# GCN_circulars

GRB_name: GRB140129A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15781
SUBJECT: GRB 140129A: Khureltogot optical  limit
DATE:    14/01/31 09:54:37 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), N. Tungalag (Research Centre of Astronomy and Geophysics 
MAS ) V. Voropaev (KIAM), I.Molotov (KIAM), A. Pozanenko (IKI) report on 
behalf of larger GRB
follow-up collaboration:

We observed the field of the Swift GRB 140129A (Melandri et al., GCN 15760) 
on Jan., 29 with ORI-40 telescope of  Khureltogot  observatory (Mongolia). 
We took
several unfiltered images  of 60 s exposure. Within enhanced XRT error 
circle (Evans et al., GCN 15764) we do not detect the optical afterglow 
(Melandri et al., GCN 15760).

Details of the photometry are following:

UT start        t-T0             Filter   Exp.     OT   UL (3 sigma)
                  (mid, days)                 (s)
12:02:22     0.38515         None   68x60   n/d   20.0

The photometry is based 3 SDSS stars, R (gri -> R transformations by
Lupton 2005):

SDSS id                                 R
J023133.01-013533.5       18.121
J023122.45-013411.0       18.797
J023137.01-013606.5       19.143


GRB_name: GRB140129A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15782
SUBJECT: GRB 140129A: Continued RATIR Optical and NIR Observations
DATE:    14/01/31 15:09:30 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 140129A (Melandri, et al., GCN 15760)
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 2014/01 31.11 to 2014/01 31.20 UTC
(47.35 to 49.51 hours after the BAT trigger), obtaining a total of 1.38
hours exposure in the r and i bands and 0.58 hours exposure in the Z, Y, J,
and H bands.

The afterglow observed previously by RATIR (Cucchiara, et al., GCN 15762;
Butler, et al., GCN 15779) is no longer detected.  In comparison with the
SDSS DR9 and 2MASS, we obtain the following upper limits (3-sigma):

  r     > 22.99
  i     > 22.59
  Z     > 21.59
  Y     > 21.14
  J     > 20.82
  H     > 20.49

These magnitudes are in the AB system and are not corrected for Galactic

extinction in the direction of the GRB.


GRB_name: GRB140129A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15783
SUBJECT: GRB 140129A: 5 GHz VLA observations
DATE:    14/02/05 15:41:46 GMT
FROM:    Alessandra Corsi at GWU  <corsi@email.gwu.edu>

A. Corsi (GWU) reports on behalf of a larger collaboration:

We observed the field of the Swift GRB 140129A (Melandri et al., GCN #15760) 
using the the Karl G. Jansky Very Large Array (VLA) in C-band, and starting at 
00:57:45 UT on 30 Jan 2014.  A provisional reduction shows no radio emission 
above the 3-sigma level of 30uJy (the map rms is ~10uJy at 5 GHz) within the Swift 
XRT error-circle (Evans et al. GCN #15764). The flux density at the P60 optical 
afterglow position (Perley & Cenko, GCN #15761) is -8 +/-10 uJy at 5 GHz. 

We thank the VLA staff for executing these observations.


GRB_name: GRB140206A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15784
SUBJECT: GRB 140206A: Swift detection of a burst
DATE:    14/02/06 07:49:38 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

A. Y. Lien (NASA/GSFC/ORAU), S. D. Barthelmy (GSFC),
M. M. Chester (PSU), V. D'Elia (ASDC), D. Malesani (DARK/NBI),
A. Maselli (INAF-IASFPA), K. L. Page (U Leicester),
D. M. Palmer (LANL) and M. H. Siegel (PSU) report on behalf of the
Swift Team:

At 07:17:20 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140206A (trigger=585834).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 145.350, +66.750 which is 
   RA(J2000)  =  09h 41m 24s
   Dec(J2000) = +66d 45' 01"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a multi-peaked
structure with a duration of about 80 sec.  The peak count rate
was ~19000 counts/sec (15-350 keV), at ~60 sec after the trigger. 

The XRT began observing the field at 07:18:04.0 UT, 43.9 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 145.33438, 66.76074 which
is equivalent to:
   RA(J2000)  = 09h 41m 20.25s
   Dec(J2000) = +66d 45' 38.7"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 44 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 4.79
x 10^20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 9.62e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT results are not available at this time. 

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


GRB_name: GRB140206A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15785
SUBJECT: GRB140206A: a long GRB detected by INTEGRAL
DATE:    14/02/06 08:10:46 GMT
FROM:    Diego Gotz at CEA  <diego.gotz@cea.fr>

D. Gotz (IASF Milano) S.Mereghetti (IASF-Milano), E.Bozzo, C.Ferrigno, M. Tuerler (ISDC, Versoix), and J.Borkowski (CAMK, Torun) on behalf of the IBAS Localization Team report:
a long gamma ray burst lasting at least 60 s 0.8 s has been detected by IBAS in the IBIS/ISGRI data at 07:17:26  UT of February 6th.
The refined coordinates (J2000) are:

R.A.= 145.3043  deg
DEC.= +66.7652  deg

with an uncertainty of 0.8 arcmin (90% c.l.). This position is consistent with the Swift/XRT one reported for the same event (Lien et al., GCN 15784).
The burst has been detected at the very beginning of the INTEGRAL orbit, just outside the radiation belts. Therefore the data are polluted by a high particle background, implying a high level of saturation of the IBIS/ISGRI telemetry. Hence no detailed information about the GRB duration can be derived at this stage. A preliminary lower limit on its fluence is 2x10e-6 erg/cmsq in the 20-200 keV energy band.
A plot of the light curve will  be posted at http://ibas.iasf-milano.inaf.it/IBAS_Results.html


GRB_name: GRB140206A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15786
SUBJECT: GRB140206A - Optical afterglow candidate
DATE:    14/02/06 09:42:27 GMT
FROM:    Arto Oksanen at Nyrola Obs., Finland  <oksanen@nyrola.jklsirius.fi>

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

We detect an afterglow candidate on Rc filtered images taken at 2014-02-06T08:33:09 with 
a 40 cm robotic telescope located in New Mexico, USA.

R.A. = 09 41 20 (J2000)
Decl = 66 45 38

The position matches with the XRT position given by A. Y. Lien et. al (GCN 15784).

Approximate magnitude R=18, seem to be fading. Observations and analysis is ongoing.


GRB_name: GRB140206A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15787
SUBJECT: GRB 140206A: Swift/UVOT optical detection
DATE:    14/02/06 11:03:15 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (MSSL-UCL) and A. Y. Lien (NASA/GSFC/ORAU) report on behalf 
of the Swift/UVOT team:

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 54 seconds after the BAT trigger. There is a candidate afterglow in
the finding chart image:

     RA (J2000)   9:41:20.24 = 145.33433 
    Dec (J2000)  +66:45:38.5 = 66.76069  

with an estimated uncertainty of 0.5 arcsec (radius, 90% confidence). 
This position is consistent with the XRT position (Lien et al., GCN 15784) 
and the optical afterglow position reported by Oksanen et al (GCN 15786). 
The estimated magnitude is 15.76 with a 1-sigma error of about  0.03. 
No correction has been made for the expected extinction corresponding 
to E(B-V) of 0.12. 


GRB_name: GRB140206A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15788
SUBJECT: GRB 140206A:  MASTER OT detection
DATE:    14/02/06 11:08:00 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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

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

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

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

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Blagoveschensk was pointed to the  GRB140206A (Lien et. al GCN 
15784 , Gotz et. al GCN 15784)  2h 16m (8153 s) after trigger time at 
2014-02-06 09:33:13 UT directly after sunset. On our first sets we found 
optical transient Oksanen et. al. GCN 15786.

The coordinate is:

RA= 09h 41m 20.21s
DEC= +66d 45m 37.7s
ERROR= 0.5 arcsec
Mag=18.5 +- 0.25m

Our unfiltered magnitude is calibrated by USNO
B1.0 catalog  by a parity 0.8R + 0.2B.

The message may be cited.


GRB_name: GRB140206A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15789
SUBJECT: GRB 140206A: Nanshan optical observations
DATE:    14/02/06 13:55:07 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), G.-J. Feng, J. Xu, A. Esamdin, L. Ma (XAO) report:

We observed the field of GRB 140206A (Lien et al., GCN 15784; Gotz et
al., GCN 15785) using the 1m telescope located on Mt. Nanshan,
Xinjiang, China. Observations started at 12:30:16 UT on 2014-02-06
(i.e., 5.216 hr after the burst), and a series of R-band frames were
obtained.

The optical afterglow (Oksanen et al., GCN 15786; Oates & Lien, GCN
15787) is clearly detected in each of our frames, and it decayed from
M(R)=18.48+/-0.10 to m(R)=18.64+/-0.10 from 5.40 hr to 5.71 hr
post-burst, calibrated with two nearby SDSS stars. Compared with the
previous measurements in GCNs 15786 & 15788, it shows that so far the
afterglow has been decaying rather slowly and thus spectroscopy may be
doable even for a 2m class telescope in the coming hours.

Further observations are ongoing.


GRB_name: GRB140206B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15790
SUBJECT: GRB 140206B: Fermi GBM detection
DATE:    14/02/06 14:09:48 GMT
FROM:    Andreas von Kienlin at MPE  <azk@mpe.mpg.de>

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

"At 06:36:12.84 UT on 06 February 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140206B (trigger 413361375 / 140206275).

The on-ground calculated location, using the GBM trigger data, is RA =
314.6, 
DEC = -6.6 (J2000 degrees, equivalent to 20 h 58 m, -6 d 36 '), 
with an uncertainty of 1.9 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).

The trigger resulted in an Autonomous Repoint Request (ARR)
that was accepted and the spacecraft slewed to the GBM in-flight location. 
The initial angle from the LAT boresight was 46 deg from the Fermi/GBM
position.

The GBM light curve is multi-peaked with a duration (T90) of about 120 s
(50-300 keV). 
The time-averaged spectrum  from T0+0.003 s to T0+44.993 s is well fit by a
Band function 
with Epeak = 296.6 +/- 7.3 keV, alpha = -0.97 +/-0.01 and beta = -2.14
+/-0.03
 
The event fluence (10-1000 keV) in this time interval is
(0.993 +/- 0.005)E-04 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+13.44 s in the 10-1000 keV band
is 42.4 +/- 0.4 ph/s/cm^2.

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


GRB_name: GRB140206B
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15791
SUBJECT: GRB 140206B: Fermi-LAT detection
DATE:    14/02/06 14:31:50 GMT
FROM:    Elisabetta Bissaldi at U.Innsbruk/IAPP  <Elisabetta.Bissaldi@uibk.ac.at>

E. Bissaldi (University & INFN Trieste), G. Vianello (Stanford University),
F. Longo (University & INFN Trieste), R. Desiante (Udine University & 
INFN Trieste),
J. Racusin (NASA/GSFC) report on behalf of the Fermi-LAT team:


On February 6th, 2014, Fermi LAT detected high-energy emission
from GRB 140206B, which triggered GBM at 06:36:12.84 UT
(trigger 413361375/140206275, von Kienlin et al., GCN 15790).
GBM also initiated an autonomous repoint of Fermi at 06:36:25 UT
due to high peak flux.

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

(RA, Dec) = 315.26, -8.51 (J2000)

with an error radius of 0.23 deg (90% containment, statistical error only).
This was 45 deg from the LAT boresight at the time of the trigger.

More than 25 photons above 100 MeV and 2 photons above 1 GeV are observed
within 600 seconds. The highest-energy photon is a 3.5 GeV event,
which is observed 460 seconds after the GBM trigger.

Unfortunately, the GRB position is too close to the Sun  (8.2 deg)
for Swift to conduct follow-up observations.

The Fermi LAT point of contact for this burst is
Elisabetta Bissaldi (Elisabetta.Bissaldi@ts.infn.it 
<mailto: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: GRB140206A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15792
SUBJECT: GRB 140206A: ISON-Ussuriysk optical observations
DATE:    14/02/06 15:54:46 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), A. Stepura (UAFO, ISON), A. Matkin (UAFO, ISON),  I. 
Molotov (KIAM), A. Pozanenko (IKI) report on behalf of larger GRB 
follow-up collaboration:

We observed the afterglow (Oksanen et al., GCN 15786; Oate et al., GCN 
15787) of the Swift and INTEGRAL GRB 140206A (Lien et al., GCN 15784; 
Gotz et al., GCN 15785) with VT-50 (0.5m) telescope of 
UAFO/ISON-Ussuriysk observatory starting on Feb. 6 (UT) 09:20:05, i.e. 
~2 hours after burst trigger. We took unfiltered images of 30s 
exposures.  In  stacked frames we clearly detect afterglow. A 
preliminary photometry of the afterglow is following:

T_start               T0+       Filter, Exposure,   OT,     OT_err
(UT)                  (mid, d)            (s)

2014-02-06T09:20:39   0.08783   none     9*30       17.76   0.24
2014-02-06T10:52:26   0.15309   none    19*30       18.06   0.08

The photometry is based on reference stars SDSS-DR9, (R mag,
transformation by Lupton 2005)

N   SDSS_id                       R(Lupton)errR
1   J094123.75+664429.9    15.441+/-0.013
2   J094126.54+664410.8    13.837+/-0.014
3   J094131.29+664857.0    13.972+/-0.011

Observations continuing.
The finding chart can be found in 
http://grb.rssi.ru/GRB140206A/grb140206A_VT50_fc.png


GRB_name: GRB140206A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15793
SUBJECT: GRB 140206A: Enhanced Swift-XRT position
DATE:    14/02/06 16:16:45 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Using 2549 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 140206A, 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 = 145.33452, +66.76101 which is equivalent
to:

RA (J2000): 09h 41m 20.29s
Dec (J2000): +66d 45' 39.6"

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

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

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


GRB_name: GRB140206A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15794
SUBJECT: GRB 140206A: theoretical prediction of redshift and of supernova occurrence
DATE:    14/02/06 18:05:40 GMT
FROM:    Remo Rufinni at ICRA  <ruffini@icra.it>

R. Ruffini, C.L. Bianco, M. Enderli, M. Kovacevic, M. Muccino, A.V.
Penacchioni, G.B. Pisani, J.A. Rueda, Y. Wang report:

The late Swift/XRT observations of GRB 140206A (1,2) evidences the
fullfillment of the IGC paradigm (3,4). A preliminary overlapping of
its X-ray (0.3-10 keV in rest-frame) luminosity with the one of GRB
090618, namely an IGC prototype (5), gives an estimate of the redshift
of z~0.6 (see Fig. 1 <http://www.icranet.org/images/GCN/GRB140206A.pdf>).

As a consequence, a supernova associated to GRB 140206A is expected to
emerge after 16 days after the trigger.

Continuous monitoring and complementary observations in all possible
wavelengths are encouraged.

References:
(1) Lien et al., GCN 15784
(2) Osborne et al., GCN 15793
(3) Rueda & R. Ruffini, ApJLett, 758, L7 (2012)
(4) Pisani et al., A&A, 552, L5 (2013)
(5) Izzo et al., A&A, 548, L5 (2012)


GRB_name: GRB140206A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15795
SUBJECT: GRB 140206A: Swift/UVOT Detection
DATE:    14/02/06 18:20:25 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (UCL-MSSL) and A. Y. Lien (NASA/GSFC/ORAU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140206A
52 s after the BAT trigger (Lien et al., GCN Circ. 15784).
A source consistent with the XRT position (Osborne et al. GCN Circ. 15793)
and the optical positions reported by Oksanen et al. (GCN 15786) and 
Yurkov et al. (GCN 15788) is detected in the initial UVOT exposures. The 
lack of detections in the UV filters suggests a redshift ~2 - 3.

The preliminary UVOT position is:
  RA  (J2000) =  09:41:20.26 = 145.33442 (deg.)
  Dec (J2000) = +66:45:38.6  =  66.76072 (deg.)
with an estimated uncertainty of 0.50 arc sec. (radius, 90% confidence).

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

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

white               52          202          147         15.88 +/- 0.02
v                  596          616           20         15.75 +/- 0.11
b                  522          542           20         16.51 +/- 0.09
u                  264          514          246         16.18 +/- 0.04
w1                 645        17944          963         >20.9
m2               16137        24450         1607         >21.2
w2               21898        22798          886         >21.0

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.14 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB140206A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15796
SUBJECT: GRB 140206A: Fermi GBM detection
DATE:    14/02/06 18:29:24 GMT
FROM:    Narayana Bhat at U Alabama/Huntsville/GBM  <Narayana.Bhat@nasa.gov>

A. von Kienlin (MPE) and P. N. Bhat (UAH)
report on behalf of the Fermi GBM Team:

"At 07:18:15.98 UT on 06 February 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140206A (trigger 413363898 / 140206304),
which was also detected by the Swift (Lien et al. 2014, GCN 15784)
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 123 degrees.

The GBM light curve shows a single pulse
with a duration (T90) of about 27 s (50-300 keV).
The time-averaged spectrum from T0-0.5 s to T0+14.3 s is
best fit by a Band function with Epeak = 120 +/- 6  keV,
alpha = 0.2 +/- 0.1, and beta = -2.4 +/-0.1.

The event fluence (10-1000 keV) in this time interval is
(1.47 +/- 0.03)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+4.9 s in the 10-1000 keV band
is 17.4 +/- 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: GRB140206A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15797
SUBJECT: GRB 140206A: T100 observations
DATE:    14/02/06 19:34:14 GMT
FROM:    Eda Sonbas at NASA/GSFC  <edasonbas@gmail.com>

E. Sonbas (Adiyaman Univ.), T. Guver (Istanbul Univ.), U. Temiz (Cukurova
Univ.), E. Gogus (Sabanci Univ.), M. Kocak (TUG), O. Erece (Akdeniz Univ.),
Z. Eker (Akdeniz Univ.) report on behalf of a larger collaboration


 We observed the field of Swift GRB 140206A (Lien et al., GCN#15784) with
the 1.0 meter T100 telescope (Bakirlitepe, TUBITAK National Observatory,
Turkey), starting February, 06, 16:33:24 UT (~ 9.268 hours after the
trigger). Observations were carried out in the R filter under good weather
conditions. The afterglow is clearly detected in 300 s in the R band images
at a position that is consistent with Oksanen et al. GCN#15786 and Oates et
al., GCN#15787

Using USNO-B1 star USNO-B1 1567-0128093 (R.A.=9:41:23.33, Dec=+66:44:32.31)
in the field, the magnitudes of the OT were estimated as follows;

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

9.590 300 R 18.65 0.05

9.689 300 R 18.77 0.06

9.788 300 R 18.75 0.06

10.380 300 R 18.89 0.06

 Further observations using the same filter are ongoing.

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


GRB_name: GRB140206A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15798
SUBJECT: GRB 140206A: Swift-XRT refined Analysis
DATE:    14/02/06 20:57:35 GMT
FROM:    Alessandro Maselli at INAF/IASF Palermo  <maselli@ifc.inaf.it>

A. Maselli (INAF-IASFPA), A. Y. Lien (NASA/GSFC/ORAU) and P. A. Evans
(U. Leicester) report on behalf of the Swift-XRT team:

We have analysed 14 ks of XRT data for GRB 140206A (Lien et al. GCN
Circ. 15784), from 33 s to 30.2 ks after the BAT trigger. The data
comprise 1.2 ks in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Osborne et
al. (GCN Circ. 15793).

The light curve shows initial flaring activity with two flares peaking
at about 61 s and 223 s after the trigger. The underlying emission can
be modelled with a broken power-law decay: a flat decay with an index
alpha=0.756 (+0.026, -0.028), a break at T+10.7 ks and a late-time
decay with an index 1.31 (+0.15, -0.12).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.762 (+/-0.028). The
best-fitting absorption column is 1.25 (+/-0.07) x 10^21 cm^-2, in
excess of the Galactic value of 4.8 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.95 (+0.08, -0.07)
and a best-fitting absorption column of 1.22 (+0.19, -0.18) x 10^21
cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.8 x 10^-11 (4.9 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.22 (+0.19, -0.18) x 10^21 cm^-2
Galactic foreground: 4.8 x 10^20 cm^-2
Excess significance: 6.6 sigma
Photon index:      1.95 (+0.08, -0.07)

If the light curve continues to decay with a power-law decay index of
1.31, the count rate at T+24 hours will be 0.088 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.3 x
10^-12 (4.3 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/00585834.

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


GRB_name: GRB140206A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15799
SUBJECT: GRB 140206A: TNG optical observations
DATE:    14/02/06 21:44:59 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, S. Covino, A. Melandri (INAF/OAB) L. Di Fabrizio (INAF/TNG) report on behalf of the CIBO collaboration:

We observed the field of GRB 140206A (Lien et al., GCN 15784; Gotz et al. GCN 15785) using the DOLORES camera on the 3.6-m TNG Telescope at Canary Islands.

The optical afterglow (Oates & Lien GCN 15787; Yurkov et al. GCN 15788; Xu et al. GCN 15789; Volnova et al. GCN 15792; Oates & Lien GCN 15795; Sonbas et al. GCN 15797) is clearly detected with R = 18.7 +/- 0.1 (calibrated against the USNOB1 catalogue) at t-t0 = 12.52 hours.

Further observations are ongoing.


GRB_name: GRB140206A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15800
SUBJECT: GRB 140206A: NOT redshift
DATE:    14/02/06 21:52:48 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Malesani, D. Xu, J. P. U. Fynbo (DARK/NBI), A. de Ugarte Postigo 
(IAA/CSIC and DARK/NBI), S. Schulze (PUC and MCSS), A. Finoguenov (U. 
Helsinki), P. Jakobsson (U. Iceland), A. Melandri (INAF/OABr), A. 
Cucchiara (NASA/GSFC), report on behalf of a larger collaboration:

We observed the field of GRB 140206A (Lien et al., GCN 15784; Gotz et 
al., GCN 15785; von Kienlin & Bhat, GCN 15796) with the Nordic Optical 
Telescope (NOT) equipped with ALFOSC. Observations started at 19:56 UT 
on February 6 (i.e., 12.66 hr after the burst).

We first obtained a 100-s image in R band.  We clearly detect the source 
reported in Oksanen et al. (GCN 15786). The source has faded to 19.15 
+/- 0.10 mag (Vega magnitude), based on nearby USNO stars.

We aso obtained an optical spectrum, with a total exposure of 2 x 1800 
s, using grism #4 and a blocking filter covering the wavelength range 
3750 - 9000 AA at a resolution of 8.1 AA. The mid exposure time is 13.6 
hr after the GRB.

We detect several absorption lines which we interpret as due to Lyalpha, 
Si II, C II, C IV, Al II, Fe II at a common redshift of 2.73.

This measurement is not consistent with the predicted theoretical value 
by Ruffini et al. (GCN 15794).

We thank Carlos Perez, John Teltin, and Amanda Djupvik (NOT) for 
excellent support with the observations.

[GCN OPS NOTE(07feb14): The Troja reference was corrected to the
von Kienlin & & Bhat reference.]


GRB_name: GRB140206A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15801
SUBJECT: GRB 140206A: Optical Observations via Virtual Telescope
DATE:    14/02/06 22:21:53 GMT
FROM:    Gianluca Masi at Bellatrix Astronomical Obs  <gianluca@bellatrixobservatory.org>

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

On Feb. 6.9216 2014 UT, we imaged the field around GRB 140206A (Lien et. al GCN
15784 , Gotz et. al GCN 15784) 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. = 09 41 20.23
Decl. +66 45 38.5

We also performed photometry, assuming R-mags from UCAC-4 for the stars in the
field, getting an estimate for the magnitude of 18.9CR).

Observations are ongoing.

This message can be cited


GRB_name: GRB140206A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15802
SUBJECT: GRB 140206A: TNG redshift confirmation
DATE:    14/02/06 22:52:54 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia (INAF/OAR & ASI/ASDC), P. D'Avanzo, S. Covino, A. Melandri  
(INAF-OAB), S. D. Vergani (CNRS/GEPI), L. Di Fabrizio (INAF/TNG)  
report on behalf of the CIBO collaboration:

We report further observations of the field of GRB 140206A (Lien et  
al., GCN 15784; Gotz et  al., GCN 15785) with the Telescopio Nazionale  
Galileo (TNG) equipped with DOLORES.

We obtained a spectrum of the optical source reported in  D'Avanzo et  
al. (GCN Circ. 15799), with a total exposure of 1800 s, using the  
grism LR_B covering the wavelength range 3000 - 8000 AA. The  
observation started at 2014-02-06T19:53:07, i.e., ~12.6 hrs after the  
GRB.


We detect several absorption lines which we interpret as due to Ly-alpha,
NV, Si II, C II, SiIV, C IV, Al II, AlII and Fe II at a common  
redshift of 2.74. In addition, we also detect at the same redshift  
fine structure lines from excited levels of SiII and FeII, confirming  
that this is the redshift of the GRB host galaxy. Our result is in  
perfect agreement with the reported value by Malesani et al. (GCN 15800)

Finally, we also detect a strong intervening Ly-alpha absorber at z~2.32

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GRB_name: GRB140206A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15803
SUBJECT: GRB 140206A: MITSuME Akeno detection of the optical counterpart
DATE:    14/02/07 04:33:05 GMT
FROM:    Yoichi Yatsu at Tokyo Tech.  <yatsu@hp.phys.titech.ac.jp>

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

We observed the field of GRB 140206A (A. Y. Lien et al., GCNC 15784) with
the
optical three color (g, Rc, and Ic) CCD cameras mounted on the MITSuME 50 cm
telescope of Akeno Observatory, Yamanashi, Japan.

The observation started on 2014-02-06 15:46:53 UT ( ~8.5 hour after the
burst) and we detected the previously reported afterglow.
The measured magnitudes were listed as follows.

T0+[hour]     MID-UT      T-EXP[sec]          g'
Rc               Ic
------------------------------------------------------------
-----------------------------------------
  ~8.5       17:36:31      199x60        20.74+/-0.14      18.88+/-0.08
18.37+/-0.10
------------------------------------------------------------
-----------------------------------------
(The photon flux were calibrated by SDSS(g') and GSC2.3(Rc, Ic) catalog.)


GRB_name: GRB140206B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15804
SUBJECT: Konus-Wind observation of GRB 140206B
DATE:    14/02/07 08:29:36 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration intense GRB 140206B
(Fermi-GBM detection: von Kienlin, GCN 15790;
Fermi-LAT detection: Bissaldi et al., GCN 15791)
triggered Konus-Wind at T0=23769.061 s UT (06:36:09.061).

The light curve consists of two major multi-peaked emission
episodes in the time interval from ~T0-3 s to ~T0+155 s.
The emission is seen up to ~12 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140206_T23769/

As observed by Konus-Wind, the burst
had a fluence of (1.52  0.09)x10-4 erg/cm2,
and a 64-ms peak flux, measured from T0+7.488 s,
of (1.73  0.09)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+154.368 s)
is best fit in the 25 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.07  0.08,
the high energy photon index beta = -2.28  0.09,
the peak energy Ep = 227  18 keV,
chi2 = 93.8/96 dof.

The spectrum near the maximum count rate
(measured from T0+8.448 s to T0+16.384 s)
is best fit in the 35 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.59  0.08,
the high energy photon index beta = -2.18  0.04,
the peak energy Ep = 278  16 keV,
chi2 = 84.3/93 dof.

All the quoted results are preliminary.


GRB_name: GRB140206A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15805
SUBJECT: GRB 140206A, Swift-BAT refined analysis
DATE:    14/02/07 21:56:28 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

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

Using the data set from T-240 to T+962 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140206A (trigger #585834)
(Lien, et al., GCN Circ. 15784).  The BAT ground-calculated position is
RA, Dec = 145.321, 66.762 deg which is
 RA(J2000)  =  09h 41m 16.9s
 Dec(J2000) = +66d 45' 42.7"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The mask-weighted light curve shows a multi-peaked structure with roughly three main pulse
durations. The first pulse duration starts at ~T-15 and ends at ~T+25 sec, and consists of
roughly three to four peaks. The second one starts at ~T+50 sec, peaks at ~T+60 sec,
and ends at ~T+90 sec. The third weaker pulse peaks at ~T+210 sec, with a long low-level tail
out to T+400 sec. T90 (15-350 keV) is 93.6 +- 13.8 sec (estimated error including systematics).

The time-averaged spectrum from T-37.2 to T+256.1 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.04 +- 0.15,
and Epeak of 100.9 +- 14.5 keV (chi squared 52.76 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 1.6 +- 0.03 x 10^-5 erg/cm2
and the 1-sec peak flux measured from T+60.80 sec in the 15-150 keV band is
19.4 +- 0.5 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.58 +- 0.03 (chi squared 91.21 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/585834/BA/


GRB_name: GRB140206A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15806
SUBJECT: GRB 140206A: Liverpool Telescope optical afterglow observations
DATE:    14/02/08 09:59:29 GMT
FROM:    Drejc Kopac at Math Phys U,Slovenia  <drejc.kopac@fmf.uni-lj.si>

D. Kopac, A. Gomboc (U. Ljubljana), C. Guidorzi (U. Ferrara), A. 
Melandri (INAF-OAB), I. A. Steele, C. G. Mundell (LJMU), on behalf of a 
large collaboration report:

The 2-m Liverpool Telescope automatically observed Swift-INTEGRAL-Fermi 
GRB 140206A (Lien et al., GCN 15784; Gotz et al., GCN 15785), starting 
at 07:19:30 UT (~2.2 min after the burst trigger).

We clearly detect the fading optical afterglow at the position reported 
by Oksanen et al. (GCN 15786). In our first 10 sec frame, we estimate 
the magnitude r' = 14.97 +- 0.02 at t_mid = 135 sec since the Swift/BAT 
trigger time. The magnitude is calibrated against nearby SDSS stars.


GRB_name: GRB140206A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15807
SUBJECT: GRB 140206A: Mondy optical observations
DATE:    14/02/08 16:11:34 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the afterglow (Oksanen et al., GCN 15786; Oates et al., GCN
15787) of the Swift/INTEGRAL/Fermi GRB 140206A (Lien et al., GCN 15784;
Gotz et al., GCN 15785, Kienlin et al., GCN 15796) with AZT-33IK 
telescope of Sayan observatory (Mondy) starting on Feb. 6 (UT) 14:15. 
We clearly detect afterglow in each frame of 60 s exposure. A 
preliminary photometry of the afterglow is following:

date        Filter  UT start  Exp,s     t-T0,d    OT     err
2014-02-06   R      14:15:21    120     0.29098   18.73  0.05
2014-02-06   R      14:31:29     60     0.30185   18.59  0.07
2014-02-06   R      15:02:15     60     0.32321   18.61  0.07
2014-02-06   R      18:14:26     60     0.45667   19.01  0.08
2014-02-06   R      18:53:29     60     0.48379   19.29  0.09

The photometry is based on reference stars SDSS-DR9, (R mag,
transformation by Lupton 2005)

N   SDSS_id           R(Lupton)errR
4 J094058.58+664752.4 18.030 0.022
5 J094107.93+664422.0 19.066 0.028


GRB_name: GRB140209A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15808
SUBJECT: GRB 140209A: Swift detection of a burst
DATE:    14/02/09 07:45:23 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

S. B. Cenko (GSFC), W. H. Baumgartner (GSFC/UMBC), V. D'Elia (ASDC),
L. Izzo (URoma/ICRA), H. A. Krimm (CRESST/GSFC/USRA),
A. Y. Lien (NASA/GSFC/ORAU), D. M. Palmer (LANL) and
E. Sonbas (NASA/GSFC/Adiyaman Univ.) report on behalf of the Swift
Team:

At 07:30:57 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140209A (trigger=586071).  The BAT on-board calculated location is 
RA, Dec 81.335, +32.477 which is 
   RA(J2000) = 05h 25m 20s
   Dec(J2000) = +32d 28' 37"
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 5 sec.  The peak count rate
was ~43000 counts/sec (15-350 keV), at ~2 sec after the trigger. 

Due to a Moon observing constraint, Swift cannot slew to the BAT
position until 04:37 UT on 2014 February 11. There will thus be no XRT
or UVOT data for this trigger before this time. 

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


GRB_name: GRB140209A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15809
SUBJECT: GRB 140209A: P60 optical afterglow detection
DATE:    14/02/09 09:29:44 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 alert 
for GRB 140209A (Cenko et al., GCN 15808) and began a sequence of 
60-second exposures in r, i, and z filters at 07:35:30 UT, 4.55 minutes 
after the BAT trigger.  In the reduced images, we clearly detect a 
fading, uncatalogued optical counterpart inside the BAT error circle at 
the following location:

RA  =  05:25:19.034
Dec = +32:29:53.18
(+/- 0.6 arcsec)

Calibrated relative to USNO-B1.0, the source fades steadily from R=17.6 
in the first r-band image to R=19.4 at 41.1 minutes post-GRB, which 
identifies it as the likely optical afterglow of this event.


GRB_name: GRB140209A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15810
SUBJECT: GRB 140209A: optical observations
DATE:    14/02/09 10:37:54 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed of  the field of  the Swift GRB 140209A (Cenko  et al.,  GCN 
15808)  with 0.4-m telescope of ISON-NM observatory starting on Feb., 9 (UT) 
07:43:39. Series of 30 s  unfiltered exposure were obtained. In the combined 
images we do not detect afterglow  reported by  Perley (GCN 15809).

However we detect possible object (#2) in coordinates (J2000) 05 25 25.55 
+32 27 57.2 (uncertainties of 1 arcsec) which is the BAT localization circle 
(Cenko  et al.,  GCN  15808) and not present on DSS2(R). The object was 
detected only on the combined image of first 10 frames, and not detected on 
later combine images.

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

UT mid,         Filter   Exposure,  OT (3 sigma upper limit),  object #2
                               s
07:45:32       none    10*30           > 18.7                           18.2 
+/- 0.2
07:58:47       none    10*30           > 18.4                            n/d
08:14:05       none    10*30           > 18.3                            n/d
 


GRB_name: GRB140209A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15811
SUBJECT: GRB 140209A: Fermi GBM observation
DATE:    14/02/09 17:58:11 GMT
FROM:    Andreas von Kienlin at MPE  <azk@mpe.mpg.de>

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

"At 07:30:58.23 UT on 09 February 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140209A (trigger 413623861 / 140209313),
which was also detected by the Swift/BAT (Cenko et al. 2014, GCN 15808).
The GBM on-ground location is consistent with the Swift position.

The trigger resulted in an Autonomous Repoint Request (ARR) that was
accepted and the spacecraft slewed to the GBM in-flight location. The
initial angle from the LAT boresight was 77 deg from the Fermi/GBM
position.

The GBM light curve consists of a bright pulse with a small precursor
at trigger time with a duration (T90) of about 1.4 s (50-300 keV).
The time-averaged spectrum from T0-0.192 s to T0+2.752 s is best fit by
a Band function with Epeak = 144 +/- 8 keV,
alpha = -0.56 +/- 0.06, and beta = -2.33 +/- 0.07.

The event fluence (10-1000 keV) in this time interval is
(9.5 +/- 0.2)E-06 erg/cm^2. The 0.064-sec peak photon flux measured
starting from T0+1.664 s in the 10-1000 keV band
is 120.5 +/- 3.4 ph/s/cm^2.

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


GRB_name: GRB140209A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15812
SUBJECT: GRB 140209A, Swift-BAT refined analysis
DATE:    14/02/09 19:27:41 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC),  W. H. Baumgartner (GSFC/UMBC),
S. B. Cenko (GSFC), 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-61 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140209A (trigger #586071)
(Cenko, et al., GCN Circ. 15808).  The BAT ground-calculated position is
RA, Dec = 81.328, 32.488 deg which is
    RA(J2000)  =  05h 25m 18.7s
    Dec(J2000) = +32d 29' 17.3"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 38%.

The mask-weighted light curve shows an initial weak pulse from T+0 to T+0.5 sec, 
followed by the main pulse from T+1.5 to T+3.5 sec, with a FRED-like profile 
with some superimposed structure.  This is followed by some low-level
extended emission out to ~T+50 sec.  T90 (15-350 keV) is 21.3 +- 8.0 sec 
(estimated error including systematics).

The time-averaged spectrum from T+0.15 to T+29.22 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.44 +- 0.06.  The fluence in the 15-150 keV band is 4.1 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+1.69 sec in the 15-150 keV band
is 38.1 +- 1.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

It is possible that this burst falls in the category of short burst with 
extended emission.
A lag analysis is underway that will be reported in a subsequent circular.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/586071/BA/


GRB_name: GRB140206A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15813
SUBJECT: GRB 140206A: Bassano Bresciano Observatory optical upper limit
DATE:    14/02/10 08:51:22 GMT
FROM:    Ulisse Quadri at Bassano Bresciano Obs  <oabb@ulisse.bs.it>

U.Quadri, L.Strabla and R.Girelli report:

We imaged the field of GRB 140206A detected by SWIFT(trigger 585834)
with the robotic telescope of (IAU station 565) Bassano Bresciano 
Observatory, Italy (member of ISSP:Italian Supernovae Search Project)

The observations started  85h 35m after the GRB trigger,  
with our schmidt telescope D=320/400 mm F/D=3.1.

