GRB 120514A

V. Mangano (INAF-IASFPA), S. D. Barthelmy (GSFC), D. N. Burrows (PSU),
N. Gehrels (NASA/GSFC), E. A. Hoversten (PSU), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), F. E. Marshall (NASA/GSFC),
A. Maselli (INAF-IASFPA), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU), C. A. Swenson (PSU)
and B.-B. Zhang (PSU) report on behalf of the Swift Team:

At 01:12:49 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 120514A (trigger=522197).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 282.991, -4.252 which is 
   RA(J2000) = 18h 51m 58s
   Dec(J2000) = -04d 15' 06"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure consisting of two overlapping peaks with a duration of 
about 80 sec and an additional weaker peak at ~T+150 sec coincident 
with a peak observed by the XRT.   The peak count rate was ~2500 
counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 01:14:31.2 UT, 101.3 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 282.99969,
-4.26375 which is equivalent to:
   RA(J2000)  = 18h 51m 59.93s
   Dec(J2000) = -04d 15' 49.5"
with an uncertainty of 4.0 arcseconds (radius, 90% containment). This
location is 52 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 (6.09 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 1.4
(+1.29/-0.95) x 10^22 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 3.94e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 110 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. Because of the density of catalogued stars, further
analysis is required to report an upper limit for any afterglow in the
sub-image. 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 large, but uncertain extinction
expected. 

We note that this source is 2 degrees from the Galactic plane. 
Although the BAT lightcurve and energy distribution is
typical for a GRB, the possibility of this being a Galactic
source will have to be assessed from further observations. 

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

GRB 120514A: TAROT Calern observatory optical observations
----------------------------------------------------------------------
Klotz A. (IRAP-CNRS-OMP), Gendre B. (ASDC/INAF-OAR),
Boer M. (UNS-CNRS-OCA), Atteia J.L. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 120514A detected by SWIFT
(trigger 522197) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 534s after the GRB trigger.
The elevation of the field increased from
37 degrees above horizon and weather conditions
were good.

We co-added a series of exposures.
We do not detect any OT in the XRT error box
with a limiting magnitude of:
t0+534s to t0+909s : R > 18.1

Galactic coordinates are lon= 29.2060 lat= -2.0542
and the galactic extinction in R band is 4.3 magnitudes
estimated from D. Schlegel et al. 1998ApJ...500..525S.

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

This message may be cited.

W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
V. Mangano (INAF-IASFPA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), 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+721 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 120514A (trigger #522197)
(Mangano, et al., GCN Circ. 13289
Loading...
 
 ).  The BAT ground-calculated position is
RA, Dec = 283.002, -4.258 deg which is 
   RA(J2000)  =  18h 52m 00.4s 
   Dec(J2000) = -04d 15' 28.6" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 61%.
 
The mask-weighted light curve shows 3 main peaks.  The first starts at ~T-40 sec,
and peaks at ~T+1 sec.  The second overlaps the tail of the first and peaks at ~T+52
and ends at ~T+115 sec.  The third peak starts at ~T+120 sec, peaks at ~T+150 sec
and ends at ~T+200 sec.  At the 2-sigma level, there is possible precursor emission
from ~T-160 to T-80 sec, and a possible forth peak from ~T+260 to ~T+420 sec.
T90 (15-350 keV) is 164.4 +- 5.8 sec (estimated error including systematics).
 
The time-averaged spectrum from T-8.75 to T+165.55 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.62 +- 0.10.  The fluence in the 15-150 keV band is 2.8 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+0.22 sec in the 15-150 keV band
is 1.9 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/522197/BA/

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

Using 932 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 120514A, 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 = 283.00078, -4.26359 which is equivalent
to:

RA (J2000): 18h 52m 0.19s
Dec (J2000): -04d 15' 48.9"

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

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

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

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), C. de Breuck,
T. Stanke, C. Agurto (ESO), M. Valencia-S. (U. Koeln), A. Remy 
(CEA-Saclay), F. Montenegro (ESO), J. Gorosabel, 
R. Sanchez-Ramirez (IAA-CSIC), J.P.U. Fynbo (DARK/NBI) 
report on behalf of a larger collaboration:

We have observed the field of GRB 120514A (Mangano et al. 
GCNC 13289) using LABOCA/APEX at Chajnantor (Chile) in the 
870 micrometer band. The weather conditions were good, with 
precipitable water vapour at the time of the observation of ~0.5mm. 
Observations began on May 14 at 4:55 UT (3.7 hr after the burst) 
and were performed using the photometric mode, centred at the 
enhanced X-ray position (Evans et al. GCNC 13292).

On a preliminary analysis of 160 min on source, we detect a flux 
density at the position of the afterglow of 6.2+/-2.3 mJy.

Further observations are foreseen. We encourage follow-up 
observations in other wavelengths.

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

We have analysed 6.5 ks of XRT data for GRB 120514A (Mangano  et al.
GCN Circ. 13289
Loading...
 
 ), from 90 s to 28.8 ks after the  BAT trigger. The data
comprise 132 s in Windowed Timing (WT) mode (the first 10 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Evans et
al. (GCN. Circ 13292).

