GRB 250114A
GCN Circular 39012
Subject
GRB 250114A: Swift-BAT refined analysis
Date
2025-01-22T13:51:00Z (2 years ago)
From
Mike Moss at NASA GSFC <mikejmoss3@gmail.com>
Via
Web form
A. Y. Lien (U Tampa), S. D. Barthelmy (GSFC),
R. Gupta (GSFC), N. J. Klingler (GSFC/UMBC/CRESSTII),
H. A. Krimm (NSF), S. Laha (GSFC/UMBC),
C. B. Markwardt (GSFC), M. J. Moss (GSFC),
D. M. Palmer (LANL), T. Parsotan (GSFC),
D. Sadaula (GSFC/UMBC), T. Sakamoto (AGU)
(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 250114A (trigger #1281241)
(N. J. Klingler, et al., GCN Circ. 38927). The BAT ground-calculated position is
RA, Dec = 166.572, -15.129 deg which is
RA(J2000) = 11h 06m 17.3s
Dec(J2000) = -15d 07' 44.5"
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 21%.
The mask-weighted light curves display several pulses between T0 and T0+60 sec.
There are also two additional pulses of emission starting around T0+130 and T0+260.
T90 (15-350 keV) is 293.89 +- 13.45 sec (estimated error including systematics).
The time-averaged spectrum from T-8.528 to T+305.988 sec is best fit by a power law
with an exponential cutoff. This fit gives a photon index 0.39 +- 0.62,
and Epeak of 50.9 +- 6.3 keV (chi squared 44.16 for 56 d.o.f.). For this
model the total fluence in the 15-150 keV band is 3.6 +- 0.3 x 10^-06 erg/cm2
and the 1-sec peak flux measured from T+1.72 sec in the 15-150 keV band is
1.5 +- 0.4 ph/cm2/sec. A fit to a simple power law gives a photon index
of 1.84 +- 0.11 (chi squared 66.05 for 57 d.o.f.). All the quoted errors
are at the 90% confidence level.
The results of the batgrbproduct analysis are available at
https://swift.gsfc.nasa.gov/results/batgrbcat/BAT_refined_circular/1281241
GCN Circular 38999
Subject
ATCA detection of possible radio counterpart to GRB 250114A
Date
2025-01-20T14:14:16Z (2 years ago)
From
lauren.rhodes@mcgill.ca
Via
Web form
L. Rhodes (TSI/McGill), G. E. Anderson (Curtin), A. J. van der Horst (GWU), J. K. Leung (UofT/HUJI), A. Gulati (USyd), S. Chastain (UNM) on behalf of the PanRadio GRB collaboration
We observed the position of GRB 250114A (Klingler et al., GCN 38927) starting at 2025-01-16 15:53UT for 7.5 hours with the Australia Telescope Compact Array (ATCA), as part of the “PanRadio GRB” Large ATCA follow-up programme C3542 (PI. Anderson).
We detect a radio source at the reported position (Klingler et al., GCN 38927) of the afterglow with a preliminary flux density of 70uJy/beam. The rms noise in our observation is 13 uJy/beam at 7GHz.
We thank the CSIRO Space and Astronomy staff for supporting these observations.
We acknowledge the Gomeroi people as the traditional owners of the Observatory site. The Australia Telescope Compact Array is part of the Australia Telescope National Facility (https://ror.org/05qajvd42) which is funded by the Australian Government for operation as a National Facility managed by CSIRO.
GCN Circular 38948
Subject
GRB 250114A: LCO optical counterpart detection.
Date
2025-01-15T04:57:30Z (2 years ago)
From
ankur ghosh at CAPP, University of Johannesburg <ghosh.ankur1994@gmail.com>
Via
Web form
Ankur Ghosh, Soebur Razzaque (CAPP, University of Johannesburg), Alexander Moskvitin, Yulia Sotnikova (SAO RAS), Naveen Dukiya (ARIES), Rahul Gupta (NASA GSFC) on behalf of a larger collaboration.
We observed the field of the GRB 250114A triggered by Swift (Klingler et al., GCN 38927) in V, r filter of the 1-meter Sinistro telescope at the Las Cumbres Observatory Global Telescope (LCOGT) node located at South African Astronomical Observatory (SAAO). The 1-m Sinistro telescope is equipped with a 4K x 4K CCD (FOV: 26 x 26 arcmin, scale: 0.39 arcsec/pixel).