Weather conditions were good.

We co-added 2 series of 15 exposures of 120 sec each.

We did not found any optical counterpart
in the error box of the XRTcandidate.
(Lien et. al GCN 15784 , Gotz et. al GCN 15784)

Start         End       Vlim
85h 35m     86h 47m     18.5

Magnitudes were estimated with the USNOB1.0 cat. 
and are not corrected for galactic dust extinction.

The images are available at:
http://www.osservatoriobassano.org/GRB.asp

The message may be cited.


GRB_name: GRB140209A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15814
SUBJECT: GRB 140209A: Swift-BAT Spectral lag analysis
DATE:    14/02/10 13:53:26 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. Norris (BSU), S. D. Barthelmy (GSFC), A. Lien (GSFC), C. Markwardt (GSFC),
T. Sakamoto (AGU), N. Gehrels (GSFC) report:

We report the spectral lag analysis for GRB 140209A (GCN Circ. 15808 & 15812)
based on the BAT data.  Using 4-ms binned light curve, the spectral lag
for the 25-50 keV to 100-350 keV bands is 28 (+10/-7) ms, and +34 (+8/-5) ms
for the 15-25 keV to 50-100 keV bands.  These lag values are consistant with a Long GRB.
Further, the extended emission is both shorter than the typical extended eimssion of a
Short GRB, and its shape is exponential in decay instead of more flat-like.
And lastly, there is pecursor emission.  The lag for the precursor
in the 15-25 keV to 50-100 keV bands is 150 (+36/-30) ms.


GRB_name: GRB140209A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15815
SUBJECT: GRB 140209A: Early RAPTOR Optical Detection
DATE:    14/02/10 19:32:06 GMT
FROM:    James Wren at LANL  <jwren@nis.lanl.gov>

J. Wren, W.T. Vestrand, P. Wozniak, and H. Davis,
of Los Alamos National Laboratory report:

The RAPTOR network of robotic optical telescopes made follow-up observations
of Swift trigger 586071 (Cenko, et al., GCN 15808).  Our narrow-field
instruments in Los Alamos, NM, began imaging at 07:31:24.33 UT,
26.5 seconds after the BAT trigger time.  We clearly detect the optical
counterpart (Perley, et al., GCN 15809).  Our first image at Tmid-Tbat=29.0s
shows the counterpart at an unfiltered magnitude of 14.43+-.04.  The
counterpart fades steadily to mag 15.50+-.08 by Tmid-Tbat=65.4s.  Our
unfiltered observations were calibrated to the USNO-B1 R-band.


GRB_name: GRB140211A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15816
SUBJECT: GRB 140211A: Swift detection of a burst
DATE:    14/02/11 12:39:09 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <jayc@milkyway.gsfc.nasa.gov>

J. R. Cummings (NASA/UMBC), M. M. Chester (PSU), V. D'Elia (ASDC),
L. Izzo (URoma/ICRA), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), C. B. Markwardt (NASA/GSFC),
K. L. Page (U Leicester) and R. L. C. Starling (U Leicester) report on
behalf of the Swift Team:

At 12:23:03 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140211A (trigger=586289).  Swift did not slew due to a 
Moon constraint.  The BAT on-board calculated location is 
RA, Dec 124.230, +20.244 which is 
   RA(J2000) = 08h 16m 55s
   Dec(J2000) = +20d 14' 37"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a broad
structure with a duration of about 20 sec.  The peak count rate
was ~1200 counts/sec (15-350 keV), at ~1 sec after the trigger. 

Due to a Moon observing constraint, Swift cannot slew to the BAT
position until 20:04 UT on 2014 February 14. There will thus be no XRT
or UVOT data for this trigger before this time. 

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


GRB_name: GRB140211A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15817
SUBJECT: GRB 140211A: MITSuME Okayama upper limits
DATE:    14/02/11 14:40:40 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 140211A (Cummings et al., GCNC 15816)
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 2014-02-11 12:24:38 UT (~96 sec after the burst).
We did not find any new point source within the BAT error circle
(Cummings et al., GCNC 15816) in all the three bands.

Three sigma upper limits of the OT are listed below.
We used SDSS DR7 catalog for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'     Rc     Ic
-----------------------------------------------------
0.00544    12:30:52     600.0   >18.2  >18.1  >17.4
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB140209A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15818
SUBJECT: Konus-Wind observation of GRB 140209A
DATE:    14/02/11 17:13:12 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

The bright GRB 140209A (Swift-BAT trigger #586071: Cenko et al., GCN 
15808, Palmer et al., GCN 15812; Fermi-GBM detection: von Kienlin, GCN 
15811) triggered Konus-Wind at T0=27060.493 s UT (07:31:00.493).

The burst light curve shows a double peaked pulse with a total duration 
of ~1.4 s. The emission is seen up to ~1 MeV.

As observed by Konus-Wind, the burst had a fluence of (7.2  0.6)x10^-6 
erg/cm2, and a 16-ms peak flux, measured from T0+0.280 s,
of (2.2  0.3)x10^-5 erg/cm2/s (both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+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 = -1.09(-0.21,+0.23)
and Ep = 173(-20,+15) keV (chi2 = 53.2/55 dof).
Fitting by GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy
photon index: beta < -2.8 (chi2 = 53.2/54 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140209_T27060/

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

All the quoted results are preliminary.


GRB_name: GRB140209A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15819
SUBJECT: GRB 140209A: Swift-XRT observations
DATE:    14/02/11 23:17:49 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

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

We have analysed 1.7 ks of XRT data for GRB 140209A (Cenko  et al. GCN
Circ. 15808),  from 188.1 ks to 195.5 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. Using 1439 s of PC mode
data and 1 UVOT images, we find an enhanced XRT position (using the
XRT-UVOT alignment and matching UVOT field sources to the USNO-B1
catalogue): RA, Dec = 81.32915, +32.49892 which is equivalent to:

RA (J2000): 05h 25m 19.00s
Dec(J2000): +32d 29' 56.1"

with an uncertainty of 3.0 arcsec (radius, 90% confidence). We cannot
determine at the present time whether the source is fading. The
position is consistent with that of the optical afterglow reported by
Perley (GCN Circ. 15809).


The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00586071.

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


GRB_name: GRB140211A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15820
SUBJECT: GRB 140211A: Swift-BAT refined analysis
DATE:    14/02/11 23:29:02 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+843 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 140211A (trigger #586289)
(Cummngs, et al., GCN Circ. 1816).  The BAT ground-calculated position is
RA, Dec = 124.233, 20.237 deg which is 
   RA(J2000)  =  08h 16m 56.0s 
   Dec(J2000) = +20d 14' 14.3" 
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 81%.
 
The mask-weighted light curve shows a single episode of emission starting
at ~T-30 sec, peaking at ~T=5 sec, and ending at ~T+135 sec.
T90 (15-350 keV) is 89.4 +- 18.7 sec (estimated error including systematics).
 
The time-averaged spectrum from T-16.84 to T+107.96 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.10 +- 0.14.  The fluence in the 15-150 keV band is 1.8 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+0.90 sec in the 15-150 keV band
is 0.7 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/586289/BA/


GRB_name: GRB140209A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15821
SUBJECT: GRB140209A: Swift/UVOT observations.
DATE:    14/02/12 12:43:35 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <m.depasquale@ucl.ac.uk>

M. De Pasquale (MSSL-UCL) & S. B. Cenko (GSFC) report on behalf of the 
Swift team:

Swift/UVOT started observations of GRB140209A (Cenko et al., GCN Circ. 
15808) 188.1
ks after the burst trigger.
No optical counterpart is detected at the position of XRT counterpart 
(D'Elia et al.,
GCN Circ 15819) and the P60 Source (Perley et al., GCN Circ 15809) in summed
exposures.

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

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

white    188075       195531      2689     >22.7

No correction has been made for the expected Galactic extinction 
corresponding
to E(B-V) = 0.03 in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB140209A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15822
SUBJECT: Correction to GCN 18521 "GRB140209A: Swift/UVOT observations"
DATE:    14/02/12 13:05:17 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <m.depasquale@ucl.ac.uk>

M. De Pasquale (MSSL-UCL) reports on behalf of the Swift team:

The reddening toward the direction of GRB 140209A quoted in GCN 15821
is actually not correct. The correct value is E(B-V) = 0.79.
We thank D. A. Kann  for pointing out the mistake.


GRB_name: GRB140211A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15824
SUBJECT: GRB140211A : Xinglong TNT upper limit
DATE:    14/02/13 03:37:15 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

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

We began to observe GRB 140211A  (  Cummings et al., GCN Cir. 15816)
with Xinglong 0.8-m TNT telescope at 12:25:29 (UT) , 146 sec after the burst,
under a bright sky background.

No any new object was detected within the BAT error circular 
(Cummings et al., GCNC 15816) in our combined images,
down to the upper limit of 16.0 mag in R band, calibrated by 
nearby USNO B1.0 R2 mag, at the mean time of 7.2 min after the burst.


GRB_name: GRB140213A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15825
SUBJECT: GRB 140213A: Swift detection of a burst
DATE:    14/02/13 19:36:48 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@swift.psu.edu>

S. T. Holland (STScI), V. D'Elia (ASDC), N. Gehrels (NASA/GSFC),
J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA), V. Mangano (PSU),
F. E. Marshall (NASA/GSFC), C. J. Mountford (U Leicester),
P. T. O'Brien (U Leicester), C. Pagani (U Leicester),
K. L. Page (U Leicester), J. L. Racusin (NASA/GSFC),
M. H. Siegel (PSU) and B.-B. Zhang (UAH) report on behalf of the Swift
Team:

At 19:21:37 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140213A (trigger=586569).  Swift did not slew to the burst immediately. 
The BAT on-board calculated location is 
RA, Dec 105.218, -73.136 which is 
   RA(J2000) = 07h 00m 52s
   Dec(J2000) = -73d 08' 10"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed two strong peaks 
starting at T-5, with a total duration of about 10 sec, followed by a 
third weaker pulse at T+15.  The peak count rate
was ~18,000 counts/sec (15-350 keV), at ~1 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+54.8
minutes. There will be no XRT or UVOT data until this time. 

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


GRB_name: GRB140213A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15826
SUBJECT: GRB 140213A: Swift/UVOT Detection
DATE:    14/02/13 20:37:37 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU) and S. T. Holland (STScI) report on behalf of the Swift/UVOT team:

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 3428 seconds after the BAT trigger on GRB 140213A (Holland et al., GCN Circ.
15825). There is a candidate afterglow in the rapidly available 2.7'x2.7' sub-image at
 RA(J2000)  = 07:00:37.09 = 105.15455
 DEC(J2000) = -73:08:13.5  = -73.13707
with a 90%-confidence error radius of about 0.62 arc sec. This position is 6.2
arc sec. from the center of the XRT error circle. The estimated magnitude is
17.74 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.15.


GRB_name: GRB140213A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15827
SUBJECT: GRB 140213A: Swift-XRT observations
DATE:    14/02/13 21:14:17 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

The XRT began observing the field of GRB 140213A at 20:18:43.0 UT,
3425.3 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source located at RA, Dec 105.15145,
-73.13570 which is equivalent to:
   RA(J2000)  = 07h 00m 36.35s
   Dec(J2000) = -73d 08' 08.5"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 69 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 (1.13 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 2.4
(+1.68/-1.51) x 10^21 cm^-2 (90% confidence). 


GRB_name: GRB140213A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15828
SUBJECT: GRB 140213A: Skynet R-COP Detection of Optical Afterglow
DATE:    14/02/13 23:29:52 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, J. Haislip, D. Reichart, A. LaCluyze, A. Verveer, T. Spuck, 
A. Foster, N. Frank, K. Ivarsen, J. Moore, M. Nysewander, R. Beauchemin, 
T. Berger, M. Carroll, H. T. Cromartie, R. Egger, M. Hinckle, A. 
Ireland, M. Maples, L. Scott, and J. A. Crain report:

Skynet observed the Swift-BAT localization of GRB 140213A (Holland et 
al., GCN 15825, Swift trigger 586569) with the 14-inch R-COP telescope 
at Perth Observatory, Australia.  Observations began at 59s and 
continued until 92m post-trigger, with rotating exposures in the BVRI 
bands increasing from 10s to 80s. We detect a fading optical source in 
all bands at the position of the source detected by the Swift UVOT 
(Siegel & Holland, GCN 15826). The source faded from R=14.3 at t=113s to 
R=17.8 at t=73m.

A preliminary light curve is at:
http://www.skynet.unc.edu/grb/grb140213a.png 
<https://outlook.unc.edu/owa/redir.aspx?C=y2fEeVtlHEGuQvMGxBu8RSnt2Tap_NAIeyK3ME-qCZACrK94N0zj_7W5zZXZpIb5kE5UKcCeXkY.&URL=http%3a%2f%2fwww.skynet.unc.edu%2fgrb%2fgrb140213a.png>

Photometry is calibrated to five APASS-DR7 stars in the field, and has 
not been corrected for the Galactic foreground extinction corresponding 
to E(B-V)=0.07 (Schlegel et al. 1998).

Skynet observations are ongoing.


GRB_name: GRB140213A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15829
SUBJECT: GRB 140213A: GROND Detection of the Optical/NIR Afterglow
DATE:    14/02/14 01:45:51 GMT
FROM:    Jonny Elliott at MPE/GROND  <jonnyelliott@mpe.mpg.de>

J. Elliott, K. Varela (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 140213A (Swift trigger 586569; Holland et
al., GCN #15825) 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 00:25 UT on 14 February 2014, 5 hours after the
GRB trigger, and are continuing. They were performed at an average seeing
of 1.9" and at an average airmass of 1.4.

We find a single point source within the 0.4" Swift-UVOT error circle
reported by Siegel & Holland (GCN #15826) and confirmed by Trotter et al.
(GCN #15828).

Based on the first 4.4 min of total exposures in g'r'i'z' and 4 min in
JHK, we estimate preliminary magnitudes (all in AB) of

g' = 19.7 +/- 0.1 mag,
r' = 19.4 +/- 0.1 mag,
i' = 19.2 +/- 0.1 mag,
z' = 19.1 +/- 0.1 mag,
J  = 18.7 +/- 0.1 mag,
H  = 18.5 +/- 0.1 mag, and
K  = 18.4 +/- 0.1 mag.

The spectral energy distribution is best-fit by a straight power-law with
spectral slope b = 0.8 +/- 0.1.

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)=0.07 mag in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB140213A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15830
SUBJECT: GRB 140213A: Enhanced Swift-XRT position
DATE:    14/02/14 03:11:19 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 3106 s of XRT Photon Counting mode data and 7 UVOT
images for GRB 140213A, 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 = 105.15491, -73.13725 which is equivalent
to:

RA (J2000): 07h 00m 37.18s
Dec (J2000): -73d 08' 14.1"

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: GRB140213A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15831
SUBJECT: GRB140213A: VLT/X-shooter redshift
DATE:    14/02/14 04:01:39 GMT
FROM:    Steve Schulze at U of Iceland  <sts30@hi.is>

S. Schulze (PUC and MCSS), K. Wiersema (U. Leicester), D. Xu, and J. P. U. Fynbo (DARK/NBI) report on behalf of a larger collaboration:
 
We observed the optical counterpart of GRB 140213A (Holland et al., GCN 15825; Siegel et al., GCN 15826) with the ESO VLT equipped with the X-shooter spectrograph starting 5.8 hr after the GRB. The spectrum covers the wavelength range from 3,200 to 18,000 AA. The afterglow is well detected throughout. We detect several absorption features, which we interpret as due to Fe II, Mg I, Mg II, Al II, Al III and others, at a common redshift of z = 1.2076 (wavelength solution based on archival calibration lamps).
 
We acknowledge excellent support from the observing staff in Paranal, in particular Yazan Momany.


GRB_name: GRB140213A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15832
SUBJECT: GRB 140213A: Swift-XRT refined Analysis
DATE:    14/02/14 06:42:39 GMT
FROM:    Claudio Pagani at U of Leicester  <cp232@star.le.ac.uk>

C. Pagani (U. Leicester), K. L. Page (U. Leicester) and S. T. Holland
(STScI) report on behalf of the Swift-XRT team:

We have analysed 5.0 ks of XRT data for GRB 140213A (Holland  et al.
GCN Circ. 15825),  from 3.4 ks to 22.3 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Beardmore et al. (GCN Circ.
15830).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.04 (+/-0.06).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.91 (+/-0.08). The
best-fitting absorption column is  1.4 (+1.0, -0.9) x 10^21 cm^-2, at a
redshift of 1.2076, in addition to the Galactic value of 1.1 x 10^21
cm^-2 (Kalberla et al. 2005). The counts to observed (unabsorbed)
0.3-10 keV flux conversion factor deduced from this spectrum  is 3.9 x
10^-11 (5.2 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 1.1 x 10^21 cm^-2
Intrinsic column:    1.4 (+1.0, -0.9) x 10^21 cm^-2 at z=1.2076
Photon index:      1.91 (+/-0.08)

If the light curve continues to decay with a power-law decay index of
1.04, the count rate at T+24 hours will be 0.085 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.4 x
10^-12 (4.4 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/00586569.

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


GRB_name: GRB140213A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15833
SUBJECT: GRB 140213A: Fermi GBM Detection
DATE:    14/02/14 17:49:06 GMT
FROM:    Binbin Zhang at UAH  <binbin.zhang@uah.edu>

Bin-Bin Zhang (UAH) reports on behalf of the Fermi GBM Team:

"At 19:21:32.35 UT on February 13 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located  GRB 140213A (trigger 414012095/140213807), which was also
detected by Swift (Holland et al., GCN 15825). The GBM on-ground location
is consistent with the Swift/XRT position (Evans et al., GCN 15827).

The trigger resulted in an Autonomous Repoint Request (ARR) that was
accepted and the spacecraft slewed to the GBM in-flight location. The
pre-ARR angle from LAT boresight was 48.5 deg from the Swift/XRT
position.

The GBM light curve consists of a multiple-peak structure with a duration
of about 18.6 s (50-300 keV). The time-averaged spectrum from T0+0 s to T0+19 s
is well fit with a Band function parameterized as Epeak = 80 +/- 2 keV, 
alpha = -1.01 +/- 0.03 and beta=-2.41 +/-0.04. The event fluence (10-1000 keV) 
in this time interval is (2.04 +/- 0.03)E-05 erg/cm^2. The 1.0-sec peak photon 
flux measured starting from T0+6 s in the 10-1000 keV band is 37 +/- 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: GRB140213A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15834
SUBJECT: GRB 140213A: Swift/UVOT Observations
DATE:    14/02/14 21:45:33 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU) and S. T. Holland (STScI) report on behalf of the
Swift/UVOT team:

The Swift/UVOT has continued to observe GRB 140213A (Holland
et al., GCN 15825).  We find that the optical afterglow is slowly fading
but still detected in all UVOT filters as of 68 ks after the BAT trigger.

The preliminary UVOT position is:
   RA  (J2000) =  07:00:37.13 = 105.15472 (deg.)
   Dec (J2000) = -73:08:13.5  = -73.13707 (deg.)
with an estimated uncertainty of 0.51 arc sec. (radius, 90% confidence).

Preliminary detections 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 (fc)   3428         3578         147       17.70+-0.04
white        4610         4809         196       18.08+-0.05
v            3584         3784         196       18.03+-0.12
v            9217        10124         885       19.06+-0.13
v           27349        28053         685       19.73+-0.35
b            4405         4605         196       18.40+-0.09
b           61868        62291         412       19.52+-0.13
u (fc)       4200         4399         196       17.40+-0.06
u           21642        22285         625       18.81+-0.11
u           60956        61863         885       18.91+-0.08
uvw1         3995         4194         196       17.65+-0.10
uvw1        14948        21635        1242       18.79+-0.08
uvm2         3789         3989         196       17.77+-0.14
uvm2        10129        10771         632       18.52+-0.12
uvm2        33470        49991        1348       19.47+-0.14
uvm2        66689        67589         885       19.26+-0.15
uvw2         4816         5012         193       18.46+-0.17
uvw2        26443        27343         885       20.06+-0.21

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.15 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB140206A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15835
SUBJECT: GRB140206A: Discovery Channel Telescope Optical Detection
DATE:    14/02/14 21:57:28 GMT
FROM:    Vicki Toy at UMD  <vtoy@astro.umd.edu>

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


We observed the field of GRB140206A (Swift trigger 585834, Lien et al., GCN
15784) with the Large Monolithic Imager (LMI) on the recently commissioned
4.3m Discovery Channel Telescope (DCT) at Happy Jack, AZ from 2014/02/13
5:33 to 2014/02/13 6:03 UTC (mean epoch of 6.9 d after the Swift trigger).


A source is clearly detected at the location of the optical afterglow
(Oksanen et al, GCN 15786).  Using nearby point sources from SDSS for
calibration, we measure r' = 21.69 +/- 0.07 (AB).  This value is not
corrected for Galactic extinction in the direction of the GRB.


We thank the staff of the Discovery Channel Telescope for assistance with
these observations.


GRB_name: GRB140213A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15836
SUBJECT: GRB 140213A: Swift-BAT refined analysis
DATE:    14/02/14 21:59:51 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), S. T. Holland (STScI),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/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-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140213A (trigger #586569)
(Holland, et al., GCN Circ. 15825).  The BAT ground-calculated position is
RA, Dec = 105.166, -73.136 deg which is
    RA(J2000)  =  07h 00m 39.8s
    Dec(J2000) = -73d 08' 10.8"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 50%.

The mask-weighted light curve begins at T-120 sec, when the source position
came into the BAT field-of-view during a pre-planned slew.  The emission
begins faintly at ~T-25 sec, and rises sharply beginning at ~T-5.5 sec,
peaks at T-4 sec and a stronger peak at ~T+1 sec, returning almost to baseline
around T+10 sec. Then there is a second, much weaker and softer pulse
at around T+15 sec, followed by an even weaker pulse at ~T+70 sec,
with extended emission out to ~T+160 sec.  The burst position left
the FoV after another pre-planned slew at T+780 sec. T90 (15-350 keV) is 60.0 +- 
2.6 sec (estimated error including systematics).

The time-averaged spectrum from -5.7 to +82.0 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.80 +- 0.04.  The fluence in the 15-150 keV band is 1.2 +- 0.0 x 10^-5 erg/cm2.
The 1-sec peak photon flux measured from T+0.56 sec in the 15-150 keV band
is 23.5 +- 0.8 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/586569/BA/


GRB_name: GRB140215A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15837
SUBJECT: GRB 140215A: Swift detection of a burst with optical counterpart
DATE:    14/02/15 04:16:28 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

C. B. Markwardt (NASA/GSFC), S. D. Barthelmy (GSFC),
L. M. Z. Hagen (PSU), J. A. Kennea (PSU), V. Mangano (PSU),
F. E. Marshall (NASA/GSFC), C. J. Mountford (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL) and M. H. Siegel (PSU)
report on behalf of the Swift Team:

At 04:07:10 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140215A (trigger=586680).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 104.136, +41.780 which is 
   RA(J2000)  =  06h 56m 33s
   Dec(J2000) = +41d 46' 49"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a couple of overlapping
FRED-like peaks with a duration of about 25 sec.  The peak count rate
was ~4500 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 04:09:08.0 UT, 117.7 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 104.1489, 41.7858 which is equivalent to:
   RA(J2000)  = +06h 56m 35.74s
   Dec(J2000) = +41d 47' 08.9"
with an uncertainty of 6.1 arcseconds (radius, 90% containment). This
location is 40 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 6.19e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 125 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 06:56:35.83 = 104.14928
  DEC(J2000) = +41:47:11.8  =  41.78660
with a 90%-confidence error radius of about 0.74 arc sec. This position is 3.1
arc sec. from the center of the XRT error circle. The estimated magnitude is
15.08 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.09. 

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


GRB_name: GRB140215A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15838
SUBJECT: GRB140215A: Prompt Observations with Discovery Channel Telescope
DATE:    14/02/15 04:34:40 GMT
FROM:    S. Bradley Cenko at NASA/GSFC  <brad.cenko@nasa.gov>

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

We imaged the location of the Swift GRB140215A (Markwardt et al., GCN 15837) with
the Large Monolithic Imager mounted on the 4.3m Discovery Channel Telescope.
Observations began at 4:09:50 UT on 15 February 2014, ~ 2.7 min after the
Swift BAT trigger time, and were taken under sub-optimal conditions (moderate
cloud cover and bright moon).

We detect the bright optical afterglow in individual exposures beginning at
this time.  Using several nearby point sources from USNO-B1 reference, we measure
a magnitude of r' ~ 13.5 mag in our first exposure.  Multi-color observations are
ongoing.

We thank the entire staff of the Discovery Channel Telescope for assistance with
these observations.


GRB_name: GRB140215A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15839
SUBJECT: GRB 140215A: KAIT Optical Detection
DATE:    14/02/15 04:50:23 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 140215A (Markwardt et al.,
GCN 15837) starting at 04:09:02 UT, 112 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. We detect the bright optical afterglow (Markwardt
et al., GCN 15837; Cenko et al., GCN 15838) in all the individual
images. The afterglow decayed from mag~13.7 (mid t-t0=189s) to
mag~15.9 (mid t-t0=1094s) in our clear band images calibrated to
USNO B1.0 catalog. Observations are on going.


GRB_name: GRB140215A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15840
SUBJECT: GRB140215A: Skynet PROMPT Optical Observations
DATE:    14/02/15 05:45:47 GMT
FROM:    Aaron LaCluyze at U.North Carolina  <lacluyze@email.unc.edu>

A. LaCluyze, J. Haislip, D. Reichart, A. Trotter, A. Foster, N. Frank, K. Ivarsen, J. Moore, M. Nysewander, R. Beauchemin, T. Berger, M. Carroll, H. T. Cromartie, R. Egger, M. Hinckle, A. Ireland, M. Maples, L. Scott, and J. A. Crain report:

Skynet observed the Swift-BAT localization of GRB 140215A (Markwardt et al., GCN 15837, Swift trigger 586680) with six of the PROMPT telescopes located at CTIO in Chile.  Observations began at ~59s after the burst in BVRI and luminance. We detect a fading optical source in all bands at the position of the source detected by Markwardt et al.

A preliminary light curve calibrated to USNOB and NOMAD catalog stars can be found at:
http://www.skynet.unc.edu/grb/grb140215a.png

Further observations are ongoing.


GRB_name: GRB140215A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15841
SUBJECT: GRB 140215A: RATIR Optical and NIR Observations
DATE:    14/02/15 05:53:42 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB),
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara
(ORAU/GSFC), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), 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 140215A (Markwardt, et al., GCN 15837) with
the Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on
the 1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional
on Sierra San Pedro Mrtir beginning 110 seconds after the Swift BAT
trigger.  Initial data were taken out-of-focus, and will require special
handling.  In-focus data were acquired from 2014/02 15.20 to 2014/02
15.22UTC (0.65 to 1.13 hours after the BAT trigger), corresponding to
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.

For a source within the Swift UVOT error circle, in comparison with 2MASS,
we obtain the following detections:

  r     17.45 +/- 0.01
  i     17.08 +/- 0.01
  Z     16.82 +/- 0.01
  Y     16.55 +/- 0.02
  J     16.34 +/- 0.01
  H     16.05 +/- 0.01

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 Astronmico Nacional in San Pedro
Mrtir.  Further observations are ongoing.


GRB_name: GRB140215A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15842
SUBJECT: GRB 140215A: Enhanced Swift-XRT position
DATE:    14/02/15 08:38:14 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 2359 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 140215A, 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 = 104.14917, +41.78625 which is equivalent
to:

RA (J2000): 06h 56m 35.80s
Dec (J2000): +41d 47' 10.5"

with an uncertainty of 1.7 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB140215A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15843
SUBJECT: GRB 140215A: T24 optical observations
DATE:    14/02/15 11:01:22 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 140215A optical afterglow at iTelescope observatory
T24 (Auberry, California) using 0.61-m/6.5 astrograph and FLI-PL09000
CCD camera. The observations were started at 2014-02-15 04:33:26 (UT)
and stopped at 06:05:49 (UT). Fourteen photometric V filter images and eight
unfiltered images with different exposure time were made.

The afterglow was detected at the following position RA 06:56:35.84 and
DEC +41:47:11.5.

The following magnitudes were obtained from the observations using
NOMAD1 1317-0185429 (V= 13.190 and R=13.190) as a comparison star:

Tmid(s)+T0    Filter         Exp. time      Mag              Mag err.
1107              V              3x60s           17.00V          0.12
2090              V              3x120s         17.30V          0.13
3283              V              3x60s           17.96V          0.34
3678              V              3x120s         17.97V          0.21
4496              V              2x300s         18.44V          0.20
5817              unfiltered   3x60s           18.67CR        0.32
6224              unfiltered   3x120s         18.89CR        0.25
6797              unfiltered   2x300s         19.07CR        0.21

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GRB_name: GRB140215A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15844
SUBJECT: GRB 140215A: P60 observations
DATE:    14/02/15 11:03:31 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

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

The Swift-BAT alert for GRB 140215A (Markwardt et al., GCN 15837) 
automatically triggered the Palomar 60-inch telescope, which slewed to 
the position and began started a sequence of r, i, and z images 
beginning at 04:09:54 UT, 2.74 minutes after the initial trigger.  The 
optical afterglow is well-detected in all images and filters, and 
follow-up has continued through to the present time.  The afterglow 
light curve fades as a simple unbroken power-law with a decay index of 
alpha=1.19 throughout this period.  Calibrating relative to USNO-B1.0, 
we estimate a magnitude (in the most recent imaging, at 387 minutes 
post-trigger) of R = 19.93 +/- 0.13 mag.

Spectroscopic follow-up is encouraged.


GRB_name: GRB140215A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15845
SUBJECT: GRB 140215A: Swift-XRT refined Analysis
DATE:    14/02/15 16:18:01 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page (U. Leicester) and C. B. Markwardt (NASA/GSFC) report on
behalf of the Swift-XRT team:

We have analysed 7.8 ks of XRT data for GRB 140215A (Markwardt et al.
GCN Circ. 15837),  from 124 s to 18.2 ks after the BAT trigger. The
data comprise 159 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. 15842).

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

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.49 (+0.12, -0.07). The
best-fitting absorption column is  consistent with the Galactic value
of 9.7 x 10^20 cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a
photon index of 1.91 (+0.18, -0.17) and a best-fitting absorption
column of 1.7 (+/-0.5) x 10^21 cm^-2. The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 4.0 x 10^-11 (5.4 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.7 (+/-0.5) x 10^21 cm^-2
Galactic foreground: 9.7 x 10^20 cm^-2
Excess significance: 2.5 sigma
Photon index:      1.91 (+0.18, -0.17)

If the light curve continues to decay with a power-law decay index of
1.21, the count rate at T+24 hours will be 5.1 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.0 x
10^-13 (2.8 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00586680.

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


GRB_name: GRB140215A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15846
SUBJECT: GRB 140215A: ISON-NM optical observations
DATE:    14/02/15 20:32:45 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 140215A (Markwardt et al.,  GCN 
15837)  with 0.4-m telescope of ISON-NM observatory starting on Feb., 15 
(UT)  04:08:22, i.e 72 seconds after  Swift burst trigger.  We took 35 
unfiltered images of 30 s exposures. We clearly detect the bright optical 
afterglow of GRB 140215A (Markwardt et al.,  GCN 15837; Cenko et al., GCN 
15838) in each separate image.  Coordinates of the optical afterglow 
(J2000) 06 56 35.83 +41 47 11.4 (uncertainties of 0.5 arcsec) coincide with 
OT coordinates (Markwardt et al.,  GCN 15837). Preliminary photometry  is 
following:

UT mid,      T0+        Filter    Exposure,  OT,    err OT
                  mid                   s
04:08:22      0.00101 none    30            13.60   0.03
04:37:01      0.02090 none    30            16.46   0.20

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

N USNO-B1.0id RA                Dec           R2
1 1318-0183851 06:56:13.01 +41:49:29.2 12.37
2 1317-0181981 06:56:37.13 +41:44:34.4 14.39
3 1317-0181986 06:56:38.48 +41:44:12.8 14.50

The power law index of  ~-1.2 of  our light curve starting from 0.0025 days 
and up to the end of our observations coincides with the index reported by 
Perley and Cenko  (GCN 15844). 


GRB_name: GRB140215A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15847
SUBJECT: GRB 140215A: Swift-BAT refined analysis
DATE:    14/02/15 22:06:04 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), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+824 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 140215A (trigger #586680)
(Markwardt, et al., GCN Circ. 15837).  The BAT ground-calculated position is
RA, Dec = 104.129, 41.787 deg, which is 
   RA(J2000)  =  06h 56m 31.0s 
   Dec(J2000) = +41d 47' 12.2" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 15%.
 
The mask-weighted light curve shows several overlapping peaks starting 
at ~T-15 sec, peaking at ~T+1 sec, and ending at ~T+180 sec.
T90 (15-350 keV) is 84.2 +- 53.1 sec (estimated error including systematics).
 
The time-averaged spectrum from T-1.47 to T+181.76 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.19 +- 0.08.  The fluence in the 15-150 keV band is 7.8 +- 0.3 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-0.01 sec in the 15-150 keV band
is 7.9 +- 0.7 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/586680/BA/


GRB_name: GRB140215A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15848
SUBJECT: GRB 140215A: MITSuME Okayama Optical Observation
DATE:    14/02/16 02:19:26 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 140215A (Markwardt et al., GCNC 15837)
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 2014-02-15 10:03:22 UT (~5.9 h after the burst).
We detected the previously reported afterglow (Markwardt et al., GCNC 15837;
Cenko et al., GCNC 15838) in Rc and Ic bands.

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

#T0+[day]  MID-UT    T-EXP[sec]   g'     Rc  Rc_err   Ic  Ic_err
------------------------------------------------------------------
0.26209    10:24:34    2880.0   >19.6   18.9  0.2    18.6  0.3
------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB140215A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15849
SUBJECT: GRB 140215A: Continued RATIR Optical and NIR Observations
DATE:    14/02/16 17:45:42 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 again observed the field of GRB 140215A (Markwardt, et al.,
GCN 15837) 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
2014/02 16.20 to 2014/02 16.36 UTC (24.65 to 28.57 hours after the
BAT trigger), obtaining a total of 2.18 hours exposure in the r and
i bands and 0.88 hours exposure in the Z, Y, J, and H bands.

We continue to detect the previously reported source in all bands, at
fainter magnitudes than the previous epoch of RATIR observations (Butler
et al., GCN 15841). In comparison with 2MASS, we obtain the following
detections:

  r     21.51 +/- 0.11
  i     21.19 +/- 0.10
  Z     21.37 +/- 0.24
  Y     20.68 +/- 0.21
  J     20.69 +/- 0.16
  H     20.43 +/- 0.18

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 the source has faded with
approximate power-law index of t^-1 in all bands.

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


GRB_name: GRB140215A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15850
SUBJECT: GRB140215A: Continued Discovery Channel Telescope Observations
DATE:    14/02/16 18:08:36 GMT
FROM:    Vicki Toy at UMD  <vtoy@astro.umd.edu>

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

We re-observed the bright optical afterglow of GRB140215A (Swift trigger
586680, Markwardt et al., GCN 15837, Cenko et al., GCN 15840) with the
Large Monolithic Imager (LMI) on the 4.3m Discovery Channel Telescope (DCT)
at Happy Jack, AZ from 2014/02/16 2:55 to 2014/02/16 4:05 UTC (0.95-1.0
days after the Swift-BAT trigger) in the g',r',i', and z' filters.

Compared with our previous observations, the afterglow continues to follow
an unbroken power law with decay index of alpha=-1.20 in all filters
(Perley et al., GCN 15844, and Elenin et al., GCN 15846), consistent with
the simultaneous temporal decay observed in the X-rays (Page et al., GCN
15845).  Specifically we measure r' = 21.6 mag (AB) at a time of 23.5 hr
after the trigger, calibrating relative to USNO-B1.

We thank the entire staff of the Discovery Channel Telescope for assistance
with these observations.


GRB_name: GRB140211A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15851
SUBJECT: GRB 140211A: Swift-XRT and UVOT observations
DATE:    14/02/16 18:51:10 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

M. De Pasquale (MSSL-UCL), V. D'Elia (ASDC),  L. Izzo (Uroma/ICRA) and  
J. R. Cummings (NASA/UMBC) report on behalf of the Swift-XRT team:


We have analysed 2.7 ks of XRT data for GRB 140211A (Cummings et al.  
GCN Circ. 15816), from 298.7 ks to 385.2 ks after the BAT trigger.  
The data are entirely in Photon Counting (PC) mode. The refined XRT  
position is RA, Dec = 124.22331, +20.2432 which is equivalent to:

RA (J2000): 08 16 53.59
Dec(J2000): +20 14 35.5

with an uncertainty of 4.4 arcsec (radius, 90% confidence). We cannot  
determine at the present time whether the source is fading.


