# GCN_circulars

GRB_name: GRB141017A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16929
SUBJECT: Konus-Wind observation of GRB 141017A
DATE:    14/10/20 10:22:18 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

A long-duration GRB 141017A (Swift-BAT trigger 615672:
Marshall et al., GCN 16919; Markwardt et al., GCN 16927)
triggered Konus-Wind at T0=66374.721 s UT (18:26:14.721),
or ~46 s after the BAT trigger.

The KW light curve shows two episodes of the emission.
The first, weaker episode, which triggered BAT, starts at ~T0-47 s
and ends at ~T0-42 s. The second, much more brighter episode,
which triggered KW, shows a double-peaked pulse from ~T0-3 s to ~T0+7 s.
The emission in this episode is visible up to ~1 MeV.

As observed by Konus-Wind, the burst had a fluence
of 4.0(-0.5,+0.5)x10^-6 erg/cm2, and a 64-ms peak flux,
measured from T0+0.704 s, of 1.8(-0.2,+0.2)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the second episode
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 1.5 MeV range
by the cutoff power law with the following model parameters:
the photon index alpha = -0.89(-0.28,+0.31),
and the peak energy Ep = 97(-10,+12) keV,
chi2 = 73/60 dof.
Fitting this spectrum with the Band model yields the same
values of alpha and Ep and an upper limit on beta of -3.0

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB141017_T66374/

All the quoted errors are at the 95% confidence level.
All the quoted values are preliminary.


GRB_name: GRB141020B
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16930
SUBJECT: GRB 141020B: MAXI/GSC detection
DATE:    14/10/20 13:38:33 GMT
FROM:    Motoko Suzuki at RIKEN  <motoko@crab.riken.jp>

R. Imatani (Osaka U.), M. Serino (RIKEN), S. Nakahira (JAXA), T. Sakamoto (AGU),
S. Ueno, H. Tomida, 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, T. Yoshii, Y. Tachibana (Tokyo Tech),
A. Yoshida, Y. Kawakubo, H. Ohtsuki (AGU),
H. Tsunemi, D. Uchida (Osaka U.),
H. Negoro, M. Nakajima, K. Fukushima, T. Onodera, K. Suzuki, T. Namba, M. Fujita, F. Honda (Nihon U.),
Y. Ueda, M. Shidatsu, T. Kawamuro, T. Hori (Kyoto U.),
Y. Tsuboi, A. Kawagoe (Chuo U.),
M. Yamauchi, Y. Morooka, D. Itoh (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 10:59:25 UT.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (214.296 deg, 7.984 deg) = (14 17 11, +07 59 02) (J2000)
with a statistical 90% C.L. elliptical error region
with long and short radii of 0.36 deg and 0.25 deg respectively.
The roll angle of long axis from the north direction is 57.0 deg counterclockwise.
There is an additional systematic uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 114 +- 24 mCrab
(4-10keV, 1 sigma error).
There was no significant excess flux in the previous transit at 09:26 UT
and in the next transit at 12:32 UT 
with an upper limit of 20 mCrab for each.  

Since the source is only 21 degrees from the Sun (Sun constrained for next 45 days), 
no immediate Swift observation is possible.  


GRB_name: GRB141020A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16931
SUBJECT: GRB 141020A: Enhanced Swift-XRT position
DATE:    14/10/20 14:13:36 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 2694 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 141020A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 224.99618, +55.31341 which is equivalent
to:

RA (J2000): 14h 59m 59.08s
Dec (J2000): +55d 18' 48.3"

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: GRB141020A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16932
SUBJECT: GRB 141020A: Swift/UVOT Detection
DATE:    14/10/20 15:59:40 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N.P. M. Kuin (UCL-MSSL) and S. B. Cenko (GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 141020A
92 s after the BAT trigger (Cenko et al., GCN Circ. 16928). A source
consistent with the XRT position  (Osborne et al. GCN Circ. 16931)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  14:59:59.15 = 224.99646 (deg.)
    Dec (J2000) = +55:18:46.7  =  55.31297 (deg.)
with an estimated uncertainty of 0.43 arc sec. (radius, 90% confidence).

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

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

white               92          241          147         18.02 +/- 0.04
v                  634         1409           58         18.40 +/- 0.23
b                  559          753           39         18.66 +/- 0.18
u                  304          554          246         18.48 +/- 0.09
w1                 683         6660          471        >20.9
m2                1238         6455          413        >21.1
w2                 784        11546         1196        >21.8

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.01 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB141020A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16933
SUBJECT: GRB 141020A: 1.4 GHZ observation
DATE:    14/10/20 17:19:46 GMT
FROM:    Dirk Grupe at Swift-XRT  <dgrupe007@gmail.com>

D. Grupe and B. Malphrus (Space Science Center,  Morehead State
University) report:

We observed the UVOT position of GRB 141020A (Cenko et al., GCN
Circ. 16928) with the 21m Morehead State University 21m Space
Tracking Antenna at 1.4 GHz at 2014-10-20 13:20 UT, 5.5 hours after
the burst. We did not detect any source at the position of the
burst. The minimal detactable flux density of the MSU 21m telescope
is 2 Jy.  


GRB_name: GRB141020A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16934
SUBJECT: GRB 141020A: Swift-XRT refined Analysis
DATE:    14/10/20 20:01:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

C. Pagani (U. Leicester), B. Sbarufatti (INAF-OAB/PSU), P. D'Avanzo
(INAF-OAB), V. D'Elia (ASDC), 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 9.8 ks of XRT data for GRB 141020A (Cenko  et al. GCN
Circ. 16928),  from 72 s to 23.9 ks after the  BAT trigger. The data
comprise 6 s in Windowed Timing (WT) mode (taken while Swift was
slewing), with the remainder in Photon Counting (PC) mode. The enhanced
XRT position for this burst was given by Osborne et al. (GCN Circ.
16931).

The late-time light curve (from T0+4.8 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.10 (+0.24, -0.22).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.80 (+0.16, -0.13). The
best-fitting absorption column is  2.3 (+3.6, -1.0) x 10^20 cm^-2,
consistent with the Galactic value of 1.2 x 10^20 cm^-2 (Willingale et
al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 3.5 x 10^-11 (3.7 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.3 (+3.6, -1.0) x 10^20 cm^-2
Galactic foreground: 1.2 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.80 (+0.16, -0.13)

If the light curve continues to decay with a power-law decay index of
1.10, the count rate at T+24 hours will be 3.1 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x
10^-13 (1.1 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00615873.

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


GRB_name: GRB141020A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16935
SUBJECT: GRB 141020A: Swift-BAT refined analysis
DATE:    14/10/20 21:06:53 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 (GSFC/UMBC), C. B. Markwardt (GSFC),
T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC),
T. N. Ukwatta (LANL) (i.e. the Swift-BAT team):

Using the data set from T-61 to T+242 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 141020A (trigger #615873)
(Cenko, et al., GCN Circ. 16928).  The BAT ground-calculated position is
RA, Dec = 225.054, 55.328 deg which is
    RA(J2000)  =  15h 00m 12.9s
    Dec(J2000) = +55d 19' 42.3"
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 67%.

The mask-weighted light curve shows a broad structure with multiple peaks
superimposed starting at T-8 sec and continuing until T+13 sec.  T90 (15-350
keV) is 15.55 +- 2.05 sec (estimated error including systematics).

The time-averaged spectrum from T-5.66 to T+11.30 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.74 +- 0.18.  The fluence in the 15-150 keV band is 4.6 +- 0.6 x 10^-7
erg/cm2. The 1-sec peak photon flux measured from T-0.20 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/615873/BA/


GRB_name: GRB141004A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16936
SUBJECT: GRB 141004A: La Palma late-time observations and possible brightening
DATE:    14/10/20 21:09:31 GMT
FROM:    Steve Schulze at U of Iceland  <sts30@hi.is>

S. Schulze (PUC, MAS), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), K. Wiersema (U. Leicester), D. Xu (DARK/NBI), N. R. Tanvir (U. Leicester), D. Malesani, J. P. U. Fynbo (DARK/NBI), P. Jakobsson (U. Iceland), V. Nascimbeni (INAF/OAPd), J. Harmanen (NOT), and O. Vaduvescu (ING) report on behalf of a larger collaboration:

We monitored the optical counterpart of GRB 141004A (D'Elia et al., GCN 16878; Mereghetti et al., GCN 16879) with the 2.5-m Nordic Optical Telescope (NOT), the 4.2-m William Herschel Telescope (WHT), and the 10.4-m Gran Telescopio Canarias (GTC). The latest NOT observation was secured with ALFOSC on October 14.17 (9.19 days after the burst) and consisted of 9x240-s in i' band. In the same night we obtained a deep 8x300-s image with ACAM mounted at the WHT in r' band starting at October 14.17. A GTC observation was secured on October 18.24  (13.27 days after the burst) and consisted of 3x180 s in r' band and 4x120 s in i' band.

We applied differential photometry to check for variability using six unsaturated nearby stars. The transient did not change its brightness in r band by more than ~0.10 mag, but in the i' band our photometry indicates a tentative brightening by 0.46 +/- 0.27 mag.

While the detected variability is only marginally significant, this behaviour is consistent with the emergence of a SN similar to SN 1998bw, both in terms of brightness and color evolution. We encourage further follow-up to test for the presence of an emerging SN.


GRB_name: GRB141004A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16937
SUBJECT: GRB 141004A: RATIR Late Time Optical and NIR Observations
DATE:    14/10/21 21:58:12 GMT
FROM:    Owen Littlejohns at Az State U  <olittlej@asu.edu>

Owen Littlejohns (ASU), Nat Butler (ASU), Alan M. Watson (UNAM),
Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer
(UNAM), Chris Klein (UCB), Ori Fox (UCB), J. Xavier Prochaska (UCSC),
Josh Bloom (UCB), Antonino Cucchiara (ORAU/GSFC), Eleonora Troja
(GSFC), Enrico Ramirez-Ruiz (UCSC), JosÃ© A. de Diego (UNAM), Leonid
Georgiev (UNAM), JesÃºs GonzÃ¡lez (UNAM), Carlos RomÃ¡n-ZÃºÃ±iga (UNAM),
Neil Gehrels (GSFC), and Harvey Moseley (GSFC) report:

We observed the field of GRB 141004A (D'Elia, et al., GCN 16878) with
the Reionization and Transients Infrared Camera (RATIR; www.ratir.org)
on the 1.5m Harold Johnson Telescope at the Observatorio AstronÃ³mico
Nacional on Sierra San Pedro MÃ¡rtir from 2014/10 21.31 to 2014/10 21.51
UTC (392.08 to 396.95 hours after the BAT trigger), obtaining a total
of 3.89 hours exposure in the r, i and z bands.

We continue to detect the source reported from the previous epoch of
RATIR observations (Littlejohns, et al., GCN 16887). We obtain the
following detections and upper limit (3-sigma):

  r     24.21 +/- 0.24
  i     23.24 +/- 0.14
  z     > 21.47

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

These magnitudes suggest the source to remain brighter than expected if
determined purely from a typical GRB power-law decay. This may
corroborate the claim of re-brightening (Schulze, et al., GCN 16936),
however, it may also indicate the detection of the host galaxy (de Ugarte
Postigo, et al., GCN 16902). We also note that these magnitudes are
broadly consistent with those observed by GROND at an approximate epoch
of 32 hours after the initial Swift/BAT trigger (Schmidl, et al., GCN
16899).

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


GRB_name: GRB141022A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16938
SUBJECT: GRB 141022A: Swift detection of a burst
DATE:    14/10/22 01:48:24 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. Vargas (PSU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), J. A. Kennea (PSU), V. Mangano (PSU),
D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/PSU) and
T. N. Ukwatta (LANL) report on behalf of the Swift Team:

At 01:27:42 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 141022A (trigger=616061).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 241.901, -72.129 which is 
   RA(J2000) = 16h 07m 36s
   Dec(J2000) = -72d 07' 44"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with a duration of about 30 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~8 sec after the trigger. 

The XRT began observing the field at 01:29:57.6 UT, 134.9 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 241.8698, -72.1255
which is equivalent to:
   RA(J2000)  = 16h 07m 28.75s
   Dec(J2000) = -72d 07' 31.7"
with an uncertainty of 2.2 arcseconds (radius, 90% containment). This
location is 36 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (1.04 x
10^21 cm^-2, Willingale et al. 2013), with an excess column of 7.9
(+6.17/-4.49) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
135 seconds after the BAT trigger. No credible afterglow candidate has been
found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the
XRT error circle. The typical 3-sigma upper limit has been about 19.2 mag. The
8'x8' region for the list of sources generated on-board covers 100% of the XRT
error circle. Because of the density of catalogued stars, further analysis is
required to report an upper limit for any afterglow in the region. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.10. 

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


GRB_name: GRB141022A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16939
SUBJECT: GRB 141022A: GROND Detection of a possible Optical Afterglow Candidate
DATE:    14/10/22 06:18:29 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

D.A. Kann (TLS Tautenburg), T. Schweyer, J. F. Graham, J. Greiner 
(all MPE Garching) report on behalf of the GROND team:

We observed the field of GRB 141022A (Swift trigger 616061; Vargas et
al., GCN #16938) simultaneously in g'r'i'z'JHK with GROND (Greiner et
al. 2008, PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La
Silla Observatory (Chile).

Observations started at 01:39 UT on October 22nd, approximately 20 min
after the GRB trigger. They were performed on a setting target at high
airmass (~2.7) until reaching the pointing limit.

Despite a crowed field we find only a single object in the 2.2"
Swift-XRT enhanced error circle reported by Vargas et al., GCN #16938) at

RA (J2000) = 16h 07m 28.82s
DEC (J2000) = -72d 07' 29.6"  

(error of 0".5) but cannot ascertain variability in images centered 
875 sec  and 2095 sec after the trigger, and note the possibility 
of a chance coincidence given the density of objects in the field.  
We intended subsequent observations to determine variability.

Based on a 16.5 min sequence of exposures, we estimate preliminary
magnitudes and limits (all in AB system) of:

g' = 23.6 +/- 0.2 mag
r' = 22.2 +/- 0.1 mag
i' = 21.6 +/- 0.1 mag
z' = 22.0 +/- 0.2 mag
J > 20.9 mag
H > 20.3 mag
K > 19.8 mag

Given magnitudes are calibrated against GROND zeropoints and 2MASS field
stars and are not corrected for the expected Galactic foreground
extinction corresponding to a reddening of E_(B-V)=0.1 mag in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB141015A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16940
SUBJECT: GRB141015A iTelescope observation
DATE:    14/10/22 08:37:23 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

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

We observed the field of GRB 141015A detected by Swift (trigger #615399; 
Troja et al., GCN Circ. 16909) with the iTelescope.Net (http://www.itelescope.net) 
T05 (0.25 m Takahashi Epsilon) telescope located at the New Mexico Skies Observatory 
(NM, USA).  

20 images of 60 sec exposures were taken in the Red filter starting from October 15 
09:37:23 (UT) about 26 minutes after the trigger and stopped on October 5 10:04:00 (UT).  
We do not detect the optical afterglow both in the individual images and the stacked 
image at the enhanced X-ray afterglow position (Evans et al., GCN Circ. 16913).  
The estimated five sigma upper limit of the combined image (total exposure of 1200 sec) 
is ~17.1 using the USNO-B1 catalog.


GRB_name: GRB141022A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16941
SUBJECT: GRB 141022A: Swift-XRT refined Analysis
DATE:    14/10/22 13:48:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), M. de Pasquale (INAF-IASFPA),
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 A. Vargas report on behalf of the Swift-XRT team:

We have analysed 10 ks of XRT data for GRB 141022A (Vargas  et al. GCN
Circ. 16938),  from 144 s to 25.5 ks after the BAT trigger. The data
are entirely in Photon Counting (PC) mode. The best available XRT
position  (using the promptly downlinked event data, the XRT-UVOT
alignment and matching UVOT field sources to the USNO-B1 catalogue) is
RA, Dec = 241.8696, -72.1254 which is equivalent to:

RA (J2000): 16 07 28.70
Dec(J2000): -72 07 31.4

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

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.21 (+/-0.08).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.5 (+0.5, -0.4). The
best-fitting absorption column is  1.1 (+0.5, -0.4) x 10^22 cm^-2, in
excess of the Galactic value of 1.0 x 10^21 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.9 x 10^-11 (1.2 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.1 (+0.5, -0.4) x 10^22 cm^-2
Galactic foreground: 1.0 x 10^21 cm^-2
Excess significance: 4.5 sigma
Photon index:      2.5 (+0.5, -0.4)

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 2.7 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.0 x
10^-14 (3.3 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/00616061.

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


GRB_name: GRB141022A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16942
SUBJECT: GRB 141022A: Swift-BAT refined analysis
DATE:    14/10/22 18:31:58 GMT
FROM:    Tilan Ukwatta at MSU  <tilan.ukwatta@gmail.com>

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 (GSFC/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (LANL), A. Vargas (PSU)
(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 141022A (trigger #616061) (Vargas, et al., GCN Circ. 16938).
The BAT ground-calculated position is
RA, Dec = 241.930, -72.152 deg which is
   RA(J2000)  =  16h 07m 43.1s
   Dec(J2000) = -72d 09' 06.7"
with an uncertainty of 2.2 arcmin, (radius, sys+stat,
90% containment). The partial coding was 39%.

The mask-weighted light curve shows a weak episode starting
at ~T-1.0 sec, and ending around T+10 sec. The burst location
came into the BAT FOV around ~T-140 sec. T90 (15-350 keV)
is 8.72 +- 1.56 sec (estimated error including systematics).

The time-averaged spectrum from T-0.38 to T+9.17 sec is best
fit by a simple power-law model.  The power law index of the
time-averaged spectrum is 1.31 +- 0.27.  The fluence in the
15-150 keV band is 4.8 +- 0.7 x 10^-07 erg/cm2. The 1-sec
peak photon flux measured from T+6.20 sec in the 15-150 keV
band is 0.9 +- 0.3 ph/cm2/sec.  All the quoted errors are
at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/616061/BA/


GRB_name: GRB141020A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16943
SUBJECT: GRB 141020A: Mondy optical observations
DATE:    14/10/22 18:36:37 GMT
FROM:    Alexei Pozanenko at IKI  <alex@grb.rssi.ru>

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

We observed the field of the Swift GRB 141020A  (Cenko et al., GCN 16928) with with AZT-33IK telescope of Sayan observatory (Mondy). We obtained several images on Oct. 20 starting on (UT) 13:28:20.  At the position reported in (Kuin et al., GCN 16932) we clearly detect the afterglow of GRB 141020A  (Cenko et al., GCN 16928; Kuin et al., GCN 16932). Preliminary photometry is following:

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

2014-10-20  13:28:20  10.2672     R       45*120   22.0   0.3
 

The photometry is based on SDSS stars

SDSS                     R_Lupton

J150002.80+552112.7      16.749
J150012.34+552137.2      17.210
J150017.07+551830.3      18.482
J150000.59+552221.9      17.001 

The finding chart can be found in
http://grb.rssi.ru/GRB141020A/GRB141020A_R_AZT33IK_fc.png


GRB_name: GRB141022A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16944
SUBJECT: GRB 141022A: Swift/UVOT Upper Limits
DATE:    14/10/22 20:09:48 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU) and A. Vargas (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 141022A
136 s after the BAT trigger (Vargas et al., GCN Circ. 16938).
No optical afterglow consistent with the optical position
(Kann et al. GCN Circ. 16939) 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)             136          386          246         >20.2
v                  443         1997          194         >19.9
b                  392         1946          214         >20.6
u                  136         1921          568         >20.7
uvw1               493         1895          175         >20.7
uvm2               468         2011          185         >20.5
uvw2               418         1973          194         >20.5

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.10 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB141022B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16945
SUBJECT: GRB141022B: Fermi GBM Detection
DATE:    14/10/23 19:01:08 GMT
FROM:    Matthew Stanbro at UAH/Fermi  <mcs0001@uah.edu>

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

"At 02:04:40.21 UT on 22 October 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 141022B (trigger 435636283 / 141022087).

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 = 119.4, DEC = -75.2 (J2000 degrees,
equivalent to 7h 58m, -75d 12'), with an uncertainty
of 1.0 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).

The angle from the Fermi LAT boresight is 110 degrees.

The GBM light curve consists of a single episode consisting of
several pulses with a duration (T90) of about 9.2 s (50-300 keV).
The time-averaged spectrum from T0+1.9 s to T0+12.2 s is well
fit by a Band function with Epeak = 368.1 (+/-11.2) keV,
alpha = -0.64 +/- 0.02 , and beta = -2.41 (+/-0.05).

The event fluence (10-1000 keV) in this time interval is
(7.87 +/- 0.07)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+3.328 s in the 10-1000 keV band
is 62.9 +/- 1.2 ph/s/cm^2.

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


GRB_name: GRB141022A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16946
SUBJECT: GRB141022A: Fermi GBM Detection
DATE:    14/10/23 19:54:27 GMT
FROM:    Matthew Stanbro at UAH/Fermi  <mcs0001@uah.edu>

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

"At 01:27:48.52 UT on 22 October 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 141022A (trigger 141022061 / 141022061)
which was also detected by Swift BAT (Vargas et al. 2014, GCN 16938).
The GBM on-ground location, using the Fermi GBM trigger data,
is consistent with Swift's location.

The GBM light curve shows a long burst, consisting of one main episode,
with a total duration (T90) of about 11.5 s (50-300 keV).
The time-averaged spectrum from T0-6.1 s to T0+6.1 s is well fit
by a power law function with an exponential high-energy cutoff.
The power law index is -0.8 +/- 0.3 and the cutoff energy,
parameterized as Epeak, is 231.5 +/- 71.1 keV.

The event fluence (10-1000 keV) in this time interval is
(1.2 +/- 0.2)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0-5.696 s in the 10-1000 keV band is 1.1 +/- 0.2 ph/s/cm^2.

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


GRB_name: GRB141020A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16947
SUBJECT: GRB 141020A: Khureltogot optical upper limit
DATE:    14/10/25 00:46:27 GMT
FROM:    Alexei Pozanenko at IKI  <alex@grb.rssi.ru>

E. Mazaeva (IKI), S. Schmalz (AIP), N. Tungalag (Research Center of Astronomy and Geophysics MAS),  A. Volnova (IKI), I.Molotov (KIAM), A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration:
 
We observed the field of the Swift GRB 141020A  (Cenko et al., GCN 16928) with ORI-40 telescope of Khureltogot observatory. We obtained several unfiltered images on Oct. 20 starting on (UT) 12:09:56.  At the position reported in (Kuin et al., GCN 16932) we do not detect the afterglow of GRB 141020A  (Cenko et al., GCN 16928; Kuin et al., GCN 16932; Mazaeva et al., GCN 16943). Preliminary photometry is following:

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

2014-10-20  12:09:56  0.2037     clear   60*60  n/d   19.8

The photometry is based on SDSS stars reported in GCN 16943.


GRB_name: GRB141020A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16948
SUBJECT: GRB 141020A: AAO optical upper limit
DATE:    14/10/25 00:48:28 GMT
FROM:    Alexei Pozanenko at IKI  <alex@grb.rssi.ru>

E. Mazaeva (IKI), R. Inasaridze (AAO), A. Volnova (IKI), Molotov (KIAM), A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration:
 
We observed the field of the Swift GRB 141020A  (Cenko et al., GCN 16928) with AS-32 (0.7m) telescope of Abastumani Observatory. We obtained several unfiltered images on Oct. 20 starting on (UT) 15:41:01.  At the position reported in (Kuin et al., GCN 16932) we do not detect the afterglow of GRB 141020A  (Cenko et al., GCN 16928; Kuin et al., GCN 16932; Mazaeva et al., GCN 16943). Preliminary photometry is following:

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

2014-10-20  15:41:01  0.3630      clear   38*120  n/d   21.4

The photometry is based on SDSS stars reported in GCN 16943.


GRB_name: GRB141026A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16950
SUBJECT: GRB 141026A: Swift detection of a burst
DATE:    14/10/26 02:50:59 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

L. M. Z. Hagen (PSU), S. D. Barthelmy (GSFC), N. Gehrels (NASA/GSFC),
J. A. Kennea (PSU), A. Y. Lien (GSFC/UMBC),
F. E. Marshall (NASA/GSFC), B. Sbarufatti (INAF-OAB/PSU) and
M. H. Siegel (PSU) report on behalf of the Swift Team:

At 02:36:51 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 141026A (trigger=616502).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 44.080, +26.960 which is 
   RA(J2000)  =  02h 56m 19s
   Dec(J2000) = +26d 57' 36"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The real-time TDRSS BAT light curve does not show
anything as is typical for an image trigger. 

The XRT began observing the field at 02:39:28.2 UT, 157.0 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 44.0839, 26.9262 which is equivalent to:
   RA(J2000)  = +02h 56m 20.14s
   Dec(J2000) = +26d 55' 34.3"
with an uncertainty of 6.1 arcseconds (radius, 90% containment). This
location is 122 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 0.1 s image was 1.58e-08 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of  43 seconds with the White filter
starting 165 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
0.19. 

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


GRB_name: GRB141026A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16951
SUBJECT: GRB 141026A: P60 early observations
DATE:    14/10/26 04:07:01 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

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

The Palomar 60-inch telescope automatically responded to the alert for 
GRB 141026A (Hagen et al, GCN 16950) and began imaging the field at 
02:41:55.320 UT, 5.07 minutes after the Swift trigger.  A sequence of 
60-second r, i, and z exposures was obtained.  The field was at high 
airmass (~3.3) at the start of the observations.

We do not detect any clear source inside the XRT error circle in the 
individual exposures.  After stacking the first 11 frames taken in each 
filter, in the r-band stack only there is a marginal detection of a 
possible source at RA = 02:56:19.885, dec = +26:55:35.80 with R~22 mag.

Observations are continuing and additional follow-up is planned.


GRB_name: GRB141026A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16952
SUBJECT: GRB 141026A: RATIR Optical Observations
DATE:    14/10/26 05:47:05 GMT
FROM:    Owen Littlejohns at Az State U  <olittlej@asu.edu>

Owen Littlejohns (ASU), Nat Butler (ASU), Antonino Cucchiara
(ORAU/GSFC), 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),
JosÃ© A. de Diego (UNAM), Leonid Georgiev (UNAM), JesÃºs GonzÃ¡lez
(UNAM), Carlos RomÃ¡n-ZÃºÃ±iga (UNAM), Neil Gehrels (GSFC), and
Harvey Moseley (GSFC) report:

We observed the field of GRB 141026A (Hagen, et al., GCN 16950)
with the Reionization and Transients Infrared Camera (RATIR;
www.ratir.org) on the 1.5m Harold Johnson Telescope at the
Observatorio AstronÃ³mico Nacional on Sierra San Pedro MÃ¡rtir from
26.13 to 26.20 UTC (0.54 to 2.20 hours after the BAT trigger),
obtaining a total of 1.07 hours exposure in the r and i bands.

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

  r     > 23.50
  i     > 23.56

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

We do not detect the source observed by P60 (Perley, et al., GCN
16951). We do, however, detect a source at the edge of the Swift-
XRT error circle at RA(J2000) = 44.084036, Dec(J2000) = 26.928134.

  r     21.67 +/- 0.08
  i     21.52 +/- 0.07

We cannot presently determine if this source is fading.

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


GRB_name: GRB141026A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16953
SUBJECT: GRB 141026A: GROND observations
DATE:    14/10/26 05:56:23 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

K. Varela (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 141026A (Swift trigger 616502; Hagen et al.,
GCN #16950) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La Silla
Observatory (Chile).

Observations started at 02:51 UT on October 26th, approximately 15 min
after the GRB trigger. They were performed at high airmass (2.5 but
rising) but decent seeing (1".2).

At the position of the P60 candidate (Perley, GCN #16951) we do not detect
any source. We find a source just to the north of the 5".8 Swift-XRT error
circle reported by Hagen et al. at

RA (J2000) = 02:56:20.16
DEC (J2000) = +26:55:41.4

with an error of 0".5. This source is also reported by RATIR (Littlejohns
et al., GCN #16952). We do not find any variability within errors over the
course of our observations. It is likely not associated with the GRB.

Based on images with an exposure time of 1500 s in the optical and 1200 s
in the NIR, centered at 0.05598 days after the trigger, we estimate
preliminary magnitudes and limits (all in AB system) for this source of:

g' = 23.2 +/- 0.1 mag
r' = 21.8 +/- 0.1 mag
i' = 21.5 +/- 0.1 mag
z' = 21.2 +/- 0.1 mag
J = 20.9 +/- 0.3 mag
H = 20.5 +/- 0.3 mag
K > 18.7 mag

Given magnitudes are calibrated against GROND zeropoints (g'r'i'z') and
2MASS field stars (JHK) and are not corrected for the expected Galactic
foreground extinction corresponding to a reddening of E_(B-V)=0.18 mag in
the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB141026A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16954
SUBJECT: GRB 141026A: 1.23m CAHA I-band observations
DATE:    14/10/26 06:22:36 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC/UPV-EHU), S. Hellmich (DLR), A. de Ugarte Postigo
(IAA-CSIC/DARK), S. Mottola (DLR), report on behalf of a larger
collaboration:

We observed the field of the GRB141026A (Hagen, et al., GCN 16950) with
the 1.23m CAHA telescope in the I-band filter. Observations started on
Oct. 26.11639 UT (10.75 min post burst). A faint object is detected at
RA=02:56:20.13, DEC=26:55:41.3 (+/-0.6", J2000) with Vega magnitude I~20.6
against the USNO B1.0 catalog. The coordinates of this object are
consistent with the ones reported by Littlejohns et al. (GCN 16592) and
Varela et al. (GCN 16953). No object brighter than I~21.0 (Vega) is
detected consistent with the optical source reported by Perley (GCN
16951).


GRB_name: GRB141026A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16955
SUBJECT: GRB141026A: Deep P200 optical imaging
DATE:    14/10/26 07:51:45 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley, M. Brown, I. Wong, and E. Bailey (Caltech) report:

We imaged the location of GRB 141026A (Hagen et al., GCN 16950) using 
the Large-Format Camera on the 5m Hale Telescope at Palomar Observatory. 
  Six exposures of four minutes each were acquired using the Broad-RI 
(620-920 nm) filter between 03:34:50 and 04:03:51 UT (58-87 minutes 
after the BAT trigger).

The object north of the error circle reported by Littlejohns et al. (GCN 
16592), Varela et al. (GCN 16953), and Gorosabel et. al (GCN 16954) is 
well-detected in the stacked image.  No other object is detected in or 
near the XRT error circle, including at the position of the 
previously-reported, low-significance object from the early P60 imaging 
(GCN 16951), down to a limit of RI > 25.5 mag (calibrated relative to 
the R2 magnitude of a nearby USNO B1.0 star).


GRB_name: GRB141026A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16956
SUBJECT: GRB 141026A: Enhanced Swift-XRT position
DATE:    14/10/26 12:06:07 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 2855 s of XRT Photon Counting mode data and 8 UVOT
images for GRB 141026A, 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 = 44.08435, +26.92804 which is equivalent
to:

RA (J2000): 02h 56m 20.24s
Dec (J2000): +26d 55' 40.9"

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: GRB141026A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16957
SUBJECT: GRB 141026A: MASTER early optical observations 
DATE:    14/10/26 12:24:38 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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

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

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

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


MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in 
Kislovodsk was pointed to the  GRB141026A 22 sec after notice time and 99 sec 
after trigger time at 2014-10-26 02:38:31 UT in two polarizations. On our first 
single and coadd images we haven't found optical transient  within SWIFT 
error-box (Hagen et. al. GCN 16950). The 5-sigma upper limit has been about 
16.5 on single (20s exposure) and 17.5 on coadd image (from first 3 images with 
total exposure 80 sec). The message may be cited.

The publication delay was due to time zone changes during this night.

This message may be cited.


GRB_name: GRB141026A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16958
SUBJECT: GRB 141026A: MASTER early optical observations
DATE:    14/10/26 12:26:01 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

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

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

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

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

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

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

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


MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Kislovodsk was pointed to the  GRB141026A 22 sec after notice 
time and 99 sec after trigger time at 2014-10-26 02:38:31 UT in two 
polarizations. On our first single and coadd images we haven't found 
optical transient  within SWIFT error-box (Hagen et. al. GCN 16950). The 
5-sigma upper limit has been about 16.5 on single (20s exposure) and 17.5 
on coadd image (from first 3 images with total exposure 80 sec). The 
message may be cited.

This message may be cited.

[GCN OPS NOTE: The disrtibution was delayed ~8.8 hours due to a problem
with the authentication process.]


GRB_name: GRB141026A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16960
SUBJECT: GRB 141026A: Swift-BAT refined analysis
DATE:    14/10/26 14:41:51 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

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

Using the data set from T-239 to T+380 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 141026A (trigger #616502)
(Hagen, et al., GCN Circ. 16950).  The BAT ground-calculated position is
RA, Dec = 44.049, 26.925 deg which is 
  RA(J2000)  =  02h 56m 11.8s 
  Dec(J2000) = +26d 55' 31.7" 
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 88%.

The mask-weighted light curve shows a weak episode starting at ~T+15 sec, 
and ending around ~T+180 sec.  T90 (15-350 keV) is 146 +- 13 sec (estimated 
error including systematics).  Note since this GRB went outside the FOV of 
BAT around ~T+250 sec, this duration measurement might be affected if there 
were significant emission from the source after ~T+250 sec.  

The time-averaged spectrum from T+13.96 to T+177.75 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.34 +- 0.19.  The fluence in the 15-150 keV band is 1.3 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+65.64 sec in the 15-150 keV band
is 0.4 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/616502/BA/


GRB_name: GRB141026A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16961
SUBJECT: GRB 141026A: Swift-XRT refined Analysis
DATE:    14/10/26 17:51:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 10 ks of XRT data for GRB 141026A (Hagen  et al. GCN
Circ. 16950),  from 160 s to 46.2 ks after the BAT trigger. The data
comprise 49 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. 16956).

The late-time light curve (from T0+3.5 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.35 (+0.11, -0.12).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.07 (+0.09, -0.08). The
best-fitting absorption column is  4.9 (+/-0.5) x 10^21 cm^-2, in
excess of the Galactic value of 1.6 x 10^21 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.92 (+0.28, -0.26)
and a best-fitting absorption column of 2.8 (+1.2, -1.0) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.8 x 10^-11 (5.4 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.8 (+1.2, -1.0) x 10^21 cm^-2
Galactic foreground: 1.6 x 10^21 cm^-2
Excess significance: 2.0 sigma
Photon index:      1.92 (+0.28, -0.26)

If the light curve continues to decay with a power-law decay index of
0.35, the count rate at T+24 hours will be 0.023 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 8.9 x
10^-13 (1.2 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00616502.

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


GRB_name: GRB141026A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16962
SUBJECT: GRB 141026A: Continued RATIR Optical and NIR Observations, Afterglow Detection
DATE:    14/10/26 18:50:06 GMT
FROM:    Nat Butler at UC berkeley  <natxbutler@gmail.com>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB),
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara
(ORAU/GSFC), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), JosÃ© A. de Diego (UNAM), Leonid Georgiev (UNAM), JesÃºs
GonzÃ¡lez (UNAM), Carlos RomÃ¡n-ZÃºÃ±iga (UNAM), Neil Gehrels (GSFC), and
Harvey Moseley (GSFC) report:

We observed the field of GRB 141026A (Hagen, et al., GCN 16950)) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio AstronÃ³mico Nacional on
Sierra San Pedro MÃ¡rtir from 2014/10 26.13 to 2014/10 26.26 UTC (0.54 to
3.58 hours after the BAT trigger), obtaining a total of 2.49 hours exposure
in the r, i, and z bands.

With increased time-coverage, the source reported in Littlejohns et al.
(GCN 16952; also Perley et al., GCN 16955, Varela et al., GCN 16953,
Gorosabel et al., GCN 16954, ) appears to peak on a timescale of 1 hour,
and then fade in the r and i bands.  Given also that its position is
consistent with the enhanched XRT error region (Beardmore et al., GCN
16956), this source is likely to be the afterglow to GRB 141026A.  In
comparison with 2MASS, we obtain the following detections and upper limit
(3-sigma):

  r     21.74 +/- 0.07
  i     21.54 +/- 0.06
  z  >  20.5

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

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


GRB_name: GRB141004A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16963
SUBJECT: GRB 141004A: Continued RATIR Late Time Optical and NIR Observations
DATE:    14/10/26 19:23:33 GMT
FROM:    Owen Littlejohns at Az State U  <olittlej@asu.edu>

Owen Littlejohns (ASU), Nat Butler (ASU), Alan M. Watson (UNAM),
Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer
(UNAM), Chris Klein (UCB), Ori Fox (UCB), J. Xavier Prochaska
(UCSC), Josh Bloom (UCB), Antonino Cucchiara (ORAU/GSFC), Eleonora
Troja (GSFC), Enrico Ramirez-Ruiz (UCSC), JosÃ© A. de Diego (UNAM),
Leonid Georgiev (UNAM), JesÃºs GonzÃ¡lez (UNAM), Carlos RomÃ¡n-ZÃºÃ±iga
(UNAM), Neil Gehrels (GSFC), and Harvey Moseley (GSFC) report:

We again observed the field of GRB 141004A (D'Elia, et al., GCN 16878)
with the Reionization and Transients Infrared Camera (RATIR;
www.ratir.org) on the 1.5m Harold Johnson Telescope at the Observatorio
AstronÃ³mico Nacional on Sierra San Pedro MÃ¡rtir from 2014/10 26.26 to
2014/10 26.52 UTC (21.27 to 21.55 days after the BAT trigger),
obtaining a total of 4.98 hours exposure in the r, i and z bands.