The late-time light curve (from T0+4.4 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.22 (+0.29, -0.24).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index	of 1.90 (+0.12, -0.11). The
best-fitting absorption column is  1.68 (+0.15, -0.14) x 10^22 cm^-2,
in excess of the Galactic value of 6.1 x 10^21 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 2.2 (+/-0.3) and a
best-fitting absorption column of 2.4 (+0.5, -0.4) x 10^22 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 6.8 x 10^-11 (2.3 x 10^-10) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:	     2.4 (+0.5, -0.4) x 10^22 cm^-2
Galactic foreground: 6.1 x 10^21 cm^-2
Excess significance: 6.6 sigma
Photon index:	     2.2 (+/-0.3)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00522197.

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

A.J Levan (Warwick), N.R. Tanvir, K. Wiersema (Leicester), T. Wold
(JAC) report on behalf of a larger collaboration:

"We obtained K-band observations of GRB 120514A (Mangano et al. GCN
13289
Loading...
 
 ) with the United Kingdom Infrared Telescope (UKIRT) on Mauna
Kea, with a midpoint approximately 12 hours after the initial burst
detection. Comparison of a preliminary reduction of these images
with archival images taken as part of the UKIRT Galactic Plane
Survey (GPS; Lucas et al. 2008 MNRAS 391 136) does not reveal any
new sources within the refined XRT position (Evans et al. GCN 13292
Loading...
 
 ).
Given the crowded nature of the field we do note there are several
sources whose location is formally consistent with the X-ray position,
but none of these show clear evidence for variability between the
two epochs."

E. A. Hoversten (PSU) and V. Mangano (INAF-IASFPA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 120514A
110 s after the BAT trigger (Mangano et al., GCN Circ. 13289
Loading...
 
 ).
No optical afterglow consistent with the enhanced XRT position
(Evans et al., GCN Circ. 13292
Loading...
 
 ) 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           110          260          147         >20.6
u_FC               324          574          246         >20.5
white              110         1029          295         >20.9
u                  324          574          246         >20.5

The magnitudes in the table are not corrected for the Galactic  
extinction
due to the reddening of E(B-V) = 1.63 in the direction of the burst
(Schlegel et al. 1998).

A. Nicuesa Guelbenzu (TLS Tautenburg), S. Schmidl (TLS Tautenburg), V. 
Sudilovsky (MPE Garching), and J. Greiner (MPE Garching) report on 
behalf of the GROND team:

We observed the field of GRB 120514A (Mangano et al., GCN #13289
Loading...
 
 ) 
simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 
405) mounted at the 2.2 m MPG/ESO telescope at La Silla Observatory (Chile).

Observation started at 03:39 UT, 2.4 h after the trigger and ended at 
11:10 UT.

We detect two sources just outside of the enhanced 1.8" XRT error circle 
at RA,DEC 18:52:00.1, -04:15:50.8 and 18:52:00.2, -04:15:46.8 with a 
positional uncertainty of +/- 0.3". We note that neither source varies 
in r' brightness relative to USNO field stars over a period of 2 hours. 
Additionally, the southern source exhibits a thermal spectrum. 
Therefore, neither of these two sources are likely associated with the GRB.

Based on exposures of 1480 seconds in g'r'i'z' and 1200 seconds in JHK, 
we do not detect a source within the 1.8" XRT error circle of the X-ray 
counterpart candidate (Evans et al., GCN #13292
Loading...
 
 ) to the following 
3-sigma upper limits (AB system):

g' > 22.7,
r' > 23.0
i' > 23.0
z' > 23.0
J > 20.5
H > 19.6
K > 18.5

These magnitudes are calibrated against GROND zeropoints (g'r'i'z') and 
2MASS (JHK) and are not corrected for the expected Galactic foreground 
extinction corresponding to a reddening of E_(B-V)=1.7 mag in the 
direction of the burst (Schlegel et al. 1998).

M. Akiyama, N. Ohmori,  M. Yamauchi (Univ. of Miyazaki),
K. Yamaoka, Y. E. Nakagawa (Waseda U.),
W. Iwakiri, M. Tashiro, Y. Terada, T. Yasuda, K. Takahara, M. Asahina, 
S. Kobayashi, A. Sakamoto, H. Ueno (Saitama U.), 
Y. Hanabata,  T. Kawano, K. Takaki, Y.Tanaka, R. Nakamura, M. Ohno,
Y. Fukazawa (Hiroshima U.), S. Sugita (Nagoya U.), M. Kokubun, T. Takahashi (ISAS/JAXA),
Y. Urata, P. Tsai (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo), 
on behalf of the Suzaku WAM team, report:

The long GRB 120514A (Swift/BAT trigger #522197 ; Siegel et al., GCN
13289
Loading...
 
 ) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers
an energy range of 50 keV - 5 MeV at 01:12:43.252 UT (=T0).

The observed light curve shows a single peak starting at T0-2 s, ending
at T0+16 s, with a duration (T90) of about 14 seconds. The fluence in 100
- 1000 keV was 1.62(-0.69, +0.50) x 10^-6 erg/cm^2. The 1-s peak flux 
measured from T0 s was 0.71(-0.20, +0.18) photons/cm^2/s in the same 
energy range.

Preliminary result shows that the time-averaged spectrum from T0-2 s to
T0+16 s is well fitted by a single power-law with a photon index of 2.30
(-0.54, 0.75) (chi^2/d.o.f = 43.1/32).

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

The light curves for this burst are now available at:

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