# GCN_circulars

GRB_name: GRB140330A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16062
SUBJECT: Retraction of the Fermi/LAT high-energy counterpart for GRB 140330A
DATE:    14/03/31 19:47:21 GMT
FROM:    Giacomo Vianello at SLAC  <giacomov@slac.stanford.edu>

G. Vianello (Stanford U.), D. Kocevski (NASA/Goddard), J. Racusin
(NASA/Goddard), R. Ojha (NASA/GSFC/UMBC/CRESST) <Roopesh.Ojha@gmail.com>,
and S. Ciprini (ASDC) report on behalf of the Fermi-LAT team:

The analysis of new data downloaded from Fermi has shown that emission from
the proposed high-energy counterpart of GRB 140330A (Vianello et al., GCN
16048; Pittori et al., GCN 16058) has continued up to at least 40 ks after
the GBM trigger. This is very unusual for a faint burst such as GRB
140330A. Also, our localization of the LAT excess has improved, and it is
now:

R.A., Dec. = 325.40, -64.13 with an error radius of 0.14 (90 % c.l.,
statistical only),

which is well outside the IPN error box (Hurley et al., GCN 16051).

Moreover, a search in Fermi archival data has shown a variable emission
from a source compatible with our position, which was detected in several
occasions in 2012 and 2013, and also detected on March 28 and 29, 2014.
This source has been tentatively associated with the extra-galactic radio
source PKS 2136-642 in the past (ATel #5695; Mauch et al. 2003, MNRAS, 342,
1117).

Therefore, we believe that the high-energy source detected by Fermi and by
AGILE (Pittori et al., GCN 16058) is unrelated to GRB 140330A.

Further analysis is ongoing.

[GCN OPS NOTE(01apr14): Per author's request, the "130330A" was changed
to "140330A" in the Subject-line iand the 1st & 3rd paragraphs.]


GRB_name: GRB140331A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16063
SUBJECT: GRB 140331A: Swift-BAT refined analysis
DATE:    14/03/31 21:40:07 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), D. M. Palmer (LANL),
T. Sakamoto (AGU), J. Tueller (GSFC), T. N. Ukwatta (MSU), B.-B. Zhang (UAH)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+827 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 140331A (trigger #594081)
(Zhang, et al., GCN Circ. 16049).  The BAT ground-calculated position is
RA, Dec = 134.860, 2.755 deg, which is 
   RA(J2000)  =  08h 59m 26.4s 
   Dec(J2000) = +02d 45' 19.5" 
with an uncertainty of 3.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 98%.
 
The mask-weighted light curve shows a long weak peak starting
at ~T+70 sec and ending at around T+350 sec.  T90 (15-350 keV)
is 209 +- 33 sec (estimated error including systematics).
 
The time-averaged spectrum from T87.28to T+321.14 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.01 +- 0.29.  The fluence in the 15-150 keV band is 6.7 +- 1.3 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+292.49 sec in the 15-150 keV band
is 0.31 +- 0.13 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/594081/BA/


GRB_name: GRB140301A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16064
SUBJECT: GRB 140301A: Zadko observatory - Gingin optical observations
DATE:    14/03/31 22:30:21 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 140301A detected by SWIFT
(trigger 589590) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 70.7s after the GRB trigger
(40.5s after the notice). The elevation of the field was at
26 degrees above horizon and weather conditions
were good. Images were retrieved 30 days after their
acquisitions due to a storage software 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+70.7s to t0+130.7s : Rlim = 18.4

The second image is 30.0s exposure in tracking mode:
t0+159s to t0+189s : Rlim = 19.7

We co-added series of unfiltered exposures.
The OT discovered by Kruehler et al. (GCNC 15899)
is marginally detected 841 s (+/-255 s) after
the trigger. More precisely the photometry is:

=start= =end=
  159 s   275 s  CRlim = 21.8
  289 s   465 s  CRlim = 21.8
  586 s  1096 s  CR = 21.7 +/- 0.4
1217 s  1727 s  CRlim = 21.9

This suggests this faint afterglow had culminated in
brightness R=21.7 at t0+841s. Then it had declined
to R=23.1 at t0+4.97h (Kruehler et al. GCN 15899)
and to r'=23.8 at t0+11h (Elliott et al. GCNC 15904).
This is compatible with a temporal decay of ~0.5.

A photometry follow-up was performed with the Zadko
telescope :

=start= =end=
20.4 h  20.8 h  CRlim = 22.2

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


GRB_name: GRB140331A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16065
SUBJECT: GRB 140331A: Swift-XRT refined Analysis
DATE:    14/04/01 00:20:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 8.0 ks of XRT data for GRB 140331A (-B. Zhang et al.
GCN Circ. 16049),  from 374 s to 42.6 ks after the  BAT trigger. The
data comprise 118 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. 16052).

The light curve can be modelled with an initial power-law decay with an
index of alpha=3.57 (+0.22, -0.19), followed by a break at T+1389 s to
an alpha of 0.69 (+/-0.09).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.97 (+0.13, -0.12). The
best-fitting absorption column is  6.3 (+2.9, -2.0) x 10^20 cm^-2,
consistent with the Galactic value of 4.4 x 10^20 cm^-2 (Willingale et
al. 2013). The PC mode spectrum has a photon index of 1.90 (+0.16,
-0.11) and a best-fitting absorption column of 4.8 (+3.7, -0.4) x 10^20
cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.4 x 10^-11 (3.8 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.8 (+3.7, -0.4) x 10^20 cm^-2
Galactic foreground: 4.4 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.90 (+0.16, -0.11)

If the light curve continues to decay with a power-law decay index of
0.69, the count rate at T+24 hours will be 0.011 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.8 x
10^-13 (4.2 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00594081.

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


GRB_name: GRB140330A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16066
SUBJECT: GRB 140330A: Fermi GBM observation
DATE:    14/04/01 03:24:44 GMT
FROM:    Veronique Pelassa at UAH  <vero.pelassa@gmail.com>

V. Pelassa (UAH), G. Fitzpatrick (UCD), C. Meegan and N. Bhat (UAH)
report on behalf of the Fermi GBM Team:

"At 04:19:54.47 UT on 30 March 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140330A (trigger 417845997 / 140330180),
which was also detected by Konus-Wind (S. Golenetskii et al, GCN 16056)
and localized by the Interplanetary Network (K. Hurley et al, GCN 16051).
The GBM on-ground location is consistent with the IPN location.
The angle from the Fermi LAT boresight is 13.6 degrees.

The GBM light curve consists of a FRED pulse with a duration (T90)
of about 34 s (50-300 keV).

The time-averaged spectrum from T0-0.768 s to T0+35.073 s is
well fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.66 +/- 0.10 and
the cutoff energy, parameterized as Epeak, is 197 +/- 17 keV.
(Castor statistics 578.62 for 486 d.o.f.).
A Band function fits the spectrum equally well (Castor statistics
577.22 for 485 d.o.f.) with Epeak= 172 +/- 23 keV,
alpha = -0.57 +/- 0.13 and beta = -2.4 +/- 0.3.
This result is consistent with the analysis of the Konus observation
(S. Golenetskii et al, GCN 16056).

The event fluence (10-1000 keV) in this time interval is
(5.6 +/- 0.3)E-06  erg/cm^2. The 1-sec peak photon flux measured
starting from T0+0.640 s in the 10-1000 keV band
is 4.3 +/- 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: GRB140219A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16067
SUBJECT: GRB 140219A: Correction to GCN 15885 (Suzaku-WAM fluence)
DATE:    14/04/01 12:03:07 GMT
FROM:    Kazutaka Yamaoka at Nagoya U  <yamaoka@stelab.nagoya-u.ac.jp>

W. Iwakiri (RIKEN), M. Tashiro, Y. Terada, T. Yasuda, Y. Ishida, H. Ueno,
S. Sugimoto, S. Koyama, S. Takeda, T. Nagayoshi (Saitama U.),
M. Yamauchi, N. Ohmori, M. Akiyama, R. Kinoshita (Univ. of Miyazaki),
M. Ohno, K. Takaki, T. Kawano, R. Nakamura, 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 quoted fluence in GCN 15885 was incorrect.
The correct value is 1.73 (+0.06,-0.08)x10^-4 erg/cm^2
in the 100-1000 keV range.

We apologize for any inconvenience.


GRB_name: GRB140402A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16069
SUBJECT: GRB 140402A: Fermi-LAT detection of a burst
DATE:    14/04/02 07:45:08 GMT
FROM:    Elisabetta Bissaldi at U.Innsbruk/IAPP  <Elisabetta.Bissaldi@uibk.ac.at>

E. Bissaldi (University & INFN Trieste), G. Vianello (Stanford U.)
J. Chiang (KIPAC/SLAC) report on behalf of the Fermi-LAT team:


At 00:10:07.00 on April 02, 2014, Fermi-LAT detected
high-energy emission from GRB 140402A,
which was also detected by Fermi-GBM (trigger 418090209/140402007).

The best LAT on-ground location is found to be

RA, Dec  207.47, 5.87 (J2000)

with an error radius of 0.20 deg
(90% containment, statistical error only).
This position was 13 deg from the LAT boresight
at the time of the trigger and is consistent
with the last GBM ground location.

The data from the Fermi-LAT show a significant increase
in the event rate within 10 degrees of the GBM location
after the GBM trigger that is spatially and temporally
correlated with the GBM emission with high significance.
More than 10 photons above 100 MeV
are observed within 800 seconds.
The highest-energy photon is a 3.5 GeV event which is
observed 6.8 seconds after the GBM trigger.
These numbers may increase as more data become
available.

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: GRB140402A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16070
SUBJECT: GRB 140402A: Fermi GBM detection
DATE:    14/04/02 14:29:06 GMT
FROM:    Hoi-Fung Yu at MPE  <sptfung@mpe.mpg.de>

Subject: GRB 140402A: Fermi GBM detection

Peter A. Jenke (UAH) and Hoi-Fung Yu (MPE)
report on behalf of the Fermi GBM Team:

"At 00:10:07.00 UT on 02 April 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140402A (trigger 418090209 / 140402007).
It was also detected by Fermi/LAT (Bissaldi et al. 2014, GCN 16069).
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 0.3 s (50-300 keV). The time-averaged spectrum from T0-0.064 s
to T0+0.064 s is well fit by a simple power law function with index -1.2 +/- 0.1.

The event fluence (10-1000 keV) in this time interval is
(4.0 +/- 0.4)E-07 erg/cm^2. The 64 ms peak photon flux measured
starting from T0-0.064 s in the 10-1000 keV band is 4.6 +/- 0.7 ph/s/cm^2.

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


GRB_name: GRB140402A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16071
SUBJECT: GRB 140402A: Marginal BAT detection
DATE:    14/04/02 14:44:10 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings, S. Barthelmy (GSFC), Hans Krimm (USRA/GSFC)
  on behalf of the Swift-BAT team

At 00:10:06 Swift-BAT triggered on GRB 140402A(trigger # 594308), also seen by
FERMI-LAT (Bissaldi et al. GCN Circ #16069) and Fermi-GBM (Jenke & Yu, GCN Circ
#16070) .  There is a marginal BAT source (6 sigma), which is consistent with
the Fermi-LAT position, at RA, Dec 207.651, +6.006, which is:

RA (J2000) 13h 50m 36.2s
Dec (J2000) 06d 00m 22s

with an estimated 90% uncertainty radius of 4 arcmin.  The partial coding was
73% (i.e. all of the Fermi-LAT error circle was in a fairly highly coded part
of BAT's field of view).  This burst appears to have a very hard spectrum.
We may be able to improve the detection when we receive the photon event data.

The unweighted lightcurve shows a single peak of about 0.32 seconds duration.

A previous Swift TOO at the Fermi-LAT position did not cover this position.
A new TOO has been requested.


GRB_name: GRB140402A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16072
SUBJECT: GRB 140402A : Xinglong TNT upper limit
DATE:    14/04/02 18:10:55 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

L. P. Xin,   M. Zhai,  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 140402A  (Bissaldi  et al.,  
GCN 16069;  Peter et al, GCN 16070; Cummings et al., 
GCN 16071)  under  cloudy weather, with Xinglong 
0.8-m TNT telescope at 16:04:37 (UT) , 15.95 hrs after the burst.

No any new source in our 10*300 sec combined images 
down to the upper limit of 19.2 mag in R band, calibrated by 
nearby USNO B1.0 R2 mag.


GRB_name: GRB140402A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16073
SUBJECT: GRB 140402A BAT refined analysis
DATE:    14/04/03 01:53:53 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings on behalf of the BAT team

Based on 10 seconds of photon event data, we present refined analysis of
the BAT data on GRB 140402A (Bissaldi et al. GCN Circ #16069, Cummings
et al. GCN Circ #16071).

The best BAT location is RA, Dec 207.592, +5.971, which is:

RA(J2000) 13h 50m 22.2s
Dec(J2000) 05d 58' 16"

with an estimated 90% confidence radius of 2.8 arcmin.  This is 4 arcmin
from the previously reported BAT position based on the immediately
transmitted data (4 arcmin estimated 90% error), and 9.5 arcmin from the
Fermi-LAT position (12 arcmin estimated statistical 90% error).

The mask-weighted lightcurve shows a single nearly square pulse. T90
was about 0.031 +/- 0.003 seconds (estimated 90% confidence).

A powerlaw fit to the spectrum from 15 to 150 keV has a photon index of
0.89 +/- 0.44 (90% confidence). In 0.034 seconds the fluence was
(3.8 +/- 1.2) x 10^-8 ergs/cm^2 (62% confidence).


GRB_name: GRB140402A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16074
SUBJECT: GRB 140402A: MASTER optical observations
DATE:    14/04/03 11:53:03 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

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

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

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

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

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

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

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Blagoveschensk was pointed to the  GRB140402A (Jenke et. al GCN 
16070) ~ 13.6h  (49103 sec) after trigger time at 2014-04-02 13:48:30 UT 
directly after sunset and the weather conditions became good.
We haven't found optical transient  within Fermi-LAT  (Bissaldi et. al. 
GCN 16069)  and SWIFT-BAT (Cummings et. al GCN 16073) error-boxes on 
single and coadd images.
The 5-sigma unfiltered upper limit has been about 18.2 mag on single (180 
s) image and about 19.8 on coadd of 10 images with total exposure 1800 s.

Also MASTER II  robotic telescope  located in Kislovodsk was twice pointed 
to this GRB by FERMI-GBM two alert coordinates 23 s and ~ 1h after trigger 
time. But the final Fermi-LAT and SWIFT-BAT position is out of our FOV due 
to big coordinates errors.

The message may be cited.


GRB_name: GRB140402A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16075
SUBJECT: GRB 140402A: Swift-XRT observations
DATE:    14/04/03 16:28:34 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

C. Pagani (U. Leicester) reports on behalf of the Swift team:

We report on Swift-XRT observations of the Fermi/GBM and
Fermi/LAT-detected GRB 140402A (Jenke & Yu, GCN Circ. 16070; Bissaldi,
Vianello & Chiang, GCN Circ. 16069).

The XRT observations consist of two pointings, the first centred on the
reported Fermi/LAT GRB position (Bissaldi et al., GCN Circ. 16069), the
second on the position derived from ground analysis of Swift-BAT data
(Cummings, GCN Circ. 16071).

The first XRT pointing consists of 4.5 ks of Photon Counting (PC) mode
data, from 33.3 ks to 51.2 ks after the Fermi/LAT trigger, and is centred
on the LAT position. No source is detected in the XRT data. The 3-sigma
upper limit on the count rate is 3.6E-03 cts/s, which is 1.8E-13 erg cm^-2
s^-1 using a typical flux conversion of 5E-11 erg cm^-2 count^-1. These
data only partially cover the BAT refined error circle (Cummings, GCN
Circ. 16073).

The second XRT pointing consists of 4.9 ks of PC mode data, from 56 ks to
107 ks after the Fermi/LAT trigger, and is centred on the BAT position. No
source is detected in the XRT data. The 3-sigma upper limit on the count
rate is 3.0E-03 cts/s, which is 1.5E-13 erg cm^-2 s^-1 using a typical
flux conversion of 5E-11 erg cm^-2 count^-1.

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


GRB_name: GRB140331A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16076
SUBJECT: GRB 140331A: Continued RATIR Optical and NIR Observations
DATE:    14/04/03 18:00:59 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), Jos A. de Diego (UNAM), Leonid Georgiev (UNAM), Jess
Gonzlez (UNAM), Carlos Romn-Ziga (UNAM), Neil Gehrels (GSFC), and
Harvey Moseley (GSFC) report:

We again observed the field of GRB 140331A (Zhang, et al., GCN 16049) with
the Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on
the 1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional
on Sierra San Pedro Mrtir first from 2014/04 1.13 to 2014/04 1.37 UTC
(21.27 to 27.13 hours after the BAT trigger), obtaining a total of 3.50
hours exposure in the r and i bands and 1.46 hours exposure in the Z, Y, J,
and H bands and then from 2014/04 3.18 to 2014/04 3.36 UTC (70.39 to 74.71
hours after the BAT trigger), obtaining a total of 2.56 hours exposure in
the r and i bands and 1.07 hours exposure in the Z, Y, J, and H bands.

We do not detect statistically significant flux variation for the source
reported by Littlejohns et al. (2014, GCN 16050), which was also noted to
be coincident with an SDSS galaxy at z~0.7.  We, therefore, conclude that
this source is not the GRB afterglow (see, also, Klotz et al. 2014, GCN
6057).

We can utilize the observations reported here to estimate the limiting
magnitudes for the GRB during our first night of observations (mean time ~1
hr after the GRB).  For a source within the Swift-XRT error circle
(Beardmore et al. 2014, GCN 16052) , in comparison with the SDSS DR9 and
2MASS, we obtain the following (3-sigma) upper limits:

 r > 23.5
 i > 23.2
 Z > 21.3
 Y > 21.3
 J > 21.2
 H > 21.0

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.  The r-band limit implies a very
faint or reddened afterglow.  Our r-band limit relative to the X-ray flux
at the same epoch (e.g., D'Avanzo et al. 2014, GCN 16065) implies a
broadband spectral index beta_OX<0.3 (3-sigma), which is significantly
lower than the standard cuttoff (beta_OX<0.5) defining optically-dark GRBs
(e.g, Jakobsson et al. 2004).

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


GRB_name: GRB140402A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16077
SUBJECT: GRB 140402A: Swift/UVOT Upper Limits
DATE:    14/04/03 21:19:39 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

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

The Swift/UVOT took exposures at both the pointings for GRB140402A 
described in Pagani et al., GCN Circ. 16075. No optical afterglow 
consistent with the BAT position given by Cummings (GCN Circ. 16081) is 
detected in the UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) are:

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

white            57023        57665         632          >21.5
u                56375        61574         649          >20.5
v                57672        58344         659          >19.8

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: GRB140402A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16078
SUBJECT: GRB 140402A: Swift-XRT observations
DATE:    14/04/04 07:30:49 GMT
FROM:    Claudio Pagani at U of Leicester  <cp232@star.le.ac.uk>

C. Pagani (U. Leicester) reports on behalf of the Swift team:

We report on Swift-XRT observations of the Fermi/GBM and Fermi/LAT-detected GRB 140402A (Jenke, GCN Circ. 16070, Bissaldi, GCN Circ. 16069).

The XRT observations consist of two pointings, the first centered on the reported Fermi/LAT GRB position (Bissaldi, GCN Circ. 16069), the second on the position derived from ground analysis of Swift-BAT data (Cummings, GCN Circ. 16071).

The first XRT pointing consists of 4.5 ks of Photon Counting (PC) mode data, from 33.3 ks to 51.2 ks after the Fermi/LAT trigger and are centered on the LAT position. No source is detected in the XRT data. The 3-sigma upper limit on the count rate is 3.6E-03 cts/s, which is 1.8E-13 erg cm^-2  s^-1  using a typical flux conversion of 5E-11 erg cm^-2 count^-1. These data only partially cover the BAT refined error circle (Cummings, GCN Circ. 16073).

The second XRT pointing consists of 4.9 ks of PC mode data, from 56 ks to 107 ks after the Fermi/LAT trigger and are centered on the BAT position. No source is detected in the XRT data. The 3-sigma upper limit on the count rate is 3.0E-03 cts/s, which is 1.5E-13 erg cm^-2 s^-1  using a typical flux conversion of 5E-11 erg cm^-2 count^-1.

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


GRB_name: GRB111225A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16079
SUBJECT: GRB 111225A: Archeological redshift of the Christmas Burst 2011 from GTC
DATE:    14/04/04 11:37:47 GMT
FROM:    Christina Thoene at IAA-CSIC  <christina.thoene@gmail.com>

C.C. Thoene (IAA-CSIC) and A. de Ugarte Postigo (IAA-CSIC, DARK/NBI)
report on behalf of a larger collaboration:

We observed the Christmas burst of 2011, GRB 111225A (Siegel et al. GCN
12720), with the 10.4m GTC telescope+OSIRIS on December 25, 2011 at a mean
time 23:27 UT, 19.61 hrs after the burst. The observations consisted of
2x1800 s exposure with grism R1000B, covering the wavelength range from
3700 to 7870A with a resolution of around R=1000.

Initial analysis of the spectrum revealed continuum emission over the
complete range but no significant features neither in absorption nor
emission. However, a more careful analysis recently performed on the data
with an improved pipeline revealed faint emission features of [OII], H-beta
and [OIII], and marginal absorption of CaII at a common redshift of
z=0.297, which we therefore identify as the redshift of the GRB.

We apologise for the late notification. Better late than never.


GRB_name: GRB140402A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16080
SUBJECT: GRB 140402A: Deep limit on the optical afterglow from Magellan observations
DATE:    14/04/04 17:26:41 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

W. Fong (Harvard), S. Ehlert (MIT), D. Osip (LCO/OCIW), B. Rackham
(Arizona), M. McDonald (MIT), and E. Berger (Harvard) report:

"We observed the location of the short-duration GRB 140402A, detected by
Fermi/LAT (Bissaldi et al., GCN 16069), Fermi/GBM (Jenke et al., GCN 16070)
and Swift/BAT (Cummings et al., GCN 16071) with the Inamori Magellan Areal
Camera and Spectrograph (IMACS) mounted on the Magellan/Baade 6.5-m
telescope to cover the full refined BAT position (Cummings et al., GCN
16073). We obtained 3x300-sec r-band observations on 2014 Apr 03.22 UT
(1.21 days post-burst) in 0.7" seeing at an airmass of 1.2. To check for
the presence of a fading optical source, we re-observed the field
(3x300-sec) on 2014 Apr 04.35 UT, 2.33 days post-burst and 1.12 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
BAT-refined position. Therefore, calibrated to SDSS DR9 sources in the same
field, we place a 3-sigma limit of r>25.0 mag on the optical afterglow of
GRB 140402A at 1.21 days after the burst."


GRB_name: GRB140406A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16081
SUBJECT: GRB 140406A: Fermi GBM observation
DATE:    14/04/06 14:14:15 GMT
FROM:    Hoi-Fung Yu at MPE  <sptfung@mpe.mpg.de>

Subject: GRB 140406A: Fermi GBM observation

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

"At 03:26:48.19 UT on 06 April 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140406A (trigger 418447611 / 140406144).
This burst, tentatively classified as Unreliable Location by the FSW,
is in fact due to Gamma-Ray Burst.

The on-ground calculated location, using the GBM trigger data, is
RA = 70.1, Dec = 13.5 (J2000 degrees, equivalent to 04h 40m, 13d 30'),
with an uncertainty of 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 58 degrees.

The GBM light curve consists of several pulses with a duration (T90)
of about 42 s (50-300 keV). The time-averaged spectrum from T0-4.096 s
to T0+36.864 s is well fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.3 +/- 0.2 and the cutoff
energy, parameterized as Epeak, is 138 +/- 13 keV.

The event fluence (10-1000 keV) in this time interval is
(2.8 +/- 0.2)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+30.8 s in the 10-1000 keV band is 1.5 +/- 0.2 ph/s/cm^2.

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


GRB_name: GRB140408A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16082
SUBJECT: GRB 140408A: Swift detection of a burst
DATE:    14/04/08 13:35:46 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

V. D'Elia (ASDC), D. N. Burrows (PSU), N. Gehrels (NASA/GSFC),
S. T. Holland (STScI), L. Izzo (URoma/ICRA), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester),
D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU),
R. L. C. Starling (U Leicester) and C. A. Swenson (PSU) report on
behalf of the Swift Team:

At 13:15:54 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140408A (trigger=595141).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 290.685, -12.578 which is 
   RA(J2000)  =  19h 22m 44s
   Dec(J2000) = -12d 34' 40"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single peak
with a duration of about 10 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 13:17:40.2 UT, 105.5 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 290.71576, -12.59373 which is
equivalent to:
   RA(J2000)  = 19h 22m 51.78s
   Dec(J2000) = -12d 35' 37.4"
with an uncertainty of 4.1 arcseconds (radius, 90% containment). This
location is 122 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 109 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. Because of the density of catalogued stars,  further
analysis is required to report an upper limit for any afterglow in the
region. No correction has been made for the expected extinction
corresponding  to E(B-V) of 0.19. 

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: GRB140408A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16084
SUBJECT: GRB 140408A: Fermi GBM detection
DATE:    14/04/08 20:34:47 GMT
FROM:    Peter Jenke at MSFC  <peter.a.jenke@nasa.gov>

P. Jenke (UAH), G. Fitzpatrick (UCD) reports on behalf of the Fermi GBM Team:

"At 13:15:55.24 UT on April 8 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140408A (trigger 418655758/140408553),
which was also detected by Swift (V. D'Elia et al. 2014, GCN 16082).  
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 90 degrees.

The GBM light curve consists of one main peak with a duration
 (T90) of about 13 s (50-300 keV).
The time-averaged spectrum from T0-4.1 s to T0+10.2s is
well fit by a power law with an index of -1.61 +/- 0.07.

The event fluence (10-1000 keV) in this time interval is
(1.8 +/- 0.2)E-06 erg/cm^2. The 1.0-sec peak photon flux measured
starting from T0+0.0 s in the 10-1000 keV band
is 2.0 +/- 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: GRB140408A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16085
SUBJECT: GRB 140408A: Enhanced Swift-XRT position
DATE:    14/04/08 23:33:12 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 661 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 140408A, 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 = 290.71590, -12.59525 which is equivalent
to:

RA (J2000): 19h 22m 51.82s
Dec (J2000): -12d 35' 42.9"

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: GRB140408A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16086
SUBJECT: GRB 140408A: MITSuME Okayama upper limits
DATE:    14/04/08 23:45:08 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 140408A (D'Elia et al., GCNC 16082)
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 2014-04-08 17:47:44 UT (~4.5 h after the burst).
We did not find any new point source within the enhanced XRT circle
(Evans et al., GCNC 16085) 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
-----------------------------------------------------
0.21515    18:25:43    4200.0   >19.1  >18.9  >18.3
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB140408A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16087
SUBJECT: GRB 140408A: Swift-XRT refined Analysis
DATE:    14/04/09 04:36:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.A. Kennea (PSU), V. Mangano (PSU), M.C. Stroh (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 V. D'Elia report
on behalf of the Swift-XRT team:

We have analysed 8.7 ks of XRT data for GRB 140408A (D'Elia  et al. GCN
Circ. 16082),  from 91 s to 29.8 ks after the  BAT trigger. The data
comprise 268 s in Windowed Timing (WT) mode (the first 8 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. 16085).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.77 (+0.10, -0.09).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2 (+80, -1). The
best-fitting absorption column is  1.4 (+7.3, -1.2) x 10^22 cm^-2,
consistent with the Galactic value of 1.8 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 1.5 x 10^-11 (6.9 x
10^-11) erg cm^-2 count^-1. 

A summary of the WT-mode spectrum is thus:
Total column:      1.4 (+7.3, -1.2) x 10^22 cm^-2
Galactic foreground: 1.8 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      2 (+80, -1)

If the light curve continues to decay with a power-law decay index of
0.77, the count rate at T+24 hours will be 2.1 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.1 x
10^-14 (1.5 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/00595141.

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


GRB_name: GRB140408A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16088
SUBJECT: GRB 140408A: Swift/UVOT Upper Limits
DATE:    14/04/09 07:42:56 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

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

The Swift/UVOT began settled observations of the field of GRB 140408A
109 s after the BAT trigger (D'Elia et al., GCN Circ. 16082).
No optical afterglow consistent with the XRT position (Evans et al.,
GCN Circ. 16085,) and with the non-detection reported by Kuroda et al.
(GCN Circ. 16086), is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

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

white_FC           109          259          147         >20.9
u_FC               321          571          246         >20.5
white              109         1025          334         >21.2
v                  652         4403          236         >20.0
b                  577          769           39         >18.7
u                  321          745          265         >20.5
w1                 701          720           19         >18.1
m2                 676         4572          201         >19.9
w2                 627         1046           54         >20.2

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.19 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB140408A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16089
SUBJECT: GRB 140408A: GROND Detection of an Afterglow Candidate
DATE:    14/04/09 12:58:38 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

GRB 140408A: GROND Detection of an Afterglow Candidate
  
K. Varela, C. Delvaux (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 140408A (Swift trigger 595141; d'Elia et 
al., GCN #16082) 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 La
Silla Observatory (Chile).

Observations started at 06:16:31 UT on 8th April 2014, 0.709 days
after the  GRB trigger. They were performed at an average seeing of
0".9 and at an average airmass of 1.6.
  
We find a single point source within the 2".2 Swift-XRT error circle
reported by Evans et al. (GCN #16085) at 
  
RA (J2000) = 19h 22m 51.78s  
Dec. (J2000) = -12d 35' 40.9" 
  
with an uncertainty of 0".4 in each coordinate.
  
Based on a 7380 s exposure on g'r'i'z' , and a 6000 s exposure in
JHK, we estimate preliminary magnitudes (all in AB system) of
  
g' = 25.6 +- 0.3 mag,
r' = 23.7 +- 0.2 mag,
i' = 22.7 +- 0.2 mag,
z' = 22.8 +- 0.3 mag,
J > 22.0 mag,
H > 21.5 mag, and
K > 20.0 mag.

We propose this source to be a candidate afterglow for GRB 140408A.
At the moment, fading can not be established. If it is the afterglow,
the SED suggests a redshift of z ~ 4.

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)=0.16 
mag in the direction of the burst (Schlafly & Finkbeiner 2011).

[GCN OPS NOTE(10apr14): The missing minus sign on the Declination value
in the 3rd paragraph was added. Acknowledgement to F.Marshall.]


GRB_name: GRB140408A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16090
SUBJECT: GRB 140408A: Swift-BAT refined analysis
DATE:    14/04/09 14:31:03 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

T. N. Ukwatta (MSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), V. D'Elia (ASDC), 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),
(i.e. the Swift-BAT team):

Using the data set from T-180 to T+902 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140408A (trigger #595141)
(D'Elia, et al., GCN Circ. 16082).  The BAT ground-calculated position is
RA, Dec = 290.723, -12.585 deg which is
   RA(J2000)  =  19h 22m 53.5s
   Dec(J2000) = -12d 35' 07.7"
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 40%.

The mask-weighted light curve shows a single-pulse structure starts at ~T-1 sec,
peaks at ~ T+1 sec, and ends at ~T+4 sec. T90 (15-350 keV) is 4.00 +- 1.41 sec
(estimated error including systematics).

The time-averaged spectrum from T-0.66 to T+3.34 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.49 +- 0.25.  The fluence in the 15-150 keV band is 3.1 +- 0.5 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.34 sec in the 15-150 keV band
is 1.2 +- 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/595141/BA/


GRB_name: GRB140408A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16091
SUBJECT: GRB 140408A: RATIR Optical Upper Limits
DATE:    14/04/09 23:48:05 GMT
FROM:    Owen Littlejohns at Az State U  <olittlej@asu.edu>

Owen Littlejohns (ASU), 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), Enrico Ramirez-Ruiz (UCSC), Jos A. de Diego (UNAM),
Leonid Georgiev (UNAM), Jess Gonzlez (UNAM), Carlos Romn-Ziga
(UNAM), Neil Gehrels (GSFC), and Harvey Moseley (GSFC) report:

We observed the field of GRB 140408A (D'Elia, et al., GCN 16082) with
the Reionization and Transients Infrared Camera (RATIR; www.ratir.org)
on the 1.5m Harold Johnson Telescope at the Observatorio Astronmico
Nacional on Sierra San Pedro Mrtir from 2014/04 9.41 to 2014/04 9.48
UTC (20.52 to 22.37 hours after the BAT trigger), obtaining a total of
1.42 hours exposure in the r and i bands.

For a source within the Swift-XRT error circle we obtain the following
upper limits (3-sigma):

  r     > 22.84
  i     > 22.53

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB. These upper limits are consistent
with the previously reported GROND afterglow candidate (Varela, et al.,
GCN 16089).

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


GRB_name: GRB140408A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16093
SUBJECT: GRB 140408A: MITSuME Akeno Optical observation
DATE:    14/04/10 05:21:39 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

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

We observed the field of GRB 140408A (V. D'Elia et al., GCN Circular #16082) 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 2014-04-08 17:03:08.6 UT ( 3.8h after the burst).
We did not find any new point source within the enhanced XRT circle (Evans et al., GCNC 16085) in all the three bands.
The measured magnitudes were listed below.

T0+[sec]    MID-UT    T-EXP[sec]    g'         Rc         Ic
$B!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=(B-
17105     18:00:59     6300        >20.1    >19.6     >19.1
$B!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=!=(B-
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used GSC2.3 catalog for flux calibration.


GRB_name: GRB140408A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16096
SUBJECT: GRB 140408A: 1.5m OSN optical upper limit
DATE:    14/04/10 18:34:22 GMT
FROM:    Soomin Jeong at CSIC  <soominjeong@gmail.com>

S. Jeong, S. R. Oates, J. C. Tello, J. Gorosabel, A. Sota and A. J.
Castro-Tirado (IAA-CSIC), on behalf of a larger collaboration, report:

"Following the detection of GRB140408A by Swift (D'Elia et al., GCNC
16082), we observed the field of GRB 140408A with the 1.5 m OSN telescope
at Observatorio de Sierra Nevada in the R and I-bands. The observation
started on Apr 9, 04:01:16 UT (i.e. ~0.62 d post burst). No optical
afterglow is found at the position of the optical candidate reported by
Varela et al. (GCNC 16089) in the median combined images (6 x 300s)
down to 21.7 mag (I band) and 22.5 mag (R band) (3-sigma upper limits,
with all magnitudes in Vega system and no correction for the Galaxy
reddening)."


GRB_name: GRB140412A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16097
SUBJECT: GRB 140412A: Swift detection of a burst
DATE:    14/04/12 22:33:10 GMT
FROM:    David Burrows at PSU/Swift  <burrows@astro.psu.edu>

V. D'Elia (ASDC), D. N. Burrows (PSU), S. T. Holland (STScI),
L. Izzo (URoma/ICRA), F. E. Marshall (NASA/GSFC), T. Sakamoto (AGU)
and B. Sbarufatti (INAF-OAB/PSU) report on behalf of the Swift Team:

At 22:20:49 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140412A (trigger=595608).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 145.050, -65.809 which is 
   RA(J2000) = 09h 40m 12s
   Dec(J2000) = -65d 48' 31"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a FRED-like 
structure with a duration of about 20 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 22:24:17.0 UT, 207.2 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 144.9713, -65.8226
which is equivalent to:
   RA(J2000)  = 09h 39m 53.11s
   Dec(J2000) = -65d 49' 21.3"
with an uncertainty of 3.2 arcseconds (radius, 90% containment). This
location is 125 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 236 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 0.22. 

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: GRB140413A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16098
SUBJECT: Swift Trigger 595616: a possible GRB
DATE:    14/04/13 00:29:27 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia (ASDC), S. T. Holland (STScI), L. Izzo (URoma/ICRA),
F. E. Marshall (NASA/GSFC) and B. Sbarufatti (INAF-OAB/PSU) report on
behalf of the Swift Team:

At 00:09:40 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140413A (trigger=595616).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 65.449, -51.205 which is 
   RA(J2000) = 04h 21m 48s
   Dec(J2000) = -51d 12' 17"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  This is an image trigger and we cannot 
say much about the light curve.  However, since it is 12.5 sigma detection 
at 64 sec exposure in the image domain, it is likely to be real. 

Due to an observing constraint, Swift will not slew until T0+33.6
minutes. There will be no XRT or UVOT data until this time. 

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: GRB140413A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16099
SUBJECT: GRB 140413A: GROND afterglow candidate
DATE:    14/04/13 01:37:26 GMT
FROM:    Ana Nicuesa at TLS Tautenburg  <ana@tls-tautenburg.de>

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

We observed the field of GRB 140413A (Swift trigger 595616; D'Elia et al.,
GCN #16098) 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 La Silla Observatory
(Chile).