We continue to detect the source reported in previous epochs of RATIR
observations (Littlejohns, et al., GCN 16937, Littlejohns, et al., GCN
16887), with the following detections and upper limit:

  r     23.94 +/- 0.20
  i     23.38 +/- 0.15
  z     > 20.97

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB. These magnitudes are broadly
consistent with our previous epoch of observations (Littlejohns, et al.,
GCN 16937). Further observations are planned.

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


GRB_name: GRB141026A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16964
SUBJECT: GRB 141026A: Swift/UVOT Upper Limits
DATE:    14/10/26 21:57:26 GMT
FROM:    Lea Hagen at PSU  <lea.zernow.hagen@gmail.com>

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

The Swift/UVOT began settled observations of the field of GRB 141026A
166 s after the BAT trigger (Hagen et al., GCN Circ. 16950).  No optical
afterglow consistent with the XRT position (Beardmore et al. GCN Circ. 16956)
or the likely optical afterglow (Littlejohns et al. GCN Circ. 16952, Varela
et al. GCN Circ. 16953, Gorosabel et al. GCN Circ. 16954, Perley et al. GCN
Circ. 16955, Butler et al. GCN Circ. 16962) 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 (fc)         165          208           83         >19.98
white             3462         5667          688         >21.45
v                  144         5962          290         >19.34
b                 3826         5463          393         >20.48
u                 3621         5258          393         >20.15
uvw1              4852         5052          196         >19.61
uvm2              4647         4847          196         >19.58
uvw2              4237         5873          393         >20.26

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


GRB_name: GRB141026A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16965
SUBJECT: GRB 141026A: Continued RATIR Optical and NIR Observations
DATE:    14/10/27 16:56:57 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB),
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara
(ORAU/GSFC), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), JosÃ© A. de Diego (UNAM), Leonid Georgiev (UNAM), JesÃºs
GonzÃ¡lez (UNAM), Carlos RomÃ¡n-ZÃºÃ±iga (UNAM), Neil Gehrels (GSFC), and
Harvey Moseley (GSFC) report:

We observed the field of GRB 141026A (Hagen, et al., GCN 16950)) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio AstronÃ³mico Nacional on
Sierra San Pedro MÃ¡rtir from 2014/10 27.13 to 2014/10 27.53 UTC (24.48 to
34.08 hours after the BAT trigger), obtaining a total of 4.64 hours
exposure in the r, i, and z bands.

The optical afterlow (Littlejohns et al., GCN 16952; also Perley et al.,
GCN 16955, Varela et al., GCN 16953, Gorosabel et al., GCN 16954, Butler,
et al., GCN 16962) continues to fade.  In comparison with 2MASS, we obtain
the following detections and upper limit (3-sigma):

  r     22.94 +/- 0.16
  i     23.16 +/- 0.22
  z  >  20.1

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.  The source appears to have faded
roughly as t^(-0.5) since our last epoch (GCN 16962).

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


GRB_name: GRB141026A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16966
SUBJECT: GRB 141026A: SAO RAS Zeiss-1000 observations
DATE:    14/10/27 18:37:38 GMT
FROM:    Vladimir Sokolov at SAO RAS  <sokolov@sao.ru>

A. S. Moskvitin, V. N. Komarova, T. N. Sokolova (SAO RAS) report
on behalf of the GRB follow-up team:

We observed the field of GRB 141026A (Hagen et al., GCN 16950)
with the SAO RAS 1-m telescope Zeiss-1000 at the October 26/27 night.
The observations were started at 20:09:49 UT (in 17.55 hours
after the trigger), ended at 03:32:34. We obtained 61 x 300 sec.
images in the Rc filter.

The object mentioned by Littlejohns et al. (GCN 16592, GCN 16963),
Varela et al. (GCN 16953), Gorosabel et al. (GCN 16954),
Perley et al. (GCN 16955), Butler et al. (GCN 16962, GCN 16965)
is clearly detected in the stacked image.
The magnitude of OT is R = 22.1 +/- 0.1 (in Vega system, not corrected
for the Milky Way extinction). The photometry is based on the nearby
USNO-B1 stars.

[GCN OPS NOTE(27oct14):  Per author's request, the name of the GRB
was corrected in the Subject-line:  (13-->14).]


GRB_name: GRB141026A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16967
SUBJECT: GRB 141026A: Skynet PROMPT-CTIO/Yerkes-41 Observations
DATE:    14/10/27 20:26:34 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, J. Haislip, D. Reichart, V. Hoette, K. Cudworth, D. Harper, 
R. Kron, T. Linder, R. Russell, E. Struble, A. Aji, R. Beauchemin, T. 
Berger, A. Dow, A. Foster, N. Frank, M. Hinckle, K. Ivarsen, A. 
LaCluyze, M. Maples, J. Moore, M. Nysewander, C. Salemi, L. Zbinden, and 
J. A. Crain report:

Skynet observed the Swift BAT/XRT localization of GRB 141026A (Hagen et 
al., GCN 16950, Swift trigger=616502) with one 24" telescope (PROMPT 8; 
I band) and four 16" telescopes (PROMPT 3,1,4,5; BVRI bands) of the 
PROMPT array at CTIO, Chile, and with the 41" telescope of Yerkes 
Observatory in Wisconsin, USA (g'r'i' bands).
Starting at 2014-10-26 02:38:30 UT and continuing until 03:03 UT 
(t=1.5-26m post-trigger), Skynet took a total of 89 exposures ranging 
from 10s-160s each. We stacked subsets of these images to maximize the 
S/N ratio, and detected no optical source in any band at the OT position 
first reported by RATIR (Littlejohns et al., GCN 16952), and confirmed 
in later notices.  Our 3-sigma limiting magnitudes are:

==================================
tmid  scope   expos  fil  limit
==================================
10m  PROMPT3  4x80s   B   >19.9
20m  PROMPT1  4x160s  V   >20.4
19m  PROMPT4  3x160s  R   >19.8
17m  PROMPT5  4x80s   I   >19.9
               4X160s
17m  PROMPT8 12x80s   I   >20.0
63m  Yerkes   1x80s   g'  >21.2
               2x160s
60m  Yerkes   2x80s   r'  >20.9
               1x160s
66m  Yerkes   1x80s   i'  >20.5
               1x160s
==================================

BVRI magnitudes are in the Vega System, and g'r'i' magnitudes are in the 
AB system, calibrated to 4 APASS stars in the field.  Magnitudes have 
not been corrected for line-of-sight Milky Way dust extinction, with 
expected E(B-V)=0.16 (Schlafly & Finkbeiner 2011).

No further Skynet observations are scheduled.


GRB_name: GRB141026A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16968
SUBJECT: GRB 141026A: GTC spectroscopy
DATE:    14/10/28 16:59:55 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CISC, DARK/NBI), C.C. Thoene (IAA-CSIC),
N.R. Tanvir (U. Leicester), J. Gorosabel (UPV, IAA-CSIC), 
J. Fynbo (DARK/NBI), G. Lombardi (GTC), D. Reverte-Paya (GTC), 
and D. Perez (GTC) report:

We observed the afterglow of GRB 141026A (Hagen et al. GCN 16950,
Perley GCN 16951, Littlejohns et al. GCN 16952, Varela et al. GCN 16953,
Gorosabel et al. GCN 16954, Perley et al. GCN 16955, Beardmore et al.
GCN 16956, Butler et al. GCN 16962,Moskvitin et al. GCN 16966) with
OSIRIS at the 10.4m Gran Telescopio Canarias. Observations consisted of
z-band imaging, and spectroscopy using the R1000R grism (covering from
5100 to 10000 A with a resolution of ~1000). The spectroscopic observations
were delayed due to bad weather and had a mean epoch of 6:12 UT (3.59 
hours after the burst), and consisted of 2x900s exposures. Conditions were 
not optimal, as the airmass at that time was ~1.8 and most of the observation
was performed during twilight.

The spectrum shows a low S/N continuum, which is however, visible
between 5100 and 9500 A. Some absorption features seem to be present,
and in particular we identify a broad feature at 5300 A, with an observed
equivalent width of ~30 A. This could correspond to a weak Ly-alpha
(log(N_H/cm^-2) ~< 20) absorption at z=3.35. However, no other features
corresponding to that same redshift are seen, which is not unexpected for
a low density line of sight that would correspond to such a Ly-alpha feature
and a low S/N spectrum. Further absorptions could correspond to intervening
MgII absorbers.

This redshift solution is supported by the photometric drop seen by GROND
in the g-band (Varela et al. GCN 16953), which would correspond to a similar
photometric redshift.


GRB_name: GRB141028A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16969
SUBJECT: GRB 141028A: Fermi-LAT detection
DATE:    14/10/28 17:34:43 GMT
FROM:    Elisabetta Bissaldi at U.Innsbruk/IAPP  <Elisabetta.Bissaldi@uibk.ac.at>

E. Bissaldi (University & INFN Trieste), J. L. Racusin (NASA/GSFC),
F. Longo (University & INFN Trieste), D. Kocevski (NASA/GSFC),
G. Vianello (Stanford Univ.) and M. Arimoto (Tokyo Tech)
report on behalf of the Fermi-LAT team:

At 10:54:46.78 on October 28, 2014, Fermi-LAT detected high-energy
emission from GRB 141028A, which was also detected by Fermi-GBM
(trigger 436186489/141028455) and initiated an autonomous repoint
of the spacecraft.

The best LAT on-ground location is found to be

RA, Dec  322.70, -0.28 (J2000)

with an error radius of 0.4 deg (90% containment, statistical error only).
This was 25 deg from the LAT boresight at the time of the trigger.
An improved position may be released when additional data is
downlinked from the spacecraft.

The data from the Fermi-LAT show a significant increase in the event
rate at a position consistent with the GBM localization.
More than 20 photons above 100 MeV are observed from trigger
time T0 up to T0+600 s, when the position of the burst moved
out of the LAT FoV.
The highest-energy photon is a 3.9 GeV event which is observed
160 seconds after the GBM trigger.

A Swift ToO has been approved for this burst.

The Fermi-LAT point of contact for this burst is
Makoto Arimoto (arimoto@hp.phys.titech.ac.jp).

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


GRB_name: GRB141026A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16970
SUBJECT: GRB 141026A: Continued RATIR Optical and NIR Observations
DATE:    14/10/28 17:48:18 GMT
FROM:    Owen Littlejohns at Az State U  <olittlej@asu.edu>

Owen Littlejohns (ASU), Nat Butler (ASU), Alan M. Watson (UNAM),
Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer
(UNAM), Chris Klein (UCB), Ori Fox (UCB), J. Xavier Prochaska (UCSC),
Josh Bloom (UCB), Antonino Cucchiara (ORAU/GSFC), Eleonora Troja
(GSFC), Enrico Ramirez-Ruiz (UCSC), JosÃ© A. de Diego (UNAM), Leonid
Georgiev (UNAM), JesÃºs GonzÃ¡lez (UNAM), Carlos RomÃ¡n-ZÃºÃ±iga (UNAM),
Neil Gehrels (GSFC), and Harvey Moseley (GSFC) report:

We again observed the field of GRB 141026A (Hagen, et al., GCN 16950)
with the Reionization and Transients Infrared Camera (RATIR; www.ratir.org)
on the 1.5m Harold Johnson Telescope at the Observatorio AstronÃ³mico
Nacional on Sierra San Pedro MÃ¡rtir from 2014/10 28.13 to 2014/10
28.19 UTC (48.58 to 49.84 hours after the BAT trigger), obtaining a
total of 1.07 hours exposure in the r, i and z bands.

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

  r     > 23.54
  i     > 23.31
  z     > 19.82

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB. In comparison to previous epochs
of RATIR observations (Butler, et al., GCN 16965; Littlejohns, et al.,
GCN 16962), the GRB has continued to fade. The r band upper limit
indicates a power-law decay between this and the previous epoch of RATIR
observations with a minimum approximate index of t^(-0.9). This is
steeper than that reported in Butler, et al. (GCN 16965).

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


GRB_name: GRB141028A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16971
SUBJECT: GRB 141028A: Fermi GBM detection
DATE:    14/10/28 19:00:19 GMT
FROM:    Oliver Roberts at UCD/Fermi  <oliver.roberts@ucd.ie>

O.J. Roberts (UCD) reports on behalf of the Fermi GBM Team:

"At 10:54:46.78 UT on 28 October 2014, the Fermi Gamma-Ray
Burst Monitor triggered and located GRB 141028A
(trigger 436186489 / 141028455), which was also detected by
the LAT (Bissaldi et al. 2014, GCN 16969). The GBM on-ground
location, using the Fermi GBM trigger data, is consistent with
the LAT location.

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 = 316.32, DEC = +1.67, with an uncertainty
of 1.0 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).

The angle from the Fermi LAT boresight is about 19 degrees.

The GBM light curve consists of a single episode with a duration
(T90) of about 31.5 s (50-300 keV). The time-averaged spectrum
from T0+0s to T0+31.7s is well fit by a Band function with
Epeak = 249.9 (+/-12.6) keV, alpha = -0.71 +/- 0.03 , and
beta = -1.93 (+/-0.03).

The event fluence (10-1000 keV) in this time interval is
(3.478 +/- 0.009)E-05 erg/cm^2. The 1-sec peak photon flux
measured starting from T0+12.6 s in the 10-1000 keV band
is 17.3 +/- 0.3 ph/s/cm^2.

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


GRB_name: GRB141028A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16972
SUBJECT: GRB 141028A: MASTER OT candidate detection
DATE:    14/10/28 19:35:30 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

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

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

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


MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in 
Kislovodsk was pointed to the  GRB141028A (GCN 16969, Bissaldi) in  survey mode.

MASTER-Kislovodsk auto-detection system discovered OT source at (RA, Dec) 
= 21h 30m 24.51s -00d 13m 52.3s on 2014-10-28.76451 UT.
The OT unfiltered magnitude is 18.9m (limit 19.9m).

The OT is seen in 12 images. There is no minor planet at this place.

We have reference image without OT on 2014-07-22.97505 UT with unfiltered 
magnitude limit 19.7m.

Spectral observations are required.

The discovery and reference images are available at:
http://master.sai.msu.ru/static/OT/213024.51-001352.3.png


This message may be cited.


GRB_name: GRB141028A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16973
SUBJECT: GRB 141028A Tiled Swift observations
DATE:    14/10/28 19:48:52 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a series of observations, tiled on the sky, of the
Fermi/LAT GRB 141028A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00030

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

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

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


GRB_name: GRB141026A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16974
SUBJECT: GRB 141026A: IRAM 30m millimetre observations
DATE:    14/10/28 20:26:53 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

A. J. Castro-Tirado, J. C. Tello, J. Gorosabel (IAA-CSIC Granada), C.
Kramer, I. Hermelo, G. Paubert, A. Sievers (IRAM Granada) and  J. G.
Staguhn (NASA/GSFC Greenbelt),on behalf of a larger collaboration, report:

Following the detection of GRB 141026A by Swift (Hagen et al. GCNC
16950), observations with the IRAM 30m antenna (+GISMO) at Pico Veleta
(Spain) were triggered on 26-27 Oct. At the position of the optical
afterglow (Littlejohns et al. GCNC 16952, Varela et al. GCNC 16953,
Gorosabel et al. GCNC 16954), we detect no mm afterglow (at 2 mm) down to
a preliminary flux density of 1.2 mJy (3 sigma) on Oct 26, 14:30 UT (mid
time). We acknowledge excellent assistance from the IRAM observers.


GRB_name: GRB141028A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16975
SUBJECT: IPN triangulation of GRB 141028A
DATE:    14/10/28 21:30:37 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@ssl.berkeley.edu>

K. Hurley, on behalf of the IPN,

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

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

GRB 141028A (Bissaldi et al. GCN 16969, Roberts et al. GCN 16971) has
also been observed by MESSENGER, so far.  We have triangulated it to a preliminary,
3 sigma annulus, centered at RA, Dec = 16.520, +5.123 degrees, with radius
R=54.469 +/- 0.200 degrees.  This annulus intersects the LAT error circle
at two points:

 RA  Dec
     322.487 deg -0.619 deg
     322.416 deg        +0.002 deg

forming an error box whose area is approximately 0.03 degrees.
This triangulation may be improved. 

A map has been posted at ssl.berkeley.edu/ipn3/141028A


GRB_name: GRB141020A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16976
SUBJECT: GRB 141020A: Continued Mondy Observations, optical upper limit
DATE:    14/10/29 00:06:16 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of the Swift GRB 141020A  (Cenko et al., GCN 
16928) with with AZT-33IK telescope of Sayan observatory (Mondy). We 
obtained several images on Oct. 23 starting on (UT) 14:25:05.  At the 
position of optical afterglow (Cenko et al., GCN 16928; Kuin et al., GCN 
16932; Mazaeva et al., GCN 16943) we do not detect any object down to 
R=23.0. Preliminary photometry is following:

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

2014-10-23  14:25:05  3.3309     R     80*120  n/d  23.0

The photometry is based on SDSS stars reported in GCN 16943.


GRB_name: GRB141028A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16977
SUBJECT: GRB 141028A: GROND Afterglow confirmation (MASTER source)
DATE:    14/10/29 02:03:03 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

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

We observed the field of GRB 141028A (Fermi trigger 436186489; LAT
detection: Bissaldi et al., GCN #16969; GBM Detection: Roberts; GCN
#16971) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La Silla
Observatory (Chile).

Observations started at 23:57 UT on October 28th, approximately 13 hours
after the GRB trigger. They were performed at an airmass of 1.2 and seeing
of 1".4.

At the position of the MASTER candidate afterglow (Gorbovskoy, GCN #16972)
we detect a bright source at

RA (J2000) = 322.60226 = 21:30:24.54
DEC (J2000) = -0.231314 = -00:13:52.7

with an error of 0".5.

Based on images with an exposure time of 1500 s in the optical and 1200 s
in the NIR, centered at 0.55305 days after the trigger, we estimate
preliminary magnitudes and limits (all in AB system) for this source of:

g' = 20.76 +/- 0.02 mag
r' = 19.93 +/- 0.01 mag
i' = 19.70 +/- 0.02 mag
z' = 19.49 +/- 0.02 mag
J = 19.24 +/- 0.11 mag
H = 18.94 +/- 0.08 mag
K > 18.3 mag

Compared to the MASTER detection, the source has faded significantly. We
also detect a fading by 0.1 +/- 0.03 mag over the time span of an hour.
Furthermore, the SED is adequately described by a power-law of slope beta
= 1.1, with a possible g'-band dropout, which may point to a redshift of
around 3 (which would make this a luminous afterglow).

At the position of the XRT source reported in the GRB_COUNTERPART POSITION
NOTICE (Source 3 at http://www.swift.ac.uk/xrt_products/TILED_GRB00030/),
we detect no source down to limiting magnitudes of:

g' > 24.5 mag
r' > 24.4 mag
i' > 23.7 mag
z' > 23.4 mag
J > 20.9 mag
H > 20.6 mag
K > 18.3 mag

We therefore deem it likely the MASTER source represents the afterglow of
GRB 141028A.

Given magnitudes are calibrated against SDSS field stars (g'r'i'z')
and 2MASS field stars (JHK) and are not corrected for the expected
Galactic foreground extinction corresponding to a reddening of E_(B-
V) = 0.05 mag in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB141028A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16978
SUBJECT: GRB 141028A: Swift/XRT detection of the X-ray afterglow
DATE:    14/10/29 02:14:36 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@swift.psu.edu>

J. A. Kennea (PSU), J. L. Racusin (NASA/GSFC) and C. Pagani (UL) report on 
behalf of the Swift Team:

Swift-XRT has observed the error circle of the Fermi/LAT GRB 141028A in a 
series of observations tiled on the sky. The total exposure time is 2.0 ks 
spread over 7 fields; the maximum exposure within the sky observed was 766 
s. The observations started 31.0 ks after the Fermi/LAT trigger. Within 
these data we detect a bright, uncatalogued X-ray source at RA, Dec= 
322.60078, -0.23116 which is equivalent to:

RA (J2000) = 21h 30m 24.19s
Dec (J2000) = -00d 13' 52.2"

with an uncertainty of 5.8 arcsec (radius, 90% confidence). The exposure 
at this location was 277 s. We note that this source is 4.8 arcsec from 
the position of the candidate MASTER afterglow position (GCN #16972) which 
has been confirmed to be fading by GROND (GCN #16977), and does not match 
any previously catalogued source. The source is significantly brighter 
than the RASS limit and therefore we suggest that this is the X-ray 
afterglow of GRB 141028A. More observations will be required to determine 
if the source is fading in X-rays.

The results of the automatic processing for this source are available at 
http://www.swift.ac.uk/xrt_products/TILED_GRB00030/index_4.php This 
circular is an official product of the Swift-XRT team.


GRB_name: GRB141028A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16979
SUBJECT: GRB 141028A: Swift/UVOT Detection
DATE:    14/10/29 03:58:53 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU) and C. Pagani (UL)  report on behalf of the
Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 141028A
31037 s after the LAT trigger (Bissaldi et al., GCN Circ. 16969).
We detect an optical afterglow consistent with the afterglow reported by
MASTER (Gorbovsky et a., GCN, Circ 16972), GROND (Graham et al., GCN Circ.
16977) and the XRT (Kennea, et al., GCN Circ 16978).

The preliminary UVOT position is:
   RA  (J2000) =  21:30:24.54 = 322.60226 (deg.)
   Dec (J2000) = -00:13:52.4  =  -0.23122 (deg.)
with an estimated uncertainty of 0.4 arc sec. (radius, 90% confidence). This is
consistent with the GROND and MASTER positions.

Preliminary detection using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial exposure is:

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

u                31037        37759          233         19.14+-0.19

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.05 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB141028A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16980
SUBJECT: GRB 141028A: RATIR Optical and NIR Observations
DATE:    14/10/29 04:12:02 GMT
FROM:    Eleonora Troja at GSFC  <eleonora.troja@nasa.gov>

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

We observed the field of the Fermi/LAT GRB 141028A (Bissaldi et al., GCN 
16969, Roberts et al.
GCN 16971) with the Reionization and Transients Infrared Camera (RATIR; 
www.ratir.org <http://www.ratir.org/>) on the
1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional 
on Sierra San Pedro
Mrtir from 2014/10 29.08 to 2014/10 29.13 UTC  (from 13.62 to 14.82 
hours after the
Fermi-GBM trigger),  obtaining a total of 1.07 hours exposure in the r, 
i and z bands.

At the position of the XRT and optical counterparts (Kennea et al., GCN 
16978, Gorbovskoy
et al. GCN 16972,  Graham et al. GCN 16977), in comparison with the SDSS 
DR9, we
obtain the following detections:

   r 20.09 +/- 0.02
   i 19.85 +/- 0.02
   z 19.50 +/- 0.10

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.

[GCN OPS NOTE(29oct14)" Per author's request, the Subject-line was
corrected from "29A" to "28A".]


GRB_name: GRB141029A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16981
SUBJECT: GRB 141029A: MAXI/GSC detection
DATE:    14/10/29 06:00:25 GMT
FROM:    Motoko Suzuki at RIKEN  <motoko@crab.riken.jp>

S. Nakahira (JAXA), H. Negoro (Nihon U.),
S. Ueno, H. Tomida, 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, T. Yoshii, Y. Tachibana (Tokyo Tech),
A. Yoshida, T. Sakamoto, Y. Kawakubo, H. Ohtsuki (AGU),
H. Tsunemi, D. Uchida (Osaka U.),
M. Nakajima, K. Fukushima, T. Onodera, K. Suzuki, T. Namba, M. Fujita, F. Honda (Nihon U.),
Y. Ueda, M. Shidatsu, T. Kawamuro, T. Hori (Kyoto U.),
Y. Tsuboi, A. Kawagoe (Chuo U.),
M. Yamauchi, Y. Morooka, D. Itoh (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 04:32:09 UT .
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (69.413 deg, -16.481 deg) = (04 37 39, -16 28 51) (J2000) 
with a statistical 90% C.L. elliptical error region 
with long and short radii of 0.28 deg and 0.23 deg respectively. 
The roll angle of long axis from the north direction is 170.0 deg counterclockwise. 
There is an additional systematic uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 137 +- 24 mCrab
(4-10keV, 1 sigma error).
There was no significant excess flux in the previous transit at 02:59 UT.
with an upper limit of 20 mCrab.


GRB_name: GRB141028A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16982
SUBJECT: GRB141028A: Gemini-North redshift
DATE:    14/10/29 06:04:43 GMT
FROM:    Antonino Cucchiara at NASA/GSFC  <antonino.cucchiara@nasa.gov>

A. Cucchiara (NASA/GSFC) reports on behalf of a larger collaboration:

We obtained a spectrum of the afterglow (Kennea et al., GCN 16978, Gorbovskoy et al. 
GCN 16972,  Graham et al. GCN 16977, Siegel et al. GCN 16979) of the Fermi GRB 141028A 
(Bissaldi et al., GCN 16969, Roberts et al. GCN 16971) with the Gemini Multi-Object 
Spectrograph mounted on the 8 m Gemini-North telescope.  
Observations began at 05:07 UT on 2014 October 29 (~18. hr after the Fermi-GBM trigger) 
and cover the wavelength range from 3800-8200 A. We acquired 2x600s exposure
using the R400 grism.

We detect several absorption lines, including CrII2056,ZnII2056, FeII2260, FeII2344, 
FeII2586, FeII2600, MgII2706, MgII2803, and MgI 2853 at the common redshift of z=1.82.

We therefore suggest this to be the redshift of GRB 141028A.

We thank the Gemini-North staff for their terrific support, in particular 
A. Petric and A. Smith.


GRB_name: GRB141028A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16983
SUBJECT: GRB 141028A: VLT/X-shooter redshift of z=2.33
DATE:    14/10/29 08:15:25 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Xu (DARK/NBI), A. J. Levan (Univ. Warwick), J. P. U. Fynbo 
(DARK/NBI), N. R. Tanvir (Univ. Leicester), V. D'Elia (ASI/ASDC and 
INAF/Roma), D. Malesani (DARK/NBI), report on behalf of a larger 
collaboration:

We observed the optical afterglow (Gorbovskoy et al., GCN 16972; Graham 
et al., GCN 16977) of the Fermi/LAT GRB 141028A (Roberts, GCN 16971; 
Bissaldi et al., GCN 16969; Hurley et al., GCN 16975), using the 
X-shooter spectrograph at the ESO VLT. Observations started at 02:15 UT 
on 2014 Oct 29 (15.35 hr after the GRB), and consisted of 4x600 s 
exposures in each of the UVB, VIS, and NIR arms, covering the wavelength 
range 3000-25,000 AA.

We detect a variety of absorption features throughout the entire 
spectrum. In particular, a wide trough is visible centered around 4050 
AA, which we interpret as due to H I absorption at redshift z = 2.33. 
Identification of several metal features as due to, among others, Si II, 
C II, Fe II, C IV, Mg II, allows us to refine the value to z = 2.332.

We note the presence of a strong intervening system at z = 1.823 
(detected e.g. in C IV, Fe II, Mg II), and a weaker one at z = 2.09 (C 
IV). The former coincides with the system reported by Cucchiara et al. 
(GCN 16982).

We acknowledge excellent support from the ESO observing staff at 
Paranal, in particular Cedric Ledoux and Dimitri Gadotti.


GRB_name: GRB141029A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16984
SUBJECT: GRB 141029A Tiled Swift observations
DATE:    14/10/29 08:58:18 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a series of observations, tiled on the sky, of the
MAXI GRB 141029A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00031

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: GRB141028A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16985
SUBJECT: GRB 141028A: LCOGTN observations
DATE:    14/10/29 11:39:20 GMT
FROM:    Drejc Kopac at Math Phys U,Slovenia  <drejc.kopac@fmf.uni-lj.si>

D. Kopac (LJMU), J. Japelj (U. Ljubljana), C. Guidorzi (U. Ferrara), C. 
Mundell (LJMU), S. Dichiara (U. Ferrara), on behalf of a large 
collaboration report:

Using the Las Cumbres Observatory Global Telescope Network (LCOGTN) we 
observed the field of Fermi GRB 141028A (Bissaldi et al., GCN 16969; 
Roberts, GCN 16971). Optical observations in r' and i' filters (5 x 120s 
sequences) were obtained with 1-m telescopes in Sutherland (South 
Africa) and Cerro Tololo (Chile).

At the position of the MASTER telescope detection (Gorbovskoy et al., 
GCN 16972) we detect an un-catalogued source, consistent with GROND 
(Graham et al., 16977), UVOT (Siegel et al., GCN 16979) and RATIR 
detections (Troja et al., GCN 16980). Our preliminary photometry yields:

Mid time from   Total Exp   Filter   Magnitude
trigger (hr)    (s)
-------------------------------------------------
10.2            600         r'       19.4 +- 0.1
10.6            960         i'       19.3 +- 0.2

14.9            600         i'       19.9 +- 0.2
------------------------------------------------

The magnitudes are calibrated against nearby SDSS stars and are not 
corrected for the Galactic foreground extinction. Further observations 
with the LCOGTN are scheduled.


GRB_name: GRB141028A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16986
SUBJECT: GRB 141028A: Swift-XRT observations
DATE:    14/10/29 16:39:33 GMT
FROM:    Claudio Pagani at U of Leicester  <cp232@star.le.ac.uk>

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

We have analysed 3.0 ks of XRT data for the Fermi/LAT-detected burst:
GRB 141028A,  from 31.0 ks to 71.7 ks after the Fermi/LAT trigger. The
data are entirely in Photon Counting (PC) mode.  An X-ray source is
detected within the Fermi/LAT error circle. Using 348 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 = 322.60168, -0.23145 which is equivalent to:

RA (J2000): 21h 30m 24.40s
Dec(J2000): -00d 13' 53.2"

with an uncertainty of 4.0 arcsec (radius, 90% confidence). This
position is 367 arcsec from the Fermi/LAT position (Bissaldi et al. GCN
16969) and consistent with the positions of the optical counterpart
detected by MASTER (Gorbovskoy et al. GCN 16972), GROND (Graham et al.
GCN 16977) and UVOT (Siegel et al. GCN 16979).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=2.0 (+/-1.0).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.5 (+/-0.5). The
best-fitting absorption column is  1.8 (+2.2, -1.3) x 10^21 cm^-2, in
excess of the Galactic value of 4.1 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.0 x 10^-11 (5.0 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.8 (+2.2, -1.3) x 10^21 cm^-2
Galactic foreground: 4.1 x 10^20 cm^-2
Excess significance: 1.8 sigma
Photon index:      2.5 (+/-0.5)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020420.

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


GRB_name: GRB141029B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16987
SUBJECT: GRB 141029B: Fermi GBM detection
DATE:    14/10/29 17:29:02 GMT
FROM:    Oliver Roberts at UCD/Fermi  <oliver.roberts@ucd.ie>

O.J. Roberts (UCD) reports on behalf of the Fermi GBM Team:

"At 03:13:18.62  UT on the 29th October 2014, the Fermi Gamma-Ray
Burst Monitor triggered and located GRB 141029B
(trigger 436245201 / 141029134). 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 = 105.2, DEC = +25.1, with an uncertainty
of 1.0 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).

The angle from the Fermi LAT boresight is about 42 degrees.

The GBM light curve consists of a multiple episodes with a
duration (T90) of about 202.4 s (50-300 keV). The time-averaged
spectrum from T0-12.2 s to T0+190.5 s is well fit
by a power law function with an exponential high-energy cutoff.
The power law index is -1.36 +/- 0.03 and the cutoff energy,
parameterised as Epeak, is 191 +/-13 keV.

The event fluence (10-1000 keV) in this time interval is
(3.800 +/- 0.10)E-05 erg/cm^2. The 1-sec peak photon flux
measured starting from T0+78.3 s in the 10-1000 keV band
is 20.3 +/- 0.4 ph/s/cm^2.

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


GRB_name: GRB141029B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16988
SUBJECT: IPN triangulation of GRB 141029B
DATE:    14/10/29 23:05:18 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@ssl.berkeley.edu>

K. Hurley, on behalf of the IPN,

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

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

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

GRB 141029B (Roberts et al. GCN 16987) was also observed by INTEGRAL
(SPI-ACS) and MESSENGER, so far.  We have triangulated it to a preliminary,
3 sigma annulus, whose coordinates are RA (center), Dec (center), radius=
16.850, +5.225, 87.104 +/- 0.259 degrees.  This annulus intersects the
GBM 1 sigma (statistical-only) error circle at two points:

 RA(deg)  Dec(deg)
      105.735    +24.226
      105.874    +25.894

to form an error box whose area is approximately 0.56 sq. deg.
This triangulation may be improved.

A map has been posted at ssl.berkeley.edu/ipn3/141029B


GRB_name: GRB141028A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16989
SUBJECT: GRB 141028A: P60 Observations and Decay Index
DATE:    14/10/30 03:42:40 GMT
FROM:    S. Bradley Cenko at NASA/GSFC  <brad.cenko@nasa.gov>

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

We have imaged the location of the optical afterglow (Gorbovskoy et al., GCN 16972) of the Fermi GBM (Roberts et al., GCN 16971) and LAT (Bissaldi et al., GCN 16969) GRB141028A with the robotic Palomar 60 inch telescope.  Using nearby point sources from the Sloan Digital Sky Survey for reference, we measure the following r'-band magnitudes in our P60 images:

r' = 20.09 +/- 0.06 at dt = 15.8 hr after the burst
r' = 21.00 +/- 0.05 at dt = 39.3 hr after the burst

Based on these observations, we infer a power-law decay index of alpha ~ 0.9.


GRB_name: GRB141028A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16990
SUBJECT: GRB 141028A: Swift/UVOT followup observations
DATE:    14/10/30 13:21:38 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 141028A
31037 s after the LAT trigger (Bissaldi et al., GCN Circ. 16969).
A  fading source is detected in the initial exposures (Siegel and 
Pagani, GCN Circ., 16979) in the position given in that circular, also 
consistent with MASTER (Gorbovsky et a., GCN, Circ 16972), GROND (Graham 
et al., GCN Circ. 16977) and the XRT (Pagani, et al., GCN Circ 16986).

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

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

u                31037        31179          140         19.0+-0.18
u                69790        72355          2525        20.7+-0.13
u               105469       127705          4880        21.3+-0.18

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 0.05 in the direction of the 
burst (Schlegel et al. 1998).


GRB_name: GRB141028A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16991
SUBJECT: GRB 141028A: Continued RATIR Observations
DATE:    14/10/30 16:13:49 GMT
FROM:    Eleonora Troja at GSFC  <eleonora.troja@nasa.gov>

Eleonora Troja (GSFC), Nat Butler (ASU), Alan M. Watson (UNAM),
Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM),
Chris Klein (UCB), Ori Fox (UCB), J. Xavier Prochaska (UCSC), Josh Bloom 
(UCB),
Antonino Cucchiara (ORAU/GSFC), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), JosÃ© A. de Diego (UNAM), Leonid Georgiev (UNAM),
JesÃºs GonzÃ¡lez (UNAM), Carlos RomÃ¡n-ZÃºÃ±iga (UNAM), Neil Gehrels (GSFC),
and Harvey Moseley (GSFC) report:

We observed the field of GRB 141028A (Bissaldi, et al., GCN 16969) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio AstronÃ³mico Nacional on
Sierra San Pedro MÃ¡rtir from 2014/10 30.08 to 2014/10 30.31 UTC (39.07
to 44.46 hours after the GBM trigger), obtaining a total of 4.24 hours
exposure in the r, i, and z bands.

For a source within the enhanced XRT error circle (Pagani et al., GCN 
16986),
in comparison with the SDSS DR9, we obtain the following detections:

   r    21.19 Â± 0.04
   i    20.79 Â± 0.03
   z    20.74 Â± 0.24

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.  A comparison to our previous
observations (Troja et al., GCN 16980) shows that the afterglow faded 
with a
power-law decay index of alpha ~ 0.9 in all three filters, consistent 
with the decay
reported by Cenko & Perley (GCN 16989).

Further observations are planned.

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


GRB_name: GRB140509A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16992
SUBJECT: GRB 140509A: GROND afterglow detection
DATE:    14/10/30 16:26:37 GMT
FROM:    Patricia Schady at MPE/Swift  <pschady@mpe.mpg.de>

P. Schady (MPE Garching), A. Nicuesa Guelbenzu (TLS Tautenburg)  and J. Greiner (MPE Garching) 
report on behalf of the GROND team:

We observed the field of GRB 140509A (Swift trigger 598497; Page et al., GCN #16230) 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 10:07 UT on 09 May 2014, about 8 hours after the GRB trigger. They were performed at high airmass and a mean seeing of 1.4".

