GRB 140211A

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

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

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

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

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

We observed the field of GRB 140211A (Cummings et al., GCNC 15816)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.

The observation started on 2014-02-11 12:24:38 UT (~96 sec after the burst).
We did not find any new point source within the BAT error circle
(Cummings et al., GCNC 15816) in all the three bands.

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

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

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

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

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

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

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


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

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

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


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

UVOT performed observations of GRB140211A in UVM2 and UVW1. At the  
position of the XRT source, no counterpart is detected in these  
filters in summed exposures. Preliminary 3-sigma upper limits using  
the UVOT photometric system (Breeveld et al 2011, AIP Conf. Proc.  
1358, 373) are

Filter� � �T_start (s)� � �T_Stop (s)� � �Exp (s)� � �Mag
um2� � � �298690� � � � 298860� � � � 167� � � � >19.5
uw1� � � � 338330� � � �385245� � � 2438� � � � >21.3

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

This circular is an official product of the Swift team.

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

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

Details of the photometry are following:

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

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

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