# GCN_circulars

GRB_name: GRB140606A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16353
SUBJECT: GRB 140606A: Swift detection of a short hard burst
DATE:    14/06/06 11:14:01 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. C. Stroh (PSU), A. P. Beardmore (U Leicester),
J. R. Cummings (NASA/UMBC), P. A. Evans (U Leicester),
N. Gehrels (NASA/GSFC), J. A. Kennea (PSU),
F. E. Marshall (NASA/GSFC), P. Romano (INAF-IASFPA) and
R. L. C. Starling (U Leicester) report on behalf of the Swift Team:

At 10:58:13 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140606A (trigger=600951).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 201.808, +37.579 which is 
   RA(J2000) = 13h 27m 14s
   Dec(J2000) = +37d 34' 44"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double peak
structure with a duration of about 1 sec.  The peak count rate
was ~3000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

XRT is currently not collecting science data. There will be no XRT data
on this burst until the anomaly is resolved. Details are given in GCN
Circ. 16349. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 67 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 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
0.01. 

Burst Advocate for this burst is M. C. Stroh (stroh AT astroh.org). 
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: GRB140606A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16354
SUBJECT: GRB 140606A: Swift-BAT refined analysis
DATE:    14/06/06 18:33:36 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), M. C. Stroh (PSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+962 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 140606A (trigger #600951)
(Stroh, et al., GCN Circ. 16353).  The BAT ground-calculated position is
RA, Dec = 201.799, 37.599 deg, which is 
   RA(J2000)  =  13h 27m 11.7s 
   Dec(J2000) = +37d 35' 56.5" 
with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 86%.
 
The mask-weighted light curve shows a single spike starting at ~T+0.0,
peaking at ~T+0.1, and ending at ~T+0.3 sec.  T90 (15-350 keV) is
0.34 +- 0.09 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.04 to T+0.35 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
0.53 +- 0.36.  The fluence in the 15-150 keV band is 5.1 +- 1.0 x 10^-8 erg/cm2.
The 1-sec peak photon flux measured from T-0.34 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/600951/BA/


GRB_name: GRB140606A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16357
SUBJECT: GRB 140606A: Swift-XRT upper limits
DATE:    14/06/06 20:58:06 GMT
FROM:    Michael Stroh at PSU/Swift  <stroh@astroh.org>

M. C. Stroh, J. A. Kennea (PSU), N. Gehrels (GSFC) and D. Malesani (DARK/NBI) report on behalf of the Swift-XRT team:

The Swift-XRT began observing the field of GRB 140606A 4.6 ks after the event (Stroh et al., GCN Circ. 16353). In 2.4ks of Photon Counting (PC) mode data, no source was found in the revised BAT error circle (Cummings et al., GCN Circ. 16354). The three sigma upper limit (0.5-10 keV) is 7.4e-3 counts s^-1.

The delayed XRT response was due to the XRT anomaly (Burrows and Kennea, GCN Circ. 16356).

This circular is an official product of the Swift team.


GRB_name: GRB140606A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16358
SUBJECT: GRB 140606A: Swift/UVOT Upper Limits
DATE:    14/06/06 21:40:25 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and M. C. Stroh (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140606A
68 s after the BAT trigger (Stroh et al., GCN Circ. 16353).
No optical afterglow consistent with the BAT position
(Cummings et al. GCN Circ. 16354)
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            68          218          147         >21.1
u_FC               280          530          246         >20.4
white               68         6243          746         >21.6
v                  609         6654          471         >20.2
b                  535         6039          269         >20.8
u                  280         5834          442         >20.8
w1                 833         7064          452         >20.8
m2                1063         6859          413         >20.6
w2                1188         6449          413         >20.8

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: GRB140606A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16359
SUBJECT: GRB 140606A: Nanshan optical upper limit
DATE:    14/06/06 23:25:24 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), H.-B. Niu, T.-Z. Yang, A. Esamdin, L. Ma (XAO) report:

We observed the BAT field of GRB 140606A (Stroh et al., GCN 16353)
using the 1m telescope located at Nanshan, Xinjiang, China.
Observations started at 15:49:48 UT on 2014/06/06 (4.86 hr after the
burst) and a series of 300s/500s R-band frames were obtained.

The optical afterglow of the burst is not detected within the BAT
error circle down to a limiting magnitude of R=20.8 mag, calibrated
with the nearby SDSS field.


GRB_name: GRB140606A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16361
SUBJECT: GRB 140606A: BOOTES-2 optical upper limit
DATE:    14/06/07 08:09:09 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

M. Jelinek, R. Cunniffe, A. GonzÃ¡lez-RodrÃ­guez, S. Jeong, O. Lara-Gil, S.
R. Oates, J. C. Tello (IAA-CSIC Granada), J. Gorosabel (IAA-CSIC, UPV-EHU)
and A. J. Castro-Tirado (IAA-CSIC, ISA-UMA), report:

"Following the detection of GRB 140606A by Swift (Stroh et al., GCNC
16353), the 0.6m TELMA robotic telescope at the BOOTES-2 astronomical
station Malaga (Spain), observed the GRB location under non optimal
weather conditions. A coadd of 105 images (60s each, iâ€™-band filter) taken
starting at 20:46 UT and ending at 01:33 UT (i.e. 10 hr post burst)
reveals no optical afterglow down to 18.8 mag."


GRB_name: GRB140606B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16363
SUBJECT: GRB 140606B: Fermi GBM detection
DATE:    14/06/07 16:05:57 GMT
FROM:    Eric Burns at U of Alabama  <EricKayserBurns@gmail.com>

E. Burns (UAH) reporting on behalf of the Fermi GBM Team:

"At 03:11:51.86 UT on 06 June 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140606B (trigger 423717114 / 140606133).

The on-ground calculated location, using the GBM trigger
data, is RA = 327.9, DEC = +33.7 (J2000 degrees,
equivalent to 21 h 51 m, 33 d 41 '), with an uncertainty
of 1.00 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).

The angle from the Fermi LAT boresight is 66 degrees.

The optical afterglow candidates reported by iPTF (Singer et al.
GCN 16360) lie within the 1-sigma (statistical and systematic)
uncertainty regions surrounding the GBM localization.

The GBM light curve shows one long peak with a
noisy tail with a duration (T90) of about 23.6 s (50-300 keV).
The time-averaged spectrum from T0-3.0 s to T0+12.3 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.22 +/- 0.04 and
the cutoff energy, parameterized as Epeak, is 473.00 +/- 82.60 keV

The event fluence (10-1000 keV) in this time interval is
(9.018 +/- 0.369)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+0.58 s in the 10-1000 keV band is
13.31 +/- 0.37 ph/s/cm^2.


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


GRB_name: GRB140607A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16364
SUBJECT: GRB 140607A: Swift detection of a burst
DATE:    14/06/07 17:27:16 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

V. Mangano (PSU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), S. B. Cenko (GSFC),
C. B. Markwardt (NASA/GSFC), D. M. Palmer (LANL) and
T. N. Ukwatta (MSU) report on behalf of the Swift Team:

At 17:13:31 UT, the Swift Burst Alert Telescope (BAT) triggered on
GRB 140607A, (trigger=601051).  Swift did not slew due to the Sun constraint. 
The BAT on-board calculated location is 
RA, Dec 86.380, +18.917, which is 
   RA(J2000)  = +05h 45m 31s
   Dec(J2000) = +18d 55' 00"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As is typical for image triggers the real-time BAT
light curve shows nothing significant.  However, the image significance
of 7.87 sigma gives us confidence that this is a real event even
in the absence of XRT and UVOT follow-up. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 22:00 UT on 2014 August 05. There will thus be no XRT or
UVOT data for this trigger before this time. 

Burst Advocate for this burst is V. Mangano (vxm22 AT psu.edu). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB140606B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16365
SUBJECT: GRB 140606B / Fermi 432717114 / iPTF 14bfu: Keck redshift
DATE:    14/06/08 02:09:34 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley, Y. Cao (Caltech), M. Kasliwal (Carnegie), and E. Kirby 
(UCI) report:

On the night of 2014-06-07 starting at 19:16 (UT) we acquired two 900 
second optical spectra of iPTF14bfu (Singer et al., GCN 16360), an 
optical transient in the error circle of GRB 140606B / Fermi 432717114 
(Burns et al., GCN 16360), with the DEIMOS spectrograph on the Keck II 
10 meter telescope.

In the reduced spectrum of this object we identify emission lines from 
OII, OIII (5007) and H-alpha, as well as absorption features from Ca II 
(H+K), at a consistent redshift of z = 0.384.  A serendipitous galaxy 
offset by ~2 arcseconds (10 kpc) along the slit shows the same emission 
lines at identical redshift but no detectable continuum.

Given this redshift, the high luminosity inferred for the optical 
transient at the time of the initial detection (absolute magnitude ~ 
-21.7) favors the association of this source as the optical afterglow of 
GRB 140606B.


GRB_name: GRB140606B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16366
SUBJECT: GRB 140606B: Swift XRT position
DATE:    14/06/08 15:34:22 GMT
FROM:    Vanessa Mangano at PSU  <vanessa@ifc.inaf.it>

V. Mangano (PSU), P.A. Evans and M.R. Goad (U. Leicester) report
on behalf of the Swift-XRT team:


We have analysed 5 ks of XRT data for the Fermi/GBM-detected burst:
GRB 140606B,  from 184.4 ks to 192.6 ks after the  Fermi/GBM trigger.
The data are entirely in Photon Counting (PC) mode.
Using 4979 s of XRT Photon Counting mode data and 4 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 =
328.12501, 32.01458 which is equivalent to:

RA (J2000):  21 52 30.00
Dec (J2000): +32 00 52.5

with an uncertainty of 2.3 arcsec (radius, 90% confidence).
This position is a 5.2 arcsec from source iPTF 14bfu from
GCN Circular 16360.

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).

We cannot determine at the present time whether the source is fading.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020384.

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


GRB_name: GRB140606B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16368
SUBJECT: GRB 140606B:  Swift/UVOT Upper Limits
DATE:    14/06/09 02:46:27 GMT
FROM:    Margaret Chester at PSU  <chester@swift.psu.edu>

M. M. Chester (PSU) and V. Mangano (PSU) report on behalf of the Swift/UVOT team:

The Swift/UVOT observed the field of the Fermi/GBM-detected burst GRB 140606B beginning 184.4 ks after the Fermi/GBM trigger (Burns et al. GCN Circ. 16363).  No source consistent with iPTF14bfu, the optical counterpart proposed by Singer et al. (GCN Circ. 16360) and Perley et al. (GCN Circ. 16365), 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) are given in the following table:

Filter   T_start(s)   T_stop(s)   Exp(s)   Mag
u        185271       191914      1693     >21.1
b        186146       192611      1495     >20.9
v        184395       191055      1693     >20.6

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: GRB140606B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16369
SUBJECT: IPN Triangulation of GRB 140606B
DATE:    14/06/09 17:03:13 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

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

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

The long-duration GRB 140606B has been observed by Fermi (Burns GCN 
Circ. 16363), Konus-Wind, and MESSENGER (GRNS), so far, at about 11512 s 
UT (03:11:52).

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   327.109 (21h 48m 26s) +33.047 (+33d 02' 50")
  Corners:
   321.995 (21h 27m 59s) +37.333 (+37d 19' 58")
   321.768 (21h 27m 04s) +38.102 (+38d 06' 06")
   332.033 (22h 08m 08s) +27.958 (+27d 57' 29")
   332.250 (22h 09m 00s) +26.987 (+26d 59' 14")
  ---------------------------------------------
The error box area is 5.53 sq. deg, and its maximum
dimension is 14.18 deg (the minimum one is 0.414 deg).

This box may be improved.

Only two of the reported optical sources (Singer et al. GCN Circ. 
16360), namely iPTF14bfw and iPTF14bfu, are inside the box, and 
iPTF14bfw was found to be a constant source (Perley and Singer, GCN 
Circ. 16362).

The distance between the narrowest annulus (GBM-MESSENGER annulus with 3 
sigma half width of 0.207 deg) center line and the iPTF14bfu (the fading 
  source) is 2 arcsec, strengthening the association of the transient 
and the GRB.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB140606_T11511/IPN/

Details of the Konus-Wind observation will be given in a forthcoming GCN 
Circular.


GRB_name: GRB140607A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16370
SUBJECT: GRB 140607A: Swift-BAT refined analysis
DATE:    14/06/09 17:20:48 GMT
FROM:    Tilan Ukwatta at MSU  <tilan.ukwatta@gmail.com>

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

Using the data set from T-239 to ~T+240 sec from the recent
telemetry downlink, we report further analysis of BAT
GRB 140607A (trigger #601051) (Mangano, et al., GCN Circ. 16364).
The BAT ground-calculated position is RA, Dec = 86.373, 18.904 deg
which is
   RA(J2000)  =  05h 45m 29.5s
   Dec(J2000) = +18d 54' 15.5"
with an uncertainty of 1.9 arcmin, (radius, sys+stat,
90% containment). The partial coding was 16%.

The mask-weighted light curve shows a very weak multi-peaked
structure starting at ~T-10.0 sec, and ending around T+200 sec.
The burst location went out of the BAT FOV when Swift started slewing
around ~T+200 sec. Thus we have no data beyond ~T+240 sec and
we cannot say when the burst was ended. Based on the available data,
the T90 (15-350 keV) is 109.9 +- 18.5 sec (estimated error
including systematics).

The time-averaged spectrum from T-17.7 to T+103.8 sec is best fit
by a simple power-law model.  The power law index of the
time-averaged spectrum is 1.78 +- 0.23.  The fluence in the
15-150 keV band is 2.2 +- 0.3 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T+31.58 sec in the
15-150 keV band is 0.9 +- 0.4 ph/cm2/sec.  All the quoted errors
are at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://swift.gsfc.nasa.gov/results/BATbursts/601051/bascript/top.html


GRB_name: GRB140606A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16371
SUBJECT: GRB 140606A: AAO optical upper limit
DATE:    14/06/09 18:37:52 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), R. Inasaridze (AAO), O. Kvaratskhelia (AAO), V.
Ayvazian (AAO), Yu. Krugly (IA KhNU), I. Molotov (KIAM), A. Pozanenko
(IKI) report on behalf of larger GRB follow-up collaboration:

We observed a field of the Swift GRB 140606A (Stroh et al., GCN 16353) 
with AS-32 (0.7m) telescope of Abastumani Observatory starting on June,
06 (UT) 18:16:50. We obtained several unfiltered frames with exposure of 
each frame of 120 s. Within the BAT ground-calculated position (Cummings 
et al., GCN 16354) we do not detect evident variable source.

The details of the photometry are the following:

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

2014-06-06 18:16:50   0.33147    None   30*120   21.7

and based on SDSS star, R (gri -> R transformations by Lupton 2005):
J132717.88+373507.2
R_Lupton = 16.45 Â± 0.013


GRB_name: GRB140521A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16372
SUBJECT: GRB 140521A: AAO optical upper limit
DATE:    14/06/09 19:46:36 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), R. Inasaridze (AAO), O. Kvaratskhelia (AAO), V.
Ayvazian (AAO), Yu. Krugly (IA KhNU), I. Molotov (KIAM), A. Pozanenko 
(IKI) report on behalf of larger GRB follow-up collaboration:

We observed second epoch of the field of the Swift GRB 140521A (Troja et 
al., GCN 16311) with AS-32 (0.7m) telescope of Abastumani Observatory 
starting on May,  22 (UT) 21:34:30. We obtained several unfiltered 
frames with exposure of 120 s. In comparison with our first epoch 
observation (Volnova et al., GCN 16317)  we do not detect any variable 
source within the BAT ground-calculated position (Barthelmy et al.,  GCN 
16316).

A photometry is based on the same reference star used in first epoch 
(see GCN 16311):

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

2014-05-22 21:34:30 1.12809      None    38*120   21.5


GRB_name: GRB140606B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16373
SUBJECT: GRB 140606B: Swift XRT refined analysis
DATE:    14/06/09 21:37:28 GMT
FROM:    Vanessa Mangano at PSU  <vanessa@ifc.inaf.it>

V. Mangano and D.N. Burrows (PSU)
on behalf of the Swift-XRT team:

Swift XRT performed a second 5 ks ToO observation of the field of
GRB 140606B on June 09 2014, starting about 273.8 ks since the
Fermi/GBM trigger.
The XRT source reported in Mangano et al. (GCN Circ. 16366) is still
detected. The X-ray position, with a 90% error radius of 2.3 arcsec,
is 1.9 arcsec from  the optical  afterglow candidate iPTF14bfu
proposed by Singer et al. (GCN Circ. 16360).
The XRT light curve shows marginal evidence of decay. Further observations
are planned to confirm it.

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


GRB_name: GRB140606B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16374
SUBJECT: Konus-Wind observation of GRB 140606B
DATE:    14/06/10 12:20:20 GMT
FROM:    Anastasia Tsvetkova at Ioffe Institute  <tsvetkova@mail.ioffe.ru>

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

The long-duration GRB 140606B (Fermi-GBM detection: Burns, GCN 16319;
IPN triangulation: Golenetskii et al., GCN 16369) triggered Konus-Wind
at T0=11510.769 s UT (03:11:50.769).

The burst light curve shows a single pulse with a duration of ~8 s.
The emission is seen up to ~5 MeV.

As observed by Konus-Wind, the burst had a fluence of
6.6(-0.5,+0.5)x10^-6 erg/cm2, and a 64-ms peak flux, measured from
T0+0.752 s, of 2.9(-0.7,+0.7)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+8.448 s)
is best fit in the 20 keV - 5 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.60(-0.18,+0.20),
and Ep = 254(-27,+33) keV (chi2 = 78/73 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.9
(chi2 = 78/72 dof).

Assuming the redshift z=0.384 (Perley et al., GCN 16365)
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 2.5(-0.2,+0.2)x10^51 erg,
the peak luminosity L_iso is 1.5(-0.4,+0.4)x10^51 erg/s,
and the rest-frame peak energy, Ep,i, is 352(-37,+46) keV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140606_T11510/

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


GRB_name: GRB140610A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16375
SUBJECT: GRB 140610A: Swift detection of a burst
DATE:    14/06/10 16:46:34 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

P. A. Evans (U Leicester), S. D. Barthelmy (GSFC),
D. N. Burrows (PSU), J. R. Cummings (NASA/UMBC),
N. Gehrels (NASA/GSFC), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL), J. L. Racusin (NASA/GSFC) and M. H. Siegel (PSU)
report on behalf of the Swift Team:

At 16:31:29 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140610A (trigger=601259).  Swift will have a delayed slew
due to the Earth observing constraint.  The BAT on-board calculated location is 
RA, Dec 286.260, +3.907, which is 
   RA(J2000)  =  19h 05m 02s
   Dec(J2000) = +03d 54' 24"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a long peak
with a duration of at least 110 sec.  The peak count rate
was ~1500 counts/sec (15-350 keV), at ~3 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+49.4
minutes. There will be no XRT or UVOT data until this time. 

As the XRT is currently in Manual State due to an anomaly there will be
no prompt data products for this burst once Swift slews. The XRT is still 
collecting data, and the usual automated analyses will be available once the
data are on the ground. The XRT GCN circulars will be produced, once manual
verification has taken place due to the uncertain calibration of XRT in
its anomaly state. Please see GCN Circ. 16356 for details. 

Burst Advocate for this burst is P. A. Evans (pae9 AT star.le.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB140610A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16376
SUBJECT: GRB 140610A: Swift-XRT observations
DATE:    14/06/10 18:17:31 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 140610A at 17:58:18.3 UT,
5209.0 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source located at RA, Dec 286.26822, 3.90743
which is equivalent to:
   RA(J2000)  = 19h 05m 04.37s
   Dec(J2000) = +03d 54' 26.7"
with an uncertainty of 4.1 arcseconds (radius, 90% containment). This
location is 29 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 1.19
x 10^22 cm^-2 (Willingale et al. 2013). 


GRB_name: GRB140606B
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16377
SUBJECT: GRB140606B: DCT time of observation correction
DATE:    14/06/10 18:35:13 GMT
FROM:    Vicki Toy at UMD  <vtoy@astro.umd.edu>

V. Toy (UMD), A. Cucchiara (NASA-GSFC), J. Capone (UMD),
D. Kocevski (NASA-GSFC), S.B. Cenko (NASA-GSFC),
E. Troja (NASA-GSFC),  A. Kutyrev (NASA-GSFC), S. Veilleux (UMD),
and S. Gezari (UMD) report on behalf of a larger collaboration:

We report that in GCN 16367 we mistakenly estimated the time post-burst
for our DCT observations.

The optical transient was observed  from 2014/06/08 9:05 to 2014/06/08
09:41 UTC, which corresponds to 53.9 hours after the GRB discovery
(GCN 16363) and not 29.9 hours as reported.

We apologize for any confusion this might have caused and we thank
Dan Perley for pointing out this inconsistency.


GRB_name: GRB140610A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16379
SUBJECT: Konus-Wind observation of GRB 140610A
DATE:    14/06/11 10:31:09 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long GRB 140610A (Swift-BAT trigger #601259:
Evans et al., GCN 16375; T0(BAT)=16:31:29 UT)
was detected by Konus-Wind in the waiting mode.

The light curve shows a broad emission pulse which started
~3 s before the BAT trigger, peaked at ~T0(BAT)+3 s,
and lasted till ~T0(BAT)+150 s.

The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB140610A/

As observed by Konus-Wind, the burst had a fluence of
(1.6  0.3)x10^-5 erg/cm2 and a 2.944-s peak energy flux,
measured from ~T0(BAT)+3 s, of (2.3  0.3)x10^-7 erg/cm2
(both in the 20 - 10000 keV energy range).

Modeling the KW 3-channel time-integrated spectrum
(from T0(BAT)-3 s to T0(BAT)+150 s) by a power law
with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -1.75  0.15, and Ep = 200  93 keV.

All the quoted errors are estimated at the 1 sigma confidence level.
All the presented results are preliminary.


GRB_name: GRB140610A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16380
SUBJECT: GRB 140610A: Swift/UVOT Upper Limits
DATE:    14/06/11 12:33:01 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (UCL-MSSL) and P. A. Evans (U Leicester) report on behalf 
of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140610A 
3145 s after the BAT trigger (Evans et al., GCN Circ. 16375).
No optical afterglow consistent with the XRT position (Kennea et al. GCN 
Circ. 16376) 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          3145         3295          147         >21.1
white             3145         9879         1229         >22.3
v                 3301         4937          393         >19.9
b                 4122         5685          320         >20.6
u                 3916         5552          393         >20.5
w1                3712         5347          393         >20.5
m2                3506         5142          393         >20.3
w2                4533        10719         1017         >21.3

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 2.56 in the direction of the 
burst (Schlegel et al. 1998).


GRB_name: GRB140610A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16381
SUBJECT: GRB 140610A: MASTER  optical observations
DATE:    14/06/11 13:19:03 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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

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

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

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


MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Kislovodsk was pointed to the  GRB140610A   16931 sec (~4.7 h) 
after trigger time at 2014-06-10 21:13:41 UT directly after weather 
conditions became satisfactory. On our first single and coadd images  we 
haven't found optical transient  within Swift error-box (Evans et. al. GCN 
16375).
The 5-sigma unfiltgred upper limit has been about:


T_start             Exptime  dT[s]  Limit  Coadd
2014-06-10 21:13:41   180 s  17021  17.8    1
2014-06-10 21:13:41   540 s  17241  18.3    3
2014-06-10 21:13:41  3600 s  19079  18.5   20
2014-06-10 21:13:41 2x3600 s 19079  18.7   40*

* Coadd of images taken from two parallel tubes.
dT is middle time of exposition (dT = T_middle - T_trigger)
Our white (clear) band is well described by a parity 0.8R+0.2B (USNO B1).
The very high extinction E(B-V) ~ 2.6 omplicates the analysis.

The message may be cited.


GRB_name: GRB140610A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16382
SUBJECT: GRB 140610A: Swift-BAT refined analysis
DATE:    14/06/11 13:26:08 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

A. Y. Lien (NASA/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), P. A. Evans (U Leicester), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+552 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140610A (trigger #601259)
(Evans, et al., GCN Circ. 16375).  The BAT ground-calculated position is
RA, Dec = 286.261, 3.899 deg, which is 
   RA(J2000)  =  19h 05m 02.7s 
   Dec(J2000) = +03d 53' 56.7" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 67%.
 
The mask-weighted light curve shows the emission starting at ~T-10 sec,
peaking at ~T+1 sec, and continuing out to T+110 sec at which time
the location left the BAT FoV when the Swift slewed to a pre-planned
observing target.
 
The time-averaged spectrum from T-6.67 to T+105.7 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.57 +- 0.06.  The 1-sec peak photon flux measured from T+0.48 sec
in the 15-150 keV band is 1.4 +- 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/601259/BA/


GRB_name: GRB140610A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16383
SUBJECT: GRB 140610A: RATIR Optical and NIR Observations
DATE:    14/06/11 19:39:38 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB),
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara
(ORAU/GSFC), 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), and
Harvey Moseley (GSFC) report:

We observed the field of GRB 140610A (Evans, et al., GCN 16375) 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 2014/06 11.19 to 2014/06 11.20 UTC (12.06 to
12.26 hours after the BAT trigger), obtaining a total of 0.16 hours
exposure in the r and i bands and 0.07 hours exposure in the Z, Y, J, and H
bands.

We detect no new sources within Swift-XRT error circle (Kennea et al., GCN
16376).  In comparison with 2MASS, we obtain the following 3-sigma upper
limits:

 r > 20.22
 i > 19.15
 Z > 16.99
 Y > 17.40
 J > 16.68
 H > 17.62

These magnitudes 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: GRB140611A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16384
SUBJECT: IPN Triangulation of GRB 140611A (short/hard)
DATE:    14/06/11 21:49:48 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

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

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

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

The short-duration, hard spectrum, bright GRB 140611A has been observed
by Konus-Wind, Swift (BAT), MESSENGER (GRNS), and INTEGRAL (SPI-ACS),
so far, at about 13864 s UT (03:51:04). 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:
     349.931 (23h 19m 43s) -40.077 (-40d 04' 38")
    Corners:
     349.762 (23h 19m 03s) -40.115 (-40d 06' 54")
     350.246 (23h 20m 59s) -40.726 (-40d 43' 33")
     350.100 (23h 20m 24s) -40.039 (-40d 02' 21")
     349.615 (23h 18m 28s) -39.417 (-39d 25' 02")
    ---------------------------------------------
The error box area is 674 sq. arcmin, and its maximum
dimension is 1.4 deg (the minimum one is 15.6 arcmin).

This box may be improved.

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


GRB_name: GRB140610A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16385
SUBJECT: GRB 140610A: Fermi GBM Detection
DATE:    14/06/11 23:43:19 GMT
FROM:    Matthew Stanbro at UAH/Fermi  <mcs0001@uah.edu>

Matthew Stanbro (UAH) reports on behalf of the Fermi GBM Team:

"At 16:31:28.58 UT on 10 June 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140610A (trigger 424110691 / 140610689)
which was also detected by Swift BAT (Evans et al. 2014, GCN 16375).
The GBM on-ground location, using the Fermi GBM trigger data,
is consistent with Swift's location.

The GBM light curve shows a long burst, consisting of one main episode,
with a total duration (T90) of about 134.1 s (50-300 keV).
The time-averaged spectrum from T0-2.048 s to T0+133.122 s is well fit
by a power law function with an exponential high-energy cutoff.
The power law index is -1.32 +/- 0.08 and the cutoff energy,
parameterized as Epeak, is 169 +/- 24 keV.


The event fluence (10-1000 keV) in this time interval is
(1.2 +/- 0.1)E-05 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+0.00 s in the 10-1000 keV band is 2.5 +/- 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: GRB140611A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16386
SUBJECT: GRB 140611A Detection of a source in BAT ground analysis
DATE:    14/06/12 00:30:02 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings on behalf of the Swift-BAT team

Following the IPN Triangulation of GRB 140611A (Golenetskii et al., GCN Circ # 16384),
a reexamination of the BAT image shows a sub-threshold source at the edge of the BAT
field of view at RA, Dec 349.939, -40.111 which is:

RA (J2000)   23h 19m 45.4s   
Dec (J2000) -40d 06' 41"

with an estimated 90% uncertainty radius of 4 arcmin.  This location is within the
IPN error box.

In BAT, this burst had two short peaks, the first 5 times brighter, each about 0.4
seconds long, separated by about 1.8 seconds.  The total T90 was about 1.9 +/- 0.2
seconds.  Because of the partial coding, a calibrated BAT spectrum is not possible,
but the burst appears to be in the short-hard category.

A Swift TOO is being performed.


GRB_name: GRB140606B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16387
SUBJECT: GRB 140606B / iPTF 14bfu: MOSFIRE NIR imaging
DATE:    14/06/12 02:11:11 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech), M. Kasliwal (Carnegie), L. P. Singer, Y. Cao 
(Caltech), and K. Tinyanont (Harvey Mudd) report:

Beginning at 12:57 UT on 2014-06-08 we observed the field of iPTF14bfu 
(Singer et al., GCN 16360), the optical counterpart of GRB 140606B 
(Burns et al., GCN 16363), using the imaging mode of MOSFIRE on the Keck 
I 10m telescope. A sequence of nine 23-second images was acquired in the 
Ks filter.

Calibrating relative to 2MASS stars in the image, we measure a magnitude of:

Ks = 19.50 +/- 0.06  (Vega, or Ks = 21.34 AB)

at a mid-time of 2.411 days after the initial trigger.

We also measure an improved astrometric position (relative to 2MASS) of:
21:52:29.961 +32:00:50.66  (J2000, +/- 0.2")


GRB_name: GRB140610A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16388
SUBJECT: GRB 140610A: Swift-XRT refined Analysis
DATE:    14/06/12 08:33:01 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:

We have analysed 11 ks of XRT data for GRB 140610A (Evans  et al. GCN
Circ. 16375),  from 3.1 ks to 115.0 ks after the  BAT trigger. The data
comprise 586 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. Using 463 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 =
286.26899, +3.90822 which is equivalent to:

RA (J2000): 19h 05m 04.56s
Dec(J2000): +03d 54' 29.6"

with an uncertainty of 3.1 arcsec (radius, 90% confidence).

The light curve from T0+3.1-10.6 ks can be modelled with  a power-law
decay with a decay index of alpha=0.66 (+0.26, -0.25). At T0+10.6 ks
the count rate is 0.04 +/- 0.01 ct/sec. In subsequent observations,
spanning T0+61-115 ks and containing 7.5 ks of exposure, the source is
undetected with a 3-sigma upper limit of 0.002 ct/sec. This is
substantially below the extrapolated decay detailed above, and suggests
a decay index of alpha > 1.71.

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.3 (+0.9, -0.8). The
best-fitting absorption column is 3.1 (+2.0, -1.4) x 10^22 cm^-2, in
excess of the Galactic value of 1.2 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 6.0 x 10^-11 (2.0 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.1 (+2.0, -1.4) x 10^22 cm^-2
Galactic foreground: 1.2 x 10^22 cm^-2
Excess significance: 2.2 sigma
Photon index:      2.3 (+0.9, -0.8)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00601259.

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


GRB_name: GRB140611A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16389
SUBJECT: Konus-Wind observation of GRB 140611A
DATE:    14/06/12 11:53:32 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The short/hard GRB 140611A (IPN triangulation: Golenetskii at al., GCN 16384;
Swift-BAT detection in ground analysis: Cummings, GCN 16386)
triggered Konus-Wind at T0=13864.927 s UT (03:51:04.927).

The burst light curve starts, at ~T0-0.1, with a rise of short,
bright pulse with a duration of ~0.5 s, followed by a weaker,
second pulse from ~T0-1.5 s to ~T0+2.2 s.
The total duration of the burst is ~2.3 s.
The emission is seen up to ~5 MeV.

As observed by Konus-Wind, the burst
had a fluence of 1.5(-0.3,+0.4)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+0.256 s,
of 4.5(-0.5,+0.5)x10^-5 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 - 18 MeV range
by the cutoff power law with the following model parameters:
the photon index alpha = -0.68 (-0.18,+0.22),
and the peak energy Ep = 1460(-360,+520) keV,
chi2 = 111/98 dof.
Fitting this spectrum with the Band model yields the same
values of alpha and Ep with an upper limit on beta of -2.3.

The spectrum near the maximum count rate
(measured from T0 to T0+0.256 s)
is best fit in the 20 keV - 5 MeV range
by the cutoff power law with the following model parameters:
the photon index alpha = -0.24(-0.14,+0.16),
and the peak energy Ep = 1410(-160,+170) keV,
chi2 = 69/68 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140611_T13864/

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


GRB_name: GRB140611A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16390
SUBJECT: GRB 140611A: Swift-XRT observations
DATE:    14/06/12 13:59:27 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

P.A. Evans, K.L. Page and A. Amaral-Rogers (U. Leicester) report on
behalf of the Swift-XRT team:

We have analysed 4.8 ks of XRT data for the IPN-detected burst: GRB
140611A, from 80.5 ks to 92.1 ks after the IPN trigger (Golenetskii et
al., GCN Circ. 16384). The burst was also detected in ground analysis
of BAT data (Cummings, GCN Circ. 16386). The data are entirely in
Photon Counting (PC) mode.  An X-ray source is detected within the IPN
and BAT error regions. The refined XRT position is RA, Dec = 349.9173,
-40.1044 which is equivalent to:

RA (J2000): 23 19 40.15
Dec(J2000): -40 06 16.0

with an uncertainty of 5.5 arcsec (radius, 90% confidence). This
position is 64 arcsec from the BAT ground position and 106 arcsec from
the centre of the IPN error box. The source has a mean count rate of
(1.9 +0.9,-0.7) x 10^-3 count s^-1 over this time interval. Within the
4-arcmin radius BAT error circle, we would expect approximately 0.25
serendipitous sources of at least this brightness. We cannot determine
whether the source is fading and no further observations are planned.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020385.

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


GRB_name: GRB140614A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16391
SUBJECT: GRB 140614A: Swift detection of a burst
DATE:    14/06/14 01:20:49 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

K. L. Page (U Leicester), S. D. Barthelmy (GSFC), D. N. Burrows (PSU),
N. Gehrels (NASA/GSFC), F. E. Marshall (NASA/GSFC), T. Sakamoto (AGU),
M. H. Siegel (PSU) and C. A. Swenson (PSU) report on behalf of the
Swift Team:

At 01:04:59 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140614A (trigger=601646).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 231.232, -79.095 which is 
   RA(J2000) = 15h 24m 56s
   Dec(J2000) = -79d 05' 41"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As is usual for an image trigger, the
immediately-available light curve does not show significant
variation. 

The XRT began observing the field at 01:07:03.1 UT, 123.2 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
231.1723, -79.1291 which is equivalent to:
   RA(J2000)  = 15h 24m 41.34s
   Dec(J2000) = -79d 07' 44.9"
with an uncertainty of 2.2 arcseconds (radius, 90% containment). This
location is 129 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 1.26
x 10^21 cm^-2 (Willingale et al. 2013). 

The initial flux in the 2.5 s image was 7.34e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 131 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 0.12. 

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


GRB_name: GRB140614A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16392
SUBJECT: GRB 140614A: GROND afterglow candidate
DATE:    14/06/14 02:49:55 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

M. Tanga (MPE Garching), T. Kruehler (ESO, Santiago), S. Klose, D. A. Kann 
(both TLS Tautenburg), and J. Greiner (MPE Garching) report:

We observed the field of GRB 140614A (Swift trigger 601646; Page et al., 
GCN 16391) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, 
PASP 120, 405) mounted at the 2.2m MPG telescope at ESO La Silla 
Observatory (Chile).

Observations started at 01:09:27 UT on June 14, about 5 min after the GRB 
trigger. They were obtained at airmass 1.5 and a seeing of 2". Inside the 
X-ray error circle we detect a source at coordinates RA, DEC (J2000) = 
15:24:40.65, -79:07:43.5 with an error of 0".5. At a mean time of 01:40:20 
UT, we measure the following preliminary AB magnitudes:

g' > 21.6,
r' = 20.6 +/- 0.2,
i' = 19.5 +/- 0.1,
z' = 19.2 +/- 0.1,
J  = 19.0 +/- 0.2,
H  = 18.5 +/- 0.2, and
K  > 17.6.