The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00586289.

UVOT performed observations of GRB140211A in UVM2 and UVW1. At the  
position of the XRT source, no counterpart is detected in these  
filters in summed 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
um2   298690    298860    167    >19.5
uw1    338330   385245   2438    >21.3

No correction has been made for extinction corresponding to  
E(B-V)=0.04 (Schlegel et al 1998).

This circular is an official product of the Swift team.

----------------------------------------------------------------
This message was sent using IMP, the Internet Messaging Program.


GRB_name: GRB140215A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15852
SUBJECT: GRB 140215A: Swift/UVOT Detection
DATE:    14/02/17 00:15:50 GMT
FROM:    Lea Hagen at PSU  <lea.zernow.hagen@gmail.com>

L. M. Z. Hagen (PSU) and C. B. Markwardt (NASA/GSFC) report on behalf of
the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140215A 126 s
after the BAT trigger (Markwardt et al., GCN Circ. 15837). A source
consistent with the XRT position (Evans et al. GCN Circ. 15842) is detected
in the initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  06:56:35.81 = 104.14920 (deg.)
    Dec (J2000) = +41:47:11.7  =  41.78659 (deg.)
with an estimated uncertainty of 0.50 arc sec. (radius, 90% confidence).

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

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

white (fc)         125          275          147         15.01 +/- 0.04
white              617          637           19         16.26 +/- 0.07
v                  106          117           10         14.34 +/- 0.09
b                  593          612           19         16.19 +/- 0.09
u                  337          587          245         15.53 +/- 0.05
w1                4611         4811          196        >19.86
m2                4406         4606          196        >19.51
w2                 642          662           19        >17.93

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). We note that the white photometry may be affected
by a nearby bright foreground star.


GRB_name: GRB140215A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15853
SUBJECT: Konus-Wind observation of GRB 140215A
DATE:    14/02/17 15:10:00 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration GRB 140215A
(Swift-BAT trigger 586680: Markwardt et al., GCN 15837;
Barthelmy et al., GCN 15847)
triggered Konus-Wind at T0=14831.638 s UT (04:07:11.638).

The burst light curve shows a multi-peaked with a total duration of ~15 s.
The emission is seen up to ~10 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140215_T14831/

As observed by Konus-Wind, the burst
had a fluence of (1.84  0.15)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+4.800 s,
of (3.57  0.35)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+15.360 s)
is best fit in the 28 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.66  0.11,
the high energy photon index beta = -2.94  0.35,
the peak energy Ep = 214  14 keV,
chi2 = 106/95 dof.

The spectrum near the maximum count rate
(measured from T0 to T0+7.168 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 = -0.46  0.12,
the high energy photon index beta = -2.83  0.26,
the peak energy Ep = 212  14 keV,
chi2 = 92.9/96 dof.

All the quoted values are preliminary.


GRB_name: GRB140213A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15854
SUBJECT: Konus-Wind observation of GRB 140213A
DATE:    14/02/17 17:07:06 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration GRB 140213A
(Swift-BAT trigger 586569: Holland et al., GCN 15825;
Stamatikos et al., GCN 15836;
Fermi GBM Detection: Zhang, GCN 15833)
triggered Konus-Wind at T0=69693.011 s UT (19:21:33.011).

The burst light curve shows a bright, double-peaked pulse with
a total duration of ~16 s followed by a weaker emission during
the next ~50 s.
The emission is seen up to ~12 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140213_T69693/

As observed by Konus-Wind, the burst
had a fluence of (1.57  0.09)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+1.344 s,
of (4.10  0.40)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+16.640 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 = -1.39  0.06,
the high energy photon index beta = -3.55  0.88,
the peak energy Ep = 100  4 keV,
chi2 = 142/97 dof.

The spectrum near the maximum count rate
(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 = -0.46  0.12,
the high energy photon index beta = -3.28  0.40,
the peak energy Ep = 108  4 keV,
chi2 = 137/97 dof.

Assuming the redshift z=1.2076 (Schulze et al., GCN 15831),
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 (6.2  0.4)x10^52 erg,
the peak luminosity L_iso is (3.6  0.4)x10^52 erg/s,
and the rest-frame peak energy Ep,i = (221  8) keV

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


GRB_name: GRB140215A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15855
SUBJECT: GRB 140215A: Continued RATIR Optical and NIR Observations
DATE:    14/02/17 17:12:25 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 140215A (Markwardt,, et al., GCN 15837)
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 2014/02 17.11 to 2014/02 17.20 UTC
(46.46 to 48.60 hours after the BAT trigger), obtaining a total of 1.41
hours exposure in the r and i bands and 0.58 hours exposure in the Z, Y, J,
and H bands.

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

  r     22.19 +/- 0.24
  i     21.65 +/- 0.16
  Z     > 21.45
  Y     > 20.71
  J     > 20.61
  H     > 20.12

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 15849), the source flux is consistent with a
continued fading as t^-1.


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


GRB_name: GRB140211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15856
SUBJECT: GRB 140211A: Khureltogot optical upper limits
DATE:    14/02/17 20:00:50 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), N. Tungalag (Research Centre of Astronomy and 
Geophysics MAS), S. Schmalz (AIP), V. Voropaev (KIAM), I.Molotov (KIAM), 
A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration:

We observed the field of the Swift Swift GRB 140211A (Cummings et al., 
GCN 15816) with ORI-40 telescope of Khureltogot observatory (Mongolia) 
starting on Feb., 11 (UT) 12:29:12, i.e., ~6 minutes after the trigger. 
We took several unfiltered images of 60 s exposure. Within the enhanced 
BAT error circle (Cummings et al., GCN 15820) we do not detect any 
optical counterpart in differently stacked images.

Details of the photometry are following:

UT start-end        t-T0       Exp.   Filter  OT    UL (3 sigma)
                    (mid, days) (s)
12:29:12-12:30:12   0.00450    1*60   None    n/d    17.0
12:29:12-12:40:31   0.00819   10*60   None    n/d    18.0
12:29:12-15:18:33   0.10468  100*60   None    n/d    18.8

The photometry is based on reference stars SDSS-DR9, (R mag,
transformation by Lupton 2005):

N   SDSS_id               R(Lupton)
1   J081706.72+201335.6   18.171
2   J081655.77+201624.8   18.078


GRB_name: GRB140215A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15857
SUBJECT: GRB 140215A: WSRT radio observation
DATE:    14/02/18 09:22:49 GMT
FROM:    Alexander van der Horst at U of Amsterdam  <A.J.vanderHorst@uva.nl>

A.J. van der Horst (University of Amsterdam) reports on behalf
of a large collaboration:

"We observed the position of the GRB 140215A afterglow at 4.9 GHz with
the Westerbork Synthesis Radio Telescope at February 17 14.69 UT to
February 18 02.66 UT, i.e. 2.44 - 2.94 days after the burst (GCN 15837).
We do not detect a radio source at the position of the optical
counterpart (GCN 15852). The three-sigma rms noise in the map around
that position is 126 microJy per beam. The formal flux measurement for
a point source at the position of the optical counterpart is 51 +/- 42
microJy.

We would like to thank the WSRT staff for scheduling and obtaining
these observations."


GRB_name: GRB140215A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15858
SUBJECT: GRB 140215A: Continued Skynet PROMPT Observations of the Optical Afterglow
DATE:    14/02/18 15:48:45 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. LaCluyze, J. Haislip, D. Reichart, A. Trotter, S. Poshyachinda, W. 
Rujopakarn, A. Foster, N. Frank, K. Ivarsen, J. Moore, M. Nysewander, R. 
Beauchemin, T. Berger, M. Carroll, H. T. Cromartie, R. Egger, M. 
Hinckle, A. Ireland, M. Maples, L. Scott, and J. A. Crain report:

Skynet continued observing the Swift-BAT localization of GRB 140215A 
(Markwardt et al., GCN 15837, Swift trigger 586680) with six of the 
PROMPT telescopes located at CTIO in Chile.  LaCluyze et al. (GCN 15840) 
described rapid-response observations of a fading optical afterglow 
taken between ~1m and 6.5m after the burst in BVRI and luminance, and 
presented a preliminary light curve calibrated to USNOB and NOMAD 
catalog stars. A revised and recalibrated light curve, including 
observations taken at t~20-24h, is at:

http://www.skynet.unc.edu/grb/grb140215a_2.png

In stacks of ~45x160s images from the second night, we do not detect the 
afterglow with any degree of confidence (the I-band "detections" in the 
light curve plot are most likely spurious.) The 3-sigma limiting 
magnitudes are:

Band      tmid      Limit
I         21.9h     >20.2
R         21.0h     >20.5
V         21.8h     >20.5
B         21.7h     >20.3

Magnitudes are in the Vega system, and were calibrated to 4 APASS DR7 
catalog stars in the field. They have not been corrected for 
line-of-sight MW dust extinction corresponding to E(B-V)=0.09 (Schlegel 
et al. 1998).

No further Skynet observations are scheduled.


GRB_name: GRB140213A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15859
SUBJECT: GRB 140213A: Continued Skynet R-COP/PROMPT Detections of a Rebrightening Optical Afterglow
DATE:    14/02/18 18:25:08 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, J. Haislip, D. Reichart, A. LaCluyze, A. Verveer, T. Spuck, 
A. Foster, N. Frank, K. Ivarsen, J. Moore, M. Nysewander, R. Beauchemin, 
T. Berger, M. Carroll, H. T. Cromartie, R. Egger, M. Hinckle, A. 
Ireland, M. Maples, L. Scott, and J. A. Crain report:

Skynet continued observing the Swift-BAT localization of GRB 140213A 
(Holland et al., GCN 15825, Swift trigger 586569) with the 14-inch R-COP 
telescope at Perth Observatory, Australia, and with 4 16-inch telescopes 
of the PROMPT array at CTIO, Chile.  Previous observations with R-COP 
began at 59s and continued until 92m post-trigger (Trotter et al., GCN 
15828). Observations resumed with PROMPT-CTIO at t=5.5h, and continued 
at R-COP and PROMPT-CTIO until t=32h, with a total of ~600x160s new 
exposures in the BVRI bands.

We continue to detect an uncatalogued optical source in all bands at the 
position of the source detected by the Swift UVOT (Siegel & Holland, GCN 
15826). The source faded from R=14.3 at t=113s to R=17.8 at t=73m, 
bottomed out at R=19.0 at t~6h, and then rebrightened to R=18.6 by 
t=23h.  Flattening or rebrightening of the light curve is observed in 
all four bands.

An updated light curve is at:
http://www.skynet.unc.edu/grb/grb140213a_2.png

Magnitudes are in the Vega system, calibrated to ten APASS-DR7 stars in 
the field, and have not been corrected for the Galactic foreground 
extinction corresponding to E(B-V)=0.07 (Schlegel et al. 1998).

Skynet observations are ongoing.


GRB_name: GRB140215A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15861
SUBJECT: GRB 140215A: RAPTOR Observations During Gamma-Ray Emitting Interval
DATE:    14/02/19 15:35:54 GMT
FROM:    James Wren at LANL  <jwren@nis.lanl.gov>

J. Wren, W.T. Vestrand, P. Wozniak, and H. Davis,
of Los Alamos National Laboratory report:

The RAPTOR network of robotic optical telescopes made follow-up observations
of Swift trigger 586680 (Markwardt, et al., GCN 15837).  Our narrow-field
instruments in Los Alamos, NM, began imaging at 04:07:37.21 UT,
26.9 seconds after the BAT trigger time.  We do not detect the counterpart
in our three initial images, with limiting magnitudes near 14.0.  The
counterpart then rises above our detection limit and reaches peak brightness
at magnitude 13.5 around T-Tbat=90s.  The counterpart then plateaus for
a period of about 50 seconds before beginning a power-law decay.  Our
unfiltered observations were calibrated to the USNO-B1 R-band.  The following
table summarizes some of our early observations.

t-mid(s)    exp(s)    mag     error
------------------------------------
29.45       5      >14.0
56.85       5      13.8287    0.033
83.85       5      13.5381    0.011
128.95      10     13.5608    0.008
283.35      10     14.3725    0.024
470.75      30     14.9185    0.020


GRB_name: GRB140213A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15862
SUBJECT: GRB 140213A: Continued Skynet R-COP/PROMPT Observations of the Optical Afterglow
DATE:    14/02/19 16:39:45 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, J. Haislip, D. Reichart, A. LaCluyze, A. Verveer, T. Spuck, 
A. Foster, N. Frank, K. Ivarsen, J. Moore, M. Nysewander, R. Beauchemin, 
T. Berger, M. Carroll, H. T. Cromartie, R. Egger, M. Hinckle, A. 
Ireland, M. Maples, L. Scott, and J. A. Crain report:

Skynet continued observing the Swift-BAT localization of GRB 140213A 
(Holland et al., GCN 15825, Swift trigger 586569) with the 14-inch R-COP 
telescope at Perth Observatory, Australia, and with four 16-inch 
telescopes of the PROMPT array at CTIO, Chile.  Previous observations 
with R-COP began at 59s and continued until 92m post-trigger (Trotter et 
al., GCN 15828). Observations resumed with PROMPT-CTIO at t=5.5h, and 
continued at R-COP and PROMPT-CTIO until t=32h, during which time the 
afterglow rebrightened (Trotter et al., GCN 15859).

R-COP and PROMPT-CTIO took a total of 284x160s exposures in BVRI between 
t~5-5.3d. In stacked images, we continue to detect an uncatalogued 
optical source in R and I bands at the position of the source detected 
by the Swift UVOT (Siegel & Holland, GCN 15826). After the rebrightening 
at t~1d, the source clearly resumed fading.

Band      tmid       mag
I         5.3d       20.7 (+/-0.2)
R         5.2d       21.3 (+/-0.3)
V         5.3d      >21.7
B         5.3d      >21.6

An updated light curve is at:
http://www.skynet.unc.edu/grb/grb140213a_3.png

Magnitudes are in the Vega system, calibrated to ten APASS-DR7 stars in 
the field, and have not been corrected for the Galactic foreground 
extinction corresponding to E(B-V)=0.07 (Schlegel et al. 1998).

No further Skynet observations are scheduled.


GRB_name: GRB140219A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15864
SUBJECT: IPN Triangulation of extremely bright long GRB 140219A
DATE:    14/02/20 13:42:33 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

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

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

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

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

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

The extremely bright long 140219A has been observed by Fermi/GBM 
(trigger 414531995), INTEGRAL (SPI-ACS), Suzaku (WAM), Mars Odyssey 
(HEND) and MESSENGER (GRNS), so far, at about 71192 s UT (19:46:32).

We have triangulated it to a preliminary, 3 sigma error box whose 
coordinates are:
---------------------------------------------
idx  RA(2000),deg  Dec(2000),deg
---------------------------------------------
Center:
      156.44         7.46
Corners:
1    157.06     10.06
2    156.56     7.30
3    155.51     4.70
4    156.31     7.66
---------------------------------------------
The error box area is 0.644 sq. deg, and its maximum dimension is 5.57 
deg (the minimum one is 0.36 deg).

This box can be improved.

A triangulation map is posted at 
http://www.ioffe.ru/LEA/GRBs/GRB140219_T71192/IPN/


GRB_name: GRB140219A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15865
SUBJECT: GRB 140219A Tiled Swift observations
DATE:    14/02/20 15:16:24 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
IPN GRB 140219A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00024

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 IPN 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: GRB140219A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15866
SUBJECT: GRB 140219A: Fermi GBM Detection
DATE:    14/02/20 19:08:45 GMT
FROM:    Binbin Zhang at UAH  <binbin.zhang@uah.edu>

Bin-Bin Zhang (UAH) reports on behalf of the Fermi GBM Team:

At 19:46:32.24 UT on February 19 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located an extremely bright long GRB 140219A (trigger 414531995/140219824),
which was also detected by INTEGRAL (SPI-ACS), Suzaku (WAM), Mars Odyssey (HEND) and
MESSENGER (GRNS) (Holland et al., GCN 15825). The GBM on-ground location is consistent 
with IPN error box.

The GRB position was occulted by the Earth during the brightest period of emission and 
only the weaker tail emission was observed by GBM. Using the available data we find that 
the GBM light curve consists of a multiple-peak structure with a duration of about 80 s
(50-300 keV). The time-averaged spectrum from T0-2 s to T0+78 s is well fit with
a power law  function with an exponential high energy cutoff, which is parameterized
as Epeak = 194 +/- 61 keV,  alpha = -1.3 +/- 0.1. The event fluence (10-1000 keV)
in this time interval is (4.9 +/- 0.6)E-06 erg/cm^2. The 1.0-sec peak photon flux
measured starting from T0-0.9 s in the 10-1000 keV band is 3.2 +/- 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: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15867
SUBJECT: GRB 140219A: Fermi-LAT detection of a burst
DATE:    14/02/20 20:47:28 GMT
FROM:    Sylvain Guiriec at UAH  <sylvain.guiriec@lpta.in2p3.fr>

S. Guiriec (GSFC/CRESST/UMD), J. Racusin (GSFC), G. Vianello (Stanford)
and E. Bissaldi (University & INFN Trieste),
report on behalf of the Fermi-LAT team:

At 19:46:32.2 on February 19, 2014, Fermi LAT detected high-energy emission
from GRB 140219A, which was also detected by Fermi-GBM (trigger 414531995
- Zhang et al., GCN 15866) and located by IPN (Hurley et al., GCN 15864).
GRB 140219A was not observable by LAT until ~T0+500 s due to
Earth occultation and it remained in the LAT field of view from ~T0+500 s
until T0+2300 s.

An analysis of the LAT data over a period covering ~T0+500 s to ~T0+2300 s
reveals a marginal detection with a TS of about 25 using the center of
the IPN error box.

The best LAT on-ground location is RA, Dec 158.2, 7.2 (J2000). The 90%
containment region (statistical error only) is asymmetrical with a width of
2.75 deg
and a height of 1.65 deg compatible with the IPN contour
(see http://fermigrb.stanford.edu/GRB140219A_tsmap.jpg).

The highest energy photon with a probability of being associated with
the GRB > 90% is a 1.6 GeV photon at T0+1350 s.

The Fermi LAT point of contact for this burst is Sylvain Guiriec
(sylvain.guiriec*@nasa.gov <http://nasa.gov>*).

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


GRB_name: GRB140221A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15868
SUBJECT: GRB 140221A: MAXI/GSC detection
DATE:    14/02/21 08:56:11 GMT
FROM:    H. Negoro at Nihon U.  <negoro@phys.cst.nihon-u.ac.jp>

GRB 140221A: MAXI/GSC detection

Y. Morooka (Miyazaki U.), H. Negoro (Nihon U.), Y. Ogawa (Miyazaki U.), 
S. Ueno, H. Tomida, S. Nakahira, M. Kimura, M. Ishikawa, Y. E. Nakagawa (JAXA),
T. Mihara, M. Sugizaki, M. Morii, M. Serino,  J. Sugimoto, T. Takagi, A. Yoshikawa, M. Matsuoka (RIKEN),
N. Kawai, R. Usui, T. Yoshii, Y. Tachibana (Tokyo Tech), 
A. Yoshida, T. Sakamoto, Y. Nakano, Y. Kawakubo, A. Kawagoe,H. Ohtsuki (AGU), 
H. Tsunemi, M. Sasaki (Osaka U.), 
M. Nakajima, H. Sakakibara, T. Onodera, K. Fukushima, K. Suzuki (Nihon U.), 
Y. Ueda, M. Shidatsu, T. Kawamuro, T. Hori (Kyoto U.), 
Y. Tsuboi, M. Higa (Chuo U.), 
M. Yamauchi, K. Yoshidome, H. Yamada (Miyazaki U.), 
K. Yamaoka (Nagoya U.)
report on behalf of the MAXI team:

The MAXI/GSC nova alert system triggered a bright uncatalogued X-ray transient source at UT 2014-02-21 T07:12:50.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (107.447 deg, -17.336 deg) = (07 09 47, -17 20 09) (J2000)
with a statistical 90% C.L. elliptical error region
with long and short radii of 0.40 deg and 0.34 deg, respectively.
The roll angle of the long axis from the north direction is 146.0 deg counterclockwise.
There is an additional systematic uncertainty of 0.1 deg (90% containment  radius).
The X-ray flux averaged over the scan was 68 +- 18 mCrab
(4-10keV, 1 sigma error).
There was no significant excess flux in the previous transit at UT 5:40.


GRB_name: GRB140221A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15869
SUBJECT: GRB 140221A Tiled Swift observations
DATE:    14/02/21 10:16:24 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
MAXI GRB 140221A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00025

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 MAXI 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: GRB140219A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15870
SUBJECT: Konus-Wind observation of exceptionally bright GRB 140219A
DATE:    14/02/21 11:42:29 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 long-duration, exceptionally bright and hard GRB 140219A (localized 
by IPN: Hurley et al., GCN 15864; GBM detection: Zhang, GCN 15866; LAT 
detection: Guiriec et al., GCN 15867) triggered Konus-Wind at 
T0=71162.611 s UT (19:46:02.611).

The burst light curve shows an extremely bright multi-peaked pulse with 
a duration of ~2.5 s followed by a less intense multi-peaked emission 
episodes until ~T0+26 s and a very weak tail until ~T0+35 s.
The emission is seen up to ~18 MeV.

As observed by Konus-Wind, the burst had a fluence of (1.14  
0.02)x10^-3 erg/cm2, and a 16-ms peak flux, measured from T0+0.240 s,
of (1.44  0.12)x10^-3 erg/cm2/s (both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+38.912 s)
is best fit (in the 26 keV - 18 MeV range)
by a GRB (Band) model with the following model parameters:
the low-energy photon index alpha = -1.07  0.01,
the high energy photon index beta = -3.26(-0.88,+0.38),
the peak energy Ep = 2777  70 keV,
chi2 = 112.7/96 dof.

The spectrum of the main pulse (measured from T0 to T0+2.304 s)
is best fit (in the 26 keV - 18 MeV range)
by a GRB (Band) model with the following model parameters:
the low-energy photon index alpha = -0.65  0.04,
the high energy photon index beta = -3.28(-0.89,+0.39),
the peak energy Ep = 3363  141 keV,
chi2 = 47.9/77 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140219_T71162/

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

The derived peak flux and Epeak are the highest ever measured for GRBs 
with Konus-Wind during almost 20 years of its continuous observations:
the peak flux is ~50% higher than the previous record holder, GRB 
110918A, with the measured peak flux of ~0.9x10^-3 erg/cm2/s (Frederiks 
et al. ApJ, 779, 151 (2013)).

Follow-up observations are strongly encouraged.


GRB_name: GRB140219A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15871
SUBJECT: GRB 140219A: MASTER before and after GRB observational arguments of the exceptionally Dark GRB
DATE:    14/02/21 15:42:34 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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


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.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 VWF robotic very wide field cameras (FOV=2x384 square degrees,
D=72mm, f/1.2, 1 pix = 22 arcsec) installed on  MASTER-II robotic
telescope in Tunka covered full IPN error box (Hurley et. al. GCN15864)
for very short time before and after the trigger.
Fortunatelly we have set of 26 continous  5 seconds exposure images since 
19:43:16 to 19:45:21 UT i.e.  since 196 s to 71 s before the trigger and 
set of continous  5 seconds exposure  images since 19:47:01 to 19:58:31 UT 
i.e. 3 sec after Notice Time and 29 s  after the trigger.
We haven't found credible optical transient  with 3-sigma  upper limit
10.5m on single and about 12.0 m on coadd  (20 x 5 sec = 100 sec) images.
The Very Wide Field Cameras observation schedule with respect to GRB light 
curve (S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin et al., GCN 
15870)  is available at 
http://master.sai.msu.ru/static/GRB/GRB140219A_schedule.png

The first images movie available here
http://master.sai.msu.ru/static/GRB/GRB140219A_IPN_single.gif

The coadd images move available here

http://master.sai.msu.ru/static/GRB/GRB140219A_IPN_coadd1.gif
http://master.sai.msu.ru/static/GRB/GRB140219A_IPN_coadd2.gif

The same MASTER VWF robotic very wide field cameras  installed on
MASTER-II robotic telescope in Blagoveschensk also made the observations
of IPN error box  after the trigger. However the upper limit on them on
1.5m worse than in Tunka due to adverse weather conditions.

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Tunka was pointed to the  GRB140219A  78 sec after trigger 
time  at 2014-02-19 19:47:50.943 UT by FERMI GBM trigger N414531995 in two 
polarizations. On our first (10s exposure) set we haven't found optical 
transient  within 4 sq. degree center part of FERMI-GBM first  error-box 
(ra=10 11 55 dec=+12 14 00 radius = 32, Zhang et. al. GCN 15866)  .
The 5-sigma upper limit has been about 15.1 mag.

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Blagoveschensk was pointed to the  GRB140219A 30 sec after 
notice time and 57 sec after trigger time at 2014-02-19 19:47:29.9 UT by 
FERMI GBM trigger .414531995 in two polarizations. On our first (10s 
exposure) set we haven't found optical transient within 4 sq. degree 
center part of  FERMI-GBM first error-box (ra=10 11 55 dec=+12 14 00 
radius = 32 ).
The 5-sigma upper limit has been about 14.9 mag.

After IPN notice  (Hurley et. al. GCN15864) we cover full IPN and LAT 
(Guiriec et. al GCN 15867) error boxes in survey mode using 3 fields on 
two MASTER II telescope in Tunka and Blagoveschensk. The first images was 
obtained 18h 22m after trigger time at 2014-02-20 14:08:49 with upper 
limit  19.5 m in Tunka and 18.0 m in Blagoveschensk. We also haven't found 
credible optical transient up to 20.5 m  here.

The obseravtions argue that GRB 140219A is extremely dark GRB with low 
Optical to Gamma Emission  Ratio:

F_opt/F_gamma <~  1 : 130 000

On the figure 
( http://master.sai.msu.ru/static/GRB/GRB140219A_schedule.png ) 
you can find the Gamma-Optic diagramm for the prompt 
fluence of GRBs observed by MASTER (Gorbovskoy et. al Astronomy Reports, 
Volume 57, Issue 4, pp.233-286).

The message may be cited.


GRB_name: GRB140219A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15872
SUBJECT: GRB 140219A: results from Swift XRT and UVOT tiled observations
DATE:    14/02/21 17:19:26 GMT
FROM:    Vanessa Mangano at PSU  <vxm22@psu.edu>

V. Mangano (PSU), P. A. Evans (U. Leicester), F. E. Marshall (NASA/GSFC)

report on behalf of the Swift Team:



Swift-XRT has observed the central part of the error region of the 

IPN GRB 140219A in a series of observations tiled on the sky. 

The total exposure time is 5.9 ks spread over 3 fields; 

the maximum exposure within the sky observed was 3.9 ks. 

The observations started 70.3 ks after the IPN trigger.

Within these data there are 2 objects which are not catalogued in

X-rays. At the present time we cannot be sure which, if either, 

of these is the afterglow.

Source details:



Source 1

RA:  156.49768    = 10h 25m 59.44s (J2000)

Dec:  7.52128  = +07d 31' 16.6" (J2000)

Err: 10.0 (radius, 90% confidence)

Exposure time: 2.2 ks

Online products:

http://www.swift.ac.uk/xrt_products/TILED_GRB00024/index_1.php



Source 2

RA:  156.44031    = 10h 25m 45.67s (J2000)

Dec:  7.96378  = +07d 57' 49.6" (J2000)

Err: 10.0 (radius, 90% confidence)

Exposure time: 1.5 ks

Online products:

http://www.swift.ac.uk/xrt_products/TILED_GRB00024/index_2.php





UVOT observed both of the XRT source regions.

In the region for XRT Source 1, UVOT finds a bright

optical source that we identify with the star

SDSS J102559.46+073114.1.

UVOT finds no optical counterpart to XRT Source 2

in a 803-second exposure with the white filter 

starting 82.3 ks after the trigger.

The preliminary 3-sigma upper limit 

using the UVOT photometric system 

(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373)

is 21.7 mag. No correction has been made

for Galactic extinction due to the reddening of

E(B-V) of 0.03 in the direction of the source

(Schlegel et al. 1998).



This circular is an official product of the Swift team.


GRB_name: GRB140219A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15873
SUBJECT: GRB 140219A: Xuyi and Nanshan upper limits
DATE:    14/02/21 17:51:56 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), D.-M. Wei, H.-B. Zhao, Y. Xia (PMO), C.-H. Bai, X.
Zhang, H.-B. Niu, A. Esamdin, L. Ma (XAO), Y. Osorio (NOT) report on
behalf of a large collaboration:

We observed the whole IPN field and its surrounding region of GRB
140219A (Hurley et al., GCN 15864). The first epoch was done at ~15:40
UT on 2014-02-20 using the 1m telescope located at Xuyi, Jiangsu,
China, equipped with a 3x3 deg^2 CCD camera. The second epoch was done
at ~17:50 UT on 2014-02-20 using the 1m telescope located at Nanshan,
Xinjiang, China, equipped with a 1.2x1.2 deg^2 CCD camera. For both
epochs, a series of R-band 120s exposures were obtained.

The depths of the images of the two epochs are largely comparable and
it has R~19 mag. Within the IPN field, we found two relatively bright
sources, but they can be ruled out to be an afterglow by cross
checking the Xuyi, Nanshan, and DSS images. A third epoch was done at
the 2.5m Nordic Optical Telescope (NOT) and the NOT images confirm the
above ruling-out. Therefore, assuming GRB 140219A is a conventional
cosmological burst happening within the IPN field, its afterglow would
be fainter than R~19 mag at T~20 hrs post-burst, which is a possible
case according to previous GRB follow-ups. Inspection of some
surrounding region of the IPN field also leads to no credible
afterglow candidate detection.

For the reported two Swift/XRT sources in the central part of the IPN
field (Mangano et al., GCN 15872), S2 is not present in the Xuyi and
Nanshan images as well, while S1 is a known source.


GRB_name: GRB140221A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15874
SUBJECT: GRB 140221A: Results from Swift XRT tiled observations
DATE:    14/02/21 20:49:23 GMT
FROM:    Michael Stroh at PSU/Swift  <stroh@astroh.org>

M.C. Stroh (PSU), J. Kennea (PSU), D. Burrows (PSU), K. Page (U. Leicester) and P. A. Evans (U. Leicester) report on behalf of the Swift Team:

Swift-XRT has observed the error circle of the MAXI GRB 140221A in a
series of observations tiled on the sky. The total exposure time is 4.9
ks spread over 7 fields; the maximum exposure within the sky observed
was 1.4 ks. The observations started 10.9 ks after the MAXI trigger.
Within these data there are 2 objects detected, both of which are catalogued in
X-rays.

Source 1: 
Catalogued source: 1SXPS J071032.3-171853
RA:  107.63465 = 07h 10m 32.32s (J2000)
Dec:  -17.31486 = -17d 18' 53.5" (J2000)
Err: 10.0 arcsec (radius, 90% confidence)
This is an enhanced position, determined by using UVOT field stars to
determine the astrometry.Exposure time: 536 s
Online products:
http://www.swift.ac.uk/xrt_products/TILED_GRB00025/index_1.php

Source 2:
Catalogued source: 1SXPS J071108.3-171031
RA:  107.78605 = 07h 11m 8.65s (J2000)
Dec:  -17.17431 = -17d 10' 27.5" (J2000)
Err: 10.0 arcsec (radius, 90% confidence)
Exposure time: 817 s
Online products:
http://www.swift.ac.uk/xrt_products/TILED_GRB00025/index_2.php

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


GRB_name: GRB140219A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15875
SUBJECT: GRB 140219A: XRT afterglow candidate
DATE:    14/02/22 18:03:46 GMT
FROM:    Vanessa Mangano at PSU  <vanessa@ifc.inaf.it>

V. Mangano (PSU) and P. A. Evans (U. Leicester)
report on behalf of the Switf-XRT team

Swift-XRT has observed the error circle of the IPN GRB 140219A in a
series of observations tiled on the sky. The total exposure time is 9.9
ks spread over 5 fields; the maximum exposure within the sky observed
was 3.9 ks. The observations started 70.3 ks after the IPN trigger.
Within these data we detect a fading,  uncatalogued X-ray source at RA,
Dec= 156.02772, 6.49399 which is equivalent to:
   RA (J2000) = 10h 24m 6.65s
   Dec (J2000) = +06d 29' 38.4"
with an uncertainty of 7.9 arcsec (radius, 90% confidence). The
exposure at this location was 3.0 ks.

This previously uncatalogued source is fading, and we thus consider it
the likely GRB afterglow.

The results of the automatic processing for this source are available
athttp://www.swift.ac.uk/xrt_products/TILED_GRB00024/index_5.php
This circular is an official product of the Swift-XRT team.


GRB_name: GRB140219A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15876
SUBJECT: GRB 140219A: optical observations of XRT source #5
DATE:    14/02/22 19:50:38 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed  the field of XRT afterglow candidate (Mangano  et al., GCN 
15875) of the GRB 140219A (Hurley et al., GCN 15864, Zhang GCN 15866, 
Guiriec et al.,GCN 15867, Golenetskii et al. GCN 15870) with AZT-33IK 
telescope of Mondy observatory starting on Feb. 22 (UT) 14:45. We 
obtained 60 images in R-filter. In the initial images within XRT error 
circle  (Mangano  et al., GCN 15875) we detected two objects which are 
present in SDSS DR9. One of them is a galaxy (SDSS 3015-301-3-0280-0458) 
and other one is a star (SDSS 3015-301-3-0280-0457). No new objects were 
detected. Upper limit of the initial image of 60-s exposure is R=20.8.

A finding chart can be found in 
http://grb.rssi.ru/GRB140219A/GRB140219A_XRT_5_fc.png


GRB_name: GRB140102A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15877
SUBJECT: GRB 140102A: TAOS early optical afterglow detection
DATE:    14/02/23 01:09:24 GMT
FROM:    Ying-Tung Chen at ASIAA/TAOS  <ytchen@asiaa.sinica.edu.tw>

Y. T. Chen, S. K. King, C. Y. Wen, K. Y. Huang, S. Y. Wang, M. Lehner and
TAOS team

We observed the field of the Swift GRB 140102A (Hagen et al., GCN 15653)
with TAOS 0.5-m telescope of Lulin observatory (Taiwan) starting on Jan., 2
(UT) 21:19:49, i.e., 2.2 minutes after the trigger.

We detected the fading optical afterglow at the time between few early
optical afterglow observations (Xu et al., GCN 15655; Guziy et al., GCN
15685; Yoshii et al. GCN 15778). The details of the photometry were listed
below.

DATE_T_START          T0+   T_EXP   MAG
(UT)                  sec   sec     R

2014-01-02 21:19:49   132   49      15.3+/-0.11
2014-01-02 21:20:38   181   49      15.7+/-0.15
2014-01-02 21:21:27   230   49      16.1+/-0.26
2014-01-02 21:22:16   279   49      (Upper Limit = 16.2)

The R-band magnitude of nearby USNOB1 stars have been used for calibration.
We note that a special filter (5000-7200 A) was used in TAOS telescopes.


GRB_name: GRB140219A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15878
SUBJECT: GRB 140219A: iPTF optical observations
DATE:    14/02/23 02:36:37 GMT
FROM:    Leo Singer at CIT/PTF  <lsinger@caltech.edu>

L. P. Singer (Caltech), M. M. Kasliwal (Carnegie Observatories/Princeton),
and S. B. Cenko (NASA/GSFC) report on behalf of the intermediate Palomar
Transient Factory (iPTF) collaboration:

We have searched for optical counterparts of GRB 140219A using the Palomar
48-inch Oschin telescope (P48). We observed 9 fields covering an area of
67.8 deg2 intersecting the Fermi GBM 1-sigma contour (Fermi trigger
414531995, Zhang et al., GCN 15866) and a preliminary MESSENGER-Suzaku IPN
annulus (K. Hurley, personal communication) that was available when the
GBM localization was first observable from Palomar. We observed all 9
fields for several epochs, with the first epoch extending from 7.0 to 8.1
hours after the burst. Sifting through candidate variable sources using
image subtraction and standard iPTF vetting procedures, we found no
compelling optical afterglow candidates to an average limiting magnitude
of r=21.1 mag.