Observations began on January 14, 2025, starting from 6.06 hours after the GRB trigger.
We clearly detect the optical transient (OT) reported by GCNs (Beardmore et al., GCN 38936, An et al., GCN 38929; Malesani & Izzo, GCN 38930; Francile et al., GCN 38931; Brivio et al., GCN 38933, Malesani et al., GCN 38934, Pérez-Fournon & Poidevin, GCN 38943) in our V, r band image. The optical afterglow detected in our images is consistent with the UVOT coordinates (Klingler et al., GCN 38927).
|Date| |UTstart| |t-T0 (hours)| |Exp (sec)| |Filter| |Magnitude|
--------------------------------------------------------------------------------------------------
2025-01-14 13:36:54.720 6.06 1 x 1200 V V = 21.88 +/- 0.52
2025-01-14 14:11:39.552 6.64 1 x 1200 r r = 22.01 +/- 0.35
--------------------------------------------------------------------------------------------------
The field was calibrated against nearby APASS stars, with magnitudes converted using Lupton (2005) equations, and has not been corrected for Galactic extinction.
GCN Circular 38946
Subject
GRB 250114A: GRANDMA/TAROT optical afterglow detection
Date
2025-01-14T21:01:29Z (2 years ago)
Edited On
2025-01-15T16:35:01Z (2 years ago)
From
Sarah Antier at OCA <sarah.antier@oca.eu>
Edited By
Judith Racusin at NASA/GSFC <judith.racusin@nasa.gov> on behalf of Sarah Antier at OCA <sarah.antier@oca.eu>
Via
Web form
S. Antier (OCA/IJCLAB), A. Klotz (IRAP), D. Akl (AUS), S. Karpov (FZU), M. Coughlin (UMN), C. Limonta, M. Boer, Q. Andre, A. Durroux (OCA), C. Andrade (UMN), P. Hello (IJCLAB), P-A Duverne (APC), T. Pradier (Unistra/IPHC), D. Turpin (CEA-Saclay/Irfu), N. Guessoum (AUS) on behalf of the GRANDMA collaboration:
We observed the field of GRB 250114A, detected by Swift (Klingler et al., GCN 38927) using TAROT/TCH. Observations began 1 min after T0 without filter, and we took a series of one trailed image lasting 60s and then 5x30s.
We detected the optical afterglow candidate in all images. We measured the decaying flux from 15.4 +/- 0.2 r-mag after the first minute, 16.3 +/-0.1 r-mag after the second minute, and 17.4 +/- 0.2 r-mag 5 minutes post T0.
The first 60s trailed image was analysed using techniques from Klotz et al., 2006, A&A 451, L39. The data from 2 to 5 min was reduced by a single data processing pipeline, STDPipe (Karpov et al., 2022), using Skymapper.
The light curve and its measurements can be found at : https://skyportal-icare.ijclab.in2p3.fr/public/sources/GRB250114
Our measurements are compatible with GCNs 38927, 38929, 38930, 38933, 38934, 38943.
GRANDMA is a worldwide telescope network (grandma.ijclab.in2p3.fr) devoted to the observation of transients in the context of multi-messenger astrophysics (Antier et al. 2020 MNRAS 497, 5518). Kilonova-Catcher (KNC) is the citizen science program of GRANDMA (http://kilonovacatcher.in2p3.fr/).
GCN Circular 38945
Subject
GRB 250114A: Swift-XRT refined Analysis
Date
2025-01-14T19:41:44Z (2 years ago)
From
Phil Evans at U of Leicester <pae9@star.le.ac.uk>
Via
email
S. Dichiara (PSU), J.A. Kennea (PSU), K.L. Page (U. Leicester), A.P.
Beardmore (U. Leicester), V. D'Elia (SSDC & INAF-OAR), B. Sbarufatti
(INAF-OAB), C. Salvaggio (INAF-OAB), D.N. Burrows (PSU) and P.A. Evans
report on behalf of the Swift-XRT team:
We have analysed 8.6 ks of XRT data for GRB 250114A, from 117 s to 28.1
ks after the BAT trigger. The data comprise 317 s in Windowed Timing
(WT) mode (the first 9 s were taken while Swift was slewing) with the
remainder in Photon Counting (PC) mode.