We also detect clear fading in the J band. We propose this source to be 
the afterglow of GRB 140614A.

Given magnitudes are calibrated against GROND zeropoints (g'r'i'z') as 
well as 2MASS (JHK) field stars and are not corrected for the expected 
Galactic foreground extinction corresponding to a reddening of E(B-V) = 
0.12 mag in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB140614A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16393
SUBJECT: GRB 140614A: Enhanced Swift-XRT position
DATE:    14/06/14 05:24:14 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 1478 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 140614A, 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 = 231.16955, -79.12882 which is equivalent
to:

RA (J2000): 15h 24m 40.69s
Dec (J2000): -79d 07' 43.8"

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: GRB140614B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16394
SUBJECT: GRB 140614B: Swift detection of a burst
DATE:    14/06/14 06:53:41 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

K. L. Page (U Leicester), J. R. Cummings (NASA/UMBC),
N. P. M. Kuin (UCL-MSSL), T. Sakamoto (AGU) and M. H. Siegel (PSU)
report on behalf of the Swift Team:

At 06:38:11 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140614B (trigger=601662).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 322.625, +14.920 which is 
   RA(J2000) = 21h 30m 30s
   Dec(J2000) = +14d 55' 13"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single weak broad 
peak with a duration of about 35 sec.  The peak count rate was ~1248 
counts/sec (15-350 keV), at ~2 sec after the trigger. 

The XRT began observing the field at 06:40:16.9 UT, 125.2 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source with an enhanced position: RA, Dec 322.6313,
14.9299 which is equivalent to:
   RA(J2000)  = 21h 30m 31.50s
   Dec(J2000) = +14d 55' 47.5"
with an uncertainty of 2.1 arcseconds (radius, 90% containment). This
location is 41 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (8.06 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 3.7
(+2.77/-2.35) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 1.21e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 132 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
0.08. 

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


GRB_name: GRB140614B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16395
SUBJECT: GRB 140614B: Enhanced Swift-XRT position
DATE:    14/06/14 12:11:37 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 1221 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 140614B, 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 = 322.63127, +14.92970 which is equivalent
to:

RA (J2000): 21h 30m 31.50s
Dec (J2000): +14d 55' 46.9"

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: GRB140614A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16396
SUBJECT: GRB 140614A: Swift-XRT refined Analysis
DATE:    14/06/14 13:21:02 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 7.7 ks of XRT data for GRB 140614A (Page  et al. GCN
Circ. 16391),  from 112 s to 19.0 ks after the BAT trigger. The data
comprise 141 s in Windowed Timing (WT) mode (the first 10 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Beardmore
et al. (GCN Circ. 16393).

The light curve can be modelled with an initial power-law decay with an
index of alpha=1.75 (+0.11, -0.09), followed by a break at T+948 s to
an alpha of 0.96 (+0.07, -0.09).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.73 (+0.14, -0.12). The
best-fitting absorption column is  1.45 (+0.53, -0.19) x 10^21 cm^-2,
consistent with the Galactic value of 1.3 x 10^21 cm^-2 (Willingale et
al. 2013). The PC mode spectrum has a photon index of 1.78 (+0.11,
-0.09) and a best-fitting absorption column consistent with the
Galactic value. The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 3.8 x 10^-11 (4.3 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.26 (+0.23, -0.00) x 10^21 cm^-2
Galactic foreground: 1.3 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.78 (+0.11, -0.09)

If the light curve continues to decay with a power-law decay index of
0.96, the count rate at T+24 hours will be 7.8 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.0 x
10^-13 (3.4 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/00601646.

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


GRB_name: GRB140614A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16397
SUBJECT: GRB 140614A: Swift/UVOT Upper Limits
DATE:    14/06/14 14:11:43 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (UCL-MSSL) and K. L. Page (U Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140614A
132 s after the BAT trigger (Page et al., GCN Circ. 16391).
No optical afterglow consistent with the XRT position
(Beardmore et al. GCN Circ. 16393)
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           132          281          147         >21.5
u_FC               290          539          246         >20.5
white              132          763          186         >21.6
v                  620         1668           39         >19.1
b                  546          739           39         >19.6
u                  290          714          265         >20.5
w1                 670         1718           39         >19.1
m2                 645         1693           39         >18.9
w2                 596          783           34         >20.4

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: GRB140606B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16398
SUBJECT: GRB 140606B / iPTF 14bfu: AAO optical observations
DATE:    14/06/14 14:21:20 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), R. Inasaridze (AAO), O. Kvaratskhelia (AAO), V.
Ayvazian (AAO), Yu. Krugly (IA KhNU), I. Molotov (KIAM), A. Pozanenko
(IKI) report on behalf of larger GRB follow-up collaboration:

We observed a field of the GBM GRB 140606B / iPTF 14bfu (Singer et al., 
GCN 16360) with AS-32 (0.7m) telescope of Abastumani Observatory 
starting on June, 07 (UT) 21:40:06. We obtained several unfiltered 
frames with exposure of each frame of 120 s. The  optical transient   is 
well detected on the stacked image.

A photometry is based on nearby USNO-B1.0 stars:

date       UT start   t-T0       Filter  Exp.    OT        err
                      (mid, days)         (s)

2014-06-07 21:40:06  1.82039     None    46*120  21.95 +/- 0.20


GRB_name: GRB140614B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16399
SUBJECT: GRB 140614B: RATIR Optical and NIR Observations
DATE:    14/06/14 15:27:28 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

---------- Forwarded message ----------
From: "Nat Butler" <natbutler@asu.edu>
Date: Jun 14, 2014 7:32 AM
Subject: GRB 140614B: RATIR Optical and NIR Observations
To: "Nat Butler" <natbutler@asu.edu>
Cc:

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB),
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara
(ORAU/GSFC), 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), and
Harvey Moseley (GSFC) report:

We observed the field of GRB 140614B (Page, et al., GCN 16394) 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 2014/06 14.28 to 2014/06 14.47 UTC (0.11 to
4.62 hours after the BAT trigger), obtaining a total of 0.71 hours exposure
in the r and i bands and 0.30 hours exposure in the Z, Y, J, and H bands.

For a source within the Swift-XRT error circle, in comparison with 2MASS,
we obtain the following upper limits (3-sigma):

  r     > 22.70
  i     > 22.53
  Z     > 21.64
  Y     > 21.08
  J     > 21.04
  H     > 20.51

These magnitudes 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: GRB140614B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16400
SUBJECT: GRB 140614B: Swift/UVOT Upper Limits
DATE:    14/06/14 15:28:38 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (UCL-MSSL) and K. L. Page (U Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140614B
132 s after the BAT trigger (Page et al., GCN Circ. 16394).
No optical afterglow consistent with the XRT position
(Evans et al. GCN Circ. 16395)
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           132          282          147         >21.0
u_FC               291          540          246         >20.4
white              132         6723          766         >22.2
v                  621         7133          490         >20.1
b                  546         6518          471         >20.9
u                  291         6314          697         >20.8
w1                 670         6108          293         >20.5
m2                1073         7222          298         >20.1
w2                 597         6929          471         >21.0

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: GRB140614A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16401
SUBJECT: GRB 140614A: X-shooter redshift
DATE:    14/06/14 15:39:49 GMT
FROM:    Paul Vreeswijk at Weizmann Inst of Science  <paul.vreeswijk@weizmann.ac.il>

T. Kruehler (ESO, Santiago), P. M. Vreeswijk (Weizmann),
J. P. U. Fynbo, D. Xu (DARK/NBI) report on behalf of the X-shooter GRB
collaboration:

We observed the optical afterglow (Tanga et al., GCN 16392) of GRB
140614A (Swift trigger 601646; Page et al., GCN 16391; Beardmore et
al., GCN 16393; Melandri et al., GCN 16396) with the VLT/X-shooter
spectrograph, equipped with the UVB/VIS/NIR arms and covering the
wavelength range 3000-25000 AA.

A spectral nodding sequence of 4x600s was started at June 14.20 (3.8
hours after the Swift trigger). A preliminary reduction shows the lack
of any signal in the UVB arm, but a clear trace, albeit with moderate
signal-to-noise ratio, in both the VIS and NIR arms starting at around
6450 AA. Several absorption features can be identified with the
transitions SiII 1526, CII 1334, CII* 1335, AlII 1670, AllIII 1854,
FeII 2344, 2382, 2600, and MgII 2796, 2803 at a common redshift of z=4.233.

We acknowledge excellent support from the observing staff at Paranal,
in particular Zahed Wahhaj, Jonathan Smoker, Yazan Momany and
Stephane Brillant.


GRB_name: GRB140614A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16402
SUBJECT: GRB 140614A: Swift-BAT refined analysis
DATE:    14/06/14 16:27:03 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/UMBC), K. L. Page (U Leicester), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 140614A (trigger #601646)
(Page, et al., GCN Circ. 16391).  The BAT ground-calculated position is
RA, Dec = 231.171, -79.110 deg, which is 
   RA(J2000)  =  15h 24m 41.1s 
   Dec(J2000) = -79d 06' 36.9" 
with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 97%.
 
The mask-weighted light curvea shows a broad peak starting at ~T-80 sec,
peaking at ~T+55 sec, and returning to baseline at ~T+200 sec (and 
possibly out to  around T+600 sec).  The formal T90 (15-350 keV) is 720 +- 160 sec,
but with the long weak possible tail of this event it is hard to determine
the true end of the event (estimated error including systematics).
 
The time-averaged spectrum from T+0.51 to T+957 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.50 +- 0.46.  The fluence in the 15-150 keV band is 1.3 +- 0.4 x 10^-6 erg/cm2.
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/601646/BA/


GRB_name: GRB140606B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16403
SUBJECT: GRB 140606B / iPTF 14bfu: Mondy optical observations
DATE:    14/06/14 16:46:44 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed a field of the GBM GRB 140606B / iPTF 14bfu (Singer et al.,
GCN 16360) with with AZT-33IK telescope of Sayan observatory (Mondy). We 
obtained several images on June, 08 (UT) 17:17:29 with exposure of each 
frame of 120 s. The  optical transient Singer et al., GCN 16360) is well 
detected on the stacked image. A photometry is based on nearby USNO-B1.0 
stars:

date        UT start  t-T0        Filter  Exp.    OT
                       (mid, days)          (s)

2014-06-08  17:17:29  2.62892     R       60*120  22.00+/-0.12

The finding chart can be found in
http://grb.rssi.ru/GRB140606B/grb140606B_AZT33IK_R_fc.png

The light curve based on published photometry in r, R and unfiltered 
observations (GCNs 16360, 16362, 16367, 16398) can be found in
http://grb.rssi.ru/GRB140606B/grb140606B_lc.png

Based on the lc  above one can suggest that a host galaxy of GRB 140606B 
may influence on the photometry of the afterglow.


GRB_name: GRB140614B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16404
SUBJECT: GRB 140614B: Swift-BAT refined analysis
DATE:    14/06/14 21:16:24 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), K. L. Page (U Leicester),
T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+962 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 140614B (trigger #601662)
(Page, et al., GCN Circ. 16394).  The BAT ground-calculated position is
RA, Dec = 322.636, 14.895 deg, which is 
   RA(J2000)  =  21h 30m 32.6s 
   Dec(J2000) = +14d 53' 41.5" 
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 71%.
 
The mask-weighted light curve shows a FRED pulse starting at ~T0,
peaking at ~T+5 sec, and ending at ~T+75 sec.  T90 (15-350 keV) is
49.8 +- 7.9 sec (estimated error including systematics).
 
The time-averaged spectrum from T-3.28 to T+55.59 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.04 +- 0.26.  The fluence in the 15-150 keV band is 5.5 +- 1.0 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+6.93 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/601662/BA/


GRB_name: GRB140614B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16405
SUBJECT: GRB 140614B: MITSuME Okayama upper limits
DATE:    14/06/15 01:44:49 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 collaboration:

We observed the field of GRB 160614B (Page et al., GCNC 16394)
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 2014-06-14 16:44:18 (~10.1 h after the burst).
We did not find any new point source within the enhanced XRT circle
(Evans et al., GCNC 16395) in all the three bands.

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

#T0+[day]  MID-UT    T-EXP[sec]   g'     Rc     Ic
-----------------------------------------------------
0.46713    17:50:51    6060.0   >19.2  >19.3  >18.6
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB140614B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16406
SUBJECT: GRB 140614B: Swift-XRT refined Analysis
DATE:    14/06/15 03:53:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 7.8 ks of XRT data for GRB 140614B (Page  et al. GCN
Circ. 16394),  from 115 s to 52.7 ks after the BAT trigger. The data
comprise 86 s in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Evans et
al. (GCN Circ. 16395).

The light curve can be modelled with an initial power-law decay with an
index of alpha=1.35 (+/-0.13), followed by a break at T+515 s to an
alpha of 3.93 (+0.28, -0.26).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 0.99 (+0.20, -0.18). The
best-fitting absorption column is  3.6 (+2.1, -1.6) x 10^21 cm^-2, in
excess of the Galactic value of 8.1 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.46 (+0.19, -0.18)
and a best-fitting absorption column of 2.3 (+1.0, -0.9) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 5.1 x 10^-11 (5.9 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.3 (+1.0, -0.9) x 10^21 cm^-2
Galactic foreground: 8.1 x 10^20 cm^-2
Excess significance: 2.9 sigma
Photon index:      1.46 (+0.19, -0.18)

If the light curve continues to decay with a power-law decay index of
3.93, the count rate at T+24 hours will be 3.7 x 10^-9 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.9 x
10^-19 (2.2 x 10^-19) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00601662.

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


GRB_name: GRB140614B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16407
SUBJECT: GRB 140614B: MITSuME Akeno upper limits
DATE:    14/06/15 13:07:16 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

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

We observed the field of GRB 140614B (K. L. Page et al., GCN Circular #16394) 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 2014-06-14 14:18:14 UT ( 7.7h after the burst).
We did not find any new point source within XRT circle in all the three bands.


The measured magnitudes were listed below.

T0+[sec] MID-UT T-EXP[sec] g' Rc Ic
27602 16:26:47 14280 >19.7 >19.8 >18.9

T0+ : Elapsed time after the burst 
T-EXP: Total Exposure time 
We used GSC2.3 catalog for flux calibration.


GRB_name: GRB140614C
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16408
SUBJECT: GRB 140614C found in ground analysis of BAT data
DATE:    14/06/15 14:51:46 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings reports on behalf of the Swift-BAT team:

The IPN reported a burst at 20:06:56. It occurred near the end of a Swift
pointing on top of an approach to the SAA.  No source was found onboard.
In ground analysis a significant source was found at RA, Dec  147.423, 71.945,
which is:

RA (J2000)    09h 49m 41.5s
Dec (J2000)   71d 56' 41"

with an estimated 90% uncertainty radius of 3 arcmin.

The burst was a single peak about 20 seconds long.

The spectrum during the peak 10 seconds of the burst is best fit by a
simple power law function with a photon index of 1.0  0.3.  The fluence
from 15-150 keV in the 10 seconds was (1.6  0.5) x 10^-7 ergs/cm^2.
Errors quoted are 68% confidence.

A Swift TOO has been requested.


GRB_name: GRB140614B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16409
SUBJECT: GRB 140614B: MOSFIRE Ks-band nondetection
DATE:    14/06/15 15:25:35 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) reports:

I imaged the field of GRB 140614B (Page et al., GCN 16394) using MOSFIRE 
on the Keck I 10m telescope in the Ks-band filter.  A sequence of 12 
36-second images was obtained at a midtime of 13:18 UT on 2014-06-15 
(1.27 days after the Swift trigger).

No sources are detected within the XRT error circle (Evans et al, GCN 
16395) to a limiting mag of approximately Ks > 21.9 mag (3-sigma, 
calibrating relative to 2MASS.)

A faint source (Ks = 21.5 +/- 0.2 mag) is detected outside the XRT error 
circle, at a position of RA = 21:30:31.364, dec = +14:55:48.79 (J2000).


GRB_name: GRB140614C
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16410
SUBJECT: GRB 140614C: 1.23m CAHA (+EDIPO) observations
DATE:    14/06/15 23:17:26 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

A. J. Castro-Tirado (IAA-CSIC, ISA-UMA), J. Gorosabel (IAA-CSIC, UPV-EHU),
S. Guziy (Univ. of Nikolaev), O. Rabaza (UGR), I. Syniavskyi, Y. Ivanov
(Kiev Main Astronomical Observatory), R. Cunniffe, A. Gonzalez-Rodriguez,
M. Jelinek, S. Jeong, O. Lara-Gil, S. R. Oates, R. Sanchez-Ramirez and J.
C. Tello (IAA-CSIC) report:

â€œFollowing the detection of GRB 140614C by Swift/BAT (Cummings et al. GCNC
16408) we obtained R-band images at the 1.23m telescope (+EDIPO) at Calar
Alto Observatory in southern Spain, starting on June 15, 20:27 UT  (i.e.
24.4 hr postburst). In the coadded image (6 x 300s), we see no credible
optical candidate within the BAT error box when compared to the DSS-1 down
to R = 20.5. Further observations are ongoing.â€


GRB_name: GRB140606A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16411
SUBJECT: GRB 140606A: BTA and OSN optical observations
DATE:    14/06/16 09:46:39 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

A. S. Moskvitin (SAO RAS), A. F. Valeev (SAO RAS, Kazan Federal U.),
V. N. Komarova (SAO RAS), V. V. Sokolov, T.N. Sokolova (SAO RAS),
J. Aceituno, S. R. Oates (IAA-CSIC), J. Gorosabel (IAA-CSIC, EPV-EHU) and
A. J. Castro-Tirado (IAA-CSIC, ISA-UMA) on behalf of larger collaboration
report:

We observed the field of the short GRB 140606A (Stroh et al., GCNC 16353)
11.3 h after with the 6-meter BTA (+Scorpio-I) at SAO-RAS (Zelenchuk,
Russia). Comparison images (R-band) were obtained with the 1.5m telescope
at Observatorio de Sierra Nevada (south Spain) 60 h post burst. Within the
refined BAT gamma-ray burst error circle (Cummings et al., GCNC 16354), we
identify no variable object down to R = 22, in agreement with the limit
reported by Volnova et al. (GCNC 16371).


GRB_name: GRB140606B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16412
SUBJECT: GRB 140606B: Swift XRT final light curve
DATE:    14/06/16 16:41:48 GMT
FROM:    Vanessa Mangano at PSU  <vxm22@psu.edu>

V. Mangano (PSU)
on behalf of the Swift-XRT team:

Swift XRT observed the field of GRB 140606B twice after
its return to normal operations for a total of 9 ks exposure.
We confirm that the light curve of the X-ray source given
in Mangano et al. (GCN Circ. 16366 and 16373) shows a
power-law decay with slope 1.0 (+0.7,-0.6).

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


GRB_name: GRB140619A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16415
SUBJECT: GRB 140619A: Swift detection of a burst with a possible optical counterpart
DATE:    14/06/19 11:56:35 GMT
FROM:    David Burrows at PSU/Swift  <burrows@astro.psu.edu>

M. De Pasquale (INAF-IASFPA), D. N. Burrows (PSU), S. B. Cenko (GSFC),
J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA),
N. P. M. Kuin (UCL-MSSL), A. Y. Lien (NASA/GSFC/ORAU),
F. E. Marshall (NASA/GSFC), A. Maselli (INAF-IASFPA),
K. L. Page (U Leicester), B. Sbarufatti (INAF-OAB/PSU) and
T. N. Ukwatta (MSU) report on behalf of the Swift Team:

At 11:38:35 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140619A (trigger=602080).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 27.092, -39.261 which is 
   RA(J2000) = 01h 48m 22s
   Dec(J2000) = -39d 15' 40"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As is usual with an image trigger, the available
BAT light curve shows no significant structure. 

The XRT began observing the field at 11:40:54.9 UT, 139.1 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 27.1084, -39.2586 which is equivalent to:
   RA(J2000)  = +01h 48m 26.02s
   Dec(J2000) = -39d 15' 31.0"
with an uncertainty of 4.8 arcseconds (radius, 90% containment). This
location is 46 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 5.85e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of  98 seconds with the White filter
starting 147 seconds after the BAT trigger. There is a weak 20.5 mag source
near the XRT position. No aspect UVOT aspect solution is available
because of the paucity of stars. Confirmation of the afterglow
will require the full data set. No correction has been made
for the expected extinction corresponding to E(B-V) of 0.01. 

Burst Advocate for this burst is M. De Pasquale (mdp 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: GRB140619A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16416
SUBJECT: GRB 140619A: Enhanced Swift-XRT position
DATE:    14/06/19 19:11:16 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 2297 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 140619A, 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 = 27.10849, -39.25934 which is equivalent
to:

RA (J2000): 01h 48m 26.04s
Dec (J2000): -39d 15' 33.6"

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

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

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


GRB_name: GRB140619A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16417
SUBJECT: GRB 140619A: Swift-XRT refined Analysis
DATE:    14/06/19 23:56:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 7.3 ks of XRT data for GRB 140619A (De Pasquale  et
al. GCN Circ. 16415),  from 129 s to 30.3 ks after the BAT trigger.
The data comprise 112 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. 16416).

The late-time light curve (from T0+5.1 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.93 (+/-0.09).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 0.67 (+/-0.05). The
best-fitting absorption column is  1.9 (+/-0.4) x 10^21 cm^-2, in
excess of the Galactic value of 1.6 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.09 (+0.15, -0.14)
and a best-fitting absorption column of 2.5 (+/-0.5) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.4 x 10^-11 (5.1 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.5 (+/-0.5) x 10^21 cm^-2
Galactic foreground: 1.6 x 10^20 cm^-2
Excess significance: 7.7 sigma
Photon index:      2.09 (+0.15, -0.14)

If the light curve continues to decay with a power-law decay index of
0.93, the count rate at T+24 hours will be 0.031 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x
10^-12 (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/00602080.

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


GRB_name: GRB140619A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16418
SUBJECT: GRB 140619A: Swift/UVOT Observations
DATE:    14/06/20 00:27:09 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU), F. E. Marshall (NASA/GSFC), J. Linevsky (PSU),
and M. De Pasquale (INAF-IASFPA) report on behalf of the
Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140619A
147 s after the BAT trigger (De Pasquale et al., GCN Circ. 16415).
We confirm a faint afterglow consistent with the XRT position is detected in the
initial UVOT exposures. We have corrected the positions in the 2.7' x 2.7 UVOT
sub-image by comparing positions with the Digital Sky Survey. The UVOT afterglow
is located at:
  RA  (J2000) =  01:48:26.15 =  27.10896 (deg.)
  Dec (J2000) = -39:15:32.6  = -39.25906 (deg.)
with an estimated uncertainty of 1.0 arc sec. (radius, 90% confidence).

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

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

white (fc)     147          245        96     20.39+-0.24
white         5112         5312       196     >21.05
b            11745        12179       422     >20.65
u            10833        11740       885     >20.82
uvw1          5933         6133       196     >19.77
uvm2          5727         5927       196     >19.59
uvw2          5317         5517       196     >19.87

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: GRB140619B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16419
SUBJECT: GRB 140619B: Fermi GBM detection of a short GRB
DATE:    14/06/20 00:40:16 GMT
FROM:    Valerie Connaughton at UAH/NSSTC  <valerie.connaughton@nasa.gov>

V. Connaughton, B-B. Zhang (UAH), G. Fitzpatrick, and O. Roberts (UCD)
report on behalf of the Fermi GBM Team:

"At 11:24:40.52 UT on 19 June 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140619B (trigger 424869883  / 140619475)

The on-ground calculated location, using the GBM trigger
data, is RA = 133.4, DEC = -3.7 (J2000 degrees,
equivalent to 08h 54m, -3d 42'), with an uncertainty
of 5 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).

The GBM light curve consists of a single peak with substructure,
with a duration (T90) of about 0.5 s (50-300 keV).
The time-averaged spectrum from T0-0.192 s to T0+0.640 s is
well fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.11 +/- 0.16 and
the cutoff energy, parameterized as Epeak, is 1450 +/- 220 keV

The event fluence (10-1000 keV) in this time interval is
(1.70 +/- 0.09)E-6 erg/cm^2. The 64-msec peak photon flux measured
starting from T0+0.38 s in the 10-1000 keV band is 7.6 +/- 3.4 ph/s/cm^2.

A Band function fits the spectrum equally well
with Epeak= 1356 +/- 252 keV, alpha = -0.06 +/- 0.19
and beta = 3.3 +/- 1.4.


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


GRB_name: GRB140619B
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16420
SUBJECT: GRB 140619B: Fermi-LAT Detection
DATE:    14/06/20 01:02:03 GMT
FROM:    Daniel Kocevski at SLAC  <dankocevski@gmail.com>

GRB 140619B: Fermi-LAT detection

D. Kocevski (NASA/GSFC), F. Longo (University and INFN Trieste), G. Vianello (Stanford University), V. Connaughton (University of Alabama, Huntsville), J. McEnery (NASA/GSFC) and E.Sonbas (Adiyaman Univ.) report on behalf of the Fermi-LAT team:

At UT 11:24:47 on June 19, 2014, Fermi-LAT detected high-energy emission from GRB 140619B, which was also detected by Fermi-GBM (trigger 424869883 / 140619475).  A preliminary analysis of GBM data characterizes this event as a short hard burst, with a T90 duration of ~0.5s (GCN 16419).

The best LAT on-ground location is found to be:

(RA, Dec) = 132.68, -9.66 (deg, J2000)

with an approximate error radius of 0.06 deg (90% containment, statistical error only).

This was 32 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 within ~3 degree of the GBM location after the GBM trigger that is spatially and temporally correlated with the GBM emission with high significance. More than 19 photons above 100 MeV and more than 5 photons above 1 GeV are observed within 5 seconds. The highest-energy photon is a 24 GeV event which is observed 0.61 seconds after the GBM trigger.  

The Fermi-LAT point of contact for this burst is Eda Sonbas edasonbas@yahoo.com.

A Swift ToO has been requested for this burst.

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: GRB140619B
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16421
SUBJECT: GRB 140619B: Fermi-LAT detection
DATE:    14/06/20 01:02:23 GMT
FROM:    Valerie Connaughton at UAH/NSSTC  <valerie.connaughton@nasa.gov>

D. Kocevski (NASA/GSFC), F. Longo (University and INFN Trieste), G.
Vianello (Stanford University), V. Connaughton (University of Alabama,
Huntsville), J. McEnery (NASA/GSFC) and E.Sonbas (Adiyaman Univ.) report on
behalf of the Fermi-LAT team:

"At UT 11:24:41 on June 19, 2014, Fermi-LAT detected high-energy
emission from GRB 140619B, which was also detected by Fermi-GBM
(trigger 424869883 / 140619475).  A preliminary analysis of GBM
data characterizes this event as a short hard burst, with a T90
duration of ~0.5s (Connaughton et al. GCN 16419).

The best LAT on-ground location is found to be:

(RA, Dec) = 132.68, -9.66 (deg, J2000)

with an approximate error radius of 0.06 deg (90% containment,
statistical error only).

This was 32 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 
within ~5 degrees of the GBM location after the GBM trigger time  that 
is spatially and
temporally correlated with the GBM emission with high significance. More 
than
19 photons above 100 MeV and more than 5 photons above 1 GeV are
observed within 5 seconds. The highest-energy photon is a 24 GeV event 
which
is observed 0.61 seconds after the GBM trigger.

The Fermi-LAT point of contact for this burst is Eda Sonbas 
edasonbas@yahoo.com <mailto:edasonbas@yahoo.com>.

A Swift ToO has been requested and accepted for this burst.

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: GRB140610A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16422
SUBJECT: GRB 140610A: TShAO optical upper limit
DATE:    14/06/20 09:37:19 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), W. Mundrzyjewski (Fesenkov Astrophysical Institute), 
A. Kusakin (Fesenkov Astrophysical Institute), A. Pozanenko (IKI) report 
on behalf of larger GRB follow-up collaboration:

We observed the field of the Swift GRB 140610A (Evans  et al., GCN 
16375) with Zeiss-1000 (East) telescope of Tien Shan Astronomical 
Observatory starting on June 10, (UT) 16:49:37, i.e. 18 minutes after 
GRB trigger. We took several images in R-filter. Within enhanced XRT 
position (Evans et al., GCN 16388) we do not find any new source neither 
in the first image nor in a stacked image.

Details of the photometry are following:

date        UT start   t-T0       Filter  Exp.   UL(3 sigma)
                       (mid, days)          (s)
2014-06-10  16:49:37  0.04487     R       56*60  19.9

The photometry is based on USNO-B1.0 star
USNO-B1.0    RA           Dec        R2
0939-0410021 19:05:04.48 +03:54:23.3 16.75


GRB_name: GRB140619A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16423
SUBJECT: GRB 140619A: Swift-BAT refined analysis
DATE:    14/06/20 12:24:35 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

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

Using the data set from T-239 to T+421 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140619A (trigger #602080)
(De Pasquale, et al., GCN Circ. 16415).  The BAT ground-calculated position is
RA, Dec = 27.096, -39.249 deg which is
   RA(J2000)  =  01h 48m 23.2s
   Dec(J2000) = -39d 14' 57.1"
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 41%.

The mask-weighted light curve shows a complex structure with multiple peaks.
The main visible structure starts with roughly two long weaker pulses from
~T+20 s to T+150 s. The two weak pulses were followed by the major bright
structure lasting until ~T+260 s, and it consists of many sub-pulses. Afterward
there is another weaker long pulse lasting until ~T+350 s. T90 (15-350 keV) is
233.9 +- 13.4 sec (estimated error including systematics).

Note that the main structure of the burst happened at ~150 s after the original image trigger,
and was not described in the first circular (De Pasquale, et al., GCN Circ. 16415).

The time-averaged spectrum from T+32.3 to T+340.4 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.45 +- 0.14,
and Epeak of 117.8 +- 46.2 keV (chi squared 54.23 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 2.1 +- 0.04 x 10^-5 erg/cm2
and the 1-sec peak flux measured from T+219.52 sec in the 15-150 keV band is
4.6 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.71 +- 0.03 (chi squared 64.34 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/602080/BA/


GRB_name: GRB140619B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16424
SUBJECT: GRB 140619B: Swift-XRT observations
DATE:    14/06/20 16:16:03 GMT
FROM:    Alessandro Maselli at INAF/IASF Palermo  <maselli@ifc.inaf.it>

A. Maselli (INAF-IASFPA) and P. D'Avanzo (INAF-OAB) report on behalf of 
the Swift-XRT team:

"We have analysed 3.9 ks of XRT data for the Fermi/GBM and LAT-detected 
short GRB 140619B (Connaughton et al., GCN Circ. 16419; Kocevski et al., 
GCN Circ. 16420), from 48.7 ks to 71.6 ks after the GBM trigger. The 
data are entirely in Photon Counting (PC) mode. No bright X-ray 
afterglow is detected within the LAT error circle. The three sigma upper 
limit is 2.9E-03 cts/s.

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


GRB_name: GRB140620A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16426
SUBJECT: GRB 140620A / iPTF14cva: Fermi GBM observations
DATE:    14/06/20 18:08:48 GMT
FROM:    Gerard Fitzpatrick at UCD  <gerard.fitzpatrick@ucdconnect.ie>

G. Fitzpatrick (UCD), V. Connaughton (UAH)
report on behalf of the Fermi GBM Team:

At 05:15:28.02 UT on 20 June 2014, the Fermi Gamma-Ray Burst Monitor
triggered
and located GRB 140620A, which was observed by the intermediate Palomar
Transient Factory beginning 10 minutes after trigger time, and was reported
in GCN 16425 (Kasliwal, Cenko, and Singer) as iPTF14cva.

The on-ground calculated location, using the GBM trigger
data, is RA = 278, DEC = +43 (J2000 degrees,
equivalent to 18h 34m, +43d 0.0'), with an uncertainty
of 2 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).
The angle from the Fermi LAT boresight is 110 degrees.

The GBM light curve consists of a single peak
with a duration (T90) of about 46 s (50-300 keV).
The time-averaged spectrum from T0-4 s to T0+35 s is
adequately fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.1 +/- 0.1 and
the cutoff energy, parameterized as Epeak, is 77 +/- 5 keV.

The event fluence (10-1000 keV) in this time interval is
(5.3 +/- 0.2)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+1 s in the 10-1000 keV band is 6.3 +/- 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: GRB140619C
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16427
SUBJECT: IPN Triangulation of GRB 140619C (long/very intense)
DATE:    14/06/21 10:29:40 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

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

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

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

The long-duration, very intense GRB 140619C has been observed by
Konus-Wind, MESSENGER (GRNS), Mars-Odyssey (HEND), INTEGRAL (SPI-ACS),
and Suzaku (WAM), so far, at about 81966 s UT (22:46:06).

We have triangulated it to a preliminary, 3 sigma error box whose 
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   233.018 (15h 32m 04s) -25.599 (-25d 35' 55")
  Corners:
   233.298 (15h 33m 12s) -25.530 (-25d 31' 48")
   232.810 (15h 31m 14s) -26.672 (-26d 40' 18")
   232.738 (15h 30m 57s) -25.666 (-25d 39' 56")
   233.252 (15h 33m 00s) -24.382 (-24d 22' 57")
  ---------------------------------------------
The error box area is 0.549 sq. deg, and its maximum
dimension is 2.3 deg (the minimum one is 0.426 deg).

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB140619_T81966/IPN/

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


GRB_name: GRB140620A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16428
SUBJECT: GRB 140620A: Swift-XRT observations
DATE:    14/06/21 14:14:24 GMT
FROM:    Alessandro Maselli at INAF/IASF Palermo  <maselli@ifc.inaf.it>

M. De Pasquale (IASF-Palermo) reports on behalf of the Swift-XRT team:

We have analysed 3.0 ks of XRT data for the Fermi/GBM-detected
burst GRB 140620A (Fitzpatrick et al., GCN circ 16426), from 37.6
ks to 43.9 ks after the Fermi/GBM trigger. The data are entirely
in Photon Counting (PC) mode.
An X-ray source is detected within the Fermi/GBM error circle
at the position of the iPTF transient (Kasliwal et al., GCN circ.
16425). Using 2966 s of PC mode data and 2 UVOT images, we find an
enhanced XRT position (using the XRT-UVOT alignment and matching
UVOT field sources to the USNO-B1 catalogue): RA, Dec = 281.87089,
+49.73093 which is equivalent to:

RA (J2000): 18h 47m 29.01s
Dec(J2000): +49d 43' 51.4"

with an uncertainty of 2.2 arcsec (radius, 90% confidence). This
is 0.4 arcsec from the iPTF position.

The late-time light curve (from T0+37.6 ks) is consistent with a
constant source of mean count rate 1.2e-01 ct/sec. A power-law fit
formally gives an index of -0.1 (+2.4, -1.3). Further observations
might be needed to confirm that this source is the X-ray afterglow
of 140620A.

A spectrum formed from the PC mode data can be fitted with an
absorbed power-law with a photon spectral index of 2.04 (+0.26,
-0.24). The best-fitting absorption column is 1.4 (+0.7, -0.6) x
10^21 cm^-2, in excess of the Galactic value of 5.2 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 3.3 x 10^-11
(4.3 x 10^-11) erg cm^-2 count^-1.

A summary of the PC-mode spectrum is thus:

Total column:         1.4 (+0.7, -0.6) x 10^21 cm^-2
Galactic foreground: 5.2 x 10^20 cm^-2
Excess significance: 2.3 sigma
Photon index:         2.04 (+0.26, -0.24)

If the light curve continues to evolve with a power-law index
of -0.1, the count rate at T+24 hours will be 0.13 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.3 x
10^-12 (5.6 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/00020387.

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


GRB_name: GRB140619C
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16429
SUBJECT: Konus-Wind observation of GRB 140619C
DATE:    14/06/21 14:56:08 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

A long-duration, very intense GRB 140619C (IPN triangulation: Hurley et 
al., GCN 16427) triggered Konus-Wind at T0=81966.864 s UT (22:46:06.864).

The burst light curve shows two separate multipeaked episodes: the first
from ~T0-6 s to ~T0+12 s and the second longer and brighter
from ~T0+68 s to ~T0+93 s. The total duration of the burst is ~105 s.
The emission is seen up to ~10 MeV.