Observations started at 00:13 UT on 13 April 2014, less than 5 min after
the GRB trigger, and are continuing. They are performed at a mean airmass
of 1.9 and a mean seeing of 0.9".

We find a single point source within the 5.8" Swift/XRT error circle at
coordinates

   RA(J2000)  =  04:21:49.23
   Dec(J2000) = -51:10:58.0.

At a midtime of 00:17 UT we measure the following preliminary AB magnitudes:

r' = 20.2 +/- 0.1,
i' = 19.6 +/- 0.1,
z' = 19.3 +/- 0.1.

The source is also visible in g. At present we cannot decide if the source
is fading. Data processing is still ongoing, observations are continuing.

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: GRB140412A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16100
SUBJECT: GRB 140412A: Enhanced Swift-XRT position
DATE:    14/04/13 04:13:35 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 862 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 140412A, 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 = 144.97315, -65.82169 which is equivalent
to:

RA (J2000): 09h 39m 53.55s
Dec (J2000): -65d 49' 18.1"

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: GRB140413A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16101
SUBJECT: GRB 140413A: Swift-XRT observations
DATE:    14/04/13 08:44:37 GMT
FROM:    Luca Izzo at ICRA  <Luca.Izzo@ICRA.it>

V. D'Elia (ASDC) and L. Izzo (URoma/ICRA) report for the Swift/XRT team:

The XRT began observing the field of GRB 140413A at 00:46:31.37 UT, 2211.2 seconds after the BAT trigger. We find an uncatalogued X-ray source located at RA, Dec 65.4544, -51.1831 which is equivalent to:
RA(J2000) =+04h 21m 49.0s
Dec(J2000) =-51d 10' 59.1"
with an uncertainty of 4.7 arcseconds (radius, 90% containment). This location is 80 arcseconds from the BAT onboard position, within the BAT error circle. This position may be improved as more data are received.


GRB_name: GRB140413A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16102
SUBJECT: GRB 140413A: TAROT La Silla observatory optical observations
DATE:    14/04/13 10:43:21 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 140413A detected by SWIFT
(trigger 595616) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 92.3s after the GRB trigger
(16.4s after the notice) probably during the end of
the prompt gamma emission regarding the BAT light curve.
The elevation of the field decreased from 36 degrees
above horizon and weather conditions were good.

The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
We do not detect the GROND OT candidate (Varela et al.
GCNC 16099) with a limiting magnitude of:
t0+92.3s to t0+152.3s : Rlim = 17.0

The second image is 30.0s exposure in tracking mode:
t0+165.6s to t0+195.6s : Rlim = 17.6

We co-added series of exposures:
t0+165.6s to t0+457.5s : Rlim = 19.3
t0+468.3s to t0+ 1362s : Rlim = 19.3

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


GRB_name: GRB140412A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16103
SUBJECT: GRB 140412A: Swift-BAT refined analysis
DATE:    14/04/13 14:22:16 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. N. Ukwatta (MSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), V. D'Elia (ASDC), 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)
(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 140412A (trigger #595608)
(D'Elia, et al., GCN Circ. 16097).  The BAT ground-calculated position is
RA, Dec = 145.032, -65.826 deg, which is 
   RA(J2000)  =  09h 40m 07.6s 
   Dec(J2000) = -65d 49' 33.7" 
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 77%.
 
The mask-weighted light curve shows two peaks strting at ~T-35 sec,
peaking at ~T+1 sec, and ending at ~T+35 sec.
T90 (15-350 keV) is 39.6 +- 8.2 sec (estimated error including systematics).
 
The time-averaged spectrum from T-36.94 to T+12.18 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.95 +- 0.19.  The fluence in the 15-150 keV band is 7.2 +- 0.8 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.04 sec in the 15-150 keV band
is 1.1 +- 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/595608/BA/


GRB_name: GRB140412A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16104
SUBJECT: GRB 140412A: Swift-XRT refined Analysis
DATE:    14/04/13 15:33:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

V. Mangano (PSU), M.C. Stroh (PSU), D.N. Burrows (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 V. D'Elia report on behalf of the Swift-XRT team:

We have analysed 6.1 ks of XRT data for GRB 140412A (D'Elia  et al. GCN
Circ. 16097),  from 198 s to 41.3 ks after the BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Goad et al. (GCN Circ. 16100).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.60 (+0.10, -0.09).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 3.2 (+0.9, -0.6). The
best-fitting absorption column is  9.1 (+4.6, -3.3) x 10^21 cm^-2, in
excess of the Galactic value of 2.6 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 2.8 x 10^-11 (1.7 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      9.1 (+4.6, -3.3) x 10^21 cm^-2
Galactic foreground: 2.6 x 10^21 cm^-2
Excess significance: 3.3 sigma
Photon index:      3.2 (+0.9, -0.6)

If the light curve continues to decay with a power-law decay index of
0.60, the count rate at T+24 hours will be 3.7 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.0 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/00595608.

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


GRB_name: GRB140413A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16105
SUBJECT: GRB 140413A: Swift-BAT refined analysis
DATE:    14/04/13 16:31:11 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),
V. D'Elia (ASDC), 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-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 140413A (trigger #595616)
(D'Elia, et al., GCN Circ. 16098).  The BAT ground-calculated position is
RA, Dec = 65.439, -51.188 deg, which is 
   RA(J2000)  =  04h 21m 45.4s 
   Dec(J2000) = -51d 11' 15.1" 
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 12%.
 
The mask-weighted light curve shows a slow rise starting at ~T-65 sec,
peaking at ~T+80 sec, and a faster decay out to ~T+115 sec.
T90 (15-350 keV) is 139.6 +- 12.6 sec (estimated error including systematics).
 
The time-averaged spectrum from T-52.0 to T+120.4 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.49 +- 0.08.  The fluence in the 15-150 keV band is 9.4 +- 0.5 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+77.05 sec in the 15-150 keV band
is 2.3 +- 0.5 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/595616/BA/


GRB_name: GRB140413A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16106
SUBJECT: GRB 140413A: Swift-XRT refined Analysis
DATE:    14/04/14 11:39:30 GMT
FROM:    Luca Izzo at ICRA  <Luca.Izzo@ICRA.it>

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

We have analysed 13 ks of XRT data for GRB 140413A,  from 2.2 ks to
83.3 ks after the  BAT trigger. The data comprise 2.1 ks in Windowed
Timing (WT) mode with the remainder in Photon Counting (PC) mode. Using
3951 s of PC mode data and 4 UVOT images, we find an enhanced XRT
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 65.45475, -51.18310 which is
equivalent to:

RA (J2000): 04h 21m 49.14s
Dec(J2000): -51d 10' 59.2"

with an uncertainty of 1.6 arcsec (radius, 90% confidence).

The late-time light curve (from T0+38.1 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.7 (+/-0.4).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.989 (+0.025, -0.024). The
best-fitting absorption column is  4.04 (+/-0.13) x 10^21 cm^-2, in
excess of the Galactic value of 1.4 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 3.9 x 10^-11 (6.0 x 10^-11) erg
cm^-2 count^-1. 

A summary of the WT-mode spectrum is thus:
Total column:      4.04 (+/-0.13) x 10^21 cm^-2
Galactic foreground: 1.4 x 10^20 cm^-2
Excess significance: 49.9 sigma
Photon index:      1.989 (+0.025, -0.024)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00595616.

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


GRB_name: GRB140413A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16107
SUBJECT: Konus-Wind observation of GRB 140413A
DATE:    14/04/14 12:09:24 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, and T. Cline
on behalf of the Konus-Wind team, report:

The long GRB 140413A (Swift-BAT trigger #595616:
D'Elia et al., GCN 16098; T0(BAT)=00:09:40 UT)
was detected by Konus-Wind in the waiting mode.

The light curve shows a broad emission pulse which started
~65 s before the BAT trigger, peaked at ~T0(BAT)+80 s,
and lasted till ~T0(BAT)+120 s.

A possible soft precursor is seen at ~T0(BAT)-950 s
in the softest KW energy band, however its association with
GRB 140413A is not confirmed yet.

The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB140413A/

As observed by Konus-Wind, the burst had a fluence of
(2.9  0.3)x10^-5 erg/cm2 and a 2.944-s peak energy flux,
measured from ~T0(BAT)+80 s, of (5.2  0.5)x10^-7 erg/cm2
(both in the 20 - 10000 keV energy range).

Modeling the KW 3-channel time-integrated spectrum
(from T0(BAT)-60 s to T0(BAT)+121 s) by a power law
with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -1.37  0.11, and Ep = 228  42 keV.

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


GRB_name: GRB140412A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16108
SUBJECT: GRB 140412A: Swift/UVOT Upper Limits
DATE:    14/04/14 12:46:51 GMT
FROM:    Stephen Holland at STScI  <sholland@stsci.edu>

S. T. Holland (STScI) and V. D'Elia (ASDC) report on behalf of the
Swift/UVOT team:

    Swift/UVOT began settled observations of the field of GRB 140412A
237 s after the BAT trigger (D'Elia et al. 2014, GCNC 16097).  We do
not detect any new source consistent with the UVOT-enhanced XRT
afterglow position (Goad et al. 2014, GCNC 16100) in any of the UVOT
exposures.  Preliminary 3-sigma upper limits, using the UVOT
photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373),
for the finding chart and summed exposures are presented below.

---------------------------------------------------
Filter        TSTART     TSTOP   Exposure       Mag
---------------------------------------------------
v                393      1055         69     >19.0
b                491      6805        255     >21.0
u                466      6599        309     >20.6
uvw1             442      4815        255     >20.0
uvm2             418      4610        255     >19.6
uvw2             541      1040         58     >18.7
white            237      6811        336     >21.8
---------------------------------------------------

    The quoted upper limits have not been corrected for the expected
extinction due to the Galactic reddening along the line of sight to
this burst of E(B-V) = 0.19 mag (Schlafly et al. 2011, ApJS, 737,
103).


GRB_name: GRB140413A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16109
SUBJECT: GRB 140413A: Swift/UVOT Observations of the Optical Afterglow
DATE:    14/04/14 12:50:51 GMT
FROM:    Stephen Holland at STScI  <sholland@stsci.edu>

S. T. Holland (STScI) and V. D'Elia (ASDC) report on behalf of the
Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140413A
2221 s after the BAT trigger (D'Elia et al., 2014, GCNC 16098).  The
preliminary UVOT position is

     RA (J2000)  04:21:49.23  =   65.45512 (deg)
    Dec (J2000) -51:10:58.0   =  -51.18278 (deg)

with an estimated uncertainty of 1.79 arcsec (radius, 90% confidence,
statistical + systematic).  We detect the optical afterglow at the
position reported by Varela et al. (2014, GCNC 16099).  Preliminary
UVOT photometry and 3-sigma upper limits are presented below.

----------------------------------------------------------------
Filter        TSTART     TSTOP   Exposure       Mag   Err  Sigma
----------------------------------------------------------------
v               2377      4303        375     >19.7
b               2476      3747        235     >21.0
u               2451      3542        236     >19.9
uvw1            2427      3336        236     >19.8
uvm2            2931      3131        197     >19.5
uvw2            3957      4157        197     >20.1
white           2221      2370        147     >20.3
                3752      3951        197      21.10 0.29    3.8
----------------------------------------------------------------

The quoted magnitudes and upper limits have not been corrected for the
Galactic extinction along the line of sight to this burst of E_{B-V} =
0.01 mag (Schlafly et al. 2011, ApJS, 737, 103).  The photometry is in
the UVOT photometric system (Breeveld et al. 2011, AIP
Conf. Proc. 1358, 373).


GRB_name: GRB140414A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16110
SUBJECT: GRB 140414A: Short burst found in ground analysis of BAT slew data
DATE:    14/04/14 15:38:15 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

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

At 2014-04-14T06:06:29, IPN spacecraft triggered on GRB 140414A.  The burst
was about 0.7 seconds long, and appears to be in the SHB category. Swift was
executing a pre-planned slew maneuver at this time.  A mosaic image made from
BAT event data collected during the slew shows a 12 sigma source at
RA, Dec 195.310, +56.902, which is:

RA (J2000) 13h 01m 14.3s  
Dec (J2000) 56d 54' 06"

with an estimated uncertainty radius of 4 arcmin (90% containment)

A Swift TOO request has been submitted to locate the afterglow with XRT.


GRB_name: GRB140414A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16111
SUBJECT: GRB 140414A: Swift-BAT refined analysis
DATE:    14/04/14 20:13:34 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

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

We present refined analysis of the short-hard burst GRB 140414A (Cummings,
GCN Circ. #16110).  The best BAT position is still RA, Dec 195.310, +56.902,
which is:

RA (J2000) 13h 01m 14.3s  
Dec (J2000) 56d 54' 06"

with an estimated uncertainty radius of 4 arcmin (90% containment).

The light curve shows two main peaks each about 0.3 seconds long, the second
about 3 times as intense and peaking about 0.3 seconds after the first.  T90 is
estimated as 0.7 +- 0.1 seconds.

The spectrum is best fit by a simple powerlaw function with a photon index of
0.74 +- 0.18.  The fluence in 0.7 seconds was (1.22 +- 0.10) x 10^-7 ergs/cm^2.
Errors are 90% confidence.

A Swift TOO request was approved to locate the afterglow with XRT, with the
observation ID 20375.  Unfortunately, the star tracker did not find enough
targets to lock.  Swift will not reobserve the target.


GRB_name: GRB140414A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16112
SUBJECT: GRB 140414A: TNG optical observations
DATE:    14/04/14 23:11:04 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, D. Fugazza (INAF/OAB) L. Di Fabrizio, G. Mainella (INAF/TNG) report on behalf of the CIBO collaboration:

We observed the field of the short GRB 140414A (Cummings, GCN 16110) using the DOLORES camera on the 3.6-m TNG Telescope at Canary Islands.

We obtained 30 minutes of imaging observations under seeing of ~ 2" with the r SDSS filter at a mean t-t0 of 15.2 hours. No object brighter than the SDSS limit is found inside the BAT error circle (Cummings, GCN 16111). The 3sigma limiting magnitude of the co-added image is r~22 (calibrated against SDSS stars).


We thank the TNG visiting astronomer Luca Malavolta.


GRB_name: GRB140414A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16113
SUBJECT: GRB 140414A: Swift-XRT observations
DATE:    14/04/15 15:45:46 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, M. G. Bernardini, S. Campana (INAF-OAB) report on behalf of  the Swift team:

We have analysed 1.7 ks of XRT data for GRB 140414A (Cummings, GCN 16110), from 40.4 ks to 42.1 ks after the IPN trigger. 
The data are all in Photon Counting (PC) mode. As mentioned by Cummings (GCN 16111), too few stars were present in the field for the star tracker to lock. 
In light of this, the data were processed relaxing some constraints on the attitude file with respect to the standard procedure.

No bright X-ray afterglow is detected inside the refined BAT error circle (Cummings, GCN 16111). The formal 3sigma upper limit is 2.3 x 10^-2 cts/s even if, given the non standard processing, it might result in a slightly higher limit.


GRB_name: GRB140414A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16114
SUBJECT: GRB 140414A: Swift/UVOT Upper Limit
DATE:    14/04/15 21:52:27 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC), L.M.Z. Hagen (PSU), and P. D'Avanzo (INAF-OAB)
report on behalf of the Swift/UVOT team:

The Swift/UVOT observed the field of GRB 140414A
in the U, White, and V filters starting about 40 ks
after the BAT trigger (Cummings GCN Circ. 16110).
Because the star tracker failed to lock, stars are trailed
in all the images, and the usual UVOT sensitivities
are not achieved.
No optical afterglow consistent with the BAT position
is detected in the any of the UVOT exposures.
The results for the most sensitive exposure is reported
in the table below. The limiting magnitude is
estimated from the list of detected stars.

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

white            40958        41502          536         >20

The magnitude in the table is 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: GRB140416A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16115
SUBJECT: GRB 140416A: Fermi GBM detection
DATE:    14/04/16 21:08:48 GMT
FROM:    Peter Jenke at MSFC  <peter.a.jenke@nasa.gov>

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

"At 01:26:40.94 UT on April 16 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140416A (trigger 419304403/140416060).  
The GBM on-ground location, using the Fermi GBM trigger
data, is RA = 35.4, Dec = 43.9 (J2000 degrees, equivalent to 
02h 21m 36s, 43d 54'), with an uncertainty of 1 
degree (radius, 1-sigma containment,
statistical only; there is additionally a systematic error which is
currently estimated to be 2 to 3 degrees).

The angle of the burst direction to the Fermi LAT boresight is 
138 degrees.

The GBM light curve consists of several peaks with a duration
 (T90) of about 28.5 s (50-300 keV).
The time-averaged spectrum from T0-10.0 s to T0+31.0s is
well fit by a Band function with Epeak = 78 +/- 2 keV, 
Alpha = -1.01 +/- 0.04 and Beta = -2.44 +/- 0.03.

The event fluence (10-1000 keV) in this time interval is
(7.20 +/- 0.06)E-05 erg/cm^2. The 1.0-sec peak photon flux measured
starting from T0+6.4 s in the 10-1000 keV band
is 71 +/- 1 ph/s/cm^2.

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


GRB_name: GRB140416A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16116
SUBJECT: IPN Triangulation of GRB 140416A (long/very intense)
DATE:    14/04/18 14:35:36 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,

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

G. Di Cocco, F. Fuschino, M. Galli, C. Labanti, and M. Marisaldi, on
behalf of the AGILE MCAL team, report:

The long-duration very intense GRB 140416A (P. Jenke, GCN Circ. 16115) 
has been observed by Fermi (GBM: trigger 419304403), Konus-Wind, AGILE 
(MCAL), MESSENGER (GRNS), and Mars-Odyssey (HEND), so far, at about 5201 
s UT (01:26:41).

These annuli intersect to form a long arc, whose coordinates are:
  ---------------------------------------------
     RA(2000), deg                 Dec(2000), deg
    ---------------------------------------------
    Center:
      40.186 (02h 40m 45s) +39.527 (+39d 31' 37")
    Corners:
      25.842 (01h 43m 22s) +45.226 (+45d 13' 35")
      27.972 (01h 51m 53s) +44.893 (+44d 53' 35")
      50.081 (03h 20m 20s) +30.017 (+30d 01' 02")
      50.783 (03h 23m 08s) +28.603 (+28d 36' 11")
    ---------------------------------------------
The error box area is 2.023 sq. deg, and its maximum dimension is 25.8 
deg (the minimum one is 0.164 deg).

This error box may be improved.

Because the Earth, the Wind, the Mars-Odyssey, and the MESSENGER 
satellites are nearly aligned at the moment (the angular distance 
between Wind and MESSENGER is 10.3 deg and between Wind and Mars-Odyssey 
is 170 deg), the annuli intersect at grazing incidence and the resulting 
3-sigma box is long.

The center of the GBM ground position given in P. Jenke, GCN Circ. 16115 
(that is RA, Dec, RErr = 35.4, 43.9, 1.0 deg) is 5.4 deg from the box 
center and is 1.5 deg from the center line of the Konus-MESSENGER annulus.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB140416_T05196/IPN/


GRB_name: GRB140416A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16117
SUBJECT: Konus-Wind observation of GRB 140416A
DATE:    14/04/18 14:46:57 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, and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration, very intense GRB 140416A
(Fermi GBM detection: Jenke, GCN 16115;
IPN triangulation: Hurley at al., GCN 16116)
triggered Konus-Wind at T0=5196.209 s UT (01:26:36.209).

The burst light curve shows multiple peaks from ~T0-24 s to ~T0+28 s.
The emission is seen up to ~8 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140416_T05196/

As observed by Konus-Wind, the burst
had a fluence of 6.9(-0.1,+0.1)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+7.168 s,
of 1.5(-0.1,+0.1)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+32.768 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.43 (-0.06,+0.07),
the high energy photon index beta = -2.95 (-0.31,+0.18),
the peak energy Ep = 97 (-4,+4) keV,
chi2 = 88.4/96 dof.

The spectrum near the maximum count rate
(measured from T0+6.912 to T0+7.424 s)
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.78 (-0.14,+0.15),
the high energy photon index beta = -3.8 (-6.2,+0.6),
the peak energy Ep = 176 (-16,+18) keV,
chi2 = 81.5/90 dof.

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


GRB_name: GRB140419A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16118
SUBJECT: GRB 140419A: Swift detection of a burst with optical afterglow
DATE:    14/04/19 04:21:34 GMT
FROM:    Caryl Gronwall at PSU/Swift-UVOT  <caryl@astro.psu.edu>

F. E. Marshall (NASA/GSFC), J. R. Cummings (NASA/UMBC),
C. Gronwall (PSU), J. A. Kennea (PSU), A. Maselli (INAF-IASFPA),
T. Sakamoto (AGU), M. H. Siegel (PSU) and T. N. Ukwatta (MSU) report
on behalf of the Swift Team:

At 04:06:51 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140419A (trigger=596426).  Swift slewed immediately to the 
burst.  The BAT on-board calculated location is 
RA, Dec 126.999, +46.221 which is 
   RA(J2000) = 08h 28m 00s
   Dec(J2000) = +46d 13' 15"
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 80 sec.  The peak count rate
was ~5611 counts/sec (15-350 keV), at ~52 sec after the trigger. 

The XRT began observing the field at 04:08:17.5 UT, 86.5 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 126.9909, 46.2416 which is equivalent to:
   RA(J2000)  = +08h 27m 57.82s
   Dec(J2000) = +46d 14' 29.8"
with an uncertainty of 4.8 arcseconds (radius, 90% containment). This
location is 76 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 5.09e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White
filter  starting 96 seconds after the BAT trigger. A bright
uncatalogued source is  identified in the 2.7'x2.7' sub-image near the
position of the XRT afterglow. However, a more precise position is
unavailable at this time. The approximate  magnitude in the White
filter is 16.1.  No correction has been made  for the expected
extinction corresponding to E(B-V) of 0.03. 

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: GRB140419A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16119
SUBJECT: GRB 140419A (Swift trigger 596426) : KAIT optical candidate
DATE:    14/04/19 04:29:15 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 trigger 596426. A bright
(R~13.5) optical counterpart un-cataloged in DSS image was detected
at location of Ra, DEC (J2000):

08:27:57.56
+46:14:25.11

with uncertainty of about 1". We suggest this to be the afterglow of
the GRB. Follow-up observations encouraged. 


GRB_name: GRB140419A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16120
SUBJECT: GRB 140419A: ROTSE-III Detection of Optical Counterpart
DATE:    14/04/19 04:40:43 GMT
FROM:    Tolga Guver at UA  <tolga@physics.arizona.edu>

GRB 140419A: ROTSE-III Detection of Optical Counterpart

T. Guver (Istanbul Univ.), F. V. Ferrante (SMU), H. Flewelling  
(IfA/Hawaii), R. Kehoe (SMU), G. Dhungana (SMU) report on behalf of  
the ROTSE collaboration:

ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB  
140419A (Swift trigger 596426, GCN 16118). The first image was at  
04:07:18.7 UT, 27.3 s after the burst (8.7 s after the GCN notice  
time). The unfiltered images are calibrated relative to USNO A2.0. We  
detect a new object, not visible in the DSS (second epoch), with  
coordinates:

08:27:57.7 +46:14:25.9 (J2000), with positional uncertainty of 1' or better

start UT mag mlim(of image)
----------------------------------
04:07:18.7 13.5 15.0

The object first detected with a magnitude of ~13.5, brightened to  
12.5 magnitudes in ~70 seconds then the brightness decayed fast to  
~14.3 magnitudes at about 350 seconds.

A jpeg image is available at  
http://www.rotse.net/images/gsq596426_3b01_img.jpg Note that the  
object marked 8 is the candidate in question.

Continuing observations are in progress.

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GRB_name: GRB140419A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16121
SUBJECT: GRB 140419A: RATIR Optical and NIR Observations
DATE:    14/04/19 05:30:28 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 140419A (Marshall, et al., GCN 16118) 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 2014/04 19.18 to 2014/04 19.20 UTC (9 to 40
minutes after the BAT trigger), obtaining a total of 0.36 hours exposure in
the r and i bands and 0.15 hours exposure in the Z, Y, J, and H bands.

We detect the UVOT optical transient (see also, Zheng, et al., GCN 16116;
Guver et al., GCN 16120).  In comparison with the SDSS DR9 and 2MASS, we
obtain the following detections:

  r     16.22 +/- 0.01
  i     15.81 +/- 0.01
  Z     15.66 +/- 0.01
  Y     15.46 +/- 0.02
  J     15.31 +/- 0.01
  H     15.26 +/- 0.02

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.  The source appears to be fading
approximately as t^(-1) in all of our bands during the observation.

Further observations are ongoing.  We thank the staff of the Observatorio
AstronÃ³mico Nacional in San Pedro MÃ¡rtir.


GRB_name: GRB140419A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16122
SUBJECT: GRB 140419A: CARMA early 3mm detection
DATE:    14/04/19 07:07:57 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

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

We observed the location of GRB 140419A (Marshall et al., GCN 16118) 
with the Combined Array for Research in Millimeter Astronomy at a mean 
frequency of 93 GHz starting at 05:23:45, 77 minutes after the GRB 
trigger.

In the first hour of observations, we marginally detect a weak source 
consistent with the location of the optical afterglow (Zheng et al., GCN 
16119; Guver et al., GCN 16120) with a flux of approximately 1.5 mJy. 
Observations are continuing.

We thank J. Carpenter and D. Segura-Cox for assistance with rapidly 
scheduling and executing the observations.


GRB_name: GRB140419A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16123
SUBJECT: GRB140419A: UVOT detects fading afterglow in white but not in u filter
DATE:    14/04/19 07:56:22 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

NPM Kuin (MSSL-UCL), and F. E. Marshall (NASA/GSFC) report on behalf of
the Swift Team:

UVOT started observing GRB 140419A starting 96 seconds after the BAT
trigger.
The initial finding chart exposures with the White and U filter show a
fading source in the white filter which we identify with the afterglow:

The estimated magnitudes are as follows:

filter starttime endtime magnitude error
wh      96         246    16.01    0.06
u      308         558    >19.6
wh     862        1012    17.96    0.09.

The source is not seen in the u filter, which suggests a redshift larger
then
2.8.

No correction has been made for the expected extinction corresponding to
E(B-V) of 0.03.


GRB_name: GRB140419A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16124
SUBJECT: GRB 140419A: Enhanced Swift-XRT position
DATE:    14/04/19 11:56:14 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 3698 s of XRT Photon Counting mode data and 7 UVOT
images for GRB 140419A, 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 = 126.98969, +46.24009 which is equivalent
to:

RA (J2000): 08h 27m 57.53s
Dec (J2000): +46d 14' 24.3"

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

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

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


GRB_name: GRB140419A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16125
SUBJECT: GRB 140419A: Gemini-N redshift
DATE:    14/04/19 13:21:37 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir (U. Leicester), A. J. Levan (U. Warwick),
A. Cucchiarra (ORAU/GSFC), D. Perley (Caltech), S. B. Cenko (GSFC) 
D. Coulson, L. Fuhrman report:

We observed the afterglow of GRB 140419A (Marshall et al. GCN 16118;
Zheng et al. GCN 16119; Guver et al. GCN 16120; Butler et al. GCN 16121)
with the GMOS-N spectrograph on Gemini-N.  Observations began
at 06:24 UT, approximately 2.3 hr post burst, and two different
settings covered a total wavelength range from about 4400AA to 10100AA.

The spectra reveal several strong absorption lines and in particular
there is a marked break at about 6027 AA which we identify as
Ly-a at a redshift z=3.956.  Blueward is a clear Ly-a forest.
At the same redshift we see strong lines of CIV (1548/1551) and
SiIV (1394/1403), and weaker lines of NV (1239/1243), CII (1335),
SiII (1527), AlII (1671).  We therefore infer z=3.956 as the redshift of 
the burst.

We note that there also appears to be an intervening system at z=2.686.

[GCN OPS NOTE(19apr14): Per author's request, DC and LF were added
to the author list.]


GRB_name: GRB140419A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16126
SUBJECT: GRB 140419A: T24 optical observations
DATE:    14/04/19 13:23:00 GMT
FROM:    Veli-Pekka Hentunen at Taurus Hill Obs,A95  <veli-pekka.hentunen@kassiopeia.net>

Veli-Pekka Hentunen, Markku Nissinen and Tuomo Salmi (Taurus Hill
Observatory, Varkaus, Finland) report:

We have detected GRB 140419A optical afterglow at iTelescope observatory
T24 (Auberry, California) using 0.61-m/6.5 astrograph and FLI-PL09000 CCD.
The observations were started at 2014-04-19 06:34:54 (UT) and stopped at
06:56:31 (UT). Four unfiltered images with 300 sec exposure time were made.

The afterglow was detected at the following position RA 08:27:57.56 and
DEC +46:14:25.2.

The following magnitude was obtained from the observations using
NOMAD1 1362-0196617 (R=17.110) as a comparison star:

Tmid(s)+T0    Filter            Exp. time         Mag              Mag err.
9536              unfiltered      4x300s            17.86CR      0.12

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GRB_name: GRB140419A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16127
SUBJECT: GRB 140419A: Swift-BAT refined analysis
DATE:    14/04/19 15:19:34 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), 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-240 to T+485 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 140419A (trigger #596426)
(Marshall, et al., GCN Circ. 16118).  The BAT ground-calculated position is
RA, Dec = 127.001, 46.234 deg, which is 
   RA(J2000)  =  08h 28m 00.4s 
   Dec(J2000) = +46d 14' 03.7" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 33%.
 
The mask-weighted light curve shows two slightly overlapping clusters of
peaks, starting at ~T-10 sec, peaking at ~T+10 and ~T+51 sec, and ending
at ~T+220 sec.  T90 (15-350 keV) is 94.7 +- 11.0 sec (estimated error
including systematics).
 
The time-averaged spectrum from T-8.69 to T+222.32 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.21 +- 0.04.  The fluence in the 15-150 keV band is 1.59 +- 0.03 x 10^-5 erg/cm2.
The 1-sec peak photon flux measured from T+51.42 sec in the 15-150 keV band
is 4.9 +- 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/596426/BA/

[GCN OPS NOTE(22apr14): Per author's request, the fluence value
was changed from "1.6 +- 0.0" to "1.59 +- 0.03". Acknowledgement
to F.Marshall for pointing out the missing error value.]


GRB_name: GRB140419A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16128
SUBJECT: GRB 140419A: Swift-XRT refined Analysis
DATE:    14/04/19 17:31:39 GMT
FROM:    Alessandro Maselli at INAF/IASF Palermo  <maselli@ifc.inaf.it>

A. Maselli, M. De Pasquale (INAF-IASFPA), P. A. Evans (U Leicester) and
F. E. Marshall (NASA/GSFC) report on behalf of the Swift-XRT team:

We have analysed 10 ks of XRT data for GRB 140419A (Marshall et al. GCN
Circ. 16118), from 79 s to 24.3 ks after the BAT trigger. The data
comprise 849 s in Windowed Timing (WT) mode (the first 5 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Osborne et
al. (GCN Circ. 16124).

The late-time light curve (from T0+5.4 ks) can be modelled with a
power-law decay with a decay index of alpha=1.29 (+/-0.07).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.803 (+0.029, -0.028). The
best-fitting absorption column is 1.7 (+2.8, -1.7) x 10^21 cm^-2, at a
redshift of 3.956, in addition to the Galactic value of 3.9 x 10^20
cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index
of 1.83 (+/-0.06) and a best-fitting absorption column of 1.2 (+/-0.6)
x 10^22 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum is 3.6 x 10^-11 (4.0 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 3.9 x 10^20 cm^-2
Intrinsic column:    1.2 (+/-0.6) x 10^22 cm^-2 at z=3.956
Photon index:      1.83 (+/-0.06)

If the light curve continues to decay with a power-law decay index of
1.29, the count rate at T+24 hours will be 0.042 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.5 x
10^-12 (1.7 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/00596426.

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


GRB_name: GRB140419A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16129
SUBJECT: GRB 140419A: P60 Observations
DATE:    14/04/19 20:26:32 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 optical afterglow (Zheng et al., GCN 16119; Guver et al., GCN 16120; Butler et al., GCN 16121; Kuin et al., GCN 16123; Hentunen et al., GCN 16126) of the Swift GRB 140419A (Marshall et al., GCN 16118) with the robotic Palomar 60 inch telescope.  Observations were obtained in the r', i', and z' filters beginning at 4:40 UT on 2014 April 19 (33 minutes after the Swift trigger).

The optical afterglow is clearly detected in all three filters.  Using nearby point sources from SDSS for calibration, we measure the following magnitudes in our initial images:

r' = 16.91 +/- 0.03 at dt = 33.7 min
i' = 16.56 +/- 0.03 at dt = 35.1 min
z' = 16.45 +/- 0.04 at dt = 36.5 min

The redder r'-i' color is consistent with the Lyman break falling in the observed r' bandpass, as reported by Tanvir et al. (GCN 16125).

Further observations are planned.


GRB_name: GRB140419A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16130
SUBJECT: GRB 140419A: Swift UVOT refined analysis
DATE:    14/04/19 21:55:33 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (UCL-MSSL) 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 140419A
97 s after the BAT trigger (Marshall et al. GCN Circ. 16118).
Optical and IR photometry and positions were reported, as well as a redshift
(Cenko, et al., GCN Circ. 16129; Hentunen et al., GCN Circ. 16126; Tanvir
et
al., GCN Circ. 16125; Kuin et al., GCN Circ. 16123; Butler et al., GCN
Circ.
16121; Guver et al., GCN Circ. 16120; and Zheng et al., GCN Circ. 16119.)
 A source consistent with the XRT position is detected in the initial UVOT
exposures.

The preliminary UVOT position is:
    RA  (J2000) =  08:27:57.56 = 126.98982 (deg.)
    Dec (J2000) = +46:14:25.3  =  46.24037 (deg.)
with an estimated uncertainty of 0.50 arc sec. (radius, 90% confidence).

Due to the GRB lying on the edge of a large scattered light feature from
the
bright star nearby, photometry errors are large until a good background
template can be made at late times.
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               97          246          147         16.2 +/- 0.2
v                  638          658           19         16.1 +/- 0.2
b                  564          756           39         18.4 +/- 0.2
u                  309         2003          362        >21.0
w1                 687          707           19        >18.1

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: GRB140419A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16131
SUBJECT: GRB 140419A: MITSuME Okayama Optical Observation
DATE:    14/04/20 07:34:30 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

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

We observed the field of GRB 140419A (Marshall et al., GCNC 16118)
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 2014-04-19 11:17:09 UT (~7.2 h after the burst).
We detected the previously reported afterglow (Marshall et al., GCNC 16118;
Zheng et al., GCNC 16119) in Rc and Ic bands.

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

#T0+[day]  MID-UT    T-EXP[sec]   g'     Rc  Rc_err   Ic  Ic_err
-----------------------------------------------------------------------
0.36126    12:47:03    8700.0    >20.1  19.8  0.3    19.1  0.3
------------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB140419A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16132
SUBJECT: GRB 140419A: MITSuME Ishigakijima Optical Observation
DATE:    14/04/20 10:22:25 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 collaboration:

We observed the field of GRB 140419A (Marshall et al., GCNC 16118)
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 2014-04-19 12:40:26 UT (~8.6 h after the burst).
We detected the previously reported afterglow (Marshall et al., GCNC 16118;
Zheng et al., GCNC 16119) 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
----------------------------------------------------------------------
0.39781    13:39:41    5820.0    20.6  0.1    19.5  0.1    19.1  0.1
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB140419A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16133
SUBJECT: GRB 140419A, Optical Observations
DATE:    14/04/20 14:50:33 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 140419A field (Marshall et al., GCN 16118) using
1.04m ST telescope at ARIES Nainital. Observations were started at 14:44:38
UT on 2014-04-19 (approximately 10.6 h after the burst). Several frames
with an exposure time of 300 s each in R_c band were obtained in good sky
conditions.

The optical counterpart of GRB 140419A (Zheng et al., GCN 16119; Guver et
al., GCN 16120; Butler et al.,GCN 16121; Kuin et al., GCN 16123; Hentunen
et al., GCN 16126; Cenko et al., GCN 16129) is clearly detected  in each
individual frames. The preliminary photometry of the first frame is 19.8 +-
0.1 mag. The photometry was performed in comparison to nearby USNO stars.

This massage may be cited.


GRB_name: GRB140419A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16134
SUBJECT: Konus-Wind observation of GRB 140419A
DATE:    14/04/20 15:07:10 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, and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration, intense GRB 140419A
(Swift-BAT trigger #596426: Marshal et al., GCN 16118;
Baumgartner et al., GCN 16127)
triggered Konus-Wind at T0=14811.110 s UT (04:06:51.110).