Using the first ~8 minutes of data with a midtime of 10.18UT after the trigger, we detect a source consistent with the UVOT position (Marshall et al., GCN #16241) with the following AB magnitudes:

g = 21.6 +/- 0.2
r' = 21.1 +/- 0.1 
i' = 20.9 +/- 0.1
z' = 20.7 +/- 0.1
J = 20.4 +/- 0.4
H = 20.1 +/- 0.4
K > 20.0

In a later epoch of observations taken on September 24th the source is no longer detected in any of the optical or NIR filters down to the following AB 3sigma limits:

g > 25.8
r > 25.3
i > 24.7
z > 24.3
J > 22.1
H > 21.6
K > 20.7

thus confirming that the source detections in our initial observations corresponded to the GRB optical afterglow and not to a potential host. 

All given magnitudes are calibrated against GROND zero points in the optical, and against 2MASS field stars in the NIR, and are not corrected for the expected Galactic foreground extinction corresponding to a reddening of E_(B-V)=0.02 mag in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB141028A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16993
SUBJECT: GRB 141028A: SAO RAS Zeiss-1000 photometry
DATE:    14/10/30 17:32:39 GMT
FROM:    Vladimir Sokolov at SAO RAS  <sokolov@sao.ru>

A.S. Moskvitin, V.N. Komarova, T.N. Sokolova and O.I. Spiridonova
SAO RAS) report on behalf of the GRB follow-up team:

We observed the field of GRB 141028A (Bissaldi et al., GCN 16969)
with the SAO RAS 1-m telescope Zeiss-1000 on October, 29. The observations
were started at 18:09:57 UT, ended at 19:40:42. We obtained 14 x 300 sec.
images in the Rc filter.

The OT discovered by the MASTER team (Gorbovskoy et al., GCN 16972)
and observed by numerous telescopes is clearly detected in our stacked
frame. The magnitude of OT is R = 20.6 +/- 0.1 in 8 hours since the Fermi
trigger (in Vega system, not corrected for the Milky Way extinction). The
photometry is based on the nearby USNO-B1 stars and checked with the other
catalogues.

On the occasion of the twenty-fifth anniversary of the Zeiss-1000 telescope
we would like to thank our colleagues S.V. Drabek, V.V. Komarov,
V.S. Shergin and V.V. Vlasyuk who have modernized the telescope control
system and provided its reliable operation.


GRB_name: GRB141029A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16994
SUBJECT: GRB 141029A: Nanshan optical upper limit
DATE:    14/10/30 19:08:31 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

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

We observed the field of the three X-ray afterglow candidates (see
http://www.swift.ac.uk/xrt_products/TILED_GRB00031/) of GRB 141029A
detected by MAXI/GSC (Nakahira et al., GCN16981), using the 1m
telescope located at Nanshan, Xinjiang, China. We obtained 2x300s and
1x600s R-band images, starting at 19:37 UT on 2014-10-29 (i.e., 15.09
hr after the trigger).

As reported, the X-ray source 1 (S1) and source 2 (S2) have catalogued
optical counterparts already, and the X-ray source 3 (S3) located at
R.A. = 04:37:20.17, Dec. = -16:08:09.3  (with Error Radius=8.8â€²â€²)
doesn't have a catalogued optical counterpart. However, no optical
source is detected at the S3 position in the Nanshan images, down to a
limiting magnitude of R=20.5 mag.


GRB_name: GRB141031A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16995
SUBJECT: GRB 141031A: Swift detection of a burst
DATE:    14/10/31 07:33:33 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

B.P. Gompertz (U Leicester), J. R. Cummings (NASA/UMBC),
K. L. Page (U Leicester) and M. H. Siegel (PSU) report on behalf of
the Swift Team:

At 07:18:26 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 141031A (trigger=617110).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 128.599, -59.138 which is 
   RA(J2000) = 08h 34m 24s
   Dec(J2000) = -59d 08' 15"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed one peak with a 
duration of about 20 sec.  The peak count rate was ~1437 counts/sec 
(15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 07:20:05.5 UT, 98.9 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 128.60808, -59.16815 which is
equivalent to:
   RA(J2000)  = 08h 34m 25.94s
   Dec(J2000) = -59d 10' 05.3"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 109 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (2.17 x
10^21 cm^-2, Willingale et al. 2013), with an excess column of 2.4
(+2.45/-2.14) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 102 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers none of
the XRT error circle. The 8'x8' region for the list of sources generated
on-board covers 100% of the XRT error circle. The list of sources is typically
complete to about 18 mag. No correction has been made for the expected
extinction corresponding to E(B-V) of 0.17. 

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


GRB_name: GRB141031A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16996
SUBJECT: GRB 141031A: GROND detection of a possible optical afterglow candidate
DATE:    14/10/31 11:35:31 GMT
FROM:    Corentin Delvaux at MPE  <delvaux@mpe.mpg.de>

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

We observed the field of GRB 141031A (Swift trigger 617110; Gompertz et
al., GCN #16995) 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 the ESO La
Silla Observatory (Chile).

Observations started at 07:46 UT on 31 October 2014, 0.45 hrs after the
GRB trigger. They were performed at an average seeing of 1.3" and at an
average airmass of 1.33.

We found one single point source at the NW edge of the 2.1" Swift-XRT
error circle reported by Gompertz et al. (GCN #16995) at

RA (J2000) = 08h 34m 25.75s

DEC (J2000) = -59d 10' 05.0"

with an uncertainty of 0.3" in each coordinate.

Based on the first 8.8 min of total exposures in g'r'i'z' and 8.0 min in
JHK, we estimate preliminary magnitudes (all in AB system) of

g' = 22.7 +/- 0.1 mag,
r' = 21.7 +/- 0.1 mag,
i' = 21.5 +/- 0.1 mag,
z' = 21.5 +/- 0.1 mag,
J > 20.9 mag,
H > 20.3 mag, and
K > 18.7 mag.

At the moment we cannot confirm if the source is fading.

Given magnitudes are calibrated against GROND zeropoints as well as 2MASS
field stars and are not corrected for the expected Galactic foreground
extinction corresponding to a reddening of E_(B-V)=0.17 mag in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB141031A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16997
SUBJECT: GRB 141031A: Enhanced Swift-XRT position
DATE:    14/10/31 12:16:43 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Using 1789 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 141031A, 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 = 128.60838, -59.16828 which is equivalent
to:

RA (J2000): 08h 34m 26.01s
Dec (J2000): -59d 10' 05.8"

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

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

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


GRB_name: GRB141031B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16998
SUBJECT: GRB 141031B: Swift detection of a burst
DATE:    14/10/31 15:10:05 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

B.P. Gompertz (U Leicester), J. R. Cummings (NASA/UMBC),
V. D'Elia (ASDC), P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC),
H. A. Krimm (CRESST/GSFC/USRA), K. L. Page (U Leicester),
D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/PSU) and
M. H. Siegel (PSU) report on behalf of the Swift Team:

At 14:56:45 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 141031B (trigger=617149).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 356.932, +41.365 which is 
   RA(J2000) = 23h 47m 44s
   Dec(J2000) = +41d 21' 56"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 20 sec.  The peak count rate
was ~500 counts/sec (15-350 keV), at ~5 sec after the trigger. 

The XRT began observing the field at 14:58:42.5 UT, 117.5 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 356.9056, 41.3519 which
is equivalent to:
   RA(J2000)  = 23h 47m 37.33s
   Dec(J2000) = +41d 21' 07.0"
with an uncertainty of 2.6 arcseconds (radius, 90% containment). This
location is 85 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 1.22
x 10^21 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 119 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
BAT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.15. 

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


GRB_name: GRB141031B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  16999
SUBJECT: GRB 141031B: MASTER early optical observations
DATE:    14/10/31 15:23:47 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

V.Krushinsky, I.Zalozhnih,  A. Popov
Ural Federal University, Yekaterinburg, Kourovka

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

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



MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Tunka was pointed to the  GRB141031B 33 sec after notice time 
and 88 sec after trigger time at 2014-10-31 14:58:13 UT in two 
polarizations. On our first (20s exposure) set we haven't found optical 
transient  within SWIFT error-box (Gompertz et al GCN 16998).
The 5-sigma upper limit has been about 16.0 mag

MASTER II  robotic telescope located in Kislovodsk was pointed  to the 
GRB141031B 23 sec after notice time and 77 sec after trigger time at 
2014-10-31 14:58:03 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 15.5 mag.

The message may be cited.


GRB_name: GRB141031B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17000
SUBJECT: GRB 141031B: Nanshan optical upper limit
DATE:    14/10/31 16:33:01 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

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

We observed the field of GRB 141031B (Gompertz et al., GCN 16998),
using the 1m telescope located at Nanshan, Xinjiang, China. We
obtained 2x300s and 1x600s R-band images, starting at 16:02:08 UT on
2014-10-31 (i.e., 1.090 hr after the burst).

No optical source is detected at the XRT position (R.A.=23:47:37.24,
Dec.=+41:21:07.7, Err. Rad.=2.4"), down to a limiting magnitude of
R=20.6 mag.


GRB_name: GRB141031A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17001
SUBJECT: GRB 141031A: Fermi GBM detection
DATE:    14/10/31 16:44:12 GMT
FROM:    Oliver Roberts at UCD/Fermi  <oliver.roberts@ucd.ie>

O.J. Roberts (UCD) reports on behalf of the Fermi GBM Team:

"At 07:18:21.67 UT on the 31st of October 2014, the Fermi
Gamma-Ray Burst Monitor triggered and located GRB 141031A
(trigger 436432704 / 141031304), which was also detected by
Swift (Gompertz et al. 2014, GCN 16995). The GBM on-ground
location, using the Fermi GBM trigger data, is consistent with
the Swift location.

The angle from the Fermi LAT boresight is about 34 degrees.

The GBM light curve consists of a single peak with a duration
(T90) of about 19.4 s (50-300 keV). The time-averaged spectrum
from T0-6.1 s to T0+13.3 s is well fit by a power law function
with an exponential high-energy cutoff.  The power law index is
-1.09 +/- 0.06  and the cutoff energy, parameterized as Epeak,
is 410 +/- 66 keV.

A Band function fits the spectrum equally well with
Epeak = 221 (+/-57) keV, alpha = -0.92 +/- 0.12 , and
beta = -1.76 (+/-0.09).

The event fluence (10-1000 keV) in this time interval is
(5.7 +/- 0.2)E-06  erg/cm^2. The 1-sec peak photon flux
measured starting from T0+3.8 s in the 10-1000 keV band
is 2.7 +/- 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: GRB141031A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17002
SUBJECT: GRB 141031A: VLT/X-shooter optical observations
DATE:    14/10/31 18:46:44 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Xu (DARK/NBI), A. de Ugarte Postigo (IAA/CSIC and DARK/NBI), S. D. 
Vergani (CNRS/GEPI), A. J. Levan (Univ. Warwick), J. P. U. Fynbo 
(DARK/NBI), N. R. Tanvir (Univ. Leicester), B. Milvang-Jensen 
(DARK/NBI), D. Malesani (DARK/NBI), K. Wiersema (Univ. Leicester), 
report on behalf of a larger collaboration:


We observed the field of GRB 141031A (Gompertz et al., GCN 16995) using 
the VLT X-shooter spectrograph, using the robotic rapid response mode (RRM).

In a 15-s acquisition image, taken at 7:41:19 UT (22.8 min after the 
GRB1), we identify three objects consistent with, or in the close 
vicinity of, the currently available XRT error circle (1.4" error 
radius; Evans et al., GCN 16997 and http://www.swift.ac.uk/xrt_positions/).

Their coordinates are (all J2000):

A)
RA = 08:34:26.11
Dec = -59:10:04.2

B)
RA = 08:34:25.73
Dec = -59:10:04.8

C)
RA = 08:34:26.05
Dec = -59:10:04.9

Sources A and C are partially blended. Source B is the one detected by 
GROND (GCN 16996), looks extended in our data (under 0.6" seeing), and 
is now formally outside the latest XRT position (2.7"+-1.4" away). The 
limiting magnitude of the image is R ~ 21.7. A finding chart is 
available at http://www.astro.ku.dk/~malesani/GRB/141031A/finder_XS.jpg

A later image (30 s exposure) was taken 104.5 min after the GRB. Image 
subtraction reveals no obvious variation of any of the sources, despite 
the significant time difference between the two epochs (factor of 4.5 in 
time since GRB).

A spectrum was secured of source A, covering the wavelength range 
3000-25,000 AA. Several features are observed in absorption, including 
the Balmer series from Halpha to H15, and Ca H and K, at z = 0.0013. 
Such redshift is consistent with the Milky Way or the Local Group, 
though the corresponding velocity (390 km/s) is substantial for an 
origin in the MW disk.

Our slit did not cover, unfortunately, objects B and C. Further analysis 
is in progress, and we invite further monitoring of these object to 
single out variability.

We acknowldge excellent support from the observing staff in Paranal, in 
particular Juan Carlos Munoz-Mateos, Francisco Caceres, Rodrigo Romero, 
and Steffen Mieske.


GRB_name: GRB141004A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17003
SUBJECT: GRB 141004A: Continued Late Time RATIR Optical and NIR Observations
DATE:    14/10/31 18:59:43 GMT
FROM:    Owen Littlejohns at Az State U  <olittlej@asu.edu>

Owen Littlejohns (ASU), Nat Butler (ASU), Alan M. Watson (UNAM),
Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer
(UNAM), Chris Klein (UCB), Ori Fox (UCB), J. Xavier Prochaska (UCSC),
Josh Bloom (UCB), Antonino Cucchiara (ORAU/GSFC), Eleonora Troja
(GSFC), Enrico Ramirez-Ruiz (UCSC), JosÃ© A. de Diego (UNAM), Leonid
Georgiev (UNAM), JesÃºs GonzÃ¡lez (UNAM), Carlos RomÃ¡n-ZÃºÃ±iga (UNAM),
Neil Gehrels (GSFC), and Harvey Moseley (GSFC) report:

We again observed the field of GRB 141004A (D'Elia, et al., GCN 16878)
with the Reionization and Transients Infrared Camera (RATIR;
www.ratir.org) on the 1.5m Harold Johnson Telescope at the Observatorio
AstronÃ³mico Nacional on Sierra San Pedro MÃ¡rtir from 2014/10 31.31 to
2014/10 31.46 UTC (26.34 to 26.48 days after the BAT trigger), obtaining
a total of 2.84 hours exposure in the r, i and z bands.

We continue to detect the source reported from previous epochs of RATIR
observations (Littlejohns, et al., GCN 16963; GCN 16937; GCN 16887). We
obtain the following detections and upper limit (3 sigma):

  r     23.62 +/- 0.19
  i     23.17 +/- 0.15
  z     > 21.09

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB. In comparison to our previous
epochs of observations, the source appears to have brightened in the r
and i bands, consistent with an emerging supernova similar to SN 1998bw
(Schulze, et al., GCN 16936).

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


GRB_name: GRB141031A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17004
SUBJECT: GRB 141031A: Skynet PROMPT-CTIO Observations
DATE:    14/10/31 19:20:02 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, J. Haislip, D. Reichart, A. Aji, R. Beauchemin, T. Berger, 
A. Dow, A. Foster, N. Frank, M. Hinckle, K. Ivarsen, A. LaCluyze, M. 
Maples, J. Moore, M. Nysewander, C. Salemi, L. Zbinden, and J. A. Crain 
report:

Skynet observed the Swift BAT/XRT localization of GRB 141031A (Gompertz 
et al., GCN 16995, Swift trigger=617110) with one 24" telescope (PROMPT 
8; I band) and three 16" telescopes (PROMPT 3,4,5; B,R,I bands) of the 
PROMPT array at CTIO, Chile.
Starting at 2014-10-31 07:19:46 UT and continuing until 08:53 UT 
(t=79s-94m post-trigger), Skynet took a total of 196 exposures ranging 
from 10s-160s each. We stacked subsets of these images to maximize the 
S/N ratio, and detected no optical source in any band at the OT position 
reported by GROND (Tanga et al., GCN 16996).  Our 3-sigma limiting 
magnitudes are:

==================================
tmid  scope   expos  fil  limit
==================================
52m  PROMPT3 26x160s  B   >20.9
54m  PROMPT4 24x160s  R   >21.6
53m  PROMPT5 27x160s  I   >20.9
48m  PROMPT8 45x80s   I   >20.9
==================================

Limiting magnitudes are in the Vega System, calibrated to 6 APASS stars 
in the field.  Magnitudes have not been corrected for line-of-sight 
Milky Way dust extinction, with expected E(B-V)=0.15 (Schlafly & 
Finkbeiner 2011).

No further Skynet observations are scheduled.


GRB_name: GRB141031A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17005
SUBJECT: GRB 141031A: Swift-XRT refined Analysis
DATE:    14/10/31 19:33:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 8.0 ks of XRT data for GRB 141031A (Gompertz  et al.
GCN Circ. 16995),  from 102 s to 24.0 ks after the  BAT trigger. The
data comprise 847 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. 16997).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.06 (+/-0.05).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.43 (+0.12, -0.11). The
best-fitting absorption column is  2.44 (+0.64, -0.27) x 10^21 cm^-2,
consistent with the Galactic value of 2.2 x 10^21 cm^-2 (Willingale et
al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 5.2 x 10^-11 (6.0 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.44 (+0.64, -0.27) x 10^21 cm^-2
Galactic foreground: 2.2 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.43 (+0.12, -0.11)

If the light curve continues to decay with a power-law decay index of
1.06, the count rate at T+24 hours will be 4.0 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.1 x
10^-13 (2.4 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00617110.

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


GRB_name: GRB141031B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17006
SUBJECT: GRB 141031B: 1.23m CAHA I-band observations
DATE:    14/10/31 19:40:47 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC/UPV-EHU), S. Hellmich (DLR), S. Mottola (DLR),
report on behalf of a larger collaboration:

We observed the field of the GRB 141031B (Gompertz et al., GCN 16998) with
the 1.23m CAHA telescope in the I-band filter. Observations started on
Oct. 31.74693 UT (2.98 hours post burst). No object brighter than I~20.5
(Vega) is detected within the XRT error circle. Further observations are
ongoing.


GRB_name: GRB141031B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17007
SUBJECT: GRB 141031B: TShAO optical upper limit
DATE:    14/10/31 20:03:58 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI),  A. Khruslov (INASAN), A. Volnova (IKI), A. Pozanenko 
(IKI) report on behalf of larger GRB follow-up collaboration:

We observed the field of the GRB 141031B (Gompertz et al., GCN 16998) 
with  Zeiss-1000 (East) 1m telescope of Tien Shan Astronomical 
Observatory on Oct., 31  starting on (UT) 15:39:02, i.e. ~0.7 hours 
after burst trigger. We took several images in R-filter of 600 exposure. 
In the first image we do not detect any object brighter than R=21.5 in 
XRT error circle (Gompertz et al., GCN 16998).

Details of the photometry are following:

date        UT start   t-T0       Filter  Exp. UL (3 sigma)
                       (mid, days)          (s)
2014-10-31 15:39:02    0.03284    R       600  21.5


The photometry is based on  nearby SDSS DR9 stars.


GRB_name: GRB141031A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17008
SUBJECT: GRB 141031A: Swift/UVOT Upper Limits
DATE:    14/10/31 20:11:19 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (IAA-CSIC/UCL-MSSL) and B. P. Gompertz (U Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 141031A
102 s after the BAT trigger (Gompertz et al., GCN Circ. 16995).
No optical afterglow consistent with the possible optical position
(Tanga et al. GCN Circ. 16996) or enhanced XRT position 
(Evans et al. GCN Circ. 16997) is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

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

white_FC           102          252          147         >20.9
u_FC               315          565          246         >19.9
white              102        18038          967         >21.8
v                  646        13448          759         >20.0
b                  571        17791         1414         >21.4
u                  315        23978         1180         >20.7
w1                 696        23537         1396         >21.0
m2                 670         6964          529         >20.2
w2                 621        12030         1238         >21.0

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.17 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB141031B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17009
SUBJECT: GRB 141031B: Enhanced Swift-XRT position
DATE:    14/10/31 21:02:11 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 712 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 141031B, 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 = 356.90499, +41.35253 which is equivalent
to:

RA (J2000): 23h 47m 37.20s
Dec (J2000): +41d 21' 09.1"

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: GRB141031A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17010
SUBJECT: GRB 141031A, Swift-BAT refined analysis
DATE:    14/10/31 21:30:21 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

T. N. Ukwatta (LANL), S. D. Barthelmy (GSFC),  W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings, N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC)
(i.e. the Swift-BAT team):
  
Using the data set from T-250 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 141031A (trigger #617110)
(Gompertz, et al., GCN Circ. 16995).  The BAT ground-calculated position is
RA, Dec = 128.632, -59.160 deg which is
    RA(J2000)  =  08h 34m 31.6s
    Dec(J2000) = -59d 09' 36.8"
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 32%.
  
The mask-weighted light curve shows three widely separated peaks.  The first
is a single symmetric peak from about T-20 to T+20 seconds, the second is
another symmetric peak ~20 sec long at about T+800, and the third is two
overlapping peaks from about T+850 to T+920 seconds.  T90 (15-350 keV) is
about 920 +- 10 sec (estimated error including systematics).
  
The time-averaged spectrum from T-22 to T+20 sec is best fit by a simple
power-law model with a power law index of 1.21 +- 0.13.  The time-averaged
spectrum from T+770 to T+920 sec is also best fit by a simple power-law model
with a power law index of 1.75 +- 0.18.  The total fluence for both intervals
in the 15-150 keV band is 2.9 +- 0.5 x 10^-06 erg/cm2.  The 1-sec peak photon
flux measured from T+5.08 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/617110/BA/


GRB_name: GRB141031B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17011
SUBJECT: GRB 141031B: Swift-BAT refined analysis
DATE:    14/10/31 23:49:19 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@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 (GSFC/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):
  
Using the data set from T-240 to T+962 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 141031B (trigger #617149) (Gompertz, et al.,
GCN Circ. 16998).  The BAT ground-calculated position is
RA, Dec = 356.883, 41.355 deg which is
    RA(J2000)  =  23h 47m 31.9s
    Dec(J2000) = +41d 21' 19.1"
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
  
The mask-weighted light curve shows one weak FRED peak.  T90 (15-350 keV) is
16.0 +- 3.6 sec (estimated error including systematics).
  
The time-averaged spectrum from T+1.21 to T+18.21 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.36 +- 0.35.  The fluence in the 15-150 keV band is 2.5 +- 0.5 x 10^-07 erg/cm2.
The 1-sec peak photon flux measured from T+4.21 sec in the 15-150 keV band
is 0.3 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.
  
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/617149/BA/


GRB_name: GRB141031B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17012
SUBJECT: GRB 141031B: MITSuME Ishigakijima upper limits
DATE:    14/11/01 01:40:01 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

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

We observed the field of GRB 141031B (Gompertz et al., GCNC 16998)
with the optical three color (g', Rc and Ic) CCD camera attached
to the Murikabushi 1m telescope of Ishigakijima Astronomical
Observatory.

The observation started on  2014-10-31 15:02:03 (~5.3 min after the burst).
We did not find any new point source within the enhanced XRT circle
(Osborne et al., GCNC 17009) in all the three bands.

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

#T0+[day]  MID-UT    T-EXP[sec]   g'     Rc     Ic
-----------------------------------------------------
0.04563    16:02:27    6120.0   >22.6  >22.4  >21.3
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB141031B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17013
SUBJECT: GRB 141031B: NOT optical observations
DATE:    14/11/01 01:53:00 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

Daniele Malesani (DARK/NBI) and Vania Lorenzi (INAF/TNG) report on 
behalf of the CIBO collaboration:

We observed the field of GRB 141031B (Gompertz et al., GCN 16998) with 
the Nordic Optical Telescope (NOT) equipped with StanCam. Observations 
were carried out in the Johnson R (9x300 s) and SDSS z (6x300 s) filters 
under moderate weather conditions (1.5" seeing).

No objects are detected in either bands within the refined X-ray 
position (Goad et al., GCN 17009), down to limiting magnitudes of R = 
22.5 (Vega) and z = 21.5 (AB), with mean times 7.93 and 8.48 hr after 
the GRB (calibration against USNO B1 and SDSS, respectively).


GRB_name: GRB141031B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17014
SUBJECT: GRB 141031B: Bassano Bresciano Observatory upper limit
DATE:    14/11/01 07:20:56 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 141031B detected by SWIFT(trigger 617149)
with the robotic telescope of (IAU station 565) Bassano Bresciano 
Observatory, Italy (member of ISSP:Italian Supernovae Search Project)

The observations started 2.16 hour after the GRB trigger, at the end of twilight, 
with our schmidt telescope D=320/400 mm F/D=3.1.

Weather conditions were good.

We did not found any optical counterpart
in the error box of the XRTcandidate.
(B.P. Gompertz (U Leicester) et al, GCN 16998)

Start T0+      End T0+      Vlim
2.16 hour     4.48 hour      18

Magnitudes were estimated with the USNO-B1.0 cat. 
and are not corrected for galactic dust extinction.

The message may be cited.


GRB_name: GRB141031B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17015
SUBJECT: GRB 141031B: Swift-XRT refined Analysis
DATE:    14/11/01 09:10:31 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 12 ks of XRT data for GRB 141031B (Gompertz  et al.
GCN Circ. 16998),  from 126 s to 51.8 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Goad et al. (GCN Circ. 17009).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.84 (+0.09, -0.08).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.8 (+/-0.4). The
best-fitting absorption column is  5.5 (+2.5, -2.7) x 10^21 cm^-2, in
excess of the Galactic value of 1.2 x 10^21 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.6 x 10^-11 (6.8 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.5 (+2.5, -2.7) x 10^21 cm^-2
Galactic foreground: 1.2 x 10^21 cm^-2
Excess significance: 2.6 sigma
Photon index:      1.8 (+/-0.4)

If the light curve continues to decay with a power-law decay index of
0.84, the count rate at T+24 hours will be 1.5 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.9 x
10^-14 (1.0 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00617149.

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


GRB_name: GRB141029A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17016
SUBJECT: MAXI GRB 141029A is likely an X-ray flare from 1RXS J043657.1-161258
DATE:    14/11/01 10:09:44 GMT
FROM:    Satoshi Nakahira at JAXA/MAXI  <nakahira.satoshi@jaxa.jp>

S. Nakahira (JAXA), N. Kawai (Tokyo Tech), T. Sakamoto (AGU), K. Yamaoka (Nagoya U),$B!!(B
H. Negoro (Nihon U.), M. Serino (RIKEN), P. A. Evans (U. Leicester), K. L. Page (U Leicester)
on behalf of the MAXI team and the Swift-MAXI collaboration

The Swift ToO observation of GRB141029A (Nakahira et al., GCN16981)
was performed starting from 2014-10-29T09:00:37
with 4-point tiling to cover the MAXI error circle.

We found three X-ray sources in the MAXI error circle
as shown in the Swift observation summary page
http://www.swift.ac.uk/xrt_products/TILED_GRB00031/.
One of the sources ("source 1") showed suggestive fading between the
two tilings centered at 15500 s and 20700 s after the MAXI detection
with count rates of 2.7 +- 0.3 c/s and 1.7 +- 0.2 c/s respectively.
Assuming a power-law spectrum with photon index of 2.4 the X-ray flux
at the first Swift pointing is estimated as 6.8 x 10^-11 erg/cm2/s,
two order of magnitude fainter than 5.6 x 10^-9 erg/cm2/s at the MAXI detection.

The fading behavior was confirmed by additional Swift TOO observation
conducted from 2014-10-30T10:14:59 with a detected count rate of 0.27+-0.02 c/s.

This fading source matches a catalogued X-ray source 1RXS J043657.1-161258,
whose position in the ROSAT All-Sky Survey Bright Source Catalog is
9.1" away from the Swift position with a 3-sigma positional error of 40.1".
The source flux in the catalog corresponds to 9.3 x 10^-12 erg/s/cm2,
indicating that the fluxes in the present Swift observations were
in much elevated states.
The source was also reported to be variable (Fuhrmeister and Schmitt 2003).

Thus, we conclude that 1RXS J043657.1-161258 is the most likely source of the MAXI transient.

This optical counterpart of 1RXS J043657.1-161258 has been studied,
and found to be variable with with possible rotational period of P=0.3787d or P =2.74d
(Kiraga et al. 2012).

These characteristics of the source suggest that the X-ray transient
observed by MAXI was a strong flare from an active star system
such as RS CVn star, dMe star, or a cataclysmic variable.

Non-detection of an optical counterpart of source 3 reported by Xu et al. ( GCN16994)
further supports that this transient was not a gamma-ray burst.

We thank the Swift team for performing the observation.


GRB_name: GRB141031B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17017
SUBJECT: GRB 141031B: Swift/UVOT Upper Limits
DATE:    14/11/01 11:09:58 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (IAA-CSIC/UCL-MSSL) and B. P. Gompertz (U Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 141031B
120 s after the BAT trigger (Gompertz et al., GCN Circ. 16998).
No optical afterglow consistent with the XRT position
(Goad et al. GCN Circ. 17009)
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           120          270          147         >21.0
u_FC               278          528          246         >20.3
white              120         6181          580         >21.8
v                  608        11035         1317         >20.6
b                  534         5976          432         >20.9
u                  278         5771          659         >20.9
w1                 658        12348          620         >20.7
m2                 633        11940         1121         >20.9
w2                 584         6386          432         >20.5

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: GRB141031B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17018
SUBJECT: GRB 141031B: RATIR Optical and NIR Observation
DATE:    14/11/01 16:05:34 GMT
FROM:    Nat Butler at UC berkeley  <natxbutler@gmail.com>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB),
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara
(ORAU/GSFC), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), JosÃ© A. de Diego (UNAM), Leonid Georgiev (UNAM), JesÃºs
GonzÃ¡lez (UNAM), Carlos RomÃ¡n-ZÃºÃ±iga (UNAM), Neil Gehrels (GSFC), and
Harvey Moseley (GSFC) report:

We observed the field of GRB 141031B (Gompertz, et al., GCN 16998) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio AstronÃ³mico Nacional on
Sierra San Pedro MÃ¡rtir from 2014/11 1.10 to 2014/11 1.11 UTC (11.34 to
11.75 hours after the BAT trigger), obtaining a total of 0.36 hours
exposure in the r, i, and z bands.

For a source within the enhanced Swift-XRT error circle (Goad, et al., GCN
17009), in comparison with the SDSS DR9, we obtain the following upper
limits (3-sigma):

  r > 22.98
  i > 22.81
  z > 19.91

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

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


GRB_name: GRB141026A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17019
SUBJECT: GRB 141026A: VLA observations
DATE:    14/11/02 15:39:26 GMT
FROM:    Alessandra Corsi at Texas Tech U  <alessandra.corsi@ttu.edu>

A. Corsi (Texas Tech U.) reports on behalf of a larger collaboration:

We observed the location of GRB 141026A (Hagen et al., GCN 16950) with the 
Karl G. Jansky Very Large Array (VLA) in its C configuration. Observations were 
carried out in the frequency bands 18.7-24.9 GHz and 4.5-7.8 GHz. A provisional 
reduction shows marginal detections at 21.8 GHz (at about 1.1 d and 4.3 d after the 
burst), and a clearer detection at 6.2 GHz (at about 6 d after the burst), of a source 
consistent with the location of the GRB optical afterglow (Littlejohns et al. GCN 16952; 
Varela et al., GCN 16953; Gorosabel et al., GCN 16954; Perley et al. GCN 16955). 
We estimate preliminary fluxes for this source of: 

Mean epoch |  Freq. (GHz) | Flux (uJy) | map rms (uJy)
------------------------------
6.5 hr  | 21.8 | 11 | 11
------------------------------
1.1 d | 21.8 | 43 | 11
------------------------------
4.3 d | 21.8 | 31 | 8
------------------------------
6.0 d | 6.2 | 91 | 7
------------------------------


GRB_name: GRB141102A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17020
SUBJECT: GRB 141102A found in ground analysis of BAT data
DATE:    14/11/02 21:48:26 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

J. R. Cummings on behalf of the Swift science team:

A possibly short burst occurred at 12:51:40 UT (BAT trigger 617313).  No source was found
onboard.  Ground analysis shows a significant source at RA, Dec 208.614, -47.100 which is:

RA (J2000)     13h 54m 27.4s
Dec (J2000)    -47d 06' 00"

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

There were multiple peaks, at about T-0.2, T+0.4, T+1.7, and T+2.3. The latter two
were stronger than the first two and resembled them in shape, the third was the largest.
T90 is estimated as 2.5 +- 0.4 sec.

The spectrum from T-0.3 to T+2.7 seconds is best fit by a simple powerlaw function with
a photon index of 1.3 +- 0.5.  The fluence was 3.7 x 10 ^-7 ergs/cm^2.

A Swift TOO is not possible because the source is too close to the Sun for the next
39 days.


GRB_name: GRB141102A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17021
SUBJECT: GRB 141102A: Fermi GBM detection
DATE:    14/11/03 00:51:53 GMT
FROM:    Binbin Zhang at UAH  <binbin.zhang@uah.edu>

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

"At 12:51:39.26 UT on the 2nd of November 2014, the Fermi Gamma-Ray Burst Monitor
 triggered and located GRB 141102A (trigger 436625502 / 141102536), which was also 
detected by Swift (Cummings 2014, GCN 17020). The GBM on-ground location, using 
the Fermi GBM trigger data, is consistent with the Swift location. The trigger resulted in
 an Autonomous Repoint Request (ARR) that was accepted and the spacecraft slewed
 to the GBM in-flight location. The angle from the Fermi LAT boresight is about 57 degrees.

The GBM light curve consists of two main peaks with a total duration (T90) of about
 2.62 s (50â€“300 keV). The time-averaged spectrum from T0â€“0.064 s to T0+2.56 s is 
well fit by a power law function with an exponential high-energy cutoff. The power law 
index is â€“0.85 +/- 0.12 and the cutoff energy, parameterized as Epeak, is 770 +/- 243 keV.

The event fluence (10â€“1000 keV) in this time interval is (1.7 +/- 0.1)Eâ€“06 erg/cm^2. The
1-sec peak photon flux measured starting from T0+1.1 s in the 10â€“1000 keV band is 
5.0 +/- 0.2 ph/s/cm2.

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


GRB_name: GRB141102A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17022
SUBJECT: GRB 141102A: Fermi-LAT detection
DATE:    14/11/03 04:34:37 GMT
FROM:    Giacomo Vianello at SLAC  <giacomov@slac.stanford.edu>

G.Vianello (Stanford U.), D. Kocevski (NASA/GSFC),
V. Connaughton (UAH), M. Arimoto (Tokyo Tech), S. Guiriec (NASA/GSFC)

At 12:51:39.26 on November 2, 2014, Fermi-LAT detected faint high-energy
emission from the short GRB 141102A, which was also detected by Fermi-GBM
(Zhang et al., GCN 17021) and Swift/BAT (Cummings et al., GCN 17020)
and initiated an autonomous repoint of the spacecraft.  The high-energy emission
was detected during the ~300 s interval following the GBM trigger.

The best LAT on-ground location is found to be

(RA, Dec.) = 208.6, -47.7 deg

with an error radius of 0.6 deg (90% containment, statistical error
only), which is compatible
with the position measured by Swift/BAT (Cummings et al., GCN 17020).

Further follow up is encouraged.

The Fermi-LAT point of contact for this burst is
Makoto Arimoto (arimoto@hp.phys.titech.ac.jp).

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


GRB_name: GRB141022A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17023
SUBJECT: GRB 141022A: Skynet PROMPT-CTIO Observations
DATE:    14/11/03 13:24:59 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, J. Haislip, D. Reichart, A. Aji, R. Beauchemin, T. Berger, 
A. Dow, A. Foster, N. Frank, M. Hinckle, K. Ivarsen, A. LaCluyze, M. 
Maples, J. Moore, M. Nysewander, C. Salemi, L. Zbinden, and J. A. Crain 
report:

Skynet observed the Swift BAT/XRT localization of GRB 141022A (Vargas et 
al., GCN 16938, Swift trigger=616061) with one 24" telescope (PROMPT 8; 
I band) and two 16" telescopes (PROMPT 1,5; V,I bands) of the PROMPT 
array at CTIO, Chile.
Starting at 2014-10-22 01:29:40 UT and continuing until 02:50 UT 
(t=2m-83m post-trigger), Skynet took a total of 126 exposures ranging 
from 10s-160s each. We stacked subsets of these images to maximize the 
S/N ratio, and detected no optical source in either band at the OT 
position reported by GROND (Kann et al., GCN 16939). Our 3-sigma 
limiting magnitudes are:

==================================
tmid  scope   expos  fil  limit
==================================
50m  PROMPT1  25x160s V   >21.2
50m  PROMPT5  24x160s I   >20.6
45m  PROMPT8  46x80s  I   >20.3
==================================

Magnitudes are in the Vega System, calibrated to 3 APASS stars in the 
field.  Magnitudes have not been corrected for line-of-sight Milky Way 
dust extinction, with expected E(B-V)=0.09 (Schlafly & Finkbeiner 2011).

No further Skynet observations are scheduled.