As observed by Konus-Wind, the burst had a fluence
of 1.1(-0.08,+0.08)x10^-4 erg/cm2, and a 64-ms peak flux,
measured from T0+72.832 s, of 2.25(-0.16,+0.16)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+97.792 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -1.15 (-0.15,+0.19),
the high energy photon index beta = -2.37 (-0.13,+0.10),
the peak energy Ep = 129 (-12,+13) keV,
chi2 = 94/84 dof.

The spectrum near the peak count rate
(measured from T0+65.792 to T0+81.408 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -1.05 (-0.13,+0.13),
the high energy photon index beta = -2.37 (-0.14,+0.09),
the peak energy Ep = 169 (-15,+20) keV,
chi2 = 114/97 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140619_T81966/

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

[GCN OPS NOTE(21jun14) Added 140629C to the Subject line,
and changed 140616 to 140619 in the first sentence.]


GRB_name: GRB140619C
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16430
SUBJECT: Correction to GCN 16429 (GRB 140619C)
DATE:    14/06/21 15:26:33 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

V. Pal'shin reports on behalf of the Konus-Wind team:

The correct title of GCN 16429 should be
"Konus-Wind observation of GRB 140619C",
and the GRB name in the text should be also GRB 140619C (not GRB 140616C).


GRB_name: GRB140606B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16431
SUBJECT: GRB 140606B / iPTF 14bfu: SAO RAS optical observations
DATE:    14/06/21 19:30:55 GMT
FROM:    Vladimir Sokolov at SAO RAS  <sokolov@sao.ru>

A.S. Moskvitin, V.N. Komarova, V.V. Sokolov, T.N. Sokolova (SAO RAS),
A.F. Valeev (SAO RAS, Kazan Federal Uni.) report on behalf of a larger
GRB follow-up collaboration:

We observed the GRB 140606B / iPTF 14bfu field (Singer et al.,
GCNC 16360) with the 1-m Zeiss-1000 telescope of SAO RAS on June 19/20,
21:26:29 - 00:22:32 UT (13.8 days since the Fermi/GBM trigger).
25 images in Rc band with the total exposure 7500 seconds were obtained.
Near the GRB OT location we clearly detect an object with the brightness
R = 22.1 +/- 0.2, measured against nearby USNO-B1 stars.

This magnitude agrees with the value measured by Volnova et al.
on June 8 (GCNC 16403). Such stability supports an idea that it may be
the host galaxy of GRB 140606B (Perley et al., GCNC 16365).


GRB_name: GRB140620A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16432
SUBJECT: GRB 140620A: Swift/UVOT Detection
DATE:    14/06/21 21:43:23 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU) and M. De Pasquale (IASF-Palermo) report on behalf of the
Swift/UVOT team:

The Swift/UVOT observed the field of the Fermi/GBM-detected burst GRB 140620A
beginning 37.6 ks after the trigger (Fitzpatrick et al., GCN circ 16426). We confirm
the fading optical transient reported by iPTF (Kasliwal et al., GCN circ 16425) at
a position of:
  RA  (J2000) =  18:47:29.00 = 281.87082 (deg.)
  Dec (J2000) =  49:43:51.0  =  49.73085 (deg.)
with an uncertainty of 0.3 arcsec (radius, 90% confidence). This
is 0.7 arcsec from the iPTF position.

Preliminary detections using the UVOT photometric system (Breeveld et
al. 2011, AIP Conf. Proc. 1358, 373) are given in the following table:

Filter   T_start(ks)   T_stop(ks)   Exp(s)   Mag
u           37.6         43.9       1718     19.78+-0.10
u          124.0        125.3       1251     20.38+-0.18

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


GRB_name: GRB140622A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16433
SUBJECT: GRB 140622A: Swift detection of a short burst
DATE:    14/06/22 09:50:47 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

V. D'Elia (ASDC), S. D. Barthelmy (GSFC), L. Izzo (URoma/ICRA) and
M. H. Siegel (PSU) report on behalf of the Swift Team:

At 09:36:04 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140622A (trigger=602278).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 317.152, -14.430 which is 
   RA(J2000)  =  21h 08m 37s
   Dec(J2000) = -14d 25' 48"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single spike
with a duration of about 0.1 sec.  The peak count rate
was ~2200 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 09:37:37.9 UT, 93.4 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 317.1730, -14.4193
which is equivalent to:
   RA(J2000)  = 21h 08m 41.53s
   Dec(J2000) = -14d 25' 09.5"
with an uncertainty of 2.6 arcseconds (radius, 90% containment). This
location is 82 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 5.47
x 10^20 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 96 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 V. D'Elia (delia AT asdc.asi.it). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB140622A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16434
SUBJECT: GRB 140622A: Enhanced Swift-XRT position
DATE:    14/06/22 16:52:45 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 451 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 140622A, 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 = 317.17317, -14.41931 which is equivalent
to:

RA (J2000): 21h 08m 41.56s
Dec (J2000): -14d 25' 09.5"

with an uncertainty of 2.6 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: GRB140622A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16435
SUBJECT: GRB 140622A: GROND Upper limits
DATE:    14/06/22 18:07:36 GMT
FROM:    Corentin Delvaux at MPE  <delvaux@mpe.mpg.de>

M. Tanga, C. Delvaux and J. Greiner (all MPE Garching) report on behalf of
the GROND team:

We observed the field of GRB 140622A (Swift trigger 602278; D'Elia et al.,
GCN #16433) 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 09:40 UT on June 22, 2014, 0.07 hours after the
GRB trigger. They were performed at an average seeing of 1.3 and at an
average airmass of 1.23.

We do not detect a source within the Swift-XRT error circle reported by
D'Elia et al. (GCN  #16433) down to the following 3-sigma AB magnitudes:

g' > 24.3 mag,
r' > 24.3 mag,
i' > 24.1 mag,
z' > 24.1 mag,
J > 21.3 mag,
H > 20.9 mag, and
K > 19.4 mag.

We report the detection of a faint object at the border of the 2.6"
Swift-XRT error circle at coordinates

   RA(J2000)  =  21:08:41.73
   Dec(J2000) = -14:25:06.5

This object is detected in g', r', i', z' and J and there is no evidence
of fading. Its estimated AB magnitudes are

g' = 23.4 +/- 0.2 mag,
r' = 23.4 +/- 0.2 mag,
i' = 22.5 +/- 0.1 mag,
z' = 22.2 +/- 0.1 mag, and
J = 20.9 +/- 0.3 mag.

At this time, we cannot assert that this object is the host galaxy of GRB
140622A.

The given limits and magnitudes are derived based on calibrating the
images against GROND zeropoints and 2MASS field stars and are not
corrected for the Galactic foreground extinction corresponding to a
reddening of E_(B-V)= 0.07 mag in the direction of the burst (Schlegel et
al. 1998).

[GCN OPS NOTE(22jun14):  Per author's request, the Subject line was corrected
from "140422A" to 140622A".]


GRB_name: GRB140622A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16436
SUBJECT: GRB 140622A: RATIR Optical and NIR Observations
DATE:    14/06/22 19:55:21 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB),
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara
(ORAU/GSFC), 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), and
Harvey Moseley (GSFC) report:

We observed the field of short-duration GRB 140622A (D'Elia, et al., GCN
16433) 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 2014/06 22.40 to
2014/06 22.47 UTC (1.2 minutes to 1.70 hours after the BAT trigger),
obtaining a total of 1.20 hours exposure in the r and i bands and 0.51
hours exposure in the Z and Y bands.

For a source within the Swift-XRT error circle (Osborne, et al., GCN
16434), in comparison with 2MASS, we obtain the following upper limits
(3-sigma):

  r     > 23.64
  i     > 23.49
 Z     > 19.41
  Y     > 18.73

These magnitudes 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: GRB140622A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16437
SUBJECT: GRB 140622A: VLT/X-shooter redshift
DATE:    14/06/22 20:54:43 GMT
FROM:    Olga Hartoog at U of Amsterdam  <O.E.Hartoog@uva.nl>

O.E. Hartoog (API/UvA), D. Malesani (DARK/NBI), R. Sanchez-Ramirez
(IAA-CSIC), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), A.J. Levan (U. of
Warwick), J.P.U. Fynbo (DARK/NBI), P.M. Vreeswijk (Weizmann), L. Kaper
(API/UvA) report on behalf of the X-shooter GRB collaboration:

We observed the field of short GRB140622A (D'Elia et al., GCN 16433) with
the VLT X-shooter spectrograph covering a spectral range 3200A to 18000A,
with a total exposure time of 2x600s. Observations started at UT 10:10:32,
~34 minutes after the trigger. The slit was positioned on the object at
RA(J2000)  =  21:08:41.73, Dec(J2000) = -14:25:06.5 identified by Tanga et
al. (GCN 16435), at the border of the 2.6" XRT error circle.

We detect emission lines from this source at a redshift of z~0.959:
H-alpha, H-beta, [OII], [OIII]. It is likely that this is the host galaxy
of GRB140622A. A very faint trace is detected redwards of ~7000A. This
wavelength coincides with a Balmer jump at the host redshift.

We thank the staff at Paranal for their support in obtaining these
observations.


GRB_name: GRB140622A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16438
SUBJECT: GRB 140622A: An unusual short event, Swift-BAT refined analysis
DATE:    14/06/22 21:32:14 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

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

  Using the data set from T-61 to T+302 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140622A (trigger #602278) (D'Elia, et al.,
GCN Circ. 16433).  The BAT ground-calculated position is
RA, Dec = 317.153, -14.412 deg which is

    RA(J2000)  =  21h 08m 36.7s
    Dec(J2000) = -14d 24' 44.6"

with an uncertainty of 2.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 57%.

The mask-weighted light curve shows a single FRED peak.  T90 (15-350 keV) is
0.13 +- 0.04 sec (estimated error including systematics).

The time-averaged spectrum from T-0.02 to T+0.13 sec is best fit (chisqr = 0.63) by
a black body spectrum with kT = 11.6  1.8 keV.  A simple power-law model is a
relatively poor fit (chisqr 1.13), with a photon index of 3.08  0.29.  A power-law
with an exponential cutoff at 44  8 keV nominally fits the data almost as well
(chisqr = 0.64) as the black body fit, but the power-law index below the cutoff
energy and the normalization are poorly defined.  The fluence in the 15-150 keV
band using the black body spectrum is (2.7  0.5) x 10^-08 erg/cm2.  The 1-sec
peak photon flux measured from T-0.45 sec in the 15-150 keV band is
0.6  0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence level.

 From the BAT spectrum, this event does not appear to be a short hard burst.  The
quickly fading X-ray lightcurve, however (to be reported in a later circular), does
appear consistent with a SHB, and does not appear to be similar to the lightcurves
of SGRs or other Galactic sources.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/602278/BA/


GRB_name: GRB140622A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16439
SUBJECT: GRB 140622A: Swift-XRT refined Analysis
DATE:    14/06/22 21:51:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 7.3 ks of XRT data for GRB 140622A (D'Elia  et al. GCN
Circ. 16433),  from 103 s to 30.9 ks after the BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Osborne et al. (GCN Circ. 16434).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=7.1 (+/-0.9).


If the light curve continues to decay with a power-law decay index of
7.1, the count rate at T+24 hours will be 5.3 x 10^-21 count s^-1

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00602278.

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


GRB_name: GRB140620A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16440
SUBJECT: GRB 140620A / iPTF14cva: Konkoly optical observations
DATE:    14/06/22 23:56:29 GMT
FROM:    Janos Kelemen at Konkoly Obs/Hungary  <kelemen@konkoly.hu>

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

Starting on the evening of 21/06/2014 UT we observed the field of GRB 140620A
(Fermi GBM reported trigger 424934131 at 2014-06-20 05:15:28.02 UT) 
150898 sec. after the burst, using a 60/90/180 cm Schmidt telescope 
located at the Mountain Station of the Konkoly Observatory . On the 
coadded R images (total exp.time 900 sec) we easily detected the OT at the
position reported by M. M. Kasliwal et al. (GCN 16425)

Based on the nearby UCAC-4 stars we provide 21.9 +/- 0.15 magnitude in the R
band for the OT. 

time from GRB.    exp    filter     Mag.      
------------------------------------------------ 
 150898 s.       900 s     R       21.9 +/-0.15 
------------------------------------------------


GRB_name: GRB140622A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16441
SUBJECT: GRB 140622A: KAIT Optical Upper Limit
DATE:    14/06/23 02:35:34 GMT
FROM:    Weikang Zheng at UC Berkeley  <zwk@astro.berkeley.edu>

WeiKang Zheng, Alexei V. Filippenko, Adam Morgan (UC Berkeley), and
S. B. Cenko (NASA/Goddard Space Flight Center) report on behalf of the
KAIT GRB team:

The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, responded to Swift GRB 140622A (D'Elia et al.,
GCN 16433) starting at 09:39:22 UT, 198 s after the burst.
Observations were performed with an automatic sequence in the
clear (roughly R), V, and I filters, and the exposure time was
20 s per image. We do not detect any new source in our
images within the enhanced XRT error circle (Osborne et al.,
GCN 16434). The typical limiting magnitude of our single clear
image is about 19.0 calibrated to USNO B1.0.


GRB_name: GRB140619A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16443
SUBJECT: Konus-Wind observation of GRB 140619A
DATE:    14/06/23 16:41:20 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

The long GRB 140619A (Swift-BAT trigger #602080: De Pasquale, et al.,
GCN Circ. 16415, Palmer, et al., GCN Circ. 16423) was detected by
Konus-Wind in the waiting mode.

The burst light curve shows a single multipeak episode started
at ~T0(BAT)+35 s with a duration of ~340 s.

The K-W light curve of this burst is available at
http://www.ioffe.ru/LEA/GRBs/GRB140619A/

As observed by Konus-Wind, the burst had a fluence of
5.4(-0.5,+0.2)x10^-5 erg/cm2 and a 2.944-s peak energy flux,
measured from ~T0(BAT)+191 s, of 1.5(-0.3,+0.2)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

Modeling the K-W 3-channel time-integrated spectrum (from T0(BAT)+35 s
to T0(BAT)+374 s) by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -1.3 Â± 0.1, and Ep = 236 (-27,+33) keV.

All the quoted errors are estimated at the 1 sigma confidence level.
All the presented results are preliminary.


GRB_name: GRB140621A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16444
SUBJECT: IPN Triangulation of GRB 140621A
DATE:    14/06/23 17:10:14 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

K. Hurley, on behalf of the IPN 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,

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

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

The long-duration GRB 140621A has been observed by Konus-Wind, Fermi(GBM 
trigger 425073013), Swift (BAT), Suzaku (WAM), and INTEGRAL (SPI-ACS), 
so far, at about 71411 s UT (19:50:11). The burst was outside the coded 
field of view of the BAT.

We have triangulated it to a Konus-SPI-ACS annulus centered at 
RA(2000)=73.277 deg (04h 53m 07s)  Dec(2000)=+14.648 deg (+14d 38' 54"), 
whose radius is 46.161 Â± 0.185 deg (3 sigma), and to a GBM-SPI-ACS 
annulus centered at RA(2000)=295.874 deg (19h 43m 30s) Dec(2000)=+52.624 
deg (+52d 37' 26"), whose radius is 73.043 Â± 1.325 deg (3 sigma). These 
annuli intersect to form the error box whose  portion with declination 
lower than about 22.2 degrees is ruled out due to the BAT non-detection 
in the coded FoV.

The corners of the combined IPN+BAT box are:
   ---------------------------------------------
    RA(2000), deg                 Dec(2000), deg
   ---------------------------------------------
   Corners:
     24.883 (01h 39m 32s) +22.492 (+22d 29' 30")
     25.291 (01h 41m 10s) +22.804 (+22d 48' 16")
     25.278 (01h 41m 07s) +22.200 (+22d 12' 00")
     24.879 (01h 39m 31s) +22.200 (+22d 12' 00")
   ---------------------------------------------
The error box area is about 720 sq. arcmin, and its maximum
dimension is 43 arcmin.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB140621_T71407/IPN/

A Swift ToO observation has been requested.

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


GRB_name: GRB140621A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16445
SUBJECT: Konus-Wind observation of GRB 140621A
DATE:    14/06/23 17:42:22 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

GRB 140621A (IPN triangulation: Golenetskii at al., GCN 16444)
triggered Konus-Wind at T0=71407.498 s UT (19:50:07.498).

The burst light curve shows a multipeak structure
from ~T0-0.1 s to ~T0+6.2 s;
the total duration of the burst is ~6.3 s.
The emission is seen up to ~5 MeV.

As observed by Konus-Wind, the burst
had a fluence of 7.8(-1.8,+2.9)x10^-6 erg/cm2,
and a 64-ms peak flux, measured from T0-0.064 s,
of 5.6(-1.2,+1.3)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 a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -1.11 (-0.24,+0.32),
and Ep = 740(-260,+640) keV,
chi2 = 82/98 dof.
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.0.

The spectrum near the maximum count rate
(measured from T0-0.064 to T0+0.064 s)
is best fit in the 20 keV - 1.5 MeV range,
by a power law with exponential cutoff model
with alpha = -0.20(-0.35,+0.55),
and Ep = 340(-80,+140) keV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140621_T71407/

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


GRB_name: GRB140622A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16446
SUBJECT: GRB 140622A: Swift/UVOT Upper Limits
DATE:    14/06/23 19:35:49 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and V. D'Elia (ASDC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140622A
97 s after the BAT trigger (D'Elia et al. GCN Circ. 16433).
No optical afterglow consistent with the XRT position
(Osborne et al. GCN Circ. 16434) 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            97          246          147         >21.2
u_FC               309          559          246         >20.0
white               97         1358          373         >21.2
v                  639         1407           97         >19.6
b                  564         1334           78         >20.1
u                  309         1309          304         >20.2
w1                 688         1285           58         >19.6
m2                 663         1260           78         >20.6
w2                 614         1383           97         >20.2

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).


GRB_name: GRB140621A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16447
SUBJECT: GRB 140621A: Fermi GBM detection
DATE:    14/06/23 21:29:38 GMT
FROM:    George A. Younes at USRA/NASA/MSFC  <younes.ge@gmail.com>

G. Younes (USRA/NASA-MSFC) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:

"At 19:50:10.89 UT on 21 June 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140621A (trigger 425073013/140621827, IPN
triangulation: Golenetskii at al., GCN 16444), which was also detected
by Konus-Wind (Golenetskii et al., GCN 16445), and INTEGRAL SPI-ACS.

The angle from the Fermi LAT boresight, using the GBM on-ground calculated
location, is 97 degrees.

The GBM light curve consists of two prominent peaks
with a duration (T90) of about 6.4 s (50-300 keV).
The time-averaged spectrum from T0-0.064 s to T0+6.14 s is
adequately fit by a Band function with Epeak = 298 +/- 24 keV,
alpha = -0.3 +/- 0.1, and beta = -2.3 +/- 0.2

The event fluence (10-1000 keV) in this time interval is
(1.13 +/- 0.03)E-05 erg/cm^2. The 1 second peak photon flux measured
starting from T0-0.128 s in the 10-1000 keV band
is 8.3 +/- 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: GRB140622A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16448
SUBJECT: GRB 140622A: iTelescope.Net T11 Optical Observation
DATE:    14/06/24 11:00:15 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

D. Kawamura, T. Sakamoto, A. Yoshida (AGU)

We observed the field of GRB 140622A detected by Swift (trigger #602278; 
D'Elia et al., GCN Circ. 16433) with the iTelescope.Net (http://www.itelescope.net) 
T11 (0.51 m Planewave) telescope located at the New Mexico Skies Observatory 
(NM, USA).  

60 images of 60 sec exposures were taken in the R filter starting from June 22 09:50:33 (UT) 
about 14.5 minutes after the trigger and stopped on June 22 11:01:25 (UT).  We do not detect 
the optical afterglow both in the individual images and the stacked image at the enhanced X-ray 
afterglow position (Osborne et al., GCN Circ. 16434).  The estimated five sigma upper limit of 
the combined image (total exposure of 3600 sec) is ~18.5 using the USNO-B1 catalog.


GRB_name: GRB140621A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16449
SUBJECT: GRB 140621A: Swift-XRT observations
DATE:    14/06/24 13:35:43 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia (ASDC), L. Izzo (URoma/ICRA) & J. R. Cummings (NASA/UMBC)  
report on behalf of the Swift-XRT team:

The XRT began observing the field of GRB 140621A on 2014-06-23 at  
21:01:54 UT, 177 ks after the IPN trigger (Golenetskii et al. GCN Circ  
16444, 16445; Younes & Meegan, GCN Circ 16447). An observation  
centered on RA, Dec: 25.0642, 22.4111 has been secured.

In the 4 ks exposure covering 60% of the IPN box that remained after  
the BAT non-detection exclusion, we do not find any new X-ray source,  
down to a three sigma upper limit of 3.05E-03 cts/s.

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


GRB_name: GRB140623A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16450
SUBJECT: GRB 140623A / iPTF14cyb: Fermi GBM detection
DATE:    14/06/24 14:58:54 GMT
FROM:    Andreas von Kienlin at MPE  <azk@mpe.mpg.de>

A. von Kienlin (MPE) reports on behalf of the Fermi GBM Team:

"At 05:22:06.60 UT on 23 June 2014, the Fermi Gamma-Ray Burst Monitor
triggered 
and located GRB 140623A (trigger 425193729 / 140623224), which was observed 
by the intermediate Palomar Transient Factory beginning 11 minutes after 
trigger time, and was reported in GCN 16425 (Bhalerao et al. 2014) as
iPTF14cvb.

The on-ground calculated location, using the GBM trigger
data, is RA = 202.8, DEC = 75.8 (J2000 degrees,
equivalent to 13h 31m, 75d 48'), with an uncertainty
of 5.6 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).
The angle from the Fermi LAT boresight is 32 degrees.

The GBM light curve shows a multiple-peak structure  
with a duration (T90) of about 110 s (50-300 keV).
The time-averaged spectrum from T0-49.2 s to T0+73.7 s is
well fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.46 +/- 0.1  and
the cutoff energy, parameterized as Epeak, is 350(+220/-100) keV

The event fluence (10-1000 keV) in this time interval is
(6.8 +/- 0.6)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0-3.65 s in the 10-1000 keV band
is 1.9 +/- 0.2 ph/s/cm^2.

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


GRB_name: GRB140623A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16451
SUBJECT: GRB 140623A: Swift-XRT and UVOT observations
DATE:    14/06/24 15:21:15 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia (ASDC), F. E. Marshall (NASA/GSFC), L. Izzo (URoma/ICRA) &  
D. Malesani (DARK/NBI) report on behalf of the Swift team:

Following the report of a potential optical afterglow iPTF14cyb  
(Bhalerao et al., GCN Circ. 16442) to the Fermi/GBM-detected burst GRB  
140623A (von Kienlin, GCN Circ. 16450), Swift began a follow-up  
observation of the iPTF field.

We have analyzed all the 3.0 ks of XRT data for GRB 140623A,  from  
38.7 ks to 49.6 ks after the Fermi/GBM trigger. The data are entirely  
in Photon Counting (PC) mode. An X-ray source is detected at a  
position consistent with the candidate optical afterglow (Bhalerao et  
al., GCN Circ. 16442) within the Fermi/GBM error circle.

Using 1153 s of PC mode data and 1 UVOT images, we find an enhanced  
XRT position (using the XRT-UVOT alignment and matching UVOT field  
sources to the USNO-B1 catalogue): RA, Dec = 225.47927, +81.19049  
which is equivalent to:

RA (J2000): 15h 01m 55.02s
Dec(J2000): +81d 11' 25.7"

with an uncertainty of 5.8 arcsec (radius, 90% confidence). This  
position is 5.0 arcsec from the the optical counterpart iPTF14cyb, and  
consistent with it. We cannot determine at the present time whether  
the source is fading.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020388.

The Swift/UVOT began settled observations of the field of GRB 140423A  
38708 s after the GBM trigger. No optical afterglow consistent with  
the optical position (Bhalerao et al. GCN Circ. 16442) 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) are:

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

u                38708        44173          925         >22.0
white            38926        44863          851         >21.9

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.037 in the direction of the burst
(Schlegel et al. 1998).

This circular is an official product of the Swift team.


GRB_name: GRB140624A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16452
SUBJECT: GRB 140624A: Fermi GBM observation of a short burst
DATE:    14/06/24 19:23:39 GMT
FROM:    George A. Younes at USRA/NASA/MSFC  <younes.ge@gmail.com>

G. Younes (USRA/NASA-MSFC), A. von Kienlin (MPE), and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:

"At 10:08:40.90 UT on 24 June 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140624A (trigger 425297323/140624423).

The trigger resulted in an Autonomous Repoint Request (ARR) that was
accepted and the spacecraft slewed to the GBM in-flight location.

The on-ground calculated location, using the GBM trigger
data, is RA = 23.16, DEC = -0.56 (J2000 degrees,
equivalent to 01h 32m, -00d 33'), with an uncertainty
of 4.6 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).

The angle from the Fermi LAT boresight, using the GBM on-ground
calculated location, is 54 degrees.

The GBM light curve consists of a single peak
with a duration of about 0.1 s (50-300 keV).
The time-averaged spectrum from T0-0.064 s to T0+0.064 s is
adequately fit by a Comptonized function with Epeak = 365 +/- 81 keV,
and alpha = -0.8 +/- 0.1.

The event fluence (10-1000 keV) in this time interval is
(3.0 +/- 0.3)E-07 erg/cm^2. The 0.064 second peak photon flux
measured starting from T0+0.0 s in the 10-1000 keV band
is 19.2 +/- 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: GRB140620A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16453
SUBJECT: GRB 140620A / iPTF14cva: TShAO optical observations
DATE:    14/06/24 23:39:18 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), W. Mundrzyjewski (Fesenkov Astrophysical Institute),  A. 
Kusakin (Fesenkov Astrophysical Institute), A. Pozanenko (IKI) report on 
behalf of larger GRB follow-up collaboration:

We observed the optical candiadate iPTF14cva (Kasliwal et al., GCN 16425) of 
Fermi GRB 140620A  (Fermi trig. # 424934131)  (Fitzpatrick  et al., GCN 
16426)   with Zeiss-1000 (East) 1m telescope of Tien Shan Astronomical 
Observatory on June, 20 starting (UT)  21:22:56.  We took several images in 
R-filter. We clearly detected optical transient (Siegel et al., GCN 16432; 
Kelemen  GCN 16440) in a stacked image.

Details of the photometry are following:

date               UT start       t-T0           Filter   Exp.       OT
                       (mid, days)                               (s)

2014-06-20  21:22:56     0.68914    R        20*120  20.37 +/- 0.09

The photometry is based on  star USNO-B1.0 1397-0294956 (RA 18:47:28.76 Dec 
+49:43:44.5) assuming  R=16.35. 


GRB_name: GRB140606B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16454
SUBJECT: GRB140606B/iPTF14bfu: Keck detection of an associated supernova
DATE:    14/06/25 05:24:36 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech), M. L. Graham, A. V. Filippenko (UC Berkeley), 
and S. B. Cenko (GSFC) report:

We acquired a single 1200-second spectrum of iPTF14bfu (Singer et al., 
GCN 16360; Perley et al., GCN 16365), the optical transient associated 
with GRB 140606B (Burns et al., GCN 16363), using the Low Resolution 
Imaging Spectrometer (LRIS) on the Keck I 10-meter telescope.  The 
observation was conducted starting at 13:00 UT on 2014-06-24, 18.4 days 
after the GBM trigger, and covers a wavelength range from 320-1028 
nanometers.

The spectrum shows several broad emission features and a significant 
decrease in flux toward both the blue and red ends.   A comparison with 
SN 1998bw* using superfit (Howell et al. 2005, ApJ 634, 1190) shows a 
good match between the observed features and the spectrum of SN 1998bw 
near maximum light, indicating that the transient has evolved into a 
Type Ic-BL supernova.

* http://www.astro.caltech.edu/~dperley/grb/140606b/140606b_98bw.png


GRB_name: GRB140626A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16456
SUBJECT: GRB 140626A: Swift detection of a burst
DATE:    14/06/26 00:47:35 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

J. R. Cummings (NASA/UMBC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), V. D'Elia (ASDC),
N. Gehrels (NASA/GSFC), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), N. P. M. Kuin (UCL-MSSL),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC) and
D. M. Palmer (LANL) report on behalf of the Swift Team:

At 00:33:01 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140626A (trigger=602604).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 77.350, -82.630 which is 
   RA(J2000)  =  05h 09m 24s
   Dec(J2000) = -82d 37' 46"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a double pulse 
structure with a duration of about 35 sec.  The peak count rate
was ~1500 counts/sec (15-350 keV), at ~5 sec after the trigger. 

The XRT began observing the field at 00:34:41.7 UT, 99.9 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 77.37387, -82.63218 which is equivalent
to:
   RA(J2000)  = 05h 09m 29.73s
   Dec(J2000) = -82d 37' 55.8"
with an uncertainty of 4.0 arcseconds (radius, 90% containment). This
location is 13 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 1.42
x 10^21 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 103 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
0.15. 

Burst Advocate for this burst is J. R. Cummings (jayc AT milkyway.gsfc.nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB140619B
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16457
SUBJECT: GRB 140619B: Suzaku WAM observation of the prompt emission
DATE:    14/06/26 02:16:41 GMT
FROM:    Masanori Ohno at Hiroshima U  <ohno@hep01.hepl.hiroshima-u.ac.jp>

W. Iwakiri(RIKEN), M. Tashiro, Y. Terada, T. Yasuda, S. Koyama, S. Takeda,
T. Nagayoshi, J. Enomoto, S. Nakaya, T. Fujinuma, S. Matsuoka (Saitama U.),
M. Yamauchi, N. Ohmori, R. Kinoshita (Univ. of Miyazaki),
M. Ohno, T. Kawano, S. Furui, Y. Fukazawa(Hiroshima U.),
K. Yamaoka (Nagoya U.), S. Sugita (Ehime U.),
Y. Hanabata (ICRR), Y. E. Nakagawa, M. Kokubun, T. Takahashi (ISAS/JAXA),
Y. Urata (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo)
on behalf of the Suzaku WAM team, report:

The short GRB 140619B (Fermi-GBM detection : Connaughton et al, GCN
16419; Fermi-LAT detection: Kocevski et al., GCN 16420) triggered the
Suzaku Wide-band All-sky Monitor (WAM) which covers an
energy range of 50 keV - 5 MeV at 11:24:40.128 UT (=T0).

The observed light curve shows a single peak, lasting from T0 to T0+1 s
with a duration
(T90) of about 0.7 seconds. The fluence in 100 - 1000 keV was 1.50
(+0.07, -0.22) x10^-6 erg/cm^2.
The 1-s peak flux measured from T0 was 2.29 (+0.19, -0.53)
photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0 to T0+1
s is well fitted by a power-law with exponential cutoff model:
dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
alpha 0.45 (+0.31, -0.37), and
Epeak 1418 (+292, -239) keV (chi^2/d.o.f. = 23.78/29).

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

The light curves with 1-sec time resolution for this burst will be
appeared at:

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


GRB_name: GRB140626A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16458
SUBJECT: GRB 140626A: GROND Afterglow Candidate
DATE:    14/06/26 02:43:50 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

M. Tanga, J. F. Graham (both MPE Garching), D. A. Kann (TLS Tautenburg),
and J. Greiner (MPE Garching) report on behalf of the GROND team:

We observed the field of GRB 140626A (Swift trigger 602604; Cummings et
al., GCN #16456) 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 00:45:12 UT on June 26, 2014, 12 minutes after the
GRB trigger. They were performed at an average seeing of 2.4 and at an
average airmass of 2.5.

We detect a source at the north-eastern edge of the the Swift-XRT error
circle reported by Cummings et al., GCN #16456 at RA (J2000) =
05:09:30.79, Dec. (J2000) = -82:37:50.2, at AB magnitude:

g' = 21.9 +/- 0.1 mag,
r' = 20.9 +/- 0.1 mag,
i' = 20.4 +/- 0.1 mag, and
z' = 19.8 +/- 0.1 mag.

This object is not detected in the DSS. We propose it to be the afterglow
of GRB 140626A but at this time cannot ascertain fading.

The magnitude was derived based on calibrating the image against the GROND
zeropoint and is not corrected for the Galactic foreground extinction
corresponding to a reddening of E_(B-V)= 0.15 mag in the direction of the
burst (Schlegel et al. 1998).

[GCN OPS NOTE(26jun14): Per author's request, the typo of the observation
date in the second paragraph was changed from Jun 22 to Jun 26.]


GRB_name: GRB140626A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16459
SUBJECT: GRB 140626A: Enhanced Swift-XRT position
DATE:    14/06/26 06:37:23 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 1162 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 140626A, 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 = 77.38009, -82.63084 which is equivalent
to:

RA (J2000): 05h 09m 31.22s
Dec (J2000): -82d 37' 51.0"

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

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

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


GRB_name: GRB140626A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16460
SUBJECT: GRB 140626A: Swift/UVOT Upper Limits
DATE:    14/06/26 12:44:27 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (UCL-MSSL) and J. R. Cummings (NASA/UMBC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140626A
103 s after the BAT trigger (Cummings et al., GCN Circ. 16456).
No optical afterglow consistent with the XRT position
(Beardmore et al. GCN Circ. 16459)
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           103          253          147         >20.9
u_FC               262          511          246         >20.3
white              103         1538          392         >21.1
v                  592         1590          117         >19.0
b                  517         1514           97         >20.0
u                  262         1489          343         >20.4
w1                 642         1639          117         >19.4
m2                 617         1440           39         >19.1
w2                 568         1563          117         >19.9

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: GRB140626A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16461
SUBJECT: GRB 140626A: Swift-XRT refined Analysis
DATE:    14/06/26 12:47:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.A. Kennea (PSU), B.P. Gompertz (U. Leicester), J.P. Osborne (U.
Leicester), K.L. Page (U. Leicester), M. de Pasquale (INAF-IASFPA), A.
Maselli  (INAF-IASFPA), A. Melandri (INAF-OAB), V. Mangano (PSU), M.C.
Stroh (PSU) and J.R. Cummings report on behalf of the Swift-XRT team:

We have analysed 8.5 ks of XRT data for GRB 140626A (Cummings  et al.
GCN Circ. 16456),  from 86 s to 18.9 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 Beardmore et al. (GCN Circ.
16459).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.52 (+/-0.11).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.06 (+0.34, -0.27). The
best-fitting absorption column is  1.8 (+1.2, -0.4) x 10^21 cm^-2,
consistent with the Galactic value of 1.4 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 3.4 x 10^-11 (4.6 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.8 (+1.2, -0.4) x 10^21 cm^-2
Galactic foreground: 1.4 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.06 (+0.34, -0.27)

If the light curve continues to decay with a power-law decay index of
0.52, the count rate at T+24 hours will be 7.5 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.5 x
10^-13 (3.4 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/00602604.

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


GRB_name: GRB140626A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16462
SUBJECT: GRB 140626A: Swift-BAT refined analysis
DATE:    14/06/26 12:49:33 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

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

Using the data set from T-240 to T+962 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140626A (trigger #602604)
(Cummings, et al., GCN Circ. 16456).  The BAT ground-calculated position is
RA, Dec = 77.163, -82.625 deg which is
    RA(J2000)  =  05h 08m 39.1s
    Dec(J2000) = -82d 37' 29.5"
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The mask-weighted light curve shows a double-peaked structure.  The first peak 
extends from T-10 sec to T+0 sec, while the second, comparably-sized peak 
extends from T+0 sec to T+10 sec. T90 (15-350 keV) is 16.4 +- 1.4 sec (estimated 
error including systematics).

The time-averaged spectrum from T-8.94 to T+9.08 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 0.61 +- 0.88,
and Epeak of 44.7 +- 9.5 keV (chi squared 45.83 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 3.6 +- 0.5 x 10^-7 erg/cm2
and the 1-sec peak flux measured from T+5.68 sec in the 15-150 keV band is
0.7 +- 0.1 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.91 +- 0.17 (chi squared 54.28 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/602604/BA/


GRB_name: GRB140623A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16464
SUBJECT: GRB 140623A: further Swift-XRT observations
DATE:    14/06/27 13:41:23 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia (ASDC), L. Izzo (URoma/ICRA) report on behalf of the Swift-XRT team:

We report further Swift-XRT observations of GRB 140623A (A. von  
Kienlin, GCN Circ 16450; Bhalerao et al., GCN Circ. 16442). A new  
exposure of 5 ks has been secured 285 ks after the Fermi/GBM  
detection. The X-ray counterpart detected by D'Elia et al. (GCN Circ.  
16451) is no longer present down to a three sigma upper limit of  
2.2E-3 cts/s.