The burst light curve shows a broad, hard-spectrum pulse
from ~T0-10 s to ~T0+40 s and a complex of narrow,
softer pulses around ~T0+50 s.
The total duration of the burst is ~80 s.
The emission is seen up to several MeV, however
the energy channels above ~2 MeV are strongly affected
by the high and variable solar particle background.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140419_T14811/

As observed by Konus-Wind, the burst
had a fluence of 5.8(-1.9,+2.8)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+7.744 s,
of 4.7(-1.9,+1.8)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+76.032 s)
is best fit in the 20 keV - 1.9 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.63 (-0.22,+0.36),
the high energy photon index beta = -2.3 (-2.5,+0.4),
the peak energy Ep = 293 (-84,+84) keV,
chi2 = 51.1/59 dof.

The spectrum near the maximum count rate
(measured from T0+6.144 to T0+17.408 s)
is best fit in the 20 keV - 1.9 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.52 (-0.20,+0.24),
the high energy photon index beta = -2.3 (-2.7,+0.4),
the peak energy Ep = 363 (-75,+96) keV,
chi2 = 70.7/60 dof.

Assuming the redshift z=3.956 (Tanvir et al., GCN 15645)
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 ~1.9x10^54 erg,
the peak luminosity L_iso is ~7.5x10^53 erg/s,
and the rest-frame peak energy Ep,i is ~1450 keV.
These estimates place GRB 140419A among the most
energetic GRBs.

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


GRB_name: GRB140419A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16136
SUBJECT: GRB 140419A: Continued RATIR Optical and NIR Observations
DATE:    14/04/21 01:18:52 GMT
FROM:    Owen Littlejohns at Az State U  <olittlej@asu.edu>

Owen Littlejohns (ASU), 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), 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 140419A (Marshall, et al., GCN 16118) 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 2014/04 20.14 to 2014/04 20.29
UTC (23.23 to 26.83 hours after the BAT trigger), obtaining a total of
2.49 hours exposure in the r and i bands and 1.04 hours exposure in the Z,
Y, J, and H bands.

We continue to detect the UVOT optical transient (Zheng, et al., GCN 16116;
Guver et al., GCN 16120). For a source within the GCN-16119 error circle,
in comparison with the SDSS DR9 and 2MASS, we obtain the following
detections:

  r     21.35 +/- 0.04
  i     20.76 +/- 0.04
  Z     20.61 +/- 0.06
  Y     20.45 +/- 0.07
  J     20.35 +/- 0.08
  H     20.32 +/- 0.10

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB. In comparison to the previous
epoch of RATIR observations (Butler, et al., GCN 16121) we find that the
source has continued to fade with an approximate power-law index of
alpha = 1.2 in all six bands.

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


GRB_name: GRB140419A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16137
SUBJECT: GRB 140419A: KAIT Refined Analysis
DATE:    14/04/21 05:21:29 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) at
Lick Observatory responded to Swift GRB 140419A (Marshall et al.,
GCN 16118) starting at 04:10:00 UT, 189 s after the burst.
Observations were performed with an automatic sequence in the
V, I, and clear (roughly R) filters, and the exposure time was
20 s per image. The bright optical afterglow (Zheng et al.,
GCN 16119; Guver et al., GCN 16120) was well detected in
all three filters. Preliminary analysis shows that the afterglow
decays with a single power law (with alpha = -1.15) from the
beginning of our observations until about 3 hours later when the
position moved beyond our reach. The power-law index is consistent
with the value reported by Butler et al. (GCN 16121; GCN 16136).
We find (V - I) about 1.7 mag (no extinction correction), and no
obvious color change was detected during our observations. A
preliminary light curve is posted at
http://astro.berkeley.edu/~zwk/grb/GRB140419A/GRB140419A_kait.png


GRB_name: GRB140419A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16138
SUBJECT: GRB140419A: NOT optical observations
DATE:    14/04/21 17:59:57 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), T. Kruehler (ESO), N. Tanvir (U. Leicester), F.
Taddia, C. Fremling (Stockholm U.) report on behalf of a larger
collaboration:

We observed the optical afterglow of GRB 140419A (Marshall et al., GCN
16118; Zheng et al., GCN 16119; Kuin et al., GCN 16123) using the 2.5
Nordic Optical Telescope equipped with ALFOSC. We obtained 4x300s,
3x300s, 4x200s frames in the SDSS g-, r-, and i-filters, respectively,
with floating clouds, starting at 23:10 UT on 2014-04-20 .

Photometry is calibrated with nearby SDSS stars, and results are as follows:

Tmid-T0(hr)        Mag       MagErr
   43.24              >22.5
   43.54              23.16      0.15
   43.86              >20.3

Compared with previous measurements (e.g., from RATIR and KAIT), the
afterglow may be decaying more quickly.


GRB_name: GRB140419A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16139
SUBJECT: GRB 140419A: Continued RATIR Optical and NIR Observations
DATE:    14/04/21 19:19:13 GMT
FROM:    Owen Littlejohns at Az State U  <olittlej@asu.edu>

Owen Littlejohns (ASU), 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), 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 140419A (Marshall, et al., GCN 16118) 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 2014/04 21.14 to 2014/04 21.29 UTC (47.30
to 50.93 hours after the BAT trigger), obtaining a total of 2.49 hours
exposure in the r and i bands and 1.04 hours exposure in the Z, Y, J, and
H bands.

We continue to detect the UVOT optical transient (Zheng, et al., GCN 16116;
Guver et al., GCN 16120). For a source located at the position of the KAIT
optical counterpart candidate (Zheng, et al., GCN 16119), in comparison with
the SDSS DR9 and 2MASS, we obtain the following detections and upper limit
(3-sigma):

  r     21.92 +/- 0.07
  i     21.77 +/- 0.07
  Z     21.74 +/- 0.13
  Y     21.58 +/- 0.19
  J     21.54 +/- 0.21
  H     > 21.66

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB. In comparison to the first two
epochs of RATIR observations (Littlejohns, et al., GCN 16136; Butler, et
al., GCN 16121) we note that the decay in the NIR bands appears steeper,
now consistent with 1.4 < alpha < 1.6 in the i, Z, Y, J and H bands (see
also; Xu et al., GCN 16138). The XRT data for this GRB
(http://www.swift.ac.uk/xrt_curves/00596426/) may support a temporal break
at low significance after 100 ks. Further XRTdata can constrain this
possibility.

Conversely, the decay observed in the r band has become shallower, with
alpha = 0.8. This shallow decay in the r band could be attributed to the
presence of an underlying host galaxy or contamination from the nearby
bright star.

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


GRB_name: GRB140419A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16140
SUBJECT: GRB 140419A: Refined NOT photometry
DATE:    14/04/21 20:30:09 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI) reports:

The photometry of the NOT SDSS r-band data in GCN 16138 has been
refined. The detected object is not point-like but somewhat extended
in the NOT image. The photometry in GCN 16138 only covers a seemingly
bright part of the extended object. If the whole object is covered,
the brightness changes to m(R)=21.60+/-0.20 calibrated with the same
nearby SDSS stars, which now is consistent with the decaying law
derived from pre- and post-NOT observations (e.g., from RATIR; GCN
16139).

We thank Antonino Cucchiara for pointing out the difference in magnitudes.


GRB_name: GRB140419A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16141
SUBJECT: GRB 140419A: Mondy optical observations
DATE:    14/04/22 14:44:54 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 the field of the Swift GRB 140419A (Marshall et al., GCN
16118) with AZT-33IK telescope of Sayan observatory (Mondy) on Apr. 
19-21. We took several images in R-filter of 60 s exposure. On stacked 
images we clearly detected the optical afterglow (Zheng et al., GCN 
16119; Guver et al., GCN 16120; Butler et al., GCN 16121; Kuin et al.,
GCN 16123; Hentunen et al., GCN 16126) except the combined image of
Apr. 19 due to unfavorable weather conditions. Our photometry is 
consistent with the decaying law derived from RATIR observations 
(Littlejohns et al., GCNs 16139, 16136).

The details of the photometry are the following:

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

2014-04-19 16:26:35   0.52030   R      10*60  n/d             19.3
2014-04-20 14:49:15   1.47495   R      83*60  21.12 +/- 0.10  21.6
2014-04-21 14:58:36   2.49015   R     107*60  21.60 +/- 0.15  22.2

The photometry is based on nearby SDSS star, R (gri -> R transformations 
by Lupton 2005):

SDSS id              R
J082752.69+461357.4  17.381 +/- 0.018


GRB_name: GRB140423A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16142
SUBJECT: GRB 140423A: Swift detection of a burst
DATE:    14/04/23 08:44:16 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

E. Sonbas (NASA/GSFC/Adiyaman Univ.), M. M. Chester (PSU),
K. L. Page (U Leicester) and T. N. Ukwatta (MSU) report on behalf of
the Swift Team:

At 08:31:53 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140423A (trigger=596901).  Swift did not slew immediately
due to an observing constraint.  The BAT on-board calculated location is 
RA, Dec 197.290, +49.815 which is 
   RA(J2000) = 13h 09m 10s
   Dec(J2000) = +49d 48' 52"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a multi-peak
structure with a duration of about 80 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~20 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+47.2
minutes. There will be no XRT or UVOT data until 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.)

[GCN OPS NOTE(23apr14):  The second sentence was corrected to indicate
a delayed (not immediate) slew.]


GRB_name: GRB140423A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16143
SUBJECT: GRB 140423A: optical afterglow  candidate
DATE:    14/04/23 09:32:14 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed of  the field of  the Swift GRB 140423A (Sonbas et al.,  GCN 
16142)  with 0.4-m telescope of ISON-NM observatory starting
on Mar., 20 (UT)  09:01:03.  The start of observation was delayed due to bad 
weather. We took unfiltered images of 30 s exposures. We detect a fading 
optical source  in coordinates

(J2000)  13 09 08.50 +49 50 29.4

(with initial accuracy of about 1 arcsec). Preliminary photometry of the 
source in the first   images is  ~ 17.2m. the photometry is based on nearby 
USNO-B1.0 stars (R2 mag). Since the source is absent in USNO-B1.0 catalog 
and clearly fading we suggest it as GRB 140423A afterglow candidate.

[GCN OPS NOTE(23apr14): Please see 16148 for the correction on the start date.
Also added the "A" on the GRB name in the first and last sentences.] 


GRB_name: GRB140423A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16144
SUBJECT: GRB 140423A optical observations with pODI/WIYN at KPNO
DATE:    14/04/23 09:49:53 GMT
FROM:    Dieter Hartmann at Clemson.U  <hdieter@clemson.edu>

A. Kaur (Clemson U.), A. Delgado-Navarro (Clemson U.), D. Harbeck (WIYN
Observatory), M. Riabokin (NOAO), M. Orio (INAF, UW Madison), D. H.
Hartmann (Clemson U.) report on behalf of a larger collaboration:



We imaged the location of the Swift detected GRB 140423A (Sonbas et al.,
GCN 16142) with the pODI instrument on the 3.5 m WIYN telescope at KPNO (
http://www.wiyn.org/ODI/About/wiynpODI.html).



Observations in the ODI r' band began at 09:40:38 UT on 23 April 2014. We
clearly detect the optical afterglow candidate indicated by Elenin et al.
(GCN 16143) in individual exposures beginning at this time.


GRB_name: GRB140423A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16145
SUBJECT: GRB 140423A: ROTSE-III Detection of Optical Counterpart
DATE:    14/04/23 10:01:48 GMT
FROM:    Farley V. Ferrante at Southern Methodist U/ROTSE  <fferrante@smu.edu>

F. V. Ferrante (SMU), T. Guver (Istanbul Univ.), H. Flewelling (IfA/Hawaii), R. Kehoe (SMU),
and G. Dhungana (SMU) report on behalf of the ROTSE GRB team:

ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB 140423A
(Swift trigger 596901, GCN 16142; Elenin et al., GCN 16143; A. Kaur et al., GCN 16144).
The first image was at 08:32:45.1 UT, 51.5 s after the burst (0.1 s after the GCN notice time).
The unfiltered images are calibrated relative to USNO A2.0. We detect a 14.2 magnitude,
fading source with coordinates:

     13:09:08.08      +49:50:26.5    (J2000), with positional uncertainty of 1" or better

start UT        mag     mlim(of image)
----------------------------------
08:33:39.6     14.2     16.0

This source is not visible in DSS (second epoch), 2MASS or the MPChecker database.

The object decayed from ~14.2 magnitude to ~15.0 magnitude in ~100 seconds.

A jpeg image is available at http://www.rotse.net/images/gsq596901_3b01_img.jpg

Continuing observations are in progress.


GRB_name: GRB140423A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16146
SUBJECT: GRB 140423A: Swift-XRT observations
DATE:    14/04/23 10:13:31 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

The XRT began observing the field of GRB 140423A at 09:20:56.7 UT,
2943.5 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source located at RA, Dec 197.28927,
49.84233 which is equivalent to:
   RA(J2000)  = 13h 09m 09.42s
   Dec(J2000) = +49d 50' 32.4"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 98 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (1.09 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 3.4
(+2.57/-1.42) x 10^21 cm^-2 (90% confidence). 


GRB_name: GRB140423A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16147
SUBJECT: GRB 140423A:  Swift/UVOT detection of a possible counterpart
DATE:    14/04/23 10:49:48 GMT
FROM:    Margaret Chester at PSU  <chester@swift.psu.edu>

M. M. Chester (PSU), E. Sonbas (NASA/GSFC/Adiyaman Univ.), K. L. Page 
(U Leicester), D. Malesani (DARK/NBI), and S. R. Oates (UCL-MSSL)
report on behalf of the Swift/UVOT team:


Swift/UVOT took a finding chart exposure of 150 seconds with the White filter
starting 2946 seconds after the BAT trigger. A faint source (19.6 +/- 0.4 mag) 
is detected in the White filter which is consistent with the candidate reported 
by Elenin et al. (GCN Circ. 16143) but not consistent with the Swift/XRT position 
reported by D. N. Burrows et al. (GCN Circ. 16146).  The separation from the XRT 
position is 9.6 arcsec.  The preliminary UVOT position is

   RA (J2000)  197.28546 (13:09:08.51)
  Dec (J2000)   49.84133 (+49:50:28.8)

with an estimated uncertainty of 1.1 arcsec (radius, 90% confidence,
statistical + systematic).  No correction has been made for the
expected extinction corresponding to E(B-V) of 0.01.


GRB_name: GRB140423A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16148
SUBJECT: GRB 140423A:  ISON-MN early photometry and correction to the GCN circ. 16143
DATE:    14/04/23 11:01:48 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

After detection of the optical afterglow of GRB 140423A (Elenin et al., GCN 
16143; Kaur et al., GCN 16144; Ferrante et al., GCN 16145) and X-ray 
afterglow (Burrows et al., GCN 16146)   we report initial photometry of our 
first images taken with ISON-NM observatory:

UT start   t-T0              Exp.  Filter   OT
              (mid.,days)    (s)
09:01:18  0.02043        30     Clear   17.11 +/- 0.17
09:06:49  0.02426        30     Clear   17.60 +/- 0.21

The photometry is based on star SDSS J130858.37+494547.9 (assuming R = 
15.418 +/- 0.018).

The finding chart of GRB 140423A afterglow can be found in 
http://grb.rssi.ru/GRB140423A/GRB140423A_ISON-NM_fc.png

Also we report the corect time of observation of the first image in GCN 
16143. It  should be April, 23,  (UT)  09:01:03.
We apologize for the misprint. 


GRB_name: GRB140419A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16149
SUBJECT: GRB 140419A, LOAO R-band observations
DATE:    14/04/23 12:04:51 GMT
FROM:    Changsu Choi at Seoul Nat U  <changsu@astro.snu.ac.kr>

Changsu Choi, Myungshin Im (CEOU/SNU), Hyun-Il Sung (KASI), and Yuji Urata
(NCU), on behalf of EAFON

We observed the field of GRB 140419A Swift GRB 140419A (Marshall et al., GCN
16118) in R-band using the 1-m telescope at Mt. Lemmon Optical Observatory
(LOAO) in Arizona, US

We obtained R-band images at two epochs on Apr. 19 and on Apr. 21. 
We marginally identify the afterglow in a stacked image for each night. 
The photometry is based on R1-mag of USNO-B1 stars in the observed field.

Details of Photometry are below:

date                          UT(mid time)         Filter           mag

2014/04/19                   07:30:51               R         18.64 +/-0.29 
2014/04/21                   03:39:38               R         21.43 +/-0.27

 


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


GRB_name: GRB140423A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16150
SUBJECT: GRB 140423A: Gemini-N redshift
DATE:    14/04/23 12:14:10 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir (U. Leicester), A. J. Levan (U. Warwick), K. Wiersema (U. Leicester),
A. Petric, K. Chiboucas, J. Miller (Gemini) report:

We observed the afterglow of GRB 140423A (Sonbas et al. GCN 16142;
Elenin et al. GCN 16143; Kaur et al. GCN 16144; Ferrante et al. GCN 16145;
Chester et al. GCN 16147) with the GMOS-N spectrograph on Gemini-N.
Observations began at 10:25 UT, approximately 1.9 hr post burst.

The spectra show absorption lines due to Ly-alpha, SiII (1251/1254),
SiII* (1265), OI (1302), SiII (1304), CII (1334), SiIV (1394/1403), 
SiII (1527), CIV (1548/1551) at a common redshift of z=3.26, which 
we infer is the redshift of the GRB.


GRB_name: GRB140423A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16151
SUBJECT: GRB 140423A: KWFC z-band photometry
DATE:    14/04/23 13:55:20 GMT
FROM:    Nozomu Tominaga at Konan U  <tominaga@konan-u.ac.jp>

Hiroyuki Maehara (Univ. of Tokyo), Nozomu Tominaga (Konan Univ.), Tomoki Morokuma (Univ. of Tokyo) and Masaomi Tanaka (NAOJ) on
behalf of OISTER collaboration:

We observed the field of GRB 140423A (Sonbas et al., GCN 16142) with the 1.05-m Schmidt telescope and KWFC (Sako et al. 2012, Proc.
SPIE 8446, 84466L) at Kiso Observatory in Japan.

The observation was made in the Sloan z-band at 2014-04-23 10:30 (UT), approximately 2 hours post burst. 

We have also detected the optical source (Elenin et al., GCN 16143, 16148; Kaur et al. GCN 16144; Ferrante et al., GCN 16145;
Chester et al., GCN 16147) at RA=13:09:08.54, DEC=+49:50:29.3 (J2000).$B!!(BPreliminary photometry of the source is as follows.

obs. date (mid time)  Tmid-T0 (hr)  exp. time   filter      mag      limiting mag
2014-04-23 10:30:11     1.97         300 sec      z      18.6+/-0.1     19.5

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


GRB_name: GRB140423A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16152
SUBJECT: GRB 140423A: Fermi GBM observation
DATE:    14/04/23 15:29:40 GMT
FROM:    Andreas von Kienlin at MPE  <azk@mpe.mpg.de>

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

"At 08:32:38.54 UT on 23 April 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140423A (trigger 419934761 / 140423356)
which was also detected by the Swift/BAT (Sonbas et al. 2014, GCN 16142)
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 44 degrees.

The GBM light curve shows a multiple-peak structure 
with a duration (T90) of about 95 s (50-300 keV).
The time-averaged spectrum from T0-61.440 s to T0+32.768 s is
best fit by a Band function with Epeak = 125 +/- 9 keV,
alpha = -0.25 +/- 0.11, and beta = -1.97 +/- 0.06. 

The event fluence (10-1000 keV) in this time interval is
(2.0 +/-0.1)E-05 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+5.44 s in the 10-1000 keV band
is 3.0 +/- 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: GRB140423A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16153
SUBJECT: GRB 140423A: P60 Observations
DATE:    14/04/23 17:09:05 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 optical afterglow (Elenin et al., GCN 16143; Kaur et al., GCN 16144; Ferrante et al., GCN 16145; Chester et al., GCN 16147; Maehara et al., GCN 16151) of the Swift GRB 140423A (Sonbas et al., GCN 16142) with the robotic Palomar 60 inch telescope. Observations were obtained in the r', i', and z' filters beginning at 9:55 UT on 2014 April 23 (84 minutes after the Swift trigger).

The optical afterglow is clearly detected in all three filters. Using nearby point sources from SDSS for calibration, we measure the following magnitudes in our initial images:

r' = 18.87 +/- 0.05 at dt = 84.0 min
i' = 18.71 +/- 0.05 at dt = 87.0 min
z' = 18.67 +/- 0.11 at dt = 88.4 min

Further observations are planned.


GRB_name: GRB140423A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16154
SUBJECT: GRB 140423A: Nanshan optical upper limit
DATE:    14/04/23 17:26:52 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), X. Zhang, C.-H. Bai, A. Esamdin, L. Ma (XAO) report:

We observed the optical afterglow field of GRB 140423A (Sonbas et al.,
GCN 16142; Elenin et al., GCN 16143; Kaur et al., GCN 16144;) using
the 1m telescope located at Nanshan, Xinjiang, China. Three R-band
frames were obtained under rather bad weather. The afterglow has
decayed down to a limiting magnitude of m(R)>19.4 mag at a mean time
of 8.216 hr post-burst, calibrated with nearby SDSS stars.


GRB_name: GRB140423A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16155
SUBJECT: GRB 140423A: Enhanced Swift-XRT position
DATE:    14/04/23 18:17:20 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 5971 s of XRT Photon Counting mode data and 15 UVOT
images for GRB 140423A, 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 = 197.28544, +49.84152 which is equivalent
to:

RA (J2000): 13h 09m 8.51s
Dec (J2000): +49d 50' 29.5"

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

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

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


GRB_name: GRB140423A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16156
SUBJECT: GRB 140423A: KAIT Optical Detection
DATE:    14/04/23 18:58:38 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 140423A (Sonbas et al.,
GCN 16142) starting at 08:33:55 UT, 122 s after the burst.
Observations were performed with an automatic sequence in the
V, I, and clear (roughly R) filters, and the exposure time was
20 s per image. The bright optical afterglow (Elenin et al., GCN
16143; Kaur et al., GCN 16144; Ferrante et al., GCN 16145; Chester
et al., GCN 16147; Maehara et al., GCN 16151; Cenko et al., GCN
16153) was well detected in all three filters. Preliminary analysis
shows that the afterglow had a rather broad peak at t = 150-250 s with
R ~ 14.3 mag. It decayed faster after ~1000 s, with a single power
law having alpha about -1.7. A preliminary light curve is posted at
http://astro.berkeley.edu/~zwk/grb/GRB140423A/GRB140423A_kait.png


GRB_name: GRB140423A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16157
SUBJECT: GRB 140423A: Further Observations with Swift/UVOT
DATE:    14/04/23 21:12:24 GMT
FROM:    Margaret Chester at PSU  <chester@swift.psu.edu>

M. M. Chester (PSU), E. Sonbas (NASA/GSFC/Adiyaman Univ.), and 
F. E. Marshall (NASA/GSFC) report on behalf of the Swift/UVOT team:

Further analysis confirms UVOT's detection of the afterglow of GRB 140423A
(Sonbas et al., GCN Circ. 16142) reported by Elenin et al. (GCN Circ. 16143).

The UVOT position based on the initial exposure is:
   RA  (J2000) =  13:09:08.54 = 197.28558 (deg.)
   Dec (J2000) = +49:50:29.4  =  49.84150 (deg.)
with an estimated uncertainty of 0.48 arc sec. (radius, 90% confidence).
This position is consistent with the enhanced XRT position reported by 
Beardmore et al. (GCN Circ. 16155).

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             2947         3097          147         19.80 +/- 0.09
v                 3104         3303          197         19.33 +/- 0.19
b                 3924         4123          197         19.96 +/- 0.16
u                 3719         5353          393        >21.3
w1                3513         5148          393        >21.7
m2                4743         4943          197        >20.7
w2                4334        11161          808        >22.1

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: GRB140423A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16160
SUBJECT: GRB 140423A: MITSuME Okayama Optical Observation
DATE:    14/04/24 04:30:15 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

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

We observed the field of GRB 140423A (Sonbas et al., GCNC 16142)
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 2014-04-23 10:43:36 UT (~2.2 h after the burst).
We detected the previously reported afterglow (Elenin et al., GCNC 16143;
Kaur et al., GCNC 16144; Ferrante et al., GCNC 16145) 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
-----------------------------------------------------------------------
0.21728    13:44:45    5880.0     20.1 0.3    20.1 0.2     19.5 0.3
------------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB140423A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16161
SUBJECT: GRB 140423A: Swift-BAT refined analysis
DATE:    14/04/24 04:43:09 GMT
FROM:    Tilan Ukwatta at MSU  <tilan.ukwatta@gmail.com>

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), E. Sonbas (NASA/GSFC/Adiyaman Univ.),
M. Stamatikos (OSU), J. Tueller (GSFC),
T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):

Using the data set from T-239 to T+963 sec from the recent
telemetry downlink, we report further analysis of BAT
GRB 140423A (trigger #596901) (Sonbas, et al., GCN Circ. 16142).
The BAT ground-calculated position is
RA, Dec = 197.276, 49.838 deg which is
   RA(J2000)  =  13h 09m 06.2s
   Dec(J2000) = +49d 50' 18.3"
with an uncertainty of 1.0 arcmin, (radius, sys+stat,
90% containment). The partial coding was 39%.

The mask-weighted light curve shows a multi-peak episode
starting ~T-50 sec, highest peak at ~T+45 sec, and the episode
ends around ~T+140 sec. T90 (15-350 keV) is 134 +- 23 sec
(estimated error including systematics).

The time-averaged spectrum from T-130.13 to T+108.91 sec
is best fit by a simple power-law model. The power law index
of the time-averaged spectrum is 1.33 +- 0.06. The fluence
in the 15-150 keV band is 9.4 +- 0.3 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T+44.19 sec in
the 15-150 keV band is 2.1 +- 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/596901/BA/


GRB_name: GRB140423A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16162
SUBJECT: GRB 140423A: Swift-XRT refined Analysis
DATE:    14/04/24 05:24:46 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

A. Amaral-Rogers (U. Leicester), K.L. Page (U. Leicester) and E. Sonbas
(NASA/GSFC/Adiyaman Univ.) report on behalf of the Swift-XRT team:

We have analysed 11 ks of XRT data for GRB 140423A (Sonbas  et al. GCN
Circ. 16142),  from 3.0 ks to 40.0 ks after the  BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Beardmore et al. (GCN Circ. 16155).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.00 (+/-0.05).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.08 (+/-0.09). The
best-fitting absorption column is  5.0 (+2.0, -1.8) x 10^20 cm^-2, in
excess of the Galactic value of 1.1 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.1 x 10^-11 (3.6 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.0 (+2.0, -1.8) x 10^20 cm^-2
Galactic foreground: 1.1 x 10^20 cm^-2
Excess significance: 3.5 sigma
Photon index:      2.08 (+/-0.09)

If the light curve continues to decay with a power-law decay index of
1.00, the count rate at T+24 hours will be 0.027 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 8.5 x
10^-13 (9.8 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/00596901.

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


GRB_name: GRB140423A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16163
SUBJECT: GRB 140423A: Kanata/HONIR Optical and NIR Observations
DATE:    14/04/24 08:15:36 GMT
FROM:    Michitoshi Yoshida at HASC,Hiroshima U  <yoshidam@hiroshima-u.ac.jp>

Hiroshi Akitaya, Yuki Moritani, Takahiro Ui, Yuka Kanda, and Michitoshi
Yoshida (Hiroshima Univ.) on behalf of the OISTER collaboration:

We observed the field of GRB140423A (Sonbas et al., GCNC 16142) with
the optical and near-infrared simultaneous imager HONIR (Sakimoto et
al. 2012, Proc.SPIE 8446, 844673) attached to the 1.5-m Kanata
Telescope at Higashi-hiroshima Observatory, Japan.

We detected the afterglow at R_C and J bands at 2014-04-23 10:46 UT
(~2.2 hours after the burst). Photometric results are as follows.

MID-UT           Total exp[sec]  Band  Mag     Mag_err
----------------------------------------------------------
2014-04-23 10:46      720        Rc    19.4    0.3
2014-04-23 10:46      792        J     17.3    0.2
----------------------------------------------------------


GRB_name: GRB140423A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16164
SUBJECT: GRB 140423A, Optical Observations
DATE:    14/04/24 10:12:16 GMT
FROM:    Shashi Bhushan Pandey at ROTSE  <shaship@umich.edu>

S. B. Pandey, Brajesh Kumar and Aditi Agarwal (ARIES Nainital India,
on behalf of larger Indian GRB collaboration)

We observed the Swift GRB 140423A field (Sonbas et al., GCN 16142)
using 1.3m DFOT telescope at Devasthal operated by ARIES Nainital, India.
Observations were started at 14:36:07 UT on 2014-04-23 (~6 h after the
burst).
The optical counterpart of the burst (Elenin et al., GCN 16143; Kaur et
al.,
GCN 16144; Ferrante et al., GCN 16145; Chester et al., GCN 16147) was
clearly
detected in individual frames of exposure time 300s each.

The preliminary photometry is as following:

 (UT)Start     filter    exp(sec)       mag
 14:36:07     R_c       300            20.12 +/- 0.08
 14:42:50     I_c         300           19.76 +/- 0.15

The photometry was performed in comparison to nearby USNO stars.

This message may be cited.


GRB_name: GRB140423A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16165
SUBJECT: GRB 140423A pODI/WIYN afterglow photometry
DATE:    14/04/24 11:00:08 GMT
FROM:    Dieter Hartmann at Clemson.U  <hdieter@clemson.edu>

D. Harbeck (WIYN Observatory), A. Kaur (Clemson U.), A. Delgado-Navarro
(Clemson U.), M. Orio (INAF, UW Madison), D. H. Hartmann (Clemson U.)
report on behalf of a larger collaboration:



We imaged the location of the Swift detected GRB 140423A (Sonbas et al.,
GCN 16142) at two epochs with the pODI instrument on the 3.5 m WIYN
telescope at KPNO (http://www.wiyn.org/ODI/About/wiynpODI.html).



Observations in the sdss r' band on 23 April 2014 consist of a single 300s
exposure, and on 24 April 2014 we performed two 600s exposures. The optical
counterpart of the burst (Elenin et al., GCN 16143; Kaur et al., GCN 16144;
Ferrante et al., GCN 16145; Chester et al., GCN 16147) was detected under
fair seeing conditions (~ 1 arcsec) in all single exposures.



Date            Exp. Start Time        Magnitude



2014-04-23 UT 09:52:50.400         r' = 18.85



2014-04-24 UT 08:29:12.393         r' = 21.90



2014-04-24 UT 08:41:12.901         r' = 21.85



The photometric error is dominated by calibration and is 0.07 mag (in r')
rms for a secondary reference star ensemble (but not accounting for color
terms or galactic foreground extinction).



The photometric calibration is based on

(i) cross-correlating with the sdss dr9 star catalog in the r' band over
the entire field of view (24' X 24')

(ii) consistency check on exemplary star  SDSS J130915.57+494948.5 at sdss
r' = 19.98. The photometric error based on this reference star is < 0.02
mag rms.


GRB_name: GRB140423A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16166
SUBJECT: GRB 140423A: TNG NIR observations
DATE:    14/04/24 13:35:25 GMT
FROM:    Stefano Covino at Brera Astronomical Observatory  <stefano.covino@brera.inaf.it>

P. D'Avanzo, S. Covino, D. Malesani, A. Rossi, G. Tagliaferri, M. Pedani on behalf of the CIBO report:

We observed the field of GRB 140423A (Sonbas et al., GCN 16142) using the NICS 
near-Infrared camera on the 3.6m TNG Telescope (La Palma, Canary Islands).

We obtained a series of imaging observations in the J, H and K' bands(16 minutes per filter) 
at a mean epoch of 14.8 hours from the burst. The GRB afterglow is clearly detected in all bands. 
The observed J-band magnitude is 19.7 +- 0.1 (calibrated against the 2MASS catalogue).

[GCN OPS REPORT(24apr14): Per author's request, MP was added to the author list.]


GRB_name: GRB140423A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16167
SUBJECT: GRB 140423A: Nishi-Harima NIR Observations
DATE:    14/04/24 13:44:50 GMT
FROM:    Akira Arai at Nishi-Harima Astro. Obs/U of Hyogo  <arai@nhao.jp>

J. Takahashi and A. Arai (Univ. of Hyogo)
report on behalf of the Nayuta team and the OISTER collaboration:

We observed the field of GRB 140423A (Sonbas et al., GCN 16142)
with Nishiharima Infrared Camera (NIC) attached to the Nayuta 2-m
telescope at the Nishi-Harima Astronomical Observatory.

The observations were conducted on 2014-04-23 at 10:05-10:29 UT and
13:03-13:53 UT.
We detected the near-infrared afterglow in H and Ks bands.

Photometric results of our observations are listed below.
We used 2MASS 13085994+4951082 as a reference star for photometry.

# MID-UT   Tmid-T0 T-EXP  H_mag   Ks_mag*
-----------------------------------------------------------------------
10:17:20   1.76    300    17.0 +/- 0.2 16.6 +/- 0.2
10:25:50   1.90    300    17.2 +/- 0.2 16.6 +/- 0.2
13:11:00   4.65    480    17.7 +/- 0.2 17.1 +/- 0.3
13:27:16   4.93    480    17.7 +/- 0.2  --**
13:44:50   5.22    600    17.7 +/- 0.2  17.3 +/- 0.3
------------------------------------------------------------------------
Tmid-T0: Elapsed time after the burst (hours)
T-EXP: Total Exposure time (seconds)
* 2MASS Ks error for the reference star is not given, and thus it is
not included in our error estimates for the GRB afterglow,
** Photometry was not possible.


GRB_name: GRB140419A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16168
SUBJECT: GRB 140419A: Continued Mondy optical observations
DATE:    14/04/24 15:28:48 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 continued observation of the Swift GRB 140419A (Marshall et al., GCN
16118) with AZT-33IK telescope of Sayan observatory (Mondy) on Apr. 
19-21. We took several images in R-filter. On a stacked image we clearly 
detected the optical afterglow (Zheng et al., GCN 16119; Guver et al., 
GCN 16120; Butler et al., GCN 16121; Kuin et al., GCN 16123;  Hentunen 
et al., GCN 16126). Details of a photometry are the following:

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


2014-04-22 14:49:26   3.45342   R     120*60  22.18 +/- 0.09

The photometry is based on nearby SDSS star, R (gri -> R transformations 
by Lupton 2005):

SDSS id              R
J082752.69+461357.4  17.381 Â± 0.018


GRB_name: GRB140423A
Detection_method: KAIT
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16169
SUBJECT: GRB 140423A: NOT Afterglow Observations
DATE:    14/04/24 16:49:40 GMT
FROM:    Zach Cano at U of Iceland  <zewcano@gmail.com>

Z. Cano (U. Iceland), D. Malesani (DARK), S. Geier (NOT), J. J. Jensen
(DARK), F. Taddia, C. Fremling (Stockholm U.)

We observed the field of GRB 140423A (Sonbas et al., GCN 16142) with the
2.5-m Nordic Optical Telescope (NOT) equipped with ALFOSC starting at 23:32
UT on 23-Apr-2014. We obtained 2x150 s, 6x200 s and 7x200 s frames in
SDSS-r, SDSS-i and SDSS-z respectively.

The optical afterglow (
â€‹e.g. â€‹
Elenin et al., GCN 16143) is clearly detected in our co
â€‹-â€‹
added images.

A summary of our photometry:

filter    t-t0 (hr)      mag
---------------------------------------------
  r       15.06       21.46 +- 0.03
  i       15.33       21.28 +- 0.03
  z      15.78       21.36 +- 0.07


Our photometry has been calibrated using an SDSS star in the FOV
(13:09:09.56 +49:52:13.38, r=19.76 +- 0.02, i=19.23 +- 0.02, z=18.92 +-
0.04), it has not been corrected for foreground extinction, and the errors
include the uncertanity in the SDSS calibration star.

Comparing our observations with those in the GCNs, we derive a decay
constant of alpha~-1.0 relative to the photometry published by Cenko &
Perley (GCN 16153;
â€‹from â€‹
+1.4 hr to +15 hr), and alpha~-1.2 relative to the z-band photometry
published by Maehara et al. (GCN 16151;
â€‹from â€‹
+2hr to +15.8 hr) and the R-band photometry published by Pandey et al. (GCN
16164;
â€‹from â€‹
+6 hr to +15 hr), where a colour term of r-Rc~0.19 has been assumed in the
latter.  These decay rates are slower than those derived from the early
KAIT observations (Zheng et al., GCN 16156), who find alpha~-1.7 up to
about 6000 s.


