. Molotov (KIAM), report on behalf of larger 
GRB follow-up collaboration:

We observed the field of the INTEGRAL GRB 160629A (Gotz et al., GCN 19621) 
with AS-32 (0.7m) telescope of Abastumani Observatory  on June, 01 (UT) 
19:07:28. We obtained several unfiltered images of the field. Within XRT 
error circle (D'Ai et al., GCN 19641) we detected optical afterglow (Klotz 
et al., GCN 19622; Sokolov et al., GCN  19623) on July 1, and obtained upper 
limit on June 30. Preliminary photometry  of the optical afterglow  is 
following

Date        UT start           t-T0          Filter  Exp.    OT      UpLim 
(3 sigma)
                                        (mid, days)     (s)

2016-06-30  18:23:01   0.86572  CR     37*60   n/d               21.4
2016-07-01  19:34:47   1.93748  CR     36*120 22.2+/-0.2  23.0

Photometry is based on nearby USNO-B1.0 stars
USNO-B.1_id R2
1669-0002297 15.53
1669-0002325 15.34
1669-0002281 15.48
1669-0002346 16.43
1669-0002192 15.78

 


GRB_name: GRB160703A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19647
SUBJECT: GRB 160703A: Zadko observatory - Gingin optical observations
DATE:    16/07/03 19:25:36 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

Klotz A., Turpin D., Atteia J.L. (CNRS-OMP-IRAP),
Boer, M., Laugier, R. (CNRS-ARTEMIS),
Gendre B. (UVI - Etelman Obs.),
Coward, D. McPherson, D. Williams A., Martin R.,
Moore J., Dodson R. (UWA) report:

We imaged the field of GRB 160703A detected by SWIFT
(trigger 702699) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 5.5h after the GRB trigger.
The elevation of the field decreased from only
20 degrees above horizon and weather conditions
were good.

We co-added a series of exposures.
No credible source was found in the BAT error box:
t0+5.5h to t0+5.6h : Rlim = 19.4

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


GRB_name: GRB160703A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19648
SUBJECT: GRB 160703A: Swift-BAT refined analysis
DATE:    16/07/03 20:12:32 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC), S. B. Cenko (GSFC),
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), T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+963 sec from the recent telemetry downlinks,
we report further analysis of BAT GRB 160703A (trigger #702699)
(Cenko, et al., GCN Circ. 19645).  The BAT ground-calculated position is
RA, Dec = 287.414, 36.913 deg, which is 
   RA(J2000)  =  19h 09m 39.4s 
   Dec(J2000) = +36d 54' 46.2" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 84%.
 
The mask-weighted light curve shows many overlapping peaks starting
at ~T-26 sec, with the brightest peak at ~T+28 sec, and ending at ~T+75 sec.
T90 (15-350 keV) is 44.4 +- 2.8 sec (estimated error including systematics).
 
The time-averaged spectrum from T-26.43 to T+52.57 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.34 +- 0.04.  The fluence in the 15-150 keV band is 9.0 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+26.64 sec in the 15-150 keV band
is 5.8 +- 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/702699/BA/


GRB_name: GRB160703A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19649
SUBJECT: Konus-Wind observation of GRB 160703A
DATE:    16/07/04 11:31:52 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

D. Frederiks, S. Golenetskii, R.Aptekar, P. Oleynik, M. Ulanov,
D. Svinkin, A. Tsvetkova, A.Lysenko, A. Kozlova, and T. Cline,
on behalf of the Konus-Wind team, report:

The long GRB 160703A (Swift/BAT observation:
Cenko et al., GCN 19645; Lien et al., GCN 19648)
triggered Konus-Wind at T0=43807.015 s UT (12:10:07.015).

The light curve shows multiple overlapping pulses, a total
duration of the burst is ~50 s.
The emission is seen up to ~4 MeV.

As observed by Konus-Wind, the burst had a fluence of
(2.7 Â± 0.2)x10^-5 erg/cm2 and a 64-ms peak energy flux,
measured from T0+23.360, of (2.8 Â± 0.3)x10^-6 erg/cm2
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+41.216 s)
is best fit in the 20 keV - 10 MeV range by a cutoff power-law
(CPL) function with the following model parameters:
the photon index alpha = -1.01(-0.09,+0.10),
and the peak energy Ep = 327(-36,+46) keV,
chi2 = 93/97 dof.
Fitting this spectrum with the GRB (Band) function yields
the same alpha and Ep with only an upper limit on beta of -2.4,
chi2 = 93/96 dof.

The spectrum near the peak count rate (measured from T0 to T0+41.216 s)
is best fit in the 20 keV - 10 MeV range by a cutoff power-law
(CPL) function with the following model parameters:
the photon index alpha = -0.66(-0.15,+0.16),
and the peak energy Ep = 272(-29,+35) keV,
chi2 = 79/89 dof.
Fitting this spectrum with the GRB (Band) function yields
the same alpha and Ep with only an upper limit on beta of -3.1,
chi2 = 79/88 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB160703_T43807/

All the quoted errors are estimated at the 90% confidence level.
All the presented results are preliminary.


GRB_name: GRB160703A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19650
SUBJECT: GRB 160703A: Bassano Bresciano Observatory upper limits
DATE:    16/07/04 12:53:18 GMT
FROM:    Ulisse Quadri at Bassano Bresciano Obs  <oabb@ulisse.bs.it>

U.Quadri, L.Strabla and R.Girelli report:

We imaged the field of GRB 160703A detected by SWIFT(trigger 702699)
with the robotic telescope of (IAU station 565) Bassano Bresciano 
Observatory, Italy. Member of: 
AAVSO - American Association of Variable Star Observers.
ISSP - Italian Supernovae Search Project.
UAI/SSV - Unione Astrofili Italiani/sezione stelle variabili.

The observations started 8.31 hour after the GRB trigger,  
with our Schmidt telescope D=320/400 mm F/D=3.1.

Weather conditions were good.

We co-added a series of exposures of 120 sec each.

Start T0+      End T0+      Vlim
8.31 hour    10.28 hour      19

We did not found any optical counterpart in the error box of the XRTcandidate.
(S. B. Cenko (GSFC), V. D'Elia (ASDC), N. Gehrels (NASA/GSFC), et al.)

Magnitudes were estimated with the UCAC4 cat. and 
are not corrected for galactic dust extinction.

Reference:
http://www.osservatoriobassano.org/GRB.asp

The message may be cited.


GRB_name: GRB160625B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19651
SUBJECT: GRB 160625B: RTT150 optical observations
DATE:    16/07/04 13:42:20 GMT
FROM:    Rodion Burenin at IKI, Moscow  <rodion@hea.iki.rssi.ru>

I. Bikmaev, E. Irtuganov, N. Sakhibullin (KFU/AST),
R. Burenin, M. Pavlinsky, R. Sunyaev (IKI),
I. Khamitov, H. Kirbiyik (TUG), U. Kiziloglu (METU), E. Gogus (Sabanci Uni.)

report:

We observed field of Fermi GRB 160625B (Dirirsa et al. GCN 19580) at
the position of optical afterglow (Troja et al. ,GCN 19588) with
Russian-Turkish 1.5-m telescope (RTT150, Bakirlitepe, TUBITAK National
Observatory, Turkey) using the TFOSC instrument.

We obtained series of Rc exposures in June 30 / July 01(6 frames x 600
sec, UT = 00:21 - 01:30 ), in July 01 / 02 (4 frames x 900 sec, UT =
00:36 - 01:42), in July 02 / 03 (6 frames x 900 sec, UT = 23:49 -
01:29), and in July 03 / 04, 2016, (14 frames x 600 sec, UT = 22:50 -
01:39). The optical transient (Troja et al. GCN 19588; Oates et
al. GCN 19589; Kuroda et al. GCN 19599; Xu et al. GCN 19600; D'Elia et
al. GCN 19601; Watson at al. GCN 19602; Karpov et al. GCN 19603;
Mazaeva et al. GCN 19605, 19620; Moskvitin et al. GCN 19611;
Gorbovskoy et al. GCN 19612; Batsch et al.  GCN 19615; Cobb et al. GCN
19616; Guidorzi et al. GCN 19640; Valeev et al. GCN 19642) is clearly
detected in each images.

Using USNO-B1 0969-0608410 star at RA,DEC = 308.580912 +06.909881
(J2000) with R = 16.73 mag as a reference we estimated the
Rc-magnitudes of the afterglow in stacked images:

 T-T0,  Mag., Mag.err
 days

 5.09   20.69 +- 0.03  
 6.10   20.96 +- 0.04  
 7.08   21.04 +- 0.03  
 8.06   21.24 +- 0.04  

RTT-150 data show that OT is fading at approximately the same power
law rate as it was observed earlier.