We thus conclude that the source reported in D'Elia et al. (GCN Circ.  
16451) is the X-ray afterglow of GRB 140623A.

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


GRB_name: GRB140619B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16466
SUBJECT: GRB 140619B: Magellan near-infrared observations
DATE:    14/06/27 21:33:59 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

W. Fong (Harvard), A. Monson (OCIW), M. Bayliss (Harvard), A. Stark
(Harvard), E. Berger (Harvard), B. Stalder (Harvard), and M. Florian (U.
Chicago) report:

"We observed the location of the short-duration GRB 140619B, detected by
Fermi/GBM (Connaughton et al., GCN 16419), Fermi/LAT (Kocevski et al., GCN
16420), and Suzaku/WAM (Iwakiri et al., GCN 16457) with the FourStar
Infrared Camera mounted on the Magellan/Baade 6.5-m telescope to cover the
Fermi/LAT position (90% containment; Kocevski et al., GCN 16420). We
obtained 770 sec of J-band observations on 2014 Jun 20.96 UT (1.48 days
post-burst). To check for the presence of a fading near-infrared source, we
re-observed the field (2300 sec) on 2014 Jun 21.97 UT, 2.49 days post-burst
and 1.01 days after the first set of observations.

Digital image subtraction of the two epochs using the ISIS software package
reveals no residuals in or around the Fermi/LAT position. We therefore
place a 3-sigma limit of J>22.9 AB mag on the brightness of the
near-infrared afterglow of GRB 140619B at 1.48 days after the burst."


GRB_name: GRB140628A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16467
SUBJECT: GRB 140628A: Swift detection of a burst
DATE:    14/06/28 14:01:58 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

E. Sonbas (NASA/GSFC/Adiyaman Univ.), M. G. Bernardini (INAF-OAB),
P. D'Avanzo (INAF-OAB), H. A. Krimm (CRESST/GSFC/USRA),
N. P. M. Kuin (UCL-MSSL), A. Y. Lien (NASA/GSFC/ORAU),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL) and M. H. Siegel (PSU)
report on behalf of the Swift Team:

At 13:35:37 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140628A (trigger=602803).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 40.661, -0.366 which is 
   RA(J2000) = 02h 42m 39s
   Dec(J2000) = -00d 21' 58"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 10 sec.  The peak count rate
was ~2500 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field after coming out of SAA mode at 
13:39:40.3 UT, 243 seconds after the BAT trigger. No source was 
detected in 20 s of promptly downlinked data. We are waiting 
for the full dataset to detect and localize the XRT counterpart. 

UVOT took a finding chart exposure of  48 seconds with the White filter
starting 278 seconds after the BAT trigger. No credible afterglow candidate has
been found in a partial 2.7'x2.7' sub-image. Results from the list of sources
generated on-board are not available at this time. 

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


GRB_name: GRB140622A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16468
SUBJECT: GRB 140622A: TAROT La Silla observatory optical observations
DATE:    14/06/28 16:14:27 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

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

We imaged the field of GRB 140622 detected by SWIFT
(trigger 602278) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 23.2s after the GRB trigger
(12.7s after the notice). The elevation of the field decreased from
61 degrees above horizon and weather conditions
were excellents. Images were not accessible during one week
due to a disk access problem.

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+23.2s to t0+83.2s : R > 17.5

The second image is 30.0s exposure in tracking mode:
t0+96.6s to t0+126.6s : R > 18.0

We co-added a series of exposures:
t0+96.6s to t0+389.1s : R > 18.4

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


GRB_name: GRB140626A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16469
SUBJECT: GRB 140626A: TAROT La Silla observatory optical observations
DATE:    14/06/28 16:54:48 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

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

We imaged the field of GRB 140626A detected by SWIFT
(trigger 602604) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 72.1s after the GRB trigger
(15.9s after the notice). The elevation of the field decreased from
23 degrees above horizon and weather conditions
were good. Images were not accessible during two days
due to a disk access problem.

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+72.1s to t0+132.1s : R > 16.6

The second image is 30.0s exposure in tracking mode:
t0+145.4s to t0+175.4s : R > 17.6

We co-added a series of exposures:
t0+145.4s to t0+437.3s : R > 19.2

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


GRB_name: GRB140628A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16470
SUBJECT: GRB 140628A: Swift-XRT afterglow detection and enhanced position
DATE:    14/06/28 18:52:42 GMT
FROM:    Maria Grazia Bernardini at INAF/Brera  <grazia.bernardini@brera.inaf.it>

P. D'Avanzo, M.G. Bernardini, A. Melandri (INAF/OAB), P.A. Evans and
M.R. Goad (U. Leicester) report on behalf of the Swift-XRT team:


Using promptly downlinked data we find an uncatalogued and
fading X-ray source. Using 40 s of XRT Photon Counting mode
data and 1 UVOT image, 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 =40.66674, -0.38488 which is equivalent to:

RA (J2000):  02 42 40.02
Dec (J2000): -00 23 05.6

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 is an official product of the Swift-XRT team.


GRB_name: GRB140628A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16471
SUBJECT: GRB 140628A: Swift/UVOT Detection
DATE:    14/06/28 21:31:59 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU), N. P. M. Kuin (UCL-MSSL) and E. Sonbas (NASA/GSFC/Adiyaman Univ.)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140628A
278 s after the BAT trigger (Sonbas et al., GCN Circ. 16467).
A source consistent with the XRT position
(D'Avanzo et al. GCN Circ. 16470)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
   RA  (J2000) =  02:42:39.88 =  40.66617 (deg.)
   Dec (J2000) = -00:23:05.7  =  -0.38491 (deg.)
with an estimated uncertainty of 0.46 arc sec. (radius, 90% confidence).

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

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

white              278          327           48         17.70 +/- 0.08
v                 3749         3949          197         19.08 +/- 0.28
b                 4569         4769          197        >20.2
u                 4364         4564          197        >19.5
w1                4159         4359          197        >19.8
m2                3954         4154          197        >21.2
w2                9366        10266          886        >21.1

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


GRB_name: GRB140628A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16472
SUBJECT: GRB 140628A: Swift/UVOT Detection
DATE:    14/06/28 21:52:10 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (UCL-MSSL) and E. Sonbas (NASA/GSFC/Adiyaman Univ.)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140628A
278 s after the BAT trigger (Sonbas et al., GCN Circ. 16467).  A source
consistent with the XRT position (D'Avanzo et al. GCN Circ. 16470)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  02:42:39.88 =  40.66617 (deg.)
    Dec (J2000) = -00:23:05.7  =  -0.38491 (deg.)
with an estimated uncertainty of 0.46 arc sec. (radius, 90% confidence).

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

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

white              278          327           48         17.43 +/- 0.08
white             3593         4974          300        >21.0
v                 3749         3949          197         19.08 +/- 0.28
b                 4569         4769          197        >20.2
u                 4364         4564          197        >19.5
w1                4159         4359          197        >19.8
m2                3954         4154          197        >21.2
w2                9366        10266          886        >21.1

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


GRB_name: GRB140628A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16473
SUBJECT: GRB 140628A: Swift-BAT refined analysis
DATE:    14/06/28 23:53:48 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU),
E. Sonbas (NASA/GSFC/Adiyaman Univ.), M. Stamatikos (OSU), J. Tueller (GSFC),
T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-60 to T+243 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 140628A (trigger #602803)
(Sonbas, et al., GCN Circ. 16467).  The BAT ground-calculated position is
RA, Dec = 40.672, -0.378 deg which is 
   RA(J2000)  =  02h 42m 41.2s 
   Dec(J2000) = -00d 22' 39.8" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 73%.
 
The mask-weighted light curve ~3 overlapping peaks starting at ~T-15 sec,
peaking at ~T+2 sec, and ending at ~T+30 sec.  T90 (15-350 keV) is
10.5 +- 0.9 sec (estimated error including systematics).
 
The time-averaged spectrum from T-1.24 to T+11.12 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.56 +- 0.09.  The fluence in the 15-150 keV band is 1.3 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+0.94 sec in the 15-150 keV band
is 2.8 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/602803/BA/


GRB_name: GRB140628A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16474
SUBJECT: GRB 140628A: Zadko observatory - Gingin optical observations
DATE:    14/06/29 01:25:11 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

A. Klotz, D. Turpin (IRAP-CNRS-OMP), D. Macpherson (UWA/ICRAR),
D. Coward (UWA),
M. Boer, B. Gendre, K. Siellez, H. Dereli, O. Bardho (UNS-CNRS-OCA),
A. Williams (PO-UWA), R. Martin (PO-UWA) report:

We imaged the field of GRB 140628A detected by SWIFT
(trigger 602803) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 6.72h after the GRB trigger.
The elevation of the field increased from
22 degrees above horizon and weather conditions
were poor.

We co-added a series of exposures. We do not
see any optical counterpart at the UVOT position mentioned
by Kuin et al. (GCNC 16472):

t0+6.72h to t0+7.27h : Rlim = 19.9

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


GRB_name: GRB140628A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16475
SUBJECT: GRB 140628A: Swift-XRT refined Analysis
DATE:    14/06/29 06:59:22 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, M.G. Bernardini, A. Melandri (INAF/OAB), P.A. Evans (U.
Leicester) and E. Sonbas (NASA/GSFC/Adiyaman Univ.) report on behalf of
the Swift-XRT team:

We have analysed 8.2 ks of XRT data for GRB 140628A (Sonbas  et al. GCN
Circ. 16467),  from 231 s to 23.2 ks after the BAT trigger. The data
comprise 47 s in Windowed Timing (WT) mode with the remainder in Photon
Counting (PC) mode. Using 5310 s of PC mode data and 10 UVOT images, we
find an enhanced XRT position (using the XRT-UVOT alignment and
matching UVOT field sources to the USNO-B1 catalogue): RA, Dec =
40.66617, -0.38489 which is equivalent to:

RA (J2000): 02h 42m 39.88s
Dec(J2000): -00d 23' 05.6"

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

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.21 (+0.03, -0.04).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.88 (+0.19, -0.18). The
best-fitting absorption column is  8.9 (+5.3, -4.7) x 10^20 cm^-2, in
excess of the Galactic value of 3.2 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 3.5 x 10^-11 (4.2 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      8.9 (+5.3, -4.7) x 10^20 cm^-2
Galactic foreground: 3.2 x 10^20 cm^-2
Excess significance: 2.0 sigma
Photon index:      1.88 (+0.19, -0.18)

If the light curve continues to decay with a power-law decay index of
1.21, the count rate at T+24 hours will be 4.5 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.6 x
10^-13 (1.9 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00602803.

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


GRB_name: GRB140628A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16476
SUBJECT: GRB 140628A: GROND observation of the afterglow
DATE:    14/06/29 13:39:38 GMT
FROM:    Sebastian Schmidl at TLS Tautenburg  <schmidl@tls-tautenburg.de>

C. Delvaux (MPE Garching), S. Schmidl (TLS Tautenburg), and J. Greiner
(MPE Garching) report on behalf of the GROND team:

We observed the field of GRB 140628A (Swift trigger 602803; Sonbas et
al., GCN 16467) simultaneously in g'r'i'z'JHK with GROND (Greiner et al.
2008, PASP 120, 405) mounted at the 2.2m MPG telescope at ESO La Silla
Observatory (Chile).

Observations started at 08:39 UT on June 29, 2014, 19.1 hrs after
the GRB trigger. They were performed at an average seeing of 1.6" and at
an average airmass of 1.6.

We detect a source consistent with the Swift/UVOT position, reported by
Siegel et al. (GCN 16471).

Based on a total exposure of 50 min in g'r'i' and 40 min in JHK, at a
mid-time of 20.2 hrs after the burst, we measure the following
preliminary magnitudes (in AB):

g' = 23.6 +/- 0.2 mag
r' = 23.1 +/- 0.1 mag
i' = 22.9 +/- 0.2 mag
J  > 21.2 mag,
H  > 20.1 mag, and
K  > 19.1 mag.

In addition we measure z' = 22.1 +/- 0.2 (in AB magnitude system), based
on a total exposure of 25 min, at a midtime of 20.5 hrs after burst.

Given magnitudes are calibrated against SDSS (g'r'i'z') as well as 2MASS
(JHK) field stars and are not corrected for the expected Galactic
foreground extinction corresponding to a reddening of E_(B-V) = 0.03 mag
in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB140629A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16477
SUBJECT: GRB 140629A: Swift detection of a burst with an optical counterpart
DATE:    14/06/29 14:29:09 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC),
M. G. Bernardini (INAF-OAB), P. D'Avanzo (INAF-OAB),
J. A. Kennea (PSU) and K. L. Page (U Leicester) report on behalf of
the Swift Team:

At 14:17:30 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140629A (trigger=602884).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 248.982, +41.890 which is 
   RA(J2000)  =  16h 35m 56s
   Dec(J2000) = +41d 53' 25"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows an initial rise of the event
starting at ~T-5 sec out to ~T+5 sec, at which point there is a gap in the
TDRSS light curve so nothing can be said at this time for the light curve
past T+5 sec.  The peak count rate was ~2000 counts/sec (15-350 keV), at ~0 sec
after the trigger. 

The XRT began observing the field at 14:19:04.5 UT, 94.2 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 248.97675, 41.87702 which
is equivalent to:
   RA(J2000)  = 16h 35m 54.42s
   Dec(J2000) = +41d 52' 37.3"
with an uncertainty of 4.0 arcseconds (radius, 90% containment). This
location is 48 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. No
spectrum from the promptly downlinked event data is yet available to
determine the column density. 

The initial flux in the 2.5 s image was 6.08e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 101 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 16:35:54.46 = 248.97691
  DEC(J2000) = +41:52:36.7  =  41.87685
with a 90%-confidence error radius of about 0.74 arc sec. This position is 0.8
arc sec. from the center of the XRT error circle. The estimated magnitude is
14.81 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.01. 

Burst Advocate for this burst is A. Y. Lien (yarleen 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: GRB140629A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16478
SUBJECT: GRB 140629A: MASTER OT detection
DATE:    14/06/29 15:24:00 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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

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

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

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

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Blagoveschensk was pointed to the  GRB140629A (Lien et. al GCN 
16477) 15 sec after notice time and 33 sec after trigger time at 
2014-06-29 14:18:03.188 UT. On our first (10s exposure) set we found 
optical transient  within SWIFT error-box (ra=16 35 55 dec=+41 53 24 
r=0.050000).
The OT coordinates are Ra 16:35:54.41 Dec +41:52:36.53 and magnitude  is 
15.3 on first images. The OT rises up to 14 mag on following images.


GRB_name: GRB140629A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16479
SUBJECT: GRB 140629A: Enhanced Swift-XRT position
DATE:    14/06/29 18:14:23 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 794 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 140629A, 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 = 248.97716, +41.87689 which is equivalent
to:

RA (J2000): 16h 35m 54.52s
Dec (J2000): +41d 52' 36.8"

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: GRB140629A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16480
SUBJECT: GRB 140629A : Xinglong TNT optical observation
DATE:    14/06/29 18:19:26 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

L. P. Xin,   T. M. Zhang,  H. Liu,  J. Y. Wei,  Y. L. Qiu, J. S. Deng,  
J. Wang,  H. L. Li,   X. H. Han and C. Wu, H. Liu on behalf of EAFON report:

We began to observe GRB 140629A (Lien et al. GCN  16477)  
with Xinglong  0.8-m TNT telescope at 14:27:11 (UT) , 
581 sec after the burst. The observations are continued for 1.6 hours.

The optical counterpart reported by (Lien et al.  GCN 16477;  
Yurkov et al., GCN 16478) was clearly detected in multi-wavelength images. 
The brightness of the  optical emission is decaying from 14.7mag 
to 17.8 mag in R band. The decay slope is  estimated to be about 1.2 
in our observation epoch.

The message may be cited.


GRB_name: GRB140629A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16481
SUBJECT: GRB 140629A: Swift-BAT refined analysis
DATE:    14/06/29 18:26:41 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+622 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 140629A (trigger #602884)
(Lien, et al., GCN Circ. 16477).  The BAT ground-calculated position is
RA, Dec = 249.017, 41.897 deg, which is 
   RA(J2000)  =  16h 36m 04.1s 
   Dec(J2000) = +41d 53' 49.6" 
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 41%.
 
The mask-weighted light curve shows several overlapping peaks starting
at ~T-8 sec, peaking at ~T+12 sec, and ending at ~T+90 sec.
T90 (15-350 keV) is 42.0 +- 14.3 sec (estimated error including systematics).
 
The time-averaged spectrum from T-7.53 to T+56.47 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.86 +- 0.11.  The fluence in the 15-150 keV band is 2.4 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+12.47 sec in the 15-150 keV band
is 4.2 +- 0.4 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/602884/BA/


GRB_name: GRB140629A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16482
SUBJECT: GRB 140629A: RTT150 optical observations
DATE:    14/06/29 20:02:26 GMT
FROM:    Rodion Burenin at IKI, Moscow  <rodion@hea.iki.rssi.ru>

I. Bikmaev (KFU/AST), I. Khamitov (TUG),
E. Irtuganov, N. Sakhibullin (KFU/AST),
R. Burenin, M. Pavlinsky, R. Sunyaev (IKI),
H. Kirbiyik (TUG), U. Kiziloglu (METU), E. Gogus (Sabanci Uni.)

report:

The field of the optical afterglow of GRB 140629A (Lien et al., GCN
16477, Yurkov et al., GCN 16478) was observed with Russian-Turkish
1.5-m telescope (RTT150, Bakirlitepe, TUBITAK National Observatory,
Turkey) using the TFOSC instrument.

We obtained series of BVRcIc exposures. Start time is June 29, 18:33
UT. The optical transient is clearly detected in each images at
RA,DEC = 16:35:54.44 +41 52 36.7 +/- 0.1 arcsec (J2000).

Using the star at RA,DEC = 16:35:59.9 +41:51:10 (J2000) with USNO-B1
magnitude R1_mag = 16.49 as a reference we estimated the Rc-magnitude
of the afterglow:

Filter exptime   T-T0,   Mag. +/- Mag.err
        (sec)   (hour)
Rc       60      4.267   18.00 +/- 0.05

Further OT observations are ongoing at RTT-150.


GRB_name: GRB140629A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16483
SUBJECT: GRB 140629A : Virtual Telescope optical observations
DATE:    14/06/29 20:31:34 GMT
FROM:    Gianluca Masi at Bellatrix Astronomical Obs  <gianluca@bellatrixobservatory.org>

G. Masi, the Virtual Telescope Project - Italy, reports:

I started observations of GRB 140629A (Lien et al. GCN  16477) with the 14" 
robotic unit part of the Virtual Telescope at 20:12:00 (UT), 21300 seconds after 
the burst.

The optical afterglow reported earlier (Lien et al. GCN 16477;  Yurkov et al., 
GCN 16478; Xin et al., GCN 16480) was detected in 300 seconds exposures, 
unfiltered. The position of the source is RA: 16h35m54.43s; Decl.: +41d52'36.3" 
and the magnitude was estimated to be 18.8, assuming R mags for the reference 
stars from UCAC-4

The message may be cited.


GRB_name: GRB140629A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16484
SUBJECT: GRB 140629A: KWFC z-band photometry
DATE:    14/06/29 21:41:04 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

Hiroyuki Maehara (Univ. of Tokyo) reports on behalf of the OISTER collaboration:

We observed the field of GRB 140629A (Lien et al. GCN 16477) with the 1.05-m
Schmidt telescope and KWFC (Sako et al. 2012, Proc. SPIE 8446, 84466L) at
Kiso Observatory in Japan. The observations were made in the Sloan z-band at
2014-06-29 14:30-14:39 (UT; 13-22 min post burst) and 16:30-16:45 (133-148
min post burst).

We detected an uncatalogued fading source at RA=16:35:54.45, DEC=+41:52:36.6
(equinox 2000.0; uncertainty 0".3).$B!!(BPreliminary photometry of the source
is as follows:

obs. date (mid time)  t-T0 (days)  exp.(sec)  filter  mag           limiting mag
2014-06-29 14:30:30   0.0090       180 sec    z       14.89+/-0.02  19.4
           14:34:47   0.0120       180        z       15.23+/-0.02  19.4
           14:39:05   0.0150       180        z       15.50+/-0.02  19.4
           16:30:34   0.0924       180        z       17.68+/-0.06  19.1
           16:34:52   0.0954       180        z       18.01+/-0.08  19.1
           16:45:18   0.1026       180        z       17.87+/-0.08  18.9

The photometry is based on z-mag of SDSS stars in the observed field.


GRB_name: GRB140629A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16485
SUBJECT: GRB 140629A: NOT optical observations
DATE:    14/06/29 22:16:05 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

Daniele Malesani (DARK/NBI), Nicolaas E. Groeneboom (UiO), Jostein R. 
Kristiansen (HiOA), and Pall Jakobsson (Univ. Iceland), report on behalf 
of a larger collaboration:

We observed the field of GRB 140629A (Lien et al., GCN 16477) with the 
Nordic Optical Telescope (NOT) equipped with the MOSCA imager. 
Observations were carried out in the SDSS g, r, i, and z filters. The 
afterglow is detected in all filters.

In a 300-s image started at 21:17 UT (7.0 hr after the GRB), the 
afterglow has a magnitude r = 19.54 +- 0.02 (AB), calibrated against 
several nearby SDSS stars. Calibrated against USNO-B1, the afterglow 
coordinates are (J2000):

RA = 16:35:54.45
Dec = +41:52:36.5

with an uncertainty of 0.3". This is in good agreement with the 
determinations by UVOT (Lien et al., GCN 16477), MASTER (Yurkov et al., 
GCN 16478), and KWFC (Maehara, GCN 16484).


GRB_name: GRB140629A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16486
SUBJECT: GRB 140629A: T100 observations
DATE:    14/06/29 22:56:55 GMT
FROM:    Eda Sonbas at NASA/GSFC  <edasonbas@gmail.com>

E. Sonbas (Adiyaman Univ.), F. Dolek (Cukurova Univ.), T. Guver (Istanbul
Univ.), , E. Gogus (Sabanci Univ.), O. Erece (Akdeniz Univ.), M. Camurdan,
D. Zengin Camurdan (Ege Univ.), H. Kirbiyik (TUG) report on behalf of a
larger collaboration


 We observed the field of Swift GRB 140629A (Lien et al., GCN#16477) with
the 1.0 meter T100 telescope (Bakirlitepe, TUBITAK National Observatory,
Turkey), starting June, 29, 18:42:13 UT (~ 4.412 hours after the trigger).
The afterglow is clearly detected in 300 s in the R band images.


Using USNO-B1 star USNO-B1 1318-0308023 (R.A.=248.99, Dec=+41.85) in the
field, the magnitudes of the OT were estimated as follows;


t-t0 (hr) exp.(s) filt mag err (+/-)

4.412 300 R 18.59 0.03

4.511 300 R 18.61 0.03


 We are grateful to TUBITAK National Observatory for prompt scheduling the
observations and technical support.


GRB_name: GRB140629A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16487
SUBJECT: GRB140629A: Kanata/HOWPol optical observation
DATE:    14/06/29 23:33:24 GMT
FROM:    Koji Kawabata at HASC,Hiroshima U  <kawabtkj@hiroshima-u.ac.jp>

K. Takaki, T. Nakaoka, Y. Moritani, K. S. Kawabata (Hiroshima Univ.) report 
on behalf of Kanata team:

We performed a series of optical imaging polarimetry for the optical 
afterglow of GRB140629A (Yurkov et al., GCN 16478, Xin et. al GCN 16480,
Bikmaev et al., GCN 16482) from 73 sec after the Swift/BAT trigger 
(Lien et al., GCN 16477) with HOWPol attached to the 1.5-m Kanata telescope 
at Higashi-Hiroshima Observatory, Japan. 

Calibrated with USNO-B1 catalogue, our quick-look photometry indicates that 
the R-band magnitude of the optical afterglow was 14.0 at the beginning of 
our observation, reached its peak brightness of 13.3 mag around 160 sec, 
and then smoothly declined. Further analysis is ongoing.


GRB_name: GRB140629A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16488
SUBJECT: GRB 140629A: MITSuME Ishigakijima Optical Observation
DATE:    14/06/30 01:11:31 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 140629A (Lien et al., GCNC 16477)
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 2014-06-29 14:20:40 UT (~3.2 min after the burst).
We detected the previously reported afterglow (Yurkov et al., GCNC 16478;
Xin et al., GCNC 16480; Bikmaev et al., GCNC 16482; Masi, GCNC 16483;
Maehara, GCNC 16484) in all the three bands.

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

#T0+[day]  MID-UT    T-EXP[sec]  g'    g'_err  Rc    Rc_err  Ic    Ic_err
--------------------------------------------------------------------------
0.00254    14:21:10      60.0    14.37 0.03    13.18 0.03    13.65 0.03
0.21351    19:24:57     540.0    19.47 0.14    18.95 0.09    18.17 0.12
--------------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB140629A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16489
SUBJECT: GRB 140629A: BTA redshift
DATE:    14/06/30 02:08:02 GMT
FROM:    Rodion Burenin at IKI, Moscow  <rodion@hea.iki.rssi.ru>

A. Moskvitin (SAO-RAS, N. Arkhyz), R. Burenin (IKI, Moscow),
R. Uklein, V. Sokolov (SAO-RAS, N. Arkhyz), R. Sanchez-Ramirez,
J. Gorosabel and A. J. Castro-Tirado (IAA-CSIC, Granada), on behalf of
a larger collaboration, report:

Following the detection of GRB 140629A by Swift (Lien et al. GCNC
16477), we observed the optical counterpart (Lien et al., GCNC 16477,
Yurkov et al. GCNC 16478) with the 6-m BTA (+Scorpio-I) on June 29,
starting 4.1 hours after the event. We obtained 43.6 minutes of
spectral data in the range 4000-9800A and resolution FWHM = 13A. The
optical afterglow spectrum shows prominent absorption lines which we
interpret as AlIII, CIV, CII, FeII, MgII, SiIV at the redshift 
z = 2.275 +/- 0.003. We suggest this to be the redshift to GRB
140629A.


GRB_name: GRB140629A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16490
SUBJECT: GRB 140629A: Swift-XRT refined Analysis
DATE:    14/06/30 04:29:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 10 ks of XRT data for GRB 140629A (Lien  et al. GCN
Circ. 16477),  from 80 s to 34.9 ks after the  BAT trigger. The data
comprise 136 s in Windowed Timing (WT) mode (the first 10 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Evans et
al. (GCN Circ. 16479).

The late-time light curve (from T0+4.2 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.37 (+/-0.09).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.82 (+0.17, -0.16). The
best-fitting absorption column is  4.5 (+3.8, -3.4) x 10^20 cm^-2, in
excess of the Galactic value of 9.3 x 10^19 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.98 (+/-0.10) and a
best-fitting absorption column of 5.2 (+2.2, -2.0) x 10^20 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.3 x 10^-11 (3.7 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.2 (+2.2, -2.0) x 10^20 cm^-2
Galactic foreground: 9.3 x 10^19 cm^-2
Excess significance: 3.5 sigma
Photon index:      1.98 (+/-0.10)

If the light curve continues to decay with a power-law decay index of
1.37, the count rate at T+24 hours will be 7.4 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.4 x
10^-13 (2.8 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00602884.

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


GRB_name: GRB140629A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16491
SUBJECT: GRB 140629A: P60 observations
DATE:    14/06/30 06:10:50 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) and S. B. Cenko (NASA/GSFC) report:

We imaged the location of Swift GRB 140629A (Lien et al., GCN 16477) 
with the Palomar 60-inch (P60) robotic telescope on UT 2014-06-30 
between 04:10 and 04:44 UT, in the r' filter.  We acquired 10 exposures 
of 180 seconds each.  The optical afterglow (Lien et al., GCN 16477;
Yurkov et al. GCN 16478) is well-detected in the stacked image. 
Comparing to SDSS field stars, we measure a magnitude of:

r = 20.91 +/- 0.03   (t_mid = 0.590 days)

Further observations are ongoing.


GRB_name: GRB140629A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16492
SUBJECT: GRB140629A: VATT optical observations
DATE:    14/06/30 09:08:08 GMT
FROM:    Peter Garnavich at U of Notre Dame  <pgarnavi@nd.edu>

P. Garnavich and B. Rose (Notre Dame)

We observed the field of GRB140629A (Lien et al. GCN 16477) with the
Vatican Advanced Technology Telescope and VATT4K CCD camera
on 2014 June 30.2757 (UT). The afterglow is well-detected in two 300s
exposures through a SDSS-r filter.

Calibrating from SDSS stars in the field we estimate the afterglow to be
r=21.08 +/- 0.03 mag at 16.33 hours after the burst.

Combining the brightness reported here and SDSS magnitudes estimated by
Malesani et al. (GCN 16485) and Perley et al. (GCN 16491), the optical power
law decay index is 1.7 between 7 and 16 hours after the burst.


GRB_name: GRB140629A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16493
SUBJECT: GRB 140629A: TNG redshift confirmation
DATE:    14/06/30 10:04:17 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo (INAF-OAB), D. Malesani (DARK/NBI), V. D'Elia, L.A. Antonelli (INAF/OAR & ASI/ASDC), G. Tagliaferri (INAF-OAB), S.D. Vergani (CNRS/GEPI), A. Fiorenzano, G. Mainella (INAF/TNG) report on behalf of the CIBO collaboration:


We observed the optical afterglow of GRB 140629A (Lien et al., GCN 16477; Yurkov et al. GCN 16478) on 2014 June 30 with the 3.6m TNG telescope located in the Canary Islands, equipped with the DOLORES operated in both imaging and spectroscopic mode. The observations were carried out under poor weather conditions (clouds and calima). 

In a 120 s image started at 01:41:38 UT (~11.4 hr after the GRB), the afterglow has a magnitude r = 20.4 +/- 0.1 (AB), calibrated against nearby SDSS stars.

We also obtained three optical spectra, each one lasting 1200 s, using the grism LR-B covering the wavelength range 3000 - 8000 AA. The observation started at 02:07:21 UT (~11.8 hr after the GRB). Using a preliminary wavelength calibration, in the co-added spectrum we detect several absorption lines which we interpret as due to Ly-alpha, C II (1334), C IV (1548/1550) at a common redshift of 2.29. Our result is in agreement with the redshift reported by Moskvitin et al. (GCN 16489).


GRB_name: GRB140629A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16494
SUBJECT: GRB 140629A: Swift/UVOT Detection
DATE:    14/06/30 11:32:49 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (UCL-MSSL) and A. Y. Lien (GSFC/UMBC) report on behalf of 
the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140629A 
101 s after the BAT trigger (Lien et al., GCN Circ. 16477).
A fading source consistent with the XRT position (Evans et al. GCN Circ. 
16479) is detected in the initial UVOT exposures. The fact that it is 
not seen in uvm2 or uvw2 filters is consistent with the redshift given 
by Moskvitin et al., GCN Circ. 16489 and DAvanzo et al., GCN Circ. 16493.

The preliminary UVOT position is:
     RA  (J2000) =  16:35:54.42 = 248.97676 (deg.)
     Dec (J2000) = +41:52:36.8  =  41.87690 (deg.)
with an estimated uncertainty of 0.42 arc sec. (radius, 90% confidence).

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

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

white              101          251          147         14.78  0.02
v                  643          663           20         15.29  0.09
b                  569          589           20         15.70  0.06
u                  313          563          246         14.89  0.03
w1                 692          712           19         17.5   0.3
m2                 667          687           19        >17.5
w2                 619          639           19        >18.0

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: GRB140629A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16495
SUBJECT: Konus-Wind observation of GRB 140629A
DATE:    14/06/30 12:59:28 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long GRB 140629A (Swift-BAT trigger #602884: Lien et al., GCN 16477; 
Cummings et al., GCN 16481; T0(BAT)=14:17:30 UT)
was detected by Konus-Wind in the waiting mode.

The light curve shows a double-peaked structure which started
~4 s before the BAT trigger and lasted till ~T0(BAT)+22 s.

The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB140629A/

As observed by Konus-Wind, the burst had a fluence of
(3.4  0.5)x10^-6 erg/cm2 and a 2.944-s peak energy flux,
measured from ~T0(BAT)+13.450 s, of (4.7  0.7)x10^-7 erg/cm2
(both in the 20 - 10000 keV energy range).

Modeling the KW 3-channel time-integrated spectrum
(from T0(BAT)-4.214 s to T0(BAT)+22.282 s) by a power law
with exponential cutoff (CPL) model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -1.42  0.54, and Ep = 86  17 keV.

Modelling the 3-channel spectrum near the peak count rate
(from T0(BAT)-13.450 s to T0(BAT)+16.394 s) by
the CPL model yields alpha = -1.50  0.23, and Ep = 156  52 keV.


Assuming the redshift z=2.275 (Moskvitin et al., GCN 16489;
D'Avanzo et al., GCN 16493)
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 ~4.4x10^52 erg,
the peak luminosity L_iso is ~2.0x10^52 erg/s,
and the rest-frame peak energy of the time-integrated spectrum,
Ep,i, is ~283 keV.

All the quoted errors are estimated at the 1 sigma confidence level.
All the presented results are preliminary.


GRB_name: GRB140629A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16496
SUBJECT: GRB 140629A: Nishi-Harima NIR Observations
DATE:    14/06/30 15:01:06 GMT
FROM:    Akira Arai at Nishi-Harima Astro. Obs/U of Hyogo  <arai@nhao.jp>

S. Honda, Y. Takagi, A. Arai, K. Morihana (Univ. of Hyogo)
report on behalf of Nayuta team and OISTER collaboration:

We observed the field of GRB 140629A (A. Y. Lien et al., GCN 16477)
with Nishiharima Infrared Camera (NIC) attached to the Nayuta 2-m
telescope at the Nishi-Harima Astronomical Observatory.

The observations were conducted on 2014-06-29 at 14:27-15:32 UT.
We detected the near-infrared afterglow in J, H and Ks bands.

Photometric results of our observations are listed below.
We used 2MASS 16355059+4151367, 16355050+4151433, and 16355992+4151103
as reference stars for photometry.

# MID-UT   Tmid-T0 T-EXP  J_mag    H_mag    Ks_mag
-----------------------------------------------------------------------
14:34:02   0.28    600   14.1 +/- 0.2   13.3 +/- 0.1   12.7 +/- 0.2
14:51:34   0.57    600   15.1 +/- 0.2   14.2 +/- 0.1   13.6 +/- 0.2
15:08:16   0.85    600   15.6 +/- 0.2   14.8 +/- 0.1   14.1 +/- 0.2
15:22:49   1.08    480   16.0 +/- 0.2   15.1 +/- 0.1   14.3 +/- 0.2
------------------------------------------------------------------------
Tmid-T0: Elapsed time after the burst (hours)
T-EXP: Total Exposure time (seconds)

-- 
-------------------------------------------------
Akira Arai,
Nishi-Harima Astronomical Observatory,
University of Hyogo
mail : arai@nhao.jp
-------------------------------------------------


GRB_name: GRB140629A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16498
SUBJECT: GRB 140629A: additional P60 observations
DATE:    14/07/01 06:22:11 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) and S. B. Cenko (NASA/GSFC) report:

We acquired additional imaging of the afterglow of GRB 140629A (Lien et 
al., GCN 16477; Yurkov et al. GCN 16478) with the Palomar 60-inch (P60) 
robotic telescope on UT 2014-07-01 between 04:23 and 04:52, acquiring 
9x180s exposures in the r' filter.  We measure a magnitude of:

r = 22.92 +/- 0.14   (t_mid = 1.598 days)

This indicates a relatively rapid decay index of alpha=1.87 since our 
observation the previous night (see also Garnavich and Rose, GCN 16492).