GRB_name: GRB141102A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17024
SUBJECT: Konus-Wind observation of GRB 141102A
DATE:    14/11/03 17:30:19 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

A long duration GRB 141102A (Swift-BAT detection: Cummings et al., GCN 
17020; Fermi-GBM detection: Zhang, GCN Circ. 17021) triggered Konus-Wind 
at T0=46296.656 s UT (12:51:36.656).

The KW triggered on the most intense episode with a duration of about 
0.6 s. There is a possible precursor at ~T0-80 s.

The emission in this episode is seen up to ~1 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB141102_T46296/

As observed by Konus-Wind, the episode
had a fluence of 1.43(-0.42,+1.28)x10^-6 erg/cm2,
and a 16-ms peak flux, measured from T0-0.022 s,
of 5.95(-2.53,+7.28)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the episode
(measured from T0 to T0+0.256 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 = -0.58 (-0.61,+0.93)
and Ep = 444 (-192,+1246) keV (chi2 = 21/28 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -1.3
(chi2 = 21/27 dof)

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


GRB_name: GRB141102A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17025
SUBJECT: GRB 141102A possible precursor was another, known source
DATE:    14/11/04 01:30:34 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

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

The emission at ~T-80 that was mentioned in Golenetskii et al. (GCN
Circ # 17024) as apossible precursor to GRB 141102A was observed by
BAT (trigger # 617315).  It was not a precursor, but rather a soft
burst from GX 354-0.


GRB_name: GRB141104A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17026
SUBJECT: IPN Triangulation of GRB 141104A (long/very bright)
DATE:    14/11/05 14:01:33 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,

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

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

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

The long-duration, very bright GRB 141104A has been observed by Swift 
(BAT), Konus-Wind, Mars Odyssey (HEND), MESSENGER (GRNS), and  INTEGRAL 
(SPI-ACS), so far, at about 200 s UT (00:03:20). 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:
   279.488 (18h 37m 57s) -12.702 (-12d 42' 07")
  Corners:
   279.368 (18h 37m 28s) -12.296 (-12d 17' 45")
   279.549 (18h 38m 12s) -12.326 (-12d 19' 32")
   279.607 (18h 38m 26s) -13.111 (-13d 06' 38")
   279.426 (18h 37m 42s) -13.078 (-13d 04' 41")
  ---------------------------------------------
The error box area is 492 sq. arcmin, and its maximum
dimension is 51 arcmin (the minimum one is 10 arcmin).
The Sun distance was 58.5 deg.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB141104_T00199/IPN/

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


GRB_name: GRB141104A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17027
SUBJECT: Konus-Wind observation of GRB 141104A
DATE:    14/11/05 14:18:31 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration, very bright GRB 141104A
(IPN triangulation: Hurley et al., GCN 17026)
triggered Konus-Wind at T0=199.517 s UT (00:03:19.517).

The light curve shows a double-peaked structure with
a total duration of ~25 s.
The emission is seen up to ~10 MeV.

As observed by Konus-Wind, the burst had a fluence
of 5.9(-0.4,+0.4)x10^-5 erg/cm2, and a 64-ms peak flux,
measured from T0+8.064 s, of 1.6(-0.1,+0.1)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+27.136 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.09 (-0.11,+0.13),
the high energy photon index beta = -2.57 (-0.25,+0.15),
the peak energy Ep = 160 (-13,+16) keV,
chi2 = 96/96 dof.

The spectrum near the peak count rate (measured from T0+7.424 to T0+8.960 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 = -0.86 (-0.09,+0.11),
the high energy photon index beta = -3.32 (-0.81,+0.42),
the peak energy Ep = 232 (-18,+16) keV,
chi2 = 98/96 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB141104_T00199/

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


GRB_name: GRB141017A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17028
SUBJECT: GRB 141017A: Skynet PROMPT-CTIO/SSO Observations
DATE:    14/11/05 15:40:00 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, J. Haislip, D. Reichart, A. Aji, R. Beauchemin, T. Berger, 
A. Dow, A. Foster, N. Frank, M. Hinckle, K. Ivarsen, A. LaCluyze, M. 
Maples, J. Moore, M. Nysewander, C. Salemi, L. Zbinden, and J. A. Crain 
report:

Skynet observed the Swift XRT localization of GRB 141017A (Marshall et 
al., GCN 16919, Swift trigger=615672) with one 24" telescope (P-CTIO 8; 
I band) and three 16" telescopes (P-CTIO 1,4,5; V,R,I bands) of the 
PROMPT array at CTIO, Chile, and with one 16" telescope (P-SSO 3; R 
band) of the PROMPT array at Siding Spring Observatory, Australia.
Starting at 2014-10-18 01:10 UT and continuing until 2014-10-20 02:26 UT 
(t=6.7h-2.3d post-trigger), Skynet took a total of 2316 exposures 
ranging from 80s-160s each. We stacked subsets of these images to 
maximize the S/N ratio, and detected no optical source in any band at 
the OT position reported by Swift UVOT (Oates & Marshall, GCN 16924) and 
confirmed by GROND (Kann, Guelbenzu & Greiner, GCN 16926).  Our 3-sigma 
limiting magnitudes are:

==================================
tmid  scope   expos   fil  limit
==================================
7.4h  P-CTIO4 26x160s  R   >21.1
11.2h P-CTIO8 260x80s  I   >22.2
11.2h P-CTIO1 147x160s V   >22.6
11.3h P-CTIO5 143x160s I   >22.0
20.8h P-SSO3  134x160s R   >22.3
36.5h P-CTIO1 40x160s  V   >22.0
37.2h P-CTIO8 60x80s   I   >21.3
37.3h P-CTIO5 33x160s  I   >21.4
37.9h P-CTIO4 28x160s  R   >21.7
44.8h P-SSO3  133x160s R   >22.4
2.3d  P-CTIO1 30x160s  V   >21.4
2.3d  P-CTIO5 30x160s  I   >20.7
2.3d  P-CTIO8 53x80s   I   >20.5
2.3d  P-CTIO4 22x160s  R   >21.1
==================================

Magnitudes are in the Vega System, calibrated to 5 APASS stars in the 
field.  Magnitudes have not been corrected for line-of-sight Milky Way 
dust extinction, with expected E(B-V)=0.035 (Schlafly & Finkbeiner 2011).

No further Skynet observations are scheduled.


GRB_name: GRB141031B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17029
SUBJECT: GRB 141031B: TShAO optical observations
DATE:    14/11/05 19:27:48 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI),  A. Volnova (IKI), A. Khruslov (INASAN), A. Kusakin 
(Fesenkov Astrophysical Institute), A. Pozanenko (IKI) report on behalf 
of larger GRB follow-up collaboration:

We observed the field of the GRB 141031B (Gompertz et al., GCN 16998)
with  Zeiss-1000 (East) 1m telescope of Tien Shan Astronomical
Observatory on Oct., 31  starting on (UT) 15:39:02.  Within enhanced XRT 
error circle (Goad et al., GCN 17009)  we do not detect any object 
either in a single image (Mazaeva et al., GCN 17007) or   in combined 
image of a total exposure of 4800 s.
Details of the photometry are following:

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

2014-10-31 15:39:02   0.03284    R         600  21.5
2014-10-31 15:39:02   0.05837    R       8*600  22.3


The photometry is based on  following SDSS DR9 stars:

SDSS_id             R_Lupton err
J234748,81+411954,3 16.430 0.014
J234749,26+412154,3 16.866 0.014
J234741,02+411920,5 17.452 0.015


GRB_name: GRB141028A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17030
SUBJECT: GRB 141028A: TShAO optical observation
DATE:    14/11/05 20:23:23 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI),  A. Volnova (IKI), A. Khruslov (INASAN), A. Kusakin 
(Fesenkov Astrophysical Institute), A. Pozanenko (IKI) report on behalf 
of larger GRB follow-up collaboration:

We observed the field of GRB 141028A (Bissaldi et al., GCN 16969)
with  Zeiss-1000 (East) 1-m telescope of Tien Shan Astronomical
Observatory on Oct., 29  starting on (UT) 15:58:47.  We obtained several 
images in R-filter. In a combined image  we clearly  detect optical 
afterglow (Gorbovskoy et al., GCN 16972; Graham et al., GCN 16977). 
Details of the photometry are following:

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

2014-10-29 15:58:47   1.2300    R       10*300  20.5 0.10


The photometry is based on  following SDSS DR9 stars:

SDSS_id                   R_Lupton
J213021,99-001255,7       15.503
J213030,76-001427,8       17.205
J213035,56-001205,6       16.620


GRB_name: GRB141026A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17031
SUBJECT: GRB 141026A: Gemini-North optical and NIR imaging
DATE:    14/11/05 21:03:36 GMT
FROM:    Wen-fai Fong at U of Arizona  <wfong@email.arizona.edu>

W. Fong (U. Arizona) and D. B. Fox (PSU) report on behalf of a larger
collaboration:

"We observed the location of the long-duration GRB 141026A (Hagen et al.,
GCN 16950) with the Gemini Multi-Object Spectrograph (GMOS) and the Near
InfraRed Imager (NIRI) mounted on the Gemini-North 8-m telescope starting
on 2014 Oct 26.402 UT (7.03 hr after the BAT trigger). We obtained 540-sec
of z-band imaging, and a total of 1800-sec in the YJHKs-bands. We clearly
detect the afterglow (Littlejohns et al., GCN 16952; Varela et al., GCN
16953; Gorosabel et al., GCN 16954; Perley et al., GCN 16955; Butler et
al., GCN 16962, GCN 16970; Moskvitin et al., GCN 16966) in all bands. Using
tabulated Gemini zeropoints, we measure an afterglow brightness of z(AB) =
22.0 +/- 0.1 mag and J(AB) = 21.9 +/- 0.1 mag at 7.03 hr after the burst.
These magnitudes have not been corrected for Galactic extinction in the
direction of the burst.

We thank the Gemini staff for their assistance with these observations."


GRB_name: GRB141026A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17033
SUBJECT: GRB 141026A: CrAO optical observation
DATE:    14/11/06 18:49:43 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

V. Rumyantsev (CrAO), E. Mazaeva (IKI),  A. Volnova (IKI), A. Pozanenko 
(IKI) report on  behalf of larger GRB follow-up collaboration:

The GCN #17032 should be read as following:
(We are sorry for inconvenience)

We observed the field of the Swift GRB GRB 141026A (Hagen et al., GCN 
16950) with ZTSh telescope of CrAO observatory starting on Oct. 26 (UT) 
18:25:48. We took several images in R-filter of 120 s exposure under 
poor weather conditions and mean seeing of 5". The optical afterglow 
(Littlejohns et al. GCN 16592; Varela et al. GCN 16953; Gorosabel et al. 
GCN 16954) is clearly visible in our stacked image.   Photometry of a 
combined image is following

Date       UT start,  t-t0     Filter   Exp.      OT   OT_err
                       (mid, days)        (s)

2014-10-26 18:25:48   0.7020   R        53*120    21.88 0.18

The photometry is based on USNO-B1.0  stars

RA             DEC           R
044,065509    +26,958050     18.71
044,051792    +26,894737     18.59
044,049131    +26,929059     17.48


GRB_name: GRB141104A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17034
SUBJECT: GRB 141104A Tiled Swift observations
DATE:    14/11/06 21:40:54 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 141104A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00032

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: GRB141028A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17035
SUBJECT: GRB 141028A: Mondy optical observations
DATE:    14/11/07 08:08:50 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of GRB 141028A (Bissaldi et al., GCN 16969) with 
AZT-33IK telescope of Sayan observatory (Mondy) on Oct., 30  starting on 
(UT) 14:12:40.  We obtained several  images in R-filter. In a combined image 
we  detect optical  afterglow (Gorbovskoy et al., GCN 16972; Graham et al., 
GCN 16977).

Details of the photometry are following:

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

2014-10-30 14:12:40   2.1733  R      2520    21.66 0.22


The photometry is based on  following SDSS DR9 stars:

SDSS_id                         R_Lupton
J213021,99-001255,7       15.503
J213030,76-001427,8       17.205
J213035,56-001205,6       16.620 


GRB_name: GRB141104A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17036
SUBJECT: GRB 141104A: Swift-XRT observations
DATE:    14/11/08 21:40:43 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

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

Swift-XRT has observed the error box of the IPN GRB 141104A (Hurley et  
al. GCN 17026) in a series of observations tiled on the sky. The total  
exposure time is 14.0 ks spread over 3 fields. The observations  
started ~ 3 days after the IPN trigger. We detect four sources with  
S/N ~ 3 or higher, within or close to the IPN error box. Namely  
(ordered by ascending Dec):

Source 1
RA: 279.53959 = 18h 38m 9.50s (J2000)
Dec: -13.06216 = -13d 03' 43.8" J(2000)
Err: 4.4 arcsec (radius, 90% confidence).
Exposure time: 3.9 ks.

Source 2
RA:  279.51690 = 18h 38m 4.06s (J2000)
Dec:  -12.78750  = -12d 47' 15.0" (J2000)
Err: 4.9 arcsec (radius, 90% confidence)
Exposure time: 4.4 ks

Source 3
RA: 279.38702  = 18h 37m 32.88s (J2000)
Dec: -12.34930 = -12d 20' 57.5" (J2000)
Err: 3.8 arcsec (radius, 90% confidence).
Exposure time: 3.4 ks.

Source 4
RA: 279.49073 = 18h 37m 57.78s (J2000)
Dec: -12.30119 = -12d 18' 04.3" (J2000)
Err: 4.6 arcsec (radius, 90% confidence).
Exposure time: 3.1 ks.


The northernmost Sources #3 and #4 are close to (#3) or just outside  
(#4) the IPN error box and possess an X-ray and optical counterpart,  
so are likely unrelated to the afterglow. The central source #2 has an  
optical counterpart, while the southernmost source #1 does not have  
counterparts. The most promising XRT afterglow candidate is thus  
source #1, although the counterpart of #2 could be the host galaxy of  
the afterglow.  We cannot measure variability at this time, so a  
secure identification of the afterglow is not possible.

Details on the present analysis can be found at:

http://www.swift.ac.uk/xrt_products/TILED_GRB00032/


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


GRB_name: GRB141109A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17037
SUBJECT: GRB 141109A: Swift detection of a burst
DATE:    14/11/09 06:05:41 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

P. D'Avanzo (INAF-OAB), S. D. Barthelmy (GSFC),
M. G. Bernardini (INAF-OAB), M. M. Chester (PSU),
A. Melandri (INAF-OAB), D. M. Palmer (LANL) and M. H. Siegel (PSU)
report on behalf of the Swift Team:

At 05:49:55 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 141109A (trigger=618024).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 144.507, -0.602, which is 
   RA(J2000)  =  09h 38m 02s
   Dec(J2000) = -00d 36' 04"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a multi-peak
structure with a duration of at least 170 sec.  The peak count rate
was ~3000 counts/sec (15-350 keV), at ~118 sec after the trigger. 

The XRT began observing the field at 05:52:04.3 UT, 129.2 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 144.5334, -0.6093 which is equivalent to:
   RA(J2000)  = +09h 38m 8.02s
   Dec(J2000) = -00d 36' 33.5"
with an uncertainty of 6.5 arcseconds (radius, 90% containment). This
location is 98 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 0.1 s image was 1.18e-08 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 139 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.04. 

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


GRB_name: GRB141109B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17038
SUBJECT: GRB 141109B: Swift detection of a burst
DATE:    14/11/09 08:03:11 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

A. Melandri (INAF-OAB), S. D. Barthelmy (GSFC),
M. G. Bernardini (INAF-OAB), M. M. Chester (PSU),
P. D'Avanzo (INAF-OAB), C. B. Markwardt (NASA/GSFC) and
T. N. Ukwatta (LANL) report on behalf of the Swift Team:

At 07:47:39 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 141109B (trigger=618032).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 222.361, +73.125, which is 
   RA(J2000)  =  14h 49m 27s
   Dec(J2000) = +73d 07' 30"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows multiple peaks
with a duration of about 45 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~6 sec after the trigger. 

The XRT began observing the field at 07:50:43.7 UT, 184.6 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 222.3033,
73.1306 which is equivalent to:
   RA(J2000)  = 14h 49m 12.79s
   Dec(J2000) = +73d 07' 50.3"
with an uncertainty of 2.1 arcseconds (radius, 90% containment). This
location is 63 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (2.46 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 2.4
(+1.91/-1.72) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 187 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers none of
the XRT error circle. The 8'x8' region for the list of sources generated
on-board covers 100% of the XRT error circle. The list of sources is typically
complete to about 18 mag. No correction has been made for the expected
extinction corresponding to E(B-V) of 0.02. 

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


GRB_name: GRB141109A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17039
SUBJECT: GRB 141109A: REM NIR candidate afterglow
DATE:    14/11/09 09:56:07 GMT
FROM:    Stefano Covino at Brera Astronomical Observatory  <stefano.covino@gmail.com>

S. Covino (INAF/OAB) on behalf of the REM team:

We observed the field of the GRB141109A (D'Avanzo et al., GCN 17037) simultaneously in the optical and near infrared with the the 60-cm robotic telescope REM at La Silla Observatory (Chile). 

The observations started at 05:52:08 UT, about 2 min after the GRB, when the source was less than 10deg from the local horizon. 

A candidate afterglow in the XRT error box is detected at the coordinates:
RA(J2000) = 09:38:07:40
DEC(J2000) = -00:36:30.13

A very preliminary photometry indicates it was H~15.7 about 35 min after the burst. 

[GCN OPS NOTE(09nov14): Per author's request, "REM was added tot he Subject-line.]


GRB_name: GRB141109A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17040
SUBJECT: X-shooter redshift of GRB 141109A
DATE:    14/11/09 10:43:29 GMT
FROM:    Paul Vreeswijk at Weizmann Inst of Science  <paul.vreeswijk@weizmann.ac.il>

D. Xu (DARK/NBI), P. M. Vreeswijk (Weizmann), J. P. U. Fynbo
(DARK/NBI), V. D'Elia (ASI/ASDC and INAF/Roma), K. Wiersema,
N. R. Tanvir (Univ. Leicester), A. de Ugarte Postigo (IAA-CSIC),
S. Covino (INAF/OAB) report on behalf of a larger collaboration:

We observed the optical afterglow of the Swift GRB 141109A (D'Avanzo
et al., GCN 17037), using the X-shooter spectrograph at ESO's
VLT. Observations started at 07:45 UT on 2014 Nov 9 (1.9 hr after the
GRB), and consisted of 2x1200 s exposures in each of the UVB, VIS, and
NIR arms, covering the wavelength range 3000-20,000 AA.

In the acquisition image, we detect a point source, which is not
detected in the SDSS, at the position (J2000):

 RA = 09:38:07.44
 Dec = -00:36:29.9

with an uncertainty of about 0.5". This position is consistent with
that of the NIR afterglow reported by Covino et al. (GCN 17039).  We
measure a (preliminary) magnitude of R=19.2+-0.1 (Vega).

We detect a variety of absorption features throughout the entire
spectrum. In particular, a wide trough is visible centered around 4800
AA, which we interpret as due to H I absorption at redshift z~3.
Identification of several metal features as due to, among others, Si
II, C II, Fe II, C IV, SiIV, allows us to refine the value to
z=2.993. The presence of several fine structure lines of Fe II, Si II,
O I, Ni II and C II confirms this is the redshift of the GRB.

We note the presence of two strong intervening system at z ~ 1.67 and
z ~ 2.5 (detected in Mg II).

We acknowledge excellent support from the ESO observing staff at
Paranal, in particular Valentin Ivanov and Marcelo Lopez. We also
thank the visiting astronomer Simone Zaglia from the ESO-GAIA survey,
who made these observation possible.


GRB_name: GRB141109A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17041
SUBJECT: GRB 141109A: GROND afterglow observation
DATE:    14/11/09 12:04:14 GMT
FROM:    Sebastian Schmidl at TLS Tautenburg  <schmidl@tls-tautenburg.de>

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

We observed the field of GRB 141109A (Swift trigger 618024; P. D'Avanzo
et al., GCN 17037) simultaneously in g'r'i'z'JHK with GROND (Greiner et
al. 2008, PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La
Silla Observatory (Chile).

Observations started at 06:51 UT on November 09, 2014, approximately 1
hour after the GRB trigger. They were performed at an average seeing of
1.7" and at an average airmass of 1.6.

We detect the optical/NIR aftergow reported by Covino et al. (GCN 17039)
and Xu et al. (GCN 17040).

Based on total exposures of 25.0 minutes in g'r'i'z' and 20.0 minutes in
JHK, at a midtime of 2.3 hrs after the burst, we measure the following
preliminary magnitudes (AB magnitude system):

g' = 20.7 +/- 0.1 mag,
r' = 19.7 +/- 0.1 mag,
i' = 19.4 +/- 0.1 mag,
z' = 19.2 +/- 0.1 mag,
J = 19.0 +/- 0.1 mag,
H = 18.8 +/- 0.1 mag, and
K = 18.5 +/- 0.1 mag.

The magnitudes are calibrated against SDSS and 2MASS field stars and are
not corrected for the Galactic foreground extinction corresponding to a
reddening of E_(B-V)= 0.04 in the direction of the burst (Schlegel et al.
1998).


GRB_name: GRB141109A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17042
SUBJECT: GRB 141109A: CQUEAN Detection at 0.85 - 1.05 micron
DATE:    14/11/09 14:01:05 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

Myungshin Im, Yongjung Kim, Minhee Hyun (CEOU/SNU),
Woojin Park, and Soojong Pak (Kyunghee Univ.)

We observed the field of GRB 141109A (D'Avanzo et al. GCN 17037),
using CQEUAN (Park et al. 2012) on the 2.1-m Otto-Struve telescope
at the McDonald Observatory in Texas, US. The observation started
at 2014-11-09 10:47:05 UT, or about 5 hrs after the BAT alert.
A series of images were taken with medium-band filters centered at
0.875, 0.925, 0.975, and 1.025 micron.

We identify the optical/NIR counterpart reported in Covino et al.
(GCN 17039), Xu et al. (GCN 17040), and Graham et al. (GCN 17041),
in all of the medium-band images. A preliminary magnitude
at 0.875 micron is 20.2 +- 0.1 AB mag. Further analysis of the data
is ongoing.


GRB_name: GRB141109A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17043
SUBJECT: GRB 141109A: Enhanced Swift-XRT position
DATE:    14/11/09 14:35:35 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 1173 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 141109A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 144.53083, -0.60795 which is equivalent
to:

RA (J2000): 09h 38m 7.40s
Dec (J2000): -00d 36' 28.6"

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

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

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


GRB_name: GRB141109A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17044
SUBJECT: GRB 141109A: Swift-BAT refined analysis
DATE:    14/11/09 18:02:52 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. D'Avanzo (INAF-OAB), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 141109A (trigger #618024)
(D'Avanzo, et al., GCN Circ. 17037).  The BAT ground-calculated position is
RA, Dec = 144.563, -0.581 deg, which is 
   RA(J2000)  =  09h 38m 15.0s 
   Dec(J2000) = -00d 34' 52.4" 
with an uncertainty of 3.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 60%.
 
The mask-weighted light curve shows a weak peak from ~T+0 to ~T+40 sec,
then the bulk of the emission came from ~T+60 to ~T+190 sec,  and then a tail
extending out to ~T+380 sec.  T90 (15-350 keV) is 200 +- 47 sec
(estimated error including systematics).
 
The time-averaged spectrum from T+0.60 to T+323.15 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.52 +- 0.07.  The fluence in the 15-150 keV band is 6.8 +- 0.3 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+117.39 sec in the 15-150 keV band
is 2.5 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/618024/BA/


GRB_name: GRB141109B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17045
SUBJECT: GRB 141109B: Enhanced Swift-XRT position
DATE:    14/11/09 18:04:45 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 2820 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 141109B, 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 = 222.30317, +73.13085 which is equivalent
to:

RA (J2000): 14h 49m 12.76s
Dec (J2000): +73d 07' 51.1"

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: GRB141109B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17046
SUBJECT: GRB 141109B: Swift-BAT refined analysis
DATE:    14/11/09 18:11:35 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 (GSFC/UMBC),
C. B. Markwardt (GSFC), A. Melandri (INAF-OAB), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):
 
Using the data set from T-60 to T+243 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 141109B (trigger #618032)
(Melandri, et al., GCN Circ. 17038).  The BAT ground-calculated position is
RA, Dec = 222.453, 73.141 deg, which is 
   RA(J2000)  =  14h 49m 48.8s 
   Dec(J2000) = +73d 08' 26.3" 
with an uncertainty of 2.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 75%.
 
The mask-weighted light curve shows a couple overlapping peaks starting at 
~T-20 sec, peaking at ~T+28 sec, and ending at ~T+60 sec.
T90 (15-350 keV) is 54.2 +- 5.0 sec (estimated error including systematics).
 
The time-averaged spectrum from T-13.18 to T+44.18 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.85 +- 0.22.  The fluence in the 15-150 keV band is 6.3 +- 0.9 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+28.05 sec in the 15-150 keV band
is 0.4 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/618032/BA/


GRB_name: GRB141109B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17047
SUBJECT: GRB 141109B: BOOTES-4 and TERSKOL optical upper limit 
DATE:    14/11/09 22:02:16 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

I.V. Sokolov, A. Moskvitin, V.V. Sokolov (SAO-RAS Zelenchukaja, Russia),
S. Guziy (Nikolaev Univ. Obs., Ukraine), A.J. Castro-Tirado, J.C. Tello
(IAA-CSIC Granada, Spain), Y. Fan, X. Zhao, J. Bai, Ch. Wang and Y. Xin
(Yunnan National Astronomical Observatory, China) on behalf of a larger
collaboration, report:

Following the detection of GRB 141109B by Swift/BAT (Melandri et al., GCNC
17038), the robotic 0.6m MET telescope at the BOOTES-4 station, in Lijiang
Astronomical Observatory (China) responded to the event after the sunset,
with the first images being obtained about 3.5 h post-burst. Additional
R-band images (6 x 300s) were taken at the 2.0m Terskol telescope in the
Northern Caucasus starting 11.3 hr post-burst. No optical source is
detected at the refined Swift/XRT position (Beardmore et al., GCNC 17045)
down to the DSS limit. Observations at longer wavelengths are encouraged.


GRB_name: GRB141109A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17048
SUBJECT: GRB 141109A: Swift-XRT refined Analysis
DATE:    14/11/09 23:04:08 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

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

We have analysed 5.7 ks of XRT data for GRB 141109A (D'Avanzo  et al.
GCN Circ. 17037),  from 119 s to 46.5 ks after the  BAT trigger. The
data comprise 409 s in Windowed Timing (WT) mode (the first 8 s were
taken while Swift was slewing) with the remainder in Photon Counting
(PC) mode. The enhanced XRT position for this burst was given by
Osborne et al. (GCN Circ. 17043).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=0.80 (+0.25, -0.14). At T+212 s  the decay
steepens to an alpha of 3.25 (+0.51, -0.20) before breaking again at
T+363 s to a final decay with index alpha=1.254 (+0.021, -0.020). Some
flaring activity is observed between T+300 s and T+500 s.

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.673 (+0.028, -0.027). The
best-fitting absorption column is  1.73 (+0.11, -0.10) x 10^21 cm^-2,
in excess of the Galactic value of 3.3 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.99 (+0.14, -0.13)
and a best-fitting absorption column of 1.3 (+/-0.4) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.4 x 10^-11 (4.4 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.3 (+/-0.4) x 10^21 cm^-2
Galactic foreground: 3.3 x 10^20 cm^-2
Excess significance: 4.5 sigma
Photon index:      1.99 (+0.14, -0.13)

If the light curve continues to decay with a power-law decay index of
1.254, 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 1.1 x
10^-12 (1.4 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00618024.

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


GRB_name: GRB141109A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17049
SUBJECT: GRB 141109A: MITSuME Ishigakijima upper limits
DATE:    14/11/10 01:20:00 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

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

We observed the field of GRB 141109A (D'Avanzo et al., GCNC 17037)
with the optical three color (g', Rc and Ic) CCD camera attached
to the Murikabushi 1m telescope of Ishigakijima Astronomical
Observatory.

The observation started on 2014-11-09 18:02:45.43 UT, (~12.2 h after the burst).
We could not detect the previously reported afterglow (Covino, GCNC 17039;
Xu et al., GCNC 17040; Graham et al., GCNC 17041) in all the three bands.

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

#T0+[day]  MID-UT    T-EXP[sec]   g'     Rc     Ic
-----------------------------------------------------
0.53718    18:43:28    3660.0   >20.9  >20.9  >20.1
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB141109B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17051
SUBJECT: GRB 141109B: Swift-XRT refined Analysis
DATE:    14/11/10 08:03:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.0 ks of XRT data for GRB 141109B (Melandri  et al.
GCN Circ. 17038),  from 170 s to 70.7 ks after the  BAT trigger. The
data comprise 7 s in Windowed Timing (WT) mode (taken while Swift was
slewing), with the remainder in Photon Counting (PC) mode. The enhanced
XRT position for this burst was given by Beardmore et al. (GCN Circ.
17045).

The light curve can be modelled with an initial power-law decay with an
index of alpha=5.2 (+1.4, -1.1), followed by a break at T+291 s to an
alpha of 0.51 (+/-0.04).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.96 (+0.16, -0.15). The
best-fitting absorption column is  9.8 (+4.2, -3.8) x 10^20 cm^-2, in
excess of the Galactic value of 2.5 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.4 x 10^-11 (4.1 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      9.8 (+4.2, -3.8) x 10^20 cm^-2
Galactic foreground: 2.5 x 10^20 cm^-2
Excess significance: 3.2 sigma
Photon index:      1.96 (+0.16, -0.15)

If the light curve continues to decay with a power-law decay index of
0.51, the count rate at T+24 hours will be 0.034 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x
10^-12 (1.4 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00618032.

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


GRB_name: GRB141109B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17052
SUBJECT: GRB 141109B: IRAM 30m millimetre observations
DATE:    14/11/10 10:16:50 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

A. J. Castro-Tirado, J. C. Tello (IAA-CSIC Granada), A. Monfardini
(NEEL-CNRS Grenoble), R. Adam, B. Comis (LPSC Grenoble), N. Ponthieu
(Univ. of Grenoble), C. Kramer and I. Hermelo (IRAM Granada), on behalf of
a larger collaboration, report:

Following the detection of GRB 141109B by Swift (Melandri et al. GCNC
17038), observations with the IRAM 30m antenna (+NIKA) at Pico Veleta
(Spain) were triggered on 9 Nov under good conditions but at relatively
low elevation (25 deg). At the position of the X-ray afterglow (Beardmore
et al. GCNC 17045), we detect no mm afterglow (at 150 GHz) down to a
preliminary flux density of 1 mJy (3 sigma) on Nov 9, 20:30 UT (mid time).
We acknowledge excellent assistance from the IRAM observers.


GRB_name: GRB141109A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17053
SUBJECT: GRB141109A : Xinglong TNT optical observation
DATE:    14/11/10 13:24:14 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

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

We began to observe GRB 141109A (D'Avanzo et al., GCNC 17037)  
with Xinglong  0.8-m TNT telescope at 2014-11-09, 19:45:06(UT),
about 13.95 hour after the burst.

The optical counterpart reported by ( Covino GCN 17039;  Xu et al., 17040)
 was  detected in 24*300 sec R-band coadded image. 
The brightness of the  optical emission is estimated to be 
about R=21.84 mag at the mid-time of 15.07 hours after the burst.

Combined with the reports ( Covino GCN 17039 and  Xu et al., 17040 ), 
the decay slope of this OT is roughtly about \alpha~1.12, 
if we fit the data with a single power law.

The message may be cited.


GRB_name: GRB141109B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17054
SUBJECT: GRB 141109B: MITSuME Akeno upper limits 
DATE:    14/11/10 14:46:44 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

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

We observed the field of GRB 141109B (A.Melandri et al., GCN Circular #17038) with the 
optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan.

The observation started on 2014-11-09 18:57:42.8 UT (~11.2h after the burst).
We did not find any new point source within XRT circle in all three bands.

The measured magnitudes are listed below.

T0+[sec]      MID-UT      T-EXP[sec]         g'           Rc           Ic
---------------------------------------------------------------------------------------
  40320     19:52:29.1          780           >19.4      >19.0     > 18.4
---------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst 
T-EXP: Total Exposure time 
We used GSC2.3 catalog for flux calibration.


GRB_name: GRB141109A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17055
SUBJECT: Konus-Wind observation of GRB 141109A
DATE:    14/11/10 17:35:48 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, and T. Cline on behalf of the Konus-Wind
team report:

The most intense part of the long GRB 141109A (Swift-BAT trigger 
#618024: D'Avanzo, et al., GCN Circ. 17037, Baumgartner, et al., GCN 
Circ. 17044) was detected by Konus-Wind in the waiting mode.

The burst light curve shows two pulses started at ~T0(BAT)+31 s with a 
total duration of ~94 s, and a weak tail seen in the soft energy range 
G1 up to ~T0(BAT)+300 s.

As observed by Konus-Wind, the burst had a fluence of
1.37(-0.18,+0.20)x10^-5 erg/cm2 and a 2.944-s peak flux,
measured from ~T0(BAT)+81 s, of (4.9 +/- 0.8)x10^-7 erg/cm2 (both in the 
20 - 1200 keV energy range).

Modeling the K-W 3-channel time-integrated spectrum (from T0(BAT)+31 s
to T0(BAT)+125 s) by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -1.24(-0.25,+0.37), and Ep = 191(-43,+76) keV.

Assuming z = 2.993 (Xu et al., GCN 17040) and a standard cosmology model 
with H_0 = 71 km/s/Mpc, Omega_M = 0.27, Omega_Lambda = 0.73, the 
isotropic energy release is E_iso = 3.31(-0.59,+0.78)x10^53 erg, and
the isotropic peak luminosity is L_iso = (4.8 +/- 0.9)x10^52 erg/s in 1 
keV to 10 MeV at the GRB rest frame extrapolating the best exponential 
cutoff function fit.

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

The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB141109A/


GRB_name: GRB141109A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17056
SUBJECT: GRB 141109A: NOT r-band observation
DATE:    14/11/10 21:27:58 GMT
FROM:    Zach Cano at U of Iceland  <zewcano@gmail.com>

â€‹Z. Cano (U. Iceland), D. Malesani (DARK/NBI), K. Nilsson (FINCA), T.
Kangas (U. Turku), P. Jakobsson (U. Iceland) report on behalf of a larger
collaboration:

We observed the field of GRB 141109A (D'Avanzo et al., GCN Circ. 17037)
with the 2.5-m Nordic Optical Telescope (NOT) with ALFOSC starting at 04:39
UT on 10-Nov-2014.  We obtained 3x300 s frames in the SDSS r-band filter.

We clearly detect the optical afterglow of GRB 141109A (Covino, GCN Circ.
17039; Xu et al., GCN Circ. 17040; Graham et al., GCN Circ. 17041; Im et
al., GCN Circ. 17042; Xin et al., GCN Circ. 17053), which has an apparent
magnitude of r=22.1 +- 0.1 at a mid exposure time of +22.8 hr.  The
magnitude is not corrected for foreground extinction, and is calibrated
using several nearby SDSS stars in the FOV.â€‹


GRB_name: GRB141109A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17057
SUBJECT: GRB 141109A: Swift/UVOT Detection
DATE:    14/11/10 22:55:16 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

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

The Swift/UVOT began settled observations of the field of GRB 141109A
139 s after the BAT trigger (D'Avanzo et al., GCN Circ. 17037).
A source consistent with the optical position (Covino, GCN Circ. 17039;
Xu et al., GCN Circ. 17040) is detected in the initial UVOT exposures.

The 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              139          289          147         20.0 +/- 0.2
white             3991         4191          197         20.8 +/- 0.2
v                 5656         5856          197        >18.9
b                 3786         3986          197        >20.3
u                  297         6276          227        >19.7
w1                6066         6266          197        >20.1
m2                5861         6061          197        >20.7
w2                4197         4339          140        >20.9

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


GRB_name: GRB141109B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17058
SUBJECT: GRB 141109B: Swift/UVOT Upper Limits
DATE:    14/11/10 22:56:56 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and A. Melandri (INAF-OAB)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 141109B
188 s after the BAT trigger (Melandri et al., GCN Circ. 17038).
No optical afterglow consistent with the UVOT-enhanced XRT position
(Beardmore et al., GCN Circ. 17045)
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           188          338          147         >20.1
u_FC               347          596          246         >20.4
white              188         6699          588         >21.3
v                  677         7110          313         >20.4
b                  602         6494          294         >21.0
u                  347        13125         1061         >20.9
w1                 727        12566         1207         >21.0
m2                 701         7315          255         >20.8
w2                 828         6905          255         >21.0

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: GRB141109A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17059
SUBJECT: GRB 141109A: Terskol photometry
DATE:    14/11/11 17:27:57 GMT
FROM:    Vladimir Sokolov at SAO RAS  <sokolov@sao.ru>

I.V. Sokolov (TF INASAN, Russia), V.N. Komarova, A.S Moskvitin,
V.V. Sokolov, T.S.Sokolova (SAO RAS, Russia), report:

We observed the field of GRB 141109A (D'Avanzo et al., GCN 17037)
with the 2-meter telescope Zeiss-2000 (Terskol peak) on
November, 10, in 20.7 hours after the trigger.
10 x 300 sec. images in I filter were obtained.