GRB_name: GRB160703A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19652
SUBJECT: GRB 160703A: MITSuME Akeno Optical Observations 
DATE:    16/07/04 17:56:53 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

Y. Tachibana,  Y. Saito, Y. Muraki, Y. Ono, T. Fujiwara, T. Yoshii, K. Saisho,
H. Ohuchi, Y. Yano, S. Harita, Y. Yatsu, and N. Kawai (Tokyo Tech)
report on behalf of the MITSuME collaboration:

We report the optical follow-up observations of GRB 160703A (S. B. Cenko et al., GCN Circular #19645) with a tricolor camera (g', Rc, and Ic) attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan.

The observation started at 2016-07-03 12:10:54 UT (~30 sec after the burst).
Although the first eight frames (each exposure time is 30 sec) are covered by thick clouds, we detected a bright optical transient source in the refined BAT error circle (A. Y. Lien et al., GCN Circular #19648)  ~5 min after the trigger.
The position of the counterpart is
RA(J2000) = 19h 09m 40.1s
Dec(J2000) = +36d 55' 08.1"
with an uncertainty of ~0.5 arc sec. 

Nearby the optical transient, a known source N2JN062852 (RA, Dec = 19h 09m 40.212s, +36d 55' 06.9816$B!I(B)
catalogued in GSC2.3 is located. 
In the photometric analysis, we ignored the contamination from the nearby source because its 
flux is substantially lower (Fmag = 20.27) comparing with the optical counterpart.
The results were shown below:

  T0+[min]    MID-UT    T-EXP[sec]    g$B!G(B    g$B!G(B_err    Rc    Rc_err    Ic    Ic_err
----------------------------------------------------------------------------------------------------------------------
   5.82          12:15:54        30          15.46    0.06        14.59    0.06        14.25    0.09
   58.35        13:08:26      3900        18.18    0.05        17.08    0.04        16.87    0.06
   330.52      15:40:36      7680        19.13    0.06        17.96    0.05        17.61    0.06
----------------------------------------------------------------------------------------------------------------------
  T0+ : Elapsed time after the burst
  T-EXP: Total Exposure time

We used GSC2.3 catalog for flux calibration.
Further analysis is ongoing.


GRB_name: GRB160703A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19653
SUBJECT: GRB 160703A: MITSuME Ishigakijima Optical Observation
DATE:    16/07/05 01:03:31 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

D. Kuroda (OAO, NAOJ),  H. Hanayama, T. Miyaji, J. Watanabe (IAO, NAOJ),
K. Yanagisawa (OAO, NAOJ), S.Nagayama (NAOJ), M. Yoshida (Hiroshima),
K. Ohta (Kyoto) and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME and OISTER collaboration:

We observed the field of GRB 160703A (Cenko et al., GCNC 19645)
with the optical three color (g', Rc and Ic) CCD camera attached
to the Murikabushi 1m telescope of Ishigakijima Astronomical
Observatory.

The observation started on 2016-07-03 12:12:55 UT, (~2.8 min after
the burst). We detected the previously reported afterglow
(Tachibana et al., GCNC 19652) in in all the three bands.

The photometric results of the OT are listed below.
We used GSC2.3 catalog for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec] g'    g'_e  Rc    Rc_e  Ic    Ic_e
-------------------------------------------------------------------
0.00232    12:13:25      60.0   14.02 0.02  13.73 0.02  13.35 0.01
0.13017    15:17:31     540.0   19.32 0.07  18.37 0.04  18.22 0.08
-------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB160703A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19655
SUBJECT: GRB 160703A: Swift-XRT afterglow detection
DATE:    16/07/05 08:40:09 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia (INAF-OAR), L. Izzo (IAA-CSIC), D. Malesani (DARK/NBI), E.
Troja (GSFC), B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), T.G.R.
Roegiers (PSU), B. Mingo (U. Leicester), A.P. Beardmore (U. Leicester),
A. Maselli  (INAF-IASFPA), A. Melandri (INAF-OAB), P. D'Avanzo
(INAF-OAB) and P.A. Evans (U. Leicester) report on behalf of the
Swift-XRT team:

Swift-XRT has performed follow-up observations of the
Swift/BAT-detected burst GRB 160703A (Lien et al. GCN Circ. 19648),
collecting 5.0 ks of Photon Counting (PC) mode data between T0+107.8 ks
and T0+120.4 ks. 

An uncatalogued X-ray source is detected within the 3-sigma Swift/BAT
error region and is above the RASS limit, and is therefore likely the
GRB afterglow. The position of this source is RA, Dec=287.4168,
+36.9175 which is equivalent to:

RA (J2000): 19:09:40.04
Dec(J2000): +36:55:03.0

with an uncertainty of 3.9 arcsec (radius, 90% confidence).  This
position is 92 arcsec from the Swift/BAT position and 5.1 arcsec from
the optical transient reported by Tachibana et al. (GCN Circ. 19652). 
The light curve is consistent with a constant source of mean count rate
1.7e-02 ct/sec. A power-law fit gives an index of 2.92 (+0.03, -3.89).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.9 (+0.7, -0.5). The
best-fitting absorption column is  3.0 (+3.9, -1.5) x 10^21 cm^-2,
consistent with the Galactic value of 1.5 x 10^21 cm^-2 (Willingale et
al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 3.9 x 10^-11 (5.4 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.0 (+3.9, -1.5) x 10^21 cm^-2
Galactic foreground: 1.5 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.9 (+0.7, -0.5)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00702699.
The results of the full analysis of the XRT observations are available
at http://www.swift.ac.uk/ToO_GRBs/00702699.

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


GRB_name: GRB160703A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19656
SUBJECT: GRB 160703A: Swift/UVOT Detection
DATE:    16/07/05 18:44:25 GMT
FROM:    Lea Hagen at PSU  <lea.zernow.hagen@gmail.com>

L. M. Z. Hagen (PSU) and S. B. Cenko (GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 160703A
75 s after the BAT trigger (Cenko et al., GCN Circ. 19645). We detect a
fading source consistent with the XRT position (D'Elia et al. GCN Circ.
19655) and optical detections (Tachibana et al., GCN Circ. 19652; Kuroda
et al., GCN Circ. 19653).

Preliminary detections 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               75          225          147         14.09+-0.02
white              567         1014          186         16.64+-0.03
white             4890         5090          196         18.33+-0.05
v                  617         1064           58         16.51+-0.10
v                 5300         5500          196         18.34+-0.17
b                  543          735           38         16.38+-0.06
b                 4685         4885          196         18.76+-0.11
u                  288          537          245         15.05+-0.03
u                  691          710           19         15.88+-0.09
u                 4480         4680          196         17.79+-0.08
uvw1               666         1113           58         16.80+-0.12
uvm2               642         1089           58         17.75+-0.25
uvm2              5505         5695          187         19.07+-0.29
uvw2               593         1040           58         18.38+-0.27
uvw2              5096         5295          196         19.45+-0.30

The detection in all UVOT filters is consistent with a redshift of
z < ~1.5.

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.15 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB160705B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19657
SUBJECT: GRB 160705B: Swift detection of a burst
DATE:    16/07/05 21:19:59 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

J. K. Cannizzo (NASA/UMBC), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), C. Gronwall (PSU), J. A. Kennea (PSU),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester) and T. N. Ukwatta (LANL) report on behalf of
the Swift Team:

At 21:02:07 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 160705B (trigger=703176).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 168.086, +46.721 which is 
   RA(J2000)  =  11h 12m 21s
   Dec(J2000) = +46d 43' 17"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows some weak emission
from T_0 to about T+40 (this is a 64-sec image trigger, and as such
there is seldom anything see in the raw real-time TDRSS telemetry). 
The duration of about 40 sec.  The peak count rate
was ~600 counts/sec (15-350 keV), at ~3 sec after the trigger. 

The XRT began observing the field at 21:04:27.7 UT, 140.3 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 168.10943,
46.70085 which is equivalent to:
   RA(J2000)  = 11h 12m 26.26s
   Dec(J2000) = +46d 42' 03.1"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 92 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 (1.19 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 2.7
(+2.18/-1.93) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 9.31e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 148 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
0.01. 