GRB_name: GRB140629A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16499
SUBJECT: GRB 140629A: SAO RAS monitoring
DATE:    14/07/01 13:41:18 GMT
FROM:    Vladimir Sokolov at SAO RAS  <sokolov@sao.ru>

A. Moskvitin (SAO-RAS, N. Arkhyz), R. Burenin (IKI, Moscow),
R. Uklein, V. Sokolov, T. Sokolova (SAO-RAS, N. Arkhyz),
on behalf of a larger collaboration, report:

We performed the photometrical monitoring of the GRB 140629A OT (Lien
et al., GCNC 16477) with two optical telescopes of SAO RAS: the 6-m
BTA (V band) and the 1-m Zeiss-1000 (BVRcIc bands) on the night of
June, 29/30. Observations started 4.1 hours after the Swift trigger.
The optical transient (Lien et al., GCNC 16477; Yurkov et al.,
GCNC 16478; Bikmaev et al., GCNC 16482; Masi, GCNC 16483; Maehara,
GCNC 16484; Malesani et al., GCNC 16485; Sonbas et al., GCNC 16486;
and other teams) is clearly detected in every single image.

On the basis of the same star from USNO-B1 as Bikmaev et al. (GCNC 16482)
with the coordinates R.A., = 16:35:59.9, Decl.= +41:51:10, J2000 and
magnitude R1_mag = 16.49 we made preliminary photometric estimations
of the OT Rc images. The results are as follows:

#  Start,UT  exp,s   R_mag +/- err
====================================
 1  19:00:41  180.00  18.02 +/- 0.05
 2  19:05:38  180.00  18.20 +/- 0.05
 3  19:11:11  180.00  18.45 +/- 0.07
 4  19:28:39  300.00  18.25 +/- 0.04
 5  20:03:55  300.00  18.53 +/- 0.04
 6  20:26:36  300.00  18.58 +/- 0.04
 7  20:53:25  300.00  18.87 +/- 0.04
 8  22:10:17  300.00  19.00 +/- 0.05
 9  22:33:32  300.00  19.11 +/- 0.05
10  22:57:16  300.00  19.00 +/- 0.05
11  23:25:27  300.00  19.31 +/- 0.09
12  23:49:07  300.00  19.38 +/- 0.11

Further analysis and observations go on.


GRB_name: GRB140629A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16500
SUBJECT: GRB 140629A: MASTER-Net preliminary light curve  
DATE:    14/07/01 15:21:21 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy   (Lomonosov Moscow University)
V. Krushinski   (Ural Federal State University)
M. Pruzhinskaya (Lomonosov Moscow University)


P.Balanutsa,  A.Kuznetsov, V.V.Chazov, N.Tyurina, D.Denisenko
Lomonosov Moscow State University,
Sternberg Astronomical Institute, Moscow State University


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


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

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

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

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)

Three MASTER system telescopes located in Blagoveshchensk, Tunka and
Kislovodsk have observed GRB140629A (Lien et al., GCN 16477) from 33
seconds till ~9 hours after the trigger. MASTER II robotic telescope
(MASTER-Net: http://observ.pereplet.ru) located in Blagoveschensk was
pointed to GRB140629A 15 sec after notice time and 33 sec after
trigger time at 2014-06-29 14:18:03.188 UT and found OT in SWIFT
error-box. MASTER II Tunka was pointed to GRB140629A 78 sec after
trigger time at 2014-06-29 14:18:48.102 UT on the evening twilight sky
(Sun ~5 d. below horizon) with dark sky observations starting ~ 50 min
after trigger time. MASTER II Kislovodsk was pointed to GRB140629A
~3.2 hours after the trigger directly after the Sun set and weather
conditions became suitable.

The preliminary light curve is available here:
http://master.sai.msu.ru/static/GRB/GRB140629A_slope2.png

The optical transient (Lien et al., GCN 16477; Yurkov et al., GCN
16478; Moskvitin et al., GCN 16489; Bikmaev et al., GCN 16482; Masi,
GCN 16483; Maehara, GCN 16484; Malesani et al., GCN 16485; Sonbas et
al., GCN 16486 etc.) has a maximum at ~ 150 sec. after the burst,
reaching 13.8 mag, after which it shows a power law decay. The power
law index (alpha) from 200 to 10000 seconds after the trigger is 1.12
+- 0.1  (F ~ t^-alpha).

There was no polarization more than 3% discovered on afterglow 
stage.


GRB_name: GRB140629A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16501
SUBJECT: GRB 140629A: MITSuME Akeno Optical observation
DATE:    14/07/02 06:24:29 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

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

We observed the field of GRB 140629A (A. Y. Lien et al., GCN Circular #16477) 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 2014-06-29 14:23:32 UT (6 min after the burst).
We detected the previously reported optical afterglow of GRB140629A 
(V.Yurkov et al., GCN Circular #16478) in the g', Rc and Ic band.

The measured magnitudes are listed below.

T0+[sec]    MID-UT   T-EXP[sec]         g'                       Rc                   Ic
----------------------------------------------------------------------------------------------------
362           14:24:02     60.0          15.06+/-0.04  14.25+/-0.03 13.83+/-0.03
11482      17:43:45     600.0        18.77+/-0.23  18.06+/-0.16 17.67+/-0.21
----------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used GSC2.3 catalog for flux calibration.


GRB_name: GRB140619C
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16502
SUBJECT: GRB 140619C: Suzaku WAM observation of the prompt emission
DATE:    14/07/02 10:55:03 GMT
FROM:    Kazutaka Yamaoka at Nagoya U  <yamaoka@stelab.nagoya-u.ac.jp>

W. Iwakiri (RIKEN), M. Tashiro, Y. Terada, T. Yasuda, S. Koyama, S. Takeda,
T. Nagayoshi, J. Enomoto, S. Nakaya, T. Fujinuma, S. Matsuoka (Saitama U.),
M. Yamauchi, N. Ohmori, R. Kinoshita (Univ. of Miyazaki),
M. Ohno, T. Kawano, S. Furui, Y. Fukazawa (Hiroshima U.),
K. Yamaoka (Nagoya U.), S. Sugita (Ehime U.), Y. Hanabata (ICRR), 
Y. E. Nakagawa, M. Kokubun, T. Takahashi (ISAS/JAXA), Y. Urata (NCU), 
K. Nakazawa, K. Makishima (Univ. of Tokyo), 
on behalf of the Suzaku WAM team, report:

The bright GRB 140619C (localized by IPN: Hurley et al., GCN 16427;
Konus-Wind detection: Golenetskii et al., GCN 16429) triggered the Suzaku
Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV -
5 MeV at UT 22:46:01.623 (=T0).

The observed light curve shows a multi-peaked structure, consisting of
two separated episodes: the first one lasting from T0 to T0+6 s, and the
second brighter one lasting from T0+70 s to T0+94 s,  with a total 
duration (T90) of about 87 seconds. The fluence in 100 - 1000 keV was 
4.34 (+0.21, -0.23)x10^-5 erg/cm^2. The 1-s peak flux measured from 
T0+75 s was 8.32 (+1.12, -1.17) photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0 to
T0+92 s is well fitted by a single power-law with a photon index of 2.50
(+0.15, -0.14) (chi^2/d.o.f = 15.4/14).

All the quoted errors are at statistical 90% confidence level.
There might be some calibration uncertainties in spectral parameters
since the GRB photons came through the X-ray micro-calorimeter (XRS) dewar.

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


GRB_name: GRB140703A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16503
SUBJECT: GRB 140703A: Swift detection of a burst
DATE:    14/07/03 00:52:07 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@swift.psu.edu>

D. Kocevski (NASA/GSFC/ORAU), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (NASA/UMBC), J. A. Kennea (PSU),
N. P. M. Kuin (UCL-MSSL), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), J. L. Racusin (NASA/GSFC),
M. H. Siegel (PSU) and T. N. Ukwatta (MSU) report on behalf of the
Swift Team:

At 00:37:17 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140703A (trigger=603243).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 12.990, +45.095 which is 
   RA(J2000) = 00h 51m 58s
   Dec(J2000) = +45d 05' 41"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a two-peak
structure with a duration of about 90 sec.  The peak count rate
was ~1781 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 00:39:09.8 UT, 112.8 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 12.9958, 45.1015 which is equivalent to:
   RA(J2000)  = +00h 51m 58.99s
   Dec(J2000) = +45d 06' 05.4"
with an uncertainty of 4.7 arcseconds (radius, 90% containment). This
location is 27 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 1.12e-08 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 116 seconds with the White filter
starting 123 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 0.10. 

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: GRB140703A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16504
SUBJECT: GRB 140703A: BOOTES-2 and OSN optical observations
DATE:    14/07/03 03:30:45 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

R. Cunniffe, A. Gonzalez-Rodriguez, V. Casanova, M. Jelinek, S. Jeong, O.
Lara-Gil, S. R. Oates, R. Sanchez-Ramirez, J. C. Tello (IAA-CSIC Granada),
P. Kubanek (IP-ASCR, Prague), J. Gorosabel (IAA-CSIC, UPV-EHU) and A. J.
Castro-Tirado (IAA-CSIC, ISA-UMA), report:

Following the detection of GRB 140703A by Swift (Kocevski et al., GCNC
16503), the 0.6m TELMA robotic telescope at the BOOTES-2 astronomical
station Malaga (Spain), responded to the GRB location starting at 00:38:02
UT (i.e. 45s postburst, in the clear filter, 5s integrations). In the
longer exposures (i'-band, 60s) starting at 00:47:30 (i.e. 10 min
postburst), a faint optical source is barely detected in the images, at
the outskirts of the XRT position, which is confirmed by the 1.5m OSN
images at Sierra Nevada Observatory starting at 00:54 UT (I-band), with a
magnitude of about 20, which does not seem to be present in the DSS-2. The
preliminary position (+/- 1") is:

RA(J2000) = 00 51 59.05, Dec (J2000) = +45 06 06.

The source is detected in all optical filters. Additional observations
(imaging and spectroscopy) are ongoing.

[GCN OPS NOTE(03jul14): Per author's request, the starting time was changed
from 00:30:02 to 00:38:02 (ie 8 min later), and the characterset represenation
for the i'-band specification was changed to plain-text.]


GRB_name: GRB140703A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16505
SUBJECT: GRB140703A: 10.4m GTC redshift
DATE:    14/07/03 07:04:51 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

A. J. Castro-Tirado (IAA-CSIC), R. Cunniffe (IAA-CSIC), R. Sanchez-Ramirez (IAA-CSIC), J. Gorosabel (IAA-CSIC/UPV-EHU), M. Jelinek (IAA-CSIC), S.R. Oates (IAA-CSIC), S. Jeong (IAA-CSIC), J. R. Tello (IAA-CSIC), S. Pandey (ARIES), G. Gomez-Velarde (GTC, IAC), A. Perez (GTC), report on behalf of a larget collaboration:

"We obtained 2x450s optical spectra  of GRB 140703A (Kocevski et al. GCN16503) optical afterglow (Cunniffe et al. GCN16504) with the 10.4m GTC(+OSIRIS) with a wavelength coverage of 4000--9500 AA based on R1000R and R1000B grisms. The combined spectrum shows a deep Lyman-alpha absorption and many metallic absorption lines (AlI, CII, CIV,AlIII..). Using archival calibration lamps  we infer a common redshift of z=3.14."

[GCN OPS NOTE(03jul14):  Per author's request, G.G-V & A.P. were added to the author list.]


GRB_name: GRB140703A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16506
SUBJECT: GRB 140703A: Enhanced Swift-XRT position
DATE:    14/07/03 09:49:00 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 2188 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 140703A, 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 = 12.99574, +45.10185 which is equivalent
to:

RA (J2000): 00h 51m 58.98s
Dec (J2000): +45d 06' 06.7"

with an uncertainty of 1.7 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB140703A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16507
SUBJECT: GRB 140703A: MASTER optical observations 
DATE:    14/07/03 10:11:14 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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

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

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

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



MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Kislovodsk was pointed to the  GRB 140703A (Kocevski et. al., 
GCN 16503) 2 sec after notice time and 45 sec after trigger time at 
2014-07-03 00:38:03 UT on morning sky in two polarizations.
We have 10 good  frames with an increasing exposition from 10 to 70 
seconds that of that as there overlighting came. On our first (10s 
exposure)  set we haven't see optical transient (Cunniffe et. al., GCN 
16504; Castro-Tirado et. al., GCN 16505) on our single and coadd image.


Pro.type   T-T_trig   T_start  Exp.time   Limit   Filt.   Tube.
             (mean)     (UT)
  Alert        51     00:38:03     10      15.9     P-       EAST
  Alert        51     00:38:03     10      15.7     P|       WEST
  Coadd        77     00:38:03     40      16.8     P-       EAST
  Coadd        77     00:38:03     40      16.5     P|       WEST
  Coadd       169     00:38:03     180     16.7     P|       WEST
  Coadd       244     00:38:03     310     17.5     P-       EAST
  Coadd       244     00:38:03     570     18.0    White   WEST+EAST
  Alert        72     00:38:24     10      15.9     P-       EAST
  Alert        72     00:38:24     10      15.8     P|       WEST
  Alert        98     00:38:45     20      16.0     P|       WEST
  Alert        98     00:38:45     20      16.2     P-       EAST
  Alert       129     00:39:16     20      15.7     P|       WEST
  Alert       129     00:39:16     20      16.2     P-       EAST
  Coadd       174     00:39:16     90      17.1     P-       EAST
  Coadd       174     00:39:16     90      16.4     P|       WEST
  Alert       164     00:39:47     30      16.4     P-       EAST
  Alert       164     00:39:47     30      15.7     P|       WEST
  Alert       210     00:40:27     40      15.7     P|       WEST
  Alert       210     00:40:27     40      16.5     P-       EAST
  Alert       266     00:41:18     50      15.5     P|       WEST
  Alert       266     00:41:18     50      16.4     P-       EAST
  Coadd       342     00:41:18     80      16.5     P-       EAST

The message may be cited.

[GCN OPS NOTE(03jul14): As per GCN Circ 16508, the Subject-line
was changed from 140629A to 140703A.]


GRB_name: GRB140703A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16508
SUBJECT: Correction to GCN 16507: GRB 140703A! 
DATE:    14/07/03 12:06:21 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

The correct sublject of the GCN 16507 is
"GRB 140703A: MASTER optical observations"

I am sorry,
Vladimir Lipunov

The message may be cited.


GRB_name: GRB140703A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16509
SUBJECT: GRB 140703A: Swift-BAT refined analysis
DATE:    14/07/03 14:48:12 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), D. Kocevski (NASA/GSFC/ORAU),
A. Y. Lien (NASA/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 140703A (trigger #603243)
(Kocevski, et al., GCN Circ. 16503).  The BAT ground-calculated position is
RA, Dec = 13.010, 45.102 deg, which is 
   RA(J2000)  =  00h 52m 02.4s 
   Dec(J2000) = +45d 06' 07.5" 
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 14%.
 
The mask-weighted light curve shows several peaks starting at ~T-70 sec,
peakings at ~T-50, ~T+2 & ~T+70 sec, and ending at ~T+140 sec.
T90 (15-350 keV) is 67.1 +- 67.9 sec (estimated error including systematics).
 
The time-averaged spectrum from T-2.5 to T+134.8 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.74 +- 0.13.  The fluence in the 15-150 keV band is 3.9 +- 0.3 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+0.36 sec in the 15-150 keV band
is 2.8 +- 0.6 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/603243/BA/


GRB_name: GRB140703A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16510
SUBJECT: GRB 140703A: Swift-XRT refined Analysis
DATE:    14/07/03 14:52:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 7.5 ks of XRT data for GRB 140703A (Kocevski  et al.
GCN Circ. 16503),  from 104 s to 39.2 ks after the  BAT trigger. The
data comprise 126 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 Goad
et al. (GCN Circ. 16506).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=0.1 (+1.5, -1.6). At T+120 s  the decay
steepens to an alpha of 6.8 (+0.4, -0.3). The light curve breaks again
at T+158 s to a decay with alpha=5.1 (+/-0.4), and  again at T+319 s s
to alpha=0.1 (+0.6, -0.4),  before a final break at T+7413 s s after
which the decay index is 1.56 (+0.14, -0.13).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.84 (+0.08, -0.07). The
best-fitting absorption column is  5.2 (+/-0.6) x 10^22 cm^-2, at a
redshift of 3.14, in addition to the Galactic value of 1.3 x 10^21
cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index
of 1.82 (+/-0.09) and a best-fitting absorption column of 5.4 (+8.0,
-5.4) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV
flux conversion factor deduced from this spectrum  is 3.8 x 10^-11 (4.6
x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 1.3 x 10^21 cm^-2
Intrinsic column:    5.4 (+8.0, -5.4) x 10^21 cm^-2 at z=3.14
Photon index:      1.82 (+/-0.09)

If the light curve continues to decay with a power-law decay index of
1.56, the count rate at T+24 hours will be 0.022 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 8.4 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/00603243.

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


GRB_name: GRB140703A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16511
SUBJECT: GRB 140703A: Monte Agliale Observatory optical observations
DATE:    14/07/03 15:29:33 GMT
FROM:    Fabrizio Ciabattari at Monte Agliale Obs  <fabciaba@alice.it>

F. Ciabattari, S. Donati, E. Mazzoni, G. Petroni and M. Rossi (Monte Agliale Observatory, Borgo a 
Mozzano, Italy) report:

We observed the field of GRB 140703A (Kocevski et al., GCNC 16503) with the automatic 0.5m Newtonian
telescope + FLI ProLine PL4710 camera at Monte Agliale Observatory (Borgo a Mozzano, Italy, MPC code 
159).
The observations started at 2014-07-03 01:57:43 UT (~80 minutes after the trigger) and we co-added
20 unfiltered CCD exposures of 20 seconds each.
We detect a new source of mag. R = 19.8 +/-0.3 (USNO-B1 catalogue) at the following position:
R.A.(J2000) = 00h 51m 59.01s
Dec.(J2000) = +45d 06' 06.1"
FITS files are available on request from fabciaba@alice.it.
The message may be cited.


GRB_name: GRB140703A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16512
SUBJECT: GRB 140703A: Fermi GBM detection
DATE:    14/07/03 16:21:16 GMT
FROM:    Peter Jenke at MSFC  <peter.a.jenke@nasa.gov>

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

"At 00:37:07.19 UT on July 3 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140603A (trigger 426040630/140703026),
which was also detected by 
Swift (D. Kocevski et al. 2014, GCN 16503).  
The GBM on-ground location, using the Fermi GBM trigger
data, is consistent with the Swift/XRT location
and the TELMA robotic telescope 
location (R. Cunniffe et al. 2014 GCN16504).  

The angle of the burst direction to the Fermi LAT boresight
 is 16 degrees.

The GBM light curve consists of one main FRED-like peak near T0 and a
late smaller peak at ~T0+70s with a duration (T90) of about
84s (50-300 keV).
The time-averaged spectrum from T0-4s to T0+31s 
is well fit by a power law function with an exponential 
high-energy cutoff.  The power law index is -1.10 +/- 0.06
and the cutoff energy, parameterized as Epeak, is 177 +/- 14 keV. 

The event fluence (10-1000 keV) in this time interval is
(7.4 +/- 0.4)E-07 ergs/cm^2. The 1.0-sec peak photon flux measured
starting from T0+9.7s in the 10-1000 keV band
is 4.1 +/- 0.2 ph/s/cm^2.

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


GRB_name: GRB140703A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16513
SUBJECT: GRB 140703A: RATIR Optical and NIR Observations
DATE:    14/07/03 16:46:08 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB),
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara
(ORAU/GSFC), 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), and
Harvey Moseley (GSFC) report:

We observed the field of GRB 140703A (Kocevski, et al., GCN 16503) 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 2014/07 3.43 to 2014/07 3.47 UTC (9.74 to
10.68 hours after the BAT trigger), obtaining a total of 0.71 hours
exposure in the r and i bands and 0.29 hours exposure in the Z, Y, J, and H
bands.

For a source within the Swift-XRT error circle, in comparison with the SDSS
DR9 and 2MASS, we obtain the following detections:

  r     20.32 +/- 0.03
  i     19.72 +/- 0.03
  Z     18.53 +/- 0.05
  Y     18.31 +/- 0.05
  J     19.60 +/- 0.17
  H     18.98 +/- 0.09

These magnitudes 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: GRB140703A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16514
SUBJECT: GRB 140703A: P60 observations of a red, slowly-fading afterglow
DATE:    14/07/03 16:51:02 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) and S. B. Cenko (NASA/GSFC) report:

We observed the afterglow of GRB 140703A (Kocevski et al., GCN 16503) 
with the Palomar 60-inch (P60) robotic telescope.  We acquired 3x180s in 
each of the r, i, and z filters between 08:40:37 and 09:11:02 on 
2014-07-03 UT.  We measure the following magnitudes:

    r = 20.03 +/- 0.02   t_mid = 0.3462 days
    i = 19.46 +/- 0.02   t_mid = 0.3380 days
    z = 18.99 +/- 0.05   t_mid = 0.3533 days

This indicates very little fading since the observations of Cunniffe et 
al. (GCN 16504) and Ciabattari et al. (GCN 16511).  However, the 
spectroscopy of Castro-Tirado et al. (GCN 16505) confirms this source is 
the GRB afterglow.

We note that the afterglow color is fairly red (beta~2.2 after 
correction for foreground extinction), possibly indicating significant 
dust obscuration in the host frame.


GRB_name: GRB140703A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16515
SUBJECT: GRB 140703A: CARMA 3mm detection
DATE:    14/07/03 19:03:28 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

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

We observed the position of GRB 140703A (Kocevski et al., GCN 16503) 
with the Combined Array for Research in Millimeter Astronomy starting at 
2013-07-03 16:39:55 UT (0.668 days post-GRB) at a mean frequency of ~93 
GHz; the observation is still ongoing.

We detect a strong source in the existing data set at the location of 
the X-ray and optical afterglows (Goad et al., GCN 16506; Castro-Tirado 
et al., GCN 16504) with a flux of approximately 2 mJy.

We thank Nikolaus Volgenau, observers K. Jameson and E. Grand, and the 
CARMA staff for executing the observation.


GRB_name: GRB140703A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16516
SUBJECT: GRB 140703A: VLA K-band detection
DATE:    14/07/04 02:51:36 GMT
FROM:    Alessandra Corsi at GWU  <corsi@email.gwu.edu>

A. Corsi (GWU / TTU) reports on behalf of a larger collaboration:
 
We imaged the position of GRB 140703A (Kocevski et al., GCN 16503) with the 
Karl G. Jansky Very Large Array (VLA) in K-band, starting at about 8.5 hours after 
the burst. A provisional reduction shows a source consistent with the location of the 
GRB X-ray and optical afterglows (Goad et al., GCN 16506; Cunniffe et al., GCN 16504). 
At this time, we estimate a preliminary flux of about 280 uJy at 19 GHz.
 
Further observations are planned.


GRB_name: GRB140629A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16517
SUBJECT: GRB 140629A, Optical observations
DATE:    14/07/04 04:08:29 GMT
FROM:    Shashi Bhushan Pandey at ROTSE  <shaship@umich.edu>

S. B. Pandey and Brajesh Kumar (ARIES Nainital India,on behalf of larger
Indian GRB collaboration)

We observed the Swift GRB 140629A field (Lien et al., GCNC 16477) using
1.04m ST telescope at ARIES Nainital. Observations were started at 17:40:59
UT on 2014-06-29 (approximately 3.4 h after the burst). Several frames
with an exposure time of 300 s each in R_c and I_c bands were obtained in

good sky conditions.

The optical counterpart of GRB 140629A (Lien et al., GCNC 16477;

Yurkov et al., GCNC 16478; Bikmaev et al., GCNC 16482; Masi, GCNC

16483; ) is clearly detected  in each individual frames.


Preliminary photometry is following:
-----------------------------------------------
   UT          Exp_time     Filter     Mag

------------------------------------------------

17:40:59       300 s         R_c     18.01  +- 0.05

17:56:21       300 s         I_c       17.92 +- 0.06

------------------------------------------------


The photometry was performed in comparison to nearby USNO stars.
This massage may be cited


GRB_name: GRB140629A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16518
SUBJECT: GRB 140629A: SAO RAS Rc band photometry
DATE:    14/07/04 05:57:05 GMT
FROM:    Vladimir Sokolov at SAO RAS  <sokolov@sao.ru>

A.S. Moskvitin, V.N. Komarova, T.N. Sokolova, V.V. Sokolov (SAO RAS,
N. Arkhyz), on behalf of a larger collaboration, report:

We observed the GRB 140629A field (Lien et al., GCNC 16477)
with the 1-m SAO RAS telescope Zeiss-1000 on June, 30.
Observations started at 21:21:36 and ended at 23:48:49 UT.
22 x 300 sec. images in the Rc filter were obtained under good weather
conditions.

Unlike the previous night, the OT is not visible in single images,
but is clearly detectable in the stacked image. Based on the same
USNO-B1 star (Moskvitin et al., GCNC 16499; Bikmaev et al., GCNC 16482)
with R1_mag = 16.49, we measured the OT magnitude as R = 22.1 +/- 0.2
on the phase 1.35 days after the trigger.


GRB_name: GRB140621A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16519
SUBJECT: GRB 140621A: Suzaku WAM observation of the prompt emission
DATE:    14/07/04 08:23:11 GMT
FROM:    Tetsuya Yasuda at Saitama U  <yasuda@heal.phy.saitama-u.ac.jp>

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


The long-duration GRB 140621A (IPN localization: S. Golenetskii et al., 
GCN 16444; Konus-Wind observation: S. Golenetskii et al., GCN 16445; 
Fermi-GBM detection: G. Younes et al., GCN 16447; Swift-XRT observation: 
V. D'Elia et al., GCN 16449) triggered theSuzaku Wide-band All-sky Monitor 
(WAM) which covers an energy range of 50 keV - 5 MeV at 19:50:10.596 UT (=T0).

The observed light curve shows a multi-peaked structure lasting from T0 to T0+7 s 
with a duration(T90) of about 6.135 seconds. The fluence in 100 - 1000 keV 
was 4.96 (+0.11, -0.33) x10^-6 erg/cm^2. The 1-s peak flux measured from T0 was 
3.74 (+0.15, -0.30) photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0 to T0+7 s 
is well fitted by a power-law with exponential cutoff model:
dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with 
alpha 0.87 (+0.30, -0.25), 
and Epeak 689 (+127, -93) keV (chi^2/d.o.f. = 28.3/29).

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

The light curves for this burst will be available at:

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


GRB_name: GRB140705A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16520
SUBJECT: GRB 140705A: Swift detection of a short burst
DATE:    14/07/05 09:47:43 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

M. Stamatikos (OSU/NASA/GSFC), D. Malesani (DARK/NBI),
K. L. Page (U Leicester) and T. Sakamoto (AGU) report on behalf of the
Swift Team:

At 09:32:48 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140705A (trigger=603488).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 293.725, +21.899 which is 
   RA(J2000) = 19h 34m 54s
   Dec(J2000) = +21d 53' 57"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a short spike 
with a duration of about 0.2 sec.  The peak count rate
was ~4500 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 09:33:49.6 UT, 61.0 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 293.7318, 21.8979 which
is equivalent to:
   RA(J2000)  = 19h 34m 55.64s
   Dec(J2000) = +21d 53' 52.4"
with an uncertainty of 2.9 arcseconds (radius, 90% containment). This
location is 23 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. 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 64 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 large, but uncertain extinction expected. 

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: GRB140705A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16521
SUBJECT: GRB 140705A: Enhanced Swift-XRT position
DATE:    14/07/05 13:23:22 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 886 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 140705A, 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 = 293.73199, +21.89673 which is equivalent
to:

RA (J2000): 19h 34m 55.68s
Dec (J2000): +21d 53' 48.2"

with an uncertainty of 2.3 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB140705A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16522
SUBJECT: GRB 140705A: Swift-BAT refined analysis of a possible newly discovered SGR 1935+2154
DATE:    14/07/05 14:24:49 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

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

Using the data set from T-61 to T+242 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140705A (trigger #603488)
(Stamatikos, et al., GCN Circ. 16520).  The BAT ground-calculated position is
RA, Dec = 293.751, 21.912 deg which is 
  RA(J2000)  =  19h 35m 00.3s 
  Dec(J2000) = +21d 54' 41.7" 
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 94%.

The 2 ms mask-weighted light curve shows at least two spikes peaking at 
T+0 sec and T+0.05 sec.  T90 (15-350 keV) is 0.08 +- 0.01 sec (estimated 
error including systematics).

The time-averaged spectrum from T-0.02 to T+0.06 sec fit by a simple
power-law model shows the power law index of 2.74 +- 0.15 (chi squared 75.65 for 57 d.o.f.).
The fluence in the 15-150 keV band is 3.8 +- 0.4 x 10^-8 erg/cm2.
The 1-sec peak photon flux measured from T-0.48 sec in the 15-150 keV band
is 0.9 +- 0.2 ph/cm2/sec.

A single blackbody fit to the time-averaged spectrum shows the blackbody
temperature of 8.2 +- 1.0 keV (chi squared 74.30 for 57 d.o.f.).
A thermal bremsstrahlung model fit shows the temperature of 35.7 +- 6.1 keV
(chi squared 56.05 for 57 d.o.f.).  A double blackbody fit shows the lower temperature
of 4.8 +1.3 keV and the higher temperature of 13.7 (error not unconstrained) keV
(chi squared 54.60 for 55 d.o.f.).  All the quoted errors are at the 90% confidence level. 

Because 1) the burst is located at the galactic plane (l, b) = (57.25 deg, 0.83 deg.) and 
2) the BAT burst spectrum is rather soft, we believe this could be a short event from 
a newly discovered SGR 1935+2154.  

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/603488/BA/


GRB_name: GRB140705A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16523
SUBJECT: GRB 140705A: Swift/UVOT Upper Limits
DATE:    14/07/05 21:41:14 GMT
FROM:    Margaret Chester at PSU  <chester@swift.psu.edu>

M. M. Chester (PSU) and M. Stamatikos (OSU/NASA/GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140705A
65 s after the BAT trigger (Stamatikos et al., GCN Circ. 16520).
No optical afterglow consistent with the XRT position (Osborne et al. 
GCN Circ. 16521) 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            65          215          147         >20.6
u_FC               277          527          246         >20.2
white               65         6023          498         >21.5
v                  607         6434          432         >19.8
b                  532         7088          268         >21.1
u                  277         7048          659         >20.6
w1                 656         6843          432         >20.6
m2                5004         6638          393         >20.9
w2                 582         6229          432         >21.8

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 4.88 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB140705A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16524
SUBJECT: GRB 140705A: MITSuME Okayama upper limits
DATE:    14/07/05 23:21:57 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 140705A (Stamatikos et al., GCNC 16520)
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 2014-07-05 14:57:48 UT (~5.4 h after the burst).
We did not find any new point source within the enhanced XRT circle
(Osborne et al., GCNC 16521) 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
-----------------------------------------------------
0.30500    16:52:00    6540.0   >19.4  >19.1  >18.2
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]

[GCN OPS NOTE(06jul14): The Subject-line was changed to the correct GRB name.]


GRB_name: GRB140705A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16525
SUBJECT: GRB 140705A: Swift-XRT refined Analysis
DATE:    14/07/05 23:47:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 10 ks of XRT data for GRB 140705A (Stamatikos et al.
GCN Circ. 16520),  from 68 s to 35.0 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Osborne et al. (GCN Circ. 16521).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.15 (+0.09, -0.10).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 3.7 (+0.6, -0.5). The
best-fitting absorption column is  4.9 (+1.1, -1.0) x 10^22 cm^-2, in
excess of the Galactic value of 1.3 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 4.7 x 10^-11 (1.7 x 10^-09) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.9 (+1.1, -1.0) x 10^22 cm^-2
Galactic foreground: 1.3 x 10^22 cm^-2
Excess significance: 6.0 sigma
Photon index:      3.7 (+0.6, -0.5)

If the light curve continues to decay with a power-law decay index of
0.15, the count rate at T+24 hours will be 0.022 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.0 x
10^-12 (3.7 x 10^-11) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00603488.

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


GRB_name: GRB140705A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16526
SUBJECT: GRB 140705A: MITSuME Ishigakijima upper limits
DATE:    14/07/06 01:19:24 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 140705A (Stamatikos et al., GCNC 16520)
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 2014-07-05 13:08:26 UT (~3.6 h after the burst).
We did not find any new point source within the enhanced XRT circle
(Osborne et al., GCNC 16521) 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
-----------------------------------------------------
0.20844    14:32:57    6960.0   >22.1  >21.5  >20.5
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB140705A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16527
SUBJECT: GRB 140705A: KAIT Optical Upper Limit
DATE:    14/07/06 02:51:21 GMT
FROM:    Weikang Zheng at UC Berkeley  <zwk@astro.berkeley.edu>

WeiKang Zheng, Alexei V. Filippenko, Adam Morgan (UC Berkeley), and
S. B. Cenko (NASA/Goddard Space Flight Center) report on behalf of the
KAIT GRB team:

The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, responded to Swift GRB 140705A (Stamatikos et al.,
GCN 16520) starting at 09:34:02 UT, 74 s after the burst.
Observations were performed with an automatic sequence in the
clear (roughly R), V, and I filters, and the exposure time was
20 s per image. We do not detect any new source within the enhanced 
XRT error circle (Osborne et al. GCN 16521) in our individual images, 
nor in the coadded images of the first 5 or 10 clear band images.
The typical limiting magnitude of our single clear image is about 
19.2 calibrated to USNO B1.0.


GRB_name: GRB140705A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16528
SUBJECT: GRB 140705A / SGR 1935+2154: Optical observations from 10.4m GTC
DATE:    14/07/06 03:47:32 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), J. Gorosabel (IAA-CSIC/UPV-EHU), P. Rodriguez-Gil (IAC) and S. Campana (INAF-OAB) report on behalf of a larger collaboration:

We have observed the field of GRB 140705A / SGR 1935+2154 (Stamatikos et al. GCN 16520, Lien et al. GCN 16522) using OSIRIS on the 10.4m GTC telescope. Observations started at 00:57 UT of the 6 July 2014 (15.42 hrs after the burst onset) and consisted of 10x120s in i-band and 20x60s in z-band. Within the enhanced XRT error box (Osborne et al. GCN 16521, updated to R.A.: 293.73169, Dec.: +21.89668, +/-1.5") we detect two sources. The first of them, which we name S1, has an approximate magnitude of i(AB)~24 whereas S2 has i(AB)~25.5. Photometry is based on USNO-B1.0, and is still very preliminary. The coordinates of these sources are (J2000+/-0.5"): 

S1: 19:34:55.56, +21:53:48.2
S2: 19:34:55.68, +21:53:47.9

We have used UKIDSS nIR images for comparison, as there were not deep enough images available in the optical (there is no SDSS coverage in this field). S1 is clearly detected in J, H and K-band images of UKIDSS. S2, could be marginally detected in J-band. At this point we cannot claim variability of any of these sources and thus their relation with GRB 140705A / SGR 1935+2154 cannot be stated.

We acknowledge excellent support from the GTC staff, in particular Riccardo Scarpa.


GRB_name: GRB140705A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16529
SUBJECT: GRB 140705A / SGR 1935+2154: FTN observations
DATE:    14/07/06 12:11:44 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi, S. Dichiara (U. Ferrara) on behalf of a large
collaboration report:

The 2-m Faulkes Telescope North began observing Swift GRB 140705A/
SGR 1935+2154 (Stamatikos et al. GCN Circ 16520; Lien et al. GCN Circ
16522) on July 05 at 10:10:46 UT, i.e. ~38 min after the BAT trigger,
with the r' and i' filters.

Within the enhanced XRT error circle (Osborne et al. GCN Circ. 16521)
we found nothing down to the following limit:

Mid time from  Total Exp    Filter    Magnitude
trigger (min)   (s)
--------------------------------------------------------------
52.0            120x4       i'        > 21
--------------------------------------------------------------

Magnitudes are calibrated against nearby USNO-B1 stars.


GRB_name: GRB140706A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16531
SUBJECT: GRB 140706A: Swift detection of a burst with an optical counterpart
DATE:    14/07/06 19:42:34 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC), S. D. Barthelmy (GSFC),
S. B. Cenko (GSFC), J. R. Cummings (NASA/UMBC), J. A. Kennea (PSU),
K. L. Page (U Leicester) and D. M. Palmer (LANL) report on behalf of
the Swift Team:

At 19:33:33 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140706A (trigger=603587).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 49.306, -38.059 which is 
   RA(J2000) = 03h 17m 13s
   Dec(J2000) = -38d 03' 33"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows two main peaks
with a total duration of about 55 sec.  The peak count rate
was ~1700 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 19:34:46.0 UT, 72.8 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 49.29517, -38.05083 which
is equivalent to:
   RA(J2000)  = 03h 17m 10.84s
   Dec(J2000) = -38d 03' 03.0"
with an uncertainty of 4.1 arcseconds (radius, 90% containment). This
location is 42 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. No
spectrum from the promptly downlinked event data is yet available to
determine the column density. 