About 80% of the published IPN error box (Hurley et al., GCN 15864) was
contained in these 9 fields, with most of the remaining 20% falling on a
disabled CCD on the P48. To fill the gap in the IPN error box, we observed
two additional fields starting 33.7 hours after the burst. The deepest
epoch of observations of these two fields had a limiting magnitude of
r=20.7 mag. Since we lacked reference images for these two offset fields,
we performed a catalog comparison search, examining any source that was
detected in our two deepest epochs but was not coincident with a stellar
object in SDSS. Of 342 sources meeting this criterion, all were known
galaxies and none were compelling optical afterglow candidates.

XRT source 1
(http://www.swift.ac.uk/xrt_products/TILED_GRB00024/index_1.php, Mangano
et al., GCN 15872) is contained in our nine early fields, and we associate
a coincident optical detection with the star SDSS J102559.46+073114.1.

XRT source 2
(http://www.swift.ac.uk/xrt_products/TILED_GRB00024/index_2.php, Mangano
et al., GCN 15872) is contained in our two late fields, and we detect no
coincident optical source to a limiting magnitude of r=20.5 mag at 35.7
hours after the burst.

XRT source 4
(http://www.swift.ac.uk/xrt_products/TILED_GRB00024/index_4.php) is
contained in our nine early fields, and we find no coincident optical
source to a limiting magnitude of r=20.2 mag at 8.1 hours after the burst.

XRT source 5
(http://www.swift.ac.uk/xrt_products/TILED_GRB00024/index_5.php, Mangano
et al., GCN 15875), the most plausible afterglow candidate due to its
observed fading, is also contained in our two late fields. We detect two
optical sources within the XRT error circle: the star SDSS
J102406.41+062937.6, and the galaxy SDSS J102406.58+062945.7. These were
also the sources detected by Pozanenko et al. (GCN 15876). For the star,
we report r=20.0+/-0.1, which is about 0.5 mag brighter than the value
given by SDSS DR10. We find no additional sources inside the XRT error
circle to a limiting magnitude of r=21.0.

The diagram http://www.its.caltech.edu/~lsinger/iptf/Fermi414531995.pdf
shows the footprints of the nine early P48 fields in relation to the Fermi
GBM 1-, 2-, and 3-sigma statistical+systematic contours (black) and the
IPN INTEGRAL-MESSENGER and WAM-HEND annuli (blue). The INTEGRAL-MESSENGER
annulus is comparable to the initial MESSENGER-Suzaku localization on
which we based these observations.

The diagram
http://www.its.caltech.edu/~lsinger/iptf/Fermi414531995_inset_1.pdf shows
the early P48 fields in relation to a six-sided IPN polygon and the XRT
candidates.

The diagram
http://www.its.caltech.edu/~lsinger/iptf/Fermi414531995_inset_2.pdf shows
the late P48 fields.


GRB_name: GRB140219A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15879
SUBJECT: GRB 140219A: MASTER  optical brightening inside  XRT-5 error box detection
DATE:    14/02/23 15:59:55 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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.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)

We refined our reduction of images started 18h 22m after trigger time 
(Gorbovskoy et al., GCN 15871). We  found  the 3-sigma OT on several (at 
least 4) best unfiltered images with limit ~ 20 mag inside XRT error box 
(Mangano  and Evans, GCN 15875) at automatic position:


2014-02-20 14:08:50.873  10h 24m 06.46s , +06d 29m 40s.8

with 2 arcsec  error (2 arcsec = 1 pix).

The unfiltered magnitude is about 19.

Fortunately we have archive images of this area at the same telescope 
with slightly better limit(MASTER II, Tunka,2011-02-06 16:34:55 
180) without any optical source. The OT is brighter at least 1 magnitude 
at 18.5 hours after trigger.

The OT position does not coincide with  SDSS J102406.58+062945.7 galaxy 
(Singer, iPTF  GCN 15878, source XRT 5), closer to SDSS star
J102406.41+062937.6 .

The detection and reference images are  available at
http://master.sai.msu.ru/static/GRB/GRB140219A_OT.png

We do not see any OT at alert Very Wide Field images at this place 
(Gorbovskoy et al., GCN 15871).

The message may be cited.


GRB_name: GRB140219A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15880
SUBJECT: GRB 140219A: Retraction of X-ray afterglow
DATE:    14/02/24 09:34:59 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Further analysis of the XRT afterglow candidate of GRB 140219A (GCN
Circ. 15875) reveals that the light curve of this object had been
contaminated by the presence of a nearby, bright, catalogued X-ray
source. Refined analysis of the previously-announced afterglow candidate 
reveals it to be approximately constant, with a count rate of ~5e-3 
ct/sec, thus it is probably not the afterglow.

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


GRB_name: GRB140219A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15881
SUBJECT: GRB 140219A: the confirmation of the brightening  SDSS J102406.41+062937.6 star  
DATE:    14/02/24 11:11:24 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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.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)

We present the reduction of the best coadded image started 2014-02-20
  14:42:07, i.e. 18.92 hour  after  trigger time with total 
exposition 3960 s (Gorbovskoy et al., GCN 15871) with  unfiltered 21.0 mag 
limit.
We  found the  optical source   inside XRT-5 error box (Mangano 
and Evans, GCN 15875) at automatic position:

T_start = 2014-02-20 14:42:07.5 (T_start-T_trig = 18.92 h)
T_mid  =  2014-02-20 16:14:23.7 (T_start-T_mid = 20.45 h)
T_fin    = 2014-02-20 17:46:40.0  (T_start-T_fin  = 22.01 h)

RA 10h 24m 06.45s
Dec +6d 29m 37.86s

(156.021889     6.420445)
with 0.7 arcsec  error.

Unfiltered magnitude:
Mag = 19.7+/-0.3 
This source coincides with SDSS J102406.41+062937.6 star.

This star must be visible at archive image of this area at the same 
telescope (MASTER II, Tunka,2011-02-06 16:34:55 180, Lipunov et all., GCN 
15879) on 4 sigma level. The absence of the SDSS J102406.41+062937.6 star 
confirms its brightening ~0.7 mag.

But the absence of the X-ray variation of XRT-5 source (P.F. Evans, 
GCN15880) argues that  brightening may be usual variable star and does not 
connect with  GRB 140219A.

All our limits published earlier are still valid (GCN 15871, GCN 15879 )

The coadded image is available at
http://observ.pereplet.ru/images/10240645+062937.jpg

The message may be cited.


GRB_name: GRB140219A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15882
SUBJECT: GRB 140219A: MAXI/GSC detection
DATE:    14/02/26 03:08:11 GMT
FROM:    Motoko Suzuki at RIKEN  <motoko@crab.riken.jp>

M. Serino (RIKEN), S. Ueno, H. Tomida, S. Nakahira, M. Kimura, 
M. Ishikawa, Y. E. Nakagawa (JAXA), T. Mihara, M. Sugizaki, 
M. Morii, J. Sugimoto, T. Takagi, A. Yoshikawa, M. Matsuoka (RIKEN), 
N. Kawai, R. Usui, T. Yoshii, Y. Tachibana (Tokyo Tech), 
A. Yoshida, T. Sakamoto, Y. Nakano, Y. Kawakubo, H. Ohtsuki (AGU), 
H. Tsunemi, M. Sasaki (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, K. Yoshidome, 
Y. Ogawa, H. Yamada (Miyazaki U.), K. Yamaoka (Nagoya U.) 
report on behalf of the MAXI team:

The MAXI/GSC detected a rapid increase of the count rate in
all six working counters at 2014-02-19T19:45:58.15 UT.
The time is consistent with GRB 140219A 
(Hurley et al., GCN 15864; Zhang, GCN 15866; Guiriec et al., GCN 15867;
Golenetskii et al., GCN 15870).
The IPN postion of GRB 140219A was not in the field of view of any of the 
MAXI Gas Slit Cameras, implying that the detected counts are produced by the 
hard X-rays that penetrated the Ti counter walls with Pb shiled, or the phosphor 
bronze collimator with Al housing of GSC, or by the Compton-scattered electrons 
induced by the gamma-rays. It suggests that this GRB was exceptionally bright 
and hard.

The light curve shows an intense spike with a duration of ~0.2 s followed by
a bright emission until T0+~2.5 s. A weak emission lasts until T0+~20 s.
The peak count rate is ~2000 c/s per counter (GSC_3).
The MAXI/GSC light curve of this GRB is available at
http://maxi.riken.jp/news/en/?p=1101 .

There was no significant excess flux in the transits before and after the
GRB at UT 19:40 and 21:13 with an upper limit of 20 mCrab (4-10 keV, 1 sigma)
for each.

-- 
Motoko SERINO <motoko@crab.riken.jp>


GRB_name: GRB140219A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15885
SUBJECT: GRB 140219A: Suzaku WAM observation of the prompt emission 
DATE:    14/02/27 11:42:27 GMT
FROM:    Tetsuya Yasuda at Saitama U  <yasuda@heal.phy.saitama-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. E. Nakagawa, M. Kokubun,
T. Takahashi (ISAS/JAXA), Y. Hanabata (ICRR),
Y. Urata (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo)
on behalf of the Suzaku WAM team, report:

The extremely bright and long-duration GRB 140219A
(localized by IPN: Hurley et al., GCN 15864;
Fermi-GBM detection: Zhang, GCN 15866; Fermi-LAT detection: Guiriec et
al., GCN 15867; Konus-Wind detection: Golenetskii et al., GCN15870;
MAXI/GSC detection: Serino et al., GCN15882) triggered the Suzaku
Wide-band All-sky Monitor (WAM) which covers an
energy range of 50 keV - 5 MeV at 19:45:57.754 UT (=T0).

The observed light curve shows a strong multi-peaked structure lasting from
T0 s to T0+3 s, followed by a weaker multi-peaked emissions
seen up to T0+27 s with a total duration (T90) of about 17 seconds.ã€€

The fluence in 100 - 1000 keV was 1.73 (+0.06,-0.08)x10^-5 erg/cm^2. The 1-s
peak flux measured from T0+1.5 s was 83.6 (+6.5,-6.4) photons/cm^2/s in
the same energy range.

Preliminary result shows that the time-averaged spectrum from
T0 s to T0+27 s is fitted by a GRB Band model as follows.
the low-energy photon index alpha: -1.00 (+0.06,-0.11),
the high-energy photon index beta: -2.68 (+0.08,-0.11),
and the peak energy Epeak: 1930(+176,-79) keV (chi^2/d.o.f = 71.9/47).

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

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


GRB_name: GRB140226A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15888
SUBJECT: IPN triangulation of GRB 140226A, a possible GRB counterpart to iPTF14yb
DATE:    14/02/28 00:25:44 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@ssl.berkeley.edu>

K. Hurley, on behalf of the Interplanetary Network,

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

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,

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

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

We have examined IPN data for the period 2014-02-26T09:05:00 to
2014-02-26T10:18:00, when the optical transient source iPTF14yb was
discovered (Cenko et al. GCN 15883).  During this time, Konus, Swift,
INTEGRAL, RHESSI, Odyssey, and MESSENGER were operating and returning
data, although in the presence of increased solar activity.  Suzaku was
off.  We have identified one event, at 2014-02-26T10:02:57 (36177 s),
observed by Odyssey, INTEGRAL (SPI-ACS) and Konus (in the waiting
mode), whose duration is ~15 s, and whose localization is consistent
with iPTF14yb.  Specifically, the Odyssey-INTEGRAL triangulation
annulus is centered at RA, Dec = 206.305 degrees (13 h 45 m 13.2 s),
-7.925 degrees (-7 o 55 ' 29 "), with radius 27.577 +/- 0.607 degrees
(3 sigma).  iPTF14yb lies 0.157 degrees from the center line of the
annulus.  The probability that the transient lies within the annulus by
chance is roughly 0.005.  At the time of this event, the optical
transient was below the horizon for Swift, and no emission consistent
with a GRB was seen in the data. Fermi was in the SAA.  The RHESSI and
MESSENGER backgrounds were high and variable due to solar activity,
making the identification of this burst uncertain in their data.

If this is indeed the GRB counterpart to iPTF14yb, this would appear to
be the first GRB to be discovered on the basis of its optical
counterpart.

This triangulation can be improved.  Detailed spectral and temporal
information on this burst will be presented in a forthcoming GCN
Circular.


GRB_name: GRB140226A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15889
SUBJECT: Konus-Wind observation of GRB 140226A
DATE:    14/02/28 08:16:29 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration GRB 140226A
(IPN trangulation: Hurley et al., GCN 15888),
which is a possible counterpart to the optical
transient source iPTF14yb (Cenko et al. GCN 15883),
was detected by Konus-Wind in the waiting mode
against the high solar particle background.

The light curve shows a single pulse, which peaked
at T0=36177 s UT (10:02:57) and had a duration of ~15 s.

As observed by Konus-Wind, the burst had a fluence of
(5.6  1.1)x10^-6 erg/cm2 and a 2.944-s peak energy flux,
measured from T0 of (8.6  1.7)x10^-7 erg/cm2
(both in the 20 - 10000 keV energy range).

Modeling the KW 3-channel time-integrated spectrum
(from T0-6.263 s to T0+5.513 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 = 414  79 keV.

All the quoted errors are estimated at 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/GRB140226A/


GRB_name: GRB140219A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15890
SUBJECT: GRB 140219A: Mondy optical observations of XRT source #5
DATE:    14/02/28 14:57:36 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of possible XRT afterglow candidate (Mangano et 
al., GCN 15875) of the GRB 140219A (Hurley et al., GCN 15864, Zhang GCN 
15866, Guiriec et al.,GCN 15867, Golenetskii et al. GCN 15870, Serino et 
al. GCN 15882) with AZT-33IK telescope of Mondy observatory on Feb. 22 
(UT) 14:45-15:45 (Pozanenko et al., GCN 15876) and Feb. 27 (UT) 
15:18-16:18. We obtained several images with exposure of 60 seconds in 
R-filter during each observational set. In the stacked images within XRT 
error circle (Mangano et al., GCN 15875) we clearly detect two objects 
which are present in SDSS plates and SDSS DR9. One of them is a galaxy 
(refereed below as G5), SDSS J102406.58+062945.8, and other one is a 
star (X5), SDSS J102406.41+062937.6, both objects mentioned earlier 
(Pozanenko et al.,  GCN 15876, Singer et al.,  GCN 15878).
No new objects were detected.

The photometry of the two sources is following:

date         UT start t-T0      Exp.    Filter  G5     X5
                      (mid, days) (s)
2014-02-22  14:45:44  2.81197    51*60  R 20.77+/-0.12 19.74+/-0.05
2014-02-27  15:18:29  7.81388    60*60  R 20.51+/-0.09 19.59+/-0.06

The photometry is based on reference stars SDSS-DR9, (R mag,
transformation by Lupton 2005):

N  SDSS_id                R(Lupton)   err
1  J102410.32+062923.9    17.391       0.017
2  J102410.04+062943.6    18.163       0.023
3  J102404.63+062938.7    18.962       0.025

The known star X5 is ~0.5m brighter than assumed R mag from SDSS DR9, 
i.e. R = 20.24 +/- 0.06, in accordance with Singer et al. (GCN 15878).
We also may suspect, that known galaxy G5 might be brighter in our 
second epoch (Feb. 27) than on first epoch (Feb. 22). We encourage 
further observation of the galaxy G5 to confirm re-brightening, and if 
so the galaxy might be a host of GRB 140219A.

Also we report a redshift of G5 galaxy z= 0.12 +/- 0.12 obtained 
photometrically using SDSS DR9 catalog.


GRB_name: GRB140226A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15891
SUBJECT: GRB 140226A / iPTF14yb: Swift-XRT confirms a fading X-ray source
DATE:    14/02/28 15:11:10 GMT
FROM:    Andy Beardmore at U Leicester  <ab271@leicester.ac.uk>

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

The Swift-XRT has continued to observe the source GRB 140226A /
iPTF14yb (Cenko et al., GCN Circ. 15883; Cucchiara et al., GCN
Circ. 15886; Varela et al., GCN Circ. 15887; Hurley et al., GCN
Circ. 15888) and has now accumulated 9.1ks of data in Photon Counting
(PC) mode. The X-ray light curve shows that the source announced by
Beardmore et al. (GCN Circ. 15884) has faded, with a powerlaw decay
index of 1.47 +0.29 -0.25 (with respect to the Konus-Wind T0;
Golenetskii et al., GCN Circ. 15889).

Taken together with the fading optical source and IPN localisation,
the decaying X-ray source confirms the GRB origin of the object.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00033157.


GRB_name: GRB140226A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15893
SUBJECT: GRB 140226A/iPTF14yb: Mondy optical observations
DATE:    14/02/28 16:22:51 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of transient iPTF14yb (Cenko et al., GCN 15883,
Beardmore et al., GCN 15884, 15891) of possible GRB 140226A (Hurley et 
al., GCN 15888) with AZT-33IK telescope of Mondy observatory on Feb. 27 
between (UT) 18:59:34 - 19:59:36. On a stacked R-filter image of 30 x 
120 s we marginally detected  iPTF14yb source with S/N ~2, and 
photometry of the source R = 23.0 at Feb. 27.81221 (mid).

The photometry is based on SDSS J144600.66+145826.2 star assuming
R(Lupton transformation)= 17.624 +/- 0.018


GRB_name: GRB140301A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15896
SUBJECT: GRB 140301A: Swift detection of a burst
DATE:    14/03/01 15:39:16 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

K. L. Page (U Leicester), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
N. Gehrels (NASA/GSFC) and M. H. Siegel (PSU) report on behalf of the
Swift Team:

At 15:24:49 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140301A (trigger=589590).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 69.548, -34.283 which is 
   RA(J2000)  =  04h 38m 11s
   Dec(J2000) = -34d 16' 58"
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 ~1300 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 15:26:15.5 UT, 86.1 seconds after
the BAT trigger. Using promptly downlinked data we find a bright, fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 69.5584,
-34.2565 which is equivalent to:
   RA(J2000)  = 04h 38m 14.02s
   Dec(J2000) = -34d 15' 23.6"
with an uncertainty of 3.4 arcseconds (radius, 90% containment). This
location is 100 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 2.23
x 10^20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 3.38e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 95 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 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
0.03. 

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: GRB140301A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15897
SUBJECT: GRB 140301A: Skynet R-COP Observations
DATE:    14/03/01 16:30:27 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, J. Haislip, A. LaCluyze, D. Reichart, A. Verveer, T. Spuck, 
A. Foster, N. Frank, K. Ivarsen, J. Moore, M. Nysewander, R. Beauchemin, 
T. Berger, M. Carroll, H. T. Cromartie, R. Egger, M. Hinckle, A. 
Ireland, M. Maples, L. Scott, and J. A. Crain report:

Skynet observed the Swift-BAT localization of GRB 140301A (Page et al., 
GCN 15896, Swift trigger 589590) with the 14-inch R-COP telescope at 
Perth Observatory, Australia.  Observations began at 93s and continued 
until 33m post-trigger, with rotating exposures in the BVRI bands 
increasing from 10s to 80s. We detect no optical source in stacked 
images in any band at the position of the source detected by the Swift 
XRT. Preliminary upper limits are:
Band      tmid      mag
V         17m       >18.5
R         22m       >19.0
I         18m       >18.0

Photometry is calibrated to seven APASS-DR7 stars in the field, and has 
not been corrected for the Galactic foreground extinction corresponding 
to E(B-V)=0.03 (Schlegel et al. 1998).

No further Skynet observations are scheduled.


GRB_name: GRB140301A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15898
SUBJECT: GRB 140301A: Enhanced Swift-XRT position
DATE:    14/03/01 19:26:44 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 691 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 140301A, 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 = 69.55743, -34.25679 which is equivalent
to:

RA (J2000): 04h 38m 13.78s
Dec (J2000): -34d 15' 24.4"

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

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

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


GRB_name: GRB140301A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15899
SUBJECT: GRB 140301A: NOT afterglow candidate
DATE:    14/03/01 21:03:43 GMT
FROM:    Thomas Kruehler at Dark Cosmology Center  <tom@dark-cosmology.dk>

T. Kruehler (ESO), D. Malesani, D. Xu, J. P. U. Fynbo (DARK/NBI),
T. J. Rivera-Thorsen (Stockholm), J. Puschnig (Stockholm),
P. Jakobsson (Univ. Iceland), report on behalf of a larger
collaboration:

We observed the field of GRB 140301A (Page et al., GCN 15896) with the
Nordic Optical Telescope equipped with the MOSCA imager. Observations
were taken at high airmass, in twilight, using the R and z filters.

Consistent with the position of the XRT afterglow (Goad et al.,
GCN 15898), our images show the presence of a faint object in the
R band, with coordinates:

RA = 04:38:13.78
Dec = -34:15:23.5

and uncertainties of approximately 0.5" in each coordinate.

At a midtime of 4.97 hr after the trigger, we measure a brightness
of R = 23.1 +/- 0.3 mag. This magnitude is calibrated against stars
from the USNO-B1 catalog.

No statement about fading can be made at this point.


GRB_name: GRB140301A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15900
SUBJECT: GRB 140301A: VLT/X-shooter redshift
DATE:    14/03/02 06:16:27 GMT
FROM:    Thomas Kruehler at Dark Cosmology Center  <tom@dark-cosmology.dk>

T. Kruehler (ESO), N. R. Tanvir (Univ. Leicester) D. Malesani,
D. Xu, J. P. U. Fynbo (DARK/NBI) report on behalf of a larger
collaboration:

We observed the optical source (Kruehler et al., GCN 15899)
inside the XRT error circle (Goad et al., GCN 15898) of
GRB 140301A (Page et al., GCN 15896) with the VLT equipped
with the X-shooter spectrograph.

Our spectrum covers the wavelength range between 3000 and
20000 AA and consists of 12 nodded spectra with an
integration time of 600 s each. A preliminary analysis of
the spectrum reveals a faint continuum in which we
tentatively identify absorption lines of the MgII doublet
at z = 1.416.

At the same redshift and with a spatial offset of up to ~1"
we detect strong emission lines of [OII], Hbeta, [OIII],
Halpha and [NII], characteristic for emission from the
GRB host.

We acknowledge excellent support from the observing staff
in Paranal, in particular Julien Girard and Valentin Ivanov.


GRB_name: GRB140302A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15901
SUBJECT: GRB 140302A: Swift detection of a burst
DATE:    14/03/02 08:26:25 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

C. Pagani (U Leicester), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), V. D'Elia (ASDC),
C. B. Markwardt (NASA/GSFC), A. Maselli (INAF-IASFPA),
K. L. Page (U Leicester), M. H. Siegel (PSU) and
R. L. C. Starling (U Leicester) report on behalf of the Swift Team:

At 08:12:58 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140302A (trigger=589685).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 253.842, -12.865, which is 
   RA(J2000)  =  16h 55m 22s
   Dec(J2000) = -12d 51' 53"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows several peaks
with a total duration of about 35 sec.  The peak count rate
was ~5300 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 08:14:10.9 UT, 72.2 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 253.85859, -12.87891 which
is equivalent to:
   RA(J2000)  = 16h 55m 26.06s
   Dec(J2000) = -12d 52' 44.1"
with an uncertainty of 4.1 arcseconds (radius, 90% containment). This
location is 76 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 1.46
x 10^21 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 1.49e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 80 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
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
0.52. 

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: GRB140302A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15902
SUBJECT: GRB 140302A: Prompt enhanced Swift-XRT position
DATE:    14/03/02 08:38:49 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Using  promptly downlinked XRT event data for GRB 140302A, we find an
enhanced XRT position of the afterglow: RA, Dec: 253.8593, -12.8788
which is equivalent to:
   RA (J2000)  = 16 55 26.23
   Dec (J2000) = -12 52 43.7
with an uncertainty of 2.6 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/589685.

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

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


GRB_name: GRB140302A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15903
SUBJECT: GRB 140302A: GROND afterglow candidate
DATE:    14/03/02 11:33:18 GMT
FROM:    Sebastian Schmidl at TLS Tautenburg  <schmidl@tls-tautenburg.de>

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

We observed the field of GRB 140302A (Swift trigger 589685; Pagani et al.,
GCN #15901) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2m MPG telescope at ESO La Silla
Observatory (Chile).

Observations started at 08:21:12 UT on the 2nd March 2014, 8.2 min after
the GRB trigger. They were performed at an average seeing of 1.5" and at
an average airmass of 1.2.

We find a faint point source inside the enhanced XRT error
circle given in Evans et al. (GCN #15902)

RA (J2000) = 16:55:26.30
DEC (J2000) = -12:52:42.2

with an uncertainty of 0.5" in each coordinate.

Based on a total exposure of 1936 sec in r', at a mid-time of 0.65
hrs after the burst, we measure the following preliminary magnitude (in AB):

r = 23.7 +/- 0.2 mag.

No statement about fading can be made at this stage.

Given magnitude is calibrated against GROND zeropoint and is not
corrected for the expected Galactic foreground extinction corresponding to
a reddening of E_(B-V) = 0.52 mag in the direction of the burst (Schlegel
et al. 1998).


GRB_name: GRB140301A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15904
SUBJECT: GRB 140301A: GROND Detection of the Optical/NIR Afterglow
DATE:    14/03/02 11:43:10 GMT
FROM:    Jonny Elliott at MPE/GROND  <jonnyelliott@mpe.mpg.de>

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

We observed the field of GRB 140301A (Swift trigger 589590; Page et al.,
GCN #15896) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2 m MPG/ESO telescope at La Silla
Observatory (Chile).

Observations started at 00:07 UT on 2nd March 2014, 9.72 hrs after the GRB
trigger. They were performed at an average seeing of
2.2" and at an average airmass of 1.3.

We find a single point source within the 1.9" refined Swift-XRT error
circle reported by Goad et al. (GCN #15898) and confirm the source found
by Kruehler et al. (GCN #15899, #15900).

Based on an exposure of 2.5 hours we estimate preliminary magnitudes (AB
system) of

g' = 24.2 +/- 0.2,
r' = 23.8 +/- 0.2,
i' = 23.2 +/- 0.2,
z' = 22.4 +/- 0.2,
J  > 21.8,
H  > 21.3, and
K  > 20.6.

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) = 0.03 mag in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB140301A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15905
SUBJECT: GRB 140301A: Swift-XRT refined Analysis
DATE:    14/03/02 12:03:17 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K. L. Page (U Leicester) reports on behalf of the Swift-XRT team:

We have analysed 5.9 ks of XRT data for GRB 140301A (Page  et al. GCN
Circ. 15896),  from 92 s to 51.3 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 Goad et al. (GCN Circ. 15898).

The late-time light curve (from T0+6.4 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.95 (+0.32, -0.29).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.01 (+/-0.09). The
best-fitting absorption column is  3.3 (+/-1.0) x 10^21 cm^-2, at a
redshift of 1.416, in addition to the Galactic value of 2.2 x 10^20
cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a photon index
of 2.42 (+0.32, -0.29) and a best-fitting absorption column of 7.2
(+4.1, -3.3) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10
keV flux conversion factor deduced from this spectrum  is 3.0 x 10^-11
(4.8 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 2.2 x 10^20 cm^-2
Intrinsic column:    7.2 (+4.1, -3.3) x 10^21 cm^-2 at z=1.416
Photon index:      2.42 (+0.32, -0.29)

If the light curve continues to decay with a power-law decay index of
0.95, the count rate at T+24 hours will be 5.8 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.7 x
10^-13 (2.8 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00589590.

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


GRB_name: GRB140301A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15906
SUBJECT: GRB 140301A: Swift-BAT refined analysis
DATE:    14/03/02 14:35:47 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), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/UMBC), C. B. Markwardt (GSFC), K. L. Page (U Leicester),
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-239 to T+886 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 140301A (trigger #589590)
(Page, et al., GCN Circ. 15896).  The BAT ground-calculated position is
RA, Dec = 69.521, -34.249 deg, which is 
   RA(J2000)  =  04h 38m 05.0s 
   Dec(J2000) = -34d 14' 56.8" 
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 66%.
 
The mask-weighted light curve shows a roughly symmetric peak starting
at ~T-15 sec, peaking at ~T+1 sec, and ending at ~T+20 sec.
T90 (15-350 keV) is 31.0 +- 5.7 sec (estimated error including systematics).
 
The time-averaged spectrum from T-13.18 to T+22.82 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.96 +- 0.28.  The fluence in the 15-150 keV band is 4.4 +- 0.8 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.82 sec in the 15-150 keV band
is 0.7 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/589590/BA/


GRB_name: GRB140302A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15907
SUBJECT: GRB 140302A: Enhanced Swift-XRT position
DATE:    14/03/02 19:36:02 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Using 478 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 140302A, 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 = 253.85872, -12.87823 which is equivalent
to:

RA (J2000): 16h 55m 26.09s
Dec (J2000): -12d 52' 41.6"

with an uncertainty of 2.3 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB140302A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15908
SUBJECT: GRB 140302A: Swift-BAT refined analysis
DATE:    14/03/02 20:27:28 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), C. Pagani (U Leicester), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+303 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 140302A (trigger #589685)
(Pagani, et al., GCN Circ. 15901).  The BAT ground-calculated position is
RA, Dec = 253.862, -12.875 deg, which is 
   RA(J2000)  =  16h 55m 26.8s 
   Dec(J2000) = -12d 52' 29.8" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 82%.
 
The mask-weighted light curve shows a sharp rise starting at ~T-0.1 sec,
peaking at ~T+0.2 sec, and a roughly exponential decay with several small
peaks riding on top, finally returning to baseline at ~T+190 sec.
T90 (15-350 keV) is 87.5 +- 11.4 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.09 to T+106.25 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.09 +- 0.09.  The fluence in the 15-150 keV band is 2.7 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-0.10 sec in the 15-150 keV band
is 1.7 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/589685/BA/


GRB_name: GRB140302A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15909
SUBJECT: GRB 140302A: Swift-XRT refined Analysis
DATE:    14/03/02 20:30:15 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), V. D'Elia
(ASDC), A. Maselli  (INAF-IASFPA), A. Melandri (INAF-OAB), D.N. Burrows
(PSU), J.A. Kennea (PSU), V. Mangano (PSU) and C. Pagani report on
behalf of the Swift-XRT team:

We have analysed 6.0 ks of XRT data for GRB 140302A (Pagani  et al. GCN
Circ. 15901),  from 78 s to 23.2 ks after the  BAT trigger. The data
comprise 136 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Osborne et al. (GCN Circ. 15902).

The light curve can be modelled with an initial power-law decay with an
index of alpha=1.62 (+0.22, -0.23), followed by a break at T+183 s to
an alpha of 4.0 (+/-0.4).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.08 (+0.16, -0.15). The
best-fitting absorption column is  3.1 (+1.0, -0.9) x 10^21 cm^-2, in
excess of the Galactic value of 1.5 x 10^21 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 6.8 x 10^-11 (7.7 x 10^-11) erg
cm^-2 count^-1. 

A summary of the WT-mode spectrum is thus:
Total column:      3.1 (+1.0, -0.9) x 10^21 cm^-2
Galactic foreground: 1.5 x 10^21 cm^-2
Excess significance: 3.2 sigma
Photon index:      1.08 (+0.16, -0.15)

If the light curve continues to decay with a power-law decay index of
4.0, the count rate at T+24 hours will be 1.9 x 10^-10 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.3 x
10^-20 (1.4 x 10^-20) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00589685.

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


GRB_name: GRB140302A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15910
SUBJECT: GRB140302A: Fermi GBM detection
DATE:    14/03/02 21:04:59 GMT
FROM:    Gerard Fitzpatrick at UCD  <gerard.fitzpatrick@ucdconnect.ie>

G. Fitzpatrick (UCD) reports on behalf of the Fermi GBM Team:

At 08:12:58.89 UT on 02 March 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140302A (trigger 415440781/140302342), which was
also
detected by Swift (Pagani et al., GCN 15901). The GBM on-ground location
is consistent with the Swift/XRT position (Pagani et al., GCN 15901).

The GBM light curve consists of a single peak
with a duration (T90) of about 64 s (50-300 keV).
The time-averaged spectrum from T0 s to T0+64 s is
adequately fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.49 +/- 0.1 and
the cutoff energy, parameterized as Epeak, is 462 +/- 53 keV.

The event fluence (10-1000 keV) in this time interval is
(1 +/- 0.05)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0 s in the 10-1000 keV band is 3 +/- 0.2 ph/s/cm^2.

The main emission is preceded by an apparent precursor event with an
approximate
duration of 20 s. This event has been tentatively associated with the GRB
based on the
location derived by GBM.

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


GRB_name: GRB140302A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15911
SUBJECT: GRB 140302A: MITSuME Okayama upper limits
DATE:    14/03/03 01:15:14 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 140302A (Pagani et al., GCNC 15901)
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 2014-03-02 19:19:00 UT (~11.1 h after the burst).
We could not detect the previously reported afterglow (Elliot et al., GCNC
15903) 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
-----------------------------------------------------
0.48800    19:55:41    2400.0   >19.6  >19.4  >18.7
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB140302A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15912
SUBJECT: GRB 140302A: Swift/UVOT Upper Limits
DATE:    14/03/03 16:24:29 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (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 140302A
80 s after the BAT trigger (Pagani et al., GCN Circ. 15901).
No optical afterglow consistent with the optical position
(Elliott et al. GCN Circ. 15903)
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)          80          230          147         >20.5
white               80          593          167         >20.6
white            10575        11481          590         >21.1
v                  624          643           19         >18.3
v                16940        17847          590         >19.4
b                  549          569           19         >19.3
b                 9662        10569          590         >20.5
u (fc)             293          543          246         >19.7
uvw1               672          692           19         >19.0
uvm2             17853        17993          137         >18.9
uvw2             11487        12232          732         >20.2

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.52 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB140301A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15913
SUBJECT: GRB 140301A: Swift/UVOT Upper Limits
DATE:    14/03/04 04:27:15 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

B. Porterfield (PSU) and R. Starling (U Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140301A
95 s after the BAT trigger (Page et al., GCN Circ. 15896).
No optical afterglow consistent with the XRT position
(Goad et al. GCN Circ. 15898)
is detected in the initial UVOT exposures. 
No counterpart consistent with the optical counterpart observed by 
NOT (Kruehler et al. GCN Circ. 15899) is detected.
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           108          258          292         >21.8
u_FC               320          744          265         >20.7
white              108          920          231         >21.1
v                  650          843           38         >18.7
v                 6583        22273          392         >20.2
b                  749          769           19         >19.2
b                27968        28212          240         >21.0
u                  320          744          265         >20.7
w1                 700          719           19         >17.9
w1               11294        45552         1408         >21.1
w2                 799          818           19         >17.8
w2                6378        58531         1122         >21.4

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: GRB140304A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15914
SUBJECT: GRB 140304A: MASTER OT detecton
DATE:    14/03/04 13:33:36 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Tunka was pointed to the  GRB140304A 84 sec after trigger 
time at 2014-03-04 13:23:55.366 UT. On our first (10s exposure) set we 
found optical transient  within SWIFT error-box (ra=02 02 38 
dec=+33 29 24 r=0.050000)


02h 02m 34.13s , +33d 28m 26s.6   mag  16.5


The message may be cited.


GRB_name: GRB140304A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15915
SUBJECT: GRB 140304A: Swift detection of a burst
DATE:    14/03/04 13:57:15 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

P. A. Evans (U Leicester), A. P. Beardmore (U Leicester),
D. N. Burrows (PSU), N. Gehrels (NASA/GSFC), S. T. Holland (STScI),
J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
A. Maselli (INAF-IASFPA), K. L. Page (U Leicester),
D. M. Palmer (LANL), T. Sakamoto (AGU), M. H. Siegel (PSU) and
T. N. Ukwatta (MSU) report on behalf of the Swift Team:

At 13:22:31 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140304A (trigger=590206).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 30.668, +33.485 which is 
   RA(J2000) = 02h 02m 40s
   Dec(J2000) = +33d 29' 07"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure with a total duration of about 20 sec.  The peak count rate
was ~3600 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 13:23:46.2 UT, 75.2 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source with an enhanced position: RA, Dec 30.6412,
33.4744 which is equivalent to:
   RA(J2000)  = 02h 02m 33.90s
   Dec(J2000) = +33d 28' 27.9"
with an uncertainty of 2.2 arcseconds (radius, 90% containment). This
location is 89 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 5.98
x 10^20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 6.28e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
137 seconds after the BAT trigger. No credible afterglow candidate has been
found in the initial data products. The 2.7'x2.7' sub-image processing FAILED
because of no aspect solution. Results from the list of sources generated
on-board are not available at this time. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.08. 

This GRB will enter a Moon observing constraint around 20:00 UT and
will not be observable again by Swift until March 6 (Thursday) around
05:30 UT. 

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


GRB_name: GRB140304A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15916
SUBJECT: GRB 140304A: Afterglow decay from Nanshan observations
DATE:    14/03/04 14:26:19 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

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

We observed the field of GRB 140304A (Evans et al., GCN 15915) using
the 1m telescope located in Nanshan, Xinjiang, China. Observations
started at 13:43:26 UT on 2014-03-04 (i.e., 0.349 hr after the BAT
trigger) and a series of 120s and 500s R-band images were obtained.