Burst Advocate for this burst is J. K. Cannizzo (cannizzo 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: GRB160705B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19658
SUBJECT: GRB 160705B: LT optical candidate
DATE:    16/07/05 22:14:16 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), C.G. Mundell (U. Bath), S. Kobayashi, I.A. 
Steele (LJMU), A. Gomboc (U. Nova Gorica) on behalf of a large 
collaboration report:

The 2-m Liverpool Telescope began observing Swift GRB 160705B (Cannizzo 
et al., GCN 19657) on July 05, 21:05:14 UT (3.1 minutes after the burst 
trigger). Inside the XRT error circle we find an uncatalogued source 
which is not present in the SDSS at the following position:

RA(J2000)=  11:12:26.27
Dec(J2000)= +46:42:01.2

with an uncertainty of 0.5 arcsec and r~21 mag (AB) @ 36 minutes post GRB.


GRB_name: GRB160705B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19659
SUBJECT: GRB 160705B: Enhanced Swift-XRT position
DATE:    16/07/06 05:45:04 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 2204 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 160705B, 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 = 168.10944, +46.69990 which is equivalent
to:

RA (J2000): 11h 12m 26.27s
Dec (J2000): +46d 41' 59.6"

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: GRB160705B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19660
SUBJECT: GRB 160705B: Swift-XRT refined Analysis
DATE:    16/07/06 06:46:50 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

D.N. Burrows (PSU), T.G.R. Roegiers (PSU), A.P. Beardmore (U.
Leicester), P.A. Evans (U. Leicester), S.L. Gibson (U. Leicester), A.
Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), L.M.
McCauley (PSU) and J.K. Cannizzo report on behalf of the Swift-XRT
team:

We have analysed 6.3 ks of XRT data for GRB 160705B (Cannizzo et al.
GCN Circ. 19657), from 130 s to 23.8 ks after the  BAT trigger. The
data comprise 132 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. 19659).

The light curve can be modelled with an initial power-law decay with an
index of alpha=3.81 (+0.14, -0.13), followed by a break at T+563 s to
an alpha of 0.60 (+0.12, -0.13).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.66 (+0.14, -0.13). The
best-fitting absorption column is  10.0 (+2.5, -2.4) x 10^20 cm^-2, in
excess of the Galactic value of 1.2 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.15 (+0.23, -0.21)
and a best-fitting absorption column of 8.1 (+5.2, -4.5) x 10^20 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.1 x 10^-11 (3.8 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      8.1 (+5.2, -4.5) x 10^20 cm^-2
Galactic foreground: 1.2 x 10^20 cm^-2
Excess significance: 2.5 sigma
Photon index:      2.15 (+0.23, -0.21)

If the light curve continues to decay with a power-law decay index of
0.60, the count rate at T+24 hours will be 0.012 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.5 x
10^-13 (4.4 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/00703176.

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


GRB_name: GRB160623A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19661
SUBJECT: GRB 160623A: Astrosat CZTI detection
DATE:    16/07/06 06:58:47 GMT
FROM:    Varun Bhalerao at IUCAA  <varunb@iucaa.in>

V. Bhalerao (IUCAA), V. Kumar (IUCAA), D. Bhattacharya (IUCAA), A. R. Rao (TIFR), S. Vadawale (PRL)  report on behalf of the Astrosat CZTI collaboration:

 Analysis of Astrosat data showed the detection of very bright GRB 160623A (Fermi-LAT detection: Vianello et al., GCN 19553, Mailyan et al., GCN 19555; Mingo et al. GCN 19558; Frederiks et al. GCN 19554)

The source was clearly detected in the 40-200 keV energy range. The light curve shows a single peak at UT 04:59:45.0, 49.23 seconds before the fermi trigger At 05:00:34.23 (trigger 488350837 / 160623209). The peak count rate was 2940 counts/sec above the background (four quadrants summed together), with a total of 20385 counts.  The local mean background count rate of 193.2 is counts/sec.  Using cumulative rates, we measure a T90 of 14.2 sec.

CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=node/9 . CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.

[GCN OPS NOTE(07jul16): Per operator, the GRB name as corrected from 1600625 to 160625.]


GRB_name: GRB160705B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19662
SUBJECT: GRB 160705B: Swift-BAT refined analysis
DATE:    16/07/06 11:37:09 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC), J. K. Cannizzo (NASA/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (GSFC/UMBC), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from the recent telemetry downlinks,
we report further analysis of BAT GRB 160705B (trigger #703176)
(Cannizzo, et al., GCN Circ. 19657).  The BAT ground-calculated position is
RA, Dec = 168.107, 46.707 deg, which is 
   RA(J2000)  =  11h 12m 25.7s 
   Dec(J2000) = +46d 42' 24.8" 
with an uncertainty of 2.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 73%.
 
The mask-weighted light curve shows possible emission from before T-239 sec
(the beginning of the data), with the peak starting at ~T-30 sec, peaking
at ~T+10 sec, and ending at ~T+90 sec.
T90 (15-350 keV) is 54.4 +- 12.4 sec (estimated error including systematics).
 
The time-averaged spectrum from T-15.09 to T+54.70 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.79 +- 0.27.  The fluence in the 15-150 keV band is 7.3 +- 1.1 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+26.04 sec in the 15-150 keV band
is 0.5 +- 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/703176/BA/


GRB_name: GRB160705B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19663
SUBJECT: GRB 160705B: RATIR Optical and NIR Observations and Confirmation of the Fading Afterglow
DATE:    16/07/06 13:50:49 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), Ori Fox (STScI), J.
Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara
(GSFC/STScI), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), JosÃ© A. de Diego (UNAM), Leonid Georgiev (UNAM),
JesÃºs GonzÃ¡lez (UNAM), Carlos RomÃ¡n-ZÃºÃ±iga (UNAM), Neil Gehrels (GSFC),
Harvey Moseley (GSFC), John Capone (UMD), V. Zach Golkhou (ASU), and
Vicki Toy (UMD) report:

We observed the field of GRB 160705B (Cannizzo et al., GCN 19657) with
the Reionization and Transients Infrared Camera (RATIR; www.ratir.org)
on the 1.5m Harold Johnson Telescope at the Observatorio AstronÃ³mico
Nacional on Sierra San Pedro MÃ¡rtir from 2016/07 6.17 to 2016/07 6.21
UTC (7.04 to 8.05 hours after the BAT trigger), obtaining a total of
0.66 hours exposure in the r and i bands and 0.30 hours exposure in the
Z, Y, J, and H bands.

We detect two sources within the enhanced Swift-XRT error circle
(Osborne et al., GCN 19659). The brighter source is an uncataloged source
at 11:12:26.20 +46:42:01.2 (J2000, +/- 0.5 arcsec) with the following
detections and 3-sigma upper limit:

r = 22.89 +/- 0.15
i = 22.12 +/- 0.09
Z = 22.34 +/- 0.33
Y = 21.73 +/- 0.32
J > 21.54
H = 20.98 +/- 0.34

The fainter source is a cataloged SDSS source at 11:12:26.42 +46:41:59.6
(J2000, +/- 0.5 arcsec) with the following detections and 3-sigma upper
limits:

r = 23.39 +/- 0.24
i = 22.61 +/- 0.14
Z = 22.10 +/- 0.26
Y > 21.87
J > 21.54
H > 21.04

These magnitudes are in the AB system, are in comparison with the SDSS
DR9 and 2MASS catalogs, and are not corrected for Galactic extinction in
the direction of the GRB.

We note that Guidorzi et al. (GCN 19658) report an uncataloged source
with r of about 21 at 36 minutes after the burst trigger. Their source
is only 0.7 arcsec from our brighter uncataloged source and so we
postulate that these correspond to the afterglow of the GRB. The
afterglow has faded by about 2 magnitudes between their observations at
36 minutes and ours at 7.54 hours, which corresponds to a temporal index
of about -0.6.

We thank the staff of the Observatorio AstronÃ³mico Nacional in San Pedro
MÃ¡rtir.


GRB_name: GRB160705B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19664
SUBJECT: GRB 160705B: Swift/UVOT Upper Limits
DATE:    16/07/06 20:47:42 GMT
FROM:    Sam Emery at MSSL-UCL  <samuel.emery.15@ucl.ac.uk>

S.W.K. Emery (UCL-MSSL) and J. K. Cannizzo (NASA/UMBC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 160705B
149 s after the BAT trigger (Cannizzo et al., GCN Circ. 19657).
No optical afterglow consistent with the XRT position (Osborne et al. GCN Circ. 19659)
or the LT and RATIR position (Guidorzi et al. GCN 19658; Watson et al. GCN Circ. 19663)
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           149          298          147         >20.6
u_FC               307          557          246         >19.9
white             4780         6415          393         >21.0
v                 5191        11327         1082         >19.9
b                 6011         6210          197         >20.1
w1               12239        12529          285         >20.0
m2               11333        12232          886         >20.7
w2                6421         6603          179         >19.9

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: GRB160702A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19666
SUBJECT: IPN Triangulation of GRB 160702A (short/hard)
DATE:    16/07/08 20:18:06 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

K. Hurley, on behalf of the IPN,

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

A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks, D. Svinkin,
and T. Cline on behalf of the Konus-Wind team,

S. Barthelmy, J. Cummings, N. Gehrels, H. Krimm, and D. Palmer,
on behalf of the Swift-BAT team,

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, and

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

A short-duration GRB 160702A has been detected by Konus-Wind, INTEGRAL
(SPI-ACS), Mars-Odyssey(HEND), and Swift (BAT) at about 44544 s UT
(12:22:24). The burst was outside the coded field of view of the BAT.