The transient discovered by REM (Covino, GCN 17039) is clearly
detected in the stack frame. The OT magnitude is I = 21.1 +/- 0.1.
Photometry is based on the nearby SDSS stars.  Their magnitudes
were converted with the transformation equations from Lupon, 2005.


GRB_name: GRB141109A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17062
SUBJECT: GRB 141109A: AAO optical observations
DATE:    14/11/12 19:34:55 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of the Swift GRB 141109A  (D'Avanzo et al., GCN 
17037) with AS-32 (0.7m) telescope of Abastumani Observatory. 
Observations were performed under mean seeing (FWHM) of 2.4". We 
obtained several unfiltered images on Nov. 10 starting on (UT) 01:05:04. 
  At the position reported in (Covino, GCN 16932) we marginally 
detected (S/N =2) the afterglow of GRB 141109A  (Covino, GCN 16932; Xu 
et al., GCN 17040; Graham et al., GCN 17041). Preliminary photometry is 
following:

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

2014-11-10  01:05:04  0.836       clear   37*120  21.7  0.4

The photometry is based on several SDSS-DR9 stars R magnitudes 
transformed from SDSS-DR9 based on Lupton transformations:

SDSS-DR9            R
J093801.18-003731.5 17.6330
J093759.83-003741.8 17.2029
J093815.45-003332.9 18.2004


GRB_name: GRB141109A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17063
SUBJECT: GRB 141109A: TAROT La Silla observatory optical observations
DATE:    14/11/12 23:17:57 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 141109A detected by SWIFT
(trigger 618024) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 93s after the GRB trigger
(18s after the notice). The elevation of the field increased from
10 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).
This image was obtained when the gamma emission was still
very active. We do not detect any OT with a limiting magnitude of:

t0+93s to t0+153s : Rlim = 12.9

The optical afterglow reported by Covino (GCNC 17039)
is detected in co added images (in tracking mode):

  t0+465s to  t0+655s : Rlim = 17.3
  t0+665s to  t0+868s : R = 16.8
  t0+879s to t0+1069s : R = 16.1
t0+1093s to t0+1283s : R = 16.7
t0+1293s to t0+1497s : Rlim = 17.2

The TAROT photometry indicates that the optical afterglow
reached the maximum of light about 16 minutes after the
Swift trigger.

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


GRB_name: GRB141031A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17064
SUBJECT: GRB 141031A: TAROT La Silla observatory optical observations
DATE:    14/11/13 00:15:45 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 141031A detected by SWIFT
(trigger 617110) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 45s after the GRB trigger
(15s after the notice). The elevation of the field increased from
45 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+45s to t0+105s : Rlim = 14.8

Following images are recorded in tracking mode.
We used late images to substract non variable stars
in the XRT error box.

The second image is 30.0s exposure in tracking mode:
t0+119s to t0+149s : Rlim = 17.5

Later images (until 1800s after the trigger) do not
show any optical afterglow at Rlim = 17.5

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


GRB_name: GRB141022A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17065
SUBJECT: GRB 141022A: TAROT La Silla observatory optical observations
DATE:    14/11/13 00:35:18 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 141022A detected by SWIFT
(trigger 616061) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 71s after the GRB trigger
(16s after the notice). The elevation of the field decreased from
24 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+71s to t0+131s : Rlim = 16.4

The second image is 30.0s exposure in tracking mode:
t0+145s to t0+175s : Rlim = 17.5

Later TAROT images (until 1800s) do not show any
afterglow at Rlim = 17.5

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


GRB_name: GRB141015A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17066
SUBJECT: GRB 141015A: TAROT La Silla observatory optical observations
DATE:    14/11/13 00:47:42 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 141015A detected by SWIFT
(trigger 615399) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 55s after the GRB trigger
(19s after the notice). The elevation of the field decreased from
42 degrees above horizon but it was dawn
(sun elevation -11 deg).

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+55s to t0+115s : R > 12.2

Later images were acquired in tracking mode until 521
seconds after the trigger. We detect no optical afterglow
at Rlim = 12.5

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


GRB_name: GRB141109B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17067
SUBJECT: GRB 141109B: optical upper limits
DATE:    14/11/13 00:53:15 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), A. Stepura (UAFO, ISON),  R. Inasaridze (AAO),  B. 
Abdulloev (Institute of Astrophysics),   A. Matkin (UAFO, ISON), N. 
Minikulov (Institute of Astrophysics), A. Volnova (IKI), Molotov (KIAM), A. 
Pozanenko (IKI) report on behalf of  larger GRB follow-up collaboration:

We observed the field of the Swift GRB 141109B  (Melandri  et al., GCN 
17038) with following instruments: SANTEL-650 (0.65m) telescope of 
UAFO/ISON-Ussuriysk Observatory,  AZT-8 (0.7m) telescope of Gissar 
observatory, and AS-32 (0.7m) telescope of Abastumani Observatory  (AAO). In 
the enhanced XRT error circle (Beardmore  et al., GCN 17045)  we do not 
detect any source with  upper limits listed below:

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

2014-11-09 09:18:51  0.10220    clear  100*60  20.7          UAFO
2014-11-09 14:30:43  0.29425    R          40*60  19.9          Gissar
2014-11-09 15:26:30  0.38464    clear    71*120 22.0         AAO


The photometry is based on  stars of USNO-B1.0 and assumed R magnitudes:
RA                 DEC                 R
222.429145 +73.085200    14.97
222.517839 +73.110348    15.54
222.193512 +73.123517    17.06
222.275356 +73.104562    17.46
222.463681 +73.158509    17.55 


GRB_name: GRB141109A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17070
SUBJECT: GRB 141109A: VLA detection
DATE:    14/11/16 22:57:57 GMT
FROM:    Alessandra Corsi at Texas Tech U  <alessandra.corsi@ttu.edu>

A. Corsi (Texas Tech U.) reports on behalf of a larger collaboration:

We imaged the position of GRB 141109A (D'Avanzo et al., GCN 17037) with the 
Karl G. Jansky Very Large Array (VLA) in K-band at about 7.5 hours after the burst. 
A provisional reduction shows a source consistent with the location of the GRB NIR, 
optical, and X-ray afterglows (e.g., Covino et al., GCN 17039; Xu et al., GCN 17040; 
Osborne et al. GCN 17043).  At this time, we estimate a preliminary flux of about 
142 uJy at 21.8 GHz. The map rms is about 9.3 uJy.

Further observations are ongoing.


GRB_name: GRB141104A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17071
SUBJECT: GRB 141104A: further Swift-XRT observations and afterglow candidate
DATE:    14/11/17 17:00:02 GMT
FROM:    Valerio D'Elia at ASDC  <delia@asdc.asi.it>

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

Swift-XRT has observed again a field in the error box of the IPN GRB  
141104A (Hurley et al. GCN 17026). The total exposure time of the new  
observation, which started ~ 10 days after the IPN trigger, is 9 ks.  
Source #2 reported in D'Elia & Izzo (GCN 17036) is still detected with  
a consistent count rate, while source #1 is marginally detected at a  
S/N level just below 3. The count rate of the new detection clearly  
implies fading between the two epochs. Despite the slow temporal decay  
(t^-0.55) and the flux variation of a factor of just two that can not  
exclude another origin, source #1 is the best afterglow candidate for  
GRB 141104A. Further observations are Sun constrained until February  
2015.

Details on the present analysis can be found at:

http://www.swift.ac.uk/xrt_products/TILED_GRB00032/


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


GRB_name: GRB141109A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17072
SUBJECT: GRB 141109A: further VLA observations
DATE:    14/11/18 02:18:28 GMT
FROM:    Alessandra Corsi at Texas Tech U  <alessandra.corsi@ttu.edu>

A. Corsi and D.R. Bhakta (Texas Tech. U.) report on behalf of a larger collaboration:

We imaged again the position of GRB 141109A (D'Avanzo et al., GCN 17037) with 
the Karl G. Jansky Very Large Array (VLA) from 2.4 d to 8.3 d after the BAT trigger. 
For the radio counterpart consistent with the location of the GRB NIR, optical, and 
X-ray afterglows (Covino et al., GCN 17039; Xu et al., GCN 17040; Osborne et al. 
GCN 17043; Corsi, GCN 17070), we estimate the following preliminary fluxes: 

Mean Epoch (d) | Freq. (GHz) | Flux (uJy) | map rms (uJy)
-------------------------
 2.4 | 21.8 | 51 | 9
-------------------------
 6.3 | 14.0 | 50 | 6
-------------------------
 8.3 |  6.2 | 57 | 6


GRB_name: GRB141118A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17073
SUBJECT: IPN Triangulation of GRB 141118A
DATE:    14/11/20 13:12:27 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@ssl.berkeley.edu>

K. Hurley, on behalf of the IPN,

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

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

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

D. M. Smith, J. McTiernan, R. Schwartz, W.
Hajdas, and A. Zehnder, on behalf of the RHESSI GRB team, 

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

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

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

GRB 141118A has been observed by Fermi GBM, Konus-Wind, RHESSI, Swift
(outside the coded field of view), Odyssey (HEND), and MESSENGER
(GRNS), so far, at 58550 s (16:15:50 UT) so far.  We have triangulated
it to a preliminary, 3 sigma error box whose area is 2890 sq. arcmin.
and whose coordinates are:

              RA(2000)                      DEC(2000)
CENTER:  156.874 o =10 h 27 m 30 s     19.079 o= 19 o 04 ' 45 "
CORNERS: 157.620 o =10 h 30 m 29 s     21.134 o= 21 o 08 ' 01 "
         156.676 o =10 h 26 m 42 s     19.104 o= 19 o 06 ' 15 "
         157.071 o =10 h 28 m 17 s     19.054 o= 19 o 03 ' 13 "
         155.644 o =10 h 22 m 35 s     15.768 o= 15 o 46 ' 06 "

This error box may be improved.  A map has been posted at 
ssl.berkeley.edu/ipn3/141118A.  Details of this burst will be
given in a forthcoming GCN Circular.


GRB_name: GRB141118A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17074
SUBJECT: Konus-Wind observation of GRB 141118A
DATE:    14/11/20 13:58:43 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

A long-duration GRB 141118A (IPN triangulation: Hurley et al., GCN 17073)
triggered Konus-Wind at T0=58548.540 s UT (16:15:48.540).

The KW light curve shows a single emission episode lasting from ~T0-0.5 s
to ~T0+5 s. The emission in this episode is visible up to ~2 MeV.

As observed by Konus-Wind, the burst had a fluence
of 2.3(-0.5,+1.4)x10^-6 erg/cm2, and a 64-ms peak flux,
measured from T0, of 1.6(-0.4,+1.0)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 15 MeV range
by the cutoff power law with the following model parameters:
the photon index alpha = -1.14(-0.67,+0.89),
and the peak energy Ep = 165(-55,+198) keV,
chi2 = 95/97 dof.
Fitting this spectrum with the Band model yields the same
values of alpha and Ep and an upper limit on beta of -2.0

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB141118_T58548/

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


GRB_name: GRB141121A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17075
SUBJECT: GRB 141121A: Swift detection of a burst
DATE:    14/11/21 04:07:51 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. Y. Lien (GSFC/UMBC), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), C. B. Markwardt (NASA/GSFC),
F. E. Marshall (NASA/GSFC), C. Pagani (U Leicester) and
D. M. Palmer (LANL) report on behalf of the Swift Team:

At 03:50:43 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 141121A (trigger=619182).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 122.668, +22.225 which is 
   RA(J2000) = 08h 10m 40s
   Dec(J2000) = +22d 13' 31"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty). The BAT light curve shows no significant structure,
as usual for an image trigger. 

The XRT began observing the field at 03:56:45.6 UT, 362.4 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 122.6700, 22.2177 which is equivalent to:
   RA(J2000)  = +08h 10m 40.80s
   Dec(J2000) = +22d 13' 03.7"
with an uncertainty of 4.8 arcseconds (radius, 90% containment). This
location is 27 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

The initial flux in the 2.5 s image was 6.07e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 370 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 A. Y. Lien (amy.y.lien 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: GRB141121A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17076
SUBJECT: GRB141121A: BOOTES-2/TELMA upper limit
DATE:    14/11/21 06:26:08 GMT
FROM:    Juan Carlos Tello at IAA-CSIC  <jtello@iaa.es>

J. C. Tello (IAA-CSIC), J. Gorosabel (IAA-CSIC, UPV-EHU) and A, J.
Castro-Tirado (IAA-CSIC, ISA-UMA), on behalf of a larger collaboration,
report:

Following the detection of GRB 141121A by Swift (Lien et al., GCNC 17075),
the 0.6m TELMA robotic telescope at the BOOTES-2 astronomical station
Malaga (Spain), responded to the GRB location in poor weather conditions
(through clouds) starting at 04:01:57 UT (i.e. 11 min postburst). The
co-add of 10 images (i-band) starting at 04:06:03 UT and ending in 04:17:17
UT (i.e. 16-27min post burst) (60s integrations) provides an upper limit of
i > 16.5 for any object within the Swift/XRT error box. Further
observations are planned.


GRB_name: GRB141121A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17077
SUBJECT: GRB 141121A: MAXI/GSC detection
DATE:    14/11/21 06:31:44 GMT
FROM:    H. Negoro at Nihon U.  <negoro@phys.cst.nihon-u.ac.jp>

F. Honda, K. Fukushima, H. Negoro (Nihon U.), N. Kawai (Tokyo Tech), S. Nakahira (JAXA), 
M. Serino (RIKEN), S. Ueno, H. Tomida, M. Kimura, M. Ishikawa, Y. E. Nakagawa (JAXA), 
T. Mihara, M. Sugizaki, M. Morii, J. Sugimoto, T. Takagi, A. Yoshikawa, M. Matsuoka (RIKEN), 
Y. Tachibana, T. Yoshii (Tokyo Tech), 
A. Yoshida, T. Sakamoto, Y. Kawakubo, H. Ohtsuki (AGU), 
H. Tsunemi, D. Uchida (Osaka U.), 
M. Nakajima, T. Onodera, K. Suzuki, T. Namba, M. Fujita (Nihon U.), 
Y. Ueda, M. Shidatsu, T. Kawamuro, T. Hori (Kyoto U.), Y. Tsuboi, A. Kawagoe (Chuo U.), 
M. Yamauchi, Y. Morooka, D. Itoh (Miyazaki U.), K. Yamaoka (Nagoya U.)

We report the MAXI/GSC detection of GRB 141121A (Li et al. GCN 17075). 
The MAXI/GSC detected the source in the scan transit at 2014-11-21T03:44:47 (UT),
earlier than about 6 min before the BAT trigger.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (122.928 deg, 22.053 deg) = (08 11 42, +22 03 10) (J2000) 
with a statistical 90% C.L. elliptical error region 
with long and short radii of 0.44 deg and 0.4 deg respectively. 
The roll angle of long axis from the north direction is 174.0 deg counterclockwise. 
There is an additional systematic uncertainty of 0.1 deg (90% containment radius).
This position is consistent with that reported as GRB 141121A.

The X-ray flux averaged over the scan was 57 +- 17 mCrab (4-10keV, 1 sigma error).
There was no significant excess flux in the previous transit at UT 00:39. 
and in the next transit at 05:17 UT with an upper limit of 20 mCrab for each.
A simple power-law fit to the GSC spectrum gives a power-law index of 2.3 +/- 1.0.

These nature implies that the source is a long-GRB, or a new X-ray transient.
The followup observations are strongly encouraged to reveal the nature of the source.


GRB_name: GRB141121A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17078
SUBJECT: GRB 141121A: GROND Afterglow candidate
DATE:    14/11/21 07:15:06 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

M. Tanga (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 141121A (Swift trigger 619182; A. Y. Lien et
al., GCN 17075) simultaneously in g'r'i'z'JHK with GROND (Greiner et al.
2008, PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La Silla
Observatory (Chile).

Observations started at 05:52 UT on November 21, 2014, 2.02 hours after
the GRB trigger. They were performed at an average seeing of 1".4 and at
an average airmass of 2.3.

Within the XRT error circle reported by Lien et al., we detect a bright
source in all bands. This source is not detected in the SDSS, therefore we
consider it to be the afterglow of GRB 141121A. The source lies at:

RA (J2000) = 08:10:40.62
Dec. (J2000) = +22:13:01.8

with an error of 0".3 in each coordinate.

Based on total exposures of 7.7 minutes in g'r'i'z' and 8.0 minutes in
JHK, at a midtime of 2.34 hrs after the burst, we measure the following
preliminary magnitudes (AB magnitude system):

g' = 20.0 +/- 0.1 mag,
r' = 19.8 +/- 0.1 mag,
i' = 19.6 +/- 0.1 mag,
z' = 19.4 +/- 0.1 mag,
J = 19.4 +/- 0.2 mag, and
H = 19.2 +/- 0.2 mag.

The magnitudes are calibrated against SDSS and 2MASS field stars and are
not corrected for the Galactic foreground extinction corresponding to a
reddening of E_(B-V)= 0.05 in the direction of the burst (Schlegel et al.
1998).


GRB_name: GRB141118A
Detection_method: iPTF
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17079
SUBJECT: GRB 141118A: iPTF Optical Observations
DATE:    14/11/21 07:37:46 GMT
FROM:    Leo Singer at CIT/PTF  <lsinger@caltech.edu>

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

We searched for optical counterparts of GRB 141118A (GCN 17073, Hurley
et al.; GCN 17074, Golenetskii et al.) using the Palomar 48-inch Oschin
telescope (P48). At about 18 hours after the burst, we began imaging 20
fields spanning an area of 145 deg2, covering most of the 1-sigma
statistical+systematic region of the final Fermi GBM localization (Fermi
trigger 438020153 / 141118678). Based on the GBM localization, we estimate
a 77% chance that these fields contain the true location of the source.
Coincidentally, we estimate the same containment probability based on the
IPN error box.

Sifting through candidate variable sources using image subtraction and
standard iPTF vetting procedures, we detect the optical transient
iPTF14hvs, at the coordinates:
  RA(J2000)  =  10h 26m 05.29s (156.522055 deg)
  Dec(J2000) = +18d 34' 08.6"  (+18.569044 deg)
This position is just inside the error box. It is also in the outskirts of
the galaxy SDSS J102605.09+183411.6, which has a photoZ of ~0.1. In host-
subtracted P48 photometry, we find marginal evidence that the source faded:
  +18.41 hours:  R = 19.92 +/- 0.14
  +19.06 hours:  R = 20.03 +/- 0.08
Times are relative to the GBM trigger. Magnitudes are in the Mould R filter
and in the AB system, calibrated with respect to point sources in SDSS as
described in Ofek et al. (2012, http://dx.doi.org/10.1086/664065).

We obtained a series of spectra of iPTF14hvs with the Gemini Multi-Object
Spectrograph mounted on the 8 m Gemini North telescope beginning at 15:21
UT on 2014 Nov 11. The spectra cover the wavelength range of 3900-9200 A.
Cross-correlation with a library of supernova spectra using the
"Supernova Identification'' code (SNID; Blondin and Tonry 2007, ApJ 666,
1024) indicates the source is a type Ia supernova several weeks past
maximum light at z ~ 0.11. Spatially offset from the transient location we
identify narrow emission lines of H-alpha, [N II], and [S II] at a common
redshift of z = 0.108.

We conclude that iPTF14hvs is not related to the GRB.

The diagram http://www.its.caltech.edu/~lsinger/iptf/Fermi438020153.pdf
shows our P48 fields and the location of the optical transient in relation
to the Fermi GBM 1- and 2-sigma statistical+systematic contours and the
IPN annulus.

We thank the IPN team for promptly sharing their analysis.


GRB_name: GRB141121A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17080
SUBJECT: GRB 141121A: Enhanced Swift-XRT position
DATE:    14/11/21 10:50:36 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 1073 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 141121A, 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 = 122.66947, +22.21741 which is equivalent
to:

RA (J2000): 08h 10m 40.67s
Dec (J2000): +22d 13' 02.7"

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

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

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


GRB_name: GRB141121A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17081
SUBJECT: GRB 141121A: Keck redshift
DATE:    14/11/21 12:23:41 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley, C. P. Ott (Caltech), M. Modjaz, and D. Fierroz (NYU) report:

We acquired a spectrum of the afterglow of GRB 141121 (Lien et al., GCN 
17075; Tanga et al., GCN 17078) using the Low-Resolution Imaging 
Spectrometer (LRIS) on the Keck I 10-meter telescope.  A single exposure 
of 900 seconds was acquired using the B600 and R400 gratings, covering a 
wavelength range from 3116 to 10264 Angstroms.

In the reduced spectrum, we identify the Mg II (2796,2803) doublet, the 
Fe II (2599) doublet, Fe II (2585), and Fe II (2344) at a common 
redshift of z=1.47 (as well as many absorption lines at bluer 
wavelengths).  No higher-redshift absorption systems are observed and no 
DLA is present down to the blue limit of our spectrum (suggesting an 
upper limit of z<1.56) so we associate this with the redshift of the GRB.


GRB_name: GRB141121A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17082
SUBJECT: GRB 141121A: LCO-FTN observations
DATE:    14/11/21 12:46:18 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

S. Dichiara and C. Guidorzi (U. Ferrara) on behalf of
a large collaboration report:

The Las Cumbres Observatory 2-m Faulkes Telescope North in
Hawaii began observing Swift GRB 141121A (Lien et al. GCN
Circ 17075) on November 21 at 10:42:54 UT, i.e. ~6.9 hours
after the BAT trigger, with the r' and i' filters.

We clearly detect the optical afterglow (Tanga et al.
GCN 17078; Perley et al. GCN 17081) with the following
magnitudes:

Mid time from  Total Exp   Filter    Magnitude
trigger (hr)   (s)
-------------------------------------------------
7.0            120x5       r'        19.62 +- 0.06
7.2            120x5       i'        19.42 +- 0.06
-------------------------------------------------

Magnitudes are calibrated against nearby SDSS stars.
Compared with GROND values we note a possible hint
for rebrightening or, in any case, for a very shallow
decay between the two epochs.


GRB_name: GRB141121A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17083
SUBJECT: GRB 141121A: Swift-BAT refined analysis
DATE:    14/11/21 14:40:09 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.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 (GSFC/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):

Using the data set from T-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 141121A (trigger #619182)
(Lien, et al., GCN Circ. 17075).  The BAT ground-calculated position is
RA, Dec = 122.665, 22.206 deg which is
    RA(J2000)  =  08h 10m 39.5s
    Dec(J2000) = +22d 12' 22.5"
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 32%.

The mask-weighted light curve shows a very broad multi-peaked structure with the 
first emission episode running from T-50 to T+450 sec, with at least four 
superimposed peaks.  Then there is a return to baseline followed by another 
episode from T+550 to T+675 sec. The spacecraft slewed away from the burst 
position at around T+825 sec. T90 (15-350 keV) is 549.9 +- 37.4 sec (estimated 
error including systematics).

The time-averaged spectrum from T+46.54 to T+663.07 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.73 +- 0.13.  The fluence in the 15-150 keV band is 5.3 +- 0.4 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+230.14 sec in the 15-150 keV band
is 0.9 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/619182/BA/


GRB_name: GRB141121A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17084
SUBJECT: GRB 141121A: RATIR Optical Observations
DATE:    14/11/21 17:02:31 GMT
FROM:    Alan M. Watson at Instituto de Astronomia UNAM  <alan@astro.unam.mx>

Alan M. Watson (UNAM), Nat Butler (ASU), Alexander Kutyrev (GSFC), William H.
Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB), J.

Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (ORAU/GSFC),
Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC), JosÃ©
A. de Diego (UNAM), Leonid Georgiev (UNAM), JesÃºs GonzÃ¡lez (UNAM), Carlos
RomÃ¡n-ZÃºÃ±iga (UNAM), Neil Gehrels (GSFC), and Harvey Moseley (GSFC) report:

We observed the field of GRB 141121A (Lien et al., GCN 17075) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the 1.5m
Harold Johnson Telescope at the Observatorio AstronÃ³mico Nacional on Sierra San
Pedro MÃ¡rtir from 2014/11 21.33 to 2014/11 21.53 UTC (4.00 to 8.84 hours after
the BAT trigger), obtaining a total of 3.78 hours exposure in the r, i and z
bands.

For a source within the Swift-XRT error circle, in comparison with the SDSS DR9,
we obtain the following detections:


r 19.62 +/- 0.02
i 19.45 +/- 0.02
z 19.76 +/- 0.12

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

Over the course of our observations, the flux in r and i fades slightly as
t^-0.15, with t measured from the time of the BAT trigger. Our measurements in z
are noisier, but consistent with this shallow decay.

We confirm this as the afterglow reported by Tanga et al. (GCN 17078) and
Dichiara et al. (GCN 17082), for which Perley et al. (GCN 17081) report a
spectroscopic redshift of 1.47.

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

The RATIR team congratulates the Swift team on 10 years of operation.


GRB_name: GRB141121A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17085
SUBJECT: GRB 141121A: Swift/UVOT Detections
DATE:    14/11/21 19:03:15 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and A. Y. Lien (GSFC/UMBC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 141121A
371 s after the BAT trigger (Lien et al., GCN Circ. 17075).
A source consistent with the optical position
(Tanga et al. GCN Circ. 17078)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
   RA  (J2000) =  08:10:40.63 = 122.66928 (deg.)
   Dec (J2000) =  22:13:02.2  =  22.21728 (deg.)
with an estimated uncertainty of 0.5 arcsec. (radius, 90% confidence).

The source shows an unusual light curve with little evidence for variability.
The source is detected in all UVOT filters although the detections in v and w2
are not highly significant. 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              371          520          147        >20.1
white             6067         6266          197         20.2 +/- 0.2
v                  527          547           19        >18.3
v                15373        16025          635         20.3 +/- 0.3
b                 5862         6062          197         19.8 +/- 0.2
u                 5562         5714          149         19.4 +/- 0.2
u                27756        28325          556         19.3 +/- 0.1
w1                3830         3897           66         19.4 +/- 0.3
w1               26850        27750          886         19.7 +/- 0.1
m2               21039        21939          886         20.4 +/- 0.2
w2                9514        12083          771         21.2 +/- 0.3

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.05 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB141121A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17086
SUBJECT: GRB 141121A: Swift-XRT refined Analysis
DATE:    14/11/22 00:08:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 7.3 ks of XRT data for GRB 141121A (Lien  et al. GCN
Circ. 17075),  from 355 s to 58.1 ks after the BAT trigger. The data
comprise 305 s in Windowed Timing (WT) mode (the first 5 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Evans et
al. (GCN Circ. 17080).

The late-time light curve (from T0+3.8 ks) can be modelled with a
series of power-law decays. The initial decay index is alpha=1.50
(+/-0.13). At T+15.8 ks  the decay steepens to an alpha of 4.3 (+1.2,
-0.7) before breaking again at T+25.6 ks to a final decay with index
alpha=0.1 (+0.6, -1.5).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.52 (+/-0.04). The
best-fitting absorption column is  6.2 (+/-1.0) x 10^21 cm^-2, at a
redshift of 1.47, in addition to the Galactic value of 4.3 x 10^20
cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index
of 1.93 (+/-0.12) and a best-fitting absorption column of 3.9 (+2.2,
-2.0) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV
flux conversion factor deduced from this spectrum  is 3.4 x 10^-11 (4.1
x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 4.3 x 10^20 cm^-2
Intrinsic column:    3.9 (+2.2, -2.0) x 10^21 cm^-2 at z=1.47
Photon index:      1.93 (+/-0.12)

If the light curve continues to decay with a power-law decay index of
0.1, the count rate at T+24 hours will be 0.032 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x
10^-12 (1.3 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/00619182.

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


GRB_name: GRB141121A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17087
SUBJECT: GRB 141121A: Continued RATIR Optical Observations
DATE:    14/11/23 07:05:41 GMT
FROM:    Alan M. Watson at Instituto de Astronomia UNAM  <alan@astro.unam.mx>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC),
William H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB),
Ori Fox (UCB), J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino
Cucchiara (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 141121A (Lien et al., GCN 17075) 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 2014/11 22.28 to 2014/11 22.53 UTC (26.79
to 32.94 hours after the BAT trigger), obtaining a total of 4.93 hours
exposure in the r, i and z bands.

For a source within the Swift-XRT error circle, in comparison with the SDSS
DR9, we
obtain the following detections and upper limits (3-sigma):

 r 20.84 +/- 0.03
 i 20.68 +/- 0.03
 z > 20.02

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 r and i by 1.2 magnitudes or roughly t^-0.73 since
our observations on the first night (Watson et al., GCN 17084), confirming
that it is the afterglow. This fading is steeper than the t^-0.15 fading
seeing during our observations on the first night.

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


GRB_name: GRB141121A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17088
SUBJECT: GRB 141121A: MITSuME Akeno Optical observation
DATE:    14/11/23 11:44:55 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

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

We observed the field of GRB 141121A (Lien et al., GCN Circular #17075) with the 
optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm
telescope of Akeno Observatory, Yamanashi, Japan.

The observation started on 2014-11-21 12:59:47 UT (~9 h after the burst).
We detected the previously reported optical afterglow (Tanga et al., GCN Circular #17078) in the g',Rc and Ic band.

The measured magnitudes are listed below.

T0+[sec]  MID-UT  T-EXP[sec]    g'                Rc             Ic
----------------------------------------------------------------------
32947      17:07:07  12840     20.8 +/- 0.2  19.7 +/- 0.1  19.4 +/- 0.2
----------------------------------------------------------------------
T0+ : Elapsed time after the burst 
T-EXP: Total Exposure time 
We used GSC2.3 catalog for flux calibration.


GRB_name: GRB141121A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17089
SUBJECT: GRB 141121A: AAO optical observations
DATE:    14/11/23 13:36:48 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of GRB 141121A (Lien et al., GCN 17075) with AS-32 
(0.7m) telescope of Abastumani Observatory. Observations were performed 
under mean seeing (FWHM) of 3.5". We obtained several unfiltered images 
on Nov. 21 starting on (UT) 20:01:35.  Within enhanced XRT position 
(Evans et al., GCN 17080) we clearly detected  afterglow of GRB 141109A 
(Tanga et al., GCN 17078; Perley et al., GCN 17081). Preliminary 
photometry is following:

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

2014-11-21 20:01:35  0.73241     clear   54*120  20.08 0.05

The photometry is based on several SDSS-DR9 stars R magnitudes 
transformed from SDSS-DR9 based on Lupton transformations:

SDSS_id                 R(Lupton)
J081028,70+221318,9     16,317
J081049,68+221012,2     17,148
J081048,76+220822,7     14,413
J081106,66+221346,9     14,626


GRB_name: GRB141121A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17090
SUBJECT: GRB 141121A: Continued RATIR Optical Observations - Rebrightening
DATE:    14/11/23 16:20:16 GMT
FROM:    Alan M. Watson at Instituto de Astronomia UNAM  <alan@astro.unam.mx>

Alan M. Watson (UNAM), Nat Butler (ASU), Alexander Kutyrev (GSFC),
William H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB),
Ori Fox (UCB), J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino
Cucchiara (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 141121A (Lien et al., GCN 17075) 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 2014/11 23.31 to 2014/11 23.54 UTC (51.53
to 57.18 hours after the BAT trigger), obtaining a total of 3.80 hours
exposure in the r, i and z bands.

For a source within the Swift-XRT error circle, in comparison with the
SDSS DR9, we obtain the following detections:

 r = 20.60 +/- 0.03
 i = 20.44 +/- 0.03
 z = 20.06 +/- 0.29

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

The afterglow appears to have rebrightened by about 0.24 magnitudes in
r and i compared to our observations at 30 hours (Butler et al., GCN
17087).

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


GRB_name: GRB141121A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17091
SUBJECT: GRB 141121A: MITSuME Ishigakijima Optical Observation
DATE:    14/11/24 01:39:20 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

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

We observed the field of GRB 141121A (Lien et al., GCNC 17075)
with the optical three color (g', Rc and Ic) CCD camera attached
to the Murikabushi 1m telescope of Ishigakijima Astronomical
Observatory.

The observation started on 2014-11-23 17:42:18 UT (~2.6 days after the burst).
We detected the previously reported afterglow (Tanga et al., GCNC 17078;
Perley et al., GCNC 17081) in all the three bands.

Photometric results of the OT are listed below.
We used SDSS-DR7 catalog for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]  g'    g'_err  Rc    Rc_err  Ic    Ic_err
--------------------------------------------------------------------------
2.61049    18:29:49    4800.0    21.02 0.08    20.44 0.07    19.64 0.09
--------------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB141121A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17092
SUBJECT: GRB 141121A: LCO-FTN rebrightening confirmation
DATE:    14/11/24 09:58:43 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

S. Dichiara and C. Guidorzi (U. Ferrara) on behalf of
a large collaboration report:

The Las Cumbres Observatory 2-m Faulkes Telescope North in
Hawaii re-observed Swift GRB 141121A (Lien et al. GCN
Circ 17075) on November 23 at 10:43:39 UT, i.e. ~2.29 days
after the BAT trigger, with the r' and i' filters.

We confirm the rebrightening of the optical afterglow
reported by RATIR (Watson et al. GCN 17090) with the
following magnitudes:

Mid time from  Total Exp   Filter    Magnitude
trigger (days)  (s)
-------------------------------------------------
2.31           120x10       r'        20.61 +- 0.04
2.29           120x10       i'        20.34 +- 0.05
-------------------------------------------------

Magnitudes are calibrated against nearby SDSS stars.
Observations are going on.


GRB_name: GRB141121A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17093
SUBJECT: GRB 141121A: Mondy optical observations
DATE:    14/11/24 16:56:28 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of GRB 141121A (Lien et al., GCN 17075) with 
AZT-33IK telescope of Sayan observatory (Mondy) on Nov., 23  starting on 
(UT) 20:57:39.  We obtained several  images in R-filter. In a combined 
image we clearly  detect optical  afterglow (Tanga et al., GCN 17078; 
Perley et al., GCN 17081).

A preliminary photometry is based on nearby SDSS  stars:

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

2014-11-23 20:57:39   2.74025  R        39*120  20.53 0.04

We confirm re-brightening of the afterglow reported early (Watson et al. 
GCN 17090; Kuroda et al. GCN  17091; Dichiara  et al. GCN 17092).


GRB_name: GRB141118A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17094
SUBJECT: GRB 141118A: Fermi GBM Detection
DATE:    14/11/24 17:54:58 GMT
FROM:    Peter Jenke at MSFC  <peter.a.jenke@nasa.gov>

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

"At 16:15:50.31 on November 18 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 141118A (trigger 438020153/141118678).
The GBM on-ground location, using the Fermi GBM trigger
data, is RA = 158.1, Dec = 19.8 (J2000 degrees, equivalent to 
10h 32m 24s, 19d 48'), with an uncertainty of 2.2 
degrees (radius, 1-sigma containment,statistical 
only; there is additionally a systematic error which is
currently estimated to be 2 to 3 degrees).  
GBM's location is consistent with the IPN 
Triangulation (K. Hurley et al. 2014, GCN 17073). 

This GRB was also detected by Konus-Wind  (Golenetskii et al. GCN 17074).

A follow-up search of GBM's error box by iPTF 
produced an optical candidate, well within 
the GBM 1 sigma confidence region, that on further 
investigations turned out to be a fading SNe unrelated 
to the GRB (Singer et al. 2014, GCN 17079).

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

The GBM light curve consists of a single peak with a duration
(T90) of about 4.4 s (50-300 keV).
The time-averaged spectrum from T0-2.9 s to T0+3.2s 
is well fit by a power law function with an exponential 
high-energy cutoff.  The power law index is -0.77 +/- 0.09
and the cutoff energy, parameterized as Epeak, is 286 +/- 34 keV. 
The event fluence (10-1000 keV) in this time interval is
(3.3 +/- 0.2)E-06 erg/cm^2. The 1 sec peak photon flux measured
starting from T0+0.0 s in the 10-1000 keV band
is 6.5 +/- 0.3 ph/s/cm^2.


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


GRB_name: GRB141124A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17095
SUBJECT: GRB141124A: MASTER Detection of New Flare of QSO NVSS J075043+790917 During the Fermi Error Box inspection
DATE:    14/11/24 17:57:33 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

V.Krushinsky, I.Zalozhnih,  A. Popov
Ural Federal University, Yekaterinburg, Kourovka

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

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

MASTER OT J075043.33+790917.1 - new flare of QSO NVSS J075043+790917 = 
MASTER OT J075042.60+790918.2

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Tunka was starting survey on the FERMI  GRB141124A (GBM 
trigger  number 438503903 ) error-box   2286 sec after notice time and 
15886 sec after trigger time at 2014-11-24 11:03:07 UT.

During the inspection of the Fermi error box MASTER-Tunka
auto-detection system discovered OT source at (RA, 
Dec) = 07h 50m 43.33s +79d 09m 17.1s on 2014-11-24.62164 UT. The OT 
unfiltered magnitude is 17.5m (limit 18.4m). The OT is seen in 3 images. 
There is no minor planet at this place. We have reference image without OT 
on 2010-11-13.70064 UT with unfiltered magnitude limit 21.2m.