The initial flux in the 2.5 s image was 5.09e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 82 seconds after the BAT trigger. There is a candidate afterglow in
the list of sources generated on-board at
  RA(J2000)  = 03:17:10.40 =  49.29332
  DEC(J2000) = -38:03:07.4  = -38.05205
with a 90%-confidence error radius of about 1.10 arc sec. This position is 4.5
arc sec. from the center of the XRT error circle. The estimated magnitude is
19.05. No correction has been made for the expected extinction corresponding to
E(B-V) of 0.02. 

Burst Advocate for this burst is F. E. Marshall (marshall 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: GRB140706A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16532
SUBJECT: GRB 140706A: Enhanced Swift-XRT position
DATE:    14/07/06 23:55:10 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 1464 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 140706A, 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 = 49.29426, -38.05194 which is equivalent
to:

RA (J2000): 03h 17m 10.62s
Dec (J2000): -38d 03' 07.0"

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: GRB140705A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16533
SUBJECT: GRB 140705A / SGR 1935+2154: Probable association with supernova remnant G57.2+0.8
DATE:    14/07/07 08:19:25 GMT
FROM:    Bryan Gaensler at U of Sydney  <bmg@physics.usyd.edu.au>

B. M. Gaensler (U. Sydney / CAASTRO) reports:

I note that the newly identified magnetar SGR 1935+2154 (GCN 16522; ATel 6294) is coincident with the Galactic supernova remnant (SNR) G57.2+0.8 (Sun et al., 2011, A&A, 536, A83, and references therein).

Specifically, the location of the SGR as determined by Swift XRT (ATel 6294) sits very close to the geometric centre of the SNR. A 1.4 GHz radio image of the SNR taken from the VLA Galactic Plane Survey (Stil et al., 2006, AJ, 132, 1158), and showing the position of the SGR, is available at:

http://www.physics.usyd.edu.au/~bmg/fig_sgr1935+2154_snr.png

This is a relatively uncrowded region of the Galactic plane, implying a high probability of a physical association between SGR 1935+2154 and SNR G57.2+0.8. The SGR's location at the centre of a SNR is similar to that previously found for other SGRs such as 1E 2259+586 in CTB 109, 1E 1841-045 in Kes 73 and 1E 1547.0-5408 in G327.2-0.1.

No reliable age or distance estimate is available for SNR G57.2+0.8.


GRB_name: GRB140706A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16534
SUBJECT: GRB140706A: GROND detection of the Optical/NIR afterglow
DATE:    14/07/07 10:05:11 GMT
FROM:    Patricia Schady at MPE/Swift  <pschady@mpe.mpg.de>

P. Schady (MPE Garching), S. Klose (TLS Tautenburg) and J.Greiner (MPE Garching) report on behalf of the GROND team:

We observed the field of GRB 140706A (Swift-603587; Marshall et al., GCN #16531) 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 09:01UT on 7th-July, 13.5 hours after the GRB trigger, and are continuing. They were performed at an average seeing of 1.3 and at an average airmass of 1.5.

We found a single point source within the 2.2" Swift-XRT enhanced error circle reported by Beardmore et al. (GCN #16532) consistent with the UVOT position (Marshall et al., GCN #16531).

Based on the first 8 min exposure, we estimate preliminary magnitudes (all in AB system) of

g' = 22.4 +/- 0.1 mag,
r' = 22.1 +/- 0.1 mag,
i' = 21.9 +/- 0.1 mag,
z' = 21.5 +/- 0.1 mag,
J > 20.9 mag,
H > 20.3 mag, and
K > 18.8 mag.

Given magnitudes are calibrated against GROND zeropoints as well as 2MASS field stars and are not corrected for the expected Galactic foreground extinction corresponding to a reddening of E_(B-V)=0.02 mag in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB140703A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16536
SUBJECT: GRB 140703A: AAO optical observations
DATE:    14/07/07 15:24:58 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), R. Inasaridze (AAO), O. Kvaratskhelia (AAO), V.
Ayvazian (AAO), Yu. Krugly (IA KhNU), I. Molotov (KIAM), A. Pozanenko
(IKI) report on behalf of larger GRB follow-up collaboration:

We observed the Swift GRB 140703A (Kocevski et al., GCN 16503) with 
AS-32 (0.7m) telescope of Abastumani Observatory starting on July, 07 
(UT) 23:27:06. We obtained several unfiltered frames under exellent 
weather with exposure of each frame of 120 s. The  optical afterglow 
(Cunniffe et al. GCN16504) is well detected on the stacked image.

Details of a photometry of the pi-redsifted GRB 140703A (Castro-Tirado 
et al., GCN 16505) are following:

date       UT start   t-T0       Filter  Exp.    OT        err
                      (mid, days)         (s)

2014-07-03 23:27:06  0.97235     None    23*120  21.27 +/- 0.08

The photometry is based on following SDSS stars and gri -> R 
transformation (Lupton, 2005)

SDSS id              R_Lupton
J005158.97+450627.1  17.374 Â± 0.011
J005153.14+450619.0  16.257 Â± 0.011
J005202.70+450621.8  18.216 Â± 0.014


Finding chart can be found at
http://grb.rssi.ru/GRB140703A/GRB140703A_AAO_fc.png


GRB_name: GRB140706A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16537
SUBJECT: GRB 140706A: Fermi GBM detection
DATE:    14/07/07 16:43:23 GMT
FROM:    Binbin Zhang at UAH  <binbin.zhang@uah.edu>

Bin-Bin Zhang (UAH) reports on behalf of the Fermi GBM Team:

"At 19:33:33.86 UT on 06 July 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140706A (trigger 426368016 / 140706815)
which was also detected by Swift (Marshall et al. 2014, GCN 16531).
The GBM on-ground location, using the Fermi GBM trigger data,
is consistent with the Swift/BAT location.

The GBM light curve consists of two main peaks with a total duration 
of about  47.5 s (50-300keV). The time-averaged spectrum from T0-18 s 
to T0+39 s is well fit by a power law function with an exponential 
high-energy cutoff. The power law index is -1.37 +/- 0.15 and the 
cutoff energy, parameterized as Epeak, is 96 +/- 19 keV.


The event fluence (10-1000 keV) in this time interval is
(2.95 +/- 0.28)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+0.58 s in the 10-1000 keV band is 2.9 +/- 0.2 ph/s/cm^2.

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


GRB_name: GRB140706A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16538
SUBJECT: GRB 140706A: Swift-XRT refined Analysis
DATE:    14/07/07 19:42:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), M. de Pasquale (INAF-IASFPA),
J.A. Kennea (PSU), V. Mangano (PSU), M.C. Stroh (PSU), A.P. Beardmore
(U. Leicester), P.A. Evans (U. Leicester), B.P. Gompertz (U. Leicester)
and F.E. Marshall report on behalf of the Swift-XRT team:

We have analysed 4.6 ks of XRT data for GRB 140706A (Marshall  et al.
GCN Circ. 16531),  from 62 s to 34.8 ks after the  BAT trigger. The
data comprise 56 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. 16532).

The light curve can be modelled with an initial power-law decay with an
index of alpha=3.55 (+0.25, -0.26), followed by a break at T+219 s to
an alpha of 0.62 (+/-0.06).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.84 (+0.20, -0.19). The
best-fitting absorption column is  8.1 (+5.2, -4.6) x 10^20 cm^-2, in
excess of the Galactic value of 2.2 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 3.6 x 10^-11 (4.1 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      8.1 (+5.2, -4.6) x 10^20 cm^-2
Galactic foreground: 2.2 x 10^20 cm^-2
Excess significance: 2.2 sigma
Photon index:      1.84 (+0.20, -0.19)

If the light curve continues to decay with a power-law decay index of
0.62, the count rate at T+24 hours will be 0.015 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.6 x
10^-13 (6.4 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/00603587.

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


GRB_name: GRB140706A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16539
SUBJECT: GRB 140706A: Swift-BAT refined analysis
DATE:    14/07/07 21:30:48 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

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

Using the data set from T-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140706A (trigger #603587)
(Marshall, et al., GCN Circ. 16531).  The BAT ground-calculated position is
RA, Dec = 49.269, -38.058 deg which is 
  RA(J2000)  =  03h 17m 04.6s 
  Dec(J2000) = -38d 03' 28.6" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 77%.

The mask-weighted light curve shows several peaks starting at ~T-20 sec, 
peaking at ~T-15, ~T+1 and ~T+28 sec, and ending at ~T+40 sec.  
T90 (15-350 keV) is 48.3 +- 4.3 sec (estimated error including systematics).

The time-averaged spectrum from T-21.3 to T+39.6 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.8 +- 0.1.  The fluence in the 15-150 keV band is 2.0 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-0.12 sec in the 15-150 keV band
is 1.8 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/603587/BA/


GRB_name: GRB140703A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16540
SUBJECT: GRB 140703A: Swift/UVOT Upper Limits
DATE:    14/07/07 23:45:44 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU) and D. Kocevski (NASA/GSFC/ORAU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140703A
123 s after the BAT trigger (Kocevski et al., GCN Circ. 16503).
No optical afterglow consistent with the XRT position
(Kocevski et al. GCN Circ. 16503)
is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

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

white_FC           123          239          114         >19.7
white              123         5830          507         >20.5
v                 4606         4806          197         >19.3
b                 3991         5626          393         >20.2
u                 3785         5420          393         >20.1
w1                5016         5216          197         >19.7
m2                4811         5010          197         >20.2
w2                4401         6002          359         >20.7

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.10 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB140706A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16541
SUBJECT: GRB 140706A: Swift/UVOT Detection
DATE:    14/07/07 23:46:26 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU) and F. E. Marshall (NASA/GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140706A
82 s after the BAT trigger (Marshall et al., GCN Circ. 16531).
A fading source consistent with the XRT position
(Beardmore et al. GCN Circ. 16532)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
  RA  (J2000) =  03:17:10.39 =  49.29328 (deg.)
  Dec (J2000) = -38:03:07.8  = -38.05218 (deg.)
with an estimated uncertainty of 0.45 arc sec. (radius, 90% confidence).

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

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

white (fc)          82          232          147         19.04 +/- 0.06
white              573         1541          244         19.76 +/- 0.16
v                  624         1592          117        >18.8
b                  550         1517           97        >19.2
u (fc)             294          544          246         19.02 +/- 0.11
u                  624         1591          116        >19.6
w1                 674         1638           94        >19.1
w2                 775         1394           58        >20.1

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


GRB_name: GRB140705A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16542
SUBJECT: GRB 140705A / SGR 1935+2154: VLA 6 GHz observations
DATE:    14/07/08 01:23:52 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

W. Fong and E. Berger (Harvard) report:

"We observed the field of the Swift-detected SGR 1935+2154 (GRB 140705A;
Stamatikos et al., GCN 16520) with the Karl G. Jansky Very Large Array
(VLA) beginning on 2014 Jul 6.34 UT (22.69 hr after the BAT trigger) at a
mean frequency of 6 GHz. In 1 hour of observations, we do not detect any
radio emission within the enhanced XRT position (Osborne et al., GCN 16521)
to a 3-sigma limit of 41 microJy."


GRB_name: GRB140703A
Detection_method: AMI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16543
SUBJECT: GRB 140703A: AMI 15 GHz detection
DATE:    14/07/08 09:44:15 GMT
FROM:    Gemma Anderson at U of Oxford  <gemma.anderson@astro.ox.ac.uk>

G. E. Anderson, R. P. Fender, T. D. Staley (University of Oxford), A. J. van der Horst (University of Amsterdam) and A. Rowlinson (CASS)

We observed the position of GRB 140703A (GCN 16503) at 15 GHz with the Arcminute Microkelvin Imager (AMI-LA) starting on 2014 July 3.03 to 3.12 UT and July 4.22 to 4.38 UT, corresponding to <12 minutes and 1.19 days post-burst. No radio counterpart was detected during our first observation with a 3-sigma upper limit of 0.18 mJy. However, the radio counterpart (GCN 16515 and 16516) was detected during our second observation with a preliminary flux of 0.25 +/- 0.05 mJy.

Further AMI monitoring is planned. We thank the AMI staff for scheduling these observations.


GRB_name: GRB140705A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16544
SUBJECT: GRB 140705A: Nishi-Harima NIR upper limits
DATE:    14/07/08 12:30:45 GMT
FROM:    Akira Arai at Nishi-Harima Astro. Obs/U of Hyogo  <arai@nhao.jp>

A. Arai, J. Takahashi, Y. Takagi, S. Honda, and K. Morihana (Univ. of Hyogo)
report on behalf of the Nayuta team and the OISTER collaboration:

We observed the field of GRB 140705A (Stamatikos et al., GCNC 16520)
with Nishiharima Infrared Camera (NIC) attached to the Nayuta 2-m
telescope at the Nishi-Harima Astronomical Observatory.

The observations were conducted on 2014-07-05 at 12:53:36 -- 13:06:20 UT.
We did not find any new point source within the enhanced XRT circle
(Osborne et al., GCNC 16521) in all three bands.

Three sigma upper limits of the object are listed below.
We used 2MASS catalog for flux calibration.

# MID-UT  T0+[day] T-EXP  J_mag   H_mag   Ks_mag
--------------------------------------------------------------------------------
12:59:59   0.14388   600   >16.6   >16.0   >15.4
--------------------------------------------------------------------------------
T0+: Elapsed time after the burst (day)
T-EXP: Total Exposure time (seconds)

-- 
-------------------------------------------------
Akira Arai,
Nishi-Harima Astronomical Observatory,
University of Hyogo
mail : arai@nhao.jp
-------------------------------------------------


GRB_name: GRB140709A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16546
SUBJECT: GRB 140709A: Swift detection of a burst
DATE:    14/07/09 01:28:06 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

L. M. Z. Hagen (PSU), S. D. Barthelmy (GSFC), S. B. Cenko (GSFC),
M. M. Chester (PSU), J. R. Cummings (NASA/UMBC),
N. Gehrels (NASA/GSFC), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), B. Sbarufatti (INAF-OAB/PSU)
and M. H. Siegel (PSU) report on behalf of the Swift Team:

At 01:13:41 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140709A (trigger=603810).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 304.639, +51.223 which is 
   RA(J2000) = 20h 18m 33s
   Dec(J2000) = +51d 13' 23"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows several peaks
with a total duration of about 80 sec.  The peak count rate
was ~2800 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 01:15:04.0 UT, 82.9 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 304.66332, 51.22316 which
is equivalent to:
   RA(J2000)  = 20h 18m 39.20s
   Dec(J2000) = +51d 13' 23.4"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 54 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. No
spectrum from the promptly downlinked event data is yet available to
determine the column density. 

The initial flux in the 2.5 s image was 1.01e-08 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White
filter  starting 92 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. Results from the list of
sources generated on-board are not available at this  time. No
correction has been made for the expected extinction corresponding to
E(B-V) of 0.40. 

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: GRB140709A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16547
SUBJECT: GRB 140709A: RATIR Optical and NIR Observations
DATE:    14/07/09 06:49:03 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB),
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara
(ORAU/GSFC), 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), and
Harvey Moseley (GSFC) report:

We observed the field of GRB 140709A (Hagen, et al., GCN 16546) 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 2014/07 9.17 to 2014/07 9.25 UTC (2.76 to 4.78
hours after the BAT trigger), obtaining a total of 1.42 hours exposure in
the r and i bands and 0.60 hours exposure in the Z, Y, J, and H bands.

We detect no sources within the Swift-XRT error circle.  In comparison with
2MASS, we obtain the following upper limits (3-sigma):

  r > 23.39
  i > 23.20
  Z > 22.17
  Y > 21.61
  J > 21.55
  H > 21.13

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.  We note that a faint, red source
is detected just outside the XRT error region at a position:

 RA, DEC = 304.661780,  51.224069 +/- 0.5" (J2000), with

  r > 23.08
  i = 22.15 +/- 0.13
  Z = 21.43 +/- 0.18
  Y > 21.25
  J = 20.90 +/- 0.20
  H = 20.76 +/- 0.25

We cannot confirm fading in this source.  We thank the staff of the
Observatorio AstronÃ³mico Nacional in San Pedro MÃ¡rtir.


GRB_name: GRB140709A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16548
SUBJECT: GRB 140709A - UVOT-enhanced XRT position
DATE:    14/07/09 08:24:03 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 1569 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 140709A, 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 = 304.66235, +51.22497 which is
equivalent
to:

RA (J2000): 20h 18m 38.96s
Dec (J2000): +51d 13' 29.9"

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: GRB140709A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16549
SUBJECT: GRB 140709A: Swift/UVOT Upper Limits
DATE:    14/07/09 11:53:44 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (UCL-MSSL) and L. M. Z. Hagen (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140709A
93 s after the BAT trigger (Hagen et al., GCN Circ. 16546).  No optical
afterglow consistent with the XRT position (Evans et al. GCN Circ. 16548)
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            93          242          147         >21.0
white               93         2199          186         >21.3
v                 2055         5878          216         >19.8
b                 1979        12414          848         >21.8
u                  305         6434          330         >20.5
w1                2104         6288          216         >20.2
m2                5883         6083          197         >19.9
w2                2030         2050           19         >19.7

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: GRB140709A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16550
SUBJECT: GRB 140709A: Swift-XRT refined Analysis
DATE:    14/07/09 15:28:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

V. D'Elia (ASDC), M. de Pasquale (INAF-IASFPA), V. Mangano (PSU), M.C.
Stroh (PSU), D.N. Burrows (PSU), P.A. Evans (U. Leicester), B.P.
Gompertz (U. Leicester), J.P. Osborne (U. Leicester), A. Maselli 
(INAF-IASFPA) and L.M.Z. Hagen report on behalf of the Swift-XRT team:

We have analysed 7.1 ks of XRT data for GRB 140709A (Hagen  et al. GCN
Circ. 16546),  from 75 s to 30.7 ks after the  BAT trigger. The data
comprise 195 s in Windowed Timing (WT) mode (the first 6 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. 

The late-time light curve (from T0+5.7 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.89 (+0.08, -0.09).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.48 (+/-0.07). The
best-fitting absorption column is  9.9 (+/-0.5) x 10^21 cm^-2, in
excess of the Galactic value of 4.1 x 10^21 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.88 (+/-0.14) and a
best-fitting absorption column of 8.0 (+1.2, -1.1) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 4.9 x 10^-11 (8.0 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      8.0 (+1.2, -1.1) x 10^21 cm^-2
Galactic foreground: 4.1 x 10^21 cm^-2
Excess significance: 5.8 sigma
Photon index:      1.88 (+/-0.14)

If the light curve continues to decay with a power-law decay index of
0.89, the count rate at T+24 hours will be 0.038 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.9 x
10^-12 (3.1 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/00603810.

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


GRB_name: GRB140709B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16551
SUBJECT: GRB 140709B: Swift detection of a burst
DATE:    14/07/09 15:30:15 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@swift.psu.edu>

C. A. Swenson (PSU), W. H. Baumgartner (GSFC/UMBC),
D. N. Burrows (PSU), S. B. Cenko (GSFC), M. M. Chester (PSU),
J. R. Cummings (NASA/UMBC), P. A. Evans (U Leicester),
N. Gehrels (NASA/GSFC), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), V. Mangano (PSU),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester),
D. M. Palmer (LANL) and M. H. Siegel (PSU) report on behalf of the
Swift Team:

At 15:15:45 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140709B (trigger=603866).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 146.071, +63.505 which is 
   RA(J2000) = 09h 44m 17s
   Dec(J2000) = +63d 30' 20"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure with a duration of about 150 sec.  The peak count rate
was ~1500 counts/sec (15-350 keV), at ~20 sec after the trigger. 

The XRT began observing the field at 15:17:15.9 UT, 91.0 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 146.05394, 63.53040 which
is equivalent to:
   RA(J2000)  = 09h 44m 12.95s
   Dec(J2000) = +63d 31' 49.4"
with an uncertainty of 3.9 arcseconds (radius, 90% containment). This
location is 95 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. No
spectrum from the promptly downlinked event data is yet available to
determine the column density. 

The initial flux in the 2.5 s image was 3.60e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting 96
seconds after the BAT trigger. No credible afterglow candidate has been found
in the initial data products. The 2.7'x2.7' sub-image covers 100% of the XRT
error circle. The typical 3-sigma upper limit has been about 19.2 mag. The
8'x8' region for the list of sources generated on-board covers 100% of the XRT
error circle. The list of sources is typically complete to about 18.0 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.04. 

Burst Advocate for this burst is C. A. Swenson (cswenson AT astro.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: GRB140709B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16552
SUBJECT: GRB 140709B: MASTER optical observation
DATE:    14/07/09 16:04:23 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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

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

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

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

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Tunka was pointed to the  GRB140709B  40 sec after Notice 
time and 94 sec after trigger 
time at 2014-07-09 15:17:19 UT (Swenson et al., GCN 16551). On our first 
(20s exposure)  set we  haven't found optical transient  within SWIFT 
BAT error-box.
The 5-sigma upper limit has been about 17.1mag
We have number images with out OT brighter 18.2  at
  94s < T - T_trigger < 289s.

The message may be cited.


GRB_name: GRB140709A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16553
SUBJECT: GRB 140709A, Swift-BAT refined analysis
DATE:    14/07/09 16:29:31 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

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

Using the data set from T-239 to T+626 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140709A (trigger #603810)
(Hagen, et al., GCN Circ. 16546).  The BAT ground-calculated position is
RA, Dec = 304.666, 51.222 deg which is
    RA(J2000)  =  20h 18m 39.9s
    Dec(J2000) = +51d 13' 17.8"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 61%.

The mask-weighted light curve shows a complex structure.  Burst activity begins
at T-50 sec, with a gradual rise to a peak at T+0 sec, punctuated by several
subsidiary peaks.  Then there is a return to near background by T+8 sec,
followed by a second main peak at T+15 sec.  There are additional smaller and
softer peaks centered at T+55 and T+75 sec. T90 (15-350 keV) is 98.6 +- 7.7 sec
(estimated error including systematics).

The time-averaged spectrum from T-46.1 to T+93.4 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.23 +- 0.27,
and Epeak of 78.0 +- 20.4 keV (chi squared 57.80 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 5.2 +- 0.2 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+15.48 sec in the 15-150 keV band is
3.1 +- 0.3 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.74 +- 0.06 (chi squared 69.09 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/603810/BA/


GRB_name: GRB140709A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16554
SUBJECT: GRB 140709A: BOOTES-2 and OSN optical observations
DATE:    14/07/09 16:51:28 GMT
FROM:    Juan Carlos Tello at IAA-CSIC  <jtello@iaa.es>

A.J. Castro-Tirado (IAA-CSIC, ISA-UMA), J. Gorosabel (IAA-CSIC, UPV-EHU),
J. C. Tello, R. Cunniffe, A. Gonzalez-Rodriguez, A. Sota, M. Jelinek, S.
Jeong, O. Lara-Gil, S. R. Oates, R. Sanchez-Ramirez (IAA-CSIC, Granada), P.
Kubanek (IP-ASCR, Prague) and S. Pandey (ARIES) report:

Following the detection of GRB 140709A by Swift (Hagen et al., GCNC 16546),
the 0.6m TELMA robotic telescope at the BOOTES-2 astronomical station
Malaga (Spain), responded to the GRB location starting at 01:14:41 UT (i.e.
60s postburst, in the clear filter, 5s integrations), with an upper limit
of R > 16.5. Further optical observations were carried out at the 1.5m OSN
telescope starting on July 9.06-9.12 UT (i.e. 0.37--1.72 hours post GRB). A
source coincident with the enhanced XRT position is found (Evans et al. GCN
16548) at coordinates RA(J2000) = 20:18:38.95,  DEC(J2000) = 51:13:29.6
(+/-0.5") when the 78x60s frames are co-added.  Using USNO-B1.0 as
reference, we measure a Vega magnitude of I = 20.8 (uncorrected for
Galactic reddening), which is the potential optical afterglow. At the
present stage we do not know is the source is fading or not. We also detect
the object reported by RATIR (Butler et al. GCN 16547), which is not
consistent with the position of our candidate. Further observations are
planned.


GRB_name: GRB140709A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16555
SUBJECT: GRB 140709A: Fermi GBM detection
DATE:    14/07/09 17:01:51 GMT
FROM:    Eric Burns at U of Alabama  <EricKayserBurns@gmail.com>

E. Burns (UAH) reports on behalf of the Fermi GBM Team:

"At 01:13:41.38 UT on 09 July 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140709A (trigger 426561224 / 140709051).
which was also detected by the Swift/BAT (L. Hagen et al., GCN 16546)
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 111 degrees.

The GBM light curve consists of two main peaks
with a duration (T90) of about 70s (50-300 keV).
The time-averaged spectrum from T0-25 s to T0+45 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.10 +/- 0.07 and
the cutoff energy, parameterized as Epeak, is 126 +/- 9 keV

The event fluence (10-1000 keV) in this time interval is
(8.8 +/- 0.4)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+15.0 s in the 10-1000 keV band
is 5.2 +/- 0.3 ph/s/cm^2.

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


GRB_name: GRB140709B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16556
SUBJECT: GRB 140709B: Enhanced Swift-XRT position
DATE:    14/07/09 21:16:08 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 787 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 140709B, 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 = 146.05423, +63.52934 which is equivalent
to:

RA (J2000): 09h 44m 13.02s
Dec (J2000): +63d 31' 45.6"

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

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

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


GRB_name: GRB140709B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16557
SUBJECT: GRB 140709B: OSN optical limit
DATE:    14/07/09 22:47:34 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

A. Sota (IAA-CSIC), J. Gorosabel (IAA-CSIC, UPV-EHU) and A. J.
Castro-Tirado (IAA-CSIC, ISA-UMA), on behalf of a larger collaboration,
report:

Following the detection of GRB 140709B by Swift (Swenson et al. GCNC
16551), we have taken I-band frames with the 1.5m OSN telescope at
Observatorio de Sierra Nevada (Granada, Spain) starting at 20:45 UT (5.5 h
post burst) at high airmass. Within the enhanced XRT position (Goad et al.
GCNC 16556) we find no credible counterpart down to the DSS-2 limiting
magnitude when all the images are co-added (10 x 150s). Near-infrared
imaging is encouraged.


GRB_name: GRB140709B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16558
SUBJECT: GRB 140709B:  Khureltogot optical upper limit
DATE:    14/07/09 22:59:55 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), S. Schmalz (AIP), N. Tungalag (Research Centre 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 GRB 140709B (Swenson et al., GCN 16551) with ORI-40 
telescope of Khureltogot observatory starting on
Jul., 09 (UT) 15:31:51. In the first unfiltered images of 60 s exposure we 
do not detect any object in the enhanced XRT error circle  (Goad et al., GCN 
16556) down to 17.7m in each separate image. The photometry is based on 
nearby USNO-B1.0 stars. 


GRB_name: GRB140709A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16559
SUBJECT: GRB 140709A : Virtual Telescope optical observations
DATE:    14/07/09 23:35:27 GMT
FROM:    Gianluca Masi at Bellatrix Astronomical Obs  <gianluca@bellatrixobservatory.org>

G. Masi, the Virtual Telescope Project - Italy, reports:

I started observations of GRB 140709A (Hagen et al. GCN  16546) with the 17" 
robotic unit part of the Virtual Telescope (Ceccano, Italy) at 02:04:00 UT, 3000 
seconds after the burst.

An optical source is visible where described by Castro-Tirado et al. (GCN 16554) 
in a image coming from the sum of three, 180-seconds exposures, unfiltered. The 
position of the source is RA: 20h18m38.94s +51d13'29.9" (J2000, mean residuals 
of 0.2") and the magnitude was estimated to be 21.0, assuming R mags for the 
reference stars from UCAC-4.

The message may be cited.


GRB_name: GRB140709B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16560
SUBJECT: GRB 140709B: Swift-BAT refined analysis
DATE:    14/07/10 02:19:39 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

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

Using the data set from T-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140709B (trigger #603866)
(Swenson, et al., GCN Circ. 16551).  The BAT ground-calculated position is
RA, Dec = 146.040, 63.536 deg which is
    RA(J2000)  =  09h 44m 09.5s
    Dec(J2000) = +63d 32' 10.0"
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 99%.

The mask-weighted light curve shows a complex structure.  The first peak has a
broad, symmetrical shape, starting at T-20 sec, peaking at T+25 sec and ending
at T+60 sec.  Then the second episode begins at T+80 sec, with multiple short
(~1-2 second) peaks extending to T+140 sec, before cutting off.  The highest of
these short peaks is at T+125 sec. T90 (15-350 keV) is 155.0 +- 22.3 sec
(estimated error including systematics).

The time-averaged spectrum from T-13.94 to T+197.51 sec is best fit by a power 
law with an exponential cutoff.  This fit gives a photon index 0.79 +- 0.30,
and Epeak of 152.6 +- 111.0 keV (chi squared 48.15 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 4.2 +- 0.2 x 10^-06 erg/cm2
and the 1-sec peak flux measured from T+123.63 sec in the 15-150 keV band is
0.9 +- 0.1 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.22 +- 0.07 (chi squared 54.91 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/603866/BA/


GRB_name: GRB140709B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16561
SUBJECT: GRB 140709B: Fermi GBM detection
DATE:    14/07/10 03:08:23 GMT
FROM:    Binbin Zhang at UAH  <binbin.zhang@uah.edu>

Bin-Bin Zhang (UAH) reports on behalf of the Fermi GBM Team:

"At 15:17:52.85 UT on 09 July 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140709B (trigger 426611875 / 140709637)
which was also detected by Swift (Swenson et al. 2014, GCN 16551).
The GBM on-ground location, using the Fermi GBM trigger data,
is consistent with the Swift/BAT location.

The angle from the Fermi LAT boresight is 60 degrees.

The GBM light curve consists of two main peaks with a total duration
of about 150 s (50-300keV). The time-averaged spectrum from T0-132 s 
to T0+15 s is well fit by a power law function with an exponential 
high-energy cutoff. The power law index is -1.32 +/- 0.07 and the 
cutoff energy, parameterized as Epeak, is 530 +/- 232 keV.


The event fluence (10-1000 keV) in this time interval is
(1.6 +/- 0.1)E-05 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0-1.28 s in the 10-1000 keV band is 1.9 +/- 0.2 ph/s/cm^2.

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


GRB_name: GRB140709B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16562
SUBJECT: GRB 140709B: Swift-XRT refined Analysis
DATE:    14/07/10 04:29:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 10.0 ks of XRT data for GRB 140709B (Swenson  et al.
GCN Circ. 16551),  from 85 s to 28.9 ks after the  BAT trigger. The
data comprise 207 s in Windowed Timing (WT) mode (the first 4 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. 16556).

The late-time light curve (from T0+4.8 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.99 (+0.13, -0.12).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.14 (+/-0.07). The
best-fitting absorption column is  2.2 (+0.5, -0.4) x 10^21 cm^-2, in
excess of the Galactic value of 4.3 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.05 (+0.14, -0.13)
and a best-fitting absorption column of 1.9 (+/-0.4) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.4 x 10^-11 (4.7 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.9 (+/-0.4) x 10^21 cm^-2
Galactic foreground: 4.3 x 10^20 cm^-2
Excess significance: 5.7 sigma
Photon index:      2.05 (+0.14, -0.13)

If the light curve continues to decay with a power-law decay index of
0.99, the count rate at T+24 hours will be 0.010 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.5 x
10^-13 (4.9 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00603866.

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


GRB_name: GRB140710A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16563
SUBJECT: GRB 140710A: Swift detection of a burst
DATE:    14/07/10 10:32:36 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. H. Siegel (PSU), D. N. Burrows (PSU), M. M. Chester (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 10:16:40 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140710A (trigger=603954).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 41.087, +35.493 which is 
   RA(J2000) = 02h 44m 21s
   Dec(J2000) = +35d 29' 36"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 5 sec.  The peak count rate
was ~3000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 10:18:18.4 UT, 98.4 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 41.0678, 35.4994 which
is equivalent to:
   RA(J2000)  = 02h 44m 16.27s
   Dec(J2000) = +35d 29' 57.9"
with an uncertainty of 2.2 arcseconds (radius, 90% containment). This
location is 60 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (7.15 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 7.8
(+5.32/-4.24) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 102 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.06. 

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: GRB140709A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16564
SUBJECT: GRB 140709A: 10.4m GTC optical decay
DATE:    14/07/10 11:39:14 GMT
FROM:    Juan Carlos Tello at IAA-CSIC  <jtello@iaa.es>

A.J. Castro-Tirado (IAA-CSIC, ISA-UMA), J. Gorosabel (IAA-CSIC, UPV-EHU),
J. C. Tello, R. Cunniffe, A. Gonzalez-Rodriguez, A. Sota, M. Jelinek, S.
Jeong, O. Lara-Gil, S. R. Oates, R. Sanchez-Ramirez (IAA-CSIC, Granada), P.
Kubanek (IP-ASCR, Prague), S. Pandey (ARIES),  and A. Garcia (GTC,IAC) report:

The field of GRB 140709A (Hagen et al. GCNC  16546) was observed in i'-band
with  the 10.4m GTC telescope in two epochs centered on July 9.12955 and
10.10966 UT (1.9 and 25.4 hours post burst). Comparison between those two
epochs reveals that the optical candidate reported by Castro-Tirado et al.
(GCNC 16554) has faded by ~0.7 mags (from i'~21.3 to 22.0, both in AB),
implying a shallow decay index of ~0.2.  A similar decay is measured in
z'-band.

[GCN OPS NOTE(12jul14): Per author's request, AG was added to the author list.]


GRB_name: GRB140710A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16565
SUBJECT: GRB 140710A: GROND Detection of NIR Afterglow Candidate
DATE:    14/07/10 12:11:39 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

M. Tanga, C. Delvaux and J. Greiner (all MPE Garching) report on behalf of
the GROND team:

We observed the field of GRB 140710A (Swift trigger 603954; Siegel et al.,
GCN #16563) simultaneously in 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 10:48 UT on 2014-07-10, 0.5 hrs after the GRB
trigger, but already in morning twilight and thus without the optical
GROND channels. Observations were performed at an average seeing of 
1.5" and at an average airmass of 2.6.

We found a single point source within the 2.2" Swift-XRT error circle
reported by Siegel et al. (GCN #16563) at

RA (J2000) = 02 h 44 m 16.30 s
DEC (J2000) = +35d 29' 08.4

with an uncertainty of 0.5" in each coordinate. 

Based on 4 min of total exposure we estimate a preliminary magnitude 
of about
  
J(AB) ~ 20.5 mag

The given magnitude is calibrated against 2MASS field stars and is not
corrected for the expected Galactic foreground extinction corresponding 
to a reddening of E_(B-V)=0.06 mag in the direction of the burst 
(Schlegel et al. 1998).


GRB_name: GRB140710A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16566
SUBJECT: GRB 140710A: correction to GCN #16565
DATE:    14/07/10 13:21:04 GMT
FROM:    Corentin Delvaux at MPE  <delvaux@mpe.mpg.de>

C. Delvaux (MPE Garching) reports:

The coordinates in GCN  #16565 should read:

RA (J2000) = 02 h 44 m 16.30 s
DEC (J2000) = +35d 29' 57.1

Sorry for any confusion caused by this mistake.


GRB_name: GRB140710A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16567
SUBJECT: GRB 140710A: P60 Confirmation of Afterglow
DATE:    14/07/10 14:35:19 GMT
FROM:    S. Bradley Cenko at NASA/GSFC  <brad.cenko@nasa.gov>

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

We observed the location of GRB140710A (Siegel et al., GCN 16563) with the robotic Palomar 60 inch telescope.  Observations were obtained in the r', i', and z' filters beginning 3.1 minutes after the Swift trigger time.  We detect a faint source within the XRT error circle in all three filters, roughly consistent with the location of the candidate reported by GROND (Tanga et al., GCNs 16565; Delvaux, GCN 16566).  Using several nearby point sources from the APASS catalog for calibration, we measure the following AB magnitudes:

r' = 19.90 at dt = 3.6 min 
i' = 19.80 at dt = 5.0 min

Over the course of the first hour following the Swift trigger time, the source fades by >~ 1.0 mag in r', confirming that it is indeed the optical afterglow of GRB140710A.


GRB_name: GRB140710A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16568
SUBJECT: GRB 140710A: RATIR Optical and NIR Observations
DATE:    14/07/10 14:37:42 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB),
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara
(ORAU/GSFC), 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), and
Harvey Moseley (GSFC) report:

We observed the field of GRB 140710A (Siegel, et al., GCN 16563) 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 2014/07 10.43 to 2014/07 10.47 UTC (3.6
minutes to 1.12 hours after the BAT trigger), obtaining a total of 0.71
hours exposure in the r and i bands and 0.30 hours exposure in the Z, Y, J,
and H bands.

For a source within the Swift-XRT error circle (see also, Castro-Tirado, et
al., GCN 16564; Tanga, et al., GCN 16565), in comparison with 2MASS, we
obtain the following detections:

  r     21.36 +/- 0.08
  i     21.10 +/- 0.07
  Z     20.77 +/- 0.14
  Y     20.42 +/- 0.16
  J     20.31 +/- 0.14
  H     19.75 +/- 0.13

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.  The source appears to fade in all
bands.

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


GRB_name: GRB140710A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16569
SUBJECT: GRB 140710A: Enhanced Swift-XRT position
DATE:    14/07/10 15:44:28 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Using 528 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 140710A, 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 = 41.06775, +35.49908 which is equivalent
to:

RA (J2000): 02h 44m 16.26s
Dec (J2000): +35d 29' 56.7"

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

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

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


GRB_name: GRB140710A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16570
SUBJECT: GRB 140710A: Gemini-N redshift of likely host
DATE:    14/07/10 15:44:55 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir (U. Leicester), A. J. Levan (U. Warwick) and
D. Coulson (Gemini) report:

We observed the position of GRB 140710A (Siegel et al.
GCN 16563; Tanga et al. GCN 16565/6; Cenko et al. GCN 16567;
Butler et al. GCN 16568) with the GMOS-N spectrograph on
Gemini-North.  Observations began at 14:06 UT, approximately
3.8 hr post burst.

The spectrum shows a faint continuum and emission lines of
OII (3727), Hbeta (4863) and OIII (4959/5007) at a common 
redshift of z=0.558.  There is also some evidence for a 4000A
break at the same redshift.  Given the fading nature already reported, 
and the slight extension of the source in the acquisition images,
it is very likely that this is the redshift of the GRB host galaxy, and 
that it is already comparable to the afterglow brightness.


GRB_name: GRB140709B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16571
SUBJECT: GRB 140709B:  update of Khureltogot optical upper limit
DATE:    14/07/10 16:35:49 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

After receiving a full data set we report details of the  observation of 
the   field of GRB 140709B (Swenson et al., GCN 16551) with ORI-40 
telescope of Khureltogot observatory.  We started observation on July 09 
(UT) 15:31:51 and obtained 60 unfiltered images of 60 s exposure. 
Within enhanced XRT error circle  (Goad et al., GCN 16556) we do not 
detect any new object neither in separate, nor in stacked images. 
Details of a photometry is following

UT start   t-T0,d   Exp,s  Filter Up_lim (3 sigma)

15:31:51  0.01334   5*60   None   18.9
15:31:51  0.01940  20*60   None   19.5

The photometry is based on SDSS star J094401.61+633253.8 assuming 
R=16.010+/-0.013 (using gri -> R Lupton transformations).


GRB_name: GRB140710A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16572
SUBJECT: GRB 140710A: Swift/UVOT Upper Limits
DATE:    14/07/10 20:28:33 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (IAA-CSIC/UCL-MSSL) and M. H. Siegel (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140710A
103 s after the BAT trigger (Siegel et al., GCN Circ. 16563).
No optical afterglow consistent with the optical position
(Delvaux et al., GCN Circ. 16566, Tanga et al., GCN Circ. 16565) or the enhanced XRT position 
(Osborne et al., GCN Circ. 16569) 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           103          253          147         >20.1
u_FC               315          565          246         >19.2
white              103         5830          363         >20.7
v                  644        16380         1090         >19.8
b                  570        12165          806         >20.3
u                  315        11556         1376         >20.5
w1                4153        17926         1706         >20.7
m2                3948        17285         1245         >20.8
w2                 620         6035          216         >19.7

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


GRB_name: GRB140710A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16573
SUBJECT: GRB 140710A: Swift-BAT refined analysis
DATE:    14/07/10 21:46:28 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@nasa.gov>

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

Using the data set from T-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140710 (trigger #603954)
(Siegel, et al., GCN Circ. 16563).  The BAT ground-calculated position is
RA, Dec = 41.088, 35.499 deg which is
    RA(J2000)  =  02h 44m 21.0s
    Dec(J2000) = +35d 29' 54.8"
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 58%.

The mask-weighted light curve shows a single peak of duration ~4 seconds,
starting at T0. T90 (15-350 keV) is 3.52 +- 0.91 sec (estimated error including
systematics).

The time-averaged spectrum from T-0.23 to T+3.80 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.00 +- 0.23.  The fluence in the 15-150 keV band is 2.3 +- 0.3 x 10^-07 
erg/cm2. The 1-sec peak photon flux measured from T+0.04 sec in the 15-150 keV 
band is 1.9 +- 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/603954/BA/


GRB_name: GRB140710A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16574
SUBJECT: GRB 140710A: Swift-XRT refined Analysis
DATE:    14/07/10 22:32:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 9.4 ks of XRT data for GRB 140710A (Siegel  et al. GCN
Circ. 16563),  from 83 s to 23.7 ks after the  BAT trigger. The data
comprise 8 s in Windowed Timing (WT) mode (taken while Swift was
slewing), with the remainder in Photon Counting (PC) mode. The enhanced
XRT position for this burst was given by Osborne et al. (GCN Circ.
16569).

The late-time light curve (from T0+3.9 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.8 (+/-0.3).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.98 (+0.20, -0.19). The
best-fitting absorption column is  3.2 (+0.9, -0.8) x 10^21 cm^-2, in
excess of the Galactic value of 7.2 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 (5.6 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.2 (+0.9, -0.8) x 10^21 cm^-2
Galactic foreground: 7.2 x 10^20 cm^-2
Excess significance: 5.1 sigma
Photon index:      1.98 (+0.20, -0.19)

If the light curve continues to decay with a power-law decay index of
0.8, the count rate at T+24 hours will be 3.2 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.2 x
10^-13 (1.8 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00603954.

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


GRB_name: GRB140709A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16575
SUBJECT: GRB 140709A: Continued RATIR Optical and NIR Observations
DATE:    14/07/10 23:21:48 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB),
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara
(ORAU/GSFC), 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), and
Harvey Moseley (GSFC) report:

We observed the field of GRB 140709A (Hagen, et al., GCN 16546) 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 from 2014/07 9.17 to 2014/07 9.46 UTC (2.76 to
9.93 hours after the BAT trigger), obtaining a total of 4.98 hours exposure
in the r and i bands and 2.09 hours exposure in the Z, Y, J, and H bands
and again from 2014/07 10.17 to 2014/07 10.42 UTC (26.77 to 32.87 hours
after the BAT trigger), obtaining a total of 4.27 hours exposure in the r
and i bands and 1.79 hours exposure in the Z, Y, J, and H bands.

We detect the afterglow candidate reported by Castro-Tirado et al. (GCN
16554; also Masi, et al., GCN 16559; Castro-Tirado, et al., GCN 16564) in
both epochs, adding a deeper integration for our first epoch as compared to
our initial report (Butler, et al., GCN 16547).  Relative to 2MASS and
using the RATIR zero-points, we find:

     7/09                   7/10
  r  24.28 +/- 0.45   23.85 +/- 0.31
  i  23.05 +/- 0.16   23.28 +/- 0.20
  Z >22.92             >22.68
  Y >22.40             >22.33
  J >22.30             >22.27
  H >21.94             >21.85

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.  Upper limits are 3-sigma.  We
cannot reliably confirm fading in this source.  We note that another RATIR
source outside of the Swift XRT error region (see, GCN 16547) does not
appear to fade and is not likely to be the afterglow to GRB 140709A.

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


GRB_name: GRB140710B
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16576
SUBJECT: GRB 140710B: a long GRB detected with INTEGRAL
DATE:    14/07/10 23:59:31 GMT
FROM:    Diego Gotz at CEA  <diego.gotz@cea.fr>

D.Gotz (CEA, Saclay), S.Mereghetti (IASF-Milano), C.Ferrigno, E.Bozzo, D. Malishev (ISDC, Versoix), and J.Borkowski (CAMK, Torun) on behalf of the IBAS Localization Team report:
a gamma ray burst lasting about 30 s has been detected by IBAS in the IBIS/ISGRI data at 21:37:30 UT of July 10, 2014. Due to a S/W maintenance problem at ISDC no refined coordinates can currently be computed. So the automatic coordinates should be considered at this time. Refined coordinates will be posted as soon as the attitude files will be available again. The automatic coordinates are:

R.A.=  204.657 deg
DEC.=  -58.5854  deg

with an uncertainty of 2.8 arcmin (90% c.l.).

A preliminary analysis gives a peak flux of about 1.2 counts/cm2/s (20-200 keV, 1-s integration time) and a fluence in the same energy range of about 1e-6 erg/cm2.

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

[GCN OPS NOTE(10jul14): Per author's request, the "July 11" date in the first sentence
was corrected to "Jul10.]


GRB_name: GRB140710B
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16578
SUBJECT: GRB 140710B: improved INTEGRAL position
DATE:    14/07/11 12:10:13 GMT
FROM:    Diego Gotz at CEA  <diego.gotz@cea.fr>

D.Gotz (CEA, Saclay), S.Mereghetti (IASF-Milano), C.Ferrigno, E.Bozzo, (ISDC, Versoix), and J.Borkowski (CAMK, Torun) on behalf of the IBAS Localization Team report:
We derived for the INTEGRAL GRB 140710B (Gotz et al., GCN 16576) a refined position and a reduced error box using the updated attitude information and the IBIS/ISGRI data. The refined coordinates are:

R.A.=   204.6457 deg
Dec.=  -58.5913  deg
with an uncertainty of 1.7 arcmin (90% c.l.). We note that this refined position is fully consistent with the automatic one.


GRB_name: GRB140710B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16579
SUBJECT: GRB 140710B: Fermi GBM detection
DATE:    14/07/11 20:09:53 GMT
FROM:    Eric Burns at U of Alabama  <EricKayserBurns@gmail.com>

E. Burns (UAH) reports on behalf of the Fermi GBM Team:

"At 21:37:37.94 UT on 10 July 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140710B (trigger 426721060 / 140710901).
which was also detected by INTEGRAL IBIS/ISGRI
(Gotz et al., GCN 16576).
The GBM on-ground location is consistent with the refined INTEGRAL
position (Gotz et al., GCN 16578).

The angle from the Fermi LAT boresight is 79 degrees.

The GBM light curve shows multiple peaks
with a duration (T90) of about 30.7 s (50-300 keV).
The time-averaged spectrum from T0-56 s to T0+68 s is
best fit by a simple power law function with index -1.9 +/- 0.1.

The event fluence (10-1000 keV) in this time interval is
(2.3 +/- 0.4)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-1.2s in the 10-1000 keV band
is 2.7 +/- 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: GRB140713A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16581
SUBJECT: GRB 140713A: Swift detection of a burst
DATE:    14/07/13 18:58:44 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

V. Mangano (PSU), S. D. Barthelmy (GSFC), M. M. Chester (PSU),
J. R. Cummings (NASA/UMBC), J. A. Kennea (PSU) and
B. Sbarufatti (INAF-OAB/PSU) report on behalf of the Swift Team:

At 18:43:45 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140713A (trigger=604232).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 281.114, +59.625 which is 
   RA(J2000)  =  18h 44m 27s
   Dec(J2000) = +59d 37' 29"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows two peaks
with a total duration of about 7 sec.  The peak count rate
was ~3500 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 18:44:57.8 UT, 72.8 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 281.1053, 59.6333 which
is equivalent to:
   RA(J2000)  = 18h 44m 25.28s
   Dec(J2000) = +59d 37' 59.8"
with an uncertainty of 2.0 arcseconds (radius, 90% containment). This
location is 33 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (4.97 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 7.8
(+5.23/-4.19) x 10^21 cm^-2 (90% confidence). 

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
0.05. 

Burst Advocate for this burst is V. Mangano (vxm22 AT psu.edu). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB140710A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16582
SUBJECT: GRB 140710A: iTelescope.Net T11 Optical Observation
DATE:    14/07/13 20:00:23 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

D. Kawamura, T. Sakamoto, A. Yoshida (AGU)

We observed the field of GRB 140710A detected by Swift (trigger #603954; 
Siegel et al., GCN Circ. 16563) with the iTelescope.Net (http://www.itelescope.net) 
T11 (0.51 m Planewave) telescope located at the New Mexico Skies Observatory 
(NM, USA).  

20 images of 60 sec exposures were taken in the R filter starting from July 10 10:35:00 (UT) 
about 18 minutes after the trigger and stopped on July 10 10:58:30 (UT).  We do not detect 
the optical afterglow both in the individual images and the stacked image at the enhanced X-ray 
afterglow position (Osborne et al., GCN Circ. 16569).  The estimated five sigma upper limit of 
the combined image (total exposure of 1200 sec) is ~19.5 using the USNO-B1 catalog.


GRB_name: GRB140713A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16583
SUBJECT: GRB 140713A: T100 observations
DATE:    14/07/13 22:51:23 GMT
FROM:    Eda Sonbas at NASA/GSFC  <edasonbas@gmail.com>

Sonbas, E. (Adiyaman Univ.), Avdan, H., Dolek, F. (Cukurova Univ.), Guver,
T. (Istanbul Univ.), Gogus, E. (Sabanci Univ.), Erece, O. (Akdeniz Univ.),
Kirbiyik, H. (TUG) on behalf of a larger collaboration.


We observed the field of GRB 140713A (Mangano et al., GCN #16581) with the
1.0 meter T100 telescope (TUBITAK National Observatory, Antalya - Turkey),
starting on July 13, 20:14:06 UT (~ 1.5 hours after the trigger). We
obtained 5 x 300 s exposures with R filters under good weather conditions.


We do not detect an optical afterglow within the reported XRT error circle
down to a limiting magnitude of >19.9 (2-sigma) in the combined R band
image.


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


GRB_name: GRB140713A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16584
SUBJECT: GRB 140713A: Swift-BAT refined analysis
DATE:    14/07/13 23:17:37 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/UMBC), C. B. Markwardt (GSFC), V. Mangano (PSU),
D. M. Palmer (LANL), T. Sakamoto (AGU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+325 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 140713A (trigger #604232)
(Mangano, et al., GCN Circ. 16581).  The BAT ground-calculated position is
RA, Dec = 281.141, 59.623 deg which is 
   RA(J2000)  =  18h 44m 33.9s 
   Dec(J2000) = +59d 37' 22.3" 
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 97%.
 
The mask-weighted light curve shows two peaks starting at ~T-0.2 sec, peaking
at ~T+0.2 and ~T+5 sec, and ending at ~T+10 sec.  T90 (15-350 keV) is
5.30 +- 0.66 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.11 to T+6.68 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.84 +- 0.14.  The fluence in the 15-150 keV band is 3.7 +- 0.3 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.11 sec in the 15-150 keV band
is 1.9 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/604232/BA/


GRB_name: GRB140713A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16585
SUBJECT: GRB 140713A: Enhanced Swift-XRT position
DATE:    14/07/14 00:40:27 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 2110 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 140713A, 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 = 281.10470, +59.63356 which is equivalent
to:

RA (J2000): 18h 44m 25.13s
Dec (J2000): +59d 38' 00.8"

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

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

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


GRB_name: GRB140713A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16586
SUBJECT: GRB 140713A : Xinglong TNT upper limit
DATE:    14/07/14 07:32:10 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

L. P. Xin,   J.  Z, Yan,  J. Y. Wei,  Y. L. Qiu, J. S. Deng,  
J. Wang, X. H. Han and C. Wu on behalf of EAFON report:

We began to observe GRB 140713A (Mangano et al., GCN 16581)  
with Xinglong  0.8-m TNT telescope at 18:44:47 (UT) , 
62 sec after the burst.

No any new optical transient was detected in our single or stacked image
in the XRT error box (Mangano et al., GCN 16581).
Calibrated by nearby USNO B1.0 R2 mag, 
the 3-sigma upper limit magnitudes are shown in the following: 

T-T0(sec,mid)  exposure(sec)    Filter     Upper limit
72                       20                       W          18.0
282                     20*20                  W           19.5

The message may be cited.


GRB_name: GRB140713A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16587
SUBJECT: GRB 140713A: NOT upper limits
DATE:    14/07/14 11:21:24 GMT
FROM:    Zach Cano at U of Iceland  <zewcano@gmail.com>

â€‹â€‹Z. Cano (U. Iceland), D. Malesani (DARK/NBI) and M. Nielsen (Max Planck,
Gottingen) report on behalf of a larger collaboration:

We observed the field of GRB 140713A (Mangano et al., GCN Circ. 16581) with
the 2.5-m Nordic Optical Telescope (NOT) equipped with ALFOSC starting at
22:02 UT on 13-Jul-2014. We obtained 5x180 s frames in both SDSS-r and
SDSS-i, and 5x300s in SDSS-z.

No new object is found in the refined XRT error circle (Beardmore et al.,
GCN Circ. 16585) down to limiting magnitudes of:

  filter                t-t0 (hr)
---------------------------------
R (Vega) > 23.9    3.46
I (Vega)  > 23.0    3.77
z (AB)     > 22.5    4.17

The upper limits for an isolated point source in our combined images have
been determined using nearby USNO star at RA=18:44:21.50, Dec=+59:38:04.0,
which has R2=19.23, Imag=17.85, and z=17.87.  The z-band magnitude has been
determined using transformation equations from Table 3 in Jordi et al.
(2006,A&A,460,339).  These magnitudes have not been corrected for
foreground extinction.


GRB_name: GRB140713A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16588
SUBJECT: GRB 140713A: Swift/UVOT Upper Limits
DATE:    14/07/14 11:31:48 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (UCL-MSSL) and V. Mangano (PSU) report on behalf of the 
Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140713A 76 
s after the BAT trigger (Mangano et al., GCN Circ. 16581).
No optical afterglow consistent with the XRT position (Beardmore et al. 
GCN Circ. 16585) 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            76          226          147         >21.8
u_FC               288          538          246         >20.8
white               76         7155          608         >22.9
v                  618         7547          313         >20.9
b                  544        29522          422         >21.5
u                  288        29406         2244         >21.8
w1                 669        17514         1084         >21.3
m2                 644        11576          357         >20.5
w2                 594         7361          333         >20.7

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: GRB140713A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16589
SUBJECT: GRB 140713A: Swift-XRT refined Analysis
DATE:    14/07/14 12:58:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.7 ks of XRT data for GRB 140713A (Mangano  et al.
GCN Circ. 16581),  from 5.4 ks to 47.8 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.
16585).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.20 (+0.27, -0.24).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.8 (+/-0.5). The
best-fitting absorption column is  6.8 (+3.8, -3.2) x 10^21 cm^-2, in
excess of the Galactic value of 5.0 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 4.9 x 10^-11 (7.6 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      6.8 (+3.8, -3.2) x 10^21 cm^-2
Galactic foreground: 5.0 x 10^20 cm^-2
Excess significance: 3.2 sigma
Photon index:      1.8 (+/-0.5)

If the light curve continues to decay with a power-law decay index of
1.20, the count rate at T+24 hours will be 3.0 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.5 x
10^-13 (2.3 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00604232.

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


GRB_name: GRB140713A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16590
SUBJECT: GRB 140713A: Fermi GBM detection
DATE:    14/07/14 18:08:35 GMT
FROM:    Binbin Zhang at UAH  <binbin.zhang@uah.edu>

Bin-Bin Zhang (UAH) reports on behalf of the Fermi GBM Team:

"At 18:43:45.30 UT on 13 July 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140713A (trigger 426969828 / 140713780)
which was also detected by Swift (Mangano et al. 2014, GCN 16581).
The GBM on-ground location, using the Fermi GBM trigger data,
is consistent with the Swift/BAT location.

The angle from the Fermi LAT boresight is 70 degrees.

The GBM light curve consists of two main overlapping peaks, with a
total duration of about 4.9 s (50-300keV). The time-averaged
spectrum from T0+0 s to T0+4.6 s is well fit
by a power law function with an exponential high-energy cutoff.
The power law index is -1.2 +/- 0.2 and the cutoff energy,
parameterized as Epeak, is 96 +/- 24 keV.

The event fluence (10-1000 keV) in this time interval is
(5.2 +/- 0.7)E-07 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+0 s in the 10-1000 keV band is 3.3 +/- 0.2 ph/s/cm^2.

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


GRB_name: GRB140703A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16591
SUBJECT: Radio upper limits on the GRB 140703A with the GMRT
DATE:    14/07/15 08:41:55 GMT
FROM:    Poonam Chandra at TIFR  <poonam@ncra.tifr.res.in>

A. J. Nayana (NCRA-TIFR) and Poonam Chandra (NCRA-TIFR) reports:

We carried out Giant Metrewave Radio Telescope (GMRT) observations of
GRB 140703A  (GCN 16503) in the 1390 MHz band on 2013 July 10.12 UT and 
12.91 UT,
respectively. We do not detect the radio afterglow of the GRB in this 
frequency.
The 3-sigma upper limit at the two epochs are 174 and 177 uJy, 
respectively. The map resolutions
of the two images are 2.5"x2.0" and 3.1"x2.1", respectively.

We thank GMRT staff for making these observations possible.


GRB_name: GRB140714A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16592
SUBJECT: GRB 140714A: Fermi GBM detection
DATE:    14/07/15 15:53:20 GMT
FROM:    Hoi-Fung Yu at MPE  <sptfung@mpe.mpg.de>

H.-F. Yu (MPE) reports on behalf of the Fermi GBM Team:

"At 06:25:55.42 UT on 14 July 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140714A (trigger 427011958 / 140714268).

The trigger resulted in an Autonomous Repoint Request (ARR) that was
accepted and the spacecraft slewed to the GBM in-flight location.

The on-ground calculated location, using the GBM trigger data, is 
RA = 221.0, Dec = 40.3 (J2000 degrees, equivalent to 14h 44m, 40d 18'), 
with an uncertainty of 1.1 degrees (radius, 1-sigma containment, 
statistical only; there is additionally a systematic error which is 
currently estimated to be 2 to 3 degrees).

The initial angle from the Fermi LAT boresight, using the GBM
on-ground calculated location, is 68 degrees.

The GBM light curve consists of two main emission episodes,
with a duration (T90) of about 132 s (50-300 keV).
The time-averaged spectrum from T0+100.353 s to T0+129.026 s is
well fit by a Band function with Epeak = 81.9 +/- 2.3 keV,
alpha = -0.84 +/- 0.04, and beta = -2.8 +/- 0.1.

The event fluence (10-1000 keV) in this time interval is
(1.57 +/- 0.03)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+113.794 s in the 10-1000 keV band
is 15.6 +/- 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: GRB140713A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16593
SUBJECT: GRB 140713A: CARMA mm detection
DATE:    14/07/15 18:05:41 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

B. A. Zauderer, W. Fong, and E. Berger (Harvard) report on behalf of a
larger collaboration
as part of the CARMA Key Project "A Millimeter View of the Transient
Universe":

"We observed the position of GRB 140713A (Mangano et al., GCN 16581) with
the Combined
Array for Research in Millimeter Astronomy (CARMA) beginning 2014 Jul 15.27
(dt = 0.49 d)
at a mean frequency of 85 GHz.  Observations were conducted in the compact
E configuration.
In 3.2 hours of on-source integration, we detect a radio source with a peak
brightness of
1.5 (+/- 0.3) mJy/bm at a position consistent with the enhanced Swift-XRT
position (Beardmore et al.,
GCN 16585).  We consider this source to be the putative radio afterglow.
Further observations are planned.

We thank the CARMA observers and staff for prompt execution of
these observations."


GRB_name: GRB140709A
Detection_method: AMI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16595
SUBJECT: GRB 140709A: Possible AMI 15 GHz detection
DATE:    14/07/16 17:37:37 GMT
FROM:    Gemma Anderson at U of Oxford  <gemma.anderson@astro.ox.ac.uk>

G. E. Anderson, R. P. Fender, T. D. Staley (University of Oxford),
A. J. van der Horst (University of Amsterdam), A. Rowlinson (CASS)
and C. Rumsey (MRAO)

We observed the position of GRB 140709A (GCN 16546) at 15 GHz with
the Arcminute Microkelvin Imager (AMI-LA) starting on 2014 July 11.93 to
12.10 UT, corresponding to 2.88 days post-burst. We have detected a
possible radio counterpart consistent with the UVOT-enhanced XRT position
(GCN 16548) with a preliminary flux of 0.35 +/- 0.06 mJy. However, this
source is blended with the nearby NVSS source 201841+511349 lying
at an angular distance of 27.5 arcseconds. The angular resolution of AMI
is ~30 arcseconds. The flux was calculated by first subtracting the contribution
from the NVSS source.
Earlier AMI observations an 2014 July 9.05 to 9.14 UT and July 10.04 to 10.2,
corresponding to <5 minutes and 1 day post-burst, did not detect a radio source
at the position of the GRB with 3 sigma upper limits of 0.30 and 0.21 mJy, respectively.
Further AMI monitoring is planned. We thank the AMI staff for scheduling these observations.


GRB_name: GRB140716A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16596
SUBJECT: GRB 140716A found in ground analysis of Swift-BAT data
DATE:    14/07/16 18:14:06 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings reports on behalf of the Swift science team:

At2014-07-16T10:27:57.3 Swift-BAT rate-triggered on the first episode of GRB 140716.

A sub-threshold peak in the image was found for trigger # 604792 at
RA, Dec 108.146,-60.130.

At 2014-07-16T10:29:26.4, BAT triggered on a second episode. A sub-threshold peak in
the image for trigger # 604793 was found at RA, Dec 108.175,-60.153.

A combined image shows a bright peak at RA, Dec 108.133 -60.150, which is

RA (J2000)    07h 12m 31.9s
Dec (J2000)  -60d 08' 59"

with an estimated 90% confidence radius of 1.5 arcmin.  This is consistent with
the Fermi GBM position for trigger 427199280 reported at
http://gcn.gsfc.nasa.gov/fermi_grbs.html

The burst had three main episodes, the first 2 seconds long, the second 4 seconds long
at T+90, and the third 6 seconds long at T+100.

A Swift TOO request has been submitted.


GRB_name: GRB140716A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16598
SUBJECT: GRB 140716A BAT refined analysis
DATE:    14/07/16 22:05:17 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings, S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC),
M. Stamatikos (OSU/NASA/GSFC), J. Tueller (GSFC), T. N. Ukwatta (GWU)
on behalf of the Swift-BAT team:

We report further analysis of the ground-detected GRB 140716A (Cummings,
GCN # 16596) using 20 seconds of photon-event data that cover the first and third
peaks, and BAT survey data covering the entire burst.

The best BAT position remains RA, Dec 108.133 -60.150, which is

RA (J2000)    07h 12m 31.9s
Dec (J2000)  -60d 08' 59"

with an estimated 90% confidence radius of 1.5 arcmin.  The source was 3% coded
in BAT.

The burst had three peaks with similar maximum flux, the first 2 seconds long, the
second 4 seconds long at T+90, and the third about 8 seconds long at T+100.  The
emission was undetectable between the first and second peaks, while there was a
slight overlap between peaks 2 and 3.  The total T90 was about 104 +- 2 seconds.
At T+112 seconds, Swift executed a preplanned slew, putting the source completely
out of the BAT coded field of view, but we can say that there was no bright
emission above about 50 keV after this time.

The average spectrum from 15 to 150 keV is best fit by a simple power law function
with a photon index of 1.61 +- 0.33.  The total fluence was
(5.9 +- 1.2) x 10^-6 ergs/cm^2.  The peak 1-second flux was
5.2 +- 1.5 photons/sec/cm^2 from T+0.2 to T+1.2 seconds.  All the quoted errors are
at the 90% confidence level.

A Swift TOO request has been approved and is being executed with the target number
20390.


GRB_name: GRB140716A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16599
SUBJECT: GRB 140716A: A Fermi GBM Detection
DATE:    14/07/17 00:54:25 GMT
FROM:    Peter Jenke at MSFC  <peter.a.jenke@nasa.gov>

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

"At 10:27:57.66 UT on July 16 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140716A (trigger 427199280/140716436),
which was also detected by 
Swift (J. R. Cummings et al. 2014, GCN 16596).  
The GBM on-ground location, using the Fermi GBM trigger
data, is consistent with the Swift/BAT location. 

The angle of the burst direction to the Fermi LAT boresight
is 137 degrees.

The GBM light curve consists of one FRED-like short peak near T0 and a
longer double peak at ~T0+100s with a duration (T90) of about
106 s (50-300 keV).
The time-averaged spectrum from T0+89s to T0+108s 
is well fit by a Band function with Epeak = 92 +/- 13 keV, 
Alpha = -0.8 +/- 0.2 and Beta = -2.07 +/- 0.07.

The event fluence (10-1000 keV) in this time interval is
(1.03 +/- 0.04)E-05 ergs/cm^2. The 1.0-sec peak photon flux measured
starting from T0+100s in the 10-1000 keV band
is 11.3 +/- 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: GRB140716A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16600
SUBJECT: GRB 140716A: Swift-XRT detection of an afterglow candidate
DATE:    14/07/17 06:26:30 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page (U. Leicester) reports on behalf of the Swift-XRT team:

We have analysed 3.4 ks of XRT data for the Swift/BAT ground-detected
burst: GRB 140716A (Cummings, GCN Circ 16596; Cummings et al., GCN Circ.
16598), from 34.1 to 56.8 ks after the first of the ground-detected BAT
triggers. This burst was also detected by Fermi-GBM (Jenke & Yu, GCN Circ.
16599). The data are entirely in Photon Counting (PC) mode. We detect an
uncatalogued X-ray source with a mean count rate of 0.024 (+/- 0.003)
count s^-1, at a position of RA, Dec = 108.1731, -60.1757, which is
equivalent to:

RA (J2000):   07h 12m 41.53s
Dec (J2000): -60d 10' 32.7"

with an uncertainty of 4.7" (radius, 90% confidence). This is 1.95' from
the BAT position, a little outside the 1.5' 90% BAT error circle. We
cannot determine at the present time whether the source is fading.

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


GRB_name: GRB140716A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16601
SUBJECT: GRB 140716A: GROND afterglow candidate
DATE:    14/07/17 12:21:55 GMT
FROM:    Sebastian Schmidl at TLS Tautenburg  <schmidl@tls-tautenburg.de>

F. Knust, J. Bolmer (both MPE Garching), S. Schmidl (TLS Tautenburg), and
J. Greiner (MPE Garching) report on behalf of the GROND team:

We observed the field of GRB 140716A (Swift trigger 604792; Cummings et al.,
GCN 16596) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2m MPG telescope at ESO La Silla
Observatory (Chile).

Observations started at 10:16 UT on July 17, 2014, 23.8 hrs after
the GRB trigger. They were performed at an average seeing of 1.8" and at
an average airmass of 2.3.

We find a faint source inside the XRT error circle given in Page et al.
(GCN 16600) at coordinates

RA  (J2000) =  07:12:41.20
DEC (J2000) = -60:10:35.3

with an uncertainty of 0.5" in each coordinate.

Based on a total exposures of 264 seconds in g'r'i'z' and 240 seconds in
JHK, at a mid-time of 23.9 hrs after the burst, we measure the following
preliminary magnitudes (all in AB):

g' = 21.5 +/- 0.1,
r' = 21.0 +/- 0.1,
i' = 20.9 +/- 0.1,
z' = 20.6 +/- 0.1,
J > 20.1,
H > 19.6 and
K > 18.7.

At present we cannot decide if the source is fading.

Given magnitudes are calibrated against GROND zeropoints as well as
2MASS field stars and are not corrected for the expected Galactic
foreground extinction corresponding to a reddening of E_(B-V) = 0.13 mag
in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB140713A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16602
SUBJECT: GRB 140713A: 10.4-m GTC deep optical observation
DATE:    14/07/17 14:56:54 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

A. J. Castro-Tirado (IAA-CSIC, ISA-UMA), S. Jeong (IAA-CSIC), J. Gorosabel (IAA-CSIC, UPV-EHU) and D. Reverte (GTC, IAC), on behalf of a larger collaboration, report:

Following the detection of GRB 140713A by Swift (Mangano et al. GCN 16581), we observed the field with the 10.4m GTC telescope starting on July 16, 21:28 UT (i.e. 3.11 days postburst). In the coadded frame (900s in r) we identify in the outskirts of the enhanced Swift-XRT error box  a m_AB~24 source at RA (J2000): 18h 44m 25.48s and Dec (J2000): +59d 38' 00.5"  which we suggest as the potential host galaxy for this dark GRB, taking into account the previously reported optical limits (Cano et al. GCNC 16587) and the detection of a mm afterglow (Zauderer et al. GCN 16593).


GRB_name: GRB140713A
Detection_method: AMI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16603
SUBJECT: GRB 140713A: AMI 15 GHz detection
DATE:    14/07/17 16:14:59 GMT
FROM:    Gemma Anderson at U of Oxford  <gemma.anderson@astro.ox.ac.uk>

G. E. Anderson, R. P. Fender, T. D. Staley (University of Oxford),
A. J. van der Horst (University of Amsterdam), A. Rowlinson (CASS)

We observed the position of GRB 140713A (GCN 16581) at 15 GHz with
the Arcminute Microkelvin Imager (AMI-LA) starting on 2014 July 16.88
to 17.05 UT, corresponding to 3.1 days post-burst. We have detected the
radio counterpart (GCN 16593) with a preliminary flux of 0.66 +/- 0.07 mJy.


Earlier observations were conducted on 2014 July 13.78 to 13.87 UT and
July 14.79 to 14.96 UT, corresponding to <5 minutes and 1 day post-burst,
yielding a 3 sigma flux upper limit of 0.24 mJy and marginal detection of
0.18 +/- 0.6 mJy, respectively.


Further AMI monitoring is planned. We thank the AMI staff for scheduling these observations.


GRB_name: GRB140716A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16604
SUBJECT: GRB 140716A: Swift/UVOT Upper Limits
DATE:    14/07/17 20:23:33 GMT
FROM:    Lea Hagen at PSU  <lea.zernow.hagen@gmail.com>

L. M. Z. Hagen (PSU) and K. L. Page (U. Leicester) report on behalf
of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140716A
34072 s after the BAT trigger (Cummings, GCN Circ. 16596). No optical
afterglow consistent with the XRT candidate (Page, GCN Circ. 16600) or
GROND candidate (Knust et al., GCN Circ. 16601) 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

u (fc)           34072        34367          291        >19.17
u                40452        56904         1860        >20.20
v                40559        57641         1125        >19.52

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.131 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB140716A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16605
SUBJECT: Konus-Wind observation of GRB 140716A
DATE:    14/07/18 20:25:13 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

A long duration GRB 140716A (Swift-BAT: Cummings, GCN 16596; GCN 16598;
Fermi-GBM: Jenke and Yu, GCN 16599) triggered Konus-Wind at
T0=37676.966 s UT (10:27:56.966).

The burst light curve shows three emission episodes, the first at ~T0, 
the second double pulse episode at ~T0+90 s, and the third weak at 
~T0+167 s. The total duration of the burst is ~170 s.
The emission is seen up to ~1 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140716_T37676/

As observed by Konus-Wind, the burst
had a fluence of 9.4(-1.6,+2.2)x10^-6 erg/cm2,
and a 64-ms peak flux, measured from T0+0.354 s,
of 2.8(-0.8,+1.1)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+114.944 s)
is best fit in the 20 keV - 2 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -1.09 (-0.38,+0.51)
and Ep = 157 (-41,+84) keV (chi2 = 60/58 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.2
(chi2 = 60/57 dof)

The spectrum near the maximum count rate
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 2 MeV range
by a power law with exponential cutoff model
with  alpha = -1.09 (-0.41,+0.68)
and Ep = 196 (-72,+174) keV (chi2 = 58/58 dof).