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
 ---------------------------------------------
  RA(2000), deg                 Dec(2000), deg
 ---------------------------------------------
 Center:
  230.889 (15h 23m 33s)  +8.715 ( +8d 42' 54")
 Corners:
  231.265 (15h 25m 03s)  +9.181 ( +9d 10' 51")
  230.871 (15h 23m 29s)  +9.187 ( +9d 11' 15")
  230.515 (15h 22m 04s)  +8.245 ( +8d 14' 41")
  230.908 (15h 23m 38s)  +8.243 ( +8d 14' 33")
 ---------------------------------------------
The error box area is 1320 sq. arcsin, and its maximum
dimension is 1.194 deg (the minimum one is 22 arcmin).
The Sun distance was about 121 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB160702_T44544/IPN/

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


GRB_name: GRB160702A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19667
SUBJECT: Konus-Wind observation of GRB 160702A (short/hard)
DATE:    16/07/08 20:30:03 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

D. Frederiks, S. Golenetskii, R.Aptekar, P. Oleynik, M. Ulanov,
D. Svinkin, A. Tsvetkova, A.Lysenko, A. Kozlova, and T. Cline,
on behalf of the Konus-Wind team, report:

The short GRB 160702A (IPN triangulation: Hurley et al., GCN 19666)
triggered Konus-Wind at T0=44544.054 s UT (12:22:24.054).

The light curve shows a short, hard pulse with a total duration
of ~200 ms.
The emission is seen up to ~5 MeV.

As observed by Konus-Wind, the burst had a fluence of
(2.5 Â± 0.7)x10^-6 erg/cm2 and a 16-ms peak energy flux,
measured from T0-0.016, of (3.0 Â± 0.4)x10^-5 erg/cm2
(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 - 10 MeV range by a cutoff power-law
(CPL) function with the following model parameters:
the photon index alpha = -0.28(-0.35,+0.48),
and the peak energy Ep = 782(-186,+308) keV,
chi2 = 32.3/31 dof.
Fitting this spectrum with the GRB (Band) function yields
the same alpha and Ep with only an upper limit on beta of -2.1,
chi2 = 31.9/30 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB160702_T44544/

All the quoted errors are estimated at the 90% confidence level.
All the presented results are preliminary.


GRB_name: GRB160703A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19668
SUBJECT: GRB 160703A: Keck-I/LRIS Optical Observations
DATE:    16/07/09 04:19:22 GMT
FROM:    Weikang Zheng at UC Berkeley  <weikang@berkeley.edu>

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

We observed the field of GRB 160703A (Cenko et al., GCN 19645)
with the 10 m Keck-I telescope on July 3 starting at 13:17:55 UT, 
or 1.125 hours after the burst. A 180 s g'-band image and a 150 s 
R-band image were taken simultaneously with LRIS. We detect the
optical afterglow (Tachibana et al., GCN 19652; Kuroda et al., 
GCN 19653; Hagen & Cenko, GCN 19656) in both the g' and R 
images.

The afterglow is well separated in our images from the nearby
source N2JN062852 noted by Tachibana et al. (GCN 19652).
We measure the afterglow to be 1.58" west and 1.30" north of 
N2JN062852. A finding chart is posted at website URL
http://w.astro.berkeley.edu/~zwk/grb/GRB160703A/GRB160703A_keck_lris_g_fc.png .

We find that the afterglow had a brightness of R=17.9 mag at
1.125 hours after the burst, calibrated with the USNO B1.0 R2 system.


GRB_name: GRB160629A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19669
SUBJECT: GRB 160629A: AbAO optical observations
DATE:    16/07/09 10:22:08 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), A. Pozanenko (IKI), A. Volnova  (IKI), R. Inasaridze 
(AbAO), V. Ayvazian  (AbAO), V. Zhuzhunadze,  (AbAO),  O.Kvaratskhelia 
(AbAO), G. Inasaridze (AbAO),  I. Molotov (KIAM), report on behalf of 
larger GRB follow-up collaboration:

We observed the field of the INTEGRAL GRB 160629A (Gotz et al., GCN 
19621) with AS-32 (0.7m) telescope of Abastumani Observatory  on July, 
03 (UT) 19:07:28. We obtained several unfiltered images of the field. 
Within XRT error circle (D'Ai et al., GCN 19641) we do not detected 
optical afterglow (Klotz et al., GCN 19622; Sokolov et al., GCN  19623). 
Preliminary photometry  of the field  is following

Date        UT start   t-T0      Filter Exp.   OT   UpLim (3 sigma)
                       (mid, days)       (s)

2016-07-03  20:59:10   3.98204  CR      36*120 n/d  23.4

Photometry is based on nearby USNO-B1.0 stars
USNO-B.1_id R2
1669-0002297 15.53
1669-0002325 15.34
1669-0002281 15.48
1669-0002346 16.43
1669-0002192 15.78


GRB_name: GRB160629A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19670
SUBJECT: GRB 160629A: Mondy optical observations
DATE:    16/07/09 11:12:49 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), A. Pozanenko (IKI), E. Klunko (ISTP), A. Volnova 
(IKI),   P. Minaev (IKI), I. Korobtsev (ISTP)  report on behalf of 
larger GRB follow-up collaboration:

We observed the field of the INTEGRAL GRB 160629A (Gotz et al., GCN 
19621) with  AZT-33IK telescope of Sayan observatory (Mondy) starting on 
July, 01 (UT) 18:39:36. We obtained several images in R-filter. Within 
XRT error circle (D'Ai et al., GCN 19641) we  detected optical afterglow 
(Klotz et al., GCN 19622; Sokolov et al., GCN  19623). Preliminary 
photometry  of the field  is following

Date        UT start   t-T0      Filter Exp.   OT        UpLim (3 sigma)
                       (mid, days)       (s)

2016-07-01  18:39:36   1.86436   R      20*120 21.73+/-0.15  22.5


Photometry is based on nearby USNO-B1.0 stars
USNO-B.1_id R2
1669-0002297 15.53
1669-0002325 15.34
1669-0002281 15.48
1669-0002346 16.43
1669-0002192 15.78


GRB_name: GRB160628A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19671
SUBJECT: GRB 160628A CALET Gamma-Ray Burst Monitor detection
DATE:    16/07/09 12:46:18 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

I. Takahashi (IPMU), A. Yoshida, T. Sakamoto, Y. Kawakubo, M. Moriyama,
Y. Yamada (AGU), K. Yamaoka (Nagoya U), S. Nakahira (JAXA), I. Takahashi (IPMU),
Y. Asaoka, S. Ozawa, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U),
W. Ishizaki (ICRR), M. L. Cherry (LSU), S. Ricciarini (U of Florence)
P. S. Marrocchesi (U of Siena) and the CALET collaboration:

The long-duration GRB 160628A (Fermi-GBM trigger #488814821;
Konus-Wind trigger time on 13:53:41.910) triggered the CALET Gamma-ray
Burst Monitor (CGBM) at 13:53:37.9 on 28 June 2016.  The burst signal
was only seen by the SGM instrument.

The light curve of the SGM shows a double peak structure starting at T+0.1 sec
and ending at T+6 sec.  The peak times of the spikes are T+1 sec and T+3.5 sec.
The T90 duration measured by the SGM data is 5.1 +- 0.9 sec (40-230 keV).

The light curve is available at

http://cgbm.calet.jp/cgbm_trigger/flight/1151157163/

The CALET data used in this analysis are provided by the Waseda CALET Operation Center
located at the Waseda University.


GRB_name: GRB160705B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19672
SUBJECT: GRB 160705B: TAROT Calern observatory optical observations
DATE:    16/07/09 23:17:47 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

Klotz A., Turpin D., Atteia J.L. (CNRS-OMP-IRAP),
Boer, M., Laugier, R. (CNRS-ARTEMIS),
Gendre B. (UVI - Etelman Obs.) report:

We imaged the field of GRB 160705B detected by SWIFT
(trigger 703176) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 92s after the GRB trigger
(18s after the notice). The elevation of the field decreased from
36 degrees above horizon and weather conditions
were poor.