The OT is a new flare of quasar NVSS J075043+790917 that was previously 
detected by MASTER-Amur on 2013-04-26.694 UT as MASTER OT 
J075042.60+790918.2 (see ATel #5044, S. Shurpakov et al.). The object is 
marginally visible on the Blue Palomar plate with jmag=22.31 in GSC 2.3.2. 
There is an infrared counterpart AllWISE J075043.29+790917.1 
(W1=14.05+/-0.03 W2=13.01+/-0.03 W3=9.53+/-0.03 W4=7.20+/-0.09). This area 
of sky is not covered by SDSS and CRTS. Color-combined DSS finder chart is 
uploaded to http://master.sai.msu.ru/static/OT/J075043+790917-BRIR.jpg 
(10'x10' FOV).

We note that in our previous observations of this field by MASTER-Tunka on 
2014-10-26.644 UT (by the coincidence, also during Fermi error box 
inspection for trigger number 436028617) the object was marginally 
detected at ~18.5m. Multi-wavelength follow up observations are required.

The discovery and reference images are available at: 
http://master.sai.msu.ru/static/OT/075043.33790917.1.png

The inspection map of Fermi error box is available at: 
http://master.sai.msu.ru/static/OT/1468936236.png

The message may be cited.


GRB_name: GRB141121A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17096
SUBJECT: GRB 141121A: RATIR Optical Observations - Fading Again
DATE:    14/11/24 18:04:30 GMT
FROM:    Alan M. Watson at Instituto de Astronomia UNAM  <alan@astro.unam.mx>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC),
William H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB),
Ori Fox (UCB), J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino
Cucchiara (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 141121A (Lien et al., GCN 17075) 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 2014/11 24.27 to 2014/11 24.53 UTC (74.70
to 80.86 hours after the BAT trigger), obtaining a total of 4.93 hours
exposure in the r, i, and z band.

For a source within the Swift-XRT error circle, in comparison with the
SDSS DR9, we obtain the following detections and upper limits
(3-sigma):

r = 20.68 +/- 0.03
i = 20.51 +/- 0.04
z > 20.48

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

The afterglow has faded by about 0.08 magnitudes in r and i compared
to our observations at 54 hours (Watson et al., GCN 17090). This
corresponds to a shallow decay close to t^-0.2. Thus, the
rebrightening reported by Watson et al. (GCN 17090) and confirmed by
Dichiara et al. (GCN 17092) appears to have ended.

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


GRB_name: GRB141124A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17097
SUBJECT: GRB 141124Aâ€‹: iPTF upper limitsâ€‹
DATE:    14/11/24 18:38:42 GMT
FROM:    Varun Bhalerao at IUCAA  <varunb@iucaa.ernet.in>

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

We searched for optical counterparts of GRB 141124A
â€‹ (GCN Notice http://gcn.gsfc.nasa.gov/other/438503903.fermi)
 using the Palomar 48-inch Oschin telescope (P48). At about 18 minutes
after the burst, we began imaging 30 fields spanning an area of 2
â€‹12â€‹
 deg2, covering most of the 1-sigma statistical+systematic region of the
initial Fermi GBM localization, as well as about half of the 1-sigma
statistical + systematic region of the final Fermi GBM localization (Fermi
trigger 438503903 / 141124277). Based on the GBM localization, we estimate
a
â€‹44%
 chance that these fields contain the true location of the source.

Sifting through candidate variable sources using
â€‹
image subtraction and standard iPTF vetting procedures, we detected the
â€‹ â€‹
following optical transient candidates
â€‹:â€‹


iPTF14ihm
RA (J2000) 08:22:15.03 (125.562634 deg)
Dec (J2000) +74:50:00.5 (+74.833477 deg)
Consistent with stellar source, photometry does not show rapid evolution.

iPTF14ihn
RA (J2000) 10:36:56.79 (159.236626 deg)
Dec (J2000) +71:10:52.0 (+71.181099 deg)
Likely high proper motion star, photometry does not show rapid evolution.

iPTF14iho
RA (J2000) 09:45:09.42 (146.289253 deg)
Dec (J2000) +74:20:12.1 (+74.336707 deg)
Near undocumented galaxy, photometry does not show rapid evolution.

iPTF14ihp
RA (J2000) 10:54:59.28 (163.746991 deg)
Dec (J2000) +68:11:53.5 (+68.198184 deg)
Photometry shows decline over 60-minute period, but the image subtraction
residuals are centered on a stellar source in the reference image. This is
most likely a galactic variable.

â€‹We conclude that we have not detected the optical afterglow of GRB
141124Aâ€‹.


GRB_name: GRB141121A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17098
SUBJECT: GRB 141121A: MITSuME Ishigakijima Optical Observation after 3 days
DATE:    14/11/25 01:46:25 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

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

We observed the field of GRB 141121A (Lien et al., GCNC 17075)
with the optical three color (g', Rc and Ic) CCD camera attached
to the Murikabushi 1m telescope of Ishigakijima Astronomical
Observatory.

The observation started on 2014-11-24 17:17:04 UT (~3.6 days after the burst).
We detected the previously reported afterglow (Tanga et al., GCNC 17078;
Perley et al., GCNC 17081; Kuroda et al., GCNC 17091) in all the three bands.

Photometric results of the OT are listed below.
We used SDSS-DR7 catalog for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]  g'    g'_err  Rc    Rc_err  Ic    Ic_err
--------------------------------------------------------------------------
3.60810    18:26:22    5100.0    21.39 0.13    20.37 0.08    19.90 0.12
--------------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB141121A
Detection_method: AMI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17099
SUBJECT: GRB 141121A: AMI 15 GHz detection
DATE:    14/11/25 17:31:36 GMT
FROM:    Gemma Anderson at U of Oxford  <gemma.anderson@astro.ox.ac.uk>

G. E. Anderson, R. P. Fender, T. D. Staley (University of Oxford), 
A. J. van der Horst (University of Amsterdam), A. Rowlinson (CASS)

We observed the position of GRB 141121A (Lien et al., GCN 17075)
at 15 GHz with the Arcminute Microkelvin Imager (AMI-LA) starting on 
2014 Nov 24.17 to 24.33 UT, corresponding to 3 days post-burst. We 
have detected a radio source coincident with the optical counterpart 
(Tanga et al., GCN 17078) with a preliminary flux of 0.46 +/- 0.05 mJy.

Earlier observations were conducted on 2014 Nov 21.16 to 21.25 UT and 
Nov 22.05 to 22.21 UT, corresponding to <6 minutes and 0.9 days post-burst,
yielding a 3 sigma flux upper limit of 0.26 mJy and a marginal detection of 
0.18 +/- 0.06 mJy, respectively.

Further AMI monitoring is planned. We thank the AMI staff for scheduling these observations.


GRB_name: GRB141121A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17100
SUBJECT: GRB 141121A: RATIR Optical Observations - Steeper Fading
DATE:    14/11/25 18:21:54 GMT
FROM:    Alan M. Watson at Instituto de Astronomia UNAM  <alan@astro.unam.mx>

Alan M. Watson (UNAM), Nat Butler (ASU), Alexander Kutyrev (GSFC),
William H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB),
Ori Fox (UCB), J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino
Cucchiara (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 141121A (Lien et al., GCN 17075) 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 2014/11 25.27 to 2014/11 25.54
UTC (98.75 to 105.00 hours after the BAT trigger), obtaining a total of
4.58 hours exposure in the r, i, and z bands.

For a source within the Swift-XRT error circle, in comparison with the
SDSS DR9, we obtain the following detections and upper limits (3-sigma):

 r = 20.96 +/- 0.04
 i = 20.75 +/- 0.04
 z > 19.93

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

The afterglow has faded by about 0.25 magnitudes in r and i compared to
our observations at 78 hours (Butler et al., GCN 17096). This
corresponds to a steepening of the temporal power law from t^-0.2
between 54 and 78 hours (Butler et al., GCN 17096) to t^-0.9 between 78
and 102 hours.

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


GRB_name: GRB141121A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17101
SUBJECT: GRB 141121A: Continued RATIR Optical Observations
DATE:    14/11/26 16:47:33 GMT
FROM:    Alan M. Watson at Instituto de Astronomia UNAM  <alan@astro.unam.mx>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC),
William H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori
Fox (UCB), J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino
Cucchiara (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 141121A (Lien et al., GCN 17075) 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 2014/11 26.31 to 2014/11 26.53
UTC (123.55 to 128.80 hours after the BAT trigger), obtaining a total of
4.04 hours exposure in the r, i and z bands.

For a source within the Swift-XRT error circle, in comparison with the
SDSS DR9, we obtain the following detections and upper limits (3-sigma):

r = 21.27 +/- 0.04
i = 21.04 +/- 0.04
z > 21.04

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

The afterglow has faded by about 0.3 magnitudes in r and i compared to
our observations at 102 hours (Watson et al., GCN 17100). This
corresponds to a further steepening of the temporal power law from
t^-0.9 between 78 and 102 hours (Watson et al., GCN 17100) to t^-1.3
between 102 and 126 hours.

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


GRB_name: GRB141121A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17102
SUBJECT: GRB 141121A: Continued Mondy optical observations
DATE:    14/11/26 22:52:46 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of GRB 141121A (Lien et al., GCN 17075) with 
AZT-33IK telescope of Sayan observatory (Mondy) on Nov., 26  starting on 
(UT) 20:16:58.  We obtained several  images in R-filter. In a combined 
image we clearly  detect optical  afterglow (Tanga et al., GCN 17078; 
Perley et al., GCN 17081).

A preliminary photometry is based on nearby SDSS  stars:

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

2014-11-26 20:16:58   5.7120   R        39*120  21.38 0.09

The magnitude of the afterglow decreased about 0.9 mag since our 
previous observation (Mazaeva et al., GCN 17093) at 2.74 days after the 
burst trigger and thus we confirm gradual steepening of the afterglow 
light curve (Butler et al., GCN 17101).


GRB_name: GRB141121A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17103
SUBJECT: GRB 141121A: TSHAO optical observations
DATE:    14/11/27 00:21:38 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), I. Reva (Fesenkov Astrophysical Institute), A. Kusakin 
(Fesenkov Astrophysical Institute), E. Mazaeva (IKI), A. Pozanenko (IKI) 
report on behalf of larger GRB follow-up collaboration:

We observed the field of GRB 141121A (Lien et al., GCN 17075)
with  Zeiss-1000 (East) 1-m telescope of Tien Shan Astronomical
Observatory  starting on Nov. 22 (UT) 21:45:26.  We obtained several 
images in R-filter. In a combined image we clearly  detect optical 
afterglow (Tanga et al., GCN 17078; Perley et al., GCN 17081).

A preliminary photometry is based on nearby SDSS DR9 stars:

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

2014-11-22 21:45:26   1.8093    R       26*300  20.88  0.03


GRB_name: GRB141121A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17104
SUBJECT: GRB 141121A: WSRT radio detection
DATE:    14/11/27 13:34:17 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 141121A afterglow at 4.9 GHz with
the Westerbork Synthesis Radio Telescope at November 26 22.54 UT to
November 27 09.34 UT, i.e. 5.78 - 6.23 days after the burst (GCN 17075).
We detect a radio source with a flux density of 0.17 +/- 0.04 mJy
at the position of the optical counterpart (GCN 17078).

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


GRB_name: GRB141121A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17105
SUBJECT: GRB 141121A: Continued RATIR Optical Observations
DATE:    14/11/27 16:16:55 GMT
FROM:    Alan M. Watson at Instituto de Astronomia UNAM  <alan@astro.unam.mx>

Alan M. Watson (UNAM), Nat Butler (ASU), Alexander Kutyrev (GSFC), William H.
Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB), J.
Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (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 141121A (Lien et al., GCN 17075) 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 2014/11 27.31 to 2014/11 27.54 UTC (147.50 to 153.22 hours
after the BAT trigger), obtaining a total of 4.62 hours exposure in the r, i and
z bands.

For a source within the Swift-XRT error circle, in comparison with the SDSS DR9,
we obtain the following detections:

r = 21.59 +/- 0.04
i = 21.39 +/- 0.04
z = 20.89 +/- 0.26

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

The afterglow has faded by about 0.33 magnitudes in r and i compared to our
observations at 126 hours (Butler et al., GCN 17101). This corresponds to a
further steepening of the temporal power law from t^-1.3 between 102 and 126
hours (Watson et al., GCN 17100) to t^-1.8 between 126 and 150 hours.

We detect a source 2.3 arcsec to the east of the optical transient, with r =
23.22 +/- 0.13, i = 23.11 +/- 0.13, and z > 21.02. This source is visible in
earlier images, but due to its proximity to the brighter optical transient our
automatic pipeline failed to produce photometry for it from those earlier
images. We expect better photometry for this source once the afterglow has faded
further.

For a flat universe with H0 = 70 km/s/Mpc and OmegaM = 0.29, and at a redshift
of 1.47 (Perley et al., GCN 17081) the angular separation of the afterglow and
this source corresponds to a projected separation of 20 kpc. This separation is
consistent with the source being the host galaxy of the GRB.

If this source is the host galaxy, our photometry suggests that it is among the
brightest ever observed at this redshift for optically bright GRBs (Hjorth et
al. 2012, ApJ, 756, 187; Perley et al. 2013, ApJ, 778, 128).

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


GRB_name: GRB141121A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17106
SUBJECT: GRB 141121A: three epochs of SAO RAS optical observations
DATE:    14/11/27 18:23:54 GMT
FROM:    Vladimir Sokolov at SAO RAS  <sokolov@sao.ru>

A.S. Moskvitin and V.N. Komarova report on behalf of a larger team:

We observed the field of GRB 141121A (Lien et al., GCN 17075)
with the SAO RAS 1-m Zeiss-1000 telescope at three nights:
2014.11.24/25, 25/26, 26/27.

The GRB OT (Tanga et al., GCN 17078) is clearly detected
in our stacked frames each night. Our charts can be found at
ftp://ftp.sao.ru/pub/grb/GRB141121A/GRB141121A_z1000_24_25_26.jpg

We used nearby SDSS stars for calibration. The "ugriz" magnitudes
were converted to "UBVRI" with the Lupon-2005 equations. Our OT
brightness measurements are in good agreement with R-band values
estimated within the close epochs and reported in the GCN circulars:
Kuroda et al. (GCN 17098), Mazaeva et al. (GCN 17102). Our OT
magnitudes are also similar to r-band measurements by Watson et al.
(GCN 17100) and Butler et al. (GCN 17101).
Our preliminary results are presented in the following table:
-----------------------------------------------------
Date   T-T0  UT_start-end Exp.,s  R_mag
-----------------------------------------------------
24.942 3.782 20:14--00:59  900 20.31+/-0.09
25.956 4.796 22:16--23:38 3600 20.86+/-0.04
26.980 5.820 22:12--00:50 4800 21.36+/-0.09
-----------------------------------------------------


GRB_name: GRB141125A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17107
SUBJECT: IPN Triangulation of GRB 141125A (short/hard)
DATE:    14/11/27 18:32:37 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,

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

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

A short-duration, hard-spectrum GRB 141125A has been observed by 
Konus-Wind, INTEGRAL (SPI-ACS), MESSENGER (GRNS), and Swift (BAT), so 
far, at about 12781 s UT (03:33:01). 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:
    127.910 (08h 31m 38s) -29.874 (-29d 52' 28")
   Corners:
    127.504 (08h 30m 01s) -30.527 (-30d 31' 36")
    127.358 (08h 29m 26s) -31.092 (-31d 05' 29")
    128.315 (08h 33m 16s) -29.209 (-29d 12' 33")
    128.465 (08h 33m 52s) -28.616 (-28d 36' 57")
   ---------------------------------------------
The error box area is 857 sq. arcmin, and its maximum
dimension is 2.65 deg (the minimum one is 7 arcmin).
The Sun distance was 97 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB141125_T12782/IPN/

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


GRB_name: GRB141121A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17109
SUBJECT: GRB 141121A: RATIR Optical and NIR Observations
DATE:    14/11/28 16:04:21 GMT
FROM:    Alan M. Watson at Instituto de Astronomia UNAM  <alan@astro.unam.mx>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William H.
Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB), J.
Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (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 141121A (Lien et al., GCN 17075) 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 2014/11 28.29 to 2014/11 28.54 UTC (171.20 to 177.06 hours
after the BAT trigger), obtaining a total of 4.62 hours exposure in the r, i,
and z bands.

For a source within the Swift-XRT error circle, in comparison with the SDSS DR9,
we obtain the following detections and upper limits (3-sigma):

r = 21.87 +/- 0.05
i = 21.62 +/- 0.05
z > 21.03

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

Compared to our previous observations (Butler et al., GCN 17101; Watson et al.,
GCN 17105), the afterglow continues to fade roughly as t^-1.7.

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


GRB_name: GRB141121A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17110
SUBJECT: GRB 141121A: SPI-ACS/INTEGRAL observations
DATE:    14/11/28 18:10:04 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI), P. Minaev (IKI),  V. Vybornov (IKI), A. Volnova 
(IKI), E. Mazaeva (IKI)  report:

We inspected the SPI-ACS data  of INTEGRAL observatory covering trigger 
time of the Swift GRB 141121A (Lien et al., GCN 17075) and MAXI/GSC 
(Honda et al., GCN 17077). At the BAT/Swift trigger time of the GRB 
141121A (UT) T0=03:50:43 we do not found any significant emission above 
background in SPI-ACS data in different time scales (0.05 s, 5 s, and 50 
s).  We also do not find any activity at the second BAT episode (T0+550 
s to T0+675 s).

At the time of about T0-800 s we found in SPI-ACS data the activity 
corresponding to the first Konus-Wind episode (Golenetskii et al., GCN 
17108). The duration of the activity is about 200 s and clearly visible 
in SPI-ACS light curve. The start time of the maximal count rate of 
SPI-ACS light curve (binning with 50 s bin duration) is T0-725 s. In 
both cases TO and T0-725 s the boresight of SPI-ACS is the same and 
equal to 119 degrees. If this episode is related to the GRB 141121A and 
taking into account SPI-ACS energy threshold (>~ 80 keV) one can suggest 
the this episode of GRB 141121A is harder than main activity detected by 
BAT/Swift.

We do not detect any significant activity at the time of the MAXI/GSC 
detection (Honda et al., GCN 17077).

The SPI-ACS light curves can be found at

http://grb.rssi.ru/GRB141121A/grb141121_spi-acs_50sec.png
http://grb.rssi.ru/GRB141121A/grb141121_spi-acs_5sec.png


GRB_name: GRB141121A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17111
SUBJECT: GRB 141121A: Mondy optical observations
DATE:    14/11/28 19:21:59 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), 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 141121A (Lien et al., GCN 17075) with 
AZT-33IK telescope of Sayan observatory (Mondy) on Nov., 27  starting 
(UT) 19:13:37.  We obtained several  images in R-filter ander favorable 
weather and mean FWHM of 1.8 arcsec. In a combined image we clearly 
detect optical  afterglow (Tanga et al., GCN 17078; Perley et al., GCN 
17081). We do not detect the nearby source reported in (Watson et al., 
GCN 17075). Instead of we detect a Source (possible host?) 3 arcsec to 
the West from OT. The Source is absent in SDSS DR9. Coordinates of the 
OT and the Source are

OT
(J2000)
08 10 40.55 +22 13 03.0
with accuracy of  0.4" in both coordinates

The Source to the West
(J2000)
08 10 40.35 +22 13 03.0
with accuracy of  0.5" in both coordinates

Astrometry solutions are based on USON-B1.0 catalog.

A preliminary photometry of the OT is based on nearby SDSS  stars:

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

2014-11-27 19:13:37   6.6923   R        72*120  21.57 0.05

And preliminary photometry of the Source is R 22.95 Â± 0.11.
The source is barely visible in our earlier observations (Mazaeva et 
al., GCN 17102) and photometry of the early observation reported in 
(Mazaeva et al., GCN 17102) might be biased of this Source.

The finding chart can be found in
http://grb.rssi.ru/GRB141121A/GRB141121A.Mondy_host_chart.png


GRB_name: GRB141121A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17112
SUBJECT: IPN Triangulation of GRB 141121A (initial episode)
DATE:    14/11/28 20:00:34 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,

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

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

The possible initial emission episode of GRB 141121A reported by
Konus-Wind (Golenetskii et al., GCN Circ. 17108) has been also observed 
by INTEGRAL (SPI-ACS) and MESSENGER (GRNS) at about 13083 s UT 
(03:38:03; =T0(BAT)-760 s), so far.

We have triangulated it to a INTEGRAL-MESSENGER annulus centered at 
RA(2000)=46.543 deg (03h 06m 10s)  Dec(2000)=+16.630 deg (+16d 37' 49"), 
whose radius is 71.291 +/- 0.356 deg (3 sigma).

The distance between the Swift-XRT position of GRB 141121A (Evans et 
al., GCN Circ. 17080) and the central line of the annulus is 32 arcsec, 
which strengthen the association of the episode with GRB 141121A.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB141121A/IPN/


GRB_name: GRB141121A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17113
SUBJECT: GRB 141121A: Khureltogot optical observations
DATE:    14/11/28 22:40:39 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of We observed the field of GRB 141121A (Lien et 
al., GCN 17075) with ORI-40 telescope of Khureltogot observatory. We 
obtained several images in R-filter on Nov. 21 starting on (UT) 
17:07:01.  In a combined image we marginally detect optical afterglow 
(Tanga et al., GCN 17078; Perley et al., GCN 17081). Preliminary 
photometry is following and based on nearby SDSS DR9 stars:

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


2014-11-21  17:07:01  0.5977     R      120*60  19.0  0.3


GRB_name: GRB141121A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17114
SUBJECT: GRB 141121A: MITSuME Ishigakijima Optical Observation after 7 days
DATE:    14/11/29 02:41:50 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

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

We observed the field of GRB 141121A (Lien et al., GCNC 17075)
with the optical three color (g', Rc and Ic) CCD camera attached
to the Murikabushi 1m telescope of Ishigakijima Astronomical
Observatory.

The observation started on 2014-11-28 15:13:00 (~7.5 days after the burst).
We detected the previously reported afterglow (Tanga et al., GCNC 17078;
Perley et al., GCNC 17081; Kuroda et al., GCNC 17091) in g' and Rc bands.

Three sigma upper limit and photometric results of the OT are listed below.
We used SDSS-DR7 catalog for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]  g'    g'_err  Rc    Rc_err  Ic
--------------------------------------------------------------------------
7.50078    15:51:50    2400.0    21.9  0.3     21.0  0.2     >20.5
--------------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB141121A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17116
SUBJECT: GRB 141121A: Continued RATIR Optical Observations
DATE:    14/11/29 16:15:21 GMT
FROM:    Alan M. Watson at Instituto de Astronomia UNAM  <alan@astro.unam.mx>

Alan M. Watson (UNAM), Nat Butler (ASU), Alexander Kutyrev (GSFC), William H.
Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB), J.
Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (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 141121A (Lien et al., GCN 17075) 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 2014/11 29.29 to 2014/11 29.53 UTC (195.13 to 200.87 hours
after the BAT trigger), obtaining a total of 4.62 hours exposure in the r, i and
z bands.

For a source within the Swift-XRT error circle, in comparison with the SDSS DR9,
we obtain the following detections and upper limits (3-sigma):

  r = 22.15 +/- 0.06
  i = 21.97 +/- 0.06
  z > 21.04

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

The afterglow continues to fade with a steepening temporal index.

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


GRB_name: GRB141121A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17117
SUBJECT: GRB 141121A: TSHAO optical observations
DATE:    14/11/29 18:03:22 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), A. Kusakin (Fesenkov Astrophysical Institute), A. 
Volnova (IKI), I. Reva (Fesenkov Astrophysical Institute),  A. Pozanenko 
(IKI) report on behalf of larger GRB follow-up collaboration:

We observed the field of GRB 141121A (Lien et al., GCN 17075)
with  Zeiss-1000 (East) 1-m telescope of Tien Shan Astronomical
Observatory  starting on Nov. 26 (UT) 22:12:24.  We obtained several 
images in R-filter. In a combined image we clearly  detect optical 
afterglow (Tanga et al., GCN 17078; Perley et al., GCN 17081).

A preliminary photometry is based on nearby SDSS DR9 stars:

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

2014-11-26 22:12:24   5.8118    R       14*300  21.48 0.09


GRB_name: GRB141121A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17118
SUBJECT: GRB 141121A: Mondy optical observations
DATE:    14/11/30 14:40:57 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of GRB 141121A (Lien et al., GCN 17075) with 
AZT-33IK telescope of Sayan observatory (Mondy) Nov., 29  starting on 
(UT) 20:20:38.  We obtained several  images in R-filter under 
unfavorable seeing. In a combined image we detect optical  afterglow 
(Tanga et al., GCN 17078; Perley et al., GCN 17081).

A preliminary photometry of the OT is based on nearby SDSS DR9 stars:

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

2014-11-29 20:20:38   8.7458   R        84*120  22.03 0.17

Due to bad seeing the photometry above includes both afterglow and 
possible host (Watson et al., GCN 17105; Mazaeva et al., GCN 17111).


GRB_name: GRB141121A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17119
SUBJECT: GRB 141121A: Continued RATIR Optical Observations
DATE:    14/11/30 17:27:01 GMT
FROM:    Alan M. Watson at Instituto de Astronomia UNAM  <alan@astro.unam.mx>

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William H.
Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB), J.
Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (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 141121A (Lien et al., GCN 17075) 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 2014/11 30.28 to 2014/11 30.54 UTC (218.99 to 225.08 hours
after the BAT trigger), obtaining a total of 4.98 hours exposure in the r, i and
z bands.

For a source within the Swift-XRT error circle, in comparison with the SDSS DR9,
we obtain the following detections and upper limits (3-sigma):

r = 22.32 +/- 0.07
i = 22.14 +/- 0.07
z > 21.00

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: GRB141130A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17120
SUBJECT: GRB 141130A: Swift detection of a burst with an optical counterpart
DATE:    14/11/30 23:26:54 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

A. Vargas (PSU), S. D. Barthelmy (GSFC),
H. A. Krimm (CRESST/GSFC/USRA), D. Malesani (DARK/NBI),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL) and
B. Sbarufatti (INAF-OAB/PSU) report on behalf of the Swift Team:

At 23:10:56 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 141130A (trigger=620090).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 222.814, +47.300 which is 
   RA(J2000)  =  14h 51m 15s
   Dec(J2000) = +47d 17' 60"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single peak
structure with a duration of about 35 sec.  The peak count rate
was ~1200 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 23:12:20.3 UT, 84.3 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
222.8205, 47.3202 which is equivalent to:
   RA(J2000)  = 14h 51m 16.92s
   Dec(J2000) = +47d 19' 12.7"
with an uncertainty of 2.8 arcseconds (radius, 90% containment). This
location is 74 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 1.82
x 10^20 cm^-2 (Willingale et al. 2013). 

The initial flux in the 2.5 s image was 8.27e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of nominal 150.000 seconds with the White
filter starting 93 seconds after the BAT trigger. There is a candidate
afterglow in the list of sources generated on-board at
  RA(J2000)  = 14:51:17.28 = 222.82199
  DEC(J2000) = +47:19:07.5  =  47.31876
with a 90%-confidence error radius of about 1.10 arc sec. This position is 4.1
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.74. No correction has been made for the expected extinction corresponding to
E(B-V) of 0.02. 

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


GRB_name: GRB141130A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17121
SUBJECT: GRB 141130A: Mondy optical observations
DATE:    14/12/01 00:28:33 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of GRB 141130A (Vargas et al., GCN  17120) with 
AZT-33IK telescope of Sayan observatory (Mondy) Nov., 30  starting on 
(UT) 23:15:04, i.e 248 s after burst trigger. In first images of 10 s 
exposure we clearly detect fading object in coordinates of the OT 
candidate reported in  (Vargas et al., GCN  17120). The object is absent 
in DSS2 and we thus confirm optical afterglow of GRB 141130A.  The 
afterglow has faded from R = 18.5 +/- 0.14 at 258 s after burst trigger 
to R = 19.2 +/- 0.2 at 800 s  after burst trigger.

The photometry is stil preiminary and based on nearby USNO-B1.0 stars.


GRB_name: GRB141130A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17122
SUBJECT: GRB 141130A: Nanshan optical observations
DATE:    14/12/01 00:51:28 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

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

We observed the field of GRB 141130A (Vargas et al., GCN  17120) with
the 1m optical telescope located at Nanshan, Xinjiang, China.
Observations started at 23:36:49 UT on 2014-10-30 (i.e., 1553 s after
the burst) and a series of 120s, 180s, and 360s R-band images were
obtained under some clouds. We detect the optical afterglow at the
UVOT position with R~19.1 mag at the median time of 1982 s post-burst,
calibrated with four nearby SDSS stars (SDSS J145120.41+471920.1, SDSS
J145118.89+471810.3, SDSS J145125.69+471701.0, and SDSS
J145114.11+471610.1).


GRB_name: GRB141130A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17123
SUBJECT: GRB 141130A: Enhanced Swift-XRT position
DATE:    14/12/01 02:22:11 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 621 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 141130A, 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 = 222.82159, +47.31852 which is equivalent
to:

RA (J2000): 14h 51m 17.18s
Dec (J2000): +47d 19' 06.7"

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: GRB141121A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17124
SUBJECT: GRB 141121A: VLA radio detection
DATE:    14/12/01 05:54:12 GMT
FROM:    Alessandra Corsi at Texas Tech U  <alessandra.corsi@ttu.edu>

A. Corsi (Texas Tech U.) reports on behalf of a larger collaboration:

We imaged the position of GRB 141121A (Lien et al., GCN 17075) with the Karl G. Jansky 
Very Large Array (VLA), at a mean epoch of about 8.4 days after the burst. We detect the 
radio afterglow of GRB 141121A (Anderson et al., GCN 17099; van der Horst, GCN 17104) 
at a position consistent with the optical counterpart (Tanga et al., GCN 17078). At this time, 
we estimate a preliminary flux of about 207 uJy at 14 GHz. The map rms is about 5 uJy.


GRB_name: GRB141130A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17125
SUBJECT: GRB 141130A: Swift-XRT refined Analysis
DATE:    14/12/01 11:27:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 11 ks of XRT data for GRB 141130A (Vargas  et al. GCN
Circ. 17120),  from 75 s to 28.5 ks after the  BAT trigger. The data
comprise 327 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 Goad et al.
(GCN Circ. 17123).

The late-time light curve (from T0+4.9 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.14 (+0.26, -0.25).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.31 (+0.07, -0.06). The
best-fitting absorption column is  1.50 (+0.17, -0.16) x 10^21 cm^-2,
in excess of the Galactic value of 1.8 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.13 (+0.25, -0.21)
and a best-fitting absorption column of 3.8 (+4.7, -2.0) x 10^20 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.1 x 10^-11 (3.4 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.8 (+4.7, -2.0) x 10^20 cm^-2
Galactic foreground: 1.8 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.13 (+0.25, -0.21)

If the light curve continues to decay with a power-law decay index of
1.14, the count rate at T+24 hours will be 1.8 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.5 x
10^-14 (6.2 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/00620090.

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


GRB_name: GRB141130A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17126
SUBJECT: GRB 141130A: Swift/UVOT Detection
DATE:    14/12/01 13:26:52 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

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

The Swift/UVOT began settled observations of the field of
GRB 141130A 95 s after the BAT trigger (Vargas et al., GCN
Circ. 17120).  A source consistent with the XRT position
(Goad et al. GCN Circ. 17123)  is detected in the initial UVOT
exposures.

The preliminary UVOT position is:
    RA  (J2000) =  14:51:17.23 = 222.82181 (deg.)
    Dec (J2000) = +47:19:07.3  =  47.31870 (deg.)
with an estimated uncertainty of 0.45 arc sec. (radius, 90% confidence).

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

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

white               95          244          147         18.71 +/- 0.06
v                  636          655           19        >17.8
b                  562          753           39        >20.1
u                  306          556          246         18.85 +/- 0.13
w1                 684          704           19        >18.7
w2                 611          798           34        >19.0

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).

[GCN OPS NOTE(01dec14):  Per author's request, the "A" was added
to the GRB name.]


GRB_name: GRB141130A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17127
SUBJECT: GRB 141130A: Swift-BAT refined analysis
DATE:    14/12/01 13:29:51 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (LANL), A. Vargas (PSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+962 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 141130A (trigger #620090)
(Vargas, et al., GCN Circ. 17120).  The BAT ground-calculated position is
RA, Dec = 222.804, 47.323 deg which is 
   RA(J2000)  =  14h 51m 13.0s 
   Dec(J2000) = +47d 19' 24.3" 
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 73%.
 
The mask-weighted light curve shows the burst starting at ~T-43 sec, going
flat until ~T-10 sec, then peaking at ~T-2 sec, and then returing
to baseline ~T+60 sec.  T90 (15-350 keV) is 62.9 +- 11.4 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-42.75 to T+40.02 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.56 +- 0.08.  The fluence in the 15-150 keV band is 2.8 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-4.69 sec in the 15-150 keV band
is 1.2 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/620090/BA/


GRB_name: GRB141121A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17128
SUBJECT: GRB 141121A: Continued RATIR Optical Observations
DATE:    14/12/01 16:07:08 GMT
FROM:    Alan M. Watson at Instituto de Astronomia UNAM  <alan@astro.unam.mx>

Alan M. Watson (UNAM), Nat Butler (ASU), Alexander Kutyrev (GSFC), William H.
Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB), J.
Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (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 141121A (Lien et al., GCN 17075) 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 2014/12 1.30 to 2014/12 1.54 UTC (243.35 to 249.19 hours after
the BAT trigger), obtaining a total of 4.56 hours exposure in the r, i, and z
bands.

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

r = 22.38 +/- 0.16
i = 22.21 +/- 0.16
z > 20.41

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

Compared to our observations on previous nights (Watson et al., GCN 17116;
Butler et al., GCN 17119), the fading appears to be slowing and is now behaving
as t^-0.5. This may be evidence for an underlying host galaxy more closely
coincident with the GRB than the candidate reported by Watson et al. (GCN
17105).

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


GRB_name: GRB141030A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17129
SUBJECT: GRB 141030A: Nanshan very early optical observations
DATE:    14/12/01 21:41:57 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

D. Xu (DARK/NBI), X. Gao (Urumqi No.1 Senior High School, Xinjiang),
Z.-J. Xu (Nanjing Putian Telecommunications Co. Ltd., Jiangsu) report:

We observed the field of GRB 141130A (Vargas et al., GCN  17120) with
the 36cm robotic telescope located at Nanshan, Xinjiang, China.
Observations started at 23:12:44 UT on 2014-10-30, i.e., 108 s after
the burst, and subsequently 4x40s, 8x60s, and 10x90s R-band images
were obtained under some floating clouds.

The optical afterglow, at the UVOT position, is clearly detected in
the stacked 4x40s image, with R=17.67+/-0.20 mag at a median time of
201 s post-burst, against the same four SDSS stars in Xu et al. (GCN
17122). The afterglow is not detected any more in the subsequent
images down a limit of R~18 mag. This is consistent with the
measurement of R~18.5 mag at 258 s after post-burst in Mazaeva et al.
(GCN 17121).


GRB_name: GRB141130A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17130
SUBJECT: GRB 141130A: Mondy optical light curve
DATE:    14/12/01 22:16:19 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We report optical light curve of the GRB 141130A (Vargas et al., GCN 
17120) based on our observations with AZT-33IK telescope of Sayan 
observatory (Mondy) on  Nov., 30 (Mazaeva et al., GCN 17121).

The light curve can be found in 
http://grb.rssi.ru/GRB141130A/GRB141130A_AZT33IK_lc.png

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


GRB_name: GRB141202A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17131
SUBJECT: IPN Triangulation of GRB 141202A (short/hard)
DATE:    14/12/03 12:02:29 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

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

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

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

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

The short-duration, hard-spectrum GRB 141202A has been observed by Fermi 
(GBM trigger 439211828), MESSENGER (GRNS), INTEGRAL (SPI-ACS), 
Konus-Wind, and Swift (BAT), so far, at about 40626 s UT (11:17:06). 
This burst occurred just after Swift started a preplanned slew maneuver. 
There are no BAT event data covering the burst interval, but from the 
energy response of the quadrant rates, it appears that the source was 
partially coded in BAT.

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   143.073 (09h 32m 17s) +54.161 (+54d 09' 38")
  Corners:
   142.732 (09h 30m 56s) +52.555 (+52d 33' 17")
   143.092 (09h 32m 22s) +53.247 (+53d 14' 51")
   143.397 (09h 33m 35s) +55.706 (+55d 42' 22")
   143.039 (09h 32m 09s) +55.054 (+55d 03' 15")
  ---------------------------------------------
The error box area is 1439 sq. arcmin, and its maximum
dimension is 3.2 deg (the minimum one is 10 arcmin).
The Sun distance was 117 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB141202_T40626/IPN/

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


GRB_name: GRB141202A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17132
SUBJECT: GRB 141202A Tiled Swift observations
DATE:    14/12/03 13:24:03 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 141202A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00033

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: GRB141202A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17133
SUBJECT: GRB 141202A: Fermi GBM Detection
DATE:    14/12/03 13:53:27 GMT
FROM:    Oliver Roberts at UCD/Fermi  <oliver.roberts@ucd.ie>

O.J. Roberts (UCD) reports on behalf of the Fermi GBM Team:

"At 11:17:05.61 UT on the 2nd of December 2014, the
Fermi Gamma-Ray Burst Monitor triggered and located
GRB 141202A (trigger 439211828 / 141202470 ). The
GBM on-ground location, using the Fermi GBM trigger
data, is RA = 145.0, Dec =+59.9, with an uncertainty of
3.3 degrees (radius, 1-sigma containment,statistical only;
there is additionally a systematic error which is currently
estimated to be 2 to 3 degrees). The GBM location is
consistent with the IPN Triangulation (Golenetskii et al.
2014, GCN 17131).