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


GRB_name: GRB140719A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16606
SUBJECT: GRB 140719A: Swift detection of a burst
DATE:    14/07/19 06:14:30 GMT
FROM:    Rhaana Starling at U of Leicester  <rlcs1@star.le.ac.uk>

R. L. C. Starling (U Leicester), C. J. Mountford (U Leicester),
K. L. Page (U Leicester) and T. Sakamoto (AGU) report on behalf of the
Swift Team:

At 05:53:55.2 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140719A (trigger=605612).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 171.592, -50.135 which is 
   RA(J2000) = 11h 26m 22s
   Dec(J2000) = -50d 08' 03"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multiple 
structure with a duration of about 15 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 05:55:14.4 UT, 79.2 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 171.6008, -50.1350
which is equivalent to:
   RA(J2000)  = 11h 26m 24.20s
   Dec(J2000) = -50d 08' 06.1"
with an uncertainty of 2.4 arcseconds (radius, 90% containment). This
location is 20 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (1.63 x
10^21 cm^-2, Willingale et al. 2013), with an excess column of 1.1
(+1.09/-0.78) x 10^22 cm^-2 (90% confidence). 

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. Data from the 2.7'x2.7' sub-image are
not available at this time. 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 R. L. C. Starling (rlcs1 AT star.le.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB140719A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16607
SUBJECT: GRB 140719A: Enhanced Swift-XRT position
DATE:    14/07/19 10:49:35 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 962 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 140719A, 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 = 171.60118, -50.13491 which is equivalent
to:

RA (J2000): 11h 26m 24.28s
Dec (J2000): -50d 08' 05.7"

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

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

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


GRB_name: GRB140719A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16608
SUBJECT: GRB 140719A: Swift-XRT refined Analysis
DATE:    14/07/19 18:14:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 8.8 ks of XRT data for GRB 140719A (Starling  et al.
GCN Circ. 16606),  from 64 s to 24.1 ks after the  BAT trigger. The
data comprise 8 s in Windowed Timing (WT) mode (taken while Swift was
slewing), with the remainder in Photon Counting (PC) mode. The enhanced
XRT position for this burst was given by Evans et al. (GCN Circ.
16607).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=3.1 (+1.5, -0.8). At T+276 s  the decay
flattens to an alpha of -0.6 (+0.5, -0.8) before breaking again at
T+2558 s to a final decay with index alpha=0.76 (+/-0.15).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.09 (+0.23, -0.21). The
best-fitting absorption column is  2.8 (+0.9, -0.8) x 10^21 cm^-2, in
excess of the Galactic value of 1.6 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 3.5 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 (+0.9, -0.8) x 10^21 cm^-2
Galactic foreground: 1.6 x 10^21 cm^-2
Excess significance: 2.4 sigma
Photon index:      2.09 (+0.23, -0.21)

If the light curve continues to decay with a power-law decay index of
0.76, 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 4.4 x
10^-13 (6.8 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00605612.

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


GRB_name: GRB140719B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16609
SUBJECT: GRB 140719B: Swift detection of a burst
DATE:    14/07/19 21:03:42 GMT
FROM:    Rhaana Starling at U of Leicester  <rlcs1@star.le.ac.uk>

R. L. C. Starling (U Leicester), W. H. Baumgartner (GSFC/UMBC),
S. B. Cenko (GSFC), L. M. Z. Hagen (PSU),
C. J. Mountford (U Leicester), D. M. Palmer (LANL) and
T. Sakamoto (AGU) report on behalf of the Swift Team:

At 20:49:35.68 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140719B (trigger=605700).  Due to a Moon constraint, Swift 
could not slew to the burst. 
The BAT on-board calculated location is 
RA, Dec 39.738d,  -2.378d which is 
  RA(J2000) = 02h 38m 57s
  Dec(J2000) = -02d 22' 39"
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 50 sec.  The peak count rate
was ~900 counts/sec (15-350 keV), at ~2 sec after the trigger. 

Due to a Moon observing constraint, Swift cannot slew to the BAT
position until 06:44 UT on 2014 July 21. There will thus be no XRT or
UVOT data for this trigger before this time. 

Burst Advocate for this burst is R. L. C. Starling (rlcs1 AT star.le.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB140719B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16610
SUBJECT: GRB 140719B: Zadko observatory - Gingin optical observations
DATE:    14/07/20 00:16:00 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

A. Klotz, D. Turpin (IRAP-CNRS-OMP), D. Macpherson (UWA/ICRAR), D. 
Coward (UWA),
M. Boer, B. Gendre, K. Siellez, H. Dereli, O. Bardho (UNS-CNRS-OCA),
A. Williams (PO-UWA), R. Martin (PO-UWA)
report:

We imaged the field of GRB 140719B detected by SWIFT
(trigger 605700) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 85s after the GRB trigger
(33s after the notice). The elevation of the field increased from
46 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+85s to t0+145s : R > 16.5

The second image is 30.0s exposure in tracking mode:
t0+163s to t0+193s : R > 18.5

We co-added a series of exposures:
t0+163s to t0+446s : R > 19.0

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


GRB_name: GRB140719A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16611
SUBJECT: GRB 140719A: GROND Afterglow candidate
DATE:    14/07/20 07:32:00 GMT
FROM:    Jan Bolmer at MPE/Garching  <jan@bolmer.de>

J. Bolmer, F. Knust, K. Valera and J. Greiner (all MPE Garching)
report on behalf of the GROND team:

We observed the field of GRB 140719A (Swift trigger 605612; Cummings et al.,
GCN 16606) simultaneously in g'r'i'z'JHK with GROND (Greiner et al.  2008,
PASP 120, 405) mounted at the 2.2m MPG telescope at ESO La Silla
Observatory (Chile).

Observations started at 22:59 UT on July 19, 2014, 16.8 hrs after
the GRB trigger. They were performed at an average seeing of 1.1â€œ and 
at an average airmass of 1.5.

We find a faint source inside the XRT error circle given in Evans et al.
(GCN 16607) at coordinates RA, Dec = 171.60123, -50.13466, which is 
equal to:

RA  (J2000):  11:26:24.3
Dec (J2000): -50:08:04.8

with an uncertainty of 0.5 arcsec in each coordinate.

Based on a total exposures of 3000 seconds in g'r'i'z' and 1200 seconds 
in JHK, at a mid-time of 18.4 hrs after the burst, we measure the 
following preliminary magnitudes (all in AB):

g' > 25.3,
r' = 23.7 +/- 0.2,
i' = 22.9 +/- 0.2,
z' > 23.8,
J  > 21.4,
H  > 20.9 and
K  > 19.5.

At present we cannot confirm whether the source is fading.

Given magnitudes are calibrated against GROND zeropoints as well as
2MASS field stars and are not corrected for the expected Galactic
foreground extinction corresponding to a reddening of E_(B-V) = 0.12 mag
in the direction of the burst (Schlegel et al. 1998).

[GCN OPS NOTE(20jul14): Per author's request, the author list was added
and the arcsec symbol was replaced.]


GRB_name: GRB140719A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16612
SUBJECT: GRB 140719A: FTS observations
DATE:    14/07/20 11:50:28 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi, S. Dichiara (U. Ferrara), C.G. Mundell (LJMU)
on behalf of a large collaboration report:

The 2-m Faulkes Telescope South began observing Swift GRB 140719A
(Starling et al. GCN Circ 16606) on July 19 at 09:27:35 UT, i.e.
~3.6 hours after the BAT trigger, with the r' and i' filters.

Within the enhanced XRT error circle (Evans et al. GCN Circ. 16607)
and, in particular, at the position of the GROND candidate
(GCN Circ. 16611) we found nothing down to the following limit:

Mid time from  Total Exp   Filter    Magnitude
trigger (hr)   (s)
-------------------------------------------------
3.64           120x4       r'        > 21.0
3.80           120x4       i'        > 20.2
-------------------------------------------------

Magnitudes are calibrated against nearby USNO-B1 stars.


GRB_name: GRB140719A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16613
SUBJECT: GRB 140719A, Swift-BAT refined analysis
DATE:    14/07/20 13:02:06 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

T. N. Ukwatta (MSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), G. Sato (ISAS), M. Stamatikos (OSU), 
R. L. C. Starling (U Leicester), J. Tueller (GSFC),
(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 140719A (trigger #605612)
(Starling, et al., GCN Circ. 16606).  The BAT ground-calculated position is
RA, Dec = 171.571, -50.115 deg which is 
  RA(J2000)  =  11h 26m 17.1s 
  Dec(J2000) = -50d 06' 55.1" 
with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 75%.

The mask-weighted light curve shows a single peak starting at ~T-5 s sec, 
peaking at ~T+0 sec, and ending at T+20 sec.  T90 (15-350 keV) is 48 +- 23 sec 
(estimated error including systematics).

The time-averaged spectrum from T-31.5 to T+16.5 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.9 +- 0.3.  The fluence in the 15-150 keV band is 4.3 +- 0.8 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+8.01 sec in the 15-150 keV band
is 0.2 +- 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/605612/BA/


GRB_name: GRB140716A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16614
SUBJECT: GRB 140716A: GROND confirmation of the afterglow
DATE:    14/07/20 14:54:05 GMT
FROM:    Sebastian Schmidl at TLS Tautenburg  <schmidl@tls-tautenburg.de>

J. Bolmer, F. Knust (both MPE Garching), S. Schmidl (TLS Tautenburg), and
J. Greiner (MPE Garching) report on behalf of the GROND team:

We re-observed the field of GRB 140716A (Swift trigger 604792; Cummings et
al., GCN 16596) simultaneously in g'r'i'z'JHK with GROND (Greiner et al.
2008, PASP 120, 405) mounted at the 2.2m MPG telescope at ESO La Silla
Observatory (Chile).

Observations started on July 20, 2014, at 09:47 UT, 3.97 days after the
GRB trigger. They were performed at an average seeing of 1.8" and at an
average airmass of 2.3.

Based on a total exposure of 1782 seconds in g'r'i'z', we measure for the
optical afterglow candidate reported by Knust et al. (GCN
#16601) the following preliminary magnitudes (all AB):

g' = 22.9 +/- 0.2 mag,
r' = 22.0 +/- 0.1 mag,
i' = 21.7 +/- 0.2 mag and
z' = 21.2 +/- 0.2 mag.

Compared to the first-epoch observations the source has faded in all
bands, confirming that this is the optical afterglow of GRB 140716A.

Given magnitudes are calibrated against GROND zeropoints and are not
corrected for the expected Galactic foreground extinction corresponding to
a reddening of E_(B-V) = 0.13 mag in the direction of the burst (Schlegel
et al. 1998).


GRB_name: GRB140719B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16615
SUBJECT: GRB 140719B, Swift-BAT refined analysis
DATE:    14/07/21 06:18:24 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

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

Using the data set from T-240 to T+962 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140719B (trigger #605700)
(Starling, et al., GCN Circ. 16609).  The BAT ground-calculated position is
RA, Dec = 39.731, -2.384 deg which is
   RA(J2000)  =  02h 38m 55.4s
   Dec(J2000) = -02d 23' 03.5"
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 42%.

The mask-weighted light curve shows a single peak starting at ~T-18 s sec,
peaking at ~T+2 sec, and ending at ~T+60 sec.
T90 (15-350 keV) is 53.0 +- 13.5 sec (estimated error including systematics).

The time-averaged spectrum from T-17 to T+49 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.8 +- 0.2.  The fluence in the 15-150 keV band is 1.3 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-4.97 sec in the 15-150 keV band
is 0.7 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/605700/BA/


GRB_name: GRB140716A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16616
SUBJECT: GRB 140716A: Confirmation of the Swift-XRT afterglow
DATE:    14/07/21 13:54:29 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page (U. Leicester) reports on behalf of the Swift-XRT team:

Following the detection of an X-ray afterglow candidate for GRB 140716A
(Page, GCN Circ. 16600), Swift obtained a second epoch of observations
starting 357 ks after the BAT detection.

The X-ray source has now faded to a level of (1.4 +0.8/-0.6) x 10^-3 count
s^-1, and the light curve can be modelled with a power-law decay with a
decay index of alpha=1.16 (+0.39, -0.27). We therefore confirm that this
is the X-ray afterglow of GRB 140716A.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020390.

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


GRB_name: GRB140721A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16617
SUBJECT: GRB 140721A: Fermi GBM detection
DATE:    14/07/21 16:18:54 GMT
FROM:    Hoi-Fung Yu at MPE  <sptfung@mpe.mpg.de>

H.-F. Yu (MPE) reports on behalf of the Fermi GBM Team:

"At 08:03:22.32 UT on 21 July 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140721A (trigger 427622605 / 140721336).

The on-ground calculated location, using the GBM trigger data, is 
RA = 175.7, Dec = -41.2 (J2000 degrees, equivalent to 11h 42m 48s, 
-41d 12'), with an uncertainty of 1.0 degrees (radius, 1-sigma
containment, statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).

The angle from the Fermi LAT boresight is 118 degrees.

The GBM light curve shows a multi-pulse feature with a duration
(T90) of about 128 s (50-300 keV). The time-averaged spectrum from 
T0-6.400 s to T0+84.737 s is well fit by a Band function with 
Epeak = 129.0 +/- 10.2 keV, alpha = -1.05 +/- 0.05, 
and beta = -1.98 +/- 0.03.

The event fluence (10-1000 keV) in this time interval is
(4.95 +/- 0.08)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+18.752 s in the 10-1000 keV band
is 14.0 +/- 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: GRB140719A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16618
SUBJECT: GRB 140719A: Swift/UVOT Upper Limits
DATE:    14/07/21 21:41:59 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and R. L. C. Starling (U. Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140719A
83 s after the BAT trigger (Starling et al., GCN Circ. 16606).
No optical afterglow consistent with the optical position
(Bolmer et al. GCN Circ. 16611) or the enhanced XRT position
(Evans et al. GCN Circ. 16607) is detected in the initial UVOT exposures.
Nearby bright sources in this crowded field make estimating the
background more difficult than usual.
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            83          233          147         >20.9
u_FC               296          546          246         >20.2
white               83         1026          334         >21.3
v                  626         4558          178         >19.2
b                  552          745           39         >19.5
u                  296          720          265         >20.2
w1                 676          870           39         >19.0
m2                 651          845           39         >21.0
w2                 602         1052           58         >19.0

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.14 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB140719B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16619
SUBJECT: GRB 140719B: Swift XRT observation
DATE:    14/07/22 06:09:24 GMT
FROM:    Rhaana Starling at U of Leicester  <rlcs1@star.le.ac.uk>

R. L. C. Starling (U. Leicester) reports on behalf of the Swift-XRT team:

Swift slewed to GRB 140719B (trigger=605700, Starling et al. GCN Circ. 16609) on 2014-07-21,
delayed due to a moon constraint.
Observations with the XRT began at 07:59:24UT and comprised a total of 6.87 ks in photon counting
mode spanning 126.6 - 140.1 ks after the BAT trigger. We do not detect any X-ray sources within the
BAT refined error circle (Barthelmy et al. GCN Circ. 16615), and place a 3-sigma upper limit on the
count rate at the BAT position of 0.003 count s^-1.

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


GRB_name: GRB140721A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16620
SUBJECT: IPN Triangulation of GRB 140721A
DATE:    14/07/22 20:41:48 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

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

G. Di Cocco, F. Fuschino, M. Galli, C. Labanti, and M. Marisaldi, on
behalf of the AGILE MCAL 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

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

The long-duration GRB 140721A (Yu, GCN Circ. 16617) has been observed by 
Konus-Wind, Fermi(GBM trigger 427622605), MESSENGER (GRNS), AGILE (MCAL) 
and INTEGRAL (SPI-ACS), so far, at about 29002 s UT (08:03:22).

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   177.645 (11h 50m 35s) -37.735 (-37d 44' 06")
  Corners:
   181.410 (12h 05m 38s) -30.317 (-30d 19' 01")
   172.431 (11h 29m 43s) -44.878 (-44d 52' 41")
   174.251 (11h 37m 00s) -43.513 (-43d 30' 47")
   183.534 (12h 14m 08s) -27.322 (-27d 19' 20")
  ---------------------------------------------
The error box area is 8.7 sq. deg, and its maximum
dimension is 19.7 deg (the minimum one is 0.52 deg).

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB140721_T29009/IPN/

Details of the Konus-Wind observation will be given in a forthcoming GCN
Circular.


GRB_name: GRB140721A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16621
SUBJECT: Konus-Wind observation of GRB 140721A
DATE:    14/07/23 10:30:26 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration GRB 140721A (Fermi-GBM detection: Yu, GCN 16617;
IPN triangulation: Hurley et al., GCN 16620)
triggered Konus-Wind at T0=29009.138 s UT (08:03:29.138).

The light curve shows a multi-peaked structure which
started ~60 s before the trigger.
A total duration of the burst is ~160 s.
The emission is seen up to 5 MeV.

As observed by Konus-Wind, the burst had a fluence
of 4.7(-0.4,+0.4)x10^-5 erg/cm2, and a 64-ms peak flux,
measured from T0+10.496 s, of 5.0(-0.5,+0.5)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+98.560 s)
is best fit in the 20 keV - 10 MeV range
by the cutoff power law with the following model parameters:
the photon index alpha = -1.31(-0.11,+0.12),
and the peak energy Ep = 153(-15,+19) keV,
chi2 = 65/85 dof.
Fitting this spectrum with the Band model yields the same
values of alpha and Ep with an upper limit on beta of -2.5

The spectrum near the peak count rate (measured from T0 to T0+16.640 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.94 (-0.20,+0.24),
the high energy photon index beta = -2.15 (-0.24,+0.13),
the peak energy Ep = 166 (-29,+44) keV,
chi2 = 60/87 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140721_T29009/

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


GRB_name: GRB140709B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16622
SUBJECT: GRB 140709B: Swift/UVOT Upper Limits
DATE:    14/07/23 11:23:28 GMT
FROM:    Craig Swenson at PSU/Swift  <cswenson@astro.psu.edu>

C. A. Swenson (PSU) reports on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140709B
97 s after the BAT trigger (Swenson et al., GCN Circ. 16551).
No optical afterglow consistent with the XRT position
(Goad et al. GCN Circ. 16556)
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          4835         4985          147         >20.8
u_FC                97          346          246         >20.6
white             4835         6626          541         >21.7
v                  633         7037          491         >20.5
b                  352         6422          534         >20.9
u                   97         6216          668         >21.2
w1                 683        11259          922         >20.8
m2                1087         7230          440         >21.2
w2                 758         6832          471         >20.6

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


GRB_name: GRB140723A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16623
SUBJECT: GRB 140723A: Fermi-LAT detection
DATE:    14/07/23 14:19:02 GMT
FROM:    Elisabetta Bissaldi at U.Innsbruk/IAPP  <Elisabetta.Bissaldi@uibk.ac.at>

E. Bissaldi (University & INFN Trieste), R. Desiante (Udine
University & INFN Trieste), M. Axelsson (Stockholm University),
D. Kocevski (NASA/GSFC) and F. Piron (LUPM)
report on behalf of the Fermi-LAT team:



At UT 01:36:30.73 on July 23rd, 2014, Fermi-LAT detected
high-energy emission from GRB 140723A, which was also
detected by Fermi-GBM (trigger427772193 / 140723067).

The best LAT on-ground location is found to be

(RA, Dec) = 210.63, -3.73 (deg, J2000)

with an approximate error radius of 0.35 deg (90% containment,
statistical error only). This was 55 deg from the LAT
boresight at the time of the trigger.

An image with the 68% and 90% containment regions
have been posted at:

http://slac.stanford.edu/~bissaldi/GRB140723A_LAT_tsmap.png

The data from the Fermi-LAT show a significant increase
in the event rate that is spatially and temporally
correlated with the GBM emission with high significance.
More than 170 photons above 100 MeV and 3 photons
above 1 GeV are observed within 1200 s, before the spacecraft
entered the SAA. The source entered the FoV again around 5800 s
after the trigger. The highest-energy photon is a
1.8 GeV event, which is observed 163 s after the GBM trigger.

A Swift ToO has been requested for this burst.

The Fermi-LAT point of contact for this burst
is Elisabetta Bissaldi (Elisabetta.Bissaldi@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: GRB140723A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16624
SUBJECT: GRB 140723A Tiled Swift observations
DATE:    14/07/23 15:21:07 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 140723A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00027

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; and 2009, MNRAS, 397, 1177).

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


GRB_name: GRB140723A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16625
SUBJECT: IPN Triangulation of GRB 140723A
DATE:    14/07/23 18:20:26 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

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

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

The long-duration GRB 140723A (Bissaldi et al., GCN Circ. 16623) has 
been observed by Konus-Wind, Fermi(GBM trigger 427772193), MESSENGER 
(GRNS), and INTEGRAL (SPI-ACS), so far, at about 5791 s UT (01:36:31).

We have triangulated it to a GBM-MESSENGER annulus centered at 
RA(2000)=284.016 deg (18h 56m 04s) Dec(2000)=-22.344 deg (-22d 20' 38"), 
whose radius is 72.790 + / - 0.166 deg (3 sigma).

The LAT error circle (that is RA, Dec, RErr = 210.63, -3.73, 0.35), 
whose area is 0.4 sq. deg, is mainly outside the annulus. The distance 
between the annulus center line and the center of the LAT position is 
0.43 deg.

This localization may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB140723_T05790/IPN/


GRB_name: GRB140723A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16626
SUBJECT: GRB 140723A: Fermi GBM detection
DATE:    14/07/23 18:47:59 GMT
FROM:    Eric Burns at U of Alabama  <EricKayserBurns@gmail.com>

E. Burns (UAH) reports on behalf of the Fermi GBM Team:

"At 01:36:30.73 UT on 23 July 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140723A (trigger 427772193 / 140723067).
It was also detected by Fermi LAT (Bissaldi et al. 2014, GCN 16623).
The GBM on-ground location is consistent with the LAT position.

The GBM light curve consists of a single pulse with a duration (T90)
of about 56 s (50-300 keV). The time-averaged spectrum from T0+0.002 s
to T0+56.801 s is well fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.1 +/- 0.1 and
the cutoff energy, parameterized as Epeak, is 968 +/- 231 keV.

The event fluence (10-1000 keV) in this time interval is
(1.46 +/- 0.04)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+0.000 s in the 10-1000 keV band
is 4.8 +/- 0.2 ph/s/cm^2.

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


GRB_name: GRB140723A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16627
SUBJECT: GRB 140723A: LCO-Sutherland optical candidate
DATE:    14/07/23 22:44:56 GMT
FROM:    Simone Dichiara at Ferrara U/Italy  <dichiara@fe.infn.it>

C. Guidorzi, S. Dichiara (U. Ferrara), C.G. Mundell (LJMU)
on behalf of a large collaboration report:

We observed Fermi GRB 140723A (Bissaldi et al. GCN Circ 16623;
Burns et al. GCN Circ. 16626) with one of the Las Cumbres
Observatory 1-m telescopes in Sutherland (South Africa) on
July 23 at 16:51:02 UT, i.e. ~15.2 hours after the GBM trigger,
with the r' and i' filters.

From initial quick-look images, we identify an possible
 uncatalogued object within the LAT error circle at the
following position:

RA(J2000) = 14:02:30.25
Dec(J2000)= -03:40:21.0

with an uncertainty of 2" and R~17 mag, calibrated against
nearby USNOB1 stars.


GRB_name: GRB140723A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16628
SUBJECT: Konus-Wind observation of GRB 140723A
DATE:    14/07/24 11:27:45 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration, hard-spectrum GRB 140723A
(Fermi-LAT detection: Bissaldi et al., GCN 16623;
IPN triangulation: Hurley et al., GCN 16625;
Fermi-BBM detection: Burns, GCN 16626)
triggered Konus-Wind at T0=5790.357 s UT (01:36:30.357).

The light curve shows a single FRED-like pulse
with a total duration of ~45 s.
The emission is seen up to 10 MeV.

As observed by Konus-Wind, the burst had a fluence
of 2.3(-0.5,+0.8)x10^-5 erg/cm2, and a 64-ms peak flux,
measured from T0-0.064 s, of 5.8(-1.6,+1.9)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+33.024 s)
is best fit in the 20 keV - 15 MeV range
by the cutoff power law with the following model parameters:
the photon index alpha = -1.10(-0.20,+0.26),
and the peak energy Ep = 1142(-452,+1005) keV,
chi2 = 71/98 dof.
Fitting this spectrum with the Band model yields the same
values of alpha and Ep with an upper limit on beta of -1.9

The spectrum near the peak count rate (measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 15 MeV range
by the cutoff power law with the following model parameters:
the photon index alpha = -1.03(-0.21,+0.26),
and the peak energy Ep = 931(-287,+528) keV,
chi2 = 97/98 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140723_T05790/

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


GRB_name: GRB140723A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16629
SUBJECT: GRB 140723A: MASTER optical observation 
DATE:    14/07/24 13:49:03 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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

V.Krushinsky, I.Zalozhnih,  A. Popov
Ural Federal University, Yekaterinburg, Kourovka

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

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

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Tunka was pointed to the GRB 140723A (Fermi trigger 427772193) 
48377 s (~13.4 h) after trigger time at 2014-07-23 15:02:47 UT directly 
after sunset.  Observations were made at high zenith distance (z ~ 76d) 
with the error box setting to the horizon. Therefore we have only two 
(180s exposure) successful images.

On our images we have not found optical transient within Fermi-LAT 
error-box (Bissaldi et al. GCN 16623, Burns et. al GCN 16626) and IPN 
(Hurley et al. GCN  16625, Golenetskii et. al GCN 16628) brighter than 
18.3 mag. Thus we can not confirm the LCO-Sutherland OT (Guidorzi et al. 
GCN 16627) despite ~2 hours earlier time of observations and our upper 
limit being 1 magnitude deeper than the estimated  object magnitude.

The 6x6 acrminutes MASTER-Tunka image around probable OT position (Guidorzi et 
al. GCN 16627) is available here:
http://master.sai.msu.ru/static/GRB/GRB140723_LAT.png

Our white (clear) band is well described by a parity 0.8R+0.2B (USNO B1).

The message may be cited.


GRB_name: GRB140723A
Detection_method: retraction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16630
SUBJECT: GRB 140723A: LCO-Sutherland optical candidate retraction
DATE:    14/07/24 13:53:49 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi, S. Dichiara (U. Ferrara), C.G. Mundell (LJMU)
on behalf of a large collaboration report:

 From the analysis of the finally reduced frames we retract the
uncatalogued source reported in our previous message
(GCN Circ. 16627) as the possible optical afterglow candidate
to GRB 140723A. The source turned out to be not real.
We apologise for the confusion.


GRB_name: GRB140723A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16631
SUBJECT: GRB 140723A: Swift-XRT and UVOT observations
DATE:    14/07/25 13:23:29 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia (ASDC), L. Izzo (URoma/ICRA), A. Breeveld (UCL-MSSL), P.  
Evans (U. Leicester) report on behalf of the Swift team:

Swift began observing the field of GRB 140723A on 2014-07-23 at 15:20  
UT, 49 ks after the LAT trigger (Bissaldi et al., GCN Circ. 16623). A  
tiled observation of four contiguous fields centered on the LAT >  
coordinates has been secured. The total integration time is 3 ks, >  
i.e., about 750 s per field. Our mosaic covers more than 90% of the  
LAT error circle (Bissaldi et al., GCN Circ. 16623), but less than 10%  
of the observed area lies within the IPN error localization, published  
after our observation began (Hurley et al., GCN Circ. 16625).

In the XRT exposure, we do not find any new source, down to a three  
sigma upper limit of 1.4E-02 cts/s. In the UVOT u-band data we do not  
find any new source down to a three sigma upper limit of about 20.2 mag.

This circular is an official product of the Swift team.


GRB_name: GRB140729A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16633
SUBJECT: GRB 140729A: Fermi-LAT detection
DATE:    14/07/29 09:10:16 GMT
FROM:    Makoto Arimoto at Tokyo Inst of Tech  <arimoto@hp.phys.titech.ac.jp>

M. Arimoto (Tokyo Tech) and E. Bissaldi (University & INFN Trieste)
report on behalf of the Fermi-LAT team:


At UT 00:36:59 on July 29th, 2014, Fermi-LAT detected
high-energy emission from GRB 140729A, which was also
detected by Fermi-GBM (trigger 140729026 / 428287016).

The best LAT on-ground location is found to be

(RA, Dec) = 193.95, +15.35 (deg, J2000)

with an approximate error radius of 0.34 deg (90% containment,
statistical error only).
This was 26.2 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 GBM emission with high significance.
More than 100 photons above 100 MeV and 13 photons
above 1 GeV are observed within 550 s, before the
spacecraft entered the SAA.
The GRB does not come back into the Fermi-LAT FoV for more than 6000s.
The highest-energy photon is a 1.3  GeV event
which is observed 44 s after the GBM trigger.


A Swift ToO has been requested for this burst.


The Fermi-LAT point of contact for this burst is
Makoto Arimoto (arimoto@hp.phys.titech.ac.jp).

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: GRB140729A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16634
SUBJECT: GRB 140729A Tiled Swift observations
DATE:    14/07/29 10:13:11 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 140729A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00028

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; and 2009, MNRAS, 397, 1177).

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


GRB_name: GRB140729A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16636
SUBJECT: GRB 140729A: Fermi-GBM detection
DATE:    14/07/29 17:04:22 GMT
FROM:    Matthew Stanbro at UAH/Fermi  <mcs0001@uah.edu>

M. Stanbro (UAH) reports on behalf of the Fermi GBM Team:

"At 00:36:53.71 UT on 29 July 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140729A (trigger 428287016 / 140729026).
It was also detected by Fermi LAT (Arimoto et al. 2014, GCN 16633).
The GBM on-ground location is consistent with the LAT position.

The GBM light curve consists of a single pulse with a duration (T90)
of about 78 s (50-300 keV). The time-averaged spectrum from T0+0.0 s
to T0+78.3 s is well fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.9 +/- 0.1 and
the cutoff energy, parameterized as Epeak, is 866 +/- 162 keV.

The event fluence (10-1000 keV) in this time interval is
(1.70 +/- 0.06)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+3.328 s in the 10-1000 keV band
is 4.5 +/- 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: GRB140729A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16637
SUBJECT: IPN Triangulation of GRB 140729A
DATE:    14/07/29 17:57:46 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

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

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

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

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

The long-duration GRB 140729A (Arimoto and Bissaldi, GCN Circ. 16633)
has been observed by Konus-Wind, Fermi(GBM trigger 428287016),
MESSENGER (GRNS), Swift (BAT), and INTEGRAL (SPI-ACS), so far,
at about 2214 s UT (00:36:54). The burst was outside the coded
field of view of the BAT.

We have triangulated it to a GBM-MESSENGER annulus centered at
RA(2000)=115.909 deg (07h 43m 38s)  Dec(2000)=+22.015 deg (+22d 00' 
52"), whose radius is 73.685 +/- 0.219 deg (3 sigma).

This annulus intersects the Fermi-LAT 1 sigma error
circle (GCN 16633) to form an error box whose area is about
(654 sq. arcmin.) which is two times smaller than that
of the LAT error circle.

This localization may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB140729A/IPN/

Details of the Konus-Wind observation will be given in a forthcoming GCN
Circular.


GRB_name: GRB140729A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16638
SUBJECT: GRB 140729A: Swift-XRT and UVOT observations
DATE:    14/07/29 18:24:40 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo (INAF-OAB), F. E. Marshall (NASA/GSFC), M. G. Bernardini (INAF-OAB), P. A. Evans (U. Leicester) report on behalf of the Swift team:

Swift began observing the field of GRB 140729A (Arimoto et al., GCN Circ. 16633; Stanbro, GCN Circ. 16636) on 2014-07-29 at 10:12  UT, 34.5 ks after the LAT trigger (Arimoto et al., GCN Circ. 16633). A tiled observation of four contiguous fields centered on the LAT coordinates has been secured. The total integration time is 3.8 ks, i.e., about 1 ks per field. Our mosaic covers about 90% of the LAT error circle (Arimoto et al., GCN Circ. 16633)  and about 50% of the observed area lies within the IPN error localization, published after our observation began (Hurley et al. GCN Circ 16637).

In the XRT exposure, we do not find any new source, down to a three sigma upper limit of 9e-03 cts/s. 

UVOT observed the four fields using the U filter. No new source was found down to a 90%-confidence upper limit of about 20.0 mag. No correction is made for the Galactic extinction due to the reddening of E(B-V) = 0.02 in the direction of the burst (Schlegel et al. 1998).

This circular is an official product of the Swift team.


GRB_name: GRB140729A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16640
SUBJECT: GRB 140729A: iPTF optical upper limit
DATE:    14/07/30 04:32:40 GMT
FROM:    Leo Singer at CIT/PTF  <lsinger@caltech.edu>

L. P. Singer (Caltech), S. B. Cenko (NASA/GSFC), and M. M. Kasliwal
(Carnegie Observatories/Princeton) report on behalf of the
intermediate Palomar Transient Factory (iPTF) collaboration:

We searched for optical counterparts of GRB 140729A (Arimoto, GCN 16633;
Bissaldi, GCN 16635; Stanbro, GCN 16636) using the Palomar 48-inch
Oschin telescope (P48). Based on the final Fermi GBM localization
with a 1-sigma statistical radius of 1.57 deg, we imaged 10 fields
covering an area of 73 deg2. These fields also contained all of the
Fermi LAT error circle and its intersection with the IPN annulus
(Svinkin, GCN 16637).

In our observations on 2014-07-29 from 04:05:50 to 04:51:48 UT (3.48
to 4.5 hours after the burst), we find no plausible optical afterglow
candidates within the LAT error circle, to a limiting magnitude of
R=20.6.

The diagram http://www.its.caltech.edu/~lsinger/iptf/Fermi428287016.pdf
shows the locations of our ten P48 fields in relation to the Fermi
GBM 1- and 2-sigma statistical+systematic contours as well as the LAT
error circle and the IPN annulus.


GRB_name: GRB140713A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16641
SUBJECT: Radio upper limit on the GRB 140713A with the GMRT
DATE:    14/07/30 09:01:49 GMT
FROM:    Poonam Chandra at TIFR  <poonam@ncra.tifr.res.in>

Poonam Chandra (NCRA-TIFR) and A. J. Nayana (NCRA-TIFR)  report on behalf
of a larger collaboration:

We carried out the Giant Metrewave Radio Telescope (GMRT) observations of
GRB 140713A  (GCN Circ. 16581) in the 1390 MHz band on 2014 July 24.86 UT.
We do not detect the radio afterglow of the GRB. The 3-sigma upper limit
at the GRB position (GCN Circ. 16585) is 114 uJy and the map resolution is
"3.53 x 1.96".

We thank GMRT staff for making these observations possible.

-- 

**********************************************************************
Poonam Chandra                          +91 20 2571 9290 (Off)
National Centre for Radio Astrophysics  +91 20 2569 7257 (Fax)
Tata Institute of Fundamental Research  poonam@ncra.tifr.res.in
Post Bag 3, Pune University campus    www.ncra.tifr.res.in:8081/~poonam/
Ganeshkhind, Pune 411 007, INDIA


GRB_name: GRB140730A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16642
SUBJECT: GRB 140730A: Swift detection of a burst
DATE:    14/07/30 20:04:06 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

C. B. Markwardt (NASA/GSFC), M. G. Bernardini (INAF-OAB),
P. D'Avanzo (INAF-OAB), N. Gehrels (NASA/GSFC),
F. E. Marshall (NASA/GSFC), A. Melandri (INAF-OAB) and
D. M. Palmer (LANL) report on behalf of the Swift Team:

At 19:43:51 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140730A (trigger=607742).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 56.431, -66.539 which is 
   RA(J2000) = 03h 45m 43s
   Dec(J2000) = -66d 32' 19"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 5 sec (FWHM ~2-3 sec)  The peak 
count rate was ~1800 counts/sec (15-350 keV), at ~1 sec after the 
trigger. 

The XRT began observing the field at 19:44:55.1 UT, 63.8 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 56.39573, -66.54597 which is equivalent
to:
   RA(J2000)  = 03h 45m 34.98s
   Dec(J2000) = -66d 32' 45.5"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 56 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 7.59
x 10^20 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White
filter  starting 68 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 0.09. 

Burst Advocate for this burst is C. B. Markwardt (Craig.Markwardt 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.)