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 any OT with a limiting magnitude of:
t0+92s to t0+152s : Rlim = 15.5

The second image is 30.0s exposure in tracking mode:
t0+190s to t0+250s : Rlim = 16.6

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


GRB_name: GRB160709A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19674
SUBJECT: GRB 160709A: Tiled Swift observations
DATE:    16/07/10 01:34:19 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a series of observations, tiled on the sky, of the
Fermi/LAT GRB 160709A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00057

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the Fermi/LAT event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).

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


GRB_name: GRB160709A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19675
SUBJECT: GRB 160709A: Fermi-LAT detection
DATE:    16/07/10 01:58:47 GMT
FROM:    Sylvain Guiriec at UAH  <sylvain.guiriec@lpta.in2p3.fr>

S. Guiriec (NASA GSFC/UMD/CRESST), G. Vianello (Stanford)

& J. Racusin (NASA GSFC)

report on behalf of the Fermi-LAT team:

At 19:49:03.50 on July, 09, 2016 Fermi-LAT detected high-energy

emission from GRB 160709A, which was also detected

by Fermi-GBM (trigger 489786546 / 160709826).

The best LAT on-ground location is found to be

RA, Dec = 236.110, -28.500 (J2000)

with an error radius of 0.18 deg (90 % containment, statistical error only).

This was 48 deg from the LAT boresight at the time of the trigger.

The data from the Fermi-LAT show a significant increase in the event rate

that is spatially and temporally correlated with the trigger with high
significance.

More than 30 photons above 100 MeV are observed within 100 seconds,

with the highest-energy photons being 1 GeV events observed 2 seconds

after the GBM trigger and consistent with the GBM brightest emission
episode.

A Swift ToO has been requested for this burst.

The Fermi-LAT point of contact for this burst is Sylvain Guiriec (
sylvain.guiriec@nasa.gov).

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: GRB160709A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19676
SUBJECT: GRB 160709A: Fermi GBM Observations
DATE:    16/07/10 02:14:16 GMT
FROM:    Valerie Connaughton at USRA/NSSTC  <valerie.connaughton@nasa.gov>

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

"At 19:49:03.50 UT on 09 July 2016, the Fermi Gamma-Ray Burst Monitor triggered and 
located GRB 160709A (trigger 489786547 / 160709826), which was also detected by the LAT
(Guiriec et al. 2016, GCN 19675). The GBM on-ground location is consistent with the LAT position.

The angle from the Fermi LAT boresight at the GBM trigger time is 48 degrees.

The GBM light curve consists of two peaks with a duration (T90) of 
about 5.6 s (50-300 keV) beginning 64 ms before the trigger time.
The time-averaged spectrum from T0-0.26 s to T0+0.83 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.43 +/- 0.04 and
the cutoff energy, parameterized as Epeak, is 2211 +/- 131 keV.

The event fluence (10-1000 keV) in this time interval is
(3.33 +/- 0.09)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-0.06 s in the 10-1000 keV band
is 6.5 +/- 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: GRB160709A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19677
SUBJECT: Konus-Wind observation of GRB 160709A (short/hard)
DATE:    16/07/10 13:15:15 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

D. Frederiks, S. Golenetskii, R.Aptekar, P. Oleynik, M. Ulanov,
D. Svinkin, A. Tsvetkova, A.Lysenko, A. Kozlova, and T. Cline,
on behalf of the Konus-Wind team, report:

The short/hard GRB 160709A
(Fermi-LAT detection: Guiriec, et al., GCN Circ. 19675;
Fermi-GBM detection: Jenke, GCN Circ. 19676)
triggered Konus-Wind at T0=71345.896 s UT (19:49:05.896).

The light curve shows a short, hard pulse with a total duration
of ~0.4 s. The emission is seen up to ~8 MeV.

As observed by Konus-Wind, the burst had a fluence of
(1.5 Â± 0.3)x10^-5 erg/cm2 and a 16-ms peak energy flux,
measured from T0, of (6.3 Â± 0.9)x10^-5 erg/cm2
(both in the 20 keV - 10 MeV energy range).

The spectrum of the burst (measured from T0 to T0+0.256 s)
is best fit in the 20 keV - 10 MeV range by a cutoff power-law
(CPL) function with the following model parameters:
the photon index alpha = -0.51(-0.17,+0.19),
and the peak energy Ep = 2554(-509,+664) keV,
chi2 = 40.1/50 dof.
Fitting this spectrum with the GRB (Band) function yields
the same alpha and Ep with only an upper limit on beta of -2.1,
chi2 = 39.8/49 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB160709_T71345/

All the quoted errors are estimated at the 90% confidence level.
All the presented results are preliminary.


GRB_name: GRB160709A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19678
SUBJECT: GRB 160709A: Global MASTER Net Fermi GBM Alerts  observations  
DATE:    16/07/10 18:57:13 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, N.Tyurina, P.Balanutsa, 
V.Kornilov, A.Kuznetsov, D.Kuvshinov,
Lomonosov Moscow State University, Sternberg Astronomical Institute

D.Buckley, S. Potter, A.Kniazev, M.Kotze
South African Astronomical Observatory

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
The Instituto de Astrofisica de Canarias

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

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

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

Ricardo Podesta, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)

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

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in SAAO was pointed to the  GRB160709.83 66 sec after notice time 
and 105 sec after trigger time at 2016-07-09 19:50:49 UT. On our first 
(20s exposure)  set we no  found OT  within FERMI 
error-box (ra=15 12 59 dec=-29 48 00 r=4.32) brighter then 18.8.

But this field do not included FERMI LAT  error box (Guiriec et al., GCN 
19675).

MASTER-SAAO  robotic telescope  located in SAAO was continue inspection  of  the  GRB160709A and  1727 sec 
after FERMI GBM 
notice time (Jenke, GCN 19676) and before 9709 sec FERMI LAT notice time 
and 1750 sec after trigger time at  2016-07-09 20:18:14 UT observed FERI 
LAT error box. On our 120s exposure  set we  not found OT within FERMI LAT 
error-box (Guiriec et al., GCN 19675) brighter then 19.6.

The message may be cited.


GRB_name: GRB160709A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19679
SUBJECT: GRB 160709A: Swift-XRT observations
DATE:    16/07/10 18:57:35 GMT
FROM:    Beatriz Mingo at U of Leicester,XRT  <bm188@le.ac.uk>

T.G.R. Roegiers (PSU), S.L. Gibson (U. Leicester), J.P. Osborne (U.
Leicester), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), A. D'Ai
(INAF-IASFPA), L.M. McCauley (PSU), J.A. Kennea (PSU), 
B. Mingo (U. Leicester) and P.A. Evans (U. Leicester) report on behalf
of the Swift-XRT team:

Swift-XRT has performed follow-up observations of the
Fermi/LAT-detected burst GRB 160709A (Guiriec et al. GCN Circ. 19675)
in a series of observations tiled on the sky. The total exposure time
is 3.3 ks, distributed over 7 tiles; the maximum exposure at a single
sky location was 1.4 ks. The data were collected between T0+20.7 ks and
T0+39.1 ks, and are entirely in Photon Counting (PC) mode. 

No uncatalogued X-ray sources have been detected. The 3-sigma upper
limit in the field (not including the regions where the tiles overlap)
ranges from ~0.01 to ~0.06 ct s^-1, corresponding to a 0.3-10 keV
observed flux of 4.3e-13 to 2.2e-12 erg cm^-2 s^-1 (assuming a typical
GRB spectrum).

Two previously-catalogued X-ray sources have been detected, however
their status as catalogued objects makes them unlikely to be the
afterglow.

The results of the XRT-team automatic analysis of the tiled XRT
observations, including a position-specific upper limit calculator, are
available at http://www.swift.ac.uk/xrt_products/TILED_GRB00057.

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


GRB_name: GRB160625B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19680
SUBJECT: GRB 160625B: TSHAO optical observations
DATE:    16/07/11 12:56:47 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), A. Kusakin (Fesenkov Astrophysical Institute), P. 
Minaev (IKI), I. Reva (Fesenkov Astrophysical Institute), A. Volnova 
(IKI), A. Pozanenko (IKI) report on behalf of larger GRB follow-up 
collaboration:

We observed the field of GRB 160625B (Dirirsa et al., GCN 19580; Burns 
et al. GCN 19581) with Zeiss-1000 (East) 1-m telescopes of Tien Shan 
Astronomical Observatory. We obtained several images in R filter on July 
8 and 10. We detect optical afterglow of  GRB 160625B (Troja et al., GCN 
19588; Oates  et al., GCN  19589). Preliminary photometry of a combined 
image is following

Date       UT start   t-T0    Filter  Exp.   OT     Err.   UL
                       (mid, days)     (s)

2016-07-08 19:01:43   12.9172 R       30*300 21.60  0.15  22.7
2016-07-10 18:19:18   14.8713 R       29*300 21.64  0.08  23.3


Photometry is based on nearby USNO-B1.0 stars reported in GCN 19605 
(Mazaeva et. al).