The angle from the Fermi LAT boresight is about
78 degrees.

The GBM light curve consists of a single peak with a
duration (T90) of about 1.3 s (50-300 keV). The
time-averaged spectrum from T0+0.0 s to T0+1.3 s is
adequately fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.11 +/- 0.08
and the cutoff energy, parameterized as Epeak, is
596 +/- 40 keV.

The event fluence (10-1000 keV) in this time interval is
(4.2 +/- 0.2)E-06  erg/cm^2. The 1-sec peak photon flux
measured starting from T0+0.1 s in the 10-1000 keV band
is 8.4 +/- 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: GRB141202A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17134
SUBJECT: GRB 141202A: Swift XRT observations 
DATE:    14/12/04 13:27:51 GMT
FROM:    Claudio Pagani at U of Leicester  <cp232@star.le.ac.uk>

C. Pagani and  P. A. Evans (U. Leicester) report on behalf of the Swift team:

Swift-XRT has observed the error box of the IPN GRB 141202A (Golenetskii et al., GCN Circ. 17131) in a series of observations tiled on the sky. The total exposure time is 12.3 ks spread over 7 fields; the maximum exposure within the sky observed was 2.7 ks. The observations started 93.5 ks after the IPN trigger and extended over ~50.8 ks.

Within these data no credible X-ray afterglow is detected. The 3-sigma upper limit is 5.2E-03 cts s^-1 (0.3-10 keV). The automated analysis of the XRT data detects three X-ray sources that are classified as possible afterglow candidates, but inspection of the data shows these to be artifacts due to contamination by the bright Earth.

The automated analysis is reported online at http://www.swift.ac.uk/xrt_products/TILED_GRB00033

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


GRB_name: GRB141130A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17135
SUBJECT: GRB 141130A: Mondy optical observations
DATE:    14/12/04 16:46:27 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), 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 141130A (Vargas et al., GCN  17120) with 
AZT-33IK telescope of Sayan observatory (Mondy) Dec., 01  starting on 
(UT) 21:21:55. We obtained several  images in R-filter. In a combined 
image we do not detect optical  afterglow (Vargas et al., GCN  17120; 
Mazaeva et al., GCN 17121; Xu et al., GCN 17122).


Upper limit  is based on nearby USNO B1.0 (R2) stars:

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

2014-12-01 21:21:55   0.95417  R        43*120  n/d   22.1


The finding chart can be found in
http://grb.rssi.ru/GRB141130A/GRB141130_20141201_AZT33IK_fc.png


GRB_name: GRB141202A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17136
SUBJECT: Konus-Wind observation of GRB 141202A
DATE:    14/12/04 18:01:42 GMT
FROM:    Anastasia Tsvetkova at Ioffe Institute  <tsvetkova@mail.ioffe.ru>

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

The short-duration, hard-spectrum GRB 141202A
(IPN triangulation: Golenetskii et al., GCN 17131;
Fermi GBM detection: Roberts, GCN 17133)
triggered Konus-Wind at T0=40626.305 s UT (11:17:06.305).

The burst light curve shows a single pulse with a duration of ~1.4 s.
The emission is seen up to ~10 MeV.

As observed by Konus-Wind, the burst
had a fluence of 4.44(-1.02,+1.47)x10^-6 erg/cm2,
and a 16-ms peak flux, measured from T0+0.624 s,
of 7.37(-2.00,+2.67)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.49(-0.35,+0.47),
and Ep = 538(-150,+274) keV (chi2 = 77/84 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index:
beta < -2.0 (chi2 = 77/83 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB141202_T40626/

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


GRB_name: GRB141205A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17137
SUBJECT: GRB 141205A Short hard GRB found in ground analysis of BAT data
DATE:    14/12/05 14:51:45 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

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

At 08:05:17, BAT triggered on GRB 141205A (trigger 620534). No source was
found onboard. A significant source was found in ground analysis at
RA, Dec 92.881, +37.862, which is:

RA (J2000)   06h 11m 31.5s
Dec (J2000)  37d 51' 43"

with an estimated position uncertainty of 3 arcmin radius.

This was the same event as Fermi GBM trigger 439459520. The BAT position is
14.0 degrees from the GBM final position (4.4 degree radius 1 sigma error).

The burst was about 1 second long.

A Swift TOO has been requested.


GRB_name: GRB141121A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17138
SUBJECT: GRB 141121A: Mondy optical observations
DATE:    14/12/05 14:58:30 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), 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 continue observations of the field of GRB 141121A (Lien et al., GCN 
17075) with AZT-33IK telescope of Sayan observatory (Mondy). We obtained 
several  images in R-filter on Nov., 30, Dec. 1 - 2. In a combined image 
we detect optical  afterglow (Tanga et al., GCN 17078; Perley et al., 
GCN 17081).

A preliminary photometry of the OT is based on nearby SDSS DR9 stars:

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

2014-11-30 18:45:29    9.7139  R       119*120  22.20 0.10
2014-12-01 18:35:23   10.6644  R        72*120  22.25* 0.17
2014-12-02 18:09:52   11.6606  R        92*120  22.40* 0.25



*)Due to bad seeing the photometry  includes both afterglow and nearby 
source (Watson et al., GCN 17105; Mazaeva et al., GCN 17111).


GRB_name: GRB141202A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17139
SUBJECT: GRB 141202A: Swift/UVOT Detection of a Variable Source Near the IPN Error Box
DATE:    14/12/05 15:43:31 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and S. B. Cenko (NASA/GSFC) 
report on behalf of the Swift/UVOT team:

The short/hard GRB 141202A was localized to a 1439 sq. arcmin
error box with the IPN (Golenetskii et al. GCN Circ. 17131), and
Swift tiled the error box with 7 fields starting
93.5 ks after the trigger. No credible afterglow was detected
with the Swift/XRT (Pagani et al. GCN Circ. 17134).

In two exposures with the U filter starting 128 ks after the trigger, 
Swift/UVOT finds a bright source just outside the IPN error region
that is not seen in the DSS or the SDSS. In addition, no source at this position
was found with the Minor Planet Checker. There is a dim SDSS
galaxy with a g' magnitude (AB) of 23.0 +/- 0.2 coincident with the UVOT source.
A 3-sigma upper limit for this galaxy in the u' band is 22.4 mag.

The preliminary UVOT position is:
   RA  (J2000) =  09:32:29.78 = 143.12408 (deg.)
   Dec (J2000) =  55:19:44.4  =  55.32899 (deg.)
with an estimated uncertainty of 0.5 arcsec. (radius, 90% confidence).

There is very marginal evidence (1.8-sigma) for variability between
the two UVOT observations. The preliminary 
AB magnitudes using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) is:

Filter         T_start(ks)   T_stop(ks)    Exp(ks)        Mag (AB)

u                127.9        128.6         0.69       20.43 +/- 0.09
u                129.4        130.3         0.88       20.69 +/- 0.13

No correction is made for the Galactic extinction
due to the reddening of E(B-V) = 0.02 in the direction of the source
(Schlegel et al. 1998).

The 3-sigma upper limit for the XRT count rate at the position of the
UVOT source is 9.6e-3 counts/s in the 0.3-10 keV band.

It would be very unusual for UVOT to find a bright optical afterglow for
a short/hard GRB so long after the trigger, especially since
XRT did not find an afterglow. The long-term increase in the optical flux by
a factor of at least 6 indicates that this may nevertheless be an 
interesting object.


GRB_name: GRB141205A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17140
SUBJECT: GRB 141205A Swift-BAT refined analysis
DATE:    14/12/05 16:42:04 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

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

We report further analysis of GRB 141205A (Cummings, GCN 17137).  The best
BAT position is RA, Dec  92.859, +37.876, which is:

RA (J2000)    06 11 26.1s
Dec (J2000)  +37d 52' 32.2"

with an estimated position uncertainty of 2 arcmin radius.  The source was
41% coded in BAT.

The unweighted lightcurve shows multiple weak peaks.  T90 was 1.1 +- 0.2
seconds.

The total spectrum in  BAT is best fit by a simple power-law function with
a photon index of 0.985 +- 0.002.  The fluence in 1.4 seconds was
(1.2 +- 0.3) x 10^-7 ergs/cm^2.  Errors are 90% confidence.

Because this burst was found in ground analysis, the normal automated burst
analysis products are not available.


GRB_name: GRB141205A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17141
SUBJECT: GRB 141205A: XRT observations
DATE:    14/12/06 15:51:34 GMT
FROM:    Rhaana Starling at U of Leicester  <rlcs1@star.le.ac.uk>

R. L. C. Starling and K. L. Page (U. Leicester) report

The Swift ground-analysis-detected short/hard GRB 141205A (Cummings et al. GCN 17137, 17140) 
was observed with XRT on 2014-12-05 starting at 14:44 UT, 6.65 hours after the burst, and ending 
at 2014-12-05 at 17:55 UT.

The Photon Counting mode data comprise 4.97 ks of exposure, in which no new source is detected 
to a 3-sigma limit in the 0.3-10 keV band of 2.8e-3 count/s.

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


GRB_name: GRB141205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17142
SUBJECT: GRB 141205A: Nanshan optical upper limit
DATE:    14/12/06 16:05:50 GMT
FROM:    Dong Xu at DARK/NBI  <dong.dark@gmail.com>

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

We observed the field of GRB 141205A (Cummings, GCN 17137), using the
1m telescope located at Nanshan, Xinjiang, China. Observations were
performed between 17:26:18 UT and 21:26:52 UT on 2014-12-05, and a
series of R-band 120s/200s exposures were obtained. No credible
uncatalogued optical transient was found within the BAT error circle
(Markwardt et al., GCN 17140), down to a limiting magnitude of R~20.4
mag.


GRB_name: GRB141205A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17143
SUBJECT: GRB 141205A: Fermi GBM detection
DATE:    14/12/06 18:59:08 GMT
FROM:    Oliver Roberts at UCD/Fermi  <oliver.roberts@ucd.ie>

O.J. Roberts (UCD) reports on behalf of the Fermi GBM Team:

"At 08:05:17.49 UT on the 5th of December 2014, the Fermi
Gamma-Ray Burst Monitor triggered and located GRB 141205A
(trigger 439459520 / 141205337 ), which was also detected by
Swift (Cummings et al. 2014, GCN 17137). The GBM on-ground
location, using the Fermi GBM trigger data, is consistent
with the Swift location.

The angle from the Fermi LAT boresight is about 123 degrees.

The GBM light curve consists of a single peak with a duration
(T90) of about 1.5 s (50-300 keV). The time-averaged spectrum
from T0-0.26 s to T0+1.3 s is adequately fit by a power law
function with an exponential high-energy cutoff. The power law
index is -0.23 +/- 0.39  and the cutoff energy, parameterized
as Epeak, is 525 +/- 164 keV.

The event fluence (10-1000 keV) in this time interval is
(1.1 +/- 0.2)E-06  erg/cm^2. The 1-sec peak photon flux
measured starting from T0-0.1 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: GRB141205A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17144
SUBJECT: GRB 141205A: Swift/UVOT Upper Limits
DATE:    14/12/06 20:27:00 GMT
FROM:    Margaret Chester at PSU  <chester@swift.psu.edu>

M. M. Chester (PSU), F. E. Marshall (NASA/GSFC), and
R. L. C. Starling (U.Leicester) report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 141205A
23934 s after the BAT trigger (Cummings, GCN Circ. 17137).
No new sources are detected within the refined BAT error circle
(Markwardt et al. GCN Circ. 17140).  Using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373), we find the following
3-sigma upper limits at the center of the BAT error circle:

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

white            23975        28936          837         >21.7
v                24016        29758          826         >20.1
u                23934        28114          837         >20.7

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.24 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB141121A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17145
SUBJECT: GRB141121A: Discovery Channel Telescope Optical Observations
DATE:    14/12/07 21:48:55 GMT
FROM:    Vicki Toy at UMD  <vtoy@astro.umd.edu>

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

We observed the field of GRB141121A (Swift trigger 619182, Lien et al., GCN
17075) with the Large Monolithic Imager (LMI) on the 4.3m Discovery Channel
Telescope (DCT) at Happy Jack, AZ from 2014/12/07 6:44 to 2014/12/07 11:01
UTC (starting 386.1 hours after the Swift trigger). A source is clearly
detected at the location of the optical afterglow in g', r', i', and z'.
Using nearby point sources from SDSS R8 for calibration we measure i' =
23.26 +/- 0.12.

This magnitude is reported in AB magnitude and is not corrected for
Galactic extinction in the direction of the GRB.

Compared to RATIR observations on 12/01 (Watson, GCN 17128) the afterglow
has steepened to a decay index of ~ t^-2.1.  At this time we cannot confirm
if this is the host galaxy.  Further observations are planned.

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


GRB_name: GRB141207A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17146
SUBJECT: GRB 141207A: Fermi-LAT Detection
DATE:    14/12/08 06:29:49 GMT
FROM:    Daniel Kocevski at GSFC  <daniel.kocevski@nasa.gov>

M. Arimoto (Tokyo Tech), D. Kocevski (NASA/GSFC), R. Desiante (INFN Trieste & Udine University), and M. Axelsson (KTH Royal Institute of Technology, Sweden) report on behalf of the Fermi-LAT team:

At 19:11:21.10 on December 7, 2014, Fermi-LAT detected high-energy emission from GRB 141207A, which was also detected by Fermi-GBM (trigger 439672284/141207800).

The best LAT on-ground location is found to be

(RA, Dec.) = 159.99, +3.91 deg

with an error radius of 0.215 deg (90% containment, statistical error only). This position was 59 deg from the LAT boresight at the time of the trigger.

The data from the Fermi-LAT show a significant increase in the event rate within 2 degree of the GBM location after the GBM trigger that is spatially and temporally correlated with the GBM emission with high significance. More than 27 photons above 100 MeV and more than 6 photons above 1 GeV are observed within 100 seconds. The highest-energy photon is a ~5 GeV event which is observed ~750 seconds after the GBM trigger.

A Swift ToO has been requested for this burst.

The Fermi-LAT point of contact for this burst is Makoto Arimoto (arimoto@hp.phys.titech.ac.jp<mailto:arimoto@hp.phys.titech.ac.jp>).

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


GRB_name: GRB141207A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17147
SUBJECT: GRB 141207A Tiled Swift observations
DATE:    14/12/08 08:00:11 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a series of observations, tiled on the sky, of the
Fermi/LAT GRB 141207A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00034

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

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

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


GRB_name: GRB141130A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17148
SUBJECT: Konus-Wind observation of GRB 141130A
DATE:    14/12/08 13:10:46 GMT
FROM:    Anastasia Tsvetkova at Ioffe Institute  <tsvetkova@mail.ioffe.ru>

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

The long GRB 141130A (Swift-BAT trigger #620090: Vargas et al., GCN 17120;
Lien et al., GCN 17127) was detected by Konus-Wind in the waiting mode.

The burst light curve shows a double-peaked structure
with a total duration of ~85 s (from ~T0(BAT)-44 s to ~T0(BAT)+41 s).

As observed by Konus-Wind, the burst had a fluence of
8.79(-2.39,+2.62)x10^-6 erg/cm2 and a 2.944 s peak flux,
measured from ~T0(BAT)-2.725 s, of 2.40(-0.82,+0.87)x10^-7 erg/cm2/s
(both estimated in the 20 keV - 10  MeV energy range).

Modeling the KW 3-channel time-integrated spectrum
(from T0(BAT)-43.941 s to T0(BAT)+41.435 s) by a power law
with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha =-1.49 Â± 0.18,
and Ep =307(-108,+467) keV.

The K-W light curve of this burst is available at
http://www.ioffe.ru/LEA/GRBs/GRB141130A/

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


GRB_name: GRB141207A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17149
SUBJECT: GRB 141207A: Swift-XRT observations
DATE:    14/12/08 15:45:31 GMT
FROM:    Alex Amaral-Rogers at U.of Leicester  <aar14@leicester.ac.uk>

A. Amaral-Rogers & P.A. Evans (U. Leicester) report on behalf of the
Swift-XRT team:

We have observed the area around the Fermi-LAT GRB 141207A (Arimoto et
al., GCN Circ. 17146), in 4 XRT fields starting at 07:59:28 UT, 12 hours and 48 minutes after Fermi/LAT detection. With 1.3-1.7 ks per field, we find an uncatalogued X-ray source at a position of RA,Dec=160.0639,
3.8933, which is equivalent to:

RA (J2000)  = 10h 40m 15.34s
Dec (J2000) = +03d 53' 35.9"

with an uncertainty of 5.2" (radius, 90% confidence). Although this
source is uncatalogued, it is a factor of 3 below the ROSAT limit at
this location, with a 0.3-10 keV flux of 1.7e-13 erg/cm^2/s. We expect
~0.9 sources at this flux to be serendipitously present in our XRT
observations, therefore we caution that this may not be the afterglow.
We cannot currently tell whether the source is fading, but follow-up
observations are planned.

There is a second uncatalogued X-ray source present in the data, at
RA,Dec=159.8172, 4.0930 with an uncertainty of 6.5"; however this source
is coincident with the object [VV2006] J103916.6+040536 which SIMBAD
classifies as a quasar, thus it is unlikely to be the GRB afterglow.

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


GRB_name: GRB141207A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17150
SUBJECT: GRB 141207A: Fermi GBM detection
DATE:    14/12/08 17:01:18 GMT
FROM:    Eric Burns at U of Alabama  <zeq925@gmail.com>

Eric Burns (UAH) report on behalf of the Fermi GBM Team:

"At 19:11:21.10 UT on 07 December 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 141207A (trigger 439672284 / 141207800) which
was also detected by Fermi LAT (Arimoto et al. 2014, GCN 17146) and
observed by Swift (Evans 2014, GCN 17147). The GBM on-ground location
is consistent with the LAT/Swift positions.

The angle from the Fermi LAT boresight is 59 degrees.

The GBM light curve consists of a single pulse with multiple spikes,
with a duration (T90) of about 20 s (50-300 keV). The time-averaged
spectrum from T0-0.768 s to T0+24.83 s is adequately fit by a power law
function with an exponential high-energy cutoff.  The power law index is
-0.70 +/- 0.02 and the cutoff energy, parameterized as Epeak, is
1080 +/- 56 keV.

The event fluence (10-1000 keV) in this time interval is
(3.58 +/- 0.04)E-05 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+7.55 s in the 10-1000 keV band is 8.6 +/- 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: GRB141207A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17151
SUBJECT: GRB 141207A: Swift-UVOT Observations
DATE:    14/12/08 22:35:11 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

GRB 141207A: Swift-UVOT Observations

M. H. Siegel (PSU) and A. Amaral-Rogers (U. Leicester) report 
on behalf of the Swift-UVOT team:

We have observed the area around the Fermi-LAT GRB 141207A (Arimoto et
al., GCN Circ. 17146), in 4 UVOT fields starting at 07:59:28 UT, 12
hours and 48 minutes after Fermi/LAT detection. There is an optical source
at a position of RA,Dec=160.06441, 3.89477, which is
equivalent to:

RA (J2000)  = 10h 40m 15.46s
Dec (J2000) = +03d 53' 41.2

with an uncertainty of 0.1 (radius, 90% confidence).  This source is
5.6 from the position of the XRT source (Amaral-Rogers and Evans, GCN
Circ. 17149) and shows up as a marginal detection in the DSS. It is possibly
unrelated to the burst.  Follow-up observations will be needed to confirm its nature.

The preliminary u magnitude using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) is 19.91+-0.17.


GRB_name: GRB141207A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17152
SUBJECT: GRB141207A: Discovery Channel Telescope Optical Observations
DATE:    14/12/09 01:41:06 GMT
FROM:    Vicki Toy at UMD  <vtoy@astro.umd.edu>

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

We observed the field of the Fermi-LAT GRB141207A (Fermi-GBM trigger
439672284/141207800, Arimoto et al., GCN 17146; Burns et al., GCN 17150)
with the Large Monolithic Imager (LMI) on the 4.3m Discovery Channel
Telescope (DCT) at Happy Jack, AZ from 2014/12/08 11:08 to 2014/12/08 12:30
UTC (starting 16.0 hours after the Fermi trigger). We imaged 5 fields
covering the entire 90% LAT error region.  No source is detected at the
positions of the two X-ray sources reported by Amaral-Rogers and Evans (GCN
17149).  We estimate a 3-sigma upper limit of r > 23.2
(RA,Dec=160.0639,3.8933) and r > 21.3 (RA,Dec=159.8172, 4.0930).

We detect the source reported by Siegel and Amaral-Rogers (GCN 17151) with
r'=20.09+/-0.04.  We note that this coincides with a galactic SDSS source,
J104015.45+035341.0.

These magnitudes are reported in AB magnitude and are 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: GRB141202A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17153
SUBJECT: GRB141202A: Discovery Channel Telescope Optical Observations
DATE:    14/12/09 04:09:42 GMT
FROM:    John Capone at UMD  <jicapone@astro.umd.edu>

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

We observed the field of the variable source reported by Marshall and Cenko
(GCN 17139) with the Large Monolithic Imager (LMI) on the 4.3m Discovery
Channel Telescope (DCT) at Happy Jack, AZ from 2014/12/07 11:01 until
2014/12/07 11:08 UTC (starting 119.74 hours after the observations reported
by Golenetskii et al. in GCN 17131). A source is clearly detected at the
location of the source identified by UVOT in u', g', r', i' and z'. Using
nearby point sources from SDSS for calibration we measure r' = 20.57 +/-
0.03. The coincident SDSS R10 source has r' = 22.65 +/- 0.20, confirming
that the source is indeed transient. At 0.8 arcsecond seeing, the source is
unresolved.

This magnitude is reported in AB magnitude and is not corrected for
Galactic extinction in the direction of the source.

Further observations are planned to investigate possible variability of
this source.

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


GRB_name: GRB141207A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17155
SUBJECT: Konus-Wind observation of GRB 141207A
DATE:    14/12/09 15:28:39 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

The long-duration, hard-spectrum GRB 141207A (Fermi-LAT detection: 
Arimoto et al., GCN 17146; Fermi-GBM detection: Burns, GCN Circ. 17150) 
triggered Konus-Wind at T0=69081.298 s UT (19:11:21.298).

The burst light curve shows two pulses started at ~T0-2.3 s with a total 
duration of ~25 s.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB141207_T69081/

As observed by Konus-Wind, the burst
had a fluence of 4.87(-0.34,+0.38)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+6.224 s,
of 9.62(-2.26,+2.27)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+24.832 s)
is best fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.50 (-0.13,+0.14)
and Ep = 723(-72,+87) keV (chi2 = 105/98 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.6
(chi2 = 104/97 dof)

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


GRB_name: GRB141121A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17156
SUBJECT: GRB 141121A: further VLA observations
DATE:    14/12/10 03:48:36 GMT
FROM:    Alessandra Corsi at Texas Tech U  <alessandra.corsi@ttu.edu>

A. Corsi (Texas Tech U.), S.B. Cenko (NASA-GSFC), A. Cucchiara (NASA-GSFC), 
D. A. Perley (Caltech), A. Horesh (Weizmann Institute), D. A. Frail (NRAO) report:

We imaged again the the position of GRB 141121A (Lien et al., GCN 17075) with 
the Karl G. Jansky Very Large Array (VLA), at a mean epoch of about 16.3 days 
after the burst. At this time, we detect the radio afterglow of GRB 141121A 
(Anderson et al., GCN 17099; van der Horst, GCN 17104; Corsi, GCN 17124), 
and estimate a preliminary flux of about 228 uJy at 6.2 GHz and 186 uJy at 14 GHz. 
The map rms is about 9 uJy at 6.2 GHz and 7 uJy at 14 GHz. 
Further observations are planned.


GRB_name: GRB141207A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17157
SUBJECT: GRB 141207A: Swift-XRT afterglow candidate detection
DATE:    14/12/10 20:56:07 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has continued to observe the field of the Fermi-LAT GRB 141207A 
(Arimoto et al., GCN Circ. 17146). The uncatalogued X-ray source 
reported by Amaral-Rogers & Evans (GCN. Circ 17149) shows no evidence of 
fading.

An additional uncatalogued X-ray source has also been detected at 
RA,Dec=159.8547, 3.71139 degrees, which is equivalent to:

RA (J2000)  = 10h 39m 25.13s
Dec (J2000) = +03d 42' 41.0"

with an uncertainty of 4.9 arcsec (radius, 90% confidence). This source 
was initially detected with a count-rate of 0.012 +/- 0.003 ct/sec. In a 
second observation, from T0+191 ks to T0+231 s, the source has faded to 
a count-rate of 1.0 (+/-0.5) x 10^-3 ct/sec. We therefore suggest that 
this is likely the afterglow of GRB 141207A.

The PC mode spectrum of this source can be fitted with an absorbed 
power-law with a photon index of 2.1 (+1.5, -0.7). The best-fitting 
absorption column is 5.2 (+18, -4.8) x 10^21 cm^-2, consistent with the 
Galactic value of 0.4 x 10^21 cm^-2 (Willingale et al. 2013).

A summary of the PC-mode spectrum is thus:

Total column:      5.2 (+18, -4.8) x 10^21 cm^-2
Galactic foreground: 3.7 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.1 (+1,5, -0.7)

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


GRB_name: GRB141212A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17158
SUBJECT: GRB 141212A: Swift detection of a short burst
DATE:    14/12/12 12:27:37 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

T. N. Ukwatta (LANL), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), N. Gehrels (NASA/GSFC),
B.P. Gompertz (U Leicester), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester) and E. Troja (NASA/GSFC/UMCP) report on
behalf of the Swift Team:

At 12:14:01 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 141212A (trigger=621229).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 39.161, +18.151 which is 
   RA(J2000)  =  02h 36m 39s
   Dec(J2000) = +18d 09' 04"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single spike
with a duration of about 0.1 sec.  The peak count rate
was ~3200 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 12:15:10.0 UT, 69.1 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 39.1246, 18.1460 which
is equivalent to:
   RA(J2000)  = 02h 36m 29.90s
   Dec(J2000) = +18d 08' 45.7"
with an uncertainty of 3.5 arcseconds (radius, 90% containment). This
location is 125 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper.  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 1.03
x 10^21 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 72 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers none of
the XRT error circle. The 8'x8' region for the list of sources generated
on-board covers 100% of the XRT error circle. The list of sources is typically
complete to about 18 mag. No correction has been made for the expected
extinction corresponding to E(B-V) of 0.10. 

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


GRB_name: GRB141212B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17159
SUBJECT: GRB 141212B: Swift detection of a burst
DATE:    14/12/12 13:36:41 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

M. Stamatikos (OSU/NASA/GSFC), S. D. Barthelmy (GSFC),
D. N. Burrows (PSU), N. Gehrels (NASA/GSFC),
B.P. Gompertz (U Leicester), J. A. Kennea (PSU),
K. L. Page (U Leicester) and M. H. Siegel (PSU) report on behalf of
the Swift Team:

At 13:23:48 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 141212B (trigger=621234).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 250.869, +31.749 which is 
   RA(J2000)  =  16h 43m 28s
   Dec(J2000) = +31d 44' 57"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a multiple-peak
structure with a duration of about 15 sec.  The peak count rate
was ~7000 counts/sec (15-350 keV), at ~4 sec after the trigger. 

The XRT began observing the field at 13:25:13.4 UT, 85.2 seconds after
the BAT trigger. No source was detected in the 2.5-s promptly available
image. We are waiting for the full dataset to detect and localise the
XRT counterpart. 

Burst Advocate for this burst is M. Stamatikos (Michael.Stamatikos-1 AT nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB141212A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17160
SUBJECT: GRB 141212A: MITSuME Akeno upper limits
DATE:    14/12/12 13:38:41 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

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

We observed the field of GRB 141212A (T. N. Ukwatta et al. GCN Circular #17158) with the
optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan.

The observation started on 2014-12-12 12:14:32 UT (31 sec after the burst).
We did not find any new point source within XRT circle in all three bands.

The measured magnitudes are listed below.

T0+[sec]      MID-UT      T-EXP[sec]         g'           Rc           Ic
--------------------------------------------------------------------------------------
  61        12:17:29         240                    >19.6     >19.0       >18.3
  422      12:28:07         780                    >20.0      >19.6     > 18.9
  422      12:41:18        2340                  >20.5     >20.1       >19.6
--------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used GSC2.3 catalog for flux calibration.


GRB_name: GRB141212A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17161
SUBJECT: GRB 141212A: Skynet R-COP Observations
DATE:    14/12/12 15:14:45 GMT
FROM:    Adam S. Trotter at UNC-Chapel Hill/PROMPT/Skynet  <atrotter@physics.unc.edu>

A. Trotter, J. Haislip, D. Reichart, A. Verveer, T. Spuck, A. Aji, R. 
Beauchemin, T. Berger, A. Dow, A. Foster, N. Frank, M. Hinckle, K. 
Ivarsen, A. LaCluyze, M. Maples, J. Moore, M. Nysewander, C. Salemi, L. 
Zbinden, and J. A. Crain report:

Skynet observed the Swift BAT/XRT localization of GRB 141212A (Ukwatta 
et al., GCN 17158, Swift trigger=621229) with the 14" R-COP telescope at 
Perth Observatory, Australia. Starting at 2014-12-12 12:24 UT and 
continuing until 14:13 UT (t=10.2m-119m post-trigger), Skynet took a 
total of 24x160s exposures in the B, V, R, and I bands. We stacked 
subsets of these images to maximize the S/N ratio, and detected no 
optical source in any band at the XRT position.  Our 3-sigma limiting 
magnitudes are:

==================================
tmid  expos  fil  limit
==================================
87m   7x160s  B   >19.9
106m  8x160s  V   >20.5
41m   3x160s  R   >20.0
30m   2x80s   I   >18.5
==================================

Limiting magnitudes are in the Vega System, calibrated to 6 APASS stars 
in the field.  Magnitudes have not been corrected for line-of-sight 
Milky Way dust extinction, with expected E(B-V)=0.09 (Schlafly & 
Finkbeiner 2011).

No further Skynet observations are scheduled.


GRB_name: GRB141212A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17162
SUBJECT: GRB 141212A: MASTER early optical observations
DATE:    14/12/12 15:16:48 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

V.Krushinsky, I.Zalozhnih,  A. Popov
Ural Federal University, Yekaterinburg, Kourovka

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

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


MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in 
Tunka was pointed to the  GRB141212A 32 sec after notice time and 46 sec after 
trigger time at 2014-12-12 12:14:47 UT. On our first (10s exposure)  set we 
haven't found optical transient  within SWIFT error-box (Ukwatta et alo., GCN 
17158) .
The 5-sigma upper limit has been about 16.8 mag

Our upper limit on first single and coadd images available on table 1:

Table 1:


T_start     T0-T_start   T0-T_mid  Exptime  Limit Coadd
    UT           s           s         s 12:14:47.1    46            51 
10     16.8   -
12:14:47.1    46           497       630     19.2   9
12:30:24.4   983          2251      2160     20.6   12

The message may be cited.


GRB_name: GRB141212A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17163
SUBJECT: GRB 141212A: Correction to GCN  17162
DATE:    14/12/12 15:25:32 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

Vladimir lipunov (Lomonosow Moscow University)
I am sorry.
The correct representatio of the 
Table 1 is:



T_start     T0-T_start   T0-T_mid  Exptime  Limit Coadd
    UT           s           s         s
12:14:47.1    46            51        10      16.8   -
12:14:47.1    46           497       630     19.2   9
12:30:24.4   983          2251      2160     20.6   12

The message may be cited.


GRB_name: GRB141212A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17164
SUBJECT: GRB 141212A: Enhanced Swift-XRT position
DATE:    14/12/12 16:53:25 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 885 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 141212A, 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 = 39.12444, +18.14684 which is equivalent
to:

RA (J2000): 02h 36m 29.86s
Dec (J2000): +18d 08' 48.6"

with an uncertainty of 2.9 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: GRB141212B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17165
SUBJECT: GRB 141212B: Swift/XRT preliminary localization
DATE:    14/12/12 17:04:38 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@swift.psu.edu>

J. A. Kennea (PSU), K. L. Page (U Leicester) and T. N. Ukwatta (LANL) 
report on behalf of the Swift/XRT Team:

At 13:25:13.4 UT on December 12, 2014, 85.2 seconds after the BAT trigger, 
XRT began observing GRB 141212B. We find a uncatalogued source at an XRT 
count rate of 2-3 c/s during the first orbit, and 0.4 c/s during the 2nd 
orbit observations. Based on 140s of PC mode data, we find a preliminary 
localization of RA/Dec(J2000) = 250.87573, 31.752983, equivalent to:

RA(J2000)  = 16h 43m 30.1s
Dec(J2000) = 31d 45m 10.7s

with an estimated uncertainty of 10 arc-seconds radius (90% confidence). 
We expect this position to be improved as we collect more data.


GRB_name: GRB141212B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17166
SUBJECT: GRB 141212B: initial Swift/UVOT observations
DATE:    14/12/12 18:11:42 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (IAA-CSIC/UCL-MSSL), M. H. Siegel (PSU) and M. Stamatikos (OSU/NASA/GSFC) report 
on behalf of the Swift-UVOT team:

UVOT took a finding chart exposure of GRB 141212B of 127 seconds with the White filter
starting 402 seconds after the BAT trigger (trigger=621234). No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers the preliminary XRT error circle 
(Kennea et al. GCN Circ. 17165). The typical 3-sigma upper limit has been about 19.6 mag.
The 8'x8' region for the list of sources generated on-board covers 100% of the
BAT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.03. 


GRB_name: GRB141212A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17167
SUBJECT: GRB 141212A: 1.23m CAHA I-band observations
DATE:    14/12/12 18:51:16 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC/UPV-EHU), R. Sanchez-Ramirez (UPV/EHU), S. Hellmich (DLR), S. Mottola (DLR), report on behalf of a larger collaboration:

We observed the field of GRB 141212A (Ukwatta et al. GCN Circ. 17158) with the 1.23m CAHA telescope starting on  Dec 12.73309 UT (5.4 hours post bust). The observations were carried out in the I-band. No object brighter than I~21 (Vega) is detected within the XRT error circle (Osborne GCN Circ., 17164).


GRB_name: GRB141212A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17168
SUBJECT: GRB 141212A: Khureltogot optical upper limit
DATE:    14/12/12 20:09:31 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of GRB 141212A (Ukwatta et al., GCN 17158) with 
ORI-40 telescope of Khureltogot observatory. We obtained 2 hours of 
unfiltered images on Dec. 12 starting on (UT) 12:46:14.  In a combined 
image of the first 5 frames we  do not detect any optical source within 
  enhanced Swift-XRT position (Osborne et al., GCN 17164). Preliminary 
photometry is following

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


2014-12-12  12:46:14  0.02422    R       5*60   18.5


The photometry is based on USNO-B1.0 stars
USNO-B1_id      RA          DEC         R2
1081-0038366 039.120895 +18.127567 16.32 
1081-0038391 039.149945 +18.154739 17.15 
1081-0038340 039.085725 +18.167617 14.41


GRB_name: GRB141212A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17169
SUBJECT: GRB141212A: xinglong TNT upper limit
DATE:    14/12/12 21:58:48 GMT
FROM:    L.P. Xin at NAOC  <xlp@bao.ac.cn>

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

We began to observe GRB 141212A (Ukwatta eta l., GCN 17158)  
with Xinglong  0.8-m TNT telescope at 2014-12-12, 12:14:40(UT),
about 39 sec the burst.

In any single W-band frame or coadded image,  no any new 
optical transient was detected within XRT circle 
(Ukwatta eta l., GCN 17158; Osborne et al, GCN 17164 ) 
down to 3 sigma limit of R~20 mag at the mid-time of 4 min 
after the burst, calibrated by the nearby USNO B1.0 R2 mag.

The message may be cited.


GRB_name: GRB141212A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17170
SUBJECT: GRB 141212A: extended object within the XRT error circle
DATE:    14/12/12 22:18:17 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Malesani (DARK/NBI), P. D'Avanzo (INAF/OABr), V. D'Elia (INAF/OAR and 
ASI/ASDC), S. D. Vergani (CNRS/GEPI), G. Andreuzzi (INAF/TNG), A. Garcia 
de Gurtubai Escudero (INAF/TNG), A. Bonomo (INAF/OATo), report on behalf 
of the CIBO collaboration:

We observed the field of GRB 141212A (Ukwatta et al., GCN 17158) using 
the TNG optical telescope located in La Palma. Observations started on 
2014 Dec 12.832 UT (7.73 hr after the GRB) and consisted of 10x240 s in 
the R band. The PSF in our image was around 1.5".