The late-time light curve (from T0+4.6 ks) can be modelled with an
initial rise, with a power-law index of alpha=-0.94 (+1.18, -0.25),
followed by a break at T+8035 s to an alpha of 1.32 (+0.31, -0.29).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.09 (+/-0.03). The
best-fitting absorption column is 1.8 (+/-0.9) x 10^22 cm^-2, at a
redshift of 4.732, in addition to the Galactic value of 5.1 x 10^20
cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index
of 1.87 (+0.14, -0.13) and a best-fitting absorption column of 1.0
(+2.2, -1.0) x 10^22 cm^-2. The counts to observed (unabsorbed) 0.3-10
keV flux conversion factor deduced from this spectrum is 3.6 x 10^-11
(4.1 x 10^-11) erg cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Galactic foreground: 5.1 x 10^20 cm^-2
Intrinsic column: 1.0 (+2.2, -1.0) x 10^22 cm^-2 at z=4.732
Photon index: 1.87 (+0.14, -0.13)
If the light curve continues to decay with a power-law decay index of
1.32, the count rate at T+24 hours will be 6.8 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.4 x
10^-13 (2.8 x 10^-13) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01281241.
This circular is an official product of the Swift-XRT team.
GCN Circular 38943
Subject
GRB 250114A: LCOGT optical afterglow i-band detection
Date
2025-01-14T17:01:56Z (2 years ago)
From
Ismael Perez-Fournon at Instituto de Astrofisica de Canarias <ipf@iac.es>
Via
Web form
I. Pérez-Fournon and F. Poidevin (IAC and ULL)
We observed the field of GRB 250114A, detected by Swift BAT, XRT, and UVOT (Klingler et al., GCN 38927; Beardmore et al., GCN 38936) using one of the Las Cumbres Observatory global telescope network (LCOGT) 1-m telescopes, equipped with Sinistro cameras, at the LCOGT node at Siding Spring Observatory (Australia). The observation, a single 600-sec exposure in the SDSS i' filter, started at 2025-01-14 13:59:32 UT, i.e. ~ 6.44 hr after the Swift BAT trigger. The optical afterglow is detected at a position consistent with the UVOT coordinates (Klingler et al., GCN 38927). Me measure a magnitude of i' = 20.17 +/- 0.22, calibrated against PanSTARRS DR2 stars and not corrected for Galactic extinction.
Other groups have reported optical and near-IR detections of the afterglow: An et al. (GCN 38929), Malesani and Izzo (GCN 38930), Brivio et al. (GCN 38933) and Malesani et al. (GCN 38934). A redshift of z = 4.732 has been reported by Malesani et al. (GCN 38934).
This work makes use of observations from the Las Cumbres Observatory global telescope network (LCOGT observing programme IAC2024B-004, SGLF).
GCN Circular 38936
Subject
GRB 250114A: Enhanced Swift-XRT position
Date
2025-01-14T12:22:09Z (2 years ago)
From
Phil Evans at U of Leicester <pae9@star.le.ac.uk>
Via
email
A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester)
report on behalf of the Swift-XRT team.
Using 792 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 250114A, 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 = 166.57609, -15.11189 which is equivalent
to:
RA (J2000): 11h 06m 18.26s
Dec (J2000): -15d 06' 42.8"
with an uncertainty of 2.4 arcsec (radius, 90% confidence).
This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).
This circular was automatically generated, and is an official product of the
Swift-XRT team.
GCN Circular 38934
Subject
GRB 250114A: VLT/X-shooter spectroscopic redshift z = 4.732
Date
2025-01-14T10:32:04Z (2 years ago)
From
Daniele B. Malesani at IMAPP / Radboud University <d.malesani@astro.ru.nl>
Via
Web form
D. B. Malesani (DAWN/NBI and Radboud), A. Saccardi (CEA/Irfu), S. D. Vergani (GEPI/Obs. de Paris), P. D’Avanzo (INAF/OABr), A. de Ugarte Postigo (CNRS, OCA and LAM), K. E. Heintz (DAWN/NBI), L. Izzo (INAF/OACn and DARK/NBI), A. J. Levan (Radboud), B. Milvang-Jensen (DAWN/NBI), B. Schneider (LAM), N. R. Tanvir (Leicester), A. L. Thakur (INAF/IAPS) report on behalf of the Stargate collaboration.