GRB_name: GRB160709A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19681
SUBJECT: GRB 160709A, Swift-BAT detection and localization
DATE:    16/07/11 23:01:33 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

T. Sakamoto (AGU), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), J. P. Norris (BSU),
M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team):

At 19:49:03.464 UT on 2016-07-09, BAT detected a count rate increase and
a sub-threshold signal in the image. Due to the sub-threshold nature, this event
did not trigger a normal burst event-by-event response. Using the data set from
T-2 to T+8 sec from the recent telemetry downlink, the ground analysis found
an 8.8 sigma detection in a 10-s image in 15-350 keV. As discussed below,
this is likely the same burst, GRB160709A, that was detected by Fermi/GBM
(Jenke et al. GCN Circ. 19676), Fermi/LAT (Guiriec et al. GCN Circ. 19675),
and Konus-Wind (Frederiks et al. GCN Circ. 19677).

The BAT ground-calculated position is RA, Dec = 235.996, -28.188 deg which is
  RA(J2000)  =  15h 43m 59.1s
  Dec(J2000) = -28d 11' 18.2"
with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 19%.

The mask-weighted light curve shows a multi-peaked structure that starts at ~T0
and peaks at ~T+0.8 s. The main pulses end at ~T+1 s, but there are some
weak emissions that continue beyond the event data range. T90 (15-350 keV)
estimated from the raw light curve is 4.8 +- 1.6 sec (estimated error including
systematics).

The time-averaged spectrum from T+0.0 to T+4.8 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.11 +- 0.28.  The fluence in the 15-150 keV band is 4.5 +- 0.7 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.30 sec in the 15-150 keV band
is 2.7 +- 0.4 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

Using a 16-ms binned light curve, the lag of the initial pulse (~T0 to ~T+1 s)
for the 100-350 keV to 25-50 keV bands is 3 (+/-5) ms (with 1-sigma error).
Using a 4-ms binned light curve, the lag of the initial pulse for the same energy
bands is 6 (+/-5) ms. These values are consistent with those from a short GRB.

The detection time of this burst is only ~0.04 s from the Fermi/GBM trigger
time of GRB160709A (Jenke et al., GCN Circ. 19676). Also, the burst structure
is very similar to the one seen in the GBM. We thus believe the BAT detection
is highly likely to be GRB160709A.

However, we note that the BAT location is ~0.33 degrees from the LAT location
and outside of the reported LAT error circle of 0.18 deg (statistical error only;
Guiriec et al. GCN Circ. 19675). The large dispersion in the position
measurements may be explained by the unknown systematic uncertainty in the
LAT position. Nonetheless, we cannot rule out the possibility that these are
independent events.

The BAT location for this burst is covered by the XRT tiling search. No XRT or
UVOT afterglows are found within the BAT error circle.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/703769/BA/


GRB_name: GRB160709A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19682
SUBJECT: GRB 160709A: MASTER early imaging Swift BAT error box 
DATE:    16/07/12 08:54:53 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, N.Tyurina, P.Balanutsa, V.Kornilov, A.Kuznetsov, 
D.Kuvshinov,
Lomonosov Moscow State University, Sternberg Astronomical Institute

D.Buckley, S. Potter, A.Kniazev, M.Kotze
South African Astronomical Observatory

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
The Instituto de Astrofisica de Canarias

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

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

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

R.Podesta, C.Lopez and F.Podest
Observatorio Astronomico Felix Aguilar (OAFA)

H.Levato and C.Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)


MASTER-SAAO  robotic telescope (2x4 square 
degrees twin telescope, http://observ.pereplet.ru)  was pointing 
to the  Swift-BAT error box (Sakamoto et al., GCN 19681) during Fermi-GBM 
alert inspection   1727 sec after FERMI GBM notice time (Jenke, GCN 
19676) and before 9709 sec FERMI LAT notice time and 1750 sec after trigger
time at  2016-07-09 20:18:14 UT. On our 180s exposure  set we  not found OT
within Swift-BAT (Sakamoto et al., GCN 19681) brighter then 19.6.

The inspection and references images are available at 
http://master.sai.msu.ru/static/GRB160709A_MASTER_SAAO.png  .

The message may be cited.


GRB_name: GRB160625B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19683
SUBJECT: GRB 160625B: Global MASTER-Crimea prompt optical emission detection (fwd)
DATE:    16/07/12 19:03:59 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, N.Tyurina, V.Kornilov,
P.Balanutsa,  A.Kuznetsov, D.Kuvshinov,
Lomonosov Moscow State University, Sternberg Astronomical Institute

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
The Instituto de Astrofisica de Canarias

D.Buckley, S. Potter, A.Kniazev, M.Kotze
South African Astronomical Observatory

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

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

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

Ricardo Podesta, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)

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



MASTER-Crimea  robotic telescope (testing camera 20 cm)  pointing to LAT 
error box (Dirirsa et al., GCN 19580) 12  sec after LAT notice time and 66 
sec after trigger time at 
2016-06-25  22:44:30 UT in unfiltered mode. The OT was about 9.55 +-0.01 
mag at this  moment ( 0.2B + 0.8R with respect  to USNOB1.0 stars)
The automatic photometry and astrometry  are:


+id-      time            coord2000  mag

179841451 22:44:30.055 20h 34m 23.49s , +06d 55m 07s.6  9.55
179890027 22:44:30.055 20h 34m 23.52s , +06d 55m 07s.9 10.11
179845079 22:45:00.899 20h 34m 23.50s , +06d 55m 07s.8 10.03
179878574 22:45:37.806 20h 34m 23.52s , +06d 55m 08s.0 10.54
179909653 22:46:25.105 20h 34m 23.53s , +06d 55m 07s.8 11.46
179883969 22:46:25.105 20h 34m 23.52s , +06d 55m 07s.8 11.04
179895778 22:47:20.57 20h 34m 23.52s , +06d 55m 07s.9 11.52
179901960 22:48:26.68 20h 34m 23.52s , +06d 55m 08s.0 11.91


The delay with internet problems last time .


The message may be cited.


GRB_name: GRB160712A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19684
SUBJECT: GRB 160712A: Swift detection of a burst
DATE:    16/07/12 20:07:26 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

L. M. Z. Hagen (PSU), S. D. Barthelmy (GSFC), D. N. Burrows (PSU),
S. B. Cenko (GSFC), F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL)
and B. Sbarufatti (INAF-OAB/PSU) report on behalf of the Swift Team:

At 19:53:36 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 160712A (trigger=704155).  Swift did not slew immediately
due to an observational constraint. 
The BAT on-board calculated location is 
RA, Dec 304.149, -26.981 which is 
   RA(J2000) = 20h 16m 36s
   Dec(J2000) = -26d 58' 52"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a long burst with 
a duration of ~ 20 s and containing a short spike. The peak count rate 
was ~4500 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+47.3
minutes. There will be no XRT or UVOT data until this time. 

Burst Advocate for this burst is L. M. Z. Hagen (lea.zernow.hagen 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: GRB160712A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19685
SUBJECT: GRB 160712A: Global MASTER-Net optical observation
DATE:    16/07/12 20:34:55 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

D.Buckley, S. Potter, A.Kniazev, M.Kotze
South African Astronomical Observatory

E. Gorbovskoy, V. Lipunov, N.Tyurina, V.Kornilov,
P.Balanutsa,  A.Kuznetsov, D.Kuvshinov,
Lomonosov Moscow State University, Sternberg Astronomical Institute

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
The Instituto de Astrofisica de Canarias

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

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

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

Ricardo Podesta, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)

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

MASTER-SAAO  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in SAAO was pointed to the  GRB160712.83 26 sec after notice time 
and 48 sec after trigger time at 2016-07-12 19:54:28 UT. On our first (10s 
exposure)  set we haven't found optical transient  within SWIFT error-box 
(ra=20 16 35 dec=-26 58 52 r=0.050000).
The 5-sigma upper limit has been about 16.7 mag
The message may be cited.


The message may be cited.


GRB_name: GRB160712A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19686
SUBJECT: GRB 160712A: Swift-XRT observations
DATE:    16/07/12 21:28:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.A. Kennea (PSU), G. Cusumano (INAF-IASF PA), M. Perri (ASDC), 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 160712A at 20:47:52.7 UT,
3256.7 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 304.1600, -26.9582 which is equivalent to:
   RA(J2000)  = 20h 16m 38.40s
   Dec(J2000) = -26d 57' 29.4"
with an uncertainty of 2.1 arcseconds (radius, 90% containment). This
location is 89 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 (8.30 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 2.7
(+2.97/-2.55) x 10^21 cm^-2 (90% confidence). 


GRB_name: GRB160712A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19687
SUBJECT: GRB 160712A: Initial Swift/UVOT observations
DATE:    16/07/12 21:41:50 GMT
FROM:    Lea Hagen at PSU  <lea.zernow.hagen@gmail.com>

L. M. Z. Hagen (PSU) reports on behalf of the Swift/UVOT team:

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 3998 seconds after the BAT trigger (Hagen et al., GCN Circ.
19684). 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 (Kennea et al., GCN Circ. 19686). 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 0.08.


GRB_name: GRB160624A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19688
SUBJECT: GRB 160624A: 15 GHz upper limits from AMI
DATE:    16/07/12 22:21:47 GMT
FROM:    Kunal Mooley at Oxford U  <kunal.mooley@physics.ox.ac.uk>

K. P. Mooley, T. D. Staley, R. P. Fender (Oxford), G. E. Anderson 
(Curtin), T. Cantwell (Manchester), C. Rumsey, D. Titterington, S. 
Carey, J. Hickish, Y. C. Perrott, N. Razavi-Ghods, P. Scott (Cambridge), 
K. Grainge, A. Scaife (Manchester)

The AMI Large Array robotically triggered on the Swift alert for GRB 
160624A (D'Ai et al., GCN 19560) as part of the 4pisky program, and 
subsequent follow up observations were obtained up to 10 days 
post-burst. Our observations at 15 GHz on 2016 Jun 24.97, Jun 29.18, and 
Jul 02.05 (UT) do not reveal any radio source at the XRT location 
(Beardmore et al., GCN 19566), with 3sigma upper limits of 268 uJy, 93 
uJy, and 114 uJy respectively.

We thank the AMI staff for scheduling these observations. The AMI-GRB 
database is a log of all GRB follow up observations with the AMI, and is 
available at http://4pisky.org/ami-grb/.


GRB_name: GRB160629A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19689
SUBJECT: GRB 160629A: 15 GHz detections and upper limits from AMI
DATE:    16/07/12 22:25:43 GMT
FROM:    Kunal Mooley at Oxford U  <kunal.mooley@physics.ox.ac.uk>

K. P. Mooley, T. D. Staley, R. P. Fender (Oxford), G. E. Anderson 
(Curtin), T. Cantwell (Manchester), C. Rumsey, D. Titterington, S. 
Carey, J. Hickish, Y. C. Perrott, N. Razavi-Ghods, P. Scott (Cambridge), 
K. Grainge, A. Scaife (Manchester)

We observed the INTEGRAL/IBIS GRB 160629A (Gotz et al., GCN 19621) with 
the AMI Large Array at 15 GHz on 2016 Jul 01.23, Jul 02.23, Jul 04.19, 
and Jul 08.19 (UT) as part of the 4pisky program. We detect a transient 
radio source consistent with the SAO RAS location (Sokolov et al., GCN 
19623) at 219+/-49 uJy and 128+/-37 uJy in the first two epochs, and 
obtain 3sigma upper limits of 135 uJy and 243 uJy in the later two epochs.

We thank the AMI staff for scheduling these observations. The AMI-GRB 
database is a log of all GRB follow up observations with the AMI, and is 
available at http://4pisky.org/ami-grb/.


GRB_name: GRB160712A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19690
SUBJECT: GRB 160712A: Enhanced Swift-XRT position
DATE:    16/07/13 01:33:29 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 1053 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 160712A, 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 = 304.15987, -26.95819 which is equivalent
to:

RA (J2000): 20h 16m 38.37s
Dec (J2000): -26d 57' 29.5"

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: GRB160712A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19691
SUBJECT: GRB 160712A: Skynet R-COP observations
DATE:    16/07/13 02:31:08 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, J. Haislip, D. Reichart, A. Verveer, T. Spuck, J. Moore, N. Frank, M. Maples, D. Dutton, R. Gao, R. Joyner, J. Martin, M. Paggen, J. A. Crain, K. Ivarsen, A. LaCluyze, M. Nysewander, B. Barlow, J. LaCluyze, L. Lanier, D. Moffett, B. Tobias, G. Bennett, J. Da Rocha, M. Dryzer, D. Dutton, J. Elliott, C. Ferguson, R. J. Hegedus, E. Lutz, B. McCormack, T. Melo, K. Otto, R. Pierce, S. Simon, E. Smith, J. Taylor, M. Tierney, D. Varvir, and A. Vasquez Soto report:

Skynet observed the Swift BAT/XRT localization of GRB 160712A (Hagen et al., GCN 19684, Swift trigger=704155) with the 14" R-COP telescope at Perth Observatory, Australia. Starting at 2016-07-12 19:58 UT and continuing until 20:30 UT (t=4.3m-31.4m post-trigger), Skynet took a total of 17 20-160s exposures in the B, V, R, and I bands. We stacked subsets of these images to maximize the S/N ratio, and detected no optical source in any band at the XRT position.  Our 3-sigma limiting magnitudes are:

====================
tmid  fil  limit
====================
23m   B   >16.7
26m   V   >17.2
23m   R   >17.7
29m   I   >16.9
====================

Limiting magnitudes are in the Vega System, calibrated to 5 APASS stars in the field.  Magnitudes have not been corrected for line-of-sight Milky Way dust extinction, with expected E(B-V)=0.07 (Schlafly & Finkbeiner 2011).

No further Skynet observations are scheduled.


GRB_name: GRB160712A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19692
SUBJECT: GRB 160712A: Swift-XRT refined Analysis
DATE:    16/07/13 06:56:33 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

S.L. Gibson (U. Leicester), J.P. Osborne (U. Leicester), K.L. Page (U.
Leicester), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), A. Maselli 
(INAF-IASFPA), L.M. McCauley (PSU), J.A. Kennea (PSU), B. Sbarufatti
(INAF-OAB/PSU) and L. M. Z. Hagen (PSU) report on behalf of the
Swift-XRT team:

We have analysed 3.8 ks of XRT data for GRB 160712A (Hagen et al. GCN
Circ. 19684), from 4.0 ks to 17.2 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. 19690).

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.51 (+0.25, -0.22).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.91 (+0.28, -0.26). The
best-fitting absorption column is  2.8 (+1.3, -1.1) x 10^21 cm^-2, in
excess of the Galactic value of 8.3 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.8 x 10^-11 (5.3 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.8 (+1.3, -1.1) x 10^21 cm^-2
Galactic foreground: 8.3 x 10^20 cm^-2
Excess significance: 3.0 sigma
Photon index:      1.91 (+0.28, -0.26)

If the light curve continues to decay with a power-law decay index of
1.51, the count rate at T+24 hours will be 2.1 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 7.9 x
10^-14 (1.1 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/00704155.

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


GRB_name: GRB160712A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19693
SUBJECT: GRB 160712A: GROND observations
DATE:    16/07/13 07:45:48 GMT
FROM:    Thomas Kruehler at MPE Garching  <kruehler@mpe.mpg.de>

T. Kruehler and J. Greiner (all MPE Garching) report on behalf
of the GROND team:

We observed the field of GRB 160712A (Swift trigger 704155; Hagen et
al., GCN #19684) simultaneously in g'r'i'z'JHK with GROND (Greiner
et al. 2008, PASP 120, 405) mounted at the 2.2m MPG telescope at the
ESO La Silla Observatory (Chile).

Observations started at 03:18:21 UT on 2016-07-13, 7.4 hr after the GRB
trigger. They were performed at an average seeing of 2â€.2, at an
average airmass of 1.1, and severely affected by passing clouds.

We found a single source sightly outside of the XRT errorcircle at:

RA (J2000) = 20:16:38.50
Dec. (J2000) = -26:57:30.7

with an uncertainty of 0".5 in each coordinate. The distance to the
center of the XRT error circle (90% confidence radius 1".5 arcsec)
is 2".2.