In the first 120s R-band image, an optical source is clearly detected
at the MASTER position (Gorbovskoy et al., GCN 15914), which is also
consistent with the Swift/XRT position. We thus think this is the
afterglow of the burst, and it has decayed to R=19.4+/-0.2 mag,
calibrated with nearby SDSS stars.

Observations are ongoing.


GRB_name: GRB140304A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15917
SUBJECT: GRB 140304A: Mondy optical observations
DATE:    14/03/04 15:02:59 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of GRB 140304A (Evans et al., GCN 15915)  with 
AZT-33IK telescope of Mondy observatory starting on Mar. 04 (UT) 
13:54:10, i.e. ~0.5 hour after burst trigger. In the first images of 60 
s exposure we clearly detected afterglow of GRB 140304A reported by 
Gorbovskoy et al. (GCN 15914) and Xu et al. (GCN 15916).  Preliminary 
photometry of the fading afterglow is following:

date       UT start   t-T0      Exp.  Filter  OT
                      (mid, days) (s)
2014-03-04 13:54:10  0.02406    6*60  R       20.29 Â± 0.17

The photometry is based on reference stars SDSS-DR9, (R mag,
transformation by Lupton 2005):

N  SDSS_id          R(Lupton)   err
J020233.12+332550.3 15.665 0.012
J020219.91+332738.5 14.785 0.012


GRB_name: GRB140304A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15918
SUBJECT: GRB 140304A:  Khureltogot optical observations
DATE:    14/03/04 15:17:16 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), N. Tungalag (Research Centre of Astronomy and 
Geophysics MAS), S. Schmalz (AIP), V. Voropaev (KIAM), I.Molotov (KIAM), 
A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration:

We observed the field of the he field of GRB 140304A (Evans et al., GCN 
15915)  with ORI-40 telescope of Khureltogot observatory starting on 
Mar., 04 (UT)13:29:36, i.e., ~7 minutes after the GRB trigger. In the 
first unfiltered images of 60 s exposure we clearly detected afterglow 
of GRB 140304A reported by Gorbovskoy et al. (GCN 15914),  Xu et al. 
(GCN 15916), and Volnova et al., (GCN 15917).  Preliminary photometry of 
the fading afterglow is following:

date       UT start   t-T0      Exp.  Filter  OT
                       (mid, days) (s)
2014-03-04 13:29:36   0.00602   3*60  none    17.5 +/- 0.2

The photometry is based on reference stars SDSS-DR9, (R mag,
transformation by Lupton 2005):

N  SDSS_id          R(Lupton)err
J020233.12+332550.3 15.665 0.012
J020219.91+332738.5 14.785 0.012


GRB_name: GRB140304A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15920
SUBJECT: GRB 140304A: Swift/UVOT Upper Limits
DATE:    14/03/04 21:39:55 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and P. A. Evans (U. Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140304A
138 s after the BAT trigger (Evans et al., GCN Circ. 15915).
No optical afterglow consistent with the optical position
(Gorbovskoy et al. GCN Circ. 15914)
is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

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

u_FC               138          388          246         >20.4
v                  420         1561          165         >19.5
u                  138         1519          529         >20.9
w1                 469         1495          156         >19.7
m2                 570         1470          117         >20.1
w2                 396         1546          156         >20.0

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.08 in the direction of the burst
(Schlegel et al. 1998).

In view of the bright (16.5 mag) afterglow reported by
Gorbovskoy et al., it is likely that the GRB has large
intrinsic extinction or is at a redshift greater than
about 3.5.


GRB_name: GRB140304A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15921
SUBJECT: GRB 140304A: NOT observations and redshift estimate
DATE:    14/03/04 21:44:36 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), J. Gorosabel (EHU-UPV,
IAA-CSIC), D. Xu (DARK/NBI), D. Malesani (DARK/NBI), A. Somero (NOT), 
B. Milvang-Jensen (DARK/NBI), M.I. Andersen (DARK/NBI), P. Jakobsson 
(U. Iceland) and J.P.U. Fynbo (DARK/NBI) report on behalf of a larger collaboration:

We have observed the afterglow of 140304A (Gorbovskoy et al. GCN 15914, Evans et 
al. GCN 15915) with the Nordic Optical Telescope (NOT) equipped with ALFOSC. 
Observations started at 20:19 UT on March 4 (i.e., 6.95 hr after the burst) in r and g-bands.
The afterglow is clearly detected in r-band at 20.5 mag, but undetected in g-band down to 
a 3-sigma limit of 21.5, pointing towards a high-redshift event at z ~ 5 if the Lyman break 
is between g and r-band. 

Further observations are ongoing.


GRB_name: GRB140304A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15922
SUBJECT: GRB 140304A: 10.4m GTC redshift z = 5.39
DATE:    14/03/04 22:01:48 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

S. Jeong, R. Snchez-Ramrez (IAA-CSIC), A. J. Castro-Tirado (IAA-CSIC,
UMA), J. Gorosabel (EHU-UPV, IAA-CSIC), M. Jelinek, J. C. Tello, P.
Ferrero, O. Lara-Gil, R. Cunniffe (IAA-CSIC), D. Prez-Ramrez (U. Jan),
S. Guziy (Nikolaev Univ.), J. M. Castro Cern (ESAC), A. Fernndez-Soto
(UV), J. Cepa (IAC), M. A. Rivero and G. Gmez-Velarde (GTC), on behalf of
a larger collaboration, report:

Following the detection of the optical afterglow (Gorbovskoy et al. GCNC
15914) to GRB 140304A (Evans et al. GCNC 15915), we have obtained an
optical spectrum with the 10.4 m GTC (+OSIRIS) starting aprox. 8.2 hr
postburst, covering the 5700-10000 wavelength range. The continuum is
detected only redwards of aprox. 7750 A, with several absorption metallic
lines (N V, Si II and Si IV amongst others) at a common redshift of z =
5.39 which we propose to be the redshift of GRB 140304A. This is
consistent with the Swift/UVOT upper limits (Marshall et al. GCNC 15920)
and the NOT optical observation (de Ugarte Postigo et al. GCNC 15921).

[GCN OPS NOTE(04mar14): Per author's request, the "5.XX" was replaced with 5.39.]


GRB_name: GRB140304A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15923
SUBJECT: GRB 140304A: Fermi GBM detection
DATE:    14/03/04 22:27:39 GMT
FROM:    Peter Jenke at MSFC  <peter.a.jenke@nasa.gov>

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

"At 13:22:31.48 UT on March 4 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140304A (trigger 415632154/140304577),
which was also detected by Swift (P. A. Evans et al. 2014, GCN 15915).  
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 80 degrees.

The GBM light curve consists of two main peaks with a
combined duration (T90) of 32 +/- 6 s (50-300 keV).
The time-averaged spectrum from T0-5 s to T0+14 s is
well fit by a power law function with an exponential
 high energy cutoff. The power law index is -1.1 +/- 0.1 
and the high energy cutoff, parameterized as 
EPeak, is 185 +/- 35 keV.

The event fluence (10-1000 keV) in this time interval is
(2.6 +/- 0.2)E-06 erg/cm^2. The 1.0-sec peak photon flux measured
starting from T0+7.2 s in the 10-1000 keV band
is 2.5 +/- 0.3 ph/s/cm^2.

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


GRB_name: GRB140304A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15924
SUBJECT: GRB 140304A: Redshift from the NOT
DATE:    14/03/05 00:41:12 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), D. Xu (DARK/NBI), 
J. Gorosabel (EHU-UPV, IAA-CSIC), D. Malesani (DARK/NBI), 
B. Milvang-Jensen (DARK/NBI), M.I. Andersen (DARK/NBI), 
P. Jakobsson (U. Iceland), J.P.U. Fynbo (DARK/NBI), and
A. Somero (Tuorla Obs.) report on behalf of a larger collaboration:

Following the photometry reported in GCN 15921, we have performed spectroscopy 
of GRB 140304A (Gorbovskoy et al. GCN 15914, Evans et al. GCN 15915) with the 
Nordic Optical Telescope (NOT) equipped with ALFOSC. The observation began at 
21:20 UT (7.97 hr after the burst) and consisted of a single 1500 s exposure
covering the range between 3200 and 9100 A.

We detect continuum emission with a deep absorption consistent with a 
DLA at a redshift of 5.28+/-0.02, as well as emission down to ~5800 A, which
is consistent with the Ly-limit at a similar redshift. Despite the lack of metal 
features identified in our spectrum, a redshift of z=5.39 as reported by 
Jeong et al. (GCN 15922) is inconsistent with our data.


GRB_name: GRB140304A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15925
SUBJECT: GRB 140304A: Enhanced Swift-XRT position
DATE:    14/03/05 00:43:34 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 3335 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 140304A, 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 = 30.64267, +33.47384 which is equivalent
to:

RA (J2000): 02h 02m 34.24s
Dec (J2000): +33d 28' 25.8"

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

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

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


GRB_name: GRB140304A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15926
SUBJECT: GRB 140304A: Swift-XRT refined Analysis
DATE:    14/03/05 02:57:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.4 ks of XRT data for GRB 140304A (Evans  et al. GCN
Circ. 15915),  from 81 s to 23.1 ks after the  BAT trigger. The data
comprise 42 s in Windowed Timing (WT) mode with the remainder in Photon
Counting (PC) mode. The enhanced XRT position for this burst was given
by Beardmore et al. (GCN Circ. 15925). The late-time light curve (from
T0+5.2 ks) is consistent with a constant source of mean count rate
1.1e+00 ct/sec. A power-law fit gives an index of 0.2 (+/-0.7).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.00 (+0.15, -0.14). The
best-fitting absorption column is  9.8 (+3.4, -3.1) x 10^20 cm^-2, in
excess of the Galactic value of 6.0 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.6 x 10^-11 (4.6 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      9.8 (+3.4, -3.1) x 10^20 cm^-2
Galactic foreground: 6.0 x 10^20 cm^-2
Excess significance: 2.0 sigma
Photon index:      2.00 (+0.15, -0.14)

If the light curve continues to decay with a power-law decay index of
0.2, the count rate at T+24 hours will be 0.024 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 8.7 x
10^-13 (1.1 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00590206.

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


GRB_name: GRB140304A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15927
SUBJECT: GRB 140304A: Swift-BAT refined analysis
DATE:    14/03/05 04:14:02 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),
P. A. Evans (U Leicester), 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-61 to T+242 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 140304A (trigger #590206)
(Evans, et al., GCN Circ. 15915).  The BAT ground-calculated position is
RA, Dec = 30.653, 33.480 deg, which is 
   RA(J2000)  =  02h 02m 36.8s 
   Dec(J2000) = +33d 28' 47.4" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 74%.
 
The mask-weighted light curve shows several overlapping peaks starting
at ~T-10 sec, peaking at ~T+10 sec, and ending at ~T+30 sec.
T90 (15-350 keV) is 15.6 +- 1.9 sec (estimated error including systematics).
 
The time-averaged spectrum from T-3.94 to T+15.77 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.29 +- 0.08.  The fluence in the 15-150 keV band is 1.2 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+10.22 sec in the 15-150 keV band
is 1.7 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/590206/BA/


GRB_name: GRB140304A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15928
SUBJECT: GRB 140304A: RATIR g-band Dropout
DATE:    14/03/05 04:59:08 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), 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 140304A (Evans, et al., GCN 15915) 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 2014/03 5.12 to 2014/03 5.16 UTC (13.50 to
14.40 hours after the BAT trigger), obtaining a total of 0.26 hours
exposure in the g and r bands, 0.53 hours exposure in the i band, and 0.30
hours exposure in the Z, Y, J, and H bands.

For a source within the Swift-XRT error circle (Evans, et al., GCN 15925),
in comparison with the SDSS DR9 and 2MASS, we obtain the following
detections and 3-sigma upper limit:

  g     > 23.07
  r     21.78 +/- 0.13
  i     20.66 +/- 0.06
  Z    19.45 +/- 0.05
  Y    19.19 +/- 0.06
  J     19.11 +/- 0.07
  H     18.71 +/- 0.08

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

Using the procedure outlined in Littlejohns et al. 2013 (arXiv:1312.3967),
we derive a photometric redshift z_phot = 5.45 (-0.2,+0.1; 90% confidence).
 This photometric redshift is consistent with the one reported by de
Ugarte-Postigo et al. (GCN 15921) and the spectroscopic redshift
determinations by Jeong et al. (GCN 15922) and de Ugarte-Postigo et al.
(GCN 15924).

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


GRB_name: GRB140305A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15929
SUBJECT: GRB 140305A: Swift detection of a burst
DATE:    14/03/05 15:07:40 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

A. Maselli (INAF-IASFPA), S. D. Barthelmy (GSFC),
P. A. Evans (U Leicester), S. T. Holland (STScI), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), K. L. Page (U Leicester),
P. Romano (INAF-IASFPA) and M. H. Siegel (PSU) report on behalf of the
Swift Team:

At 15:00:20 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140305A (trigger=590446).  Swift did not slew to this burst
because of the Sun constraint. 
The BAT on-board calculated location is 
RA, Dec 344.533, +15.441, which is 
   RA(J2000)  =  22h 58m 08s
   Dec(J2000) = +15d 26' 29"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a cluster of peaks
with a total duration of about 25 sec.  The peak count rate
was ~1700 counts/sec (15-350 keV), at ~1 sec after the trigger. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 16:35 UT on 2014 April 25. There will thus be no XRT or
UVOT data for this trigger before this time. 

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


GRB_name: GRB140304A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15930
SUBJECT: GRB 140304A: VLA Detection
DATE:    14/03/05 17:10:53 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 140304A (Evans et al; GCN 15915) with
the VLA beginning on 2014 May 5.01 UT (0.45 days after the burst). At a
mean frequency of 6 GHz, we detect a radio source with a preliminary flux
density of ~ 0.05 mJy at

RA = 02:02:34.173 +/- 0.001
Dec = 33:28:26.01 +/- 0.02

consistent with the enhanced Swft/XRT position (Beardmore et al.; GCN
15925) and the optical position (Gorbovskoy et al.; GCN 15914). Follow-up
observations are planned."


GRB_name: GRB140304A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15931
SUBJECT: GRB 140304A: CARMA 3mm detection
DATE:    14/03/05 17:28:20 GMT
FROM:    Ashley Zauderer at CfA  <bevinashley@gmail.com>

B. A. Zauderer, T. Laskar, and E. Berger (Harvard) report on behalf of the
CARMA Key Project "A Millimeter View of the Transient Universe":

"We observed the position of GRB 140304A (Evans et al., GCN 15915)
with the Combined Array for Research in Millimeter Astronomy (CARMA)
beginning
2014 Mar 5.01 UT (10.8 hours post-burst) at a mean frequency of ~85 GHz.

We detect a radio source with a flux of ~0.5 mJy consistent with the
enhanced Swift-XRT
position (Beardmore et al., GCN 15925), the optical afterglow
localization (Gorbovskoy et al.,
GCN 15914), and our VLA 5.8 GHz position (Laskar et al., GCN 15930).
Follow-up observations are in progress.

We thank the CARMA staff and observers, Shaye Storm and Robin Dong,
for their support of these rapid-response observations."


GRB_name: GRB140304A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15932
SUBJECT: GRB 140304A: MASTER OT light curve
DATE:    14/03/05 18:41:37 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Tunka was pointed to the  GRB140304A (Evans et. al GCN 15915) 
26 sec after notice time and 77 sec after trigger
time at 2014-03-04 13:23:49 UT.  We detect OT (Gorbovskoy et. al GCN 
15914) in two polarization bands during ~1 h while the source was brighter 
than our upper limit.
The preliminary photometry result available in table 1 and here 
http://master.sai.msu.ru/static/GRB/grb140304A.png  .

Table 1. Preliminary early GRB140304A observations.

T_start(JD)    T_trig-T_mid   Exptime   Mag1    Mag2   Coadd
2456721.05834       82            10    16.8    16.2    -
2456721.05931      172            30    17.2    16.9    -
2456721.06073      294            50    18.0    17.6    -
2456721.06142      358           120    18.1    17.6    2
2456721.06211      413            70    18.3    18.0    -
2456721.06724      894           580    18.5    18.5    4
2456721.08121      2070         1080    19.6    19.0    6
2456721.09812      3526         1080    19.9    19.4    6

Mag1 and Mag2 - Magnitude in two perpendicular polarizations.
The power low index alpha is 0.77+-0.05  (F ~ t-apha).


MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Blagoveschensk was pointed to the  GRB140304A  5 sec after 
notice time and 46 sec after trigger time at 2014-03-04 13:23:17 UT.
The observations  on this site made on bad weather conditions and on high 
zenith distance. The 5-sigma upper limit On our first (10s exposure) image 
has been about 13.0 mag.


The message may be cited.


GRB_name: GRB140305A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15934
SUBJECT: GRB 140305A: Swift-BAT refined analysis
DATE:    14/03/05 23:43:35 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

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), A. Maselli (INAF-IASFPA), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):

Using the data set from T-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140305A (trigger #590446)
(Maselli, et al., GCN Circ. 15929).  The BAT ground-calculated position is
RA, Dec = 344.497, 15.448 deg which is 
  RA(J2000)  =  22h 57m 59.4s 
  Dec(J2000) = +15d 26' 53.3" 
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 48%.

The mask-weighted light curve shows a FRED-like peak starting at T-1 sec, 
peaking at T+0 sec, and ending at T+20 sec.  
T90 (15-350 keV) is 13.7 +- 1.8 sec (estimated error including systematics).

The time-averaged spectrum from T-1.1 to T+16.3 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 0.32 +- 0.92, 
and Epeak of 70 +- 32 keV (chi squared 45.13 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 4.7 +- 0.7 x 10^-7 erg/cm2
and the 1-sec peak flux measured from T+0.18 sec in the 15-150 keV band is
1.0 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.49 +- 0.17 (chi squared 51.59 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/590446/BA/

[GCN OPS NOTE(05mar14):  Per author's request, the peak time was changed
from "T" to "T+0".]


GRB_name: GRB140306A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15935
SUBJECT: GRB 140306A: Fermi GBM detection
DATE:    14/03/06 11:44:43 GMT
FROM:    Gerard Fitzpatrick at UCD  <gerard.fitzpatrick@ucdconnect.ie>

G. Fitzpatrick (UCD) and M. Stanbro (UAH)
report on behalf of the Fermi GBM Team:

At 03:29:44.95 UT on 06 March 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140306A (trigger 415769387/140306146).
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 = 31.3 , DEC = +45.9 (J2000 degrees,
equivalent to 02h 05m, +45d 54.0'), with an uncertainty
of 1.00  degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).
The initial angle from the Fermi LAT boresight was 61  degrees.

The GBM light curve consists of several peak
with a duration (T90) of about 68 s (50-300 keV).
The time-averaged spectrum from T0-1.21601 s to T0+69.6s is
adequately fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.10 +/- 0.01   and
the cutoff energy, parameterized as Epeak, is 1580 +/- 100   keV

The event fluence (10-1000 keV) in this time interval is
(6.9 +/- 0.06)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+6.5 s in the 10-1000 keV band is 11.7 +/- 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: GRB140304A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15936
SUBJECT: GRB 140304A: 10.4m GTC refined redshift z = 5.283
DATE:    14/03/06 16:12:38 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

S. Jeong, R. Snchez-Ramrez (IAA-CSIC), J. Gorosabel (EHU-UPV,
IAA-CSIC) and A. J. Castro-Tirado (IAA-CSIC, UMA), on behalf of a larger
collaboration, report:

Once the calibration data have been available we have reduced again the
optical spectrum taken with the 10.4 m GTC (+OSIRIS) starting aprox. 8.2
hr postburst. At the host galaxy location for GRB 140304A, we find a
damped Ly-alpha system with log N(H) ~ 21.6 and z = 5.283. We also get
the same redshift from its metal lines that we interpret as SII, SiII,
SiII*, CII, CII*, SiIV and FeII. This value supersedes the preliminary
measurement given in GCNC 15922 (Jeong et al.) and is consistent the one
reported in GCNC 15924 (de Ugarte Postigo et al.).


GRB_name: GRB140304A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15937
SUBJECT: GRB 140304A: Continued RATIR Optical and NIR Observations
DATE:    14/03/06 16:57:05 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 observed the field of GRB 140304A (Evans, et al., GCN 15915) 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 2014/03 6.12 to 2014/03 6.14 UTC (37.55 to
38.08 hours after the BAT trigger), obtaining a total of 0.36 hours
exposure in the r and i bands and 0.15 hours exposure in the Z,
Y, J, and H bands.

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

  r     > 22.77
  i     > 22.60
  Z     20.88 +/- 0.20
  Y     > 20.96
  J     > 20.65
  H     > 20.31

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.  In the Z-band, the source has
faded as a powerlaw t^(-1.3) relative to our observations conducted last
night (Butler et al., GCN 15928).

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


GRB_name: GRB140306A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15938
SUBJECT: IPN Triangulation of GRB 140306A
DATE:    14/03/07 10:36:13 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,

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,

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

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

The long-duration, intense GRB 140306A (Fitzpatrick and Stanbro, GCN 
Circ. 15935) was observed by Fermi (GBM), INTEGRAL (SPI-ACS), 
Konus-Wind, MESSENGER (GRNS), Suzaku (WAM), Swift (BAT), and Mars 
Odyssey (HEND) at about 12585 s UT (03:29:45). 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:
    27.943 (01h 51m 46s) +48.975 (+48d 58' 31")
  Corners:
    28.544 (01h 54m 11s) +48.781 (+48d 46' 52")
    28.271 (01h 53m 05s) +49.135 (+49d 08' 06")
    27.339 (01h 49m 21s) +49.163 (+49d 09' 47")
    27.617 (01h 50m 28s) +48.814 (+48d 48' 50")
  ---------------------------------------------
The error box area is 0.209 sq. deg, and its maximum
dimension is 53 arcmin (the minimum one is 20 arcmin).

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB140306_T12581/IPN/


GRB_name: GRB140306A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15939
SUBJECT: Konus-Wind observation of GRB 140306A
DATE:    14/03/07 12:17:50 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 and T. Cline on behalf of the 
Konus-Wind team, report:

The long-duration GRB 140306A (localized by IPN: Golenetskii et al., GCN 
15938; GBM detection: Fitzpatrick, GCN 15935) triggered Konus-Wind at 
T0=12581.686 s UT (03:29:41.686).

The burst light curve shows an bright multi-peaked pulse with
a duration of ~75 s. The emission is seen up to ~8 MeV.

As observed by Konus-Wind, the burst had a fluence of (1.35 +/- 
0.12)x10^-4 erg/cm2, and a 256-ms peak flux, measured from T0+4.592 s,
of (2.3 +/- 0.2)x10^-5 erg/cm2/s (both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+78.848 s)
is best fit (in the 20 keV - 15 MeV range)
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -1.21 (-0.04, 0.05)
and Ep = 1305 (-210,+273) keV (chi2 = 106/98 dof).
Fit with the GRB (Band) model yields the same alpha and Ep,
and only an upper limit on the high energy
photon index: beta < -2.37 (chi2 = 106/97 dof).

The spectrum near the maximum count rate
(measured from T0 to T0+6.656 s)
is best fit (in the 20 keV - 15 MeV range)
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -0.77 (-0.05, 0.05)
and Ep = 1524 (-142,+158) keV (chi2 = 76/98 dof).
Fit with the GRB (Band) model yields the same alpha and Ep,
and only an upper limit on the high energy
photon index: beta < -2.74 (chi2 = 76/97 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140306_T12581/

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


GRB_name: GRB140306A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15940
SUBJECT: GRB 140306A: Suzaku WAM observation of the prompt emission
DATE:    14/03/09 07:28:58 GMT
FROM:    Tetsuya Yasuda at Saitama U  <yasuda@heal.phy.saitama-u.ac.jp>

T. Yasuda, M. Tashiro, Y. Terada, 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. E. Nakagawa, M. Kokubun,
T. Takahashi (ISAS/JAXA), W. Iwakiri (RIKEN), Y. Hanabata (ICRR), 
Y. Urata (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo)
on behalf of the Suzaku WAM team, report:


The bright long-duration GRB 140306A (localized by IPN: Golenetskii et al., GCN 15938;
and by Fermi-GBM: Fitzpatrick and Stanbro, GCN 15935; 
and Konus-Wind detection: Golenetskii et al., GCN 15939) 
triggered the Suzaku Wide-band  All-sky Monitor (WAM) which covers an 
energy range of 50 keV - 5 MeV at 03:29:44.404 UT (=T0). 

The observed light curve shows a multi-peaked structure starting at T0 and 
followed by a long weak tail seen up to T0+60 s with a duration (T90) of about 54 seconds. 
The fluence in 100 - 1000 keV was 5.38 (+0.09 / -0.13) x10^-5 erg/cm^2. 
The 1-s peak flux measured from T0+4.5 s was 6.86 (+0.25 / -0.36) photons/cm^2/s 
in the same energy range.

Preliminary result shows that the time-averaged spectrum from
T0-5 s to T0+60 s is well fitted by a power-law with exponential cutoff model:
dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
alpha       0.91 (+0.05 / -0.05), and
Epeak      1426 (+87 / -81) keV (chi^2/d.o.f. = 63.5/51).

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

The light curves for this burst are available at:

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


GRB_name: GRB140308A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15941
SUBJECT: IPN Triangulation of GRB 140308A
DATE:    14/03/09 12:10:25 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,

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,

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

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

The long-duration, intense GRB 140308A has been observed by Konus-Wind, 
Suzaku (WAM), MESSENGER (GRNS), Swift (BAT), and Mars Odyssey (HEND), so 
far, at about 13766 s UT (03:49:26). 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:
   357.561 (23h 50m 15s) -33.348 (-33d 20' 54")
  Corners:
   357.844 (23h 51m 23s) -33.006 (-33d 00' 20")
   357.443 (23h 49m 46s) -33.802 (-33d 48' 06")
   357.271 (23h 49m 05s) -33.688 (-33d 41' 17")
   357.673 (23h 50m 42s) -32.891 (-32d 53' 28")
  ---------------------------------------------
The error box area is 549 sq. arcmin, and its maximum
dimension is 56 arcmin (the minimum one is 11 arcmin).
The Sun distance was 29.6 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB140308_T13764/IPN/


GRB_name: GRB140304A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15942
SUBJECT: GRB 140304A: Suzaku WAM observation of the prompt emission
DATE:    14/03/10 07:14:31 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. E. Nakagawa, M. Kokubun, T. Takahashi (ISAS/JAXA), Y. Hanabata (ICRR),
Y. Urata (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo)
on behalf of the Suzaku WAM team, report:

The long GRB 140304A (Swift/BAT trigger #590206 ; Evans et al., GCN
15915; Fermi-GBM detection: Jenke and Fitzpatrick, GCN 15923) was
detected by the the Suzaku Wide-band All-sky Monitor (WAM) which covers
an energy range of 50 keV - 5 MeV at 13:22:33 UT (=T0).

The observed light curve shows a multi-peaked structure lasting from
T0-3 s to T0+11 s with a duration (T90) of about 12 seconds. The fluence
in 100 - 1000 keV was 1.69 (+0.32/-0.34) x10^-6 erg/cm^2.
The 1-s peak flux measured from T0-1 s was 0.48 (+0.28, -0.23)
photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-3 s to
T0+11 s is well fitted by a single power-law with a photon index of 2.09
(+0.66/-0.38) (chi^2/d.o.f = 12.3/14).

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

The light curves with 1-sec time resolution for this burst are available at:

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


GRB_name: GRB140308A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15943
SUBJECT: Konus-Wind observation of GRB 140308A
DATE:    14/03/10 20:15:26 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, and T. Cline on behalf
of the Konus-Wind team, report:

The bright long-duration hard-spectrum 140308A (IPN triangulation: 
Hurley et al., GCN 15941) triggered Konus-Wind at T0=13764.906 s UT 
(03:49:24.906).

The burst light curve shows a multi-peaked structure with a total 
duration of ~90 s. The emission is seen up to ~18 MeV.

As observed by Konus-Wind, the burst
had a fluence of (1.01 +/- 0.10)x10^-4 erg/cm2,
and a 256-ms peak flux, measured from T0+16.976 s,
of (8.7 +/- 1.6)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+65.024 s)
is best fit in the 26 keV - 18 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.81 (-0.15,+0.17),
the high energy photon index beta = -2.07 (-0.16,+0.11),
the peak energy Ep = 246 (-35, 45) keV,
chi2 = 109/97 dof.

The spectrum near the maximum count rate
(measured from T0+15.872 to T0+24.064 s)
is best fit in the 26 keV - 18 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.67 (-0.26,+0.29),
the high energy photon index beta = -2.06 (-0.26,+0.14),
the peak energy Ep = 228 (-43, 74) keV,
chi2 = 96/97 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140308_T13764/

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


GRB_name: GRB140311A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15944
SUBJECT: GRB 140311A: Swift detection of a probable burst
DATE:    14/03/11 21:20:47 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

J. L. Racusin (NASA/GSFC), W. H. Baumgartner (GSFC/UMBC),
N. Gehrels (NASA/GSFC), L. Izzo (URoma/ICRA), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), V. Mangano (PSU), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/PSU) and T. N. Ukwatta (MSU) report on behalf
of the Swift Team:

At 21:05:16 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140311A (trigger=591390).  Swift could not immediately
slew to the burst due to the Earth limb constraint. 
The BAT on-board calculated location is 
RA, Dec 209.301, +0.612 which is 
   RA(J2000) = 13h 57m 12s
   Dec(J2000) = +00d 36' 41"
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. 

Due to an observing constraint, Swift will not slew until T0+50.6
minutes. There will be no XRT or UVOT data until this time. 

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


GRB_name: GRB140311B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15945
SUBJECT: GRB 140311B: Swift detection of a burst
DATE:    14/03/11 21:36:02 GMT
FROM:    Judith Racusin at GSFC  <judith.racusin@nasa.gov>

J. L. Racusin (NASA/GSFC), W. H. Baumgartner (GSFC/UMBC),
N. Gehrels (NASA/GSFC), L. Izzo (URoma/ICRA), J. A. Kennea (PSU),
D. Malesani (DARK/NBI), F. E. Marshall (NASA/GSFC),
B. Sbarufatti (INAF-OAB/PSU) and T. N. Ukwatta (MSU) report on behalf
of the Swift Team:

At 21:14:29 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140311B (trigger=591392).  Swift could not immediately
slew to the burst due to the Earth limb constraint. 
The BAT on-board calculated location is 
RA, Dec 252.291, +52.747 which is 
   RA(J2000) = 16h 49m 10s
   Dec(J2000) = +52d 44' 50"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  We are awaiting information on the BAT 
light curve. 

Due to an observing constraint, Swift will not slew until T0+55
minutes. There will be no XRT or UVOT data until this time. 

The observation of this burst will delay the observation of GRB 140311A. 

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


GRB_name: GRB140311A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15946
SUBJECT: GRB 140311A: MASTER early optical observations 
DATE:    14/03/11 21:53:51 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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


MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Tunka was pointed to the  GRB140311A  27 sec after trigger time
and  127 sec after trigger
time at 2014-03-11 21:07:23 UT in two polarizations. On our first (30s
exposure) set we haven't found optical transient  within SWIFT error-box
(Racusin et. al GCN 15944).
The 5-sigma upper limit has been about 16.27mag


MASTER II  robotic telescope located in Blagoveschensk was pointed to the  GRB140311A 10 sec after
notice time and 89 sec after trigger time at 2014-03-11 21:06:45 UT in 
two polarizations.
On our first (20s exposure) set we haven't found optical transient  within
SWIFT error-box.
The 5-sigma upper limit has been about 14mag. The observations made on the
morning sky.
The message may be cited.


GRB_name: GRB140311A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15947
SUBJECT: GRB 140311A: Nanshan OT detection
DATE:    14/03/11 21:56:00 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

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

We observed the BAT error circle of GRB 140311A (Racusin et al., GCN
15944) using the 1m telescope located in Nanshan, Xinjiang, China.
Observations started at 21:26:44 UT on 2014-03-11 and some R-band
frames were obtained.

A seemingly varying optical source is clearly detected in each image
at coordinates

R.A. (J2000) = 13:57:13.27
Dec. (J2000) = +00:38:31.07

Uncertainty radius: ~1 aecsec

This object is not present in both SDSS and DSS. We thus suggest it
may be the afterglow of the burst.

Observations are ongoing.


GRB_name: GRB140311B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15948
SUBJECT: GRB 140311B: MASTER early optical observations
DATE:    14/03/11 22:02:51 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Tunka was pointed to the  GRB140311B 29 sec after notice time 
and 107 sec after trigger time at 2014-03-11 21:16:16 UT in two 
polarizations. On our first (20s exposure) set we haven't found optical 
transient  within SWIFT error-box (Racusin et. al. GCN 15945). The 5-sigma 
upper limit has been about 17.0 mag. The observations is proceed.

MASTER II  robotic telescope located in Blagoveschensk was pointed to the 
GRB140311B 9 sec after notice time and 85 sec after trigger time at 
2014-03-11 21:15:54 UT in two polarizations. On our first (20s exposure) 
set we haven't found optical transient  within SWIFT error-box.
The 5-sigma upper limit has been about 14.0 mag. The observations on this 
place made on the bright morning sky.

The message may be cited.

[GCN OPS NOTE(12mar14): Per author's request, the Subject was changed
from "MASTER OT light curve (fwd)" to "MASTER early optical observations".]


GRB_name: GRB140311B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15949
SUBJECT: GRB 140311B: Nanshan afterglow detection
DATE:    14/03/11 22:52:01 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

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

We observed the field of  GRB 140311B (Racusin et al., GCN 15945)
using the 1m telescope located in Nanshan, Xinjiang, China.
Observations started at 21:41:05 UT on 2014-03-11 and some 300s/600s
R-band frames were obtained.

The afterglow is detected in each image within the XRT error circle
(http://www.swift.ac.uk/sper/) at coordinates

R.A. (J2000) = 16:49:17.97
Dec. (J2000) = +52:43:26.41

Uncertainty radius: ~1.5 aecsec

The first 300s image reveals that the afterglow has m(R)=20.6 at 29.1
min post-burst, calibrated with nearby two SDSS stars.

Observations are ongoing.


GRB_name: GRB140311B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15950
SUBJECT: GRB 140311B: Swift-XRT observations
DATE:    14/03/11 23:07:34 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

The XRT began observing the field of GRB 140311B at 22:11:04.3 UT,
3394.7 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source located at RA, Dec 252.32458,
52.72393 which is equivalent to:
   RA(J2000)  = 16h 49m 17.90s
   Dec(J2000) = +52d 43' 26.1"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 110 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 3.03
x 10^20 cm^-2 (Kalberla et al. 2005). 


GRB_name: GRB140311B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15951
SUBJECT: GRB140311B: Swift/XRT position
DATE:    14/03/11 23:08:55 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia (ASDC), L. Izzo (URoma/ICRA) and J. Racusin (NASA/GSFC) report:

XRT began observing GRB140311B (Racusin et al. GCN 15945) 55 minutes  
after the trigger.

Using promptly downlinked data we find a bright uncatalogued X ray  
source located at RA,Dec = 252.3242, 52.7240 which is equivalent to:

RA (J2000) = 16 49 17.81
DEC (J2000) = +52 43 26.4

with an uncertainty of 3.6 arcsec (radius, 90% containment). This  
location is 109.6 arcsec from the BAT position, inside the BAT error  
circle.

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

----------------------------------------------------------------
This message was sent using IMP, the Internet Messaging Program.


GRB_name: GRB140311A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15952
SUBJECT: GRB 140311A: Zadko observatory - Gingin optical observations
DATE:    14/03/12 00:10:54 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 140311A detected by SWIFT
(trigger 591390) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 119.5s after the GRB trigger
(46.9s after the notice). The elevation of the field was at
45 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 OT discovered by Xu et al. GCNC 15947
with a limiting magnitude of:

t0+119.5s to t0+179.5s : Rlim = 19.5

The second image is 30.0s exposure in tracking mode
We detect the OT discovered by Xu et al. GCNC 15947:
t0+208s to t0+238s : R = 19.6 +/- 0.5

Follow-up was performed until the dawn which arrived
18 minutes after the trigger.

We co-added a series of exposures:
t0+208s to t0+325s : R = 19.9 +/- 0.3
t0+338s to t0+515s : R = 19.2 +/- 0.3
t0+530s to t0+1111s : R = 18.5 +/- 0.3

Conclusions, the afterglow brightness increases
slowly during the first 18 minutes after the trigger.

Magnitudes were estimated with the nearby star
NOMAD1 0906-0229793 (R=16.44) and are not corrected
for galactic dust extinction.