Within the XRT error circle (Osborne et al., GCN 17164; see also 
http://www.swift.ac.uk/xrt_positions/), we detect a single, extended 
object (A), with coordinates (J2000):

RA = 02:36:29.95
Dec = +18:08:47.2

Its Vega magnitude is R = 22.66 +- 0.23, assuming R = 16.83 for the USNO 
star at RA = 02:36:35.95, Dec = +18:09:16.8.

We cannot yet make any claim about variability, so the connection of 
this object with GRB 141212A is unclear. This may be the GRB host, 
though some contribution from an afterglow cannot be excluded.

We also note the presence of two extended objects just outside the XRT 
error circle.

(B): RA = 02:36:30.25, Dec = +18:08:50.1, R = 22.29 +- 0.16;
(C): RA = 02:36:29.64, Dec = +18:08:50.2, R ~ 24.0

Object (C) is barely detected. No other sources are visibile in the 
proximity of the XRT error circle down to a limiting magnitude of R = 24.

A finding chart can be seen at the following URL: 
http://www.astro.ku.dk/~malesani/GRB/141212A/GRB141212A_TNG.jpg


GRB_name: GRB141212A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17171
SUBJECT: GRB 141212A: Swift-XRT refined Analysis
DATE:    14/12/13 00:27:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans (U. Leicester), B.P. Gompertz (U. Leicester), V. D'Elia
(ASDC), M. de Pasquale (INAF-IASFPA), A. Maselli  (INAF-IASFPA), V.
Mangano (PSU), M.C. Stroh (PSU), D.N. Burrows (PSU), J.P. Osborne (U.
Leicester) and T.N. Ukwatta report on behalf of the Swift-XRT team:

We have analysed 7.9 ks of XRT data for GRB 141212A (Ukwatta  et al.
GCN Circ. 17158),  from 77 s to 28.9 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Osborne et al. (GCN Circ. 17164).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.62 (+0.20, -0.16).


If the light curve continues to decay with a power-law decay index of
0.62, the count rate at T+24 hours will be 7.6 x 10^-4 count s^-1

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00621229.

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


GRB_name: GRB141212A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17172
SUBJECT: GRB 141212A: MITSuME Okayama upper limits
DATE:    14/12/13 00:54:34 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 141212A (Ukwatta et al., GCNC 17158)
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 2014-12-12 12:15:02 UT (~62 sec after the burst).
We did not find any new point source within the enhanced XRT circle
(Osborne et al., GCNC 17164) in all the three bands.

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

#T0+[day]  MID-UT    T-EXP[sec]   g'     Rc     Ic
-----------------------------------------------------
0.04216    13:14:42    6000.0   >20.5  >20.1  >19.4
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB141212B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17174
SUBJECT: GRB 141212B: Enhanced Swift-XRT position 
DATE:    14/12/13 02:26:39 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

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

Using 152 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 =
250.87617, 31.75045 which is equivalent to:

RA (J2000):  16 43 30.28
Dec (J2000): +31 45 01.6

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 is an official product of the Swift-XRT team.


GRB_name: GRB141212A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17175
SUBJECT: GRB 141212A: Swift-BAT refined analysis
DATE:    14/12/13 05:02:51 GMT
FROM:    Tilan Ukwatta at MSU  <tilan.ukwatta@gmail.com>

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

Using the data set from T-240 to T+962 sec from the recent
telemetry downlink, we report further analysis of BAT GRB
141212A (trigger #621229) (Ukwatta, et al., GCN Circ. 17158).
The BAT ground-calculated position is RA, Dec =
39.167, 18.163 deg which is
   RA(J2000)  =  02h 36m 40.1s
   Dec(J2000) = +18d 09' 47.1"
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90%
containment). The partial coding was 58%.

BAT light curve shows a strong FRED like peak starting
around T-0.05 sec and ending around T+0.2 sec. Another
softer peak can be seen starting at T+0.2 sec, peaking
at T+0.3 sec and ending around T+0.35 sec. T90 (15-350 keV)
is 0.30 +- 0.08 sec (estimated error including systematics).

The time-averaged spectrum from T+0.00 to T+0.34 sec is
best fit by a simple power-law model.  The power law index
of the time-averaged spectrum is 1.61 +- 0.23.  The fluence
in the 15-150 keV band is 7.2 +- 1.2 x 10^-08 erg/cm2.
The 1-sec peak photon flux measured from T-0.33 sec in
the 15-150 keV band is 1.2 +- 0.2 ph/cm2/sec.  All the
quoted errors are at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/621229/BA/


GRB_name: GRB141212B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17176
SUBJECT: GRB 141212B: Swift-BAT refined analysis
DATE:    14/12/13 05:05:43 GMT
FROM:    Tilan Ukwatta at MSU  <tilan.ukwatta@gmail.com>

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 (GSFC/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):

Using the data set from T-239 to T+459 sec from the recent
telemetry downlink, we report further analysis of BAT
GRB 141212B (trigger #621234) (Stamatikos, et al., GCN Circ.
17159). The BAT ground-calculated position is
RA, Dec = 250.866, 31.749 deg which is
   RA(J2000)  =  16h 43m 27.9s
   Dec(J2000) = +31d 44' 55.3"
with an uncertainty of 1.0 arcmin, (radius, sys+stat,
90% containment). The partial coding was 77%.

BAT light curve shows a single multi-peaked episode starting
around T+0 sec, and ending around T+15 sec. The two main
peaks of the light curve can be seen at T+5 sec and T+6 sec.
T90 (15-350 keV) is 10.5 +- 0.7 sec (estimated error
including systematics).

The time-averaged spectrum from T-0.06 to T+12.14 sec is
best fit by a simple power-law model.  The power law index
of the time-averaged spectrum is 1.46 +- 0.09.  The fluence
in the 15-150 keV band is 1.2 +- 0.1 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T+4.10 sec in the
15-150 keV band is 3.9 +- 0.3 ph/cm2/sec.  All the quoted
errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/621234/BA/


GRB_name: GRB141212A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17177
SUBJECT: GRB 141212A: Gemini-N spectroscopy and photometry
DATE:    14/12/13 07:52:21 GMT
FROM:    Ryan Chornock at Ohio U  <chornock@ohio.edu>

R. Chornock (Ohio University), W. Fong (University of Arizona), and D. B. Fox 
(Penn State) report:

We obtained imaging and spectroscopy of the field of the short GRB 141212A 
(Ukwatta et al., GCN 17158) using GMOS on the 8 m Gemini-North telescope 
starting at 04:35 UT on 13 December, 16.4 hours after the BAT trigger.
In 5x180s of i-band imaging with 0.5" seeing, all three objects found by 
Malesani et al. (GCN 17170) are well detected.  Using an archival calibration, 
we measure i=22.2 +/- 0.1 mag for object A, the extended object present inside 
the enhanced XRT error circle (Osborne et al., GCN 17164).

In addition, we oriented a spectroscopic slit through both extended objects A 
and B (using the terminology of Malesani et al.).  We obtained 2x900s of 
spectroscopy with the R400 grating covering the wavelength range 5890-10100 
Angs.  Both galaxies exhibit prominent nebular line emission from [O II], 
H-beta, and [O III].  Galaxy A, the likely host, has a redshift of z=0.596, 
while Galaxy B has a redshift of z=0.672.


GRB_name: GRB141212A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17178
SUBJECT: GRB 141212A: VLA upper limit
DATE:    14/12/13 09:52:03 GMT
FROM:    Wen-fai Fong at U of Arizona  <wfong@email.arizona.edu>

W. Fong (U. Arizona) and B. A. Zauderer (Harvard) report:

"We observed the field of the short-duration GRB 141212A (Ukwatta et al.,
GCN 17158) with the Karl G. Jansky Very Large Array (VLA) beginning on 2014
Dec 12.96 UT (10.9 hr post-burst) at a mean frequency of 6 GHz. In 1 hour
of observations, we do not detect any radio source within or around the
enhanced XRT position (Osborne et al., GCN 17164). We therefore place a
3-sigma limit of ~25 microJy on the radio afterglow of GRB 141212A at 10.9
hr after the burst.

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


GRB_name: GRB141212B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17179
SUBJECT: GRB 141212B: Swift/UVOT Upper Limits
DATE:    14/12/13 10:55:04 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (IAA-CSIC/UCL-MSSL) and M. Stamatikos (OSU/NASA/GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 141212B
403 s after the BAT trigger (Stamatikos et al., GCN Circ. 17159).
No optical afterglow consistent with the XRT position
(Page et al. GCN Circ. 17174)
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           403          530          125         >19.8
v                 3819         3975          153         >18.9

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: GRB141212A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17180
SUBJECT: GRB 141212A: Swift/UVOT Upper Limits
DATE:    14/12/13 10:59:10 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (IAA-CSIC/UCL-MSSL) and T. N. Ukwatta (LANL)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 141212A
72 s after the BAT trigger (Ukwatta et al., GCN Circ. 17158).
No optical afterglow consistent with the XRT position
(Osborne et al. GCN Circ. 17164)
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            72          222          147         >20.6
u_FC               286          535          246         >19.9
white               72         1531          392         >21.2
v                  615         1581          117         >18.8
b                  541         1681          117         >19.8
u                  286         1655          343         >20.1
w1                 664         1631          117         >19.3
w2                 591         1210           39         >18.6

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.10 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB141212B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17181
SUBJECT: GRB 141212B: Swift-XRT refined Analysis
DATE:    14/12/13 13:36:24 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

B. P. Gompertz, K. L. Page (U. Leicester) and M. Stamatikos
(OSU/NASA/GSFC) reports on behalf of the Swift-XRT team:

We have analysed 2.1 ks of XRT data for GRB 141212B (Stamatikos  et al.
GCN Circ. 17159),  from 350 s to 45.2 ks after the  BAT trigger. The
data comprise 179 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode.

The enhanced XRT position for this burst was given by Page et al. (GCN
Circ. 17174)

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.05 (+0.08, -0.06).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.1 (+0.4, -0.3). The
best-fitting absorption column is  7 (+12, -5) x 10^20 cm^-2,
consistent with the Galactic value of 2.2 x 10^20 cm^-2 (Willingale et
al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 3.0 x 10^-11 (3.6 x
10^-11) erg cm^-2 count^-1. 

A summary of the WT-mode spectrum is thus:
Total column:      7 (+12, -5) x 10^20 cm^-2
Galactic foreground: 2.2 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.1 (+0.4, -0.3)

If the light curve continues to decay with a power-law decay index of
1.05, the count rate at T+24 hours will be 7.2 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.1 x
10^-13 (2.5 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00621234.

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


GRB_name: GRB141212B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17182
SUBJECT: Konus-Wind observation of GRB 141212B
DATE:    14/12/13 14:26:25 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

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

The long-duration, weak GRB 141212B (Swift-BAT trigger #621234: 
Stamatikos et al., GCN 17159; Sakamoto et al., GCN 17176 ) triggered 
Konus-Wind at T0=48230.404 s UT (13:23:50.404).

The burst light curve shows a multipeak structure started at ~T0-6.8 s 
with a duration of ~8.0 s.
The emission is seen up to ~500 keV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB141212_T48230/

As observed by Konus-Wind, the burst
had a fluence of 1.65(-0.22,+0.38)x10^-6 erg/cm2,
and a 64-ms peak flux, measured from T0+0.014 s,
of 1.48(-0.24,+0.40)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 1 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -1.44(-0.28,+0.33)
and Ep = 150(-46,+136) keV (chi2 = 57/60 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -1.9
(chi2 = 56/59 dof)

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


GRB_name: GRB141212B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17183
SUBJECT: GRB 141212B: MITSuME Akeno upper limits
DATE:    14/12/13 17:34:14 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

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

We observed the field of GRB 141212B (M. Stamatikos et al., GCN Circular #17159) with the
optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm
telescope of Akeno Observatory, Yamanashi, Japan.

The observation started on 2014-12-12 19:31:43 UT (~6 h after the burst).
We did not find any new point source within the enhanced XRT circle 
(K. L. Page et al., GCN Circular #17174) in all the three bands.

The measured magnitudes are listed below.

T0+[sec]     MID-UT    T-EXP[sec]        g'         Rc        Ic
------------------------------------------------------------------------------
25180        20:31:06        840            >19.0  >18.8  >18.3
------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used GSC2.3 catalog for flux calibration.


GRB_name: GRB141212A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17184
SUBJECT: GRB 141212A: Zadko observatory - Gingin optical observations
DATE:    14/12/13 18:06:06 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 141212A detected by SWIFT
(trigger 621229) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 123s after the GRB trigger.
The elevation of the field increased from
37 degrees above horizon and weather conditions
were good.

We do not detect any optical counterpart of the XRT afterglow
(Ukwatta et al. GCNC 17158, Malesani et al. GCNC 17170).
We give the details of the limiting magnitudes during the
twelve first minutes after the trigger:

t0+123s to t0+153s : Rlim = 18.6
t0+162s to t0+192s : Rlim = 18.6
t0+200s to t0+230s : Rlim = 18.6
t0+239s to t0+269s : Rlim = 18.6
t0+279s to t0+309s : Rlim = 18.6
t0+320s to t0+410s : Rlim = 19.8
t0+421s to t0+511s : Rlim = 19.8
t0+522s to t0+612s : Rlim = 19.8
t0+622s to t0+712s : Rlim = 19.8

We co-added a series of exposures:
t0+123s to t0+712s : Rlim = 20.3

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


GRB_name: GRB141212A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17185
SUBJECT: GRB 141212A iTelescope observation
DATE:    14/12/16 09:09:27 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

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

We observed the field of GRB 141212A detected by Swift (trigger #621229; 
Ukwatta et al., GCN Circ. 17158) with the iTelescope.Net (http://www.itelescope.net) 
T11 (0.50 m Plane Wave) telescope located at the New Mexico Skies Observatory (NM, USA).  

4 images of 60 sec exposures were taken in the R filter starting from December 12 
12:38:28 (UT) about 24.5 minutes after the trigger and stopped on December 12 12:43:22 (UT).  
We do not detect the optical afterglow both in the individual images and the stacked 
image at the enhanced X-ray afterglow position (Osborne et al., GCN Circ. 17164).  
The estimated five sigma upper limit of the combined image (total exposure of 240 sec) 
is ~19.1 using the USNO-B1 catalog.


GRB_name: GRB141215A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17186
SUBJECT: IPN Triangulation of GRB 141215A (long/intense)
DATE:    14/12/16 17:14:48 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

K. Hurley, on behalf of the IPN,

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

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

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

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

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

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

D. M. Smith, J. McTiernan, R. Schwartz, W. Hajdas,
and A. Zehnder, on behalf of the RHESSI GRB team, report:

A long-duration, bright GRB 141215A has been observed by Fermi (GBM 
trigger 440342778), Konus-Wind, INTEGRAL (SPI-ACS), Mars-Odyssey (HEND), 
RHESSI, and Swift (BAT), so far, at about 48376 s UT (13:26:16). 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:
     179.056 (11h 56m 13s) -52.745 (-52d 44' 44")
    Corners:
     179.620 (11h 58m 29s) -52.523 (-52d 31' 22")
     178.533 (11h 54m 08s) -53.178 (-53d 10' 40")
     178.486 (11h 53m 57s) -52.965 (-52d 57' 53")
     179.570 (11h 58m 17s) -52.309 (-52d 18' 31")
    ---------------------------------------------
The error box area is 575 sq. arcmin, and its maximum
dimension is 1.1 deg (the minimum one is 10 arcmin).
The Sun distance was 68 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB141215_T48373/IPN/

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


GRB_name: GRB141215A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17187
SUBJECT: Konus-Wind observation of GRB 141215A
DATE:    14/12/16 17:20:54 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration, intense GRB 141215A
(IPN triangulation: Hurley et al., GCN 17186)
triggered Konus-Wind at T0=48373.645 s UT (13:26:13.645).

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

As observed by Konus-Wind, the burst had a fluence
of 2.8(-0.3,+0.3)x10^-5 erg/cm2, and a 64-ms peak flux,
measured from T0+10.560 s, of 7.7(-0.8,+0.8)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+13.824 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 = -0.29 (-0.14,+0.14),
the high energy photon index beta = -2.80 (-0.69,+0.25),
the peak energy Ep = 241 (-17,+28) keV,
chi2 = 102/97 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB141215_T48373/

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


GRB_name: GRB141215A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17188
SUBJECT: GRB 141215A Tiled Swift observations
DATE:    14/12/16 18:28:48 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 141215A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00035

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: GRB141215A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17189
SUBJECT: GRB 141215A: Fermi GBM detection
DATE:    14/12/16 22:09:07 GMT
FROM:    Peter Jenke at MSFC  <peter.a.jenke@nasa.gov>

P. Jenke (UAH), A. von Kienlin (MPE) and E. Burns (UAH) 
report on behalf of the Fermi GBM Team:

"At 13:26:15.75 on December 15 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 141215A (trigger 440342778/141215560). 
GBM's location is consistent with the IPN 
Triangulation (K. Hurley et al. 2014, GCN 17186). 

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

The GBM light curve consists of three peaks with a duration
(T90) of about 11 s (50-300 keV).
The time-averaged spectrum from T0+0.0 s to T0+14.2 s 
is best fit by a power law function with an exponential 
high-energy cutoff. The power law index is -0.62 +/- 0.03
and the cutoff energy, parameterized as Epeak, is 392 +/- 11 keV.
The spectrum is equally well fit by the BAND function 
with Beta = -3.5 +/- 0.5. 
The event fluence (10-1000 keV) in this time interval is
(2.94 +/- 0.04)E-05 erg/cm^2. The 1 sec peak photon flux measured
starting from T0+10.8 s in the 10-1000 keV band
is 20.6 +/- 0.7 ph/s/cm^2.


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


GRB_name: GRB141215A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17190
SUBJECT: GRB 141215A: Swift-XRT observations
DATE:    14/12/17 15:48:09 GMT
FROM:    Valerio D'Elia at INAF-OAR  <delia@oa-roma.inaf.it>

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

Swift-XRT has observed the error box of the IPN GRB 141215A (Hurley et  al. GCN 17186) in a series of observations tiled on the sky. The total exposure time is 8.0 ks spread over 2 fields. The observations started ~100 ks after the IPN trigger and cover ~80% of the error box. We detect three sources with S/N>2.5 within the IPN error box, namely (ordered by descending RA):

Source 1
RA:  178.98953 = 11h 55m 57.49s (J2000) 
Dec: -52.90081 = -52d 54' 02.9" (J2000)
Err: 3.6 arcsec (radius, 90% confidence)
Exposure time: 3.3 ks.

Source 2
RA:  178.95882 = 11h 55m 50.12s (J2000) 
Dec: -52.82640 = -52d 49' 35.1" (J2000)
Err: 4.3 arcsec (radius, 90% confidence)
Exposure time: 3.4 ks.

Source 3
RA:  178.80790 = 11h 55m 13.90s (J2000) 
Dec: -52.84520 = -52d 50' 42.7" (J2000)
Err: 5.1 arcsec (radius, 90% confidence)
Exposure time: 3.4 ks.


Source #1 has a 2MASS counterpart and it is fairly bright (5E-2 cts/s) for being an X-ray afterglow at more than 30 hours from the trigger. Thus, the current candidates are #2 and #3. We cannot assess variability at this time, so a secure identification of the afterglow is not possible. We caution that the XRT observations cover just 80% of the IPN error box. A further Swift-XRT follow-up is planned. 

Details on the present analysis can be found at:

http://www.swift.ac.uk/xrt_products/TILED_GRB00035/


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


GRB_name: GRB141121A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17191
SUBJECT: GRB 141121A: Keck observations
DATE:    14/12/18 12:15:16 GMT
FROM:    Daniel Perley at Caltech  <dperley@astro.caltech.edu>

D. A. Perley (Caltech) reports:

I observed the location of GRB 141121A (Lien et al., GCN
17075) using the imaging mode of the Low-Resolution Imaging
Spectrometer (LRIS) on the Keck I 10-meter telescope between 10:55 and 
11:16 UT on 2014-12-18.  A short sequence of exposures in g, R, and 
i-bands was acquired.

The optical counterpart (Tanga et al., GCN 17078) is clearly detected in 
all filters. Calibrating relative to SDSS, the magnitude is:

i = 23.96 +/- 0.07  (t = 27.3 days)

This measurement is significantly fainter than that reported by Toy et 
al. based on DCT observations on 2014-12-07, and the counterpart appears 
point-like in 0.8-arcsecond seeing.  This suggests that the light is 
still dominated by the afterglow.


GRB_name: GRB141202A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17192
SUBJECT: GRB 141202A: Suzaku WAM observation of the prompt emission
DATE:    14/12/19 04:36:16 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

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

The short and IPN localized GRB 141202A (IPN localization: S.
Golenetskii et al., GCN 17131; Fermi GBM Detection: O.J. Roberts et al.,
GCN 17133; Konus-Wind observation: S. Golenetskii et al., GCN 17136)
triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an
energy range of 50 keV - 5 MeV at 11:17:5.508 UT (=T0).

The observed light curve shows a multi-peaked structure lasting from T0s
to T0+2s, followed by a weaker emission seen with a duration (T90) of
about 1.8 seconds. The fluence in 100 - 1000 keV was
4.48 (-0.18, +0.10) x 10^-6 erg/cm^2. The 1-s peak flux measured from
T0+0.5s was 7.61 (-2.44, -0.11) photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0 s to
T0+2 s is well fitted by a power-law with exponential cutoff model:
dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
alpha       0.28 (-0.56, +0.48), and
Epeak       565 (-66, +96) keV (chi^2/d.o.f. = 24.5/25).

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

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


GRB_name: GRB141207A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17193
SUBJECT: GRB 141207A: Suzaku WAM observation of the prompt emission
DATE:    14/12/19 04:58:51 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

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

The long GRB 141207A(Fermi-LAT Detection: Kocevski et al.,GCN 17146;
Swift-XRT observation:Amaral-Rogers et al.,GCN 17149;Fermi GBM dection:
Burns et al.,GCN 17150) triggered the Suzaku Wide-band  All-sky Monitor
(WAM) which covers an energy range of 50 keV - 5 MeV at 19:11:22.452 UT
(=T0).

The observed light curve shows a multi-peaked structure starting at
T0-1s, ending at T0+22s  with a duration(T90) of about 20 seconds. The
fluence in 100 - 1000 keV was 1.94(+0.10/-0.19)x10^-5 erg/cm^2.The 1-s
peak flux measured from T0+6s was 4.74(+0.37/-1.32) photons/cm^2/s in
the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-1s to
T0+22s is well fitted by a power-law with exponential cutoff model:
  dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
  alpha       1.11(+0.40/-0.48), and
  Epeak       579(+126/-92) keV (chi^2/d.o.f. = 28.2/25).

Due to the brightness of this burst, a 3% systematic error was added for
low energy channels. There might be uncertainty since the response for
the incident angle of GRB photons to WAM is not reliable.
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: GRB141207A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17194
SUBJECT: IPN Triangulation of GRB 141207A
DATE:    14/12/19 22:01:24 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@ssl.berkeley.edu>

K. Hurley, on behalf of the IPN, 

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

D. M. Smith, J. McTiernan, R. Schwartz, W.
Hajdas, and A. Zehnder, on behalf of the RHESSI 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,

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

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

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

GRB 141207A, initially reported by the Fermi LAT and GBM teams (GCN
17146, 17150), was also observed by Konus-Wind, INTEGRAL SPI-ACS, Swift
BAT (outside the coded FoV), MESSENGER GRNS, RHESSI, and Suzaku WAM.
We have triangulated it to a preliminary, 3 sigma annulus centered at
RA(2000), Dec(2000) = 73.658 deg (04h 54m 38s), +23.585 deg (+23d 35'04"), 
whose radius is 85.031 +/- 0.100 deg.  The XRT source reported in Evans, Page,
& Amaral-Rogers, GCN 17157, lies 0.003 degrees from the center line of this annulus, 
supporting the conclusion that this source is the GRB counterpart.


GRB_name: GRB141220A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17196
SUBJECT: GRB 141220A: Swift detection of a burst with an optical afterglow
DATE:    14/12/20 06:23:27 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

J. R. Cummings (NASA/UMBC), V. D'Elia (ASDC), N. Gehrels (NASA/GSFC),
A. Y. Lien (GSFC/UMBC), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/PSU) and M. H. Siegel (PSU) report on behalf
of the Swift Team:

At 06:02:52 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 141220A (trigger=621915).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 195.050, +32.144 which is 
   RA(J2000) = 13h 00m 12s
   Dec(J2000) = +32d 08' 37"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked
structure with a duration of about 10 sec.  The peak count rate
was ~5000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 06:04:31.8 UT, 99.2 seconds after
the BAT trigger. The position determined from promptly downlinked data
differs significantly from the on-board position, suggesting that the
XRT may have centroided on a cosmic ray; the initial XRT position
notice should be treated with caution. Using promptly downlinked data
we find a fading, uncatalogued X-ray source located at RA, Dec
195.06735, 32.13361 which is equivalent to:
   RA(J2000)  = 13h 00m 16.16s
   Dec(J2000) = +32d 08' 01.0"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 64 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 1.33
x 10^20 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 105 seconds after the BAT trigger. The 2.7'x2.7' sub-image shows a
likely optical afterglow near the XRT position. We are unable to confirm or
measure a magnitude due to the loss of star tracker lock. 

We note that the XRT position may have an additional error of order
10 arcseconds due to star tracker lock.  A more accurate location
will be generated when the full dataset is available. 

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: GRB141220A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17197
SUBJECT: GRB141220A: 1.23m CAHA I-band observations
DATE:    14/12/20 07:52:06 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@iaa.es>

J. Gorosabel (IAA-CSIC/UPV-EHU), S. Hellmich (DLR), A. de Ugarte Postigo (IAA-CSIC), S. Mottola (DLR), C. Thoene (IAA-CSIC), report on behalf of a larger collaboration:

We observed the field of GRB 141220A with the 1.23m CAHA in the I-band starting  ~8 min post burst. A bright afterglow is detected at RA(J2000)=13:00:15.76, DEC(J2000)=32:08:46:4 (+/-0.8"). We note an important discrepancy with the initial position reported by Swift.


GRB_name: GRB141220A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17198
SUBJECT: GRB 141220A: Redshift from OSIRIS at the 10.4m GTC
DATE:    14/12/20 07:53:28 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), C.C. Thoene (IAA-CSIC),
J. Gorosabel (UPV, IAA-CSIC), N. Tanvir (U. Leicester), J.P.U. Fynbo (DARK/NBI),
P. Pesev (GRANTECAN), G. Gomez Velarde (GRANTECAN), and 
D. Perez Valladares (GRANTECAN) report on behalf of a larger collaboration

We observed the afterglow of GRB141220A (Cummings et al. GCN 17196, Gorosabel
et al. GCN 17197) with OSIRIS at the 10.4m GTC. Observations began at 6:45 UT 
(50 min after the burst). In a first 600 s spectrum obtained with grism R1000B covering 
from 3750 to 7800 A we detect absorption features of AlII, FeII, MgII, MgI, at a redshift 
of 1.3195, including several absorptions of FeII* which make it very likely the redshift of 
the GRB. We also detect two MgII intervening systems at redshifts of 1.280 and 0.527.


GRB_name: GRB141220A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17199
SUBJECT: GRB 141220A: LT optical afterglow observations
DATE:    14/12/20 08:32:50 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), A. Gomboc (U. Ljubljana)
on behalf of a larger collaboration report:

The 2-m Liverpool Telescope automatically began observing Swift
GRB 141220A (Cummings et al. GCN 17196) on Dec 20 at 06:04:57 UT
(125 sec after the burst trigger).
The robotic LT-TRAP pipeline identified the optical afterglow
at the position reported by Gorosabel et al. (GCN 17197)
with r=18.6 +- 0.1 mag at 34 minutes after the GRB,
calibrated against nearby SDSS-R stars.


GRB_name: GRB141220A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17200
SUBJECT: GRB 141220A: Photometry from OSIRIS/GTC
DATE:    14/12/20 11:08:46 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), C.C. Thoene (IAA-CSIC),
J. Gorosabel (IAA-CSIC, UPV-EHU), N.R. Tanvir (U. Leicester), 
J.P.U. Fynbo (DARK/NBI), P. Pesev (GRANTECAN), G. Gomez Velarde 
(GRANTECAN), and D. Perez Valladares (GRANTECAN) report on behalf 
of a larger collaboration:

Photometric observations of the afterglow of GRB 141220A (Cummings et al. 
GCN 17196, Gorosabel et al. GCN 17197, de Ugarte Postigo et al. GCN 17198) 
were obtained by OSIRIS/GTC starting 20.6 min after the GRB onset. The 
afterglow was detected at r' = 18.11+/-0.05 mag in the first image and had 
decayed by 0.6+/-0.1 mag 38.7 min after the burst. Using our photometric data 
we derive a decay slope of alpha=0.96+/-0.11 (where F_nu ~ t^-alpha). These 
results are consistent with the observations reported by Guidorzi et al. (GCN 
17199). Our photometry was performed using SDSS stars as reference.

We encourage further observations and in particular spectroscopy of the 
afterglow, in particular to check for possible variability of the FeII* features 
between 5400 and 6100 A.


GRB_name: GRB141220A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17201
SUBJECT: GRB 141220A: Swift/UVOT Detection
DATE:    14/12/20 16:08:45 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and J. R. Cummings (NASA/UMBC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 141220A
597 s after the BAT trigger (Cummings et al., GCN Circ. 17196).
There were also other exposures when the spacecraft attitude
was not stable.
A source consistent with the optical position
Gorosabel et al. (GCN Circ. 17197)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  13:00:15.76 = 195.06565 (deg.)
    Dec (J2000) = +32:08:47.0  =  32.14639 (deg.)
with an estimated uncertainty of 0.45 arc sec. (radius, 90% confidence).

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

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

white              597          617           19         17.30  0.07
v                  647          839           39         17.65  0.16
b                  573          593           20         17.58  0.13

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.01 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB141220A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17202
SUBJECT: GRB 141220A: Swift-BAT refined analysis
DATE:    14/12/20 16:48:39 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <james.r.cummings@nasa.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings, N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), J. Tueller (GSFC),
T. N. Ukwatta (LANL)
(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 141220A (trigger #621915) (Cummings, et al.,
GCN Circ. 17196).  The BAT ground-calculated position is RA, Dec = 195.058, 32.146
deg which is:
    RA(J2000)  =  13h 00m 14.0s
    Dec(J2000) = +32d 08' 46.4"
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 19%.
  
The mask-weighted light curve shows two peaks at about T+1 and T+3 seconds,
with an exponential decline noticeable out to ~T+20 seconds.  T90 (15-350 keV)
is 7.21 +- 0.48 sec (estimated error including systematics).
  
The time-averaged spectrum from T-0.91 to T+7.30 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 0.62 +- 0.38,
and Epeak of 117.4 +- 45.1 keV (chi squared 56.50 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 2.6 +- 0.1 x 10^-06 erg/cm2
and the 1-sec peak flux measured from T-0.13 sec in the 15-150 keV band is
8.9 +- 0.7 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.30 +- 0.08 (chi squared 67.35 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/621915/BA/


GRB_name: GRB141220A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17203
SUBJECT: GRB 141220A: Swift-XRT refined Analysis
DATE:    14/12/20 20:23:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.8 ks of XRT data for GRB 141220A (Cummings  et al.
GCN Circ. 17196),  from 87 s to 36.3 ks after the  BAT trigger. The
data comprise 42 s in Windowed Timing (WT) mode (the first 8 s were
taken while Swift was slewing) with the remainder in Photon Counting
(PC) mode. The refined XRT position is RA, Dec = 195.0653, +32.1466
which is equivalent to:

RA (J2000): 13 00 15.66
Dec(J2000): +32 08 47.9

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

The late-time light curve (from T0+5.6 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.38 (+0.26, -0.23).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.81 (+0.21, -0.20). The
best-fitting absorption column is  8.3 (+5.9, -5.1) x 10^20 cm^-2, in
excess of the Galactic value of 1.3 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.7 x 10^-11 (4.2 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      8.3 (+5.9, -5.1) x 10^20 cm^-2
Galactic foreground: 1.3 x 10^20 cm^-2
Excess significance: 2.3 sigma
Photon index:      1.81 (+0.21, -0.20)

If the light curve continues to decay with a power-law decay index of
1.38, the count rate at T+24 hours will be 2.6 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 9.5 x
10^-14 (1.1 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00621915.

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


GRB_name: GRB141220A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17204
SUBJECT: GRB 141220A: MITSuME Okayama upper limits
DATE:    14/12/20 23:57:05 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 141220A (Cummings et al., GCNC 17196)
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 2014-12-20 16:27:31 UT (~10.4 h after the burst)
We could not detect the previously reported afterglow (Cummings et al., GCNC
17196; Gorosabel et al., GCNC 17197; de Ugarte Postigo et al., GCNC 17198) 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
-----------------------------------------------------
0.47547    17:27:32    5940.0   >19.8  >19.9  >19.0
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB141220A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17205
SUBJECT: GRB 141220A: Fermi GBM observation
DATE:    14/12/21 04:24:48 GMT
FROM:    Hoi-Fung Yu at MPE  <sptfung@mpe.mpg.de>

H.-F. Yu (MPE) reports on behalf of the Fermi GBM Team:

"At 06:02:52.49 UT on 20 Dec 2014, the Fermi Gamma-Ray Burst Monitor triggered 
and located GRB 141220A (trigger 141220252/ 141220252), which was also detected
by Swift (Cummings et al. 2014, GCN 17196). The GBM on-ground location, using 
the Fermi GBM trigger data, is consistent with the Swift location. The trigger 
resulted in an Autonomous Repoint Request (ARR) that was accepted and the 
spacecraft slewed to the GBM in-flight location. The angle from the Fermi LAT 
boresight is about 47 degrees.

The GBM light curve consists of two main pulses with a duration (T90) of about 
7.6 s (50-300 keV). The time-averaged spectrum from T0-1.920 s to T0+8.320 s is
best fit by a power law function with an exponential high-energy cutoff. The 
power law index is -0.80 +/- 0.05 and the cutoff energy, parameterized as Epeak, 
is 180 +/- 9 keV.

The event fluence (8-1000 keV) in this time interval is
(5.23 +/- 0.15)E-06 erg/cm^2. The 1.024-sec peak photon flux measured starting 
from T0+0.128 s in the 8-1000 keV band is 12.0 +/- 0.3 ph/s/cm^2.

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


GRB_name: GRB141221A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17206
SUBJECT: GRB 141221A: Swift detection of a burst with an optical counterpart
DATE:    14/12/21 08:21:02 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

E. Sonbas (NASA/GSFC/Adiyaman Univ.), J. R. Cummings (NASA/UMBC),
V. D'Elia (ASDC), L. Izzo (URoma/ICRA), A. Y. Lien (GSFC/UMBC),
K. L. Page (U Leicester), B. Sbarufatti (INAF-OAB/PSU) and
M. H. Siegel (PSU) report on behalf of the Swift Team:

At 08:07:10 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 141221A (trigger=622006).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 198.269, +8.210 which is 
   RA(J2000) = 13h 13m 05s
   Dec(J2000) = +08d 12' 36"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked
structure with a duration of about 20 sec.  The peak count rate
was ~4000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 08:08:30.3 UT, 79.5 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 198.28642, 8.20536 which is equivalent
to:
   RA(J2000)  = 13h 13m 08.74s
   Dec(J2000) = +08d 12' 19.3"
with an uncertainty of 3.9 arcseconds (radius, 90% containment). This
location is 64 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (2.27 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 3.5
(+2.80/-2.41) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 83 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 13:13:08.80 = 198.28666
  DEC(J2000) = +08:12:18.8  = 8.20523
with a 90%-confidence error radius of about 0.61 arc sec. This position is 4.2
arc sec. from the center of the XRT error circle. The estimated magnitude is
17.18 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.03. 

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


GRB_name: GRB141220A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  17207
SUBJECT: Konus-Wind observation of GRB 141220A
DATE:    14/12/21 12:57:37 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long-duration GRB 141220A (Swift-BAT trigger #621915:
Cummings et al., GCN 17196; Stamatikos et al., GCN 17202;
Fermi-GBM observation: Yu, GCN 17205)
triggered Konus-Wind at T0=21771.666 s UT (06:02:51.666).

The KW light curve shows a single emission episode lasting from ~T0-0.5 s
to ~T0+7.5 s. The emission in this episode is visible up to ~4 MeV.

As observed by Konus-Wind, the burst had a fluence
of 4.7(-0.4,+0.5)x10^-6 erg/cm2, and a 64-ms peak flux,
measured from T0, of 2.2(-0.4,+0.5)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 15 MeV range
by the cutoff power law with the following model parameters:
the photon index alpha = -0.55(-0.26,+0.30),
and the peak energy Ep = 139(-14,+18) keV,
chi2 = 83/98 dof.
Fitting this spectrum with the Band model yields the same
values of alpha and Ep and an upper limit on beta of -2.0

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB141220_T21771/

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