Based on images with 24.2 min of total exposure in g'r'i'z'
and 24.0 min in JHK at a mid-time of 03:57:19 UT on 2016-07-13,
we derive the following preliminary magnitudes and upper limits
(all in AB system):

g > 23.3 mag
r = 22.9 +- 0.3 mag
i = 21.7 +- 0.3 mag
z = 21.4 +- 0.3 mag
J = 20.5 +- 0.2 mag
H = 20.2 +- 0.2 mag
K = 20.0 +- 0.3 mag

Given magnitudes are calibrated against USNO as well as 2MASS
field stars and are not corrected for the expected Galactic foreground
extinction corresponding to a reddening of E_(B-V) = 0.065 mag in the
direction of the burst (Schlafly & Finkbeiner 2011).

No statement about variability can be made at this point. Given its
position somewhat outside of the XRT error circle, it is uncertain
whether this source is related to GRB 160712A.


GRB_name: GRB160712A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19694
SUBJECT: Konus-Wind observation of GRB 160712A
DATE:    16/07/13 12:23:48 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

D. Frederiks, S. Golenetskii, R.Aptekar, P. Oleynik, M. Ulanov,
D. Svinkin, A. Tsvetkova, A.Lysenko, A. Kozlova, and T. Cline,
on behalf of the Konus-Wind team, report:

The long GRB 160712A (Swift/BAT observation: Hagen et al., GCN 19684)
triggered Konus-Wind at T0=71621.420 s UT (19:53:41.420).

The light curve statrs with a short spike followed
by a gradually decaying emission.
The total duration of the burst is ~25 s.
The emission is seen up to ~4 MeV.

As observed by Konus-Wind, the burst had a fluence of
(6.5 Â± 2.0)x10^-6 erg/cm2 and a 64-ms peak energy flux,
measured from T0+0.128, of (2.7 Â± 0.8)x10^-6 erg/cm2
(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 - 4 MeV range by a cutoff power-law
(CPL) function with the following model parameters:
the photon index alpha = -0.17(-0.57,+0.87),
and the peak energy Ep = 460(-117,+204) keV,
chi2 = 72/73 dof.
Fitting this spectrum with the GRB (Band) function yields
the same alpha and Ep with only an upper limit on beta of -2.3,
chi2 = 72/72 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB160712_T71621/

All the quoted errors are estimated at the 90% confidence level.
All the presented results are preliminary.


GRB_name: GRB160712A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19695
SUBJECT: GRB 160712A: RATIR Optical and NIR Observations
DATE:    16/07/13 13:46:19 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), Ori Fox (STScI), J. Xavier Prochaska (UCSC), Josh Bloom
(UCB), Antonino Cucchiara (GSFC/STScI), Owen Littlejohns (ASU),
Enrico Ramirez-Ruiz (UCSC), JosÃ© A. de Diego (UNAM), Leonid
Georgiev (UNAM), JesÃºs GonzÃ¡lez (UNAM), Carlos RomÃ¡n-ZÃºÃ±iga
(UNAM), Neil Gehrels (GSFC), Harvey Moseley (GSFC), John Capone
(UMD), V. Zach Golkhou (ASU), and Vicki Toy (UMD) report:

We observed the field of GRB 160712A (Hagen, et al., GCN 19684)
with the Reionization and Transients Infrared Camera (RATIR;
www.ratir.org) on the 1.5m Harold Johnson Telescope at the
Observatorio AstronÃ³mico Nacional on Sierra San Pedro MÃ¡rtir from
2016/07 13.21 to 2016/07 13.42 UTC (9.05 to 14.30 hours after the
BAT trigger), obtaining a total of 3.56 hours exposure in the r
and i bands and 1.45 hours exposure in the Z, Y, J, and H bands.

We detect a source slightly outside of the XRT error circle
(Beardmore, et al., GCN 19690), and consistent with the GROND
position (Kruehler, et al., GCN 19693). In comparison with the
USNO-B1 and 2MASS catalogs, we obtain the following detections:

   r    22.77 +/- 0.08
   i    21.55 +/- 0.03
   Z    20.93 +/- 0.05
   Y    20.44 +/- 0.05
   J    20.27 +/- 0.06
   H    20.15 +/- 0.08

These magnitudes are in the AB system and are not corrected for
Galactic extinction in the direction of the GRB.
Further observations to determine whether the source is fading
are planned.

We thank the staff of the Observatorio AstronÃ³mico Nacional in
San Pedro MÃ¡rtir.


GRB_name: GRB160712A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19696
SUBJECT: GRB 160712A: Swift/UVOT Upper Limits
DATE:    16/07/13 18:19:55 GMT
FROM:    Lea Hagen at PSU  <lea.zernow.hagen@gmail.com>

L. M. Z. Hagen (PSU) reports on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 160712A
3998 s after the BAT trigger (Hagen et al., GCN Circ. 19684). No
optical afterglow consistent with the XRT position (Beardmore et al.,
GCN Circ. 19690) or the possible optical afterglow candidate (Kruehler
et al., GCN Circ. 19693; Troja et al., GCN Circ. 19695) 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 exposures are:

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

white             3998         4148          147        >20.47
v                 4154         4354          196        >19.04
b                 4974         5027           52        >19.17
u                 4769         4969          196        >19.66
uvw1              4564         4764          196        >19.58
uvm2              4359         4559          196        >19.52

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: GRB160714A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19697
SUBJECT: GRB 160714A: Swift detection of a short burst
DATE:    16/07/14 02:28:39 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. H. Siegel (PSU), J. A. Kennea (PSU), A. Y. Lien (GSFC/UMBC),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL) and
B. Sbarufatti (INAF-OAB/PSU) report on behalf of the Swift Team:

At 02:19:15 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 160714A (trigger=704310).  Swift did not slew immediately
due to an observational constraint. 
The BAT on-board calculated location is 
RA, Dec 234.461, +63.831 which is 
   RA(J2000) = 15h 37m 51s
   Dec(J2000) = +63d 49' 53"
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 0.5 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~0.3 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+26.0
minutes. There will be no XRT or UVOT data until this time. 

Burst Advocate for this burst is M. H. Siegel (siegel AT swift.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: GRB160714A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19698
SUBJECT: GRB 160714A: Swift-XRT observations
DATE:    16/07/14 03:19:01 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

M. Perri (ASDC), G. Tagliaferri (INAF-OAB), 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 160714A at 02:47:12.7 UT,
1677.2 seconds after the BAT trigger. No source was detected in 1.0 ks
of promptly downlinked data, which covered 88% of the BAT error circle.
We are waiting for the full dataset to detect and localise the XRT
counterpart.


GRB_name: GRB160714A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19699
SUBJECT: GRB 160714A: Optical observations from OSN
DATE:    16/07/14 03:49:13 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), A. Sota (IAA-CSIC) 
report on behalf of a larger collaboration:

We have observed the field of GRB 160714A (Siegel et al. GCN 
19697) with the 1.5m OSN telescope, in Granada (Spain). 
Observations started at 2:33 UT (14 min after the GRB onset) and 
consisted of 3x180s + 4x300s I-band images. Each of the 
individual images cover the complete BAT error circle. In a 
preliminary analysis we detect no new source within the BAT error 
box down to a 3-sigma limit of I(AB) > 20.5 mag in the first image, 
and down to I(AB) > 21.5 mag in the combined image (mean time 
2:48 UT, 29 minutes after the burst), as compared to SDSS data.


GRB_name: GRB160709A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19701
SUBJECT: GRB 160709A CALET Gamma-Ray Burst Monitor detection
DATE:    16/07/14 06:57:55 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

Y. Asaoka (Waseda U), A. Yoshida, T. Sakamoto, Y. Kawakubo, M. Moriyama, 
Y. Yamada (AGU), K. Yamaoka (Nagoya U), S. Nakahira (JAXA), I. Takahashi (IPMU), 
S. Ozawa, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), W. Ishizaki (ICRR), 
M. L. Cherry (LSU), S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena) 
and the CALET collaboration:

The short-duration GRB 160709A (Guiriec, et al., GCN circ. 19675; 
Jenke, et al., GCN circ. 19676; Frederiks, et al. GCN circ. 19677) 
triggered the CALET Gamma-ray Burst Monitor (CGBM) at 19:49:04.67 
on 9 July 2016.  No real time CGBM GCN notice was distributed about 
this trigger because the real time communication from the ISS was 
off (loss of signal) between 19:42 and 20:04. The burst signal was 
seen by all CGBM instruments.  

The light curve of the SGM shows a single starting at T-0.2 sec, 
peaking at T0-0.1 sec and ending at T+0.2 sec.  The T90 duration 
measured by the SGM data is 0.38 +- 0.04 sec (600-3000 keV).

The light curve is available at

http://cgbm.calet.jp/cgbm_trigger/flight/1152128868/

The CALET data used in this analysis are provided by the Waseda 
CALET Operation Center located at the Waseda University.