GRB_name: GRB140423A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16170
SUBJECT: GRB 140423A: RATIR Optical and NIR Observations
DATE:    14/04/24 17:13:50 GMT
FROM:    Owen Littlejohns at Az State U  <olittlej@asu.edu>

Owen Littlejohns (ASU), 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), 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 140423A (Sonbas, et al., GCN 16142) 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 2014/04 24.29 to 2014/04
24.49 UTC (22.48 to 27.13 hours after the BAT trigger), obtaining a
total of 2.56 hours exposure in the r and i bands and 1.07 hours
exposure in the Z, Y, J, and H bands.

We detect the previously reported optical counterpart candidate
(Elenin, et al., GCN 16143; Chester, et al., GCN 16147; Chester, et
al., GCN 16157). For a source within the UVOT error circle (Chester,
et al., GCN 16147), in comparison with the SDSS DR9 and 2MASS, we
obtain the following detections:

  r     21.90 +/- 0.08
  i     21.79 +/- 0.07
  Z     21.65 +/- 0.19
  Y     21.39 +/- 0.17
  J     20.98 +/- 0.20
  H     21.33 +/- 0.26

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: GRB140413A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16172
SUBJECT: GRB 140413A: GROND Afterglow Confirmation
DATE:    14/04/25 12:56:00 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

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

We re-observed the field of GRB 140413A (Swift trigger 595616; D'Elia et
al., GCN # 16098) 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 La Silla
Observatory (Chile).

Further epochs were obtained at 1, 2, 3 and 5 days after the trigger. The
source detected in the XRT error circle in early observations (Varela et
al., GCN # 16099) has faded by about 3 magnitudes in the r' band,
confirming that it is the afterglow of GRB 140413A. In the later epochs we
obtain detections in g'r'i'z'J at a constant level, possibly the host
galaxy of the GRB. If it is the host galaxy, this may be indicative of a
relatively low redshift.


GRB_name: GRB140423A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16173
SUBJECT: GRB 140423A: MITSuME Akeno Optical observation 
DATE:    14/04/25 14:28:40 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

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

We observed the field of GRB 140423A (E. Sonbas et al., GCN Circular #16142) 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 2014-04-23 12:38:42 UT (4.1h after the burst).
We detected the previously reported optical afterglow of GRB140423A (D.Kuroda et al., GCN Circular #16160) in the Rc and Ic band.

The measured magnitudes were listed below.

T0+[sec]     MID-UT       T-EXP[sec]              g'                         Rc                      Ic
-------------------------------------------------------------------------------------------------------------------
19710       14:00:28         7740            20.49+/-0.23      19.83+/-0.15    19.72+/-0.22
31955       17:24:28         7560                    >21.3           20.35+/-0.19    19.89+/-0.23
-------------------------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst 
T-EXP: Total Exposure time 
We used GSC2.3 catalog for flux calibration.


GRB_name: GRB140423A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16174
SUBJECT: GRB 140423A: Continued RATIR Optical and NIR Observations
DATE:    14/04/25 22:10:59 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 140423A (Sonbas, et al., GCN 16142) 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 2014/04 25.15 to 2014/04 25.47 UTC (43.01 to
50.78 hours after the BAT trigger), obtaining a total of 4.07 hours
exposure in the r and i bands and 1.73 hours exposure in the Z, Y, J, and H
bands.

For a source within the Swift-UVOT error circle (Chester, et al., GCN
16147), in comparison with the SDSS DR9 and 2MASS, we obtain the following
detections and upper limit (3-sigma):

  r     22.70 +/- 0.11
  i     22.67 +/- 0.12
  Z     22.49 +/- 0.35
  Y     22.17 +/- 0.29
  J     > 21.66
  H     21.87 +/- 0.35

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.  Compared to our observations last
night (Littlejohns et al., GCN 16170), the source has faded approximately
as t^(-1.3).

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


GRB_name: GRB140423A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16175
SUBJECT: GRB 140423A Third epoch pODI photometry
DATE:    14/04/27 03:42:42 GMT
FROM:    Dieter Hartmann at Clemson.U  <hdieter@clemson.edu>

D. Harbeck (WIYN Observatory), A. Kaur (Clemson U.), A. Delgado-Navarro
(Clemson U.), M. Orio (INAF, UW Madison), D. H. Hartmann (Clemson U.)
report:



We re-imaged the location of the Swift detected GRB 140423A (Sonbas et al.,
GCN 16142) with the pODI instrument on the 3.5 m WIYN telescope at KPNO (
http://www.wiyn.org/ODI/About/wiynpODI.html).



Observations in the sdss r' band on 25 April 2014 consisted of one 300s
exposure, and one 600s exposures. The optical counterpart of the burst
(Elenin et al., GCN 16143; Kaur et al., GCN 16144; Ferrante et al., GCN
16145; Chester et al., GCN 16147) was detected under good conditions.



OBS DATE [UTC at start]      T_Exp   r' AB   stat-error seeing



2014-04-25 07:17:45.434       300.0    22.58    0.1          0.7"

2014-04-25 07:24:59.654       600.0    22.64    0.08        0.75"



Calibration was the same as described in our previous report. Calibration
rms without color correction is < 0.1", consistency check with nearby SDSS
star shows calibration variations < 0.02 mag. No color / foreground
extinction correction was applied.


GRB_name: GRB140423A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16176
SUBJECT: GRB 140423A: MITSuME Akeno upper limits
DATE:    14/04/28 12:03:53 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

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

We performed the follow-up observation for optical afterglow of GRB140423A(E.Sonbas et al., GCN Circular #16142, Elenin et al.,GCN Circular #16143 etc.) 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 2014-04-24 14:10:46 UT (31.1h after the burst).
We did not find the optical source on the position of GRB140423A.

The measured magnitudes were listed below.

T0+[sec]           MID-UT             T-EXP[sec]         g'     Rc       Ic
-------------------------------------------------------------------------
44700      14-04-24 15:42:02      9600          >21.3  >21.2  >20.6
-------------------------------------------------------------------------
T0+ : Elapsed time after the burst 
T-EXP: Total Exposure time 
We used GSC2.3 catalog for flux calibration.


GRB_name: GRB140428A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16177
SUBJECT: GRB 140428A: Swift Detection of a Possible Burst
DATE:    14/04/28 23:34:36 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

D. Kocevski (NASA/GSFC/ORAU), S. D. Barthelmy (GSFC),
A. Y. Lien (NASA/GSFC/ORAU), D. Malesani (DARK/NBI),
C. B. Markwardt (NASA/GSFC) and D. M. Palmer (LANL) report on behalf
of the Swift Team:

At 22:40:50 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140428A (trigger=597519).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 194.342, +28.357, which is 
   RA(J2000)  =  12h 57m 22s
   Dec(J2000) = +28d 21' 26"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  Most of the expected realtime products were
not available for this trigger so we have limited information.   We 
know that the trigger duration is 4 seconds and the image significance
is 9 sigma during that exposure.  A light curve is not yet available. 

We note that the position reported in TDRSS light curve notices are 
incorrect.  The position reported above is correct. 

Because of outage in the TDRSS telemetry downlink,
all but one BAT light curve notice and all of the XRT notices
are missing.  Only a pair of UVOT SourceList and Image notices were 
received on the ground. 

However, based on the strong detection in BAT, we believe that this is
most likely a real GRB.  We will issue a Circular when the full dataset
is downlinked. 

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: GRB140428A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16178
SUBJECT: GRB 140428A: Swift-XRT detection of a source
DATE:    14/04/29 05:13:35 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page (U. Leicester), D. Malesani (DARK/NBI) and D. Kocevski
(NASA/GSFC/ORAU) report on behalf of the Swift-XRT team:

We have analysed the initial downlinked Swift-XRT data for the possible
GRB 140428A (GCN Circ. 16177) and find a fading X-ray source within the
BAT field of view.

Using 1124 s of XRT Photon Counting mode data and 3 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 =
194.36852, 28.38490 which is equivalent to:

RA (J2000):  12h 57m 28.45s
Dec (J2000): +28d 23â€² 05.7â€²â€²

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).

The light curve can be modelled with a power-law decay with a decay index
of alpha=0.92 (+0.11,-0.10).

We therefore confirm that Swift trigger number 597519 is, indeed, a real
GRB.

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


GRB_name: GRB140428A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16179
SUBJECT: GRB 140428A: NOT observations
DATE:    14/04/29 05:39:59 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Malesani (DARK/NBI), D. Xu (DARK/NBI), H. Dahle (Univ. Oslo), E. Soto 
(CUA), report on behalf of the Nordic GRB collaboration:

We observed the field of GRB 140428A (Kocevski et al., GCN 16177) with 
the NOT equipped with the ALFOSC imager. Observations started on 2014 
Apr 29.223 UT (5.34 hr after the GRB) and consisted of 20 minutes in r 
and 12 in z.

Within the X-ray error circle (Page et al., GCN 16178), we do not find 
any object down to a depth r > 22.5 and z > 20.5 (all AB), calibrated to 
the SDSS.

DM thanks Thomas Kruehler (ESO) for insightful discussion.


GRB_name: GRB140428A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16180
SUBJECT: GRB 140428A: Keck detection of a red optical afterglow candidate
DATE:    14/04/29 07:23:15 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) reports:

I observed the position of GRB 140428A (Kocevski et al., GCN 16177; Page 
et al., GCN 16178) using LRIS on the Keck I 10-meter telescope.  A 
single 150-second imaging exposure was acquired simultaneously in both g 
and i filters.  An faint source is well-detected inside the XRT error 
circle in the i-band image at the following location (J2000):

RA  =  12:57:28.392
dec = +28:23:06.28

However, the object is completely absent in g-band.  Photometry relative 
to SDSS gives magnitudes of:

g > 26.42
i = 23.55 +/- 0.07

at a time of 06:09:30 UT (2014-04-29), 7.478 hours after the GRB trigger.

If this corresponds to the afterglow of the GRB, the red color suggests 
either a (moderately) high-redshift or dust-extinguished event.  Further 
observations are planned.


GRB_name: GRB140428A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16181
SUBJECT: GRB 140428A: Keck redshift estimate
DATE:    14/04/29 08:49:50 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) reports:

I re-observed the afterglow candidate of GRB 140428A in longslit mode 
using LRIS on the Keck I 10m telescope.  One 940-second exposure was 
taken using the 400/8500 grating (red camera) and 600/4000 grism (blue 
camera).

In a provisional reduction, the spectrum of the object shows a weak, 
flat continuum between 7000 Angstroms and the red limit of the 
wavelength range at approximately 10100 Angstroms.  The flux sharply 
drops to zero at 7000 angstroms, though there is faint flux detected in 
some places slightly further to the blue.  No trace is detected on the 
blue camera.

If the drop at 7000 Angstroms is interpreted as a DLA and the onset of 
the Lyman-alpha forest, this would indicate a redshift for this object 
of approximately z=4.7.


GRB_name: GRB140428A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16182
SUBJECT: GRB 140428A: 1.5m OSN I-band detection
DATE:    14/04/29 11:34:51 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

F.J. Aceituno (OSN/IAA-CSIC), A.J. Castro-Tirado (IAA-CSIC/UMA), R.
Sanchez-Ramirez (IAA-CSIC), J. Gorosabel (IAA-CSIC/UPV-EHU), report on
behalf of a larger collaboration:

We observed the field of GRB 140428A (Kocevski et al., GCN 16177; Page 
et al., GCN 16178) with the 1.5m OSN telescope at Observatorio de Sierra
Nevada. Three 300s images were acquired in the I-band starting on Apr 29,
00:09:39 UT (i.e. ~1.5 hours burst). A preliminary reduction clearly shows
the optical afterglow reported by Perley (GCNC 16180) with a Vega
magnitude of I~20.8. This magnitude must be taken with caution given the
likely presence of the Lyman-alpha break in the I-band filter pass-band.


GRB_name: GRB140428B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16184
SUBJECT: IPN Triangulation of GRB 140428B (short/hard)
DATE:    14/04/29 19:10:53 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, on behalf of the Interplanetary Network,

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

W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr, on
behalf of the GRS-Odyssey GRB 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, and V. Pelassa, on behalf of 
the Fermi GBM team, report:

The short-duration, hard spectrum GRB 140428B has been observed by
Fermi (GBM: trigger 420414281), INTEGRAL (SPI-ACS), Konus-Wind, and Mars 
Odyssey (HEND), so far, at about 78278 s UT (21:44:38).

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
   ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
     2.006 (00h 08m 01s) +68.172 (+68d 10' 20")
  Corners:
     6.132 (00h 24m 32s) +68.636 (+68d 38' 09")
     2.619 (00h 10m 29s) +68.455 (+68d 27' 18")
   358.176 (23h 52m 42s) +67.601 (+67d 36' 04")
     1.415 (00h 05m 40s) +67.887 (+67d 53' 13")
  ---------------------------------------------
The error box area is 0.608 sq. deg, and its maximum dimension is 3.14
deg (the minimum one is 18 arcmin).

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB140428_T78275/IPN/

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


GRB_name: GRB140423A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16185
SUBJECT: GRB 140423A: RTT150 optical observations
DATE:    14/04/29 19:47:26 GMT
FROM:    Rodion Burenin at IKI, Moscow  <rodion@hea.iki.rssi.ru>

I. Bikmaev (KFU/AST), I. Khamitov (TUG),
S. Melnikov, 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 140423A (Sonbas et al., GCN
16142) was observed with Russian-Turkish 1.5-m telescope (RTT150,
Bakirlitepe, TUBITAK National Observatory, Turkey) using the TFOSC
instrument.

We obtained series of 300 sec exposures in B and Rc filters with mean
time in April 24, 00:34 UT (B) and April 24, 01:58 UT (Rc). The
afterglow is clearly detected in combined images.

Using the USNO-B1 (1398-0233739) star at RA = 13:09:13.1, DEC =
+49:53:11, with B1_mag = 16.70, R1_mag = 14.76 as a reference, we
estimated the B and R-magnitudes of the afterglow:

Filter    T-T0, hours   Mag. +/- Mag.err

B         16.03         23.21 +/- 0.09
Rc        17.43         21.29 +/- 0.06


GRB_name: GRB140428A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16186
SUBJECT: GRB 140428A: Swift-BAT refined analysis
DATE:    14/04/29 19:57:28 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@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-240 to T+602 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140428A (trigger #597519)
(Kocevski et al., GCN Circ. 16177).  The BAT ground-calculated position is
RA, Dec = 194.365, 28.331 deg which is
  RA(J2000)  =  12h 57m 27.5s
  Dec(J2000) = +28d 19' 53.4"
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 70%.

The mask-weighted light curve shows a multi-peaked structure starts
at ~T-14 s and ends at ~T+6 s. The structure contains two main peaks
at ~T-4 s and ~T+2 s. T90 (15-350 keV) is 17.42 +- 5.90 sec (estimated
error including systematics).

The time-averaged spectrum from T-14.19 to T+5.82 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.54 +- 0.26.  The fluence in the 15-150 keV band is 3.4 +- 0.6 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+1.30 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.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/597519/BA/


GRB_name: GRB140428A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16187
SUBJECT: GRB 140428A: Swift/UVOT Upper Limits
DATE:    14/04/29 21:13:07 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) 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 140428A
104 s after the BAT trigger (Kocevski et al., GCN Circ. 16177).
No optical afterglow consistent with the optical position
(Perley, GCN_Circ. 16180) 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

white              104          254          147         >21.2
v                 5454         5653          197         >20.3
b                 4838         5039          197         >21.4
u                  264          271            7         >19.5
uw1               5864         6030          197         >20.5

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.009 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB140428B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16188
SUBJECT: Konus-Wind observation of GRB 140428B
DATE:    14/04/30 15:18:38 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, and T. Cline on behalf
of the Konus-Wind team, report:

The short-duration GRB 140428B (IPN triangulation: Golenetskii et al., 
GCN 16184) triggered Konus-Wind at T0=78275.456 s UT (21:44:35.456).

The burst light curve shows a single pulse with a total
duration of ~0.15 s.

As observed by Konus-Wind, the burst
had a fluence of 9.23(-0.95,+0.88)x10^-7 erg/cm2,
and a 16-ms peak flux, measured from T0-0.014 s,
of (1.43 +/- 0.38)x10^-5 erg/cm2/s
(both in the 20 keV - 1.2 MeV energy range).

Modeling the K-W 3-channel time-integrated spectrum
(from T0-0.064 s to T0+0.80 s)
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) yields
alpha = -0.75(-0.24, +0.26), and
Ep = 1050(-343,+1750) keV

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

The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB140428_T78275/


GRB_name: GRB140428B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16189
SUBJECT: GRB 140428B: Fermi GBM observation
DATE:    14/04/30 17:52:37 GMT
FROM:    George A. Younes at USRA/NASA/MSFC  <younes.ge@gmail.com>

George Younes (USRA/MSFC)
report on behalf of the Fermi GBM Team:

"At 21:44:38.60 UT on 28 April 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140428B (trigger 420414281 / 140428906, IPN
triangulation: Golenetskii et al., GCN 16184).

The angle from the Fermi LAT boresight is 111 degrees.

This burst also triggered Konus-Wind (Pal'shin et al. GCN #16188).

The GBM light curve consists of a single pulse
with a duration (T90) of about 0.5 s (50-300 keV).
The time-averaged spectrum from T0-0.32 s to T0+19 s is well fit by
a power law function with an exponential
high-energy cutoff.  The power law index is -0.6 +/- 0.2 and
the cutoff energy, parameterized as Epeak, is 410 (-80, +134) keV.

The event fluence (10-1000 keV) in this time interval is
(9.0 +/- 1.0)E-07 erg/cm^2. The 0.064-sec peak photon flux measured
starting from T0-0.064 s in the 10-1000 keV band
is 17 +/- 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: GRB140430A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16190
SUBJECT: GRB140430A: Swift detection of a burst with an optical counterpart
DATE:    14/04/30 20:48:23 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

M. H. Siegel (PSU), W. H. Baumgartner (GSFC/UMBC),
M. M. Chester (PSU), V. D'Elia (ASDC), S. T. Holland (STScI),
J. A. Kennea (PSU), N. P. M. Kuin (UCL-MSSL),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC) and
T. N. Ukwatta (MSU) report on behalf of the Swift Team:

At 20:33:36 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140430A (trigger=597722).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 102.929, +23.009 which is 
   RA(J2000)  =  06h 51m 43s
   Dec(J2000) = +23d 00' 34"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single peak
with a duration of about 10 sec.  The peak count rate
was ~4500 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 20:34:27.3 UT, 50.8 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 102.9359, 23.0227 which is equivalent to:
   RA(J2000)  = +06h 51m 44.62s
   Dec(J2000) = +23d 01' 21.7"
with an uncertainty of 4.9 arcseconds (radius, 90% containment). This
location is 54 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 3.99e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 183 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 06:51:44.61 = 102.93589
  DEC(J2000) = +23:01:25.2  =  23.02367
with a 90%-confidence error radius of about 0.62 arc sec. This position is 3.5
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.16 with a 1-sigma error of about  0.15. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.14. 

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: GRB140428A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16191
SUBJECT: GRB 140428A: GROND observations
DATE:    14/04/30 22:02:44 GMT
FROM:    Karla Varela at MPE  <kvarela@mpe.mpg.de>

F. Knust, K. Varela, J. Greiner (MPE Garching), and D. A. Kann
(TLS Tautenburg) report on behalf of the GROND team:

We observed the field of GRB 140428A (Swift trigger 597519; Kocevski et
al., GCN #16177) 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 La Silla
Observatory (Chile).

Observations started at 00:43 UT on 2014-04-29, 2 hours after the GRB
trigger. They were performed at an average seeing of 1.4" and at an
average airmass of 1.9.

We found a single point source within the 1.7" Swift-XRT error circle
reported by Page et al. (GCN #16178) at

RA (J2000) = 12h 57m 28.39s
DEC (J2000) = +28d 23' 06.4"

with an uncertainty of 0.5" in each coordinate.

This source is consistent with the one reported by Perley (GCN #16180).

Based on the first 1133 s of total exposures in g'r'i'z' and 1920 s in
JHK, we estimate preliminary magnitudes (all in AB system) of

g' > 24.4 mag,
r' = 23.6 +/- 0.2 mag,
i' = 21.7 +/- 0.1 mag,
z' = 21.5 +/- 0.1 mag,
J > 19.7 mag,
H > 20.6 mag, and
K > 19.1mag.

From our data, fading can not be established. We note that our r'-band 
magnitude is similar to that reported by Perley (GCN #16180) at a mid-time
of 7.5 hrs after the GRB.

The spectral energy distribution is best-fit by a straight power-law  and
a sharp cut-off below
the i'-band which cannot be modelled with extinction alone. If this is the
GRB afterglow, the cut-off corresponds to a photometric redshift of z =
4.8 +-0.3, consistent with the Keck spectroscopy
as reported by Perley (GCN #16181).

Given magnitudes are calibrated against SDSS (griz) 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) = 0.01 mag
in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB140430A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16192
SUBJECT: GRB 140430A : Liverpool Telescope optical afterglow observations
DATE:    14/04/30 22:21:29 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

A. Melandri (INAF-OAB), C. Guidorzi (U. Ferrara), A. Gomboc (U. Ljubljana), R. J. Smith and C. G. Mundell (LJMU), on behalf of a large collaboration report:

The 2-m Liverpool Telescope with the RINGO3 polarimeter robotically followed up Swift GRB 140430A (Siegel et al., GCN 16190) at 20:35:40 UT (~2 min after the burst trigger).

We detect the optical afterglow at the UVOT position. In a coadded 3x10s SDSS-r image, we estimate a preliminary magnitude R = 18.4 +/- 0.1 at t_mid = 33.1 min since the Swift/BAT trigger time. The magnitude is calibrated against nearby USNO-B1 stars.

Observations are ongoing.


GRB_name: GRB140430A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16193
SUBJECT: GRB 140430A: NOT optical observations
DATE:    14/04/30 23:43:05 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Malesani (DARK/NBI), T. Kruehler (ESO Santiago), A. de Ugarte Postigo 
(IAA/CSIC and DARK/NBI), H. Dahle (Univ. Oslo), E. Soto (CUA), report on 
behalf of a larger collaboration:

We observed the optical afterglow of GRB 140430A (Siegel et al., GCN 
16190; Melandri et al., GCN 16192) with the Nordic Optical Telescope 
equipped with ALFOSC. We took a single 100-s image in the R filter 
starting at 22:00 UT (86.5 min after the GRB). The optical afterglow is 
well detected at coordinates (J2000):

RA = 06:51:44.61
Dec = +23:01:25.1

with an uncertainty of 0.3". Assuming R = 15.13 for the USNO star at RA 
= 06:51:41.3, Dec = +23:01:44.0, we measure for the optical afterglow a 
magnitude R = 18.78 +- 0.02 (statistical error only).

A 1800-s spectrum was acquired starting at 22:11 UT, at airmass 2.2-2.8, 
covering the wavelength range 3200-9100 AA. From a preliminary analysis, 
no absorption or emission features are seen in the spectrum. From the 
lack of a DLA feature down to ~4000 AA, we can set a redshift limit z < 2.3.


GRB_name: GRB140430A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16194
SUBJECT: GRB 140430A: VLT/X-shooter redshift
DATE:    14/05/01 00:54:33 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

T. Kruehler (ESO Santiago), D. Malesani (DARK/NBI), A. de Ugarte Postigo 
(IAA/CSIC and DARK/NBI), A. Melandri (INAF/OABr), J. P. U. Fynbo 
(DARK/NBI), report on behalf of a larger collaboration:

We observed the optical afterglow of GRB 140430A (Siegel et al., GCN 
16190) with the ESO VLT equipped with X-shooter. Observations started at 
23:09 UT on 2014 April 30 (2.5 hr after the GRB), still in twilight, and 
two 10-minute spectra were secured. The covered wavelength range is 
3000-25000 AA.

We detect a clear continuum, and several absorption features, which we 
interpret as due, among others, to Si II, C IV, Al II, Fe II, and Mg II 
at a common redshift z = 1.60. In the infrared arm, we also detect the 
[O III] 5008 nebular line in emission at the same redshift.

We acknowledge excellent support from the ESO staff at Paranal, in 
particular Andrea Mehner, Rodrigo Romero, and Stephane Brillant.


GRB_name: GRB140430A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16195
SUBJECT: GRB 140430A: Enhanced Swift-XRT position
DATE:    14/05/01 04:15:54 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 1017 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 140430A, 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 = 102.93576, +23.02375 which is equivalent
to:

RA (J2000): 06h 51m 44.58s
Dec (J2000): +23d 01' 25.5"

with an uncertainty of 1.9 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB140430A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16196
SUBJECT: GRB 140430A: VATT Optical Observations
DATE:    14/05/01 06:43:27 GMT
FROM:    Peter Garnavich at U of Notre Dame  <pgarnavi@nd.edu>

M. Kennedy (University College Cork), P. Garnavich (Notre Dame)

We observed the region around GRB 140430A with the 1.8m Vatican Advanced
Technology Telescope (VATT) on 2014 May 1 (UT). With the VATT4K CCD we
obtained 5x120s exposures in the R-band centered around 03:22UT (408 mins
after the GRB). A source not seen in the Digitized Sky Survey is
well-detected at the coordinates reported by Malesani et al (GCN 16193).
Relative photometry was carried out using the same nearby star used by
Malesani et al. which has an R-band magnitude of R=15.13.

Our R-band magnitude for the GRB, 6.81 hours after the initial outburst,
is R=20.07 +- 0.03. Combining our results with the magnitude from GCN
16193 we estimate an optical power-law decay index of 0.76.


GRB_name: GRB140430A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16197
SUBJECT: GRB 140430A: Swift-XRT refined Analysis
DATE:    14/05/01 09:48:09 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

M.C. Stroh (PSU), D.N. Burrows (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), J.A.
Kennea (PSU) and M.H. Siegel report on behalf of the Swift-XRT team:

We have analysed 7.0 ks of XRT data for GRB 140430A (Siegel  et al. GCN
Circ. 16190),  from 132 s to 23.5 ks after the BAT trigger. The data
comprise 382 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Evans et al. (GCN Circ. 16195).

The late-time light curve (from T0+3.8 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.68 (+0.12, -0.13).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.05 (+/-0.04). The
best-fitting absorption column is  3.7 (+1.4, -1.3) x 10^21 cm^-2, at a
redshift of 1.6, in addition to the Galactic value of 2.1 x 10^21 cm^-2
(Willingale et al. 2013). The PC mode spectrum has a photon index of
2.21 (+0.20, -0.19) and a best-fitting absorption column of 5.3 (+6.5,
-5.3) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV
flux conversion factor deduced from this spectrum  is 3.3 x 10^-11 (5.2
x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 2.1 x 10^21 cm^-2
Intrinsic column:    5.3 (+6.5, -5.3) x 10^21 cm^-2 at z=1.6
Photon index:      2.21 (+0.20, -0.19)

If the light curve continues to decay with a power-law decay index of
0.68, the count rate at T+24 hours will be 0.018 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.0 x
10^-13 (9.6 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00597722.

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


GRB_name: GRB140430A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16198
SUBJECT: GRB 140430A: Swift/UVOT Observations
DATE:    14/05/01 11:42:29 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (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 140430A 
183 s after the BAT trigger (Siegel et al., GCN Circ. 16190). A fading 
source consistent with the refined XRT position (Evans et al. GCN Circ. 
16195) is confirmed in the initial UVOT exposures. The detection in the 
uvw1 filter, but not in uvm2 and uvw2 is consistent with the redshift of 
1.6 given by Kruehler et al., (GCN Circ. 16194).

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           183          333          147         18.17  0.09
white             4020         4220          197         19.61  0.17
v                  417         4630          216        >18.6
b                 3815         4015          197         19.77  0.34
u                10431        10933          490         19.46  0.19
uvw1              6178        10424          966         20.40  0.31
uvm2               442         4835          216        >19.9
uvw2               393         4425          216        >19.4

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: GRB140501A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16199
SUBJECT: GRB 140501A: Fermi GBM detection
DATE:    14/05/01 15:32:13 GMT
FROM:    Hoi-Fung Yu at MPE  <sptfung@mpe.mpg.de>

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

"At 03:19:41.41 UT on 01 May 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140501A (trigger 420607184 / 140501139).
This burst, tentatively classified as Unreliable Location by the FSW,
is in fact due to a gamma-ray burst.

The on-ground calculated location, using the GBM trigger data, is
RA = 171.9, DEC = 24.6 (J2000 degrees, equivalent to 11h 27m, 24d 36'),
with an uncertainty of 10.7 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 90 degrees.

The GBM light curve consists of a single pulse with a duration (T90)
of about 0.256 s (50-300 keV). The time-averaged spectrum from
T0-0.128 s to T0+0.064 s is well fit by a power law function with an
exponential high-energy cutoff. The power law index is -0.57 +/- 0.35
and the cutoff energy, parameterized as Epeak, is 502 +/- 222 keV.

The event fluence (10-1000 keV) in this time interval is
(2.4 +/- 0.4)E-07 erg/cm^2. The 64-ms peak photon flux measured
starting from T0 in the 10-1000 keV band is 5.6 +/- 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: GRB140430A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16200
SUBJECT: GRB 140430A: Swift-BAT refined analysis
DATE:    14/05/01 21:30:21 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), A. Y. Lien (NASA/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU),
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-152 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140430A (trigger #597722)
(Siegel, et al., GCN Circ. 16190).  The BAT ground-calculated position is
RA, Dec = 102.942, 23.033 deg, which is 
   RA(J2000)  =  06h 51m 46.0s 
   Dec(J2000) = +23d 01' 58.2" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows several well separated peaks.
The first (and brightest) starts at ~T-1 sec, peaks at ~T+4 sec,
and ends at ~T+9 sec.  The 2nd and 3rd peaks peak at ~T+30 and ~T+180,
respectively.  T90 (15-350 keV) is 173.6 +- 3.7 sec (estimated error
including systematics).
 
The time-averaged spectrum from T-0.30 to T+177.58 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.00 +- 0.22.  The fluence in the 15-150 keV band is 1.1 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+2.44 sec in the 15-150 keV band
is 2.5 +- 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/597722/BA/


GRB_name: GRB140430A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16201
SUBJECT: GRB 140430A: Further VATT Optical Observations
DATE:    14/05/02 07:41:32 GMT
FROM:    Peter Garnavich at U of Notre Dame  <pgarnavi@nd.edu>

M. Kennedy (University College Cork), P. Garnavich (Notre Dame)

We again observed the field around GRB 140430A with the 1.8m Vatican
Advanced Technology Telescope (VATT; GCN 16196). Observations with the
VATT4K CCD were centered around 3:22 UT on 2014 May 2 (1848 minutes after
the burst). We obtained 5x300s exposures with the R-band filter in good
seeing. We detect the previously reported afterglow in the combined images.

With the same USNO comparison star used by Malesani et al (GCN 16193)
and Kennedy et al. (GCN 16196) we estimate the afterglow brightness
as R=21.7 +/- 0.1 at 30.81 hours after the burst. This is fainter
than the extrapolation of the power-law decay rate estimated for the
first seven hours and we conclude that optical power-law decay index has
steepened to 1.0 over the past day.


GRB_name: GRB140502A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16202
SUBJECT: GRB 140502A: Swift detection of a burst
DATE:    14/05/02 08:44:00 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

C. A. Swenson (PSU), S. D. Barthelmy (GSFC), M. M. Chester (PSU) and
P. A. Evans (U Leicester) report on behalf of the Swift Team:

At 08:30:20 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140502A (trigger=597841).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 319.155, +49.018 which is 
   RA(J2000)  =  21h 16m 37s
   Dec(J2000) = +49d 01' 04"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single peak
with a duration of about 25 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 08:31:31.3 UT, 70.8 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 319.18744, 48.97012 which is equivalent
to:
   RA(J2000)  = 21h 16m 44.99s
   Dec(J2000) = +48d 58' 12.4"
with an uncertainty of 4.0 arcseconds (radius, 90% containment). This
location is 188 arcseconds from the BAT onboard position, outside the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 9.47
x 10^21 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 74 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 large, but
uncertain extinction expected. 

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: GRB140502A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16203
SUBJECT: GRB 140502A: Fermi GBM observation
DATE:    14/05/02 13:30:31 GMT
FROM:    Hoi-Fung Yu at MPE  <sptfung@mpe.mpg.de>

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

"At 08:30:20.11 UT on 02 May 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140502A (trigger 420712223 / 140502354),
which was also detected by Swift/BAT and XRT (Swenson et al. 2014, GCN 16202).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 64 degrees.

The GBM light curve consists of a single pulse with a duration (T90) 
of about 20 s (50-300 keV). The time-averaged spectrum from T0-2.048 s 
to T0+6.144 s is well fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.7 +/- 0.2 and
the cutoff energy, parameterized as Epeak, is 298 +/- 71 keV.

The event fluence (10-1000 keV) in this time interval is
(1.6 +/- 0.2)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+0.448 s in the 10-1000 keV band is 1.6 +/- 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: GRB140430A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16205
SUBJECT: GRB 140430A: BVR-band IAC80 observations
DATE:    14/05/02 17:44:33 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC/UPV-EHU), E. Gomez (IAC), P.A. Gonzalez-Morales (IAC), J. Cepa (IAC), report on behalf of a larger collaboration:

"We observed the field of GRB 140430A (Siegel et  al. GCN 16190) with the 0.82m IAC80 telescope located at Observatorio del Teide, Tenerife, Spain. The observations were carried on April 30.87401-30.88509 UT (25.0-40.9 min post burst) using the BVR-band filters. The optical afterglow is clearly detected in the three bands with a preliminary Vega magnitude of B=19.3 against the USNO B1.0 catalogue."


GRB_name: GRB140502A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16206
SUBJECT: GRB 140502A: Enhanced Swift-XRT position
DATE:    14/05/02 19:51:41 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 1615 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 140502A, 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 = 319.18818, +48.97021 which is equivalent
to:

RA (J2000): 21h 16m 45.16s
Dec (J2000): +48d 58' 12.7"

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: GRB140502A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16207
SUBJECT: GRB 140502A: Swift-XRT refined Analysis
DATE:    14/05/02 20:44:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

D.N. Burrows (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), J.A. Kennea (PSU), V. Mangano
(PSU) and C.A. Swenson report on behalf of the Swift-XRT team:

We have analysed 6.3 ks of XRT data for GRB 140502A (Swenson  et al.
GCN Circ. 16202),  from 84 s to 17.3 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Goad et al. (GCN Circ. 16206).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.85 (+0.23, -0.17).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.7 (+0.8, -0.6). The
best-fitting absorption column is  2.2 (+1.4, -1.1) x 10^22 cm^-2, in
excess of the Galactic value of 9.5 x 10^21 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 7.0 x 10^-11 (1.3 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.2 (+1.4, -1.1) x 10^22 cm^-2
Galactic foreground: 9.5 x 10^21 cm^-2
Excess significance: 1.8 sigma
Photon index:      1.7 (+0.8, -0.6)

If the light curve continues to decay with a power-law decay index of
0.85, the count rate at T+24 hours will be 7.5 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.3 x
10^-14 (9.5 x 10^-14) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00597841.

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


GRB_name: GRB140502A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16208
SUBJECT: GRB 140502A: Swift-BAT refined analysis
DATE:    14/05/02 22:17:48 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), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), C. A. Swenson (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 recent telemetry downlinks,
we report further analysis of BAT GRB 140502A (trigger #597841)
(Swenson, et al., GCN Circ. 16202).  The BAT ground-calculated position is
RA, Dec = 319.172, 48.975 deg, which is 
   RA(J2000)  =  21h 16m 41.3s 
   Dec(J2000) = +48d 58' 28.2" 
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 99%.
 
The mask-weighted light curve shows a FRED-shaped peak starting at ~T-3 sec,
peaking at ~T+2 sec, and ending at ~T+20 sec.  T90 (15-350 keV) is
16.9 +- 1.9 sec (estimated error including systematics).
 
The time-averaged spectrum from T-1.66 to T+17.39 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.22 +- 0.13.  The fluence in the 15-150 keV band is 6.7 +- 0.5 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+1.44 sec in the 15-150 keV band
is 0.9 +- 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/597841/BA/


GRB_name: GRB140502A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16209
SUBJECT: GRB 140502A: MITSuME Okayama upper limits
DATE:    14/05/03 04:19:32 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 140502A (Swenson et al., GCNC 16202)
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 2014-05-02 16:48:47 UT (~8.3 h after the burst).
We did not find any new point source within the enhanced XRT circle
(Goad et al., GCNC 16206) 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
-----------------------------------------------------
0.38783    17:48:49    6180.0   >19.5  >19.2  >18.5
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB140502A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16210
SUBJECT: GRB 140502A: Swift/UVOT Upper Limits
DATE:    14/05/03 11:43:15 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (IAA-CSIC,UCL-MSSL) and C. A. Swenson (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140502A
75 s after the BAT trigger (Swenson et al., GCN Circ. 16202). Two bright 
USNO-B1 sources lie close to the XRT location, with R magnitudes of 13.48 
and 13.61, lie within 3 and 9 arcseconds, respectively of the XRT position 
(Goad et al., GCN Circ. 16206). Neither of these sources are observed to 
vary significantly over the duration of the initial UVOT observations.

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

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

white_FC            75          225          147         >16.0
u_FC               287          537          246         >16.3
white               75         5702          525         >16.0
v                  616         6113          432         >15.0
b                  543        11919          337         >16.0
u                  287        11811         1347         >16.3
w1                 666        17270         1642         >17.9
m2                4681        16734         1262         >20.0
w2                 593         5908          432         >18.9

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 2.97 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB140430A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16211
SUBJECT: GRB 140430A: r'-band STELLA-I observations
DATE:    14/05/03 12:29:59 GMT
FROM:    Arto Jarvinen at AIP  <ajarvinen@aip.de>

A. Jrvinen (AIP) and J. Gorosabel (IAA-CSIC/UPV-EHU), report on behalf 
of larger collaborations:

"The field of GRB 140430A (Siegel et al. GCN 16190) was observed with 
WiFSIP on STELLA-I telescope located at Observatorio del Teide,
Tenerife, Spain.  The automatic observations were carried out on April
30., 2.9-32.5 min post trigger using the r'-band filter. The object is 
clearly detected in all 52 images with preliminary r'(AB) magnitudes
ranging from ~17.0 to ~18.6 calibrated against the USNO B1.0 catalogue."

[GCN OPS NOTE(03may14):  The distribution was delayed by 3 hours
due to a stale address in the vetting list.]


GRB_name: GRB140430A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16212
SUBJECT: GRB 140430A: iTelescope.Net T16 Optical Observation
DATE:    14/05/04 12:18:49 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

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

We observed the field of GRB 140430A detected by Swift (trigger #597722; 
Siegel et al., GCN Circ. 16190) with the iTelescope.Net (http://www.itelescope.net) 
T16 (15 cm Takahashi TOA-150) telescope located at the AstroCamp Observatory 
(Nerpio, Spain).  

Due to the elevation constraint, we were able to collect only 4 images of 60 sec 
exposures in the R filter starting from April 30 20:46:42 (UT) about 13 minutes 
after the trigger and stopped on April 30 20:52:42 (UT).  We do not detect the optical afterglow 
both in the individual images and the stacked image at the reported optical 
afterglow position (Siegel et al., GCN Circ. 16190; Malesani et al., GCN Circ. 16193).  
The estimated five sigma upper limit of the combined image (total exposure of 240 sec) 
is ~18.6 using the USNO-B1 catalog.  


GRB_name: GRB140423A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16213
SUBJECT: Konus-Wind observation of GRB 140423A
DATE:    14/05/05 07:43:26 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

The long GRB 140423A (Swift-BAT trigger #596901: Sonbas, et al., GCN 
Circ. 16142, Cummings, et al., GCN Circ. 16161) was detected by 
Konus-Wind in the waiting mode.

The burst light curve shows a single episode started at ~T0(BAT)-46 s 
with a duration of ~130 s.

As observed by Konus-Wind, the burst had a fluence of 
1.87(-0.17,+0.13)x10^-5 erg/cm2 (in the 20 - 1200 keV energy range).

Modeling the K-W 3-channel time-integrated spectrum (from T0(BAT)-46 s
to T0(BAT)+84 s) by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -1.1 +/- 0.1, and Ep = 196(-20,+30) keV.

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

The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB140423A/


GRB_name: GRB140506A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16214
SUBJECT: GRB 140506A: Swift detection of a burst with an optical counterpart
DATE:    14/05/06 21:28:16 GMT
FROM:    David Burrows at PSU/Swift  <burrows@astro.psu.edu>

B.P. Gompertz (U Leicester), D. N. Burrows (PSU), S. B. Cenko (GSFC),
S. T. Holland (Eureka), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), N. P. M. Kuin (UCL-MSSL),
A. Y. Lien (NASA/GSFC/ORAU), V. Mangano (PSU),
K. L. Page (U Leicester) and M. H. Siegel (PSU) report on behalf of
the Swift Team:

At 21:07:36 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140506A (trigger=598284).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 276.790, -55.562 which is 
   RA(J2000) = 18h 27m 10s
   Dec(J2000) = -55d 33' 43"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked
structure with a duration of about 10 sec.  The peak count rate
was ~6500 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 21:09:14.7 UT, 97.9 seconds after
the BAT trigger. XRT found a bright, fading, uncatalogued X-ray source located
at RA, Dec 276.7752, -55.6353 which is equivalent to:
   RA(J2000)  = +18h 27m 6.05s
   Dec(J2000) = -55d 38' 07.1"
with an uncertainty of 4.7 arcseconds (radius, 90% containment). This
location is 265 arcseconds from the BAT onboard position. 
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 1.01e-08 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
320 seconds after the BAT trigger. There is a candidate afterglow in the
rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 18:27:06.03 = 276.77513
  DEC(J2000) = -55:38:08.8  = -55.63577
with a 90%-confidence error radius of about 0.63 arc sec. This position is 1.7
arc sec. from the center of the XRT error circle. The estimated magnitude is
17.46 with a 1-sigma error of about  0.15. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.09. 

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


GRB_name: GRB140506A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16215
SUBJECT: GRB 140506A: Enhanced Swift-XRT position
DATE:    14/05/07 04:18:24 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 930 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 140506A, 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 = 276.77549, -55.63648 which is equivalent
to:

RA (J2000): 18h 27m 6.12s
Dec (J2000): -55d 38' 11.3"

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

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

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


GRB_name: GRB140506A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16216
SUBJECT: GRB 140506A: Swift-XRT refined Analysis
DATE:    14/05/07 09:34:53 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

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

We have analysed 7.7 ks of XRT data for GRB 140506A (Gompertz  et al.
GCN Circ. 16214),  from 87 s to 30.4 ks after the  BAT trigger. The
data comprise 531 s in Windowed Timing (WT) mode (the first 9 s were
taken while Swift was slewing) with the remainder in Photon Counting
(PC) mode. The enhanced XRT position for this burst was given by
Osborne et al. (GCN Circ. 16215).

The late-time light curve (from T0+5.1 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.91 (+/-0.08).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.65 (+/-0.03). The
best-fitting absorption column is  3.14 (+/-0.10) x 10^21 cm^-2, in
excess of the Galactic value of 1.1 x 10^21 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.79 (+/-0.09) and a
best-fitting absorption column of 2.9 (+/-0.4) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 4.2 x 10^-11 (5.6 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.9 (+/-0.4) x 10^21 cm^-2
Galactic foreground: 1.1 x 10^21 cm^-2
Excess significance: 7.6 sigma
Photon index:      1.79 (+/-0.09)

If the light curve continues to decay with a power-law decay index of
0.91, the count rate at T+24 hours will be 0.058 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.4 x
10^-12 (3.2 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/00598284.

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


GRB_name: GRB140506A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16217
SUBJECT: GRB 140506A: VLT/X-shooter spectroscopy
DATE:    14/05/07 10:06:33 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

J. P. U. Fynbo (DARK/NBI), N. R. Tanvir (U. Leicester), P. Jakobsson
(U. Iceland), D. Xu, D. Malesani, B. Milvang-Jensen  (DARK/NBI) report
on behalf of the X-shooter GRB collaboration:

We observed the optical afterglow of GRB 140506A (Gompertz et al., GCN
16214) with the VLT/X-shooter spectrograph, equipped with the
UVB/VIS/NIR arms and covering the wavelength range 3000-25000 AA.

From the first acquisition image at May 7.21 UT, the afterglow has
m(R)=20.9 +/- 0.2 mag against the USNO-B1 (R2) catalog.

The spectra (8 x 600 s) started at May 7.21 UT and ended May 7.28 UT,
and the mean time is May 7.24 UT (8.77 hr after the GRB). We detect
absorption features in the UVB/VIS arms, interpreted as due to Mg II
2796, 2803, He I 3889, and Ca II H+K, at a common redshift of z =
0.889, which is treated as the tentative redshift of the GRB's host
galaxy. The combined spectrum is very red with very weak signal in the
UVB arm, possibly due to the large host extinction.

We acknowledge excellent support from the observing staff at Paranal,
in particular Valentin D. Ivanov and Yazan Momany.


GRB_name: GRB140506A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16218
SUBJECT: GRB 140506A: Swift-BAT refined analysis
DATE:    14/05/07 11:50:34 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), B.P. Gompertz (U Leicester),
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-240 to T+962 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 140506A (trigger #598284)
(Gompertz, et al., GCN Circ. 16214).  The BAT ground-calculated position is
RA, Dec = 276.806, -55.556 deg, which is 
   RA(J2000)  =  18h 27m 13.5s 
   Dec(J2000) = -55d 33' 20.2" 
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 11%.
 
The mask-weighted light curve a bright initial pulse strting at ~T-5 sec,
peaking at ~T+0.2 sec, and returning to baseline at ~T+5 sec. Then there were
two weaker peaks at ~T+60 sec and at ~T+110 sec.  T90 (15-350 keV) is
111.1 +- 9.6 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.20 to T+120.18 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.68 +- 0.16.  The fluence in the 15-150 keV band is 2.8 +- 0.3 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+0.00 sec in the 15-150 keV band
is 10.9 +- 0.9 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/598284/BA/


GRB_name: GRB140506A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16219
SUBJECT: GRB 140506A: Swift/UVOT Detection
DATE:    14/05/07 17:00:49 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

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

The Swift/UVOT began settled observations of the field of GRB 140506A
108 s after the BAT trigger (Gompertz et al., GCN Circ. 16214).
A source consistent with the XRT position
(Osborne et al. GCN Circ. 16215)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
  RA  (J2000) =  18:27:06.04 = 276.77516 (deg.)
  Dec (J2000) = -55:38:08.7  = -55.63575 (deg.)
with an estimated uncertainty of 0.43 arc sec. (radius, 90% confidence).

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

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

white (fc)         108          257          147     17.19+-0.03
white              108         1545          390     17.82+-0.05
white             6078         6278          196     20.07+-0.14
white            11748        12655          885     21.52+-0.26
v                  650         1576           98    >18.87
v                 5053         6688          393     19.82+-0.32
b                  576         1520           97     19.40+-0.30
b                 5873         7334          221    >20.57
u (fc)             320          570          245     17.34+-0.07
u                  320         1496          323     17.50+-0.07
u                 5668         7303          393     20.04+-0.34
uvw1               700         1471           77     18.60+-0.29
uvw1              5463         7098          393    >20.29
uvm2               675         1446           97    >18.96
uvm2              5257         6893          393    >20.17
uvw2               626         1570          116    >19.41
uvw2              6284         6484          196    >19.97

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.09 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB140506A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16220
SUBJECT: GRB 140506A: Fermi GBM Detection
DATE:    14/05/07 17:22:01 GMT
FROM:    Peter Jenke at MSFC  <peter.a.jenke@nasa.gov>

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

"At 21:07:36.88 UT on May 6 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140506A (trigger 421103259/140506880),
which was also detected by 
Swift (B.P. Gompertz et al. 2014, GCN 16214).  
The GBM on-ground location, using the Fermi GBM trigger
data, is consistent with the Swift/XRT location.

The angle of the burst direction to the Fermi LAT boresight
 is 135 degrees.

The GBM light curve consists of one main peak near T0 and a
late, smaller peak at ~T0+60 s with a duration (T90) of about
64 s (50-300 keV).  The time-averaged spectrum from
T0-1.9 s to T0+2.2s is well fit by a Band function with an
Epeak of 141 +/- 36 keV, alpha = -0.9 +/- 0.2 
and beta = -2.0 +/- 0.1.

The event fluence (10-1000 keV) in this time interval is
(3.5 +/- 0.2)E-06 erg/cm^2. The 1.0-sec peak photon flux measured
starting from T0 in the 10-1000 keV band
is 14.2 +/- 0.7 ph/s/cm^2.

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


GRB_name: GRB140502A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16221
SUBJECT: GRB 140502A: ISON-NM early optical limit
DATE:    14/05/07 20:16:19 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed of  the field of  Swift GRB GRB 140502A  with 0.4-m 
telescope of ISON-NM observatory starting on May, 02 (UT)  08:31:32, 
i.e. 72 s after BAT trigger (Swenson et al.,  GCN 16202). We took series 
of unfiltered images of 30 s - 60 s exposures.  A bright star (USNO-B1.0 
1389-0392112) already mentioned (Oates et al.,  GCN 16210) lies within 
enhanced XRT error circle (Goad et al.,  GCN 16206). We investigate 
variability of  a possible OT  in presence in near vicinity of the 
bright star. The upper limit of possible variation of the OT is 16.6m 
within any of 60 s interval of our observations between (UT)  08:31:32 
and 09:24:25 which can be considered as an upper limit on the OT 
associated with GRB 140502A.

Formal photometry and limiting magnitude of point-like source in the 
observed field is following

UT start   t-T0        Exp.    Filter   OT   UL(3 sigma)
           (mid.,days)  (s)
08:31:32  0.00383      10*30   None     n/d  18.8

and based on nearby USNO-B1.0 stars, R2 magnitudes.


GRB_name: GRB140430A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16222
SUBJECT: GRB 140430A: MITSuME Akeno upper limits
DATE:    14/05/08 03:53:34 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

T. Fujiwara, T. Yoshii, Y. Saito, Y. Tachibana, H. Ohuchi,
S. Kurita, Y.Ono , Y. Yatsu, and N. Kawai (Tokyo Tech)

report on behalf of the MITSuME collaboration:
We observed the field of GRB 140430A (Siegel et al. , GCN Circular #16190) 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 2014-05-01 10:57:06 UT ( 14.4 h after the burst).
We did not find any new point source within the enhanced XRT circle (Evans et al., GCNC 16195) in all the three bands.
The measured magnitudes were listed below.

T0+[sec]    MID-UT    T-EXP[sec]    g'         Rc         Ic
---------------------------------------------------------------------------------------
   54229  11:37:25     3540        >19.2    >19.5     >19.2
---------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used GSC2.3 catalog for flux calibration.


GRB_name: GRB140506A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16223
SUBJECT: Konus-Wind observation of GRB 140506A
DATE:    14/05/08 13:33:01 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:

A long-duration GRB 140506A (Swift-BAT trigger 598284:
Gompertz et al., GCN 16214; Markwardt et al., GCN 16218;
Fermi-GBM detection: Jenke, GCN 16220)
triggered Konus-Wind at T0=76059.098 s UT (21:07:39.098).

The light curve shows two bursting episodes: a narrow,
double-peaked pulse from ~T0-1.1 s to ~T0+1.6 s,
followed by a broad, weak, soft pulse from ~T0+49 s to ~T0+63 s
A total duration of the burst is ~64 s.
The emission is seen up to ~7 MeV.

As observed by Konus-Wind, the burst had a fluence
of 6.6(-1.6,+1.8)x10^-6 erg/cm2, and a 64-ms peak flux,
measured from T0+0.640 s, of 6.2(-1.9,+2.5)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the first bursting episode
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 18 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.3 (-0.2,+0.3),
the high energy photon index beta = -2.3 (-7.7,+0.4),
the peak energy Ep = 187 (-59,+90) keV,
chi2 = 94/97 dof.

The time-averaged spectrum of the second bursting episode
(measured from T0+49.408 to T0+65.792 s)
is best fit in the 20 keV - 18 MeV range
by a simple power-law function with
the photon index 2.06(-0.13,+0.14),
chi2 = 98/98 dof.

Assuming the redshift z=0.889 (Fynbo et al., GCN 16217)
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 ~1.4x10^52 erg,
the peak luminosity L_iso is ~2.5x10^52 erg/s,
and the rest-frame peak energy, Ep,i, is ~350 keV
(as derived from the spectrum of the first episode).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140506_T76059/

All the quoted errors are at the 1 sigma confidence level.
All the quoted values are preliminary.


GRB_name: GRB140508A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16224
SUBJECT: GRB 140508A: Fermi GBM detection
DATE:    14/05/08 14:51:43 GMT
FROM:    Hoi-Fung Yu at MPE  <sptfung@mpe.mpg.de>

Hoi-Fung Yu (MPE) and Adam Goldstein (ORAU/NASA MSFC)
report on behalf of the Fermi GBM Team:

"At 03:03:54.60 UT on 08 May 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140508A (trigger 421211037 / 140508128).
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 = 250.1, Dec = 44.4 (J2000 degrees, equivalent to 16h 40m, 44d 24'),
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 initial angle from the Fermi LAT boresight is 112 degrees.

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

The GBM light curve consists of several pulses with decaying peak flux
with a duration (T90) of about 44.3 s (50-300 keV). The time-averaged
spectrum from T0-0.512 s to T0+51.712 s is well fit by a Band function
with Epeak = 256.2 +/- 11.8 keV, alpha = -1.07 +/- 0.02, and
beta = -2.38 +/- 0.09.

The event fluence (10-1000 keV) in this time interval is
(6.24 +/- 0.07)E-05 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+4.480 s in the 10-1000 keV band is 66.8 +/- 1.0 ph/s/cm^2.

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


GRB_name: GRB140508A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16225
SUBJECT: IPN triangulation of GRB 140508A
DATE:    14/05/08 19:05:02 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@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,

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

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

The long-duration, very intense GRB 140508A (Yu and Goldstein, GCN Circ.
16224) has been observed by Fermi (GBM), Konus-Wind, INTEGRAL (SPI-ACS), 
Swift (BAT), and MESSENGER (GRNS) so far, at about 11035 s UT 
(03:03:55). 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:
   255.631 (17h 02m 31s) +46.747 (+46d 44' 51")
  Corners:
   254.602 (16h 58m 24s) +47.063 (+47d 03' 48")
   256.275 (17h 05m 06s) +46.717 (+46d 43' 00")
   256.649 (17h 06m 36s) +46.418 (+46d 25' 06")
   254.988 (16h 59m 57s) +46.773 (+46d 46' 23")
  ---------------------------------------------
The error box area is 882 sq. arcmin, and its maximum dimension is 1.5
deg (the minimum one is 12 arcmin). The Sun distance was about 110 deg.

This box can be improved.

A triangulation map will be posted at 
ssl.berkeley.edu/ipn3/140508/140508.png

Details of the K-W observation will be given in a forthcoming GCN Circular


GRB_name: GRB140508A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16226
SUBJECT: GRB 140508A: iPTF optical transient candidate
DATE:    14/05/08 19:30:09 GMT
FROM:    Leo Singer at CIT/PTF  <lsinger@caltech.edu>

L. P. Singer (Caltech), S. B. Cenko (NASA/GSFC), M. M. Kasliwal
(Carnegie Observatories/Princeton), Christoffer Fremling (Stockholm
University), and Yifat Dzigan (Weizmann) report on behalf of the
intermediate Palomar Transient Factory (iPTF) collaboration:

We have searched for an optical counterpart of GRB 140508A (Yu and
Goldstein, GCN 16224), Fermi/GBM trigger 421211037 (2014-05-08
03:03:54.60), using the Palomar 48-inch Oschin telescope (P48). Based
on the final Fermi GBM localization, we observed 10 fields covering
73 deg2, with an estimated 67% chance of containing the true location
of the event. Due to weather at Palomar early in the night,
observations started at 09:48 UTC, 6.7 hours after the trigger.

Also detected by Konus-Wind, INTEGRAL, Swift BAT (outside FoV), and
MESSENGER, the IPN error box (Hurley et al., GCN 16225) was mostly
contained within two CCDs in one of our fields.

Sifting through candidate variable sources using image subtraction
and standard iPTF vetting procedures, we detected several optical
transients. Only is located within the IPN error box:

iPTF14aue, at the coordinates:
  RA(J2000)  =  17h 01m 51.95s (255.466450 deg)
  Dec(J2000) = +46d 46' 49.5"  (+46.780417 deg)

The source was detected at r = 17.89 +/- 0.01 mag and appeared to
fade. A power-law fit to the first two observations, relative to the
time of the GBM trigger, gives a decay index of alpha = 1.12 +/- 0.1.
There is no source coincident with this location in our reference
images or in SDSS DR10.

This position is also consistent with the IPN triangulation
(Hurley et al., GCN 16225), and is 7' from the center of the error
box.

Given the spatial coincidence with the IPN localization, the lack of
archival detections, and the source fading, iPTF14aue is likely
associated with the GRB. We are submitting a Swift XRT target of
opportunity. Further observations are encouraged to confirm the
association and the nature of the candidate.

The diagram
http://www.its.caltech.edu/~lsinger/iptf/Fermi421211037.pdf shows the
ten P48 fields in relation to the Fermi GBM 1- and 2-sigma
statistical+systematic contours, and the IPN error box.

We thank the Fermi-GBM and IPN teams for sharing their localizations
with us.


GRB_name: GRB140508A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16227
SUBJECT: GRB 140508A: 1.23m CAHA BVRI-band observations
DATE:    14/05/08 23:02:30 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J.  Gorosabel  (UPV-EHU/IAA-CSIC),  A. Sanchez-Lavega  (UPV/EHU), S.  Perez-Hoyos   (UPV/EHU), R. Hueso (UPV/EHU), J. Ugarte  (UPV/EHU), I. Ordonez (UPV/EHU),  E. Arandia (UPV/EHU), I. Perez de Nanclares (UPV/EHU), on behalf of the BEGIRA project:

"We observed  the  field  of GRB140508A (GCN Cir. 16224,16225) starting on May 8.93559  UT. The optical transient detected by Singer et al. (GCN Cir. 16226) is clearly detected in our images with an approximate Vega magnitude  of R=18.8 with respect to the USNO B1.0."


GRB_name: GRB140508A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16228
SUBJECT: GRB 140508A: SAO RAS and MASTER photometric and spectroscopic observations
DATE:    14/05/09 01:15:15 GMT
FROM:    Vladimir Sokolov at SAO RAS  <sokolov@sao.ru>

A. S. Moskvitin, D. I. Makarov, A. F. Valeev, V. V. Sokolov (SAO-RAS,
Russia), A. J. Castro-Tirado, J. Gorosabel (IAA-CSIC, Spain),
E. S. Gorbovskoy, D. V. Denisenko, V. M.Lipunov (MASTER-team, Russia),
on behalf of a larger collaboration, report:

"Following the detection of GRB 140508A by Fermi (Yu et al. GCNC 16224) and
the IPN (Hurley et al. GCNC 16225), we have conducted BVRc imaging and
spectroscopy of the iPTF optical candidate (Singer et al. GCNC 16226) with
the 6m BTA telescope in Zelenchukskaia, starting at 19:47:56 UT (i.e. 16.7
hr after the trigger). The 20 minutes (noisy) spectrum, covering the range
3800-7200 A, displays no clear absorption features, i.e. a conservative
upper limit of z < 2.1 is derived.

The GRB OT magnitude was measured to have R = 18.7 +/- 0.05 during the BTA
observations spanning more than 1 hr. OT magnitudes calibrated against the
USNO-B1 star 1367-0290781 with R2 = 16.48.

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Kislovodsk also pointed to the  GRB140508A  (Yu et. al GCNC
16224, Hurley et. al. GCN 16224) ~17.5 h  after trigger time at 2014-05-08
20:31:01.484 UT directly after sunset and weather conditions became
satisfactory. On the first (180s exposure) unfiltred image the iPTF
optical transient preliminary photometry is given below:

      T_start            T-T_trig  FILTER  Mag   Err.Mag Exptime
 2014-05-08 20:31:01    17h 28m     C     18.7   0.3     180 s
 2014-05-08 20:48:33    17h 45m     R     18.7   0.3     180 s
 2014-05-08 20:48:33    17h 45m     V    <19.0   0.3     180 s upper limit
 2014-05-08 21:20:36    18h 17m     R     18.9   0.3     540 s
 2014-05-08 21:20:36    18h 17m     V     19.9   0.4     540 s

 "C" is unfiltred 0.8R+0.2B magnitude.

This message can be quoted."


GRB_name: GRB140508A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16229
SUBJECT: GRB 140508A: NOT photometry and spectroscopy
DATE:    14/05/09 02:30:41 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Malesani, D. Xu (DARK/NBI), P. D'Avanzo (INAF/OAB), E. Palazzi 
(INAF/IASF Bologna), D. Perna (Obs. Paris) report on behalf of a larger 
collaboration:

We observed the optical afterglow candidate of GRB 140508A (Yu & 
Goldstein GCN 16224; Hurley et al., GCN 16225; Singer et al., GCN 16226) 
with the Nordic Optical Telescope (NOT) equipped with ALFOSC. The 
observation consisted of a 1800 s spectrum covering the wavelength range 
between 3200 and 9100 AA, carried out at a mean time of 20.63 hr after 
the GRB.

The afterglow is detected in the acquisition image (20.13 hr after the 
GRB) with r = 19.07+-0.03 (AB) calibrated against SDSS stars. Compared 
with the measurement by Singer et al. (GCN 16226), our measurement 
yields a power-law decay slope alpha ~ 1, consistent with the value 
reported by these authors.

We detect several absorption features which we intepret as due to Fe II 
2600 and Mg II 2796, 2803 at a common redshift of z = 1.03. This can be 
considered as a firm lower limit to the GRB redshift, and is consistent 
with the constraint by Moskvitin et al. (GCN 16228).


GRB_name: GRB140509A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16230
SUBJECT: GRB 140509A: Swift detection of a burst with an optical counterpart
DATE:    14/05/09 02:38:29 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

K. L. Page (U Leicester), S. D. Barthelmy (GSFC), D. N. Burrows (PSU),
J. R. Cummings (NASA/UMBC), N. Gehrels (NASA/GSFC),
J. A. Kennea (PSU), V. Mangano (PSU), C. B. Markwardt (NASA/GSFC),
F. E. Marshall (NASA/GSFC), C. J. Mountford (U Leicester),
D. M. Palmer (LANL) and M. H. Siegel (PSU) report on behalf of the
Swift Team:

At 02:22:13 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140509A (trigger=598497).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 46.608, -62.654 which is 
   RA(J2000)  =  03h 06m 26s
   Dec(J2000) = -62d 39' 12"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single peak
with a duration of about 30 sec.  The peak count rate
was ~1200 counts/sec (15-350 keV), at ~4 sec after the trigger. 

The XRT began observing the field at 02:24:06.1 UT, 112.5 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source with an enhanced position: RA, Dec 46.5952,
-62.6396 which is equivalent to:
   RA(J2000)  = 03h 06m 22.84s
   Dec(J2000) = -62d 38' 22.6"
with an uncertainty of 2.1 arcseconds (radius, 90% containment). This
location is 55 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (2.23 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 3.6
(+2.56/-2.25) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 5.99e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
279 seconds after the BAT trigger. There is a candidate afterglow in the list
of sources generated on-board at
 RA(J2000)  = 03:06:22.67 =  46.59444
 DEC(J2000) = -62:38:21.7  = -62.63937
with a 90%-confidence error radius of about 1.10 arc sec. This position is 1.7
arc sec. from the center of the XRT error circle. The estimated magnitude is
16.24. No correction has been made for the expected extinction corresponding to
E(B-V) of 0.02. 

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: GRB140508A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16231
SUBJECT: GRB 140508A: WHT spectroscopy
DATE:    14/05/09 03:06:22 GMT
FROM:    Klaas Wiersema at U Leicester  <kw113@leicester.ac.uk>

K. Wiersema (Leicester), N. Tanvir (Leicester), A. Levan (Warwick), 
R. Karjalainen (ING) report:

We observed the afterglow candidate of GRB 140508A (Singer et al. GCN 16226)
with the 4.2m William Herschel Telescope using the ACAM instrument.
We acquired 3x600s spectroscopic exposures, with midpoint 23:02 UT on 8 May 2014.
We find absorption lines of Mg II and Fe II at a common redshift of z=1.027, though we
caution this redshift is based on archival wavelength calibrations. This is consistent with 
the redshift reported by Malesani et al. (GCN 16229).


GRB_name: GRB140508A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16232
SUBJECT: GRB 140508A: Swift-XRT observations
DATE:    14/05/09 06:26:12 GMT
FROM:    Alex Amaral-Rogers at U.of Leicester  <aar14@leicester.ac.uk>

 reports on behalf of the Swift-XRT team:

We have analysed 3.0 ks of XRT data for the Fermi/GBM-detected burst:
GRB 140508A,  from 69.0 ks to 75.2 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. Using 2973 s of PC mode
data and 3 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 = 255.46650, +46.78033 which is equivalent to:

RA (J2000): 17h 01m 51.96s
Dec(J2000): +46d 46' 49.2"

with an uncertainty of 1.8 arcsec (radius, 90% confidence). This
position is 0.3 arcsec from the iPTF optical transient candidate (GCN
Circ. 16226).  The late-time light curve (from T0+69.0 ks) is
consistent with a constant source of mean count rate 2.0e-01 ct/sec.

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.01 (+0.25, -0.23). The
best-fitting absorption column is  7.8 (+5.9, -5.1) x 10^20 cm^-2, in
excess of the Galactic value of 2.1 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.3 x 10^-11 (3.9 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      7.8 (+5.9, -5.1) x 10^20 cm^-2
Galactic foreground: 2.1 x 10^20 cm^-2
Excess significance: 1.8 sigma
Photon index:      2.01 (+0.25, -0.23)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020376.

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


GRB_name: GRB140509A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16233
SUBJECT: GRB 140509A: Enhanced Swift-XRT position
DATE:    14/05/09 07:14:39 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 1253 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 140509A, 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 = 46.59538, -62.63941 which is equivalent
to:

RA (J2000): 03h 06m 22.89s
Dec (J2000): -62d 38' 21.9"

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: GRB140508A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16234
SUBJECT: Konus-Wind observation of GRB 140508A
DATE:    14/05/09 11:20:08 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, very intense GRB 140508A
(Fermi-GBM detection: Yu and Goldstein, GCN 16224;
IPN triangulation: Hurley et al., GCN 16225)
triggered Konus-Wind at T0=11038.423 s UT (03:03:58.423).

The light curve shows multiple emission episodes with decaying
peak intensity. A total duration of the burst is ~80 s.
The emission is seen up to ~9 MeV.

A hint of an extended emission in softer energy channels
can be traced to at least 250 s after the trigger; however,
its attribution to GRB 140508A is unclear due to the variable
solar particle background.

As observed by Konus-Wind, the burst had a fluence
of 7.4(-0.7,+0.8)x10^-5 erg/cm2, and a 64-ms peak flux,
measured from T0+2.576 s, of 3.0(-0.2,+0.2)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the first bursting episode
(measured from T0 to T0+72.448 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 = -1.11 (-0.08,+0.09),
the high energy photon index beta = -2.5 (-0.4,+0.2),
the peak energy Ep = 213 (-20,+23) keV,
chi2 = 70/86 dof.

The spectrum near the peak count rate (measured from T0 to T0+4.864 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 = -1.0 (-0.1,+0.1),
the high energy photon index beta = -2.4 (-0.2,+0.1),
the peak energy Ep = 345 (-47,+59) keV,
chi2 = 65/64 dof.

Assuming the redshift z=1.03 (Malesani et al., GCN 16229;
Wiersema et al., GCN 16231)
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 ~2.1x10^53 erg,
the peak luminosity L_iso is ~1.8x10^53 erg/s,
and the rest-frame peak energy, Ep,i, is ~430 keV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140508_T11038/

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


GRB_name: GRB140508A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16235
SUBJECT: GRB 140508A: Optical Observations via Virtual Telescope
DATE:    14/05/09 11:40:39 GMT
FROM:    Gianluca Masi at Bellatrix Astronomical Obs  <gianluca@bellatrixobservatory.org>

G. Masi (Ceccano, Italy) reports:

On May 09.06569 2014 UT (22.5 hours after the burst), we imaged the field around 
GRB 140508A  (Singer et al. GCN 16226) remotely using the the 0.43m-f/6.8 
robotic unit part of the Virtual Telescope robotic facility in Italy.

The source is visible on 300 seconds unfiltered CCD images at the following 
coordinates (J2000):

R.A. = 17 01 51.94
Decl. +46 46 49.2

We also performed photometry, assuming R-mags from UCAC-4 for the stars in the
field, getting an estimate for the magnitude of 19.3CR).

This message can be cited.


GRB_name: GRB140508A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16236
SUBJECT: GRB 140508A: RATIR Optical and NIR Observations
DATE:    14/05/09 14:34:57 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 140508A (Yu, et al., GCN 16224) 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 2014/05 9.19 to 2014/05 9.46 UTC (25.61 to
32.04 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.

For a source positionally coincident with the iPTF optical transient
(Singer, et al. , GCN 16226), in comparison with the SDSS DR9 and 2MASS, we
obtain the following detections:

  r     19.65 +/- 0.02
  i     19.52 +/- 0.02
  Z     19.36 +/- 0.03
  Y     19.20 +/- 0.03
  J     19.18 +/- 0.03
  H     18.98 +/- 0.03

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.  The source fades in time
approximately as t^(-1.5) in all bands during our observation.

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


GRB_name: GRB140509A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16237
SUBJECT: GRB 140509A: Swift-XRT refined Analysis
DATE:    14/05/09 14:38:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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), J.A. Kennea (PSU), V. Mangano (PSU), M.C. Stroh
(PSU) and K.L. Page report on behalf of the Swift-XRT team:

We have analysed 6.4 ks of XRT data for GRB 140509A (Page  et al. GCN
Circ. 16230),  from 102 s to 13.0 ks after the BAT trigger. The data
comprise 137 s in Windowed Timing (WT) mode (the first 8 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. 16233).

The light curve can be modelled with an initial power-law decay with an
index of alpha=1.43 (+0.18, -0.08), followed by a break at T+1030 s to
an alpha of 0.88 (+0.12, -0.10).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.66 (+0.17, -0.16). The
best-fitting absorption column is  4.9 (+4.5, -2.6) x 10^20 cm^-2,
consistent with the Galactic value of 2.2 x 10^20 cm^-2 (Willingale et
al. 2013). The PC mode spectrum has a photon index of 1.91 (+/-0.14)
and a best-fitting absorption column of 7.4 (+3.6, -3.3) x 10^20 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.4 x 10^-11 (4.0 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      7.4 (+3.6, -3.3) x 10^20 cm^-2
Galactic foreground: 2.2 x 10^20 cm^-2
Excess significance: 2.6 sigma
Photon index:      1.91 (+/-0.14)

If the light curve continues to decay with a power-law decay index of
0.88, the count rate at T+24 hours will be 8.4 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.9 x
10^-13 (3.3 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/00598497.

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


GRB_name: GRB140509A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16240
SUBJECT: GRB 140509A: Swift-BAT refined analysis
DATE:    14/05/09 17:41:50 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@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), 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 140509A (trigger #598497) (Page, et al.,
GCN Circ. 16230).  The BAT ground-calculated position is
RA, Dec = 46.564, -62.662 deg which is
    RA(J2000)  =  03h 06m 15.3s
    Dec(J2000) = -62d 39' 43"
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 19%.
  
The mask-weighted light curve shows a single FRED peak.  T90 (15-350 keV) is
23.20 +- 5.17 sec (estimated error including systematics).
  
The time-averaged spectrum from T-3.8 to T+23.1 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.59 +- 0.20.  The fluence in the 15-150 keV band is 1.2 +- 0.2 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T+1.78 sec in the 15-150 keV band
is 1.6 +- 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/598497/BA/


GRB_name: GRB140509A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16241
SUBJECT: GRB 140509A: Swift/UVOT Detection and photo-z
DATE:    14/05/09 17:42:38 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) 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 140509A
121 s after the BAT trigger (Page et al., GCN Circ. 16230).
A source consistent with the XRT position
(Beardmore et al. GCN Circ. 16233)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  03:06:22.69 =  46.59456 (deg.)
    Dec (J2000) = -62:38:21.7  = -62.63935 (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              121          271          147         17.00 +/- 0.03
v                  610          630           20         16.50 +/- 0.13
b                  536          556           20         17.04 +/- 0.10
u                  280          530          246         16.35 +/- 0.03
w1                 659         7011          490        >20.6
m2                 634         6806          490        >21.1
w2                 585         6396          432        >20.9

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).

The lack of detections in the UV filters suggests a redshift of about 2.4.


GRB_name: GRB140509B
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16242
SUBJECT: GRB 140509B: MAXI/GSC detection
DATE:    14/05/09 18:05:51 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

M. Kimura, S. Nakahira (JAXA),  M. Serino (RIKEN),  T. Sakamoto (AGU), 
S. Ueno, H. Tomida, M. Ishikawa, Y. E. Nakagawa (JAXA), T. Mihara, M. Sugizaki, 
M. Morii, J. Sugimoto, T. Takagi, A. Yoshikawa, M. Matsuoka (RIKEN), N. Kawai, 
T. Yoshii, Y. Tachibana (Tokyo Tech), A. Yoshida, Y. Kawakubo, H. Ohtsuki (AGU), 
H. Tsunemi, D. Uchida (Osaka U.), H. Negoro, M. Nakajima, K. Fukushima, 
T. Onodera, K. Suzuki (Nihon U.), Y. Ueda, M. Shidatsu, T. Kawamuro, T. Hori (Kyoto U.), 
Y. Tsuboi, M. Higa (Chuo U.), M. Yamauchi, Y. Morooka (Miyazaki U.), K. Yamaoka (Nagoya U.) 
report on behalf of the MAXI team:

The MAXI/GSC nova alert system triggered a bright uncatalogued X-ray transient source 
at 2014-05-09T16:18:38 UT.  Assuming that the source flux was constant over the transit,
we obtain the source position at

(R.A., Dec) = (312.966 deg, 21.016 deg) = (20 51 51, +21 00 57) (J2000)

with a statistical 90% C.L. elliptical error region with long and short radii of 0.27 deg and 
0.24 deg respectively.  The roll angle of long axis from the north direction is 124.0 deg 
counterclockwise.  Without the assumption about the source constancy, we obtain a rectangular 
error box for the transient source with the following corners:

(312.482 deg, 20.145 deg) = (20 49 55, +20 08 40) (J2000)
(312.039 deg, 20.483 deg) = (20 48 09, +20 28 59) (J2000)
(313.694 deg, 22.120 deg) = (20 54 46, +22 07 11) (J2000)
(314.137 deg, 21.776 deg) = (20 56 32, +21 46 32) (J2000)

There is an additional systematic uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 98 +- 23 mCrab (4-10keV, 1 sigma error).
There was no significant excess flux in the previous transit at UT 14:45 with an upper 
limit of 20 mCrab.


GRB_name: GRB140508A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16243
SUBJECT: GRB 140508A: Swift/UVOT Detection
DATE:    14/05/09 19:03:14 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F.E. Marshall (NASA/GSFC) and A. Amarel-Rogers (U. of Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140508A
68965 s after the GBM trigger (Yu and Goldstein, GCN Circ. 16224).
A source consistent with the optical position
(Singer et al., GCN Circ. 16226) and the X-ray position
(Amarel-Rogers, GCN Circ. 16232)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  17:01:51.95 = 255.46647 (deg.)
    Dec (J2000) = +46:46:49.5  =  46.78043 (deg.)
with an estimated uncertainty of 0.46 arc sec. (radius, 90% confidence).

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

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

v                68965        69792          814         19.38 +/- 0.10
b                70632        71427          782         19.59 +/- 0.06
u                69799        70626          814         18.81 +/- 0.05

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.031 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB140508A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16244
SUBJECT: GRB 140508A: â€‹HCT spectroscopy
DATE:    14/05/10 16:45:53 GMT
FROM:    Varun Bhalerao at IUCAA  <varunb@iucaa.ernet.in>

V. Bhalerao, D. K. Sahu report:
We obtained optical spectroscopy of the iPTF afterglow candidate of GRB140508A (Yu & Goldstein GCN 16224; Hurley et al., GCN 16225; Singer et al., GCN 16226) with the HFOSC instrument on the 2-m Himalayan Chandra Telescope (HCT). We obtained two spectra of 1800 sec each, spanning the wavelength range from 3800-8400A, at a mean time of 15.5 hours after the trigger. The spectrum shows weak absorption features, consistent with the Fe II and Mg II at redshift ~1.03, as identified by Malesani et al. (GCN 16229) and Wiersema et al. (GCN 16231).


GRB_name: GRB140508A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16246
SUBJECT: GRB 140508A: Continued RATIR Optical and NIR Observations
DATE:    14/05/12 16:15:45 GMT
FROM:    Nat Butler at UC berkeley  <natxbutler@gmail.com>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB),
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara
(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 140508A (Yu, et al., GCN 16224) 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 2014/05 10.31 to 2014/05 10.48 UTC (52.29 to
56.42 hours after the BAT trigger), obtaining a total of 2.49 hours
exposure in the r and i bands and 1.04 hours exposure in the Z, Y, J, and H
bands and again from 2014/05 11.23 to 2014/05 11.48 UTC (74.56 to 80.45
hours after the BAT trigger), obtaining a total of 3.91 hours exposure in
the r and i bands and 1.64 hours exposure in the Z, Y, J, and H bands.

For a source positionally coincident with the iPTF optical transient
(Singer, et al., GCN 16226), in comparison with the SDSS DR9 and 2MASS, we
obtain the following detections:

       t+54.4 hrs           t+77.5 hrs
  r    20.63 +/- 0.03    21.25 +/- 0.05
  i    20.47 +/- 0.03    21.08 +/- 0.05
  Z   20.29 +/- 0.05    21.04 +/- 0.08
  Y   20.24 +/- 0.07    20.76 +/- 0.10
  J   20.17 +/- 0.06    20.79 +/- 0.11
  H   19.92 +/- 0.08    20.58 +/- 0.13

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.  Including our initial set of
observations (Butler, et al., GCN 16236), the source appears to have faded
as t^(-1.5) in all bands.

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


GRB_name: GRB140423A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16247
SUBJECT: GRB 140423A: Mondy optical observations
DATE:    14/05/12 17:32:49 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 the optical afterglow (Elenin et al., GCN 16143; Kaur et 
al., GCN 16144; Ferrante et al., GCN 16145; Chester et al., GCN 16147;
Maehara et al., GCN 16151) of the Swift GRB 140423A (Sonbas et al.,
GCN 16142) with AZT-33IK telescope of Sayan observatory (Mondy). We took 
several images in R-filter of 60 s exposure on Apr., 25 and
of 120 s exposure on Apr., 26 and 27.

The details of the photometry are the following:

date        UT start   t-T0       Filter  Exp.    OT
                       (mid, days)          (s)
2014-04-25  16:36:21  2.36772     R       90*60   22.63+/-0.10
2014-04-26  15:56:26  3.34068     R       46*120  23.46+/-0.18
2014-04-27  14:15:32  4.27964     R       54*120  > 22.9

The photometry is based on two SDSS stars, R (gri -> R transformations 
by Lupton 2005):

SDSS id                      R
J130911.04+494854.6   20.209+/-0.053
J130924.79+494946.6   19.533+/-0.038


GRB_name: GRB140512A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16248
SUBJECT: GRB 140512A: MASTER optical observations
DATE:    14/05/12 19:49:04 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, 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

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  GRB140512A   171 sec after trigger 
time at 2014-05-12 19:34:40.212 UT. On our first (30s exposure) set we 
haven't found optical transient  within SWIFT error-box (ra=19 17 28 
dec=-15 06 00 r=0.050000).
The 5-sigma upper limit has been about 16.2 mag
Observations were made in twilight.
The message may be cited.


GRB_name: GRB140512A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16249
SUBJECT: GRB 140512A: Swift detection of a burst with an optical counterpart
DATE:    14/05/12 19:56:20 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

C. Pagani (U Leicester), S. D. Barthelmy (GSFC), D. N. Burrows (PSU),
J. R. Cummings (NASA/UMBC), N. Gehrels (NASA/GSFC),
J. A. Kennea (PSU), V. Mangano (PSU), C. J. Mountford (U Leicester),
K. L. Page (U Leicester), B. Sbarufatti (INAF-OAB/PSU),
M. H. Siegel (PSU), C. A. Swenson (PSU) and T. N. Ukwatta (MSU) report
on behalf of the Swift Team:

At 19:31:49 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140512A (trigger=598819).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 289.371, -15.100 which is 
   RA(J2000)  =  19h 17m 29s
   Dec(J2000) = -15d 05' 59"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a multi-peak event
with a total duration of about 170 sec.  The peak count rate
was ~8000 counts/sec (15-350 keV), at ~122 sec after the trigger. 

The XRT began observing the field at 19:33:27.5 UT, 98.4 seconds after
the BAT trigger. The position determined from promptly downlinked data
differs significantly from the on-board position, suggesting that the
XRT may have centroided on a cosmic ray; the initial XRT position
notice should be treated with caution. Using promptly downlinked data
we find an uncatalogued X-ray source located at RA, Dec 289.36925,
-15.09492 which is equivalent to:
   RA(J2000)  = 19h 17m 28.62s
   Dec(J2000) = -15d 05' 41.7"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 19 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 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 106 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 19:17:28.78 = 289.36991
  DEC(J2000) = -15:05:39.2  = -15.09423
with a 90%-confidence error radius of about 0.61 arc sec. This position is 3.4
arc sec. from the center of the XRT error circle. The estimated magnitude is
15.01 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.16. 

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


GRB_name: GRB140512A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16250
SUBJECT: GRB 140512A: MASTER OT decay and early light curve
DATE:    14/05/12 20:44:05 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy, V. Lipunov, 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.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  GRB140512A   171 sec after trigger time at 2014-05-12 
19:34:40.212 UT in two polarizations. We definetly see OT (Pagani et. al. 
GCN 16249)  on our images in bosh polarizations.

The preliminary automatic light curve available at Tab.1 and here:
http://master.sai.msu.ru/static/GRB/GRB140512A_lc.png

Table 1. GRB140512B early automatic light curve.

        T_start         T-T_trig   mag
  2014-05-12 19:34:44.3  175 sec  13.5
  2014-05-12 19:36:36.3  287 sec  13.9
  2014-05-12 19:38:21.9  392 sec  14.5
  2014-05-12 19:39:43.7  474 sec  14.8
  2014-05-12 19:41:05.3  556 sec  15.1
  2014-05-12 19:42:26.3  637 sec  15.2
  2014-05-12 19:43:47.3  718 sec  15.5
  2014-05-12 19:45:56.8  847 sec  16.2

Our unfiltered magnitude is well described by a parity 0.8R + 0.2B 
(USNO-B1)

The power low index alpha from 175 to 847 seconds after the trigger  is
1.5 +- 0.1  (F ~ t-apha).

We erraticly reported (Ivanov et. al. GCN 16248) that we don't see object 
earlier because of the wrong identification. We are sorry for it.

The message may be cited.


GRB_name: GRB140512A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16251
SUBJECT: GRB 140512A: Mondy optical detection
DATE:    14/05/12 20:47:05 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of GRB 140512A (Pagani et al., GCN 16249)   with 
AZT-33IK telescope of Sayan observatory (Mondy). We took several images 
in R-filter of 60 s exposure starting on May, 12 (UT) 19:56:58. We 
clearly detect a fading optical transient in the position reported early 
(Pagani et al., GCN 16249). A brightness of the OT in the first image is 
about R=16.7 (at (UT) 19:57:28, mid time). Observation is continuing.

The finding chart can be found in 
http://grb.rssi.ru/GRB140512A/GRB140512A_AZT33IK_R_fc.png


GRB_name: GRB140428A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16252
SUBJECT: GRB 140428A: GROND afterglow confirmation
DATE:    14/05/12 21:05:18 GMT
FROM:    Karla Varela at MPE  <kvarela@mpe.mpg.de>

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

We re-observed the field of GRB 140428A (Swift trigger 597519; Kocevski et
al.,
GCN #16177) 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 La Silla Observatory
(Chile).

A second epoch obtained on May 6th at 02:01 UT, about 7 days after the
trigger,
shows that the source reported by Knust et al. (GCN # 16191) has clearly
faded.
We find z' > 23.3, suggesting that the source has faded by at least 1.9 mag,
and confirming that this was the afterglow of GRB 140428A.


GRB_name: GRB140512A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16253
SUBJECT: GRB 140512A: Optical observations from the 2.5 m NOT
DATE:    14/05/13 03:16:22 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), D. Xu (DARK/NBI), T. Kruehler (ESO), A.A. Djupvik (NOT),
E. Gafton (OKC, Stockholm Univ.) and T. Libbrecht (Stockholm Univ.)
report on behalf of a larger collaboration:

We have observed the field of GRB 140512A (Pagani et al. GCN 16249)
with the AlFOSC instrument on the 2.5 m Nordic Optical Telescope (La
Palma, Spain), as part of the Stockholm remote observing school.
Observations consisted of 3x300s imaging in R, starting at 02:10 UT
(6.65 hrs after the burst). Observations were performed under variable
seeing conditions of 2.0-2.5". Preliminary photometry, based on the
USNO-B1.0 catalogue yields R~19.5 mag. Spectroscopic observations
are ongoing.


GRB_name: GRB140508A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16254
SUBJECT: Swift Observations of GRB 140508A
DATE:    14/05/13 05:30:00 GMT
FROM:    Alex Amaral-Rogers at U.of Leicester  <aar14@leicester.ac.uk>

Alex Amaral-Rogers reports on behalf of the Swift-XRT team:

Swift has reobserved the field of GRB 140508A for a further 4.6 ks from 253.9 ks
to 288.1 ks after the Fermi/GBM trigger.

The source reported in GCN 16232 has been observed in the XRT to be fading;
consistent with a power-law decay with an index of alpha = 1.48 (+0.15, -0.14).

We now confirm the the source is the afterglow of GRB 140508A.


GRB_name: GRB140512A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16255
SUBJECT: GRB 140512A: Enhanced Swift-XRT position
DATE:    14/05/13 06:52:43 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Using 5222 s of XRT Photon Counting mode data and 10 UVOT
images for GRB 140512A, 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 = 289.37006, -15.09430 which is equivalent
to:

RA (J2000): 19h 17m 28.81s
Dec (J2000): -15d 05' 39.5"

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

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

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


GRB_name: GRB140512A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16256
SUBJECT: GRB 140512A: Swift-XRT refined Analysis
DATE:    14/05/13 07:56:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.1 ks of XRT data for GRB 140512A (Pagani  et al. GCN
Circ. 16249),  from 87 s to 12.6 ks after the  BAT trigger. The data
comprise 841 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 late-time light curve (from T0+4.6 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.06 (+/-0.09).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.460 (+0.029, -0.016). The
best-fitting absorption column is  consistent with the Galactic value
of 1.5 x 10^21 cm^-2 (Willingale et al. 2013). The PC mode spectrum has
a photon index of 1.80 (+/-0.07) and a best-fitting absorption column
of 2.02 (+0.28, -0.26) x 10^21 cm^-2. The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 4.0 x 10^-11 (5.1 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.02 (+0.28, -0.26) x 10^21 cm^-2
Galactic foreground: 1.5 x 10^21 cm^-2
Excess significance: 3.4 sigma
Photon index:      1.80 (+/-0.07)

If the light curve continues to decay with a power-law decay index of
1.06, the count rate at T+24 hours will be 0.15 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.8 x
10^-12 (7.4 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00598819.

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


GRB_name: GRB140512A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16257
SUBJECT: GRB140512A : GROND observations
DATE:    14/05/13 09:52:24 GMT
FROM:    Karla Varela at MPE  <kvarela@mpe.mpg.de>

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

We observed the field of GRB 140512A (Pagani et al., GCN 16249)
simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120,
405) mounted at the 2.2m MPG telescope at La Silla Observatory (Chile).

Observations started at 03:36 UT on May 13, about 8.0 hrs after the GRB
trigger. They were performed at an average seeing of 1.7" and at an
average airmass
of 2.3.

The afterglow discovered by Gorbovskoy et al. (GCN 16250)
is detected in all optical bands and the JH bands. At a mean time of 04:02
UT, with
a 264 s exposure in griz bands and 240 s in JHK, we measure the following
preliminary AB magnitudes:

g'= 20.3 +/- 0.1 mag,
r'= 19.7 +/- 0.1 mag,
i'= 19.5 +/- 0.1 mag,
z'= 19.3 +/- 0.1 mag,
J = 19.0 +/- 0.1 mag,
H = 18.6 +/- 0.1 mag, and
K > 18.2 mag.

The given optical and NIR magnitudes are calibrated against GROND
zeropoints and
2MASS field stars in g'r'i'z and JHK respectively, and are not corrected
for the
Galactic foreground extinction corresponding to a reddening of E(B-V)=0.16
in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB140512A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16258
SUBJECT: GRB 140512A: Swift-BAT refined analysis
DATE:    14/05/13 13:34:16 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.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), C. Pagani (U Leicester),
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-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140512A (trigger #598819)
(Pagani, et al., GCN Circ. 16249).  The BAT ground-calculated position is
RA, Dec = 289.366, -15.087 deg which is
    RA(J2000)  =  19h 17m 27.9s
    Dec(J2000) = -15d 05' 14.8"
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 35%.

The mask-weighted light curve shows a complex structure.  The first group of 
multiple peaks begins at ~T-15 sec, reaches maximum at T+0 sec, and returns to 
background by ~T+40 sec.  Then a second longer, brighter group of multiple peaks 
begins at ~T+85 sec, reaches maximum at T+120 sec and falls to background by 
T+170 sec. T90 (15-350 keV) is 154.8 +- 4.88 sec (estimated error including 
systematics).

The time-averaged spectrum from T-22.84 to T+186.29 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.45 +- 0.04.  The fluence in the 15-150 keV band is 1.4 +- 0.03 x 10^-5 
erg/cm2. The 1-sec peak photon flux measured from T+121.96 sec in the 15-150 keV 
band is 6.8 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence 
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/598819/BA/


GRB_name: GRB140508A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16259
SUBJECT: GRB 140508A: MITSuME Akeno Optical observation
DATE:    14/05/13 13:52:06 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

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

We observed the field of GRB 140508A (H.Yu et al., GCN Circular #16224) 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 2014-05-09 11:07:31 UT (32.1h after the burst).
We detected the optical afterglow of GRB140508A in the g',Rc and Ic band.

The measured magnitudes were listed below.

T0+[h]         T-EXP[sec]               g'                Rc              Ic
----------------------------------------------------------------------------------------
 35.3            19800             20.16+/-0.22      19.74+/-0.24    18.85+/-0.17
----------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst 
T-EXP: Total Exposure time 
We used GSC2.3 catalog for flux calibration.


GRB_name: GRB140508A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16260
SUBJECT: GRB 140508A: Mondy upper limit
DATE:    14/05/13 14:17:02 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 the field of GRB 140508A (Yu et al., GCN 16224) with
AZT-33IK telescope of of Sayan observatory (Mondy) starting on May, 12 
(UT) 15:32:03. Within enhanced Swift-XRT error circle (Amarel-Rogers et 
al., GCN 16232) we do not detect the optical source reported by Singer 
et al. (GCN 16226).

Details of the photometry are the following:

date         UT start   t-T0        Exp.     Filter   UpperLimit
                        (mid, days)  (s)               (3sigma)
2014-05-12   15:32:03   4.56124     60x120   R        22.9

The photometry is based on a reference star from SDSS-DR9,
(R mag, transformation by Lupton 2005):

SDSS_id               R(Lupton)   err
J170144.75+464707.7   18.272      0.018


GRB_name: GRB140512A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16261
SUBJECT: GRB 140512A:  Xinglong TNT optical observation
DATE:    14/05/13 16:25:20 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

L. P. Xin,   X. F. Wang,  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 140512A (Pagani et al., GCN 16429)  with Xinglong 
0.8-m TNT telescope at 19:33:54  (UT) , 126 sec after the burst.

The optical counterpart (Pagani et al., GCN 16429) was clearly detected
 in our white and R band images.  A preliminary analysis shows that 
the brightness of the OT was fading from 13.0 mag to 17.0 mag, 
calibrated by nearby USNO B1.0 R2mag, during our observation epoch,  
with an index of  1.54  after fitting by a single power law.

The message may be cited.


GRB_name: GRB140512A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16262
SUBJECT: GRB 140512A: Fermi GBM detection
DATE:    14/05/13 18:01:19 GMT
FROM:    Matthew Stanbro at UAH/Fermi  <mcs0001@uah.edu>

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

"At 19:31:42.50 UT on 12 May 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140512A (trigger 421615905 / 140512814)
which was also detected by Swift (C. Pagani et al. 2014, GCN 16249).
The GBM on-ground location, using the Fermi GBM trigger data,
is consistent with the Swift/BAT location.

The GBM light curve shows a complex structure, consisting of two main
separated episodes with a total duration (T90) of about 148.0 s (50-300
keV).
The time-averaged spectrum from T0-10.240 s to T0+152.578 s is well fit
by a power law function with an exponential high-energy cutoff.
The power law index is -1.33 +/- 0.03 and the cutoff energy,
parameterized as Epeak, is 588 +/- 84 keV.


The event fluence (10-1000 keV) in this time interval is
(4.30 +/- 0.10)E-05 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+128.70 s in the 10-1000 keV band is 11.0 +/- 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: GRB140512A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16263
SUBJECT: GRB 140512A: Continued UVOT Observations
DATE:    14/05/13 20:08:32 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

B. Porterfield (PSU) and C. Pagani (U Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140512A
106 s after the BAT trigger (Pagani et al., GCN Circ. 16249).
We can confirm the detection of a fading source  with the
UVOT position
  RA(J2000)  = 19:17:28.78 = 289.36991
  DEC(J2000) = -15:05:39.2  = -15.09423

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

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

white (fc)         106          256          293       14.91 +/- 0.07
white              106         1022          186       16.99 +/- 0.07
white             1175         6197          412       19.07 +/- 0.08
v                   88         1072           68       15.97 +/- 0.09
v                 4973         6608          393       18.68 +/- 0.15
b                  574         1344           76       16.84 +/- 0.08
b                 5793         5992          196       19.56 +/- 0.19
u (fc)             319          568          491       15.37 +/- 0.07
u                 5587         7102          275       19.08 +/- 0.18
uvw1               697         1295           58       17.52 +/- 0.19
uvw1              5383         7018          393       20.10 +/- 0.34
uvm2               672         1270           77      >18.71
uvm2              5177         6812          393      >20.17
uvw2               624         1220           77      >19.05
uvw2              4769         6403          393      >20.47

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.162 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB140423A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16264
SUBJECT: GRB 140423A: AAO optical upper limits
DATE:    14/05/14 14:27:00 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the optical afterglow (Elenin et al., GCN 16143; Kaur et 
al., GCN 16144; Ferrante et al., GCN 16145; Chester et al., GCN 16147; 
Maehara et al., GCN 16151) of the Swift GRB 140423A (Sonbas et al., GCN 
16142) with AS-32 (0.7m) telescope of Abastumani Observatory on Apr. 24 
at (UT) 00:29-01:16 and Apr. 24 (UT) 17:46-19:16. We obtained several 
unfiltered   frames with exposures of 120 s. Within the enhanced XRT 
circle (Beardmore et al., GCN 16155) in the stacked images from both 
epochs we do not detect the afterglow.

The details of the photometry are the following:

UT start   t-T0         Filter   Exp.    Uplim
           (mid, days)   (s)              (3 sigma)
00:29:23  0.68139       None    16*120   20.3


The photometry is based on SDSS stars, R mag (R mag obtained using ugriz
transformations in BVRI (Lupton, 2005):

SDSS id                R_Lupton
J130858.37+494547.9   15.418 Â± 0.018
J130914.51+494636.5   18.661 Â± 0.019


GRB_name: GRB140512A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16265
SUBJECT: Konus-Wind observation of GRB 140512A
DATE:    14/05/14 15:26:32 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:

A long-duration GRB 140512A (Swift-BAT trigger 598819: Pagani et al., 
GCN 16249; Sakamoto et al., GCN 16258; Fermi-GBM detection: Stanbro, GCN 
16262) triggered Konus-Wind at T0=70310.769 s UT (19:31:50.769).

The light curve shows two separated multipeaked episodes: the first from 
~T0-21 s to ~T0+12 s and the second longer and brighter from ~T0+88 s to 
~T0+158 s. A total duration of the burst is ~179 s.

As observed by Konus-Wind, the burst had a fluence
of 4.8(-0.8,+2.0)x10^-5 erg/cm2, and a 256-ms peak flux,
measured from T0+121.856 s, of 3.7(-1.2,+1.3)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the first bursting episode
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 1.2 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -0.85 (-0.47,+0.61)
and Ep = 279 (-69,+148) keV (chi2 = 62/60 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy
photon index: beta < -2.1 (chi2 = 62/59 dof).

The time-averaged spectrum of the second bursting episode
(measured from T0+90.368 to T0+155.904 s)
is best fit in the 20 keV - 6 MeV range
by a power law with exponential cutoff model with the following parameters:
alpha = -1.30 (-0.18,+0.21)
and Ep = 466 (-124, +287) keV (chi2 = 79/79 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy
photon index: beta < -1.9 (chi2 = 78/78 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140512_T70310/

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


GRB_name: GRB140508A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16266
SUBJECT: GRB 140508A: VLA detection
DATE:    14/05/14 21:23:46 GMT
FROM:    Assaf Horesh at Caltech  <assafh@astro.caltech.edu>

A. Horesh (Weizmann Institute), L. P. Singer (Caltech), S. B. Cenko (NASA/GSFC),  M. M. Kasliwal (Carnegie Observatories/Princeton), and D. Perley (Caltech) report on behalf of a larger collaboration: 

We observed iPTF14aue, the afterglow candidate of GRB140508A (Yu & Goldstein, GCN 16224; Hurley et al., GCN 16225; Singer et al., GCN 16226) with the Jansky Very Large Array (VLA). The observations were undertaken on 2014 May 13 UT, 5.2 days after the Fermi trigger. We detected the source at 6.1 GHz (C-band) with a flux of 127 +/- 9 micro Jy. The source was also detected at 22 GHz (K-band). 

We thank the VLA staff for scheduling this target of opportunity.


GRB_name: GRB140515A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16267
SUBJECT: GRB 140515A: Swift detection of a burst
DATE:    14/05/15 09:30:47 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

P. D'Avanzo (INAF-OAB), M. G. Bernardini (INAF-OAB), V. D'Elia (ASDC),
P. A. Evans (U Leicester), P. T. O'Brien (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL) and
B. Sbarufatti (INAF-OAB/PSU) report on behalf of the Swift Team:

At 09:12:36 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140515A (trigger=599037).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 186.036, +15.077 which is 
   RA(J2000) = 12h 24m 09s
   Dec(J2000) = +15d 04' 38"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked
structure with a duration of about 30 sec.  The peak count rate
was ~1200 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 09:13:52.4 UT, 75.8 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 186.0639,
15.1045 which is equivalent to:
   RA(J2000)  = 12h 24m 15.35s
   Dec(J2000) = +15d 06' 16.4"
with an uncertainty of 2.2 arcseconds (radius, 90% containment). This
location is 138 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 2.54
x 10^20 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 79 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 0.02. 

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


GRB_name: GRB140515A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16269
SUBJECT: GRB 140515A: Gemini-N redshift
DATE:    14/05/15 13:55:55 GMT
FROM:    Ryan Chornock at Harvard  <rchornock@cfa.harvard.edu>

R. Chornock (Harvard), D. B. Fox (Penn State), and E. Berger (Harvard) report:

We observed the field of GRB 140515A (D'Avanzo et al., GCN 16267) using GMOS on 
the Gemini-N 8-m telescope, starting at 10:48 UT on 15 May. A faint source was 
present in the i band acquisition image at a position consistent with the X-ray 
afterglow.  We obtained 2x900s of spectroscopy of this likely afterglow, 
covering the wavelength range 5900-10150 Angstroms at a resolution of R~1200. 
The afterglow has a strong continuum at long wavelengths that sharply drops to 
near zero at wavelengths shortward of lambda~8900 Angs, consistent with the 
onset of Lyman-alpha absorption at z=6.32.  Isolated wavelength intervals of IGM 
transmission exist between 7500 and 8000 Angs (corresponding to z~5.2-5.6 
relative to Ly-alpha).  Further analysis is ongoing.

We acknowledge excellent support from Gemini observer Lucas Fuhrman.


GRB_name: GRB140515A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16270
SUBJECT: GRB 140515A: Enhanced Swift-XRT position
DATE:    14/05/15 14:10:01 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 2066 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 140515A, 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 = 186.06452, +15.10491 which is equivalent
to:

RA (J2000): 12h 24m 15.48s
Dec (J2000): +15d 06' 17.7"

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: GRB140515A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16271
SUBJECT: GRB 140515A: MITSuME Akeno upper limits
DATE:    14/05/15 14:19:22 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

H. Ohuchi, T. Yoshii, Y. Saito, Y. Tachibana, 
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 140515A  (P.D'Avanzo et al., GCN Circular #16267) 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 2014-05-15 10:32:10 UT ( 1.3h after the burst).
We did not find any new point source within the enhanced XRT circle 
in all the three bands.The measured magnitudes were listed below.

T0+[sec]     MID-UT    T-EXP[sec]     g'            Rc          Ic
---------------------------------------------------------------------------------------------------------
 9301         11:47:37        9180         > 20.8    >20.5    >19.4
---------------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst 
T-EXP: Total Exposure time 
We used GSC2.3 catalog for flux calibration.


GRB_name: GRB140423A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16272
SUBJECT: GRB 140423A: HCT optical observations
DATE:    14/05/15 16:31:36 GMT
FROM:    D.K. Sahu at Indian Inst of Astrophysics,Bangalore  <dks@iiap.res.in>

D.K. Sahu (Indian Institute of Astrophysics, Bangalore, India) reports:

The optical afterglow of Swift detected GRB 140423A (E.Sonbas et al., 
GCN 16142) was observed in Bessell R band, with the 2m. Himalayan 
Chandra Telescope of the Indian Astronomical Observatory, Hanle, India. 
Observations were made between 15:12 UT and 20:48 UT on 23/04/2014.
The optical afterglow (Elenin et al., GCN 16143; Kaur et al., 
GCN 16144; Ferrante et al., GCN 16145) was detected in our 
individual frames. The preliminary R magnitudes of the optical 
afterglow calibrated using nearby USNO B1 stars is as under.

Date Mid UT Exp R Magnitude
(sec) 
23-04-2014 15:03 180+300 20.35 +/- 0.05 
23-04-2014 17:44 2x300 20.68 +/- 0.06 
23-04-2014 20.40 2x300 21.08 +/- 0.06 


GRB_name: GRB140515A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16273
SUBJECT: GRB 140515A: Swift/UVOT Upper Limits
DATE:    14/05/15 18:09:41 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (IAA-CSIC,UCL-MSSL) and P. D'Avanzo (INAF-OAB)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140515A
79 s after the BAT trigger (D'Avanzo et al., GCN Circ. 16267).
No optical afterglow consistent with the XRT position
(Goad et al. GCN Circ. 16270) is detected in the initial UVOT exposures.
The lack of detection in all UVOT filters is consistent with a redshift of  
6.32 (Chornock et al., GCN Circ. 16269).

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            79          229          147         >20.7
u_FC               293          542          246         >20.0
white               79         7407          638         >21.5
v                  628         7818          471         >19.7
b                  548         7202          456         >20.6
u                  293        13671          1398        >20.9
w1                1618        12925          1140        >20.9
m2                6387        12019          1082        >20.6
w2                5977         7612          393         >20.5

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: GRB140515A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16274
SUBJECT: GRB 140515A: Gemini-North imaging
DATE:    14/05/15 19:26:23 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

W. Fong (Harvard), R. Chornock (Harvard), D. Fox (PSU), and E. Berger
(Harvard) report:

"We observed the location of the long-duration GRB 140515A (D'Avanzo et
al., GCN 16267) with the Gemini Multi-Object Spectrograph (GMOS) mounted on
the Gemini-North 8-meter telescope at a mid-time of 2014 May 15.458 UT
(1.78 hr after the BAT trigger). We obtained 480 sec in each of the i- and
z-bands in 0.45" seeing. We detect the optical afterglow (Chornock et al.,
GCN 16269), within the enhanced XRT position (Goad et al., GCN 16270),
located at

RA(J2000) = 12:24:15.51
Dec(J2000) = +15:06:16.6

with a positional uncertainty of 0.1" in each coordinate. The optical
afterglow has a brightness of z = 20.27 +/- 0.11 AB mag, and is at least 3
mag fainter in our i-band observations. Both the astrometry and photometry
are calibrated to SDSS.

We thank the Gemini staff for their assistance with these observations."


GRB_name: GRB140515A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16275
SUBJECT: GRB 140515A: KAIT Optical Upper Limit
DATE:    14/05/15 19:34:45 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 140515A (D'Avanzo et al.,
GCN 16267) starting at 09:14:22 UT, 106 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 the optical afterglow (Chornock
et al., GCN 16269; Fong et al., GCN 16274) in our
images within the enhanced XRT error circle (Goad et al., GCN 16270).
The typical limiting magnitude of our single clear image is about 
17.8, and about 17.1,16.9 mag for the V and I bands respectively.

[GCN OPS NOTE(15may14): Per author's request, the Sahu/16272 reference
was removed as it refers to a different GRB.]


GRB_name: GRB140515B
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16276
SUBJECT: GRB 140515B: MAXI/GSC detection
DATE:    14/05/15 23:22:58 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

M. Morii (RIKEN), S. Ueno, H. Tomida, S. Nakahira, M. Kimura, M. Ishikawa, 
Y. E. Nakagawa (JAXA), T. Mihara, M. Sugizaki, J. Sugimoto, T. Takagi, 
A. Yoshikawa, M. Matsuoka (RIKEN), N. Kawai, T. Yoshii, Y. Tachibana (Tokyo Tech),
A. Yoshida, T. Sakamoto, Y. Kawakubo, H. Ohtsuki (AGU), H. Tsunemi, 
D. Uchida (Osaka U.), H. Negoro, M. Nakajima, K. Fukushima, T. Onodera, 
K. Suzuki (Nihon U.), Y. Ueda, M. Shidatsu, T. Kawamuro, T. Hori (Kyoto U.),
Y. Tsuboi (Chuo U.), M. Yamauchi, Y. Morooka (Miyazaki U.), K. Yamaoka (Nagoya U.)
report on behalf of the MAXI team:

The MAXI/GSC nova alert system triggered a bright uncatalogued X-ray transient 
source at 2014-05-15T13:00:53 UT.  Assuming that the source flux was constant 
over the transit, we obtain the source position at

(R.A., Dec) = (289.354 deg, -11.701 deg) = (19 17 24, -11 42 03) (J2000)

with a rectangular error box in the following corners:

(289.185 deg, -12.277 deg) = (19 16 44, -12 16 38) (J2000)
(288.651 deg, -11.941 deg) = (19 14 36, -11 56 28) (J2000)
(289.546 deg, -10.794 deg) = (19 18 11, -10 47 39) (J2000)
(290.074 deg, -11.136 deg) = (19 20 17, -11 08 10) (J2000).

There is an additional systematic uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 80 +- 18 mCrab (4-10keV, 1 sigma error).
There was no significant excess flux in the previous transit at UT 11:28
and in the next transit at 14:33 UT with an upper limit of 20 mCrab for each.  


GRB_name: GRB140515A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16277
SUBJECT: GRB 140515A: Swift-XRT refined Analysis
DATE:    14/05/15 23:58:11 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

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

We have analysed 7.1 ks of XRT data for GRB 140515A (D'Avanzo  et al.
GCN Circ. 16267),  from 60 s to 13.6 ks after the  BAT trigger. The
data comprise 9 s in Windowed Timing (WT) mode (taken while Swift was
slewing), with the remainder in Photon Counting (PC) mode. The enhanced
XRT position for this burst was given by Goad et al. (GCN Circ. 16270).


The light curve can be modelled with  a power-law decay with an initial
decay index of alpha=2.5 (+0.5, -0.3). Then at T0+1100 s the light
curve rises, reaching a count rate ~ 0.3 ct/sec. The remaining two
orbits show irregular rate variations likely due to an underlying
flaring activity, with a count rate ~ 0.3 ct/sec and ~ 0.1 ct/sec
respectively.

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.75 (+0.12, -0.11). The
best-fitting absorption column is  1.7 (+3.2, -1.7) x 10^22 cm^-2, at a
redshift of 6.32 (Chornock et al., GCN Circ. 16269), in addition to the
Galactic value of 2.5 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 3.7 x 10^-11 (3.9 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 2.5 x 10^20 cm^-2
Intrinsic column:    1.7 (+3.2, -1.7) x 10^22 cm^-2 at z=6.32
Photon index:      1.75 (+0.12, -0.11)


The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00599037.

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


GRB_name: GRB140515A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16278
SUBJECT: GRB 140515A: Optical observations from the 2.5 m NOT
DATE:    14/05/16 00:30:12 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), D. Xu (DARK/NBI), J.P.U. Fynbo

(DARK/NBI), P. Jakobsson (U. Iceland), D. Malesani

(DARK/NBI), N.R. Tanvir (U. Leicester), E. Gafton

(OKC, Stockholm Univ.) and T. Libbrecht (Stockholm Univ.)

report on behalf of a larger collaboration:


We have observed the afterglow of GRB 140515A (D'Avanzo et al.,

GCN 16267) with the 2.5m NOT telescope. Observations consisted

of 5x300s imaging in the z-band and have an average epoch of

12.10 hr after the burst. The images reveal the optical afterglow

detected by Chornock et al. (GCN 16269) and Fong et al. (GCN

16274) at a magnitude of z(AB) = 22.15+/-0.15, as compared with

SDSS stars. This indicates a decay with a slope of alpha ~ -0.9

(where F_nu~t^alpha) as compared with the photometry of Fong

et al. (GCN 16274). Further observations are ongoing.


GRB_name: GRB140515A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16279
SUBJECT: GRB 140515A: Spectroscopy from the 10.4m GTC
DATE:    14/05/16 02:49:04 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), C.C. Thoene (IAA-CSIC), A. Cabrera-Lavers, D. Reverte and C.
Alvarez (IAC-ULL) report on behalf of a larger collaboration:


We have obtained spectroscopic observations of the afterglow of GRB 140415A
(D'Avanzo et al., GCN 16267; Chornock et al. GCN 16269; Fong et al. GCN
16274; de Ugarte Postigo et al. GCN 16278) using the 10.4m GTC telescope
(+OSIRIS). Our observation started at 22:37 UT (13.41 hr after the burst),
with a seeing of 0.6", and consisted of 3x1800s exposures using grism
R2500I, which covers the range between 7330 and 10000 A at a resolution of
~2500.


In a preliminary reduction we detect a strong continuum above 8900 A, with
no significant absorption features. The sharp decay below 8900 A is
consistent with Ly-alpha absorption at the redshift of 6.32 suggested by
Chornock et al. (GCN 16269). The transmission of the Ly-forest is low, but
some emission is detected down to the blue limit of our spectrum.


GRB_name: GRB140515A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16280
SUBJECT: GRB 140515A: GROND observation of the afterglow
DATE:    14/05/16 12:22:49 GMT
FROM:    Sebastian Schmidl at TLS Tautenburg  <schmidl@tls-tautenburg.de>

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

We observed the field of GRB 140515A (Swift trigger 599037; D'Avanzo et
al., GCN 16267) 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 22:53 UT on March 15, 2014, 13.7 hrs after
the GRB trigger. They were performed at an average seeing of 0.9" and at
an average airmass of 1.4.

We detect the afterglow reported by Chornock et al. (GCN 16269).

Based on a total exposure of 50 min in g'r'i'z' and 40 min in JHK, at
a mid-time of 17.0 hrs after the burst, we measure the following
preliminary magnitudes (in AB):

g' > 24.1 mag,
r' > 24.5 mag,
i' > 24.2 mag,
z' = 22.1 +/- 0.1 mag,
J  = 20.9 +/- 0.2 mag,
H  = 20.9 +/- 0.2 mag, and
K  > 19.1 mag.

Based on these data, the photometric redshift is z= 6.5 +/-0.2, which is
consistent with the spectroscopic redshift reported by Chornock et al.
(GCN 16269).

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) = 0.02 mag in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB140419A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16281
SUBJECT: GRB 140419A: Continued Mondy optical observations
DATE:    14/05/16 15:49:12 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 continued observation of the Swift GRB 140419A (Marshall et al., GCN 
16118) with AZT-33IK telescope of Sayan observatory (Mondy) on Apr.
25-26. We took several images in R-filter with the exposure of 60 
seconds. On a stacked image from Apr. 25 we detect the optical afterglow
(Zheng et al., GCN 16119; Guver et al., GCN 16120; Butler et al., GCN 
16121; Kuin et al., GCN 16123; Hentunen et al., GCN 16126). On the 
stacked frame from Apr. 26 in the Swift/XRT error circle (Osborne et 
al., GCN 16124) we do not detect any source.

Details of a photometry are the following:

date         UT start   t-T0      Filter   Exp.     OT
                         (mid, days)        (s)
2014-04-25   14:48:25   6.47713   R        90*60    22.81+/-0.17
2014-04-26   14:21:55   7.45841   R        90*60   >21.7 (3 sigma)

The photometry is based on nearby SDSS star, R (gri -> R transformations 
by Lupton 2005):

SDSS id               R
J082752.69+461357.4   17.381+/-0.018


GRB_name: GRB140515A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16282
SUBJECT: GRB 140515A : TNG near-infrared observations
DATE:    14/05/16 15:51:49 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

A. Melandri, P. D'Avanzo (INAF/OAB), A. Fiorenzano and G. Mainella (INAF/TNG) report on behalf of the CIBO collaboration:.

We observed the field of GRB 140515A (D'Avanzo et al., GCN 16267) using the NICS near-Infrared camera on the 3.6m TNG Telescope (La Palma, Canary Islands).

We obtained a series of imaging observations in the J and H bands for a total exposure time of 30 and 60 minutes respectively. The GRB afterglow is clearly detected in both bands at a level of

      Dt                Exposure    Filter      Mag (err)
[hr from GRB]      [min]        

    14.54    60          H   19.35 (0.12)
    15.60    30   J   19.52 (0.18)


Magnitudes are in the Vega system, calibrated against the 2MASS catalogue. We thank the TNG staff for the support.


GRB_name: GRB140515A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16283
SUBJECT: GRB 140515A: VLA Detection
DATE:    14/05/16 17:06:52 GMT
FROM:    Tanmoy Laskar at Harvard U  <tanmoylaskar@gmail.com>

T. Laskar, A. Zauderer, and E. Berger (Harvard) report:

"We observed the position of GRB 140515A (D'Avanzo et al; GCN 16267) at
multiple frequencies with the VLA beginning 2014 May 16.00 UT (0.62 days
after the burst). At a mean frequency of 21.8 GHz, we detect a radio source
with a preliminary flux density of ~ 0.1 mJy at

RA = 12:24:15.5055 +/- 0.0005
Dec = +15:06:16.609 +/- 0.005

consistent with the enhanced Swft/XRT position (D'Avanzo et al.; GCN 16277)
and the optical position (Fong et al.; GCN 16274). Follow-up observations
are planned."


GRB_name: GRB140515A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16284
SUBJECT: GRB 140515A: Swift-BAT refined analysis
DATE:    14/05/16 20:03:00 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), P. D'Avanzo (INAF-OAB), 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-288 to T+962 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140515A (trigger #599037)
(D'Avanzo, et al., GCN Circ. 16267).  The BAT ground-calculated position is
RA, Dec = 186.071, 15.099 deg which is
  RA(J2000)  =  12h 24m 17.0s
  Dec(J2000) = +15d 05' 55.8"
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 99%.

The mask-weighted light curve shows a double-peaked structure. The first pulse
starts at ~T-22 s and peaks at ~T-18 s. The second pulse starts at ~T-10 s, peaks
at ~T+2 s, and ends at ~T+4 s.  T90 (15-350 keV) is 23.4 +- 2.1 sec (estimated
error including systematics).

The time-averaged spectrum from T-22.0 to T+3.8 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 0.98 +- 0.64,
and Epeak of 51.3 +- 14.7 keV (chi squared 54.37 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 5.9 +- 0.6 x 10^-7 erg/cm2
and the 1-sec peak flux measured from T+1.51 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 1.85 +- 0.13 (chi squared 61.03 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/599037/BA/


GRB_name: GRB140516A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16285
SUBJECT: GRB 140516A: Swift detection of a short burst
DATE:    14/05/16 20:44:47 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

M. G. Bernardini (INAF-OAB), S. D. Barthelmy (GSFC),
S. B. Cenko (GSFC), P. D'Avanzo (INAF-OAB), J. A. Kennea (PSU),
N. P. M. Kuin (UCL-MSSL), A. Y. Lien (NASA/GSFC/ORAU),
V. Mangano (PSU), C. B. Markwardt (NASA/GSFC),
F. E. Marshall (NASA/GSFC), A. Maselli (INAF-IASFPA),
A. Melandri (INAF-OAB), D. M. Palmer (LANL),
J. L. Racusin (NASA/GSFC), B. Sbarufatti (INAF-OAB/PSU),
M. H. Siegel (PSU) and T. N. Ukwatta (MSU) report on behalf of the
Swift Team:

At 20:30:54 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140516A (trigger=599188).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 252.988, +39.915 which is 
   RA(J2000) = 16h 51m 57s
   Dec(J2000) = +39d 54' 53"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 0.1 sec.  The peak count rate
was ~3000 counts/sec (15-350 keV), at ~0.1 sec after the trigger. 

The XRT began observing the field at 20:32:14.0 UT, 79.3 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 252.9890, 39.9626 which
is equivalent to:
   RA(J2000)  = 16h 51m 57.35s
   Dec(J2000) = +39d 57' 45.4"
with an uncertainty of 2.7 arcseconds (radius, 90% containment). This
location is 171 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 1.52
x 10^20 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 83 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 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 0.02. 

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


GRB_name: GRB140516A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16286
SUBJECT: GRB 140516A: TNG optical observations
DATE:    14/05/16 23:11:44 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P D'Avanzo, A. Melandri, M. G. Bernardini (INAF-OAB), M. Cecconi, G. Mainella (INAF/TNG) 
report on behalf of a larger collaboration:


We observed the field of the short GRB 140516A (Bernardini et al. GCN 16285)
using the DOLORES camera on the 3.6m TNG telescope sited in Canary Islands. 
We obtained four images with the r SDSS filter, each one lasting 180 s, at a mean
time of 1.55 hours after the burst.

In the co-added image we do not detect any optical afterglow inside the XRT 
error circle reported by Bernardini et al. (GCN 16285). The 3sigma limiting
magnitude is r = 23.0 (AB).


GRB_name: GRB140516A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16287
SUBJECT: GRB 140516A:  ISON-Kislovodsk optical observations
DATE:    14/05/16 23:52:01 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

V. Nevskiy (ISON), V. Linkov (ISON), A. Volnova (IKI),  I. Molotov (KIAM), 
A. Pozanenko (IKI),  report on  behalf of larger collaboration:

We observed the field of  GRB 140516A (Bernardini et al., GCN 16285) with 
ORI-40 (0.4-m f/3)  telescope of ISON-Kislovodsk observatory. Observations 
started on  May 16 (UT) 20:39:04 and continued up to (UT) 21:11:60.   We 
obtained  several unfiltered images  of 30 s and 100 s exposures. In a 
preliminary analysis we do not detect evident source within XRT error circle 
(Bernardini et al., GCN 16285) .  The upper limit of a combined image is 
20.5m and based on USNO-B1.0 (R2) nearby stars. 


GRB_name: GRB140516A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16288
SUBJECT: GRB 140516A: MASTER early optical observations
DATE:    14/05/17 01:13:41 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy, V. Lipunov, 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  GRB140516A 22 sec after notice 
time 44 sec after trigger time at 2014-05-16 20:31:39 UT in two 
polarizations. On our first (10s exposure) set we haven't found optical 
transient  within SWIFT error-box (Bernardini et. al GCN 16285). The 
5-sigma upper limit has been about 17.0 mag.
As we have a set of observations after that with exposures from 10 to 180 
seconds during several hours.  In table 1 some limits are provided.

Table 1
-------
T_start     Exptime   T-T_mead  T-T_start  T-T_stop  Filter  mlimit  Coadd
2014-05-16 20:31:39     10     49 sec     44 sec     54 sec   P|     17.0    1
2014-05-16 20:31:39     10     49 sec     44 sec     54 sec   P-     16.9    1
2014-05-16 20:31:39    780    466 sec     44 sec    889 sec   P|     19.6    13*
2014-05-16 20:31:39    780    466 sec     44 sec    889 sec   P|     19.3    13*
2014-05-16 20:45:54   3600   2914 sec    899 sec   4930 sec   P|     20.6    20
2014-05-16 20:45:54   3600   2914 sec    899 sec   4930 sec   P-     20.4    20
2014-05-16 20:45:54   7200   2914 sec    899 sec   4930 sec P| + P-  21.0    40**
---------------------------------------------------------------------------------
*  This is a set images with diffrent exposure times from 10 to 180 seconds.
** We has images synchronously in 2 channels. Therefore we can increase 
twice exptime in case of constant t_start and t_stop.

P- and P| is a polarization filter which are oriented at an angle 0 and 90 
degrees to RA axis respectivel. T is a  GRB trigger time.


The message may be cited.


GRB_name: GRB140516A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16289
SUBJECT: GRB 140516A: Enhanced Swift-XRT position
DATE:    14/05/17 01:35:11 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 461 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 140516A, 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 = 252.98931, +39.96284 which is equivalent
to:

RA (J2000): 16h 51m 57.43s
Dec (J2000): +39d 57' 46.2"

with an uncertainty of 2.4 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB140516A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16290
SUBJECT: GRB 140516A: NOT optical observations
DATE:    14/05/17 03:32:40 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

J. Gorosabel (IAA-CSIC, UPV-EHU), D. Xu (DARK/NBI), A. de Ugarte Postigo
(IAA-CSIC, DARK/NBI), J.P.U. Fynbo (DARK/NBI), P. Jakobsson (U. Iceland),
D. Malesani (DARK/NBI), N.R. Tanvir (U. Leicester), D. Watson (DARK/NBI),
E. Gafton (OKC, Stockholm Univ.) and T. Libbrecht (Stockholm Univ.), report
on behalf of a larger collaboration:

We imaged the field of GRB 140516A (Bernardini et al. GCNC 16285) with the
2.5m Nordic Optical telescope equipped with ALFOSC. The observations were
carried out in the R-band on May 16.89163-16.97005 UT (0.88-2.77 hours post
burst) with a total exposure time of 13x300s. We did not detect any objects
brighter than R=24.5 (3 sigma Vega limit calibrated against USNO B1.0)
consistent with the enhanced XRT position (Osborne et al. GCNC 16289).

[GCN OPS NOTE(17may14): Changed the Subject-line from 150416A to 140516A.]


GRB_name: GRB140516A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16291
SUBJECT: GRB 140516A: Swift-XRT refined Analysis
DATE:    14/05/17 08:45:02 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 11 ks of XRT data for GRB 140516A (Bernardini et al.
GCN Circ. 16285),  from 64 s to 25.6 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.
16289).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.38 (+0.14, -0.12).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.2 (+0.7, -0.4). The
best-fitting absorption column is  2 (+14, -0) x 10^20 cm^-2,
consistent with the Galactic value of 1.5 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 2.9 x 10^-11 (3.1 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2 (+14, -0) x 10^20 cm^-2
Galactic foreground: 1.5 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.2 (+0.7, -0.4)

If the light curve continues to decay with a power-law decay index of
0.38, the count rate at T+24 hours will be 1.6 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.7 x
10^-14 (5.0 x 10^-14) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00599188.

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


GRB_name: GRB140516A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16292
SUBJECT: GRB 140516A: Swift-BAT refined analysis
DATE:    14/05/17 08:58:49 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
M. G. Bernardini (INAF-OAB), 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 recent telemetry downlinks,
we report further analysis of BAT GRB 140516A (trigger #599188)
(Bernardini, et al., GCN Circ. 16285).  The BAT ground-calculated position is
RA, Dec = 252.972, 39.958 deg, which is 
   RA(J2000)  =  16h 51m 53.2s 
   Dec(J2000) = +39d 57' 28.5" 
with an uncertainty of 2.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 75%.
 
The mask-weighted light curve shows a single spike starting at ~T+0.0,
peaking at ~T+0.05, and ending at ~T+0.3 sec.  T90 (15-350 keV)
is 0.19 +- 0.09 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.01 to T+0.18 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.87 +- 0.33.  The fluence in the 15-150 keV band is 2.3 +- 0.6 x 10^-8 erg/cm2.
The 1-sec peak photon flux measured from T-0.38 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/599188/BA/


GRB_name: GRB140516A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16293
SUBJECT: GRB 140516A: Swift/UVOT Upper Limits
DATE:    14/05/17 12:23:23 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (UCL-MSSL) and Bernardini (INAF-OAB) report on
behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140516A
84 s after the BAT trigger (Bernardini et al., GCN Circ. 16285).
No optical afterglow consistent with the XRT enhanced position
(Osborne et al. GCN Circ. 16289) is detected in the initial UVOT
exposures. The Enhanced position overlaps with the PSF wings of
a star, and the light curve is consistent with a constant source.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

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

white_FC            84          234          147         >20.5
u_FC               298          547          246         >21.2
white               84        12686         1178         >20.6
v                  627         7762          607         >19.5
b                  553        12381         1294         >20.9
u                  298         8313          770         >21.0
w1                 676         8172          607         >21.6
m2                 651         7967          529         >21.0
w2                 602         7558          607         >21.1

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: GRB140516A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16294
SUBJECT: GRB 140516A: Gemini-North limit on an optical afterglow
DATE:    14/05/17 16:56:25 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

W. Fong and E. Berger (Harvard) report:

"We observed the location of the short-duration GRB 140516A (Bernardini et
al., GCN 16285) with the Gemini Multi-Object Spectrograph (GMOS) mounted on
the Gemini-North 8-meter telescope at a mid-time of 2014 May 17.373 UT
(12.38 hr post-burst). We obtained i-band observations for a total of
1800-sec in 0.5" seeing. We do not detect any optical source within the XRT
position (Osborne et al., GCN 16289). Calibrated to SDSS, we therefore
place a 3-sigma limit of i>26.1 AB mag on the optical afterglow of GRB
140516A at 12.38 hr after the burst.

We thank Gemini observer Lucas Fuhrman for assistance with these
observations."


GRB_name: GRB140516A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16295
SUBJECT: GRB 140516A: 6 GHz upper limit
DATE:    14/05/17 22:23:29 GMT
FROM:    Wen-fai Fong at CFA  <wfong@cfa.harvard.edu>

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

"We observed the field of the short-duration GRB 140516A (Bernardini et
al., GCN 16285) with the Karl G. Jansky Very Large Array (VLA) beginning on
2014 May 17.48 UT (14.94 hr post-burst) at a mean frequency of 6 GHz. In 1
hour of observations, we do not detect any radio source in or around the
enhanced XRT position (Osborne et al., GCN 16289). We therefore place a
3-sigma limit of 24 microJy on the radio afterglow of GRB 140516A at 14.94
hr after the burst.

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


GRB_name: GRB140516A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16296
SUBJECT: GRB 140516A: Subaru NIR imaging observations
DATE:    14/05/18 03:49:48 GMT
FROM:    Nobuyuki Kawai at Tokyo Tech  <nkawai@hp.phys.titech.ac.jp>

Y. Minowa, T.-S. Pyo, J.-H. Kim (Subaru, NAOJ)
and N. Kawai (Tokyo Tech) report on behalf of the Subaru GRB team:

We observed the field of the short GRB 140516A (Bernardini et al.,
GCN 16285) using IRCS+AO188 on the 8.2 m Subaru telescope, 
starting from 06:56 on May 17, 2014 UTC (about 10.4 hrs from the 
burst). We obtained the Kp-band images in 52 mas/pixel mode 
without AO correction for a total exposure time of 5880 sec under 
0".7 seeing condition. We do not detect any source within the 
error circle reported by Osborne et al. (GCN 16289). We obtained 
the 3-sigma limit on the near-infrared afterglow of GRB 140516A 
of Kp>22.2 mag (Vega) at 10.4-12.7 hrs after the burst.


GRB_name: GRB140516A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16297
SUBJECT: GRB 140516A: RATIR Optical and NIR Observations
DATE:    14/05/18 05:22:31 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB),
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara
(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 the short-duration GRB 140516A (Bernardini, et
al., GCN 16285) 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 2014/05
17.33 to 2014/05 17.46 UTC (11.41 to 14.56 hours after the BAT trigger),
obtaining a total of 2.13 hours exposure in the r and i bands and 0.89
hours exposure in the Z, Y, J, and H bands.

For a source within the Swift-XRT error circle (Osborne, et al., GCN
16289), in comparison with the SDSS DR9 and 2MASS, we obtain the following
upper limits (3-sigma):

  r     > 23.57
  i     > 23.39
  Z     > 21.70
  Y     > 21.52
  J     > 22.00
  H     > 21.48

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: GRB140518A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16298
SUBJECT: GRB 140518A: Swift detection of a burst
DATE:    14/05/18 09:43:46 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. Melandri (INAF-OAB), M. G. Bernardini (INAF-OAB),
P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), D. Malesani (DARK/NBI),
D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/PSU) and
M. H. Siegel (PSU) report on behalf of the Swift Team:

At 09:17:46 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140518A (trigger=599287).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 227.269, +42.416 which is 
   RA(J2000) = 15h 09m 05s
   Dec(J2000) = +42d 24' 56"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a multiple-peaked
structure with a  duration of about 60 s.  The peak count rate
was ~1500 counts/s (15-350 keV) at ~0 sec after trigger. 

The XRT began observing the field at 09:18:55.0 UT, 69 seconds
after the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source with an enhanced position: RA, Dec 227.2519,
42.4185 which is equivalent to:
   RA(J2000)  = 15h 09m 00.45s
   Dec(J2000) = +42d 25' 06.6"
with an uncertainty of 2.0 arcseconds (radius, 90% containment). This
position may be improved as more data are received; the latest position
is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (1.56 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 2.5
(+2.30/-2.03) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 3.67e-09 erg cm^-2 s^-1 (0.2-10
keV). 

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
0.02. 

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


GRB_name: GRB140518A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16299
SUBJECT: GRB 140518A: KAIT optical candidate
DATE:    14/05/18 10:17:13 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 GRB 140518A (Swift trigger 599287;
Melandri et al., GCN 16298) starting at 09:22:16 UT, 270 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 detect a faint object within XRT error
circle at J2000 coordinates of:

RA =  15:09:00.62
DEC= +42:25:05.9

with uncertainty of about 1". The object was only detected in the
first clear band single image with mag R~18.3, no detection in
following single images. But it is marginally detected in the co-add
of next 5 single images with mag R~19.0. We suggest this to be the
afterglow of the GRB. All mags are calibrated to USNO B1.0 catalog. 

[GCN OPS NOTE(18may14): Per author's request, the Subject-line was
corrected from "140418A" to "140518A".]


GRB_name: GRB140518A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16300
SUBJECT: GRB 140518A: P60 i-/z-band detections
DATE:    14/05/18 12:22:01 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

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

The Palomar 60-inch telescope responded automatically to the Swift 
trigger for GRB 140518A (Melandri et al., GCN 16298) and began a 
repeating cycle of 60-second exposures in r, i, and z-band observations 
at 09:22:28 UT, 4.70 minutes after the burst.

We weakly detect the afterglow reported by Zheng et al. (GCN 16299) in 
the i and z filters, but not in r-band.   Only marginal detections are 
evident in any individual exposure in any filter, but a stack of the 
first six exposures in each band gives magnitudes (calibrated relative 
to SDSS) of:

r > 20.31  (2 sigma)
i = 19.03 +/- 0.16
z = 18.20 +/- 0.17

at a mid-time of approximately 16 minutes after the burst.


GRB_name: GRB140518A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16301
SUBJECT: GRB 140518A: Gemini-N redshift
DATE:    14/05/18 14:01:58 GMT
FROM:    Ryan Chornock at Harvard  <rchornock@cfa.harvard.edu>

R. Chornock (Harvard), D. B. Fox (Penn State), A. Cucchiara (Goddard), D. A. 
Perley (Caltech), and A. Levan (Warwick) report on behalf of a larger collaboration:

We obtained 2x900s of spectroscopy of the optical afterglow (Zheng et al., GCN 
16299; Perley et al., GCN 16300) of GRB140518A (Melandri et al., GCN 16298) 
using GMOS on the 8-m Gemini-North telescope starting at 12:22 UT on May 18. Our 
spectra covered the wavelength range 5900-10150 Angstroms at a resolution of 
R~1200. A damped Lyman-alpha system is present near 6940 Angs, corresponding to 
z~4.71.  A fit to the absorber gives z=4.706 and the log of the HI column 
density (in cm^-2) is 21.65 +- 0.1. Strong narrow absorption lines of S II, Si 
II, Si II*, O I, O I*, Si IV, C II, C IV, Fe II, and Al II associated with this 
absorption system have a common redshift of z=4.707.  The combination of the DLA 
and the excited fine structure lines allow us to identify this as the redshift 
of the GRB.

We thank the Gemini staff, in particular Rachel Mason and Joy Chavez, for their 
assistance with these observations.


GRB_name: GRB140518A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16302
SUBJECT: GRB 140518A: RATIR Optical and NIR Observations
DATE:    14/05/18 14:24:59 GMT
FROM:    Antonino Cucchiara at NASA/GSFC  <antonino.cucchiara@nasa.gov>

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

We observed the field of GRB 140518A (Melandri, et al., GCN 16298) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional on
Sierra San Pedro Mrtir from 2014/05 18.41 to 2014/05 18.46 UTC (0.60
to 1.75 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.

We detect the fading source identified by Zheng et al. (GCN 16299) and 
Perley et al. (GCN 16300) within the Swift-XRT error circle.
We confirm this to be the optical afterglow of GRB 140518A.

In comparison with the SDSS DR9 and 2MASS, we
obtain the following detections:

  r 20.50 +/- 0.04
  i 19.00 +/- 0.02
  Z 18.59 +/- 0.03
  Y 18.19 +/- 0.03
  J 18.13 +/- 0.02
  H 17.80 +/- 0.02

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.
Based on these observations, and using our automatic photo-z
analysis tool (Littlejohns et al. arXiv:1312.3967) we determine two possible
photometric redshifts: assuming a Milky Way extinction curve for the GRB 
host we derive a photo-z of z=1.88 (+- 0.06) and A_V=1.8, while a SMC 
extinction law gives a z=4.63 (+- 0.11) and A_V=0.5. 
The second solution is consistent with the spectroscopic redshift
reported by Chornock et al. (GCN 16301).


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

[GCN OPS NOTE(19may14):  Per author's request, the "9.90 to 11.05"
was changed to "0.60 to 1.75".]


GRB_name: GRB140518A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16303
SUBJECT: GRB 140518A: Swift/UVOT Upper Limits
DATE:    14/05/18 17:18:01 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

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

The Swift/UVOT began settled observations of the field of
GRB 140518A  77 s after the BAT trigger (Melandri et al.,
GCN Circ. 16298).  No optical afterglow consistent with the
XRT position (Melandri et al. GCN Circ. 16298) 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            77          226          147         >20.7
u_FC               289          539          246         >20.7
white               77        13719         1583         >22.6
v                  619         7499          568         >20.2
b                  545        12953         1060         >22.0
u                  289        12041         1286         >21.6
w1                 668         7910          568         >21.4
m2                1071         7705          413         >21.1
w2                 595         7295          510         >21.3

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: GRB140518A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16304
SUBJECT: GRB 140518A: Skynet GORT Detections of the Optical Afterglow
DATE:    14/05/18 18:24:41 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, A. LaCluyze, J. Haislip, D. Reichart, K. McLin, L. Cominsky, 
H. T. Cromartie, A. Foster, N. Frank, K. Ivarsen, M. Maples, J. Moore, 
M. Nysewander, R. Beauchemin, T. Berger, A. Dow, M. Hinckle, A. 
Patterson, H. Pegues, J. Pozo, D. Waddell, and J. A. Crain report:

Skynet observed the Swift-XRT localization of GRB 140518A (Melandri et 
al., GCN 16298, Swift trigger 599287) with the 14" GLAST Optical Robotic 
Telescope (GORT) at the Hume observatory in CA, USA. Observations began 
at t=130s and continued until 2.4h post-trigger. Skynet took alternating 
exposures in the Rc and Ic bands, increasing from 10s to 160s. In early 
Ic and Rc images, and in later stacked Ic images, we detect an 
uncatalogued fading optical source at a position consistent with the 
afterglow candidate reported by Zheng et al. (GCN 16299).

The source faded from Ic=16.8 at t=130s to Ic > 18.7 at a mean time 
t~70m. In Rc band, we detect the source marginally at Rc~18.3 at t=4m, 
with Rc>20.1 at a mean time t~55m.

A preliminary light curve is at:
http://www.skynet.unc.edu/grb/grb140518a.png

Photometry is calibrated to six APASS-DR7 stars in the field, and has 
not been corrected for the Galactic foreground extinction corresponding 
to E(B-V)=0.016 (Schlegel et al. 1998).

No further Skynet observations are scheduled.


GRB_name: GRB140518A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16305
SUBJECT: GRB 140518A: Swift-XRT refined Analysis
DATE:    14/05/18 21:44:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 8.3 ks of XRT data for GRB 140518A (Melandri  et al.
GCN Circ. 16298),  from 58 s to 19.5 ks after the  BAT trigger. The
data comprise 92 s in Windowed Timing (WT) mode (the first 8 s were
taken while Swift was slewing) with the remainder in Photon Counting
(PC) mode. Using 4543 s of PC mode data and 6 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 = 227.25249, +42.41821
which is equivalent to:

RA (J2000): 15h 09m 00.60s
Dec(J2000): +42d 25' 05.6"

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

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=3.42 (+0.22, -0.19). At T+251 s  the decay
flattens to an alpha of 0.25 (+0.15, -0.18) before breaking again at
T+2747 s to a final decay with index alpha=1.51 (+0.32, -0.27).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.66 (+/-0.10). The
best-fitting absorption column is  2.5 (+1.7, -1.6) x 10^22 cm^-2, at a
redshift of 4.707, in addition to the Galactic value of 1.6 x 10^20
cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index
of 1.94 (+/-0.12) and a best-fitting absorption column of 2.9 (+1.7,
-1.6) x 10^22 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV
flux conversion factor deduced from this spectrum  is 3.4 x 10^-11 (3.8
x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 1.6 x 10^20 cm^-2
Intrinsic column:    2.9 (+1.7, -1.6) x 10^22 cm^-2 at z=4.707
Photon index:      1.94 (+/-0.12)

If the light curve continues to decay with a power-law decay index of
1.51, the count rate at T+24 hours will be 2.0 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.9 x
10^-14 (7.8 x 10^-14) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00599287.

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


GRB_name: GRB140518A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16306
SUBJECT: GRB 140518A, Swift-BAT refined analysis
DATE:    14/05/19 00:27:52 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

T. N. Ukwatta (MSU), 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), A. Melandri (INAF-OAB),
D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU),
J. Tueller (GSFC) (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 140518A (trigger #599287)
(Melandri, et al., GCN Circ. 16298).  The BAT ground-calculated position is
RA, Dec = 227.231, 42.396 deg which is
  RA(J2000)  =  15h 08m 55.3s
  Dec(J2000) = +42d 23' 44.2"
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 89%.

The mask-weighted light curve shows multiple peaks with roughly three main pulse
structures. The first main pulse starts at ~T-4 s and ends at ~T+8 s. The second main
pulse starts at ~T+38 s, followed immediately by the third main pulse structure that
starts at ~T+48 s and ends at ~T+61 s. Additionally, each of these main pulse structure
contains several  sub-pulses. T90 (15-350 keV) is 60.5 +- 2.4 sec (estimated error
including systematics).

The time-averaged spectrum from T-4.1 to T+60.0 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 0.92 +- 0.61,
and Epeak of 43.9 +- 7.6 keV (chi squared 54.15 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 1.0 +- 0.1 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+41.94 sec in the 15-150 keV band is
1.0 +- 0.1 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.97 +- 0.13 (chi squared 65.02 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/599287/BA/


GRB_name: GRB140512A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16307
SUBJECT: GRB 140512A: MASTER prompt and afterglow optical observations
DATE:    14/05/19 05:47:51 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

E. Gorbovskoy, V. Lipunov, 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  Tunka  began observations of   GRB140512A  (Pagani et. al. GCN 
16249) from  pointing  on several FERMI alerts.
During the second set of observations by FERMI coordinates the GRB140512A 
error box was covered by our  very wide field cameras MASTER VWF 
(FOV=2x384 square degrees, D=72mm, f/1.2, 1 pix = 22 arcsec) which 
installed on  MASTER-II telescope. So we have 5 images with 5 second 
exptime without time gap since 2014-05-12 19:32:38 i.e. 29 sec. after the 
trigger and 49 sec. after the burst. We did not see optical transient 
(Pagani et. al. GCN 16249)  at GRB140512A place. The  5-sigma upper limit 
on coadd of 5 MASTER-VWF images since 49 sec. till 74 sec. after the burst 
has been about 12.3 mag. The prompt images available here 
http://master.sai.msu.ru/static/GRB/GRB140512A.png .

After several repointing by FERMI alerts MASTER II was pointed to the 
GRB140512A 171 sec after trigger time at 2014-05-12 19:34:40.212 UT in two 
polarizations by Swift coordinates. We definitely see OT on our images in 
both polarizations.

Out final light curve  is  available in Tab. 1

        Start time       Exptime T-T_mid     P/      eP/      P\    eP\
2014-05-12T19:34:40.212     30     186    14,45    0,04    14,37  0,03
2014-05-12T19:36:37.643     60     318    14,72    0,05    14,74  0,04
2014-05-12T19:38:24.484     60     425    15,60    0,12    15,35  0,06
2014-05-12T19:39:47.447     60     508    15,41    0,10    15,65  0,07
2014-05-12T19:41:10.651     60     591    15,75    0,13    15,75  0,08
2014-05-12T19:42:32.663     60     673    15,98    0,16    15,94  0,09
2014-05-12T19:43:54.083     60     754    16,46    0,22    16,42  0,12
2014-05-12T19:45:56.002    170     931    16,37    0,20    16,79  0,15
2014-05-12T19:50:30.564    180    1211    17,50    0,39    16,84  0,15
2014-05-12T19:56:11.667    180    1552    16,82    0,27    17,57  0,22

P/ and P\ is a polarization filter which are oriented at an angle 45 and 
135 degrees to RA axis respectivel.  eP/ and eP\ is a error of P/ and P\ 
values.  T is a  GRB trigger time.

The dimensionless Stokes parameter averaged over 5 first expositions is 
estimated to be less than observational error which equals to 2.9% (i.e. q 
= 0.3 +- 2.9%). So big error is connected to observation in a morning 
twilight (sun altitude ~ 12 d) and high object zenith distance (z ~ 70 d).

Our  unfiltered magnitude is well described by a parity 0.8R + 0.2B  (USNO-B1)

The message may be cited.


GRB_name: GRB140518A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16308
SUBJECT: GRB 140518A: Continued RATIR Optical and NIR Observations
DATE:    14/05/19 15:01:09 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 140518A (Melandri, et al., GCN 16298) 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 2014/05 19.24 to 2014/05 19.46 UTC (20.37 to
25.71 hours after the BAT trigger), obtaining a total of 2.47 hours
exposure in the r and i bands and 2.06 hours exposure in the Z an J bands.

For a source at the optical transient position (Zheng et al., GCN 16299),
in comparison with the SDSS DR9 and 2MASS, we obtain the following upper
limits (3-sigma):

  r  > 22.03
  i  > 22.20
  Z  > 21.28
  J  > 21.07

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.  Compared to our observations last
night (Cucchiara, et al., GCN 16302), during which the source faded
approximately as t^(-0.5), the source has now apparently faded more rapidly
as t^(-1) or faster.

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


GRB_name: GRB140518A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16309
SUBJECT: GRB 140518A: T100 observations
DATE:    14/05/19 16:13:14 GMT
FROM:    Eda Sonbas at NASA/GSFC  <edasonbas@gmail.com>

E. Sonbas (Adiyaman Univ.), T. Guver (Istanbul Univ.), U. Temiz, F.Dolek
(Cukurova Univ.), E. Gogus (Sabanci Univ.), O. Erece (Akdeniz Univ.), O.
Basturk (Ankara Univ.) report on behalf of a larger collaboration


 We observed the field of Swift GRB 140518A (Melandri et al., GCN#16298)
with the 1.0 meter T100 telescope (Bakirlitepe, TUBITAK National
Observatory, Turkey), starting May, 18, 21:35:41 UT (~ 12.3 hours after the
trigger). 5 x 300 s exposures were obtained in the R filter under moderate
weather conditions.


We do not detect an optical afterglow within the reported XRT error circle
down to a limiting magnitude of >20.37 (2-sigma) in the combined R band
image.


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


GRB_name: GRB140512A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16310
SUBJECT: GRB 140512A: Redshift from NOT
DATE:    14/05/19 21:17:34 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),
D. Xu (DARK/NBI), D. Malesani (DARK/NBI), G. Leloudas (DARK/NBI),P.
Jakobsson (U. Iceland), T. Kruehler (ESO), A.A. Djupvik (NOT), E. Gafton
(OKC, Stockholm Univ.) and T. Libbrecht (Stockholm Univ.) report on behalf
of a larger collaboration:


Following the photometric observations of the counterpart of GRB 140512A
(Pagani et al. GCN 16249) from the 2.5 m NOT (+ALFOSC) reported by de
Ugarte Postigo et al. (GCN 16253) we obtained spectroscopic data.
Observations consisted in 2x1800s exposures using Grism #4, which covers
the range from 3800 to 9100. The mean observing epoch was May 13, 3:18:50
UT (7.78 hrs after the burst).


The spectrum presents absorption features consistent with FeII and MgII at
a common redshift of z=0.725, which we consider the most probable redshift
for this event.


GRB_name: GRB140521A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16311
SUBJECT: GRB 140521A: Swift detection of a burst
DATE:    14/05/21 17:51:56 GMT
FROM:    Eleonora Troja at GSFC  <eleonora.troja@nasa.gov>

E. Troja (NASA/GSFC/UMCP), S. B. Cenko (GSFC),
J. R. Cummings (NASA/UMBC), V. D'Elia (ASDC), L. M. Z. Hagen (PSU),
L. Izzo (URoma/ICRA), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), V. Mangano (PSU),
A. Melandri (INAF-OAB), P. T. O'Brien (U Leicester),
K. L. Page (U Leicester), B. Sbarufatti (INAF-OAB/PSU),
M. H. Siegel (PSU) and T. N. Ukwatta (MSU) report on behalf of the
Swift Team:

At 17:34:18 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140521A (trigger=599546).  Swift did not slew to the burst
due to an observing constraint.   The BAT on-board calculated location 
is RA, Dec 320.013, +67.602 which is 
   RA(J2000) = 21h 20m 03s
   Dec(J2000) = +67d 36' 06"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 12 sec.  The peak count rate
was ~3000 counts/sec (15-350 keV), at ~0.1 sec after the trigger. 

Due to an observing constraint, Swift will not 
slew until 00:39UT on May 22. There will be no XRT or UVOT 
data until this time. 

Burst Advocate for this burst is E. Troja (eleonora.troja 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: GRB140521A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16312
SUBJECT: GRB 140521A: MASTER  optical observations 
DATE:    14/05/21 22:28:09 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

V. Vladimirov, P.Balanutsa, E. Gorbovskoy, V. Lipunov, V.Kornilov, 
D.Kuvshinov, A.Belinski, N.Tyurina,
N.Shatskiy,  D.Zimnukhov, A.Kuznetsov, V.V.Chazov, D.Denisenko, 
A.Sankovich, A. Krylov, M.Pruzhinskaya
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  Vostryakovo (Alexander Krylov Observatory) was pointed to the 
GRB140521A 4553 sec after trigger time at 2014-05-21 18:50:11 directly 
after sunset.  We haven't found optical transient  within SWIFT error-box 
(Troja et. al GCN 16311) on single and coadd images.
In table 1 the images upper limits are provided.

Table 1.
-------
T_start       Exptime   T-T_mead  T-T_start  T-T_stop  Filter  mlimit  Coadd
2014-05-21 18:50:11     15       4561       4553      4568     C      14.5     1*
2014-05-21 19:10:18    600       6531       5760      7302     C      18.0     10
2014-05-21 19:10:18   1020       7210       5760      8659     C      18.8     17
2014-05-21 19:38:52    600       8067       7474      8659     C      18.7     10
2014-05-21 20:07:53   1200      10390       9215     11566     C      19.4     20
-----------------------------------------------------------------------------------
* First image with stars on bright evening sky.
C is  our white (clear) band which is well described by a parity 0.8R+0.2B (USNO B1).
T is a  GRB trigger time.


Another  two  MASTER II  robotic telescope  located in Kislovodsk and  Blagoveschensk
was pointed to the  GRB140521A 21 sec after notice time and 36 sec after 
trigger time at 2014-05-21 17:34:54 UT. But observations were spoiled due 
to bad weather condition.  We have a set of images from that observatories 
with different exposures from 10 to 180 and formal upper limit from 13 to 
16 during first hour after the burst. However bad quality of images (due 
to wind and clouds) don't allow to carry out transient search.

The message may be cited.


GRB_name: GRB140516A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16313
SUBJECT: GRB 140516A: further Swift-XRT analysis
DATE:    14/05/21 23:42:20 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

M. G. Bernardini, P. D'Avanzo, A. Melandri, S. Campana (INAF-OAB), P. A. Evans, K. L. Page (U. Leicester), 
E. Troja (NASA/GSFC/UMCP) report on behalf of the Swift-XRT team:


We have analysed 24.4 ks of XRT data for GRB 140516A (Bernardini et al. GCN Circ. 16285),  
from 92 s to 397.8 ks after the  BAT trigger, in Photon Counting (PC) mode. 

The X-ray counterpart reported by Bernardini et al. (GCN Circ. 16285) and Gompertz 
et al. (GCN Circ. 16291) apparently disappeared in the data collected from t-t0=92.8 ks onwards. 
However, in the same dataset we find evidence for the presence of an unrelated source at 
the position RA, Dec = 252.99269, +39.95659 which is equivalent to:

RA (J2000): 16h 51m 58.25s
Dec (J2000): +39d 57' 23.7"

with an uncertainty of 4.0 arcsec (radius, 90% confidence).

This position is 24" away from the enhanced position for this burst reported by
Osborne et al. (GCN Circ. 16289) while it is consistent with the source
165158.53+395728.9 reported in the Krawczyk et al. (2013; ApJS, 206, 4) QSO
catalogue. 
We therefore caution that this field source is likely contaminating the automated late-time 
X-ray light curve of GRB 140516A, given the spatial proximity to its transient 
X-ray counterpart.

[GCN OPS NOTE(22may14): Per author's request, the word "automated" was added 
to the last sentence.]


GRB_name: GRB140521A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16314
SUBJECT: GRB 140521A: MITSuME Okayama upper limits
DATE:    14/05/22 07:20:25 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 140521A (Troja et al., GCNC 16311)
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 2014-05-21 17:35:25 (~68 sec after the burst).
We did not find any new point source within the BAT circle
(Troja et al., GCNC 16311) 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
-----------------------------------------------------
0.02943    18:16:40    4320.0   >19.5  >19.3  >18.5
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB140521A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16315
SUBJECT: GRB 140521A: AROMA-N Optical Observation
DATE:    14/05/22 10:31:49 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

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

We observed the field of GRB 140521A detected by Swift (trigger #599546; 
Troja et al., GCN Circ. 16311) with the 12-inch AGU Robotic Optical 
Monitor for Astrophysical object - Narrow (AROMA-N) located at the Sagamihara 
campus of Aoyama Gakuin University.  

15 images of 60 sec exposures were taken in the R filter starting from 
May 21 17:36:17 (UT) about 119 sec after the trigger 
(104 sec after the BAT position notice) and stopped on May 21 18:03:04 (UT).  
We do not detect the optical afterglow both in the individual images and 
the stacked image inside the BAT flight position (Troja, et al., GCN #16311).  
The estimated five sigma upper limit of the combined image (total exposure of  900 sec) 
is ~17.2 mag using the USNO-B1 catalog.


GRB_name: GRB140521A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16316
SUBJECT: GRB 140521A: Swift-BAT refined analysis
DATE:    14/05/22 13:27:00 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), T. Sakamoto (AGU),
M. Stamatikos (OSU), E. Troja (NASA/GSFC/UMCP), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 140521A (trigger #599546)
(Troja, et al., GCN Circ. 16311).  The BAT ground-calculated position is
RA, Dec = 320.177, 67.587 deg, which is 
   RA(J2000)  =  21h 20m 42.6s 
   Dec(J2000) = +67d 35' 12.7" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 55%.
 
The mask-weighted light curve shows a single peak starting at ~T-2 sec,
peaking at ~T+1 sec, and ending at ~T+11 sec with a tail out to ~T+50 sec.
T90 (15-350 keV) is 9.88 +- 1.09 sec (estimated error including systematics).
 
The time-averaged spectrum from T+0.15 to T+11.44 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.42 +- 0.11.  The fluence in the 15-150 keV band is 9.5 +- 0.6 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.64 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/599546/BA/


GRB_name: GRB140521A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16317
SUBJECT: GRB 140521A: AAO optical observations
DATE:    14/05/22 13:59:41 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 140521A(Troja et al., GCN 16311) 
with AS-32 (0.7m) telescope of Abastumani Observatory starting on May, 
21 (UT) 18:12:00. We obtained several unfiltered  frames with exposure 
of 120 s. Within the BAT ground-calculated position (Barthelmy et al., 
GCN 16316) we do not detect evident variable source. Since our stacked 
image is somewhat deeper than USNO-B1.0 we need one more epoch of 
observation.

The details of the photometry are the following:

UT start             t-T0         Filter   Exp.    Uplim
                     (mid, days)   (s)              (3 sigma)
2014-05-21 18:12:00  0.05746      None    28*120   21.2

and based on USNO-B1.0 star 1575-0248114  (21:20:10.32 +67:35:37.5) 
assuming R=15.70.


GRB_name: GRB140423A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16318
SUBJECT: GRB 140423A: TShAO optical observations
DATE:    14/05/22 16:23:31 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the optical afterglow (Elenin et al., GCN 16143; Kaur et 
al., GCN 16144; Ferrante et al., GCN 16145; Chester et al., GCN 16147;
Maehara et al., GCN 16151) of the Swift GRB 140423A (Sonbas et al.,
GCN 16142) with Zeiss-1000 (East) 1m telescope of Tien Shan Astronomical 
Observatory on Apr., 23 and Apr., 24. We took several images in R-filter 
of 300 and 540 s  exposures in three epochs.

Details of the photometry are following:

date        UT start   t-T0       Filter  Exp.  OT
                       (mid, days)          (s)
2014-04-23 R 15:04:19  0.291036   R     8*300  20.47 0.14
2014-04-23 R 19:04:44  0.450758   R     6*300  20.70 0.20
2014-04-24 R 15:20:01  1.322830   R    12*540  22.17 0.10

The photometry is based on  SDSS stars, R (gri -> R transformations by 
Lupton 2005):

SDSS id                      R
J130914.51+494636.5   18.661+/-0.019
J130911.04+494854.6   20.209+/-0.053
J130924.79+494946.6   19.533+/-0.038

The light curve of the afterglow based on our previous an later 
observations (GCNs  16143, 16148, 16168, 16247, 16264) can be found in
http://grb.rssi.ru/GRB140423A/grb140423a-lc.png


GRB_name: GRB140521A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16319
SUBJECT: GRB 140521A: Fermi GBM Detection
DATE:    14/05/22 19:18:56 GMT
FROM:    Matthew Stanbro at UAH/Fermi  <mcs0001@uah.edu>

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

"At 17:34:18.73 UT on 21 May 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140521A (trigger 422386461 / 140521732)
which was also detected by Swift (E. Troja et al. 2014, GCN 16311).
The GBM on-ground location, using the Fermi GBM trigger data,
is consistent with the Swift/BAT location.

The GBM light curve consists of one main episode with a total
duration (T90) of about 11.5 s (50-300keV). The time-averaged
spectrum from T0-0.864 s to T0+10.400 s is well fit
by a power law function with an exponential high-energy cutoff.
The power law index is -1.04 +/- 0.08 and the cutoff energy,
parameterized as Epeak, is 273 +/- 44 keV.


The event fluence (10-1000 keV) in this time interval is
(2.99 +/- 0.21)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0-0.10 s in the 10-1000 keV band is 3.9 +/- 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: GRB140521A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16320
SUBJECT: GRB 140521A : Xinglong TNT upper limit
DATE:    14/05/23 07:50:38 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

L. P. Xin,   X. F. Wang,  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 140521A (Troja et al., GCN 16311)  
with Xinglong  0.8-m TNT telescope at 15:35:50 (UT) , 
92 sec after the burst.

No any optical transient was detected in our single or stacked image.
The 3-sigma upper limit magnitude is about 18.4 mag at the mean time of
7.3 min , calibrated by nearby USNO B1.0 R2 mag.

The message may be cited.


GRB_name: GRB140523A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16321
SUBJECT: GRB 140523A: Fermi GBM detection
DATE:    14/05/23 15:02:50 GMT
FROM:    Andreas von Kienlin at MPE  <azk@mpe.mpg.de>

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

"At 03:05:57.62 UT on 23 May 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140523A (trigger 422507160 / 140523129).

The on-ground calculated location, using the GBM trigger
data, is RA = 128.7, DEC = 26.9 (J2000 degrees,
equivalent to 08 h 35 m, 26 d 54 '), 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 60 degrees.

The GBM light curve consists of multiple peaks 
with a duration (T90) of about 20 s (50-300 keV).
The time-averaged spectrum from T0+0.003 s to T0+22.720 s is
well fit by a Band function with Epeak = 270.7 (+8.1/-8.6) keV,
alpha = -1.05 +/- 0.01 , and beta = -2.73 (+0.14/-0.19).

The event fluence (10-1000 keV) in this time interval is
(5.13 +/- 0.04)E-05 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+7.232 s in the 10-1000 keV band
is 37.7 +/- 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: GRB140523A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16322
SUBJECT: GRB 140523A: Fermi-LAT detection
DATE:    14/05/23 18:39:14 GMT
FROM:    Giacomo Vianello at SLAC  <giacomov@slac.stanford.edu>

G. Vianello (Stanford University), J. Racusin (NASA/GSFC), M. Arimoto
(Tokyio Tech)

report on behalf of the Fermi-LAT team:

At UT 03:05:57.62  on May 23, 2014, Fermi-LAT detected high-energy
emission from GRB 140523A, which was also detected by Fermi-GBM
(trigger 422507160 / 140523129, von Kienlin et al., GCN 16321).

The best LAT on-ground location is found to be

(RA, Dec) = 133.3, 24.95 (deg, J2000)

with an approximate error radius of 0.4 deg (90% containment,
statistical error only).

This was 60 deg from the LAT boresight at the time of the trigger. At
this large off-axis angle, the LAT PSF is not symmetric, therefore the
error region is elongated on the direction pointing towards the center
of the instrument.

An image with the 68% and 90% containment regions have been posted at:

http://www-glast.stanford.edu/Software/GRB140523A_localization.jpg

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 20 photons above 100 MeV and 6 photons above 1 GeV are
observed within 300 seconds. After that the GRB went out of the LAT
FoV. It entered again around 4500 s after the trigger, but no further
emission is detected at that point. The highest-energy photon is a 6.5
GeV event which is observed 43 seconds 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: GRB140523A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16323
SUBJECT: GRB 140523A Tiled Swift observations
DATE:    14/05/23 18:43:43 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/GBM GRB 140523A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00026

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/GBM 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: GRB140523A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16324
SUBJECT: GRB 140523A: possible X-ray afterglow candidate from tiled Swift/XRT observations
DATE:    14/05/24 07:51:23 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

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

Swift began a series of observations, tiled on the sky, of the  
Fermi/GBM and /LAT GRB 140523A (von Kienlin et al. GCN 16321, Vianello  
et al. GCB 16322).

Observations cover four contiguous fields, starting on May 23 at 18:34  
UT, i.e., 15.5 h after the GBM detection. Each field was observed for  
about 2 ks.

A possible XRT candidate counterpart for the GBM/LAT source is  
detected at Ra, Dec 133.111250, +24.957111, which is equivalent to:

Ra(J2000)   =    08h 52m 26.7s
Dec(J2000) =  +24d 57' 25.6"

with an uncertainty of 6.4" (S/N~3). This location is 10.3 arcmins  
from the LAT position, within the LAT error box.

No statement about fading can be made at this stage.

We note the presence of a SDSS galaxy (r=22.27) a few arcsec SW to the  
center of the XRT detection, consistent with the X-ray position.


GRB_name: GRB140524A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16325
SUBJECT: Swift trigger 599860 probably not real
DATE:    14/05/24 14:03:58 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

S. D. Barthelmy (GSFC), V. D'Elia (ASDC), N. Gehrels (NASA/GSFC),
L. Izzo (URoma/ICRA), A. Y. Lien (NASA/GSFC/ORAU),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester) and
M. H. Siegel (PSU) report on behalf of the Swift Team:

At 13:25:47 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140524A (trigger=599860).  Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 53.405, -36.096 which is
   RA(J2000) = 03h 33m 37s
   Dec(J2000) = -36d 05' 46"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty).  This is a low-threshold trigger due to its position
matching a nearby galaxy in the on-board catalog. As is usual with an image
trigger, the available BAT light curve shows no significant structure.

The XRT began observing the field at 13:28:12.0 UT, 144.2 seconds after
the BAT trigger. Using promptly downlinked data we find an X-ray source
with an enhanced position: RA, Dec 53.4016, -36.1396 which is
equivalent to:
   RA(J2000)  = 03h 33m 36.39s
   Dec(J2000) = -36d 08' 22.5"
with an uncertainty of 2.6 arcseconds (radius, 90% containment). This
location is 157 arcseconds from the BAT onboard position, within the
BAT error circle; and in the nearby AGN NGC1365 in the BAT catalogue. The
XRT position may be improved as more data are received; the latest position is
available at http://www.swift.ac.uk/sper. This position is 3.0 arcseconds from
that of a known X-ray source: 3XMM J033336.4-360825 in the XMM-NEWTON XMMSSC
catalogue which we assume is the AGN X-ray emission from the galaxy.

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 1.39
x 10^20 cm^-2 (Willingale et al. 2013).

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 148 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 25% of
the BAT error circle. The typical 3-sigma upper limit has been about 19.6 mag.
The 8'x8' region for the list of sources generated on-board covers 100% of the
BAT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.02.


GRB_name: GRB140523A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16326
SUBJECT: GRB 140523A: Nanshan optical upper limit
DATE:    14/05/24 15:43:48 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), C.-H. Bai, J. Xu, A. Esamdin, L. Ma (XAO) report:

We observed the field of the possible XRT afterglow (D'Elia et al.,
GCN 16324) of GRB 140523A (von Kienlin et al., GCN 16321; Vianello et
al., GCN 16322) using the 1m telescope located at Nanshan, Xinjiang,
China. Observations started at 15:06:12 UT on 2014-05-24 (i.e., 36.0
hr after the burst), and 2x180s and 2x600s R-band frames were
obtained.

No optical source is detected at the XRT position down to a limiting
magnitude of R=20.5, calibrated with the SDSS field.


GRB_name: GRB140523A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16327
SUBJECT: IPN Triangulation of GRB 140523A
DATE:    14/05/24 15:50:16 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,

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

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

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

The long-duration, bright GRB 140523A (von Kienlin and Connaughton, GCN 
Circ. 16321) has been observed by Fermi (GBM), Konus-Wind, INTEGRAL 
(SPI-ACS), Swift (BAT) and MESSENGER (GRNS), so far, at about 11157 s UT 
(03:05:57). 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
------------------------------------------------
Corners:
1: 133.480 (08h 53m 55s) +25.815 (+25d 48' 56")
2: 133.425 (08h 53m 42s) +25.820 (+25d 49' 11")
3: 132.929 (08h 51m 43s) +24.467 (+24d 28' 02")
4: 132.267 (08h 49m 04s) +21.927 (+21d 55' 36")
5: 132.459 (08h 49m 50s) +21.913 (+21d 54' 46")
6: 132.669 (08h 50m 41s) +22.509 (+22d 30' 32")
-----------------------------------------------
The error box area is ~0.7 sq.deg, and its maximum dimension is 4.0 deg 
(the minimum one is 12 arcmin).

This box can be improved.

The box partially overlaps the LAT error circle (Vianello, Racusin, and 
Arimoto, GCN Circ. 16322).

The possible X-ray afterglow candidate (D'Elia and Izzo, GCN Circ. 
16324) is marginally consistent with the box.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB140523_T11157/IPN/

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


GRB_name: GRB140523A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16328
SUBJECT: Konus-Wind observation of GRB 140523A
DATE:    14/05/24 15:57:50 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, intense GRB 140523A
(Fermi-GBM detection: Stanbro, GCN 16319;
Fermi-LAT detection: von Kienlin and Connaughton, GCN 16321;
IPN triangulation: Golenetskii et al., GCN 16327)
triggered Konus-Wind at T0=11157.811 s UT (03:05:57.811).

The light curve shows a multi-peaked structure with total duration
of ~22 s. The emission is seen up to ~7 MeV.

As observed by Konus-Wind, the burst had a fluence
of 5.5(-0.4,+0.4)x10^-5 erg/cm2, and a 64-ms peak flux,
measured from T0+0.640 s, of 1.6(-0.1,+0.1)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+27.648 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.22 (-0.09,+0.10),
the high energy photon index beta = -2.7 (-0.4,+0.2),
the peak energy Ep = 212 (-17,+18) keV,
chi2 = 118/97 dof.

The spectrum near the peak count rate (measured from T0 to T0+4.864 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.58 (-0.14,+0.16),
the high energy photon index beta = -2.7 (-0.4,+0.2),
the peak energy Ep = 287 (-26,+29) keV,
chi2 = 100/97 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140523_T11157/

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


GRB_name: GRB140523A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16329
SUBJECT: GRB 140523A: NOT observation
DATE:    14/05/25 12:03:59 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Malesani (DARK/NBI), D. Xu (DARK/NBI), A. Somero (NOT), A. de Ugarte 
Postigo (IAA/CSIC and DARK/NBI), Z. Cano (Univ. Iceland), and P. 
Jakobsson (Univ. Iceland), report on behalf of a larger collaboration:

We observed the field of the Fermi GRB 140523A (von Kienlin & 
Connaughton, GCN 16321; Vianello et al., GCN 16322; Golenetskii et al., 
GCN 16327) with the NOT equipped with the AlFOSC camera. Observations 
were started on 2014 May 24 at 21:23 UT (1.76 days after the GRB), using 
an SDSS r filter. Exposure time was 20 or 30 min, depending on the 
pointing. We targeted the XRT sources reported by Evans (GCN 16323; see 
also D'Elia & Izzo, GCN 16324):

http://www.swift.ac.uk/xrt_products/TILED_GRB00026/

XRT source #3 is spatially coincident with the bright star BD+25 2008 
and is likely unrelated to the GRB. XRT source #1 is inconsistent with 
the IPN triangulation annulus (Golenetskii et al., GCN 16327).

Within or close to the positions of XRT sources #1, 2, 4, and 5, several 
objects are visible in our images. Some of them may be responsible for 
the X-ray emission.

A pointlike object consistent with XRT source #3 (at RA = 08:52:25.38, 
Dec = +24:57:27.3) is found to be brighter by about 0.5 mag in the NOT 
image compared to its archival SDSS magnitude r = 19.50 +- 0.02 (AB). 
Given the bright historical counterpart and lack of spatial extension, 
this is unlikely to be related to the GRB.

None of the other objects have significantly varied compared to their 
catalog values. Within the position of XRT source #5, an extended object 
(possibly an interacting galaxy, or a blend of sources) is apparent. 
Consistent with XRT source #2, an extra, dim object is visible (r ~ 24), 
fainter than the SDSS limit. A bright pointlike source (r = 19.8) is 
consistent with the position of XRT source #1.

Our data do not reveal any obvious candidate optical afterglow for this 
GRB. We encourage further Swift/XRT follow-up in order to ascertain 
whether any of the X-ray sources is variable. Our analysis suggests that 
XRT sources #3 and #4 are not related to the GRB, as also indicated in 
the web page by Evans (GCN 16323). Sources #2 and #5 remain viable 
afterglow candidates.


GRB_name: GRB140515A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16338
SUBJECT: Chandra late-time observations of GRB140515A
DATE:    14/05/28 19:03:45 GMT
FROM:    Raffaella Margutti at Harvard  <rmargutti@cfa.harvard.edu>

R. Margutti, E. Berger, R. Chornock, W. Fong, T. Laskar and A. Zauderer
(Harvard U.) report:

"We observed the location of GRB 140515A (D'Avanzo et al., GCN 16267)
at z=6.32 (Chornock et al., GCN 16269)
with the Chandra X-ray Observatory (Program 15508477, PI Margutti).
Our observations started on May 25th, 07:38:38 UT,  858.6 ks after the BAT
trigger.
No X-ray source is detected at the position of the optical and radio
afterglow
(Fong et al., GCN 16274, Laskar et al., GCN 16283),
with a 3-sigma count-rate limit of 1.5E-4 c/s (0.3-10 keV energy range,
total exposure time of 19.8 ks).

Adopting the best fitting parameters from the total PC-mode spectrum
(photon index Gamma=1.8, intrinsic neutral hydrogen column density
NHint=2.3E+22 cm-2 at z=6.32), we compute an observed flux limit of
1.5E-15 erg/s/cm2 (0.3-10 keV).  The Galactic hydrogen column density
in the direction of the burst is NHgal=2.5E+20 cm-2 (Kalberla et al.,
2005).
Our observations constrain the late-time (t> 100 ks) X-ray afterglow decay
to be steeper than t^-2.6.

We thank Belinda Wilkes and the entire Chandra team for making these
observations possible."


GRB_name: GRB140528A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16339
SUBJECT: IPN Triangulation of GRB 140528A
DATE:    14/05/29 16:23:35 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 and J. Goldsten, on behalf of the MESSENGER NS GRB 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 140528A has been observed by Fermi (GBM: trigger 
423000325), Konus-Wind, INTEGRAL (SPI-ACS), and MESSENGER (GRNS), so 
far, at about 72323 s UT (20:05:23).

We have triangulated it to a preliminary, 3 sigma error box whose 
coordinates are:
   ---------------------------------------------
    RA(2000), deg                 Dec(2000), deg
   ---------------------------------------------
   Center:
    280.731 (18h 42m 55s) -59.080 (-59d 04' 47")
   Corners:
    281.417 (18h 45m 40s) -58.757 (-58d 45' 25")
    281.160 (18h 44m 38s) -59.219 (-59d 13' 09")
    280.032 (18h 40m 08s) -59.394 (-59d 23' 38")
    280.306 (18h 41m 13s) -58.938 (-58d 56' 16")
   ---------------------------------------------
The error box area is 864 sq. arcmin, and its maximum dimension is 57 
arcmin (the minimum one is 24 arcmin).

The center of the GBM ground position (given in 
glg_tcat_all_bn140528837_v01.fit) is 1.29 deg from the center of the box.

This box may be improved.

A triangulation map is posted at 
http://www.ioffe.ru/LEA/GRBs/GRB140528_T72325/IPN/

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


GRB_name: GRB140529A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16340
SUBJECT: GRB 140529A found in ground analysis of BAT slew data
DATE:    14/05/30 01:27:44 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

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

At 09:28:06 the IPN detected GRB 140529A.  Swift was slewing at this time.  A
mosaic of images from BAT event data shows a very strong detection at
RA, Dec 228.816, -41.044, which is

RA (J2000)   15h 15m 15.8s  
Dec (J2000) -41d 02' 39"

with an estimated 90% uncertainty radius of 1.5 arcmin.

The burst consisted of a single FRED peak about 5 seconds long.  The maximum
count rate in BAT was about 5000 counts/sec.

A Swift TOO has been requested.


GRB_name: GRB140408A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16341
SUBJECT: GRB 140408A: Withdrawal of afterglow candidate
DATE:    14/05/30 06:57:16 GMT
FROM:    Fabian Knust at MPE/GROND  <fabian.knust@hotmail.de>

GRB 140408A: Withdrawal of afterglow candidate

F. Knust, K. Varela, C. Delvaux (all MPE Garching), D.A. Kann (TLS
Tautenburg) and J. Greiner (MPE Garching)  report on behalf of the GROND
team: 

We observed the GRB 140408A field again on further three epochs,
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).


The afterglow candidate reported in Varela et al. (GCN #16089) remained
constant, thus this source is a fore- or background source and not the
afterglow of GRB 140408A.

For the first epoch as reported in Varela et al. (GCN #16089), no other
source is seen in the 1".8 Swift-XRT refined error circle
(http://www.swift.ac.uk/xrt_positions/00595141/) down to limiting magnitudes
(all in the AB system) of

g' > 25.8 mag, 
r' > 25.6 mag, 
i' > 25.0 mag, 
z' > 25.0 mag, 
J > 22.1 mag, 
H > 21.5 mag, and 
K > 20.0 mag.

The given limits are 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)= 0.16 in the
direction of the burst (Schlegel et al. 1998). 


GRB_name: GRB140529A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16342
SUBJECT: GRB 140529A: Swift-XRT afterglow detection.
DATE:    14/05/30 10:16:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans (U. Leicester) and J.L. Racusin (GSFC) report on behalf of
the Swift-XRT team:

We have analysed 2.5 ks of XRT data for the ground-detected GRB 140529A
(Cummings, GCN. Circ. 16340) from 65.0 ks to 75.4 ks after the BAT
trigger time. The data are entirely in Photon Counting (PC) mode.  An
X-ray source is detected within the Swift/BAT error circle. Using 1098
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 = 228.78202, -41.05295 which is equivalent
to:

RA (J2000): 15h 15m 07.68s
Dec(J2000): -41d 03' 10.6"

with an uncertainty of 3.3 arcsec (radius, 90% confidence). This
position is 97 arcsec from the Swift/BAT position. 

In the first two spacecraft orbits, totalling 1.2 ks of data, the
source is present with a count rate of 0.012+/-0.004 ct/sec. In the
final orbit, with 1.3 ks of data the source is not detected, with a
3-sigma upper limit of 0.0045 ct/sec. We thus conclude that this was
the afterglow of GRB 140529A.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020383.

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


GRB_name: GRB140529A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16343
SUBJECT: GRB 140529A: Swift/UVOT Upper Limits
DATE:    14/05/30 12:31:31 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (IAA-CSIC, MSSL-UCL) and J.L. Racusin (GSFC) 
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of the ground-detected 
GRB 140529A 65ks after the BAT trigger (Cummings, GCN. Circ. 16340).
No optical afterglow consistent with the XRT position 
(Evans et al., GCN Circ. 16342) 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

white             65040       69412          287         >21.0
u                 65017       74873         1635         >21.0

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.13 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB140528A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16344
SUBJECT: Konus-Wind observation of GRB 140528A
DATE:    14/05/30 13:27:09 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, and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration, moderately intense GRB 140528A (Golenetskii et al., 
GCN 16339) triggered Konus-Wind at T0=72325.953 s UT (20:05:25.953).
The burst light curve shows a multi-peaked structure with a total 
duration of ~16 s. The emission is seen up to ~3 MeV.

As observed by Konus-Wind, the burst had a fluence of 
2.4(-0.3,+0.3)x10^-5 erg/cm2, and a 64-ms peak flux, measured from 
T0+10.112 s, of 5.1(-1.3,+1.3)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+16.640 
s) is best fit in the 20 keV - 5 MeV range
by a GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.59(-0.14,+0.17),
the high energy photon index beta = -2.8(-0.7,+0.3),
the peak energy Ep = 202(-20,+21) keV,
chi2 = 47/72 dof.

The spectrum near the maximum count rate (measured from T0+8.448 s to 
T0+16.640 s) is best fit in the 20 keV - 5 MeV range
by a GRB (Band) model with the following parameters:
the low-energy photon index alpha =-0.40(-0.23,+0.27),
the high energy photon index beta = -2.7(-1.1,+0.3),
the peak energy Ep = 177(-22,+27) keV,
chi2 = 60/69 dof.

The Konus-Wind light curve of this GRB is available at 
http://www.ioffe.ru/LEA/GRBs/GRB140528_T72325/

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


GRB_name: GRB140529A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16345
SUBJECT: Konus-Wind observation of GRB 140529A
DATE:    14/05/30 14:28:45 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, and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration, soft spectrum GRB 140529A (Cummings, GCN 16340)
triggered Konus-Wind at T0=34086.312 s UT (09:28:06.312).
The burst light curve shows a single peak with a total duration of ~3 s.
The emission is seen up to ~1 MeV.

As observed by Konus-Wind, the burst had a fluence of 
2.6(-0.3,+0.3)x10^-6 erg/cm2,
and a 64-ms peak flux, measured from T0+0.248 s, of 1.7(-0.4,+0.4)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+8.448 s)
is best fit in the 20 keV - 1 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -1.50(-0.45,+0.54),
and Ep = 52(-31,+17) keV, chi2 = 66/50 dof.
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.92 (chi2 = 
66/49 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140529_T34086/

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


GRB_name: GRB140529A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16346
SUBJECT: GRB 140529A BAT refined analysis
DATE:    14/05/30 17:38:50 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),
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):

We report further analysis of GRB 140529A (Cummings, GCN Circ. #16340). The
best BAT position is RA, Dec 228.810,-41.042 which is

RA (J2000)    15h 15m 14.4s
Dec (J2000)  -41d 02' 33"

with an estimated 90% uncertainty radius of 1.2 arcmin.  This is 16 arcsec
from the previously reported BAT position and 85 arcsec from the position of
the XRT source reported in Evans et al. (GCN Circ #16342).  The partial coding
was about 18%.

The maskweighted lightcurve shows a single FRED peak with an estimated T90
of 4.5 +- 0.5 seconds.

The best fit to the spectrum from 15-150 keV is a powerlaw with an exponential
cutoff.  The photon index is 0.85 +- 0.35 with a cutoff energy of 75 +- 10 keV.
The best simple powerlaw fit has a photon index of 1.66 +- 0.08.  The total
fluence from 15-150 keV in5.0 seconds was (2.2 +- 0.1) x 10^-6 ergs/cm^2.  The
1-second peak flux in the energy range 15-150 keV was 11.5 +- 0.7 photons/cm^2.

Because this was not a normal onboard trigger, the usual automated BAT data
products are not available.


GRB_name: GRB140528A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16347
SUBJECT: GRB 140528A: Fermi GBM Detection
DATE:    14/05/30 22:51:39 GMT
FROM:    Matthew Stanbro at UAH/Fermi  <mcs0001@uah.edu>

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

"At 20:05:22.75 UT on 28 May 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140528A (trigger 423000325 / 140528837)
which was triangulated by IPN (Golenetskii et al. 2014, GCN 16339).
The GBM on-ground location, using the Fermi GBM trigger data,
is consistent with IPN triangulation.

The GBM light curve shows a complex structure, consisting of multiple peaks
with a total duration (T90) of about 13.6 s (50-300 keV).
The time-averaged spectrum from T0+1.024 s to T0+14.591 s is well fit
by a power law function with an exponential high-energy cutoff.
The power law index is -0.56 +/- 0.03 and the cutoff energy,
parameterized as Epeak, is 270 +/- 6 keV.


The event fluence (10-1000 keV) in this time interval is
(2.3 +/- 0.3)E-05 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+11.20 s in the 10-1000 keV band is 13.6 +/- 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: GRB140523A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16348
SUBJECT: GRB 140523A: further Swift-XRT observations
DATE:    14/06/02 20:59:57 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia (ASDC) reports on behalf of the Swift-XRT team:

We have observed again the field of the Fermi GRB 140523A (von Kienlin  
and Connaughton, GCN 16321; Vianello et al. GCN 16322), to search for  
variability of the X-ray afterglow candidates.
In the 5 ks of XRT data acquired, starting on 2014-05-31 at 02:33:06  
UT (i.e., ~ 8 days after the burst), all X-ray candidates are still  
detected with no hint of afterglow-like variability behavior.
We thus conclude that none of the candidate sources is the X-ray  
afterglow of GRB 140523A.

More details about this analysis can be found on:
http://www.swift.ac.uk/xrt_products/TILED_GRB00026


GRB_name: GRB140604A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16350
SUBJECT: IPN Triangulation of GRB 140604A (short/hard)
DATE:    14/06/05 15:27:42 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 and J. Goldsten, on behalf of the MESSENGER NS GRB team,

G. Di Cocco, F. Fuschino, M. Galli, C. Labanti, and M. Marisaldi, on
behalf of the AGILE MCAL 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 140604A has been observed
by Konus-Wind, AGILE (MCAL), MESSENGER (GRNS), and INTEGRAL (SPI-ACS),
so far, at about 17411 s UT (04:50:11).

We have triangulated it to a preliminary, 3 sigma error box whose 
coordinates are:
---------------------------------------------
    RA(2000), deg                 Dec(2000), deg
   ---------------------------------------------
   Center:
    263.170 (17h 32m 41s) -40.406 (-40d 24' 22")
   Corners:
    262.578 (17h 30m 19s) -40.773 (-40d 46' 24")
    263.162 (17h 32m 39s) -41.034 (-41d 02' 02")
    263.750 (17h 35m 00s) -40.031 (-40d 01' 53")
    263.172 (17h 32m 41s) -39.770 (-39d 46' 12")
   ---------------------------------------------
The error box area is 2020 sq. arcmin, and its maximum
dimension is 76 arcmin (the minimum one is 31 arcmin).

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB140604_T17415/IPN/

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


GRB_name: GRB140604A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16351
SUBJECT: Konus-Wind observation of GRB 140604A
DATE:    14/06/05 15:35:03 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, and T. Cline
on behalf of the Konus-Wind team, report:

The short-duration, hard spectrum, bright GRB 140604A (Golenetskii et 
al., GCN ) triggered Konus-Wind at T0=17415.447 s UT (04:50:15.447).
The burst light curve shows several peaks with a total duration of ~1s. 
The emission is seen up to ~3 MeV.

As observed by Konus-Wind, the burst had a fluence of
7.2(-1.8,+2.4)x10^-6 erg/cm2, and a 16-ms peak flux, measured from 
T0+0.592 s, of 2.55(-0.65,+0.89)x10^-5 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 - 4 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.54(-0.32,+0.43),
and Ep = 795(-236,+414) keV (chi2 = 62/68 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -1.7 (chi2 = 
62/67 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140604_T17415/

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