GRB_name: GRB140311A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15953
SUBJECT: GRB 140311A: NOT observations of the optical afterglow
DATE:    14/03/12 00:36:08 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, A. Melandri (INAF-OAB), D. Malesani (Dark/NBI), T. Pursimo (NOT), M. C. Baglio, I. Andreoni (INAF-OAB) report on behalf of the CIBO collaboration:

We observed the field of GRB 140311A (Racusin et al. GCN 15944) with the Nordic Optical Telescope (NOT) equipped with ALFOSC. 
The optical afterglow reported by Xu et al. (GCN 15947) and Klotz et al. (GCN 15952) is detected in the R band at 21.1 +/- 0.2 mag (calibrated against the USNOB1 catalogue) at t-t0=2.6 hours.


GRB_name: GRB140311A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15954
SUBJECT: GRB 140311A: Optical follow-up observation with Kottamia 188cm telescope
DATE:    14/03/12 00:41:43 GMT
FROM:    Michitoshi Yoshida at HASC,Hiroshima U  <yoshidam@hiroshima-u.ac.jp>

M. Yoshida, R. Itoh, Y. Moritani (HASC, Hiroshima Univ.),
G. B. Ali, A. Essam, A. Takey, and G. Hamed (NRIAG, Egypt)

We made an optical follow-up observation of GRB 140311A (Racusin
et al. GCN 15944) with the Newtonian CCD camera attached to the
188cm telescope at Kottamia astronomical observatory of NRIAG in
Egypt. We started the observation at 22:08:26 UT on Marth 11 2014;
1.053 hours after the trigger. We combined six 300 sec exposure
R-band frames and detected a faint point source at the position
of the optical transient reported by Xu et al. (GCN 15947).

Rough photometric result of the source is shown below. We used the
nearby star NOMAD1 0906-022793 (Klotz et al. GCN 15952) for flux
calibration.

 MID-UT    T-EXP[sec]  R[mag]  err[mag]
----------------------------------------
 23:19:29  1800.0      21.9    +- 0.3
----------------------------------------


GRB_name: GRB140311B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15955
SUBJECT: GRB 140311B: TAROT Calern observatory optical observations
DATE:    14/03/12 00:42:49 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

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

We imaged the field of GRB 140311B detected by SWIFT
(trigger 513505) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 5 minutes after the GRB trigger
The elevation of the field increased from
20 degrees above horizon and weather conditions
were good.

The first image is 60.0s exposure in tracking mode.
We do not detect the OT discovered by Xu et al.
(GCNC 15949) with a limiting magnitude of:
t0+246s to t0+306s : Rlim = 17.3

We co-added a series of exposures:
We do not detect the OT with limiting magnitudes of:
t0+246s to t0+511s : Rlim = 17.8
t0+541s to t0+1568s : Rlim = 18.4

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

N.B. Galactic coordinates are lon= 80.3934 lat=+39.5637
and the galactic extinction in R band is about 0.2 magnitude
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.


GRB_name: GRB140311A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15956
SUBJECT: GRB 140311A: Nanshan afterglow decay
DATE:    14/03/12 00:51:27 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

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

The previously reported afterglow candidate (Xu et al., GCN 15947) has
been decaying throughout our R-band observations. Part of the
photometry are listed below

Tmid (hr)   Mag(R)  MagErr(R)
2.06778     21.06      0.10
1.53056     20.80      0.10
0.49306     19.96      0.10

All magnitude are calibrated with the following three SDSS stars using
Lupton (2005) transformation:
SDSS J135709.54+003731.9   m(r)=16.81, m(i)=16.30
SDSS J135716.45+003657.3   m(r)=16.41, m(i)=16.10
SDSS J135713.38+003942.0   m(r)=18.57, m(i)=18.47

Together with measurements in Klotz et al. (GCN 15952) and D'Avanzo et
al. (GCN 15953), it shows that the optical afterglow peaks at ~0.23 hr
post-burst and is decaying roughly as F(t) ~ t^-0.75 since ~0.5 hr
post-burst.


GRB_name: GRB140311A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15957
SUBJECT: GRB 140311A: Recalibration of photometry of OT detected with Kottamia 188cm telescope
DATE:    14/03/12 01:06:41 GMT
FROM:    Michitoshi Yoshida at HASC,Hiroshima U  <yoshidam@hiroshima-u.ac.jp>

M. Yoshida, R. Itoh, Y. Moritani (HASC, Hiroshima Univ.),
G. B. Ali, A. Essam, A. Takey, and G. Hamed (NRIAG, Egypt)

We performed recalibration of the photometry of the OT of GRB 140311A
(Racusin et al. GCN 15944), and found that the R-band magnitude we
previously reported (Yoshida et al. GCN 15954) is about 1 magnitude
fainter than the newly calibrated value. The recalibration result is
as follows:

 MID-UT    T-EXP[sec]  R[mag]  err[mag]
----------------------------------------
 23:19:29  1800.0      20.9    +- 0.3
----------------------------------------


GRB_name: GRB140311B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15958
SUBJECT: GRB 140311B: Enhanced Swift-XRT position
DATE:    14/03/12 02:30:17 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 2577 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 140311B, 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 = 252.32518, +52.72426 which is equivalent
to:

RA (J2000): 16h 49m 18.04s
Dec (J2000): +52d 43' 27.3"

with an uncertainty of 1.7 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB140311A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15959
SUBJECT: GRB 140311A: Enhanced Swift-XRT position
DATE:    14/03/12 09:56:51 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Using 1977 s of XRT Photon Counting mode data and 4 UVOT
images, we find an astrometrically corrected X-ray position (using the
XRT-UVOT alignment and matching UVOT field sources to the USNO-B1
catalogue): RA, Dec =
209.30516, 0.64193 which is equivalent to:

RA (J2000):  13 57 13.24
Dec (J2000): +00 38 31.0

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

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

This position is 0.5 arc sec from the optical counterpart reported by
Xu et al (GCN Circ. 15947), thus we believe this is the X-ray afterglow.

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


GRB_name: GRB140311B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15960
SUBJECT: GRB 140311B: final MASTER OT light curve
DATE:    14/03/12 10:53:33 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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


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

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

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

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

MASTER-II robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Tunka was pointed to the  GRB140311B  (Racusin et al., GCN 
15945) 29 sec after notice time and 107 sec after trigger time (Gorbovskoy 
et. al GCN 15948 ) and  made observations during ~ 1.5 h before sunrise.
We see OT  (Xu et. al.  GCN 15949) only on several coadditional images. On 
all of them the object is close to  limit  and has s/n from 3 to 6.
Our preliminary ligth curve available in table below and on image here 
http://master.sai.msu.ru/static/GRB/grb140311B.png.

T_start       T_t-T_m  Exptime   Mag.   Coadd
                 [s]     [s]      [m]
21:17:12        326      220     19.4     4
21:18:18        432      300     19.0     4
21:16:16        557      650     19.4     8
21:19:44        557      380     18.7     4
21:19:44        661      550     18.9     5
21:21:19        708      490     18.9     4
21:18:18        834      960     19.4     8
21:25:40       1485     1380     19.8     8
21:25:40       1702     1740     20.0    10

T_t is GRB trigger time, T_m is middle time of our exposure.
Our unfiltered magnitude is well described by a parity 0.8R + 0.2B (USNO 
B1)

The power low index alpha from 380 to 1740 seconds after the trigger  is 
1.07+-0.10  (F ~ t-apha).

We also apologize for an error in the title of our previous telegram (GCN 
15948) if it misled somebody.


The message may be cited.


GRB_name: GRB140311A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15961
SUBJECT: GRB 140311A: Gemini-South redshift
DATE:    14/03/12 11:51:40 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. Cucchiara (NASA/GSFC) report:

We observed the afterglow of GRB 140311A (Racusin et al. GCN 15944;
Xu et al. GCN 15947) with Gemini-South using the GMOS-S spectrograph,
beginning March 12 08:24 UT, approximately 11.3 hours post-trigger.
The spectrograph was configured to cover wavelength range from
about 4000 AA to 6700 AA.

The optical trace of the afterglow is clearly detected, with many
absorption lines suggesting we are only seeing the region
blueward of Ly-alpha in the rest frame.  Based on several strong 
absorption features and a break, which would correspond to Ly-beta, 
Ly-gamma, Ly-delta and the Ly-limit at approximately z=4.95, we 
conclude this is likely to be the redshift of the GRB. Further
analysis of the spectrum is ongoing.

We thank the observatory staff, particularly Peter Pessev,
for excellent support in obtaining these observations.


GRB_name: GRB140311A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15962
SUBJECT: GRB 140311A: Swift-BAT refined analysis
DATE:    14/03/12 12:37:56 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.krimm@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), J. L. Racusin (NASA/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-239 to T+423 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140311A (trigger #591390)
(Racusin, et al., GCN Circ. 15944).  The BAT ground-calculated position is
RA, Dec = 209.293, 0.607 deg which is
    RA(J2000)  =  13h 57m 10.4s
    Dec(J2000) = +00d 36' 23.9"
with an uncertainty of 3.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 10%.

The mask-weighted light curve shows two weak peaks, the first from roughly T-5 
sec to T+5 sec and the second from approximately T+40 to T+60 sec. T90 (15-350 
keV) is 71.4 +- 9.5 sec (estimated error including systematics).

The time-averaged spectrum from -4.456 to 83.736 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.67 +- 0.23.  The fluence in the 15-150 keV band is 2.3 +- 0.3 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-2.40 sec in the 15-150 keV band
is 1.3 +- 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/591390/BA/


GRB_name: GRB140311B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15963
SUBJECT: GRB 140311B: Swift-XRT refined Analysis
DATE:    14/03/12 13:20:17 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

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

We have analysed 7.8 ks of XRT data for GRB 140311B (Racusin  et al.
GCN Circ. 15945),  from 3.4 ks to 46.3 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Evans et al. (GCN Circ. 15958).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.66 (+0.18, -0.15).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.68 (+0.25, -0.23). The
best-fitting absorption column is  1.6 (+0.9, -0.8) x 10^21 cm^-2, in
excess of the Galactic value of 3.6 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.1 x 10^-11 (4.9 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.6 (+0.9, -0.8) x 10^21 cm^-2
Galactic foreground: 3.6 x 10^20 cm^-2
Excess significance: 2.7 sigma
Photon index:      1.68 (+0.25, -0.23)

If the light curve continues to decay with a power-law decay index of
1.66, the count rate at T+24 hours will be 9.6 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.0 x
10^-14 (4.8 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/00591392.

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


GRB_name: GRB140311A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15964
SUBJECT: GRB 140311A: NOT redshift confirmation
DATE:    14/03/12 13:37:59 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

P. D'Avanzo (INAF-OAB), V. D'Elia (INAF-OAR/ASI-ASDC), S. Piranomonte  
(INAF-OAR), A. Melandri (INAF-OAB), D. Malesani (DARK/NBI), T. Pursimo  
(NOT), M. C. Baglio, I. Andreoni (INAF-OAB) report on behalf of the  
CIBO collaboration:

Following the detection of the optical afterglow reported in D'Avanzo  
et al. (GCN 15953), we carried out optical spectroscopy of GRB 140311A  
(Racusin et al. GCN 15944) with the Nordic Optical Telescope (NOT)  
equipped with ALFOSC. The observation consisted of two 1800 s  
exposures covering the range between 3200 and 9100 A carried out at a  
mean t-t0=3.37 hours.

Despite the low SNR and a seeing of ~2, we detect broad absorption  
features at lambda ~ 7300 and 6100 AA which we interpret as Ly-alpha  
and Ly-beta at z ~ 5.

This is consistent with the redshift reported by Tanvir et al(GCN 15961).

----------------------------------------------------------------
This message was sent using IMP, the Internet Messaging Program.


GRB_name: GRB140302A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15965
SUBJECT: GRB 140302A: GROND confirmation of the afterglow
DATE:    14/03/12 14:08:14 GMT
FROM:    Jonny Elliott at MPE/GROND  <jonnyelliott@mpe.mpg.de>

J. Elliott (MPE Garching), S. Schmidl (TLS Tautenburg), J.Greiner, J. F.
Graham, M. Tanga (all MPE Garching) report on behalf of the GROND team:

We re-observed the field of GRB 140302A (Swift trigger 589685; Pagani et
al., GCN #15901) 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 07:18 UT on 4th March 2014, 2 days after the GRB
trigger. They were performed at an average seeing of 1.1" and at an
average airmass of 1.3.

We no longer detect the source noted in our previous observations (Elliott
et al.; GCN #15903) that had a magnitude of r' = 23.7 +/- 0.2 mag. For a
total exposure of 1.2 hours we obtain an upper limit (AB) of r' > 25.2 mag
and confirm this as the afterglow of GRB 140302A.

The given limit is derived based on calibrating the image against GROND
zeropoints and is not corrected for the Galactic foreground extinction
corresponding to a reddening of E(B-V)= 0.52 mag in the direction of the
burst (Schlegel et al. 1998).


GRB_name: GRB140311A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15966
SUBJECT: GRB 140311A: Gemini-North redshift
DATE:    14/03/12 16:33:51 GMT
FROM:    Ryan Chornock at Harvard  <rchornock@cfa.harvard.edu>

R. Chornock (Harvard), D. B. Fox (Penn State), N. R. Tanvir (U. Leicester), and 
E. Berger (Harvard) report:

We obtained 2x900s of spectroscopy of the optical afterglow (Xu et al., GCN 
15947) of GRB 140311A (Racusin et al., GCN 15944) using GMOS on the 8-m Gemini-N 
telescope beginning at 12:56 UT on March 12. We used the R831 grating to cover 
the wavelength range of 6950-9075 Angs at a resolution of approximately 2.8 
Angs. Our data exhibit a broad damped Lyman-alpha feature centered near 7250 
Angs (redshift~4.95), in agreement with previous reports from Gemini-South 
(Tanvir et al., GCN 15961) and NOT (D'Avanzo et al., GCN 15964).  In addition, 
we detect many metal lines, including C II, C II*, O I, O I*, Si II, Si II*, and 
Si IV at a common redshift of 4.954, which we adopt as the redshift of the GRB.

We thank the Gemini staff, particularly Jesse Ball, for their excellent 
assistance in obtaining these data.


GRB_name: GRB140311A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15968
SUBJECT: GRB 140311A: Swift-XRT refined Analysis
DATE:    14/03/12 17:02:28 GMT
FROM:    Luca Izzo at ICRA  <Luca.Izzo@ICRA.it>

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

We have analysed 6.2 ks of XRT data for GRB 140311A (Racusin  et al.
GCN Circ. 15944),  from 9.5 ks to 57.1 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. Using 2850 s of PC mode
data and 7 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 = 209.30521, +0.64191 which is equivalent to:

RA (J2000): 13h 57m 13.25s
Dec(J2000): +00d 38' 30.9"

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

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.13 (+0.16, -0.14).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.61 (+0.17, -0.12). The
best-fitting absorption column is  consistent with the Galactic value
of 2.8 x 10^20 cm^-2 (Kalberla et al. 2005). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 3.9 x 10^-11 (4.1 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 2.8 x 10^20 cm^-2
Intrinsic column:    0 (+2.2, -0) x 10^22 cm^-2 at z=4.95
Photon index:      1.61 (+0.17, -0.12)

If the light curve continues to decay with a power-law decay index of
1.13, the count rate at T+24 hours will be 0.013 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.1 x
10^-13 (5.3 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/00591390

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


GRB_name: GRB140311A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15969
SUBJECT: GRB 140311A: Bassano Bresciano Observatory optical upper limit
DATE:    14/03/12 17:12:37 GMT
FROM:    Ulisse Quadri at Bassano Bresciano Obs  <oabb@ulisse.bs.it>

U.Quadri, L.Strabla and R.Girelli report:

We imaged the field of GRB 140311A detected by SWIFT(trigger 591390)
with the robotic telescope of (IAU station 565) Bassano Bresciano 
Observatory, Italy (member of ISSP:Italian Supernovae Search Project)

The observations started 1.89 hour after the GRB trigger,  
with our Newton telescope D=250 mm F/D=5.

Weather conditions were good.

We co-added 15 exposures of 120 sec each.

We did not found any optical counterpart
in the error box of the XRTcandidate.
(J. L. Racusin (NASA/GSFC) et al, GCN 15944)

Start T0+      End T0+      R.Lim
1.89 hour     2.37 hour     18.5

Magnitudes were estimated with the USNO-B1.0 cat. 
and are not corrected for galactic dust extinction.

The message may be cited.


GRB_name: GRB140311B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15970
SUBJECT: GRB 140311B: RATIR Optical and NIR Observations
DATE:    14/03/12 17:17:37 GMT
FROM:    Owen Littlejohns at Az State U  <olittlej@asu.edu>

Owen Littlejohns (ASU), Antonino Cucchiara (ORAU/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), 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 140311B (Racusin, et al., GCN 15945)
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
2014/03 12.37 to 2014/03 12.52 UTC (11.52 to 15.25 hours after the
BAT trigger), obtaining a total of 2.84 hours exposure in the r and
i bands and 1.19 hours exposure in the Z and Y bands.

For a source within the Swift-XRT error circle, in comparison with
the SDSS DR9 and 2MASS, we obtain the following upper limits (3-sigma):

  r     > 23.99
  i     > 23.82
  Z     > 22.85
  Y     > 22.26

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB. In comparison to the earlier
detection of the optical afterglow (Xu, et al., GCN 15949) the GRB has
faded. A power-law temporal decay with an index of alpha = -0.94 or
steeper is required for our r-band upper limit to be consistent with the
earlier detection.

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


GRB_name: GRB140311B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15972
SUBJECT: GRB 140311B: Swift/UVOT Upper Limits
DATE:    14/03/12 19:26:59 GMT
FROM:    Stephen Holland at STScI  <sholland@stsci.edu>

S. T. Holland (STScI) and J. L. Racusin (NASA/GSFC) report on behalf
of the Swift/UVOT team:

    The Swift/UVOT began settled observations of the field of GRB
140311B 3398 s after the BAT trigger (Racusin et al. 2014, GCNC
15945). We do not detect any new source consistent with the Nansan
afterglow position (Xu et al. 2014, GCNC 15949) 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
---------------------------------------------------
white (FC)      3398      3548        147     >21.2
---------------------------------------------------
v               3555      5191        393     >20.0
b               4375      5990        372     >20.4
u               4170      5806        393     >20.2
uvw1            3965      5601        393     >20.3
uvm2            3760      5396        393     >20.2
uvw2            4787      4986        197     >20.1
white           4580      4780        197     >21.4
---------------------------------------------------

    The quoted upper limits have not been corrected for the expected
extinction due to the Galactic reddening along the line of sight to
this burst of E(B-V) = 0.05 mag (Schlafly et al. 2011, ApJS, 737,
103).


GRB_name: GRB140311A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15973
SUBJECT: GRB 140311A: Swift/UVOT Upper Limits
DATE:    14/03/12 19:27:01 GMT
FROM:    Stephen Holland at STScI  <sholland@stsci.edu>

S. T. Holland (STScI) and J. L. Racusin (NASA/GSFC) report on behalf
of the Swift/UVOT team:

    The Swift/UVOT began settled observations of the field of GRB
140311A 9540 s after the BAT trigger (Racusin et al. 2014, GCNC
15944). We do not detect any new source consistent with the Nansan
afterglow position (Xu et al. 2014, GCNC 15947) 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 summed exposures are presented below.

---------------------------------------------------
Filter        TSTART     TSTOP   Exposure       Mag
---------------------------------------------------
v            11,358     11,533        171     >19.0
b            37,852     38,759        885     >21.3
uvw1         40,124     40,366        238     >19.8
uvw2         10,542     11,352        886     >21.2
white          9540     10,446        885     >22.0
---------------------------------------------------

    The quoted upper limits have not been corrected for the expected
extinction due to the Galactic reddening along the line of sight to
this burst of E(B-V) = 0.03 mag (Schlafly et al. 2011, ApJS, 737,
103). The non-detection in the UVOT data is consistent with a redshift
of z = 4.95 (Tanvir et al, 2014, GCNC 15961).


GRB_name: GRB140311A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15974
SUBJECT: GRB 140311A: Kottamia I-band observation
DATE:    14/03/12 19:43:56 GMT
FROM:    Michitoshi Yoshida at HASC,Hiroshima U  <yoshidam@hiroshima-u.ac.jp>

M. Yoshida, R. Itoh, Y. Moritani (HASC, Hiroshima Univ.),
G. B. Ali, A. Essam, A. Takey, and G. Hamed (NRIAG, Egypt)

We report the I-band photometry of GRB 140311A. The observation
was performed with the Newtonian camera of the 188cm telescope
at Kottamia observatory just before the R-band observation
reported by Yoshida et al. (GCN 15954; 15957). We started the
I-band observation at 21:57:30 UT on Marth 11 2014; 0.8706 hours
after the trigger.

Photometric result of the source is shown below. We used the
nearby star NOMAD1 0906-0229809 for flux calibration.

             MID-UT   T-EXP[sec]  I[mag]  err[mag]
---------------------------------------------------
 2014-03-11 22:02:45  300.0 x 2   19.0    +- 0.1
---------------------------------------------------


GRB_name: GRB140311B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15975
SUBJECT: GRB 140311B: Fermi GBM Detection
DATE:    14/03/12 20:40:40 GMT
FROM:    Matthew Stanbro at UAH/Fermi  <mcs0001@uah.edu>

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

"At 21:14:35.65 UT on 11 March 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140311B (trigger 416265278/140311885),
which was also detected by Swift (J. L. Racusin et al. 2014, GCN 15945).
The GBM on-ground location, using the Fermi GBM trigger
data, is consistent with the Swift/BAT location.The angle to the
Fermi LAT boresight is 110 deg. from Swift location.

The GBM light curve consists of several overlapping peaks with a
combined duration (T90) of 72 s (50-300 keV).
The time-averaged spectrum from T0-3 s to T0+69 s is
well fit by a power law function with an exponential
 high energy cutoff. The power law index is -0.5 +/- 0.1
and the high energy cutoff, parameterized as
Epeak, is 117 +/- 8 keV.

The event fluence (10-1000 keV) in this time interval is
(7.9 +/- 0.4)E-06 erg/cm^2. The 1.0-sec peak photon flux measured
starting from T0+0.6 s in the 10-1000 keV band
is 3.2 +/- 0.3 ph/s/cm^2.

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


GRB_name: GRB140311A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15976
SUBJECT: GRB 140311A: Montarrenti Observatory optical upper limit
DATE:    14/03/12 22:20:45 GMT
FROM:    Simone Leonini at Monarrenti Obs  <s.leonini@iol.it>

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

We observed the field of GRB140311A (Swift trigger 591390, Racusin et al., GCN 
Circ. 15944) with the automatic 0.53m RC telescope + U47 detector at 
Montarrenti Observatory (Siena, Italy, IAU code C88). 

The observations were started at 2014-03-12 00:20:19 UT (approximately 3 hours 
post-burst) stacking 5 unfiltered CCD exposures of 60s each.

We have not found optical transient within the error-box given by Swift. 

Mag. upper limit R = 20.02+/-0.16

Magnitudes were obtained using Astrometrica software using USNO-B1 catalogue 
and are not corrected for galactic extinction.

The message may be cited.


GRB_name: GRB140311C
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15977
SUBJECT: GRB 140311C: Fermi GBM Detection
DATE:    14/03/12 22:28:45 GMT
FROM:    Matthew Stanbro at UAH/Fermi  <mcs0001@uah.edu>

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

"At 14:49:13.10 UT on 11 March 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140311C (trigger 416242156/140311618).
iPTF reported an optical counterpart candidate for this
source (L.P. Singer et al. 2014, GCN 15971).

The GBM on-ground location, using the Fermi GBM trigger data,
is RA = 183.7 , DEC = +62.81 (J2000 degrees, equivalent to
12h 14m, 62d 48'), with an uncertainty of 3 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 to the Fermi LAT boresight is 53 deg.

The GBM light curve consists of single peak with a
duration (T90) of 14 s (50-300 keV).
The time-averaged spectrum from T0-2 s to T0+12 s is
well fit by a Band function parameterized as Epeak = 56 +/- 6 keV,
alpha = -0.9 +/- 0.16 and beta = -2.4 +/- 0.12.

The event fluence (10-1000 keV) in this time interval is
(4.6 +/- 0.2)E-06 erg/cm^2. The 1.0-sec peak photon flux measured
starting from T0+0.3 s in the 10-1000 keV band
is 10.7 +/- 0.4 ph/s/cm^2.

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


GRB_name: GRB140311A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15978
SUBJECT: GRB 140311A: RATIR Optical and NIR Detection
DATE:    14/03/13 00:11:31 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 140311A (Racusin, et al., GCN 15944) 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 2014/03 12.24 to 2014/03 12.36
UTC (8.75 to 11.51 hours after the BAT trigger), obtaining a total of
2.10 hours exposure in the r and i bands and 0.89 hours exposure in the
Z and Y bands.

For a source within the Swift-XRT error circle (Evans, et al., GCN
15959), in comparison with the SDSS DR9 and 2MASS, we obtain the
following detections:

  r     22.33 +/- 0.13
  i     21.56 +/- 0.08
  Z     20.58 +/- 0.08
  Y     20.09 +/- 0.08

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB. The source has faded in comparison
to observations from other facilities (D'Avanzo et, al., GCN 15953),
requiring a power-law with a temporal decay index of alpha = -0.83.

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


GRB_name: GRB140311B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15979
SUBJECT: GRB 140311B: Swift-BAT refined analysis
DATE:    14/03/13 03:07:06 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

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

Using the data set from T-0 to T+3 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140311B (trigger #591392)
(Racusin, et al., GCN Circ. 15945).  The BAT ground-calculated position is
RA, Dec = 252.333, +52.733 deg which is
    RA(J2000)  =  16h 49m 20.0s
    Dec(J2000) = +52d 44' 00"
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 89%.

This trigger followed that of GRB 140311A by only about 9 minutes, which led
to a complication in recording the photon-event data.  Only 3 seconds of
photon-event data was recorded, so no mask-weighted lightcurve is available.
T90 (15-350 keV) is estimated to be 70 +- 10 sec.  The burst had multiple
peaks.  Peak emission occurred about 15 seconds after the trigger time.

The time-averaged spectrum for the limited range of data available (about
5% of T90) from T+0 to T+3 sec is best fit by a simple power-law model.  The
power law index of the time-averaged spectrum is 1.12 +- 0.15 (90% confidence).
Because of the lack of event data, the fluence is not available.  Based on an
eye-ball estimate comparing the non-maskweighted lightcurve to those of other
bursts with a similar partial coding, the fluence in the 15-150 keV band was on
the order of several times 10^-6 ergs/cm^2


GRB_name: GRB140311A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15980
SUBJECT: GRB 140311A: further NOT observations
DATE:    14/03/13 10:30:24 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Malesani (DARK/NBI), P. D'Avanzo (INAF/Brera), Y. F. Martinez Osorio 
(NOT and Univ. Uppsala), report on behalf of the CIBO collaboration:

We observed the optical afterglow of GRB 140311A (Racusin et al., GCN 
15944; Xu et al., GCN 15947) with the Nordic Optical Telescope equipped 
with ALFOSC. A total exposure of 24 min was secured in the SDSS i band.

At a mean epoch of March 13.043 UT (1.16 days after the GRB), the 
optical counterpart is well detected with an AB magnitude i = 22.45 +- 
0.08, calibrated to several nearby SDSS stars. The position of the 
afterglow is (J2000):

RA = 13:57:13.29
Dec = +00:38:31.7

referenced to the USNO-B1 catalog (0.3" error).

Compared to the i-band value reported by Littlejohns et al. (GCN 15978), 
our measurement implies a decay index alpha = 0.81 +- 0.10 (Fnu propto 
nu^-alpha), consistent with the value reported by these authors.


GRB_name: GRB140311C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15981
SUBJECT: GRB 140311C: MASTER before, during and after trigger optical observations 
DATE:    14/03/13 15:55:07 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  GRB140311C (M. Stanbro, 
GCN15977) 14 sec after 
notice time and 29 sec after trigger time at 2014-03-11 14:49:42.721 UT . 
On our first (10s exposure) set we haven't found optical transient  within 
FERMI error-box (ra=12 47 02 dec=+58 49 46 FOV=2x4 square degrees).
The 5-sigma upper limit has been about 16.3 mag

MASTER II  robotic telescope located in Tunka was pointed to the
GRB140311C (M. Stanbro,GCN15977) 35 sec after trigger time at 2014-03-11 
14:49:48.874 UT.
On our first (10s exposure) set we haven't found optical transient  within
FERMI error-box (ra=12 47 02 dec=+58 49 46 FOV=2x4 square degrees).
The 5-sigma upper limit has been about 16.0 mag.

We have done survey of the large area around initial error box up to ~18 
unfiletred magnitude which was begun in 15 minutes after GRB.

The GBM error box (M. Stanbro, GCN15977) completely observed by 4-th Very 
Wide Field Cameras (FOV = 4x380 square degrees) before, during and after 
GRB without time gap up to 11 unfiltered magnitude limit on each 5 sec 
image. The reduction is continued now.

The IPN is very desirable.

The covarege map is available at 
http://master.sai.msu.ru/static/GRB/GRB140311C_map.png . The elliptical 
region is the Fermi GBM 1 sigma+3 degrees systematic error box.

The message may be cited.


GRB_name: GRB140311C
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15982
SUBJECT: GRB 140311C: Swift-XRT and UVOT observations
DATE:    14/03/13 18:05:25 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

V. D'Elia (ASDC), L.M.Z. Hagen (PSU), L. Izzo (URoma/ICRA), P.  
D'Avanzo (INAF-OAB), S. Holland (STScI) report on behalf of the Swift  
team:


We report on Swift observations of the field of the GBM discovered  
GRB140311C burst (Stanbro, GCN Circ 15977), for which a possible  
optical counterpart was reported by iPTF (Singer et al., GCN Circ  
15971).

XRT began observing the field on 2014-03-12 at 23:43:48 UT, i.e., 118  
ks after the trigger, for a total of 2.7ks. No source is detected at  
the iPTF coordinates, nor in the whole XRT field of view. The 3-sigma  
upper limit on the count rate is 5E-03 cts/s.

The Swift/UVOT began settled observations of the field of GRB 140311C  
118480 s after the trigger. No optical afterglow consistent with the  
iPTF position (Singer et al., GCN Circ. 15971) is detected in the  
initial UVOT exposure. The preliminary 3-sigma upper limit using the  
UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358,  
373) for the initial exposures are:

Filter T_start(s) T_stop(s) Exp(s) Mag
u 118480 125414 2916 >21.43

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). We note that the photometry may be  
affected by a nearby bright foreground star.


----------------------------------------------------------------
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GRB_name: GRB140311C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15983
SUBJECT: GRB 140311C: MASTER optical observations 
DATE:    14/03/14 15:01:38 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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)


As previously reported (Yurkov et. al. GCN 15981) MASTER VWF robotic very 
wide field cameras (FOV=2x384 square degrees, D=72mm, f/1.2, 1 pix = 22 
arcsec) installed on  MASTER-II robotic telescope in Tunka covered full 
FERMI GBM error-box (M. Stanbro, GCN15977)  before, during and after GRB. 
We haven't found credible optical transient with 3-sigma  upper limit 
10.5m.
We also didn't find credible optical counterpart on the survey (Yurkov et. 
al. GCN 15981) of part of error box carried out directly after GRB on 
MASTER-II robotic telescope up to 18 mag.

The synchronous move of FERMI GBM error-box available here
http://master.sai.msu.ru/static/GRB/GRB140311C_FERMI.gif
http://master.sai.msu.ru/static/GRB/GRB140311C_diff.gif
The circle on move  is the Fermi GBM 1 sigma+3 degrees systematic error 
box.

Also   very wide field cameras covered a place of possible iPTF 
counterpart (Singer et. al. GCN 15971).
Unfortunately the bright star is projected into OT place. We didn't find a 
noticeable brightening of this star.
The syncronous move from  very wide field cameras of possible iPTF 
counterpart place available here
  http://master.sai.msu.ru/static/GRB/GRB140311C_IPTF.gif
This place was not  covered on MASTER-II survey.

The Prompt Optical to Gamma Fluence  Ratio during this burst is:
F_opt/F_gamma <~  1 : 820.

The covarege map is available at 
http://master.sai.msu.ru/static/GRB/GRB140311C_map1.png .

The message may be cited.


GRB_name: GRB140308A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15984
SUBJECT: GRB140308A: Suzaku WAM observation of the prompt emission
DATE:    14/03/15 08:46:38 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

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

The long GRB 140308A (Konus-Wind detection: S. Golenetskii et al.,
GCN 15943, IPN localization: S. Golenetskii et al., GCN 15941)
was triggered the Suzaku Wide-band All-sky Monitor (WAM)
which covers an energy range of 50 keV - 5 MeV at 03:49:26.030 UT (=T0).

The observed light curve shows a multi-peaked structure starting at 
T0-10 s, ending at T0+80 s with a duration (T90) of about 64 seconds.
The fluence in 100 - 1000 keV was 4.02 (-0.78, +0.14) x10^-5 erg/cm^2.
The 1-s peak flux measured from T0+20 s was
7.71 (-5.71, +0.07) photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-10 s
to T0+80 s is well fitted by a GRB Band model in 90 keV to 5 MeV.
the low-energy photon index alpha: -0.95 (-0.44, +1.11),
the high-energy photon index beta: -2.20 (-0.23, +0.14),
and the peak energy Epeak: 386 (-128, +132) keV
(chi^2/d.o.f = 24.9/25).

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

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


GRB_name: GRB140311A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15985
SUBJECT: GRB 140311A: VLA Detection
DATE:    14/03/16 03:24:52 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 140311A (Racusin et al; GCN 15944) with
the VLA beginning on 2014 March 14.35 UT (2.48 days after the burst). At a mean
frequency of 21.8 GHz, we detect a radio source with a preliminary flux density
of ~ 0.25 mJy at

RA = 13:57:13.2763 +/- 0.0002
Dec = 00:38:31.423 +/- 0.003

consistent with the enhanced Swft/XRT position (Evans et al.; GCN 15959)
and the optical position (Xu et al.; GCN 15947). Follow-up observations are
planned."


GRB_name: GRB140318A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15986
SUBJECT: GRB 140318A: Swift detection of a burst
DATE:    14/03/18 00:35:21 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@swift.psu.edu>

S. B. Cenko (GSFC), M. G. Bernardini (INAF-OAB), D. N. Burrows (PSU),
P. D'Avanzo (INAF-OAB), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU),
F. E. Marshall (NASA/GSFC), A. Melandri (INAF-OAB), T. Sakamoto (AGU),
B. Sbarufatti (INAF-OAB/PSU) and M. H. Siegel (PSU) report on behalf
of the Swift Team:

At 00:09:07 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140318A (trigger=592204).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 184.053, +20.207 which is 
   RA(J2000) = 12h 16m 13s
   Dec(J2000) = +20d 12' 27"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single peak 
structure with a duration of about 30 sec.  The peak count rate
was ~1320 counts/sec (15-350 keV), at ~5 sec after the trigger. 

The XRT began observing the field at 00:11:12.7 UT, 124.8 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 184.0906, 20.2080 which is equivalent to:
   RA(J2000)  = +12h 16m 21.74s
   Dec(J2000) = +20d 12' 28.8"
with an uncertainty of 6.9 arcseconds (radius, 90% containment). This
location is 127 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 3.63e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 132 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. Results from the 2.7'x2.7' sub-image
are not available at this time. The 8'x8' region for the list of sources
generated on-board covers 100% of the 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 S. B. Cenko (brad.cenko AT nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB140318A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15987
SUBJECT: GRB 140318A: NOT detection of the afterglow
DATE:    14/03/18 02:04:47 GMT
FROM:    Steve Schulze at U of Iceland  <sts30@hi.is>

S. Schulze (PUC and MCSS), T. Kruehler (ESO Chile), N. R. Tanvir (U Leicester),  A. A. Djupvik (NOT), and P. Jakobsson (U Iceland) report on behalf of a larger collaboration:

We observed the field of GRB 140318A (Cenko et al., GCN 15986) with 2.5m the Nordic Optical Telescope (NOT) equipped with StanCAM. We obtained 3 x 300 s in the R band. Observations started at 00:52:00 UT on March 18 (i.e. 43 min after the burst).

We detect a bright point source at the position

R.A.(J2000)  = 12:16:21.40
Dec. (J2000) = +20:12:31.9

We measure R = 19.7 +/- 0.1 mag at 45 min after the trigger. The object coincides with a faint galaxy in the SDSS catalog which we identify as the putative host galaxy.  SDSS J121621.38+201232.1 has a r'-band magnitude of 22.87 +/-0.26 mag(AB) and a photometric redshift of 0.42 +/- 0.02.


GRB_name: GRB140318A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15988
SUBJECT: GRB 140318A: WHT spectroscopy
DATE:    14/03/18 04:25:02 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir (U. Leicester), T. Kruehler (ESO Chile),
S. Schulze (PUC and MCSS), R. Karjalainen (ING) report:

We observed the afterglow of GRB 140318A (Cenko et al. GCN 15986;
Schulze et al. GCN 15987) with the WHT using the ACAM spectrograph,
beginning March 18 02:06 UT, approximately 2 hours post-trigger.
The wavelength range covered was from about 5000 AA to 9500 AA.

In our provisional reduction, the continuum trace of the
aftergow+host is well detected, and a single emission line is seen
at ~7520 AA.  It is most likely that this is OII 3727, given the
absence of any other lines.  We therefore infer a redshift of
z=1.02, and tentatively identify this as the redshift of the burst.

Further analysis is ongoing.


GRB_name: GRB140318A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15989
SUBJECT: GRB140318A: Discovery Channel Telescope Optical Detection
DATE:    14/03/18 06:55:48 GMT
FROM:    John Capone at UMD  <jicapone@astro.umd.edu>

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

We observed the field of GRB140318A (Cenko et al., GCN 15986) with the
Large Monolithic Imager (LMI) on the recently commissioned 4.3m Discovery
Channel Telescope (DCT) at Happy Jack, AZ. We started a sequence of r', i'
and z' images beginning at 2014-03-18 03:32 UTC (approximately 3.5 hours
after the Swift trigger).

A source is clearly detected in all filters at the location of the optical
afterglow (Schulze et al, GCN 15987). Using nearby point sources from SDSS
for calibration, we measure preliminary magnitudes of r' = 21.6 +/- 0.2, i'
= 21.14 +/- 0.06 and z' = 20.86 +/- 0.04 at an average time of ~5 hours
after the GRB. These values are not corrected for Galactic extinction in
the direction of the GRB.

The source shows evidence of fading when compared with the NOT observation,
confirming that this is the optical afterglow.

Additional multi-band observations are ongoing.

We thank the staff of the Discovery Channel Telescope for assistance with
these observations.


GRB_name: GRB140318A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15990
SUBJECT: GRB 140318A: RATIR Optical and NIR Detections
DATE:    14/03/18 08:32:11 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 140318A (Cenko, et al., GCN 15986) 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 2014/03 18.15 to 2014/03 18.31
UTC (3.36 to 7.40 hours after the BAT trigger) obtaining a total of 0.99
hours exposure in the r and i bands and 0.60 hours exposure in the Z, Y,
J, and H bands.

We detect the previously reported optical counterpart (Schulze, et al. GCN
15987). In comparison with the SDSS DR9 and 2MASS, we obtain the following
detections:

  r     21.88 +/- 0.33
  i     21.37 +/- 0.18
  Z     20.67 +/- 0.20
  Y     20.76 +/- 0.29
  J     20.60 +/- 0.21
  H     20.29 +/- 0.19

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB. In comparison to the observations
of Schulze, et al. (GCN 15987) the measured r-band magnitude is consistent
with a power-law decay with a temporal index alpha = -1.0.

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


GRB_name: GRB140318A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15991
SUBJECT: GRB 140318A: Enhanced Swift-XRT position
DATE:    14/03/18 08:51:12 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 2346 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 140318A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 184.08924, +20.20902 which is equivalent
to:

RA (J2000): 12h 16m 21.42s
Dec (J2000): +20d 12' 32.5"

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: GRB140318A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15992
SUBJECT: GRB 140318A: Liverpool Telescope optical observations
DATE:    14/03/18 09:01:24 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

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

The 2-m Liverpool Telescope robotically followed up Swift GRB 140318A (Cenko et al., GCN 15986) at 00:27:37 UT (~18.5 min after the burst trigger).

We clearly detect the optical afterglow at the position reported by Schulze et al. (GCN 15987). In a coadded 6x10s SDSS-r image, we estimate the magnitude r' = 19.84 +- 0.11 at t_mid = 50.6 min since the Swift/BAT trigger time. The magnitude is calibrated against nearby SDSS stars.


GRB_name: GRB140318A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15993
SUBJECT: GRB 140318A: Swift-XRT refined Analysis
DATE:    14/03/18 19:35:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.7 ks of XRT data for GRB 140318A (Cenko  et al. GCN
Circ. 15986),  from 114 s to 46.2 ks after the BAT trigger. The data
comprise 219 s in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Goad et al.
(GCN Circ. 15991).

The light curve can be modelled with an initial power-law decay with an
index of alpha=0.48 (+/-0.20), followed by a break at T+263 s to an
alpha of 1.88 (+0.07, -0.06).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.21 (+0.12, -0.11). The
best-fitting absorption column is  1.14 (+0.27, -0.25) x 10^21 cm^-2,
in excess of the Galactic value of 2.6 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 2.9 x 10^-11 (3.9 x 10^-11) erg
cm^-2 count^-1. 

A summary of the WT-mode spectrum is thus:
Total column:      1.14 (+0.27, -0.25) x 10^21 cm^-2
Galactic foreground: 2.6 x 10^20 cm^-2
Excess significance: 5.8 sigma
Photon index:      2.21 (+0.12, -0.11)

If the light curve continues to decay with a power-law decay index of
1.88, the count rate at T+24 hours will be 2.1 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.2 x
10^-15 (8.3 x 10^-15) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00592204.

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


GRB_name: GRB140311A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15994
SUBJECT: GRB 140311A: Mondy optical limits
DATE:    14/03/18 20:40:18 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of GRB 140311A (Racusin et al., GCN 15944)  with 
AZT-33IK telescope of Mondy observatory  on Mar. 12 and Mar. 13. Within 
enhanced Swift-XRT error circle (Evans et al., GCN 15959) we do not 
detect the optical afterglow (Xu et al., GCN 15947;  Klotz et al., GCN 
15952).  Details of the photometry is following:

date       UT start   t-T0      Exp.    Filter  UpperLimit (3sigma)
                     (mid, days) (s)
2014-03-12 17:35:08  0.87145    25x120  R       21.4
2014-03-13 20:29:49  2.01082    51x120  R       21.6

The photometry is based on reference star SDSS-DR9, (R mag,
transformation by Lupton 2005):

N  SDSS_id          R(Lupton)   err
J135713.39+003942.0 18.447      0.015


GRB_name: GRB140311B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15995
SUBJECT: GRB 140311B: Mondy optical limit
DATE:    14/03/18 20:45:27 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of GRB 140311B (Racusin et al., GCN 15945)  with 
AZT-33IK telescope of Mondy observatory starting on Mar. 12 (UT) 
20:21:16. Within enhanced Swift-XRT eror circle (Evans et al., GCN 
15958) we do not detect the optical afterglow (Xu  et al., GCN 15949). 
Details of the photometry is following:

date       UT start   t-T0      Exp.    Filter  UpperLimit (3sigma)
                     (mid, days) (s)
2014-03-12 20:21:16  0.98389    30x120  R       20.2

The photometry is based on reference star SDSS-DR9, (R mag,
transformation by Lupton 2005):

N  SDSS_id          R(Lupton)   err
J164910.91+524333.6 17.449    0.009


GRB_name: GRB140318A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15996
SUBJECT: GRB 140318A: Swift-BAT refined analysis
DATE:    14/03/18 23:58:07 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
S. B. Cenko (GSFC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC),
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 the recent telemetry downlink,
we report further analysis of BAT GRB 140318A (trigger #592204)
(Cenko, et al., GCN Circ. 15986).  The BAT ground-calculated position is
RA, Dec = 184.049, 20.225 deg which is
  RA(J2000)  =  12h 16m 11.8s
  Dec(J2000) = +20d 13' 30.8"
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 49%.

The mask-weighted light curve shows a main single pulse starts at ~T+2 s and
ends at ~T+12 s, with some weak extented emissions starting before the main pulse
at ~T-20 s and extended after the pulse to ~T+50 s. T90 (15-350 keV) is 8.43 +- 1.27 sec
(estimated error including systematics).

The time-averaged spectrum from T+2.24 to T+11.68 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.35 +- 0.28.  The fluence in the 15-150 keV band is 2.9 +- 0.5 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+5.48 sec in the 15-150 keV band
is 0.5 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/592204/BA/


GRB_name: GRB140318A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15997
SUBJECT: GRB 140318A: Swift/UVOT Upper Limits
DATE:    14/03/19 14:07:38 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

B. Porterfield (PSU) and Cenko (GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140318A
132 s after the BAT trigger (Cenko et al., GCN Circ. 15986).
No optical afterglow consistent with the XRT position
(Cenko et al. GCN Circ. 15986) or NOT position (Schulze et al., GCN 
Circ 15987) is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

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

white_FC           132          282          147         >21.2
white              132         5340          541         >21.9
v                 4115         5750          393         >19.6
b                 3499         5135          393         >20.9
u                 4730         4930          197         >20.1
w1                4525         6063          298         >20.5
m2                4320         5955          393         >21.2
w2                3910         5546          393         >20.7

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: GRB140318A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15998
SUBJECT: GRB 140318A: Mondy optical limit
DATE:    14/03/19 15:00:05 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of GRB 140318A (Cenko et al., GCN 15986)  with 
AZT-33IK telescope of Mondy observatory starting on Mar. 18 (UT) 
13:18:36. Within enhanced Swift-XRT eror circle (Goad et al., GCN 15991) 
we do not detect the optical afterglow (Schulze et al., GCN 15987). 
Details of preliminary photometry is following:

date       UT start   t-T0      Exp.    Filter  UpperLimit (3sigma)
                     (mid, days) (s)
2014-03-18 13:18:36  0.59896    58x120  R       21.1

The photometry is based on reference star SDSS-DR9, (R mag,
transformation by Lupton 2005):

N  SDSS_id          R(Lupton)   err
J121613.64+200907.3 16.984    0.008


GRB_name: GRB140318A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  15999
SUBJECT: GRB 140318A: Continued RATIR Optical and NIR Observations
DATE:    14/03/19 21:38:45 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 140318A (Cenko, et al., GCN 15986) 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 2014/03 19.13 to 2014/03 19.50
UTC (26.91 to 35.94 hours after the BAT trigger), obtaining a total of
4.88 hours exposure in the r and i bands and 2.46 hours exposure in the
Z and Y bands.

We continue to detect the previously reported optical counterpart
(Littlejohns, et al., GCN 15990; Schulze, et al., GCN 15987). In
comparison with the SDSS DR9 and 2MASS, we obtain the following detections:

  r     22.52 +/- 0.11
  i     22.05 +/- 0.09
  Z     21.58 +/- 0.12
  Y     21.51 +/- 0.16

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB. Fading of the source is detected
for all of the four bands measured in both epochs of RATIR observations.
We note that the temporal decay index between these two epochs appears to
be shallower than that reported in Littlejohns, et al. (GCN 15990), with
-0.5 < alpha < -0.3 for all four bands. This can be interpretted as the
magnitude approaching that of the underlying SDSS galaxy reported in
Schulze, et al. (GCN 15987).

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


GRB_name: GRB140320A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16000
SUBJECT: GRB 140320A: Swift detection of a burst
DATE:    14/03/20 02:42:04 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

J. K. Cannizzo (NASA/UMBC), J. A. Kennea (PSU),
A. Y. Lien (NASA/GSFC/ORAU), C. J. Mountford (U Leicester),
D. M. Palmer (LANL) and B. Sbarufatti (INAF-OAB/PSU) report on behalf
of the Swift Team:

At 02:12:45 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140320A (trigger=592544).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 281.857, -11.173 which is 
   RA(J2000) = 18h 47m 26s
   Dec(J2000) = -11d 10' 21"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked
structure with two peaks separated by ~140 sec and a total duration 
of about 150 sec.  The peak count rate
was ~3700 counts/sec (15-350 keV), at ~0 sec after the trigger. 

No source was detected in 57 s of promptly downlinked data. We are
waiting for the full dataset to detect and localise the XRT
counterpart. 

Due to partial real-time telemetry, no further information is
available at this time.  However the burst was also detected
by the Fermi-GBM instrument, verifying its reality. 
More details will be available following the next ground pass 
telemetry dump. 

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


GRB_name: GRB140320A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16001
SUBJECT: GRB 140320A: Fermi GBM observations suggest a short GRB
DATE:    14/03/20 04:55:01 GMT
FROM:    George A. Younes at USRA/NASA/MSFC  <younes.ge@gmail.com>

G. Younes (USRA/MSFC) and V. Connaughton (UAH) report on behalf of the Fermi GBM Team:

"At 02:12:46.11 UT on 19 March 2014, the Fermi Gamma-Ray Burst Monitor
Triggered and located GRB 140320A (trigger 416974369/140320092), which
was  also detected by Swift (Cannizzo et al. 2014, GCN 16000).

The double peaked structure seen with BAT, with ~150 s separation, and
reported by Cannizzo et al. is also visible with FERMI/GBM, however, a
location analysis with GBM shows that the two peaks are unrelated. The
first peak (trigger peak) is most likely due to a short/hard GRB located at
RA~284.6 DEC~-5.0 deg, consistent with the BAT location. The second peak,
150 s after the trigger, is much softer and locates at RA~265.0 DEC~-28.0,
the location of the bursting pulsar GRO J1744-28, which is currently active.

Hence, we encourage multi-wavelength follow-up observations of this candidate short/hard GRB.


GRB_name: GRB140320B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16003
SUBJECT: GRB 140320B: FTN optical afterglow candidate
DATE:    14/03/20 10:18:18 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), A. Melandri (INAF-OAB), D. Kopac,
A. Gomboc (U. Ljubljana), C.G. Mundell, F. Virgili (LJMU)
on behalf of a larger collaboration report:

The 2-m Faulkes Telescope North automatically began observing INTEGRAL
GRB 140320B on March 20 at 09:31:27 UT (~4.6 min after the burst trigger).

We find a fading uncatalogued object at coordinates

RA(2000.0)=   09:42:14.17
Dec(2000.0)=  +60:16:05.7  (error 1.0")

with i=19.7 +- 0.1 mag at 16 minutes after the GRB,
calibrated against nearby SDSS-I stars.


GRB_name: GRB140320B
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16004
SUBJECT: GRB 140320B: A long GRB detected by INTEGRAL
DATE:    14/03/20 10:20:11 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@iasf-milano.inaf.it>

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

a gamma ray burst lasting about 100 s has been detected by IBAS in the 
IBIS/ISGRI data at 09:26:00 UT of March 20.

The refined coordinates (J2000) are:

R.A.=  145.5409 deg
DEC.=  +60.2794 deg

with an uncertainty of   2  arcmin (90% c.l.).

A preliminary analysis gives a peak flux of 0.2 counts/cm2/s (20-200 keV, 
1-s integration time) and a fluence in the same energy range of about 5e-7 
erg/cmq.

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


GRB_name: GRB140320B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16005
SUBJECT: GRB 140320B: ISON-NM optical observations
DATE:    14/03/20 11:15:24 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 INTEGRAL GRB 140320B (Mereghetti et 
al.,  GCN 16004)  with 0.4-m telescope of ISON-NM observatory starting 
on Mar., 20 (UT)  09:35:41.  We took unfiltered images of 30 s 
exposures. We detect a fading optical afterglow of GRB  140320B 
(Guidorzi  et al.,   GCN 16003) in a stacked image of total exposure 300 
s and do not detect it in the next stacked image of the same exposure. 
  Coordinates of the optical afterglow (J2000) 09 42 13.96 +60 16 05.9 
(uncertainties of 1 arcsec) coincide with OT coordinates (Guidorzi et 
al.,  GCN 16003). Preliminary photometry  of first stacked images is 
based on nearby USNO-B1.0 stars:

UT mid,      T0+      Filter  Exposure,  OT,    err OT
                  mid          s
09:38:39      0.00878 none    10Ñ…30     19.1    0.2
09:44:40      0.03102 none    10Ñ…30   > 19.3    UpperlLimit


GRB_name: GRB140320B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16006
SUBJECT: GRB 140320B:  Xinglong TNT upper limit
DATE:    14/03/20 14:05:01 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

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

We began to observe GRB 140320B  (Mereghetti et al.,  GCN 16004)  
with Xinglong 0.8-m TNT telescope at 12:15:47(UT) , 2.83 hrs after the burst.

We do not detect the reported afterglow counterpart
 (Guidorzi et al.,  GCN 16003,Elenin et al., GCN 16005). 
in our combined images down to the upper limit 
of 21.8 mag in R band, calibrated by nearby USNO B1.0 R2 mag,
 at the mean time of 3.22 hrs after the burst.


GRB_name: GRB140320C
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16007
SUBJECT: GRB 140320C: A long GRB detected by INTEGRAL
DATE:    14/03/20 14:48:47 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@iasf-milano.inaf.it>

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

a gamma ray burst lasting about 30 s has been detected by IBAS in the 
IBIS/ISGRI data at 13:17:20 UT of March 20, 2014.

The refined coordinates (J2000) are:

R.A.=  134.4175 deg
DEC.=  +71.2002  deg

with an uncertainty of 3 arcmin (90% c.l.).

A preliminary analysis gives a peak flux of about 0.15 counts/cm2/s 
(20-200 keV, 1-s integration time) and a fluence in the same energy range 
of about 2e-7 erg/cmq.

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


GRB_name: GRB140320C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16008
SUBJECT: GRB 140320C: FTN optical observations
DATE:    14/03/20 15:10:15 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

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

The 2-m Faulkes Telescope North automatically began observing INTEGRAL GRB 140320C (Mereghetti et al. GCN 16007) on March 20 at 13:21:39.3 UT (~4.3 min after the burst trigger).

We do not find any fading candidate in our first 10s image within the entire INTEGRAL error circle down to a limiting magnitude or R>19.5 (5 sigma upper limit).


GRB_name: GRB140320C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16009
SUBJECT: GRB 140320C: MASTER optical observations
DATE:    14/03/20 15:12:11 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.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  GRB140320C (Mereghetti et. 
al GCN 16007) 25 sec after notice time and 33 sec after trigger time at 2014-03-20 13:18:13 UT in two 
polarizations. We haven't found optical 
transient  within INTEGRAL error-box  on single and coadd images.
The 5-sigma upper limit has been about 16.8 mag on first single 10 sec 
image.
On coadd of 11 first images with different exposures and total exosure 
time 610 sec the 5-sigma upper limit has been about 20.0 mag in bosh 
polarization.

The message may be cited.


GRB_name: GRB140320A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16010
SUBJECT: GRB 140320A: Swift-XRT detection of an afterglow candidate
DATE:    14/03/20 19:36:01 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page, C. Pagani (U. Leicester) and J.K. Cannizzo (NASA/UMBC) report
on behalf of the Swift-XRT team:

We have analysed 5 ks of XRT data for GRB 140320A (Cannizzo et al. GCN
Circ. 16000), from 93 s to 11.8 ks after the BAT trigger. The data are
entirely in Photon Counting (PC) mode. We detect a faint, uncatalogued
X-ray source with a mean count rate of (5.9 +/- 1.3) x 10^-3 count s^-1,
at a position of RA, Dec = 281.85583, -11.19333, which is equivalent to

RA(J2000) =   18 47 25.4
Dec(J2000) = -11 11 36.9

with an uncertainty of 5.3 arcsec (radius, 90% confidence). This is 73
arcsec from the initial BAT position, within the BAT error circle. We
cannot determine at this time whether the source is fading.

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


GRB_name: GRB140320A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16011
SUBJECT: GRB 140320A: Enhanced Swift-XRT position 
DATE:    14/03/20 20:29:53 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page, C. Pagani, P.A. Evans and M.R. Goad (U. Leicester) report on
behalf of the Swift-XRT team:

Using 715 s of XRT Photon Counting mode data and 1 UVOT images, we find an
astrometrically corrected X-ray position (using the XRT-UVOT alignment and
matching UVOT field sources to the USNO-B1 catalogue): RA, Dec =
281.85530, -11.19412 which is equivalent to:

RA (J2000):  18 47 25.27
Dec (J2000): -11 11 38.8

with an uncertainty of 4.9 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 is an official product of the Swift-XRT team.


GRB_name: GRB140320C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16012
SUBJECT: GRB 140320C: Mondy optical observations
DATE:    14/03/20 20:31:29 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of GRB 140320C (Mereghetti  et al., GCN 16007) 
with AZT-33IK telescope of Mondy observatory starting on Mar. 20 (UT) 
15:12:44. We obtained several images of 120 s exposure in R-filter. 
Within entire INTEGRAL error circle we identified sources which are not 
presented in the DSS2(R) image:

N  RA(J2000)    Dec. (J2000)

1. 08 57 55.04 +71 13 36.5
2. 08 57 16.68 +71 10 10.6
3. 08 57 34.11 +71 11 55.0

(Uncertainty of all coordinates are 1 arcsec.)

However,  our  images are more deep than DSS2(R), down to a limiting 
magnitude R~21, and at present time we cannot determine whether the 
sources are fading.


GRB_name: GRB140320B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16013
SUBJECT: GRB 140320B: Swift-XRT detection of the afterglow
DATE:    14/03/20 21:57:31 GMT
FROM:    Claudio Pagani at U of Leicester  <cp232@star.le.ac.uk>

C. Pagani, K.L. Page, R.L.C. Starling, (U. Leicester) report on behalf 
of the Swift-XRT team:

We have analysed 4 ks of XRT data for the INTEGRAL detected GRB 140320B 
(Mereghetti et al. GCN Circ. 16004), from 11.6 s to 23.1 ks after the 
trigger. The data are entirely in Photon Counting (PC) mode. An 
uncatalogued, fading X-ray source is detected inside the INTEGRAL error 
circle.

Using 3683 s of XRT PC data and 4 UVOT images, we find an 
astrometrically corrected X-ray position (using the XRT-UVOT alignment 
and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 
145.55932, 60.26822 which is equivalent to:

RA (J2000):  09 42 14.24
Dec (J2000): +60 16 05.6

with an uncertainty of 1.7 arcsec (radius, 90% confidence). This is 
consistent with the optical position reported by Guidorzi et al. (GCN 
16003) and Elenin et al. (GCN 16005).

The light curve can be modelled with a power-law decay with an index of 
alpha=1.12 (+1.21, -0.05).

A spectrum formed from the PC mode data can be fitted with an absorbed 
power-law with a photon spectral index of 2.3 (+0.4, -0.3). The 
best-fitting absorption column is  6 (+8, -6) x 10^20 cm^-2, consistent 
with the Galactic value of 2.4 x 10^20 cm^-2 (Kalberla et al. 2005). The 
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor 
deduced from this spectrum  is 2.8 x 10^-11 (3.0 x 10^-11) erg cm^-2 
count^-1.

If the light curve continues to decay with a power-law decay index of 
1.12, the count rate at T+24 hours will be 7.8 x 10^-3 count s^-1, 
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.2 x 
10^-14 (2.3 x 10^-14) erg cm^-2 s^-1.

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


GRB_name: GRB140320A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16014
SUBJECT: GRB 140320A: Fermi GBM detection
DATE:    14/03/20 22:12:14 GMT
FROM:    George A. Younes at USRA/NASA/MSFC  <younes.ge@gmail.com>

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

"At 02:12:46.11 UT on 20 March 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140320A (trigger 416974369/140320092),
which was also detected by Swift (Cannizzo et al. 2014, GCN 16000).
The GBM on-ground location, using the Fermi GBM trigger
data, is consistent with the Swift/BAT location.

The angle to the Fermi LAT boresight is 24 deg. using the Swift location.

The GBM light curve consists of a single pulse with a
duration (T90) of 1 s (50-300 keV).
The time-averaged spectrum from T0-0.32 to T0+0.704 s is
well fit by a simple power law function with index of -1.5 +/- 0.1.

The event fluence (10-1000 keV) in this time interval is
(4.0 +/- 0.5) E-07 erg/cm^2. The 0.064-sec peak photon flux measured
starting from T0-0.128 s in the 10-1000 keV band
is 5.0 +/- 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: GRB140320C
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16015
SUBJECT: GRB 140320C: Swift-XRT detection of the X-ray afterglow
DATE:    14/03/21 07:10:35 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

C. Pagani and K.L. Page (U. Leicester) report on behalf of the Swift-XRT team:

We have analysed 4 ks of XRT data for the INTEGRAL detected GRB 140320C
(Mereghetti et al. GCN Circ. 16007), from 19.5 s to 37.2 ks after the
trigger. The data are entirely in Photon Counting (PC) mode. We detect an
uncatalogued X-ray source. Using 1552 s of XRT Photon Counting mode data
astrometrically corrected X-ray position (using the XRT-UVOT alignment and
matching UVOT field sources to the USNO-B1 catalogue): RA, Dec =
134.39401, 71.19829, which is equivalent to:

RA(J2000) =  08 57 34.56
Dec(J2000) =  71 11 53.9

with an uncertainty of 2.6 arcsec (radius, 90% confidence). This is 28
arcsec from the initial INTEGRAL position, within the INTEGRAL error
circle. This is consistent with the optical source N3 from Volnova et al.
(GCN 16012).

The source has faded from a count rate of 0.013 (+/- 0.003) at 20.5 ks
after the INTEGRAL trigger to 0.003 (+0.002,-0.001) by 33.9 ks, so we
confirm it as the X-ray afterglow.

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


GRB_name: GRB140320A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16016
SUBJECT: GRB 140320A: Confirmation of a fading X-ray afterglow
DATE:    14/03/21 10:08:11 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page, C. Pagani, P.A. Evans (U. Leicester) & J.K. Cannizzo
(NASA/UMBC) report on behalf of the Swift-XRT team:

We have now analysed 9.8 ks of Swift-XRT data for GRB 140320A, between 93
s and 33.5 ks after the trigger. The X-ray source given by Page, Pagani &
Cannizzo in GCN Circ. 16010 has now faded, with a 3-sigma upper limit on
the count rate centred at 27 ks after the trigger of 1.2 x 10^-3 count
s^-1. We therefore confirm this source as the X-ray afterglow of GRB
140320A.

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


GRB_name: GRB140320C
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16017
SUBJECT: GRB 140320C: Swift-XRT observations
DATE:    14/03/21 10:34:38 GMT
FROM:    Claudio Pagani at U of Leicester  <cp232@star.le.ac.uk>

C. Pagani, K.L. Page and P.A. Evans report on behalf of the Swift-XRT
team:

We have analysed 4.0 ks of XRT data for the INTEGRAL-detected burst:
GRB 140320C,  from 19.5 ks to 37.3 ks after the  INTEGRAL trigger. The
data are entirely in Photon Counting (PC) mode.  An X-ray source is
detected within the INTEGRAL error circle. Using 1552 s of PC mode data
and 1 UVOT images, we find an enhanced XRT position (using the XRT-UVOT
alignment and matching UVOT field sources to the USNO-B1 catalogue):
RA, Dec = 134.39421, +71.19839 which is equivalent to:

RA (J2000): 08h 57m 34.61s
Dec(J2000): +71d 11' 54.2"

with an uncertainty of 2.6 arcsec (radius, 90% confidence). This
position is 27 arcsec from the INTEGRAL position. 

The light curve can be modelled with  a power-law decay with a decay
index of alpha=2.8 (+1.0, -1.7).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.3 (+0.9, -0.3) and an
absorption column consistent with the Galactic value of 3.6 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 5 x
10^-11 (5 x 10^-11) erg cm^-2 count^-1.

If the light curve continues to decay with a power-law decay index of
2.8, the count rate at T+24 hours will be 2.4 x 10^-4 count s^-1

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020371.

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


GRB_name: GRB140320A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16018
SUBJECT: GRB 140320A: Swift/UVOT Upper Limits
DATE:    14/03/21 11:18:38 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (UCL-MSSL) and J. K. Cannizzo (NASA/UMBC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140320A
3723 s after the BAT trigger (Cannizzo et al., GCN Circ. 16000).
No optical afterglow consistent with the enhanced XRT position
(Page et al., GCN Circ 16011) is detected in the initial UVOT exposures.

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

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

v                 3723         5358          393         >19.2
b                 4543        10186         1149         >20.8
u                 4338         5973          393         >19.7
w1                4133         5768          393         >19.8
m2                3928         5563          393         >20.0
w2                3518         5153          393         >20.2

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.51 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB140320B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16019
SUBJECT: GRB 140320B: Swift/UVOT Upper Limits
DATE:    14/03/21 13:02:09 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (UCL-MSSL) and R. L. C. Starling, (U. Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140320B
11975 s after the INTEGRAL trigger (Mereghetti et al., GCN Circ. 16004).
No optical afterglow consistent with the XRT position
(Pagani et al., GCN Circ. 16013) and the FTN optical position 
(Guidorzi et al., GCN Circ. 16003) 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            11975        29408         5864         >23.1

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: GRB140320A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16020
SUBJECT: GRB 140320A: Swift-BAT refined analysis
DATE:    14/03/21 13:04:45 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. K. Cannizzo (NASA/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 140320A (trigger #592544)
(Cannizzo, et al., GCN Circ. 16000).  The BAT ground-calculated position is
RA, Dec = 281.843, -11.188 deg which is
   RA(J2000)  =  18h 47m 22.4s
   Dec(J2000) = -11d 11' 18.5"
with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 88%.

The mask-weighted light curve shows a double short-peaked structure starts
at ~T-0.1 s. The second peak starts immediately at the end of the first peak
at ~T+0.3 s, and ends at ~T+0.4 s. T90 (15-350 keV) is 0.45 +- 0.07 sec
(estimated error including systematics).

The time-averaged spectrum from T-0.08 to T+0.44 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.24 +- 0.36.  The fluence in the 15-150 keV band is 4.9 +- 1.0 x 10^-8 erg/cm2.
The 1-sec peak photon flux measured from T-0.32 sec in the 15-150 keV band
is 0.6 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

As noted in the Fermi/GBM circular (Younes et al.; GCN Circ. 16001), the pulse
at ~T+140 s initially reported in Cannizzo, et al. (GCN Circ. 16000) is
originated from a different source, the bursting pulsar GROJ1744-28.
Therefore, GRB 140320A is a short burst.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/592544/BA/


GRB_name: GRB140320C
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16021
SUBJECT: GRB 140320C: Swift/UVOT Upper Limits
DATE:    14/03/21 13:05:13 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (UCL-MSSL) and J. K. Cannizzo (NASA/UMBC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140320C
19435 s after the INTEGRAL trigger (Mereghetti et al., GCN Circ. 16007).
No optical afterglow consistent with the XRT position 
(Pagani et al., GCN Circ. 16015; 16017) 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            20211        32984         1056         >22.1
v                20986        33302         1087         >20.5
u                19435        37277         1741         >21.4

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.07 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB140320C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16022
SUBJECT: GRB 140320C: Mini-GWAC prompt observation
DATE:    14/03/21 14:03:44 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

J. Y. Wei,  L. P. Xin,  Y. L. Qiu,  J. S. Deng,   J. Wang, 
X. H. Han,  C. Wu,  H. L. Huang,  X. M. Meng, 
Y. F. Xuan and Y. Xu on behalf of EAFON report:

Mini-GWAC system is located at Xinglong observatory, 
National Astronomical Observatories, China,
including 6 mounts and 12 Canon 85/f1.2 cameras.
Each mount is equipped with 2 cameras.
For each camera, the Apogee U9000X CCD was used, which gives 
about 400 square degree of FOV. The total field of view of this system
is about 5000 sq.deg.

The field of INTERGRAL GRB 140320C (Mereghetti et al. GCN 16007) 
was monitored by Mini-GWAC system continuously 
during about 2 hrs before and 4 hrs after the burst.
The exposure time for each frame is 10 sec. 

No any new optical counterpart in single frame  
was detected down to the 5 sigma upper limit of 13.1 mag 
calibrated by nearby USNO B1.0 R2 mag, 
at the epoch of prompt emission phase.
Combining 5 frames after the burst trigger initially 
with total exposure time of 50 sec 
gives a 5 sigma upper limit of 13.7 mag.

This message may be cited.


GRB_name: GRB140320D
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16023
SUBJECT: IPN Triangulation of very intense GRB 140320D
DATE:    14/03/21 16:28:50 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

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

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

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 140320D has been observed by 
Konus-Wind, INTEGRAL (SPI-ACS), Swift (BAT), and MESSENGER (GRNS), so 
far, at about 73297 s UT (20:21:37). 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:
      87.893 (05h 51m 34s) +85.429 (+85d 25' 46")
    Corners:
      98.997 (06h 35m 59s) +86.721 (+86d 43' 15")
      98.219 (06h 32m 53s) +87.023 (+87d 01' 23")
      81.849 (05h 27m 24s) +84.026 (+84d 01' 35")
      83.033 (05h 32m 08s) +83.741 (+83d 44' 28")
    ---------------------------------------------
The error box area is 0.635 sq. deg, and its maximum dimension is 3.474
deg (the minimum one is 0.196 deg).

This box may be improved.

A triangulation map is posted at 
http://www.ioffe.ru/LEA/GRBs/GRB140320_T73298/IPN/

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


GRB_name: GRB140320B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16024
SUBJECT: GRB 140320B: P60 detection of a very red afterglow
DATE:    14/03/21 16:39:00 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

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

The Palomar 60-inch telescope automatically responded to the INTEGRAL 
trigger for GRB 130420B (Mereghetti et al. GCN 16004) and began taking a 
series of 60-second exposures in the r, i, and z filters starting at 
2014-03-20 09:31:41.744 (7.12 minutes after the trigger).

The afterglow candidate reported by Guidorzi et al. (GCN 16003) is 
well-detected in the initial z-band exposure, weakly detected in the 
initial i-band exposure, and not detected in the initial r-band 
exposure.  However, a weak r-band detection is recovered by stacking 
several images.

The light curve (in the i- and z-band filters) shows a rise to a peak at 
around 15 minutes post-trigger, followed by a decline up until the end 
of our sequence at 1.3 hours after the GRB.

Stacking the first 7 exposures in each filter, we estimate magnitudes of:

r = 21.29 +/- 0.24
i = 20.07 +/- 0.09
z = 17.97 +/- 0.03

At a mid-UT time of approximately 09:46 in each filter (20 minutes after 
the trigger).

The redder apparent color in i-z compared to r-i may suggest a highly 
reddened afterglow with host contribution to the r-band, or a reddened 
afterglow with a very strong 2175 dust feature at z~2.5, or a Lyman 
break in the i-band with some Lyman-alpha forest blueward (z~5).  We 
encourage further observations, particularly in the NIR.


GRB_name: GRB140320D
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16025
SUBJECT: Konus-Wind observation of GRB 140320D
DATE:    14/03/21 17:15:12 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, and T. Cline on behalf of the 
Konus-Wind team, report:

A very intense, long-duration, hard-spectrum GRB 140320D (IPN 
triangulation: K. Hurley et al., GCN 16023) triggered Konus-Wind at 
T0=73298.804 s UT (20:21:38.804).

The burst light curve shows a bright, double-peaked pulse with a total
duration of ~50 s. The emission is seen up to ~10 MeV.

As observed by Konus-Wind, the burst had
a fluence of (2.1 +/- 0.1)x10^-4 erg/cm2, and
a 64-ms peak flux, measured from T0+15.456 s, of (6.7 +/- 0.7)x10^-5 
erg/cm2/s (both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+45.568 s) is best fit 
in the 20 keV - 10 MeV range by the GRB (Band) function with the 
following model parameters:
the low-energy photon index alpha = -0.83 (-0.03,+0.03),
the high energy photon index beta = -2.75 (-0.32,+0.20),
the peak energy Ep = 575 (-30,+32) keV,
chi2 = 100/87 dof.

The spectrum near the maximum count rate
(measured from T0+15.360 to T0+15.872 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.30 (-0.11,+0.13),
the high energy photon index beta = -2.59 (-0.62,+0.30),
the peak energy Ep = 655 (-89,+102) keV,
chi2 = 82/56 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140320_T73298/

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


GRB_name: GRB140320A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16026
SUBJECT: GRB 140320A: RATIR Optical and NIR Observations
DATE:    14/03/21 23:44:39 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 140320A (Cannizzo, et al., GCN 16000) 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 2014/03 21.42 to 2014/03 21.51
UTC (31.77 to 33.94 hours after the BAT trigger), obtaining a total of
1.40 hours exposure in the r and i bands and 0.56 hours exposure in the
Z, Y, J, and H bands.

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

  r     > 22.70
  i     > 22.38
  Z     > 21.23
  Y     > 21.27
  J     > 20.82
  H     > 20.24

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 Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB140323A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16027
SUBJECT: GRB 140323A: Swift detection of a burst
DATE:    14/03/23 10:40:32 GMT
FROM:    Eleonora Troja at GSFC  <eleonora.troja@nasa.gov>

E. Troja (NASA/GSFC/UMCP), V. D'Elia (ASDC),
H. A. Krimm (CRESST/GSFC/USRA), C. J. Mountford (U Leicester),
K. L. Page (U Leicester) and T. N. Ukwatta (MSU) report on behalf of
the Swift Team:

At 10:23:11 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140323A (trigger=592916).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 356.888, -79.917 which is 
   RA(J2000) = 23h 47m 33s
   Dec(J2000) = -79d 55' 00"
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 120 sec.  The peak count rate
was ~6700 counts/sec (15-350 keV), at ~89 sec after the trigger. 

The XRT began observing the field at 10:24:49.4 UT, 97.5 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source with an enhanced position: RA, Dec 356.9593,
-79.9050 which is equivalent to:
   RA(J2000)  = 23h 47m 50.23s
   Dec(J2000) = -79d 54' 17.9"
with an uncertainty of 2.2 arcseconds (radius, 90% containment). This
location is 62 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 7.93
x 10^20 cm^-2 (Willingale et al. 2013). 

The initial flux in the 0.1 s image was 1.95e-08 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 105 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
0.14. 

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: GRB140323A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16028
SUBJECT: GRB 140323A: Enhanced Swift-XRT position
DATE:    14/03/23 16:58:18 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 876 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 140323A, 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 = 356.95962, -79.90455 which is equivalent
to:

RA (J2000): 23h 47m 50.31s
Dec (J2000): -79d 54' 16.4"

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

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

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


GRB_name: GRB140323A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16029
SUBJECT: GRB 140323A: Swift-BAT refined analysis
DATE:    14/03/23 19:27:36 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), D. M. Palmer (LANL),
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+693 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140323A (trigger #592916)
(Troja, et al., GCN Circ. 16027).  The BAT ground-calculated position is
RA, Dec = 356.975, -79.916 deg which is
    RA(J2000)  =  23h 47m 54.1s
    Dec(J2000) = -79d 54' 57.3"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 12%.

The mask-weighted light curve shows a complex structure.  Low-level emission
starts around T-60 sec, then the first episode runs from T-20 to T+55 sec, and
is a slow rise and fall with multiple sub-peaks superimposed.  The second
episode has a similar shape and runs from T+60 to T+110 sec, followed by
more low-level emission out to T+140 sec.  The second episode is spectrally
softer than the first. T90 (15-350 keV) is 104.9 +- 2.6 sec (estimated error
including systematics).

The time-averaged spectrum from T-7.09 to T+117.37 sec is best fit by a
power law with an exponential cutoff.  This fit gives a photon index 1.35 +- 0.17,
and Epeak of 127.1 +- 59.2 keV (chi squared 50.15 for 56 d.o.f.). For this
model the total fluence in the 15-150 keV band is 1.6 +- 0.0 x 10^-05 erg/cm2
and the 1-sec peak flux measured from T+6.42 sec in the 15-150 keV band is
6.2 +- 0.7 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.64 +- 0.04 (chi squared 59.02 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/592916/BA/


GRB_name: GRB140323A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16030
SUBJECT: GRB 140323A: Swift/UVOT Upper Limits
DATE:    14/03/23 19:47:02 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <m.depasquale@ucl.ac.uk>

M. De Pasquale (UCL-MSSL) and E. Troja (NASA/GSFC/UMCP)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140323A
106 s after the BAT trigger (Troja et al., GCN Circ. 16027).
No optical afterglow consistent with the XRT position
(Osborne et al. GCN Circ. 16028) 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           106          256          147         >20.4
u_FC               319          569          246         >19.5
white              106          793          186         >20.5
v                  649         5918          216         >19.1
b                  574        12334          773         >20.2
u                  319         6532          462         >19.9
w1                 698         6328          216         >19.5
m2                5923        16174          725         >20.4
w2                 798          818           19         >17.9

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: GRB140323A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16031
SUBJECT: GRB 140323A: BOOTES-3 optical upper limit.
DATE:    14/03/23 20:00:23 GMT
FROM:    Juan Carlos Tello at IAA-CSIC  <jtello@iaa.es>

M. Jelinek, J. C. Tello, R. Cunniffe, S. Jeong, O. Lara-Gil, J. Gorosabel
(IAA-CSIC Granada), P. Kubnek (IP-ASCR Praha), M. Wildi (Obs. Vermes),
Ph. Yock (Univ. of Auckland), W. H. Allen (Vintage Lane Observatory) and
A. J. Castro-Tirado (IAA-CSIC), on behalf of a larger collaboration,
report:

"Following the detection of GRB 140323A by Swift (Troja et al., GCNC
16027), the 0.6m YA robotic telescope at the BOOTES-3 astronomical station
in Blenheim (New Zealand), responded ito the Swift BAT alert #592916. The
co-add of the second set of unfiltered images starting at 10:26:15 UT and
ending at 10:35:02 UT (i.e. 184-710 s postburst) reveals no optical
afterglow at the enhanced Swift XRT position (Osborne et al., GCNC 16028)
down to 18.5 mag. A first set only provides a shallower limit."


GRB_name: GRB140323A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16032
SUBJECT: GRB 140323A: Fermi GBM observation
DATE:    14/03/23 20:34:07 GMT
FROM:    Hoi-Fung Yu at MPE  <sptfung@mpe.mpg.de>

Subject: GRB 140323A: Fermi GBM observation

Hoi-Fung Yu and Andreas von Kienlin (MPE)
report on behalf of the Fermi GBM Team:

"At 10:22:53.12 UT on 23 March 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140323A (trigger 417262976 / 140323433),
which was also detected by Swift/BAT and XRT (Troja et al. 2014, GCN 16027).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 31 degrees.

The GBM light curve consists of multiple peaks in two main episodes
with a duration (T90) of about 111 s (50-300 keV).
The time-averaged spectrum from T0-2.560 s to T0+138.755 s is
well fit by a power law function with an exponential
high-energy cutoff. The power law index is -1.09 +/- 0.02 and
the cutoff energy, parameterized as Epeak, is 142 +/- 4 keV

The event fluence (10-1000 keV) in this time interval is
(3.15 +/- 0.05)E-05 erg/cm^2. The 1.024 s peak photon flux measured
starting from T0+25.0884 s in the 10-1000 keV band
is 9.7 +/- 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: GRB140323A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16033
SUBJECT: GRB 140323A: Swift-XRT refined Analysis
DATE:    14/03/24 01:40:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.3 ks of XRT data for GRB 140323A (Troja  et al. GCN
Circ. 16027),  from 90 s to 34.5 ks after the  BAT trigger. The data
comprise 650 s in Windowed Timing (WT) mode (the first 6 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Osborne et
al. (GCN Circ. 16028).

The late-time light curve (from T0+5.7 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.30 (+/-0.09).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.73 (+/-0.06). The
best-fitting absorption column is  5.0 (+/-0.4) x 10^21 cm^-2, in
excess of the Galactic value of 7.9 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.00 (+/-0.12) and a
best-fitting absorption column of 5.3 (+/-0.7) 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 (6.8 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.3 (+/-0.7) x 10^21 cm^-2
Galactic foreground: 7.9 x 10^20 cm^-2
Excess significance: 10.8 sigma
Photon index:      2.00 (+/-0.12)

If the light curve continues to decay with a power-law decay index of
1.30, the count rate at T+24 hours will be 0.033 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.4 x
10^-12 (2.3 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/00592916.

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


GRB_name: GRB140323A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16034
SUBJECT: GRB 140323A: Fermi-LAT detection
DATE:    14/03/24 09:54:39 GMT
FROM:    Elisabetta Bissaldi at U.Innsbruk/IAPP  <Elisabetta.Bissaldi@uibk.ac.at>

G. Vianello (Stanford), F. Longo and E. Bissaldi (University and
INFN Trieste) report on behalf of the Fermi-LAT team:

On March 23, 2014, Fermi-LAT detected high-energy emission from
GRB 140323A, initially detected by Swift (Troja et al., GCN 16027)
and also detected by Fermi-GBM (Yu et al., GCN 16032).
We note that the GBM and the Swift trigger times are different.
Here we will use as a reference the GBM trigger time,
i.e. 10:22:53.12 UT.

The data from the Fermi-LAT show a significant increase
in the event rate within 10 degrees of the Swift location.
More than 11 photons above 100 MeV and 3 photons above 1 GeV
are observed within 1000 seconds from the GBM trigger time.
The highest-energy photon is a 2.5 GeV event,
which is observed ~220 seconds after the trigger.

The best LAT on-ground location is found to be

RA, Dec 356.46, -79.87 (J2000)

with an error radius of 0.19 deg (90% containment, statistical
error only). This is 0.09 deg from the Swift/XRT localization
(GCN 16028) and is consistent with it.
The source was 31 deg from the LAT boresight
at the time of the trigger.

The Fermi-LAT point of contact for this burst is
Daniel Kocevski (daniel.kocevski@nasa.gov).

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


GRB_name: GRB140323A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16035
SUBJECT: Konus-Wind observation of GRB 140323A
DATE:    14/03/24 13:39:28 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

A long-duration GRB 140323A (Swift-BAT trigger 592916:
Troja et al., GCN 16027; Sakamoto et al., GCN 16029;
Fermi-GBM detection: Yu & von Kienlin, GCN 16032;
Fermi-LAT detection: Vianello et al., GCN 16034)
triggered Konus-Wind at T0=37392.356 s UT (10:23:12.356).

The burst light curve shows multiple peaks in two major bursting episodes.
A total duration of the burst is ~130 s.
The emission is seen up to ~10 MeV.

As observed by Konus-Wind, the burst had a fluence
of 3.1(-0.4,+0.7)x10^-5 erg/cm2, and a 64-ms peak flux,
measured from T0+5.376 s, of 3.2(-0.6,+0.7)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+106.752 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 = -1.09 (-0.15,+0.31),
the high energy photon index beta = -3.0 (-7.0,+0.6),
the peak energy Ep = 127 (-24,+16) keV,
chi2 = 93.4/97 dof.

The spectrum near the maximum count rate
(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 = -0.79 (-0.18,+0.20),
the high energy photon index beta = -2.7 (-6.0,+0.3),
the peak energy Ep = 184 (-24,+31) keV,
chi2 = 96.8/87 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140323_T37392/

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


GRB_name: GRB140320C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16036
SUBJECT: GRB 140320C: Mondy optical observations and afterglow confirmation
DATE:    14/03/25 12:03:24 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of GRB 140320C (Mereghetti  et al., GCN 16007)
with AZT-33IK telescope of Mondy observatory starting on Mar. 20 (UT)
15:12:44 and Mar. 23 (UT) 15:37:46. Several images of 120 s exposure in 
R-filter ere obtained in both epochs.  After receiving all data sets we 
refined our measurements of the optical source N3 reported early as one 
of a possible afterglow candidate (Volnova et al., GCN 16012). Enhanced 
position of the source is (J2000) 08 57 34.40 +71 11 54.7 (uncertainty 
of  0.35" is each coordinate) is within XRT error circle and  apart 1.1" 
of the center of XRT localization (Pagani  et al., GCN 16017). A 
photometry of the source:


date       UT start   t-T0      Exp.  Filter  OT     err
                      (mid, days) (s)
2014-03-20 15:12:44  0.08918    1560  R       22.63  0.24
2014-03-20 15:38:46  0.12147    3840  R       23.14  0.28
2014-03-23 15:37:46  3.13782    6960  R       23.5   (3 sigma upper limit)

is based on two USNO-B1.0 stars (R2 mags)

N       Id                      RA               Dec.           R
1       1612-0081687            08:57:32.78     +71:12:43.9     18.9
3       1611-0081293            08:57:55.56     +71:10:05.6     18.8

Based on our photometry we confirm the source N3 (Volnova et al., GCN 
16012) is the afterglow of GRB 140320C.

Finding chart can be found at
http://grb.rssi.ru/GRB140320C/140320C_AZT33IK_fc.png


GRB_name: GRB140226A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16037
SUBJECT: GRB 140226A/iPTF14yb: Mondy optical observations
DATE:    14/03/25 15:11:32 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of transient iPTF14yb (Cenko et al., GCN 15883,
Beardmore et al., GCN 15884, 15891) a possible counterpart of GRB 
140226A (Hurley et al., GCN 15888) with AZT-33IK telescope of Mondy 
observatory on Feb. 28 between (UT) 19:22:46 - 21:52:52 R-filter. On a 
stacked image of 75 x 120 s we clearly detected iPTF14yb source with a 
magnitude of R = 22.86 Â± 0.17 at Feb. 28.85959 (mid) or 2.44087 days 
after GRB 140226A trigger (Hurley et al., GCN 15888).

The photometry is based on SDSS J144600.66+145826.2 star assuming
R(Lupton transformation)= 17.624 +/- 0.018.


GRB_name: GRB140323A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16039
SUBJECT: GRB 140323A : Suzaku WAM observation of the prompt emission 
DATE:    14/03/27 07:53:42 GMT
FROM:    Tetsuya Yasuda at Saitama U  <yasuda@heal.phy.saitama-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 long GRB 140323A (Swift/BAT trigger #592916 ; Troja et al., GCN
16027; Sakamoto et al., GCN 16029; Fermi-GBM detection : Yu and von
Kienlin, GCN 16032; Fermi-LAT detection: Vianello et al., GCN 16034;
Konus-Wind detection : Golenetskii et al., GCN16035) triggered the
Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of
50 keV - 5 MeV at 10:23:12.262 UT (=T0).

The observed light curve shows a multi-peaked structure in two main
episodes lasting from T0-15 s to T0+95 s with a duration (T90) of about
90 seconds. The fluence in 100 - 1000 keV was 1.36 (+/- 0.12) x10^-6 erg/cm^2.
The 1-s peak flux measured from T0+6 s was 2.17 (+0.35, -0.45)
photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-10 s to
T0+95 s is well fitted in 200 keV to 5 MeV by a single power-law with a
photon index of 2.64 (+0.34, -0.28) (chi^2/d.o.f = 12.5/14).

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

The light curves for this burst will be available at:

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


GRB_name: GRB140320D
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16040
SUBJECT: GRB 140320D: Suzaku WAM observation of the prompt emission 
DATE:    14/03/29 03:42:36 GMT
FROM:    Tetsuya Yasuda at Saitama U  <yasuda@heal.phy.saitama-u.ac.jp>

T. Yasuda, M. Tashiro, Y. Terada, 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.), W. Iwakiri(RIKEN), 
Y. Hanabata (ICRR), Y. E. Nakagawa, M. Kokubun, T. Takahashi (ISAS/JAXA), 
Y. Urata (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo)
on behalf of the Suzaku WAM team, report:


The bright, long, and IPN localized GRB 140320D 
(Hurley et al., GCN 16023; Golenetskii et al., GCN 16025) 
triggered the Suzaku Wide-band  All-sky Monitor (WAM) which covers an 
energy range of 50 keV - 5 MeV at 20:21:38.309 UT (=T0). 

The observed light curve shows a multi-peaked structure 
lasting from T0-5 s to T0+50 s with a duration (T90) of about 22 seconds. 
The fluence in 100 - 1000 keV was 1.14 (+0.03, -0.04) x10^-4 erg/cm^2. 
The 1-s peak flux measured from T0+17 s was 35.4 (+0.8, -0.9) photons/cm^2/s 
in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-10.5 s to T0+49.5 s 
is well fitted in 200 keV to 5 MeV by a power-law with exponential cutoff model:
dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
alpha       0.99 (+0.12, -0.13), and
Epeak      746 (+33, -31) keV (chi^2/d.o.f. = 72.1/48).

Fitting by a GRB Band model yields the following parameters:
the low-energy photon index alpha: -0.97 (+0.14, -0.13),
the high-energy photon index beta: <-3.62,
and the peak energy Epeak: 742 (+34, -22) keV (chi^2/d.o.f = 71.4/47).

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

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


GRB_name: GRB140329A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16042
SUBJECT: GRB 140329A: Fermi GBM observation of a bright burst
DATE:    14/03/30 04:31:55 GMT
FROM:    George A. Younes at USRA/NASA/MSFC  <younes.ge@gmail.com>

Andreas von kienlin (MPE) and George Younes (USRA/MSFC)
report on behalf of the Fermi GBM Team:

"At 07:04:38.33 UT on 29 03 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140329A (trigger 417769481 / 140329295).
The trigger resulted in an Autonomous Repoint Request (ARR), but FERMI
went into SAA 120 seconds after trigger.

The on-ground calculated location, using the GBM trigger
data, is RA = 149.8, DEC = -27.44 (J2000 degrees), 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 from the Fermi LAT boresight is 114 degrees.

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

The GBM light curve consists of two pulses seperated by about 25 seconds
with a duration (T90) of about 21.5 s (50-300 keV).
The time-averaged spectrum from T0-2.3 s to T0+33.6 s is
best fit by a Band function with Epeak = 244 +/- 5 keV,
alpha = -0.83 +/- 0.01, and beta = -2.38 +/- 0.04.

The event fluence (10-1000 keV) in this time interval is
(7.07 +/- 0.05)E-5 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+23.6 s in the 8-1000 keV band
is 102.0 +/- 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: GRB140320D
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16043
SUBJECT: GRB 140320D: MASTER optical observations
DATE:    14/03/30 08:42:43 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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.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 located in Tunka  (MASTER-Net: 
http://observ.pereplet.ru)  have done a survey of the large area 
around IPN error box (Hurley et. al. GCN16023). The survey  was started 
2014-03-21 13:15:06  i.e.  16h 53m after the burst and proceeded during 5 
hours. The 5 sigma unfiltered upper limit was ~17.5 m on single 
180 image and ~18.8 m on coadd of 5 images with total exposure  900 s.

We haven't found  credible  optical afterglow candidate within IPN error box.

The covarege map is available at
http://master.sai.msu.ru/static/GRB/GRB140320D_map.png

The message may be cited.


GRB_name: GRB140329A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16045
SUBJECT: IPN Triangulation of GRB 140329A
DATE:    14/03/30 16:09:37 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,

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

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

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

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

The long-duration, bright GRB 140329A (von Kienlin and Younes, GCN Circ. 
16042) has been observed by Fermi (GBM), Konus-Wind, INTEGRAL (SPI-ACS), 
MESSENGER (GRNS), and Mars Odyssey (HEND), so far, at about 25478 s UT 
(07:04:38).

We have triangulated it to a preliminary, 3 sigma error box whose 
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   146.246 (09h 44m 59s) -32.103 (-32d 06' 09")
  Corners:
   145.867 (09h 43m 28s) -31.797 (-31d 47' 49")
   145.948 (09h 43m 47s) -32.076 (-32d 04' 33")
   146.627 (09h 46m 31s) -32.404 (-32d 24' 13")
   146.544 (09h 46m 10s) -32.127 (-32d 07' 39")
  ---------------------------------------------
The error box area is 491 sq.arcmin, and its maximum dimension is 53 
arcmin (the minimum one is 12 arcmin).

The center of the GBM ground position (von Kienlin and Younes, GCN Circ. 
16042) is 5.6 deg from the center of the box.

This box can be improved.

A triangulation map is posted at 
http://www.ioffe.ru/LEA/GRBs/GRB140329_T25481/IPN/


GRB_name: GRB140329A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16046
SUBJECT: Konus-Wind observation of GRB 140329A
DATE:    14/03/30 16:56:28 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:

A long-duration, very intense GRB 140329A
(Fermi-GBM detection: von Kienlin & Younes, GCN 16042;
IPN triangulation: Hurley at al., GCN 16045)
triggered Konus-Wind at T0=25481.877 s UT (07:04:41.877).

The burst light curve starts with a short pulse at ~T0 followed
by a bright multi-peaked complex from ~T0+19 s to ~T0+30 s.
The emission is seen up to ~10 MeV.

As observed by Konus-Wind, the burst had a fluence
of 8.5(-0.7,+0.7)x10^-5 erg/cm2, and a 64-ms peak flux,
measured from T0+23.744 s, of 2.7(-0.3,+0.3)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+33.024 s)
is best fit in the 20 keV - 18 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.04 (-0.09,+0.11),
the high energy photon index beta = -2.30 (-0.17,+0.11),
the peak energy Ep = 238 (-28,+32) keV,
chi2 = 132/95 dof.

The spectrum near the maximum count rate
(measured from T0+23.296 to T0+23.808 s)
is best fit in the 20 keV - 18 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.90 (-0.11,+0.13),
the high energy photon index beta = -2.7 (-1.1,+0.3),
the peak energy Ep = 388 (-66,+75) keV,
chi2 = 68.0/80 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140329_T25481/

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


GRB_name: GRB140329A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16047
SUBJECT: GRB 140329A: Fermi-LAT detection  
DATE:    14/03/30 21:25:29 GMT
FROM:    Daniel Kocevski at GSFC  <daniel.kocevski@nasa.gov>

D. Kocevski (NASA/Goddard), G. Vianello (Stanford U.),  E. Bissaldi (University & INFN Trieste), and J. McEnery (NASA/Goddard)

report on behalf of the Fermi-LAT team:

An on-ground analysis of the IPN triangulation of GRB 140329A (Hurley et. al. GCN16045), which was detected by Fermi-GBM (trigger 417769481, GCN 16042) and initiated an autonomous repoint of the spacecraft, has revealed long-lived high-energy emission detected by Fermi-LAT.  The best LAT on-ground location is found to be:

RA, Dec 145.698,  -32.229 (J2000)

with an error radius of 0.2 deg (90% containment, statistical error only). The burst was outside the LAT field of view at the time of trigger and remained so for an additional 2000 seconds.  The analysis above covers a period from 2000s to 5000s post GBM trigger and an energy range of 100 MeV to 10 GeV.

The Fermi-LAT point of contact for this burst is D. Kocevski (daniel.kocevski@nasa.gov<mailto:daniel.kocevski@nasa.gov>).

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


GRB_name: GRB140330A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16048
SUBJECT: GRB 140330A: Fermi-LAT Detection  
DATE:    14/03/31 04:05:34 GMT
FROM:    Daniel Kocevski at GSFC  <daniel.kocevski@nasa.gov>

G. Vianello (Stanford U.), D. Kocevski (NASA/Goddard), and J. Racusin (NASA/Goddard) report on behalf of the Fermi-LAT team:

At 04:19:54.47 UT on March 30, 2014, Fermi-LAT detected high-energy emission from GRB 140330A, which was also detected by Fermi-GBM (trigger 417845997).

The best LAT on-ground location is found to be

RA, Dec 325.59, -64.30 (J2000)

with an error radius of 0.2 deg (90% containment, statistical error only). This was within 15 deg from the LAT boresight at the time of the trigger.  More than 10 photons above 100 MeV and 2 photons above 1 GeV are observed within 6000 seconds after the GBM trigger. The highest-energy photon is a 4.5 GeV event, which is observed 252 seconds after the GBM trigger.

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

The Fermi-LAT point of contact for this burst is Daniel Kocevski (daniel.kocevski@<mailto:xxxx@xxx.xxx>nasa.gov<http://nasa.gov>).

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


GRB_name: GRB140331A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16049
SUBJECT: GRB 140331A: Swift detection of a burst
DATE:    14/03/31 06:19:48 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

B.-B. Zhang (UAH), S. D. Barthelmy (GSFC), V. D'Elia (ASDC),
J. A. Kennea (PSU), K. L. Page (U Leicester), D. M. Palmer (LANL) and
M. H. Siegel (PSU) report on behalf of the Swift Team:

At 05:49:48 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140331A (trigger=594081).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 134.845, +2.707 which is 
   RA(J2000) = 08h 59m 23s
   Dec(J2000) = +02d 42' 25"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As is usual for an image trigger,
there is no obvious variation in the BAT light curve. 

The XRT began observing the field at 05:56:13.2 UT, 385.0 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source with an enhanced position: RA, Dec 134.8644,
2.7174 which is equivalent to:
   RA(J2000)  = 08h 59m 27.45s
   Dec(J2000) = +02d 43' 02.7"
with an uncertainty of 2.2 arcseconds (radius, 90% containment). This
location is 79 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. No
spectrum from the promptly downlinked event data is yet available to
determine the column density. 

The initial flux in the 2.5 s image was 6.70e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 393 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.05. 

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


GRB_name: GRB140331A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16050
SUBJECT: GRB 140331A: RATIR Optical and NIR Observations
DATE:    14/03/31 08:45:28 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 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 from 2014/03 31.26 to 2014/03
31.32 UTC (0.35 to 1.87 hours after the BAT trigger), obtaining a total of
1.04 hours exposure in the r and i bands and 0.44 hours exposure in the
Z, Y, J, and H bands.

For a source within the Swift-XRT error circle, in comparison with
the SDSS DR9 and 2MASS, we obtain the following detections:

  r     22.02 +/- 0.11
  i     20.79 +/- 0.04
  Z     20.14 +/- 0.06
  Y     19.81 +/- 0.07
  J     19.75 +/- 0.08
  H     19.76 +/- 0.12

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB. This position coincides with a
previously detected source, SDSS J085927.51+024304.0. We note that our
r, i and Z band magnitudes are broadly consistent with those of the SDSS.

Fitting Milky Way, LMC and SMC extinction laws in addition to the IGM
(see Littlejohns, et al. 2014) we find the source is possibly of high
redshift, with a photometric redshift of z = 4.65 (+0.34,-2.80; 90% conf.).
The large lower limit in the confidence region is due to a potential
solution
with a high quantity of Milky Way type dust.

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


GRB_name: GRB130330A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16051
SUBJECT: IPN triangulation of GRB 130330A
DATE:    14/03/31 10:23:19 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,

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

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

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

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

The long-duration GRB 140330A (LAT detection: Vianello, Kocevski, and 
Racusin, GCN 16048) has been observed by Fermi (GBM: trigger 417845997), 
Konus-Wind, INTEGRAL (SPI-ACS), MESSENGER (GRNS), and Mars Odyssey 
(HEND), so far, at about 15594 s UT (04:19:54).

We have triangulated it to a preliminary, 3 sigma error box whose 
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   328.068 (21h 52m 16s) -57.745 (-57d 44' 42")
  Corners:
   326.549 (21h 46m 12s) -57.180 (-57d 10' 46")
   327.145 (21h 48m 35s) -57.662 (-57d 39' 43")
   329.617 (21h 58m 28s) -58.274 (-58d 16' 25")
   328.989 (21h 55m 57s) -57.817 (-57d 49' 00")
  ---------------------------------------------
The error box area is 1482 sq. arcmin, and its maximum dimension is 1.97 
deg (the minimum one is 17 arcmin).

The center of the LAT position (Vianello, Kocevski, and Racusin, GCN 
16048) is 6.6 deg from the center of the box and, hence, this position 
is incorrect (or the LAT source is unrelated to this GRB).

This box may be improved.

A triangulation map is posted at 
http://www.ioffe.ru/LEA/GRBs/GRB140330_T15594/IPN/


GRB_name: GRB140331A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16052
SUBJECT: GRB 140331A: Enhanced Swift-XRT position
DATE:    14/03/31 11:35:29 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Using 4193 s of XRT Photon Counting mode data and 7 UVOT
images for GRB 140331A, 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 = 134.86440, +2.71729 which is equivalent
to:

RA (J2000): 08h 59m 27.46s
Dec (J2000): +02d 43' 02.3"

with an uncertainty of 1.7 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB140331A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16053
SUBJECT: GRB 140331A: MITSuME Okayama upper limits
DATE:    14/03/31 15:22:50 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 140331A (Zhang et al., GCNC 16049)
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 2014-03-31 10:40:24 UT (~4.8 h after the burst).
We could not detect the previously reported afterglow (Littlejohns et al.,
GCNC 16050) in all the three bands.

Three sigma upper limits of the OT are listed below.
We used SDSS-DR7 catalog for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'     Rc     Ic
-----------------------------------------------------
0.21730    11:02:43    2040.0   >19.6  >19.7  >18.7
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB140129A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16054
SUBJECT: GRB 140129A: Mondy optical observations
DATE:    14/03/31 16:05:39 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

GRB 140129A: Mondy optical observations

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 140129A (Melandri et al., GCN
15760)with AZT-33IK telescope of Sayan observatory (Mondy) starting on
on Jan. 29 (UT) 12:21:46. We took several images in R-filter of 60 s
exposure. Within enhanced XRT error circle (Evans, GCN 15764) we
detected the optical afterglow (Melandri et al., GCN 15760).


The details of the photometry are the following:

UT start t-T0 Filter Exp. OT
(mid, days) (s)
12:21:46 0.38805 R 42x60 21.39 +/- 0.25

The photometry is based 3 SDSS stars, R (gri -> R transformations by
Lupton 2005):

SDSS id R
J023133.01-013533.5 18.121
J023122.45-013411.0 18.797
J023137.01-013606.5 19.143


GRB_name: GRB140129B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16055
SUBJECT: GRB 140129B: AAO optical upper limit
DATE:    14/03/31 16:06:47 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

GRB 140129B: AAO optical upper limit

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

We observed the field of Swift GRB 140129B (Bernardini et al., GCN
15765) with AS-32 (0.7m) telescope of Abastumani Observatory starting
on on Jan. 29 (UT) 15:23:49. We obtained several unfiltered frames
with exposures of 120 s. Within the enhanced XRT circle (Goad et al.,
GCN 15770) we do not detect the afterglow (Bernardini et al., GCN
15765; Ivanov et al., GCN 15766).


The details of the photometry are the following:

UT start t-T0 Filter Exp. Uplim
(mid, days) (s) (3 sigma)
15:23:49 0.10949 None 4*120 18.7


The photometry is based on SDSS stars, R mag (R mag obtained using ugriz
transformations in BVRI (Lupton, 2005):

SDSS id R
J214659.19+261356.3 16.404
J214707.35+261127.0 15.825
J214657.00+261421.1 15.385


GRB_name: GRB140330A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16056
SUBJECT: Konus-Wind observation of GRB 140330A
DATE:    14/03/31 16:16:25 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 GRB 140330A
(Fermi LAT detection: Vianello, Kocevski, & Racusin, GCN 16048;
IPN triangulation: Hurley at al., GCN 16051)
triggered Konus-Wind at T0=15594.217 s UT (04:19:54.217).

The burst light curve shows a single pulse from ~T0-3 s to ~T0+15 s.
The emission is seen up to ~10 MeV.

As observed by Konus-Wind, the burst
had a fluence of 3.9(-0.5,+0.6)x10-6 erg/cm2,
and a 64-ms peak flux, measured from T0+0.320 s,
of 1.5(-0.4,+0.4)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+16.640 s)
is best fit in the 20 keV - 18 MeV range
by the cutoff power law with the following model parameters:
the photon index alpha = -0.60(-0.45,+0.55),
and the peak energy Ep = 158(-24,+34) keV,
chi2 = 105/96 dof.
Fitting this spectrum with the Band model yields the same
values of alpha and Ep with an upper limit on beta of -3.3.

The spectrum near the maximum count rate
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 18 MeV range
by the cutoff power law with the following model parameters:
the photon index alpha = -0.18(-0.45,+0.55),
and the peak energy Ep = 172(-21,+28) keV,
chi2 = 89.2/95 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140330_T15594/

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


GRB_name: GRB140331A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16057
SUBJECT: GRB 140331A: Zadko observatory - Gingin optical observations
DATE:    14/03/31 17:22:24 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 140331A detected by SWIFT
(trigger 594081) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 8.26h after the GRB trigger.
The elevation of the field was at 50 degrees above
horizon and weather conditions were good.

We co-added two series of unfiltered
exposures. They show clearly the presence of the object
reported by Littlejohns  et al. (GCNC 16050) that
coincides with SDSS J085927.51+024304.0:

=start=  =end=  Rmag
  8.26h   8.68h  20.1 +/- 0.3
  9.74h  10.43h  20.1 +/- 0.3

The magnitude remains constant during our observation
and is compatible with the magnitude found in visible
bands by Littlejohns  et al. (GCNC 16050) with RATIR
less than two hours after the trigger.
This suggests that the optical object is probably not
the afterglow of GRB 130331A.

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


GRB_name: GRB140330A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16058
SUBJECT: GRB 140330A: intense and persistent gamma-ray emission detected by AGILE
DATE:    14/03/31 17:32:53 GMT
FROM:    Carlotta Pittori at ASDC  <carlotta.pittori@asdc.asi.it>

C. Pittori, F. Verrecchia (ASDC and INAF/OAR),
A. Bulgarelli (INAF/IASF-Bo), A. Giuliani (INAF/IASF-Mi),
M. Tavani (INAF/IAPS Rome, and Univ. Roma Tor Vergata), P. Caraveo 
(INAF/IASF-Mi), F. Lucarelli (ASDC and INAF/OAR), M. Marisaldi
(INAF/IASF-Bo), F. Longo (Univ. of Trieste and INFN Trieste), E. Del
Monte, F. Lazzarotto, I. Donnarumma, Y. Evangelista, M. Feroci,
L. Pacciani, P. Soffitta, E. Costa, I. Lapshov, M. Rapisarda (INAF/IAPS
Rome), G. Barbiellini, (INFN Trieste), F. Fuschino, F. Gianotti,
M. Trifoglio, G. Di Cocco, C. Labanti, V. Fioretti, M. Galli
(INAF/IASF-Bo), S. Mereghetti, F. Perotti (INAF/IASF-Mi), M. Cardillo,
E. Striani, (INAF/IAPS Rome, and Univ. Roma Tor Vergata), A. Argan,
G. Piano, S. Sabatini, V. Vittorini (INAF/IAPS Rome), G. Pucella (ENEA
Frascati), A. Pellizzoni, A. Trois (INAF/OA Cagliari), M. Pilia
(ASTRON), S. Vercellone (INAF/IASF-Pa), P. W. Cattaneo, A. Rappoldi
(INFN Pavia), A. Morselli, P. Picozza (INFN Roma-2), M. Prest,
E. Vallazza (Universita' dell'Insubria), P. Lipari, D. Zanello (INFN
Roma-1), A. Chen (Wits University), S. Colafrancesco (INAF/OAR and Wits
University), P. Giommi, and G. Valentini (ASI),
on behalf of the AGILE Team, report:


The AGILE Gamma Ray Imaging Detector (GRID) observed an intense and
prolonged high-energy emission above 100 MeV from GRB 140330A
(Fermi-LAT detection: G. Vianello et al., GCN 16048).

Despite a data telemetry gap of about 30 minutes occurring during the
prompt emission of this GRB, a maximum likelihood analysis of the
AGILE-GRID data integrated from 2014-03-30 04:50 UT (1805 s since
trigger time) to 2014-03-31 08:00 UT yields a detection at a
significance level larger than 4 sigma, with an average flux of
F=(2.30 +/- 0.98) 10-6 ph/cm2/s (E > 100 MeV).

Due to the high fluence of this burst at E>100 MeV, comparable only to
the one of GRB 130427A as recorded in the AGILE database, it was
possible to derive its properties using the maximum likelihood
techniques routinely used in the standard data analysis of AGILE-GRID
point sources.

This measurement was obtained with AGILE observing a large portion of
the sky in spinning mode.


GRB_name: GRB140323A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16059
SUBJECT: GRB 140323A: Zadko observatory - Gingin optical observations
DATE:    14/03/31 17:47:35 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 140323A detected by SWIFT
(trigger 592916) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 1.0 hour after the GRB trigger.
The elevation of the field was at 27 degrees above
horizon and weather conditions were good.

We co-added a series of exposures. We do not
detect any optical candidate in the XRT error box
provided by Troja et al. (GCNC 16027) at the
limiting magnitude of:

 From t0+1.0h to t0+1.6h Rlim=20.8

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

N.B. Galactic coordinates are lon=306.3802 lat=-36.7801


GRB_name: GRB140302A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16060
SUBJECT: GRB 140302A: TAROT La Silla observatory optical observations
DATE:    14/03/31 18:10:50 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 140302A detected by SWIFT
(trigger 589685) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 36.5s after the GRB trigger
(14.3s after the notice). The elevation of the field increased from
48 degrees above horizon and weather conditions
were excellent.

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+36.5s to t0+96.5s : Rlim = 15.9

The second image is 60.0s exposure in tracking mode.
No afterglow candidate is seen:
t0+140s to t0+200s : Rlim = 19.0

The next images does not show the candidate identified
by Elliott et al. (GCNC 15903) at R=23.7 8.2 min after
the trigger.

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


GRB_name: GRB140331A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16061
SUBJECT: GRB 140331A: Swift/UVOT Upper Limits
DATE:    14/03/31 18:41:14 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU) and B.-B. Zhang (UAH)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140331A
394 s after the BAT trigger (Zhang et al., GCN Circ. 16049).
No optical afterglow consistent with either the enhanced XRT position
(Beardmore et al. GCN Circ. 16052) or the RATIR detection
(Littlejohns et al. GCN Circ. 16050) 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           394          543          147         >21.1
white              394         8016          764         >21.9
v                  550         7092          568         >19.7
b                  649         7912          568         >20.8
u                  624         7707          568         >21.1
w1                 600         7502          563         >21.1
m2                 575         7297          529         >20.5
w2                 700         6887          352         >21.4

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.05 in the direction of the burst
(Schlegel et al. 1998).