We observed the optical afterglow of GRB 250114A (Klingler et al., GCN 38927; An et al., GCN 38929; Malesani & Izzo, GCN 38930; Francile et al., GCN 38931; Brivio et al., GCN 38933) using the ESO VLT UT3 (Melipal) equipped with the X-shooter spectrograph. Our spectra cover the wavelength range 3000-25000 AA, and consist of 4 exposures by 600 s each. The observation mid time was 2025 Jan 14.3549 UT (0.962 hr after the GRB).
In a 30 s image taken with the acquisition camera on Jan 14.339 UT, we detect the optical afterglow, for which we measure a magnitude r = 21.58 +- 0.12 AB (calibrated against two nearby stars from the Pan-STARRS catalog).
Continuum is clearly detected in the red end of the VIS arm, showing a strong break at 7000 AA, which we interpret as the Lyman break and the onset of the Lyman-alpha forest. From the detection of multiple absorption features, which we interpret as due to Si II 1260, Si II* 1264, O I 1302, C IV 1548,1540, Si II* 1264, and Mg II 2796,2803 (among others), we infer a redshift of z = 4.732.
An intervening system at z = 1.642 is also identified via the Mg II 2796,2803 doublet.
We acknowledge expert support from the ESO observing staff at UT3, in particular Rodrigo Palominos and Ana Jimenez.
GCN Circular 38933
Subject
GRB 250114A: REM detection of the optical and NIR counterpart
Date
2025-01-14T10:22:11Z (2 years ago)
From
Riccardo Brivio at INAF-OAB <riccardo.brivio@inaf.it>
Via
Web form
R. Brivio, P. D’Avanzo, M. Ferro (INAF-OAB), D.B. Malesani (DAWN/NBI and Radboud Univ.), A. Melandri (INAF-OAR), M. De Pasquale (Univ. of Messina), S. Covino, D. Fugazza (INAF-OAB) report on behalf of the REM team:
We observed the field of GRB 250114A, detected by Swift (Klingler et al., GCN 38927) with the REM 60cm robotic telescope located at the ESO observatory of La Silla (Chile). The observations were carried in the g, r, i, z, J, H, K bands, starting on 2025 January 14 at 07:34:43 UT (i.e. 84 sec after the Swift trigger).
We detect the counterpart in the optical and NIR images at the position of the optical afterglow (Klingler et al., GCN 38927; An et al., GCN 38929; Malesani & Izzo, GCN 38930; Francile et al., GCN 38931). From preliminary photometry, we measure:
r-i ~ 1.4 (calibrated against the Pan-STARRS catalogue),
at t - t0 = 84 s;
H = 13.2 +/- 0.1 (Vega; calibrated against the 2MASS catalogue),
at t - t0 = 101 s.
GCN Circular 38931
Subject
Swift GRB250114A: Global MASTER-Net OT detection
Date
2025-01-14T08:47:59Z (2 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
Via
email
C.Francile, F. Podesta, R.Podesta, E. Gonzalez (Observatorio Astronomico Felix Aguilar (OAFA),
V.Lipunov, E.Gorbovskoy, N.Tiurina, P.Balanutsa, D.Vlasenko, I.Panchenko, A.Kuznetsov, G.Antipov,
A.Sankovich, A.Sosnovskij, Yu.Tselik, M.Gulyaev, Ya.Kechin, V.Senik, A.Chasovnikov, K.Labsina (Lomonosov MSU),
O.Gress, N.Budnev(ISU),
A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),
A. Gabovich, V.Yurkov (Blagoveschensk Educational StateUniversity)
D.Buckley (SAAO),
R.Rebolo (The Instituto de Astrofisica de Canarias),
L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez (INAOE, Guillermo Haro Astrophysics Observatory)
MASTER-OAFA robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Argentina (OAFA observatory of San Juan National University) was pointed to the GRB250114A 24 sec after notice time and 63 sec after trigger time at 2025-01-14 07:34:22 UT. On our first (10s exposure) set we found 1 optical transient within Swift error-box (ra=166.588 dec=-15.1422 r=0.05).
T-Tmid Date Time Expt. Ra Dec Mag
---------|---------------------|-------|-----------------|-----------------|-------
68 2025-01-14 07:34:22 10 (11h 06m 18.39s , -15d 06m 41.2s) 15.9
The 5-sigma upper limit has been about 17.7mag
The message may be cited.
GCN Circular 38930
Subject
GRB 250114A: LCO optical observations
Date
2025-01-14T08:41:29Z (2 years ago)
From
luca.izzo@inaf.it
Via
Web form
D. B. Malesani (DAWN/NBI and Radboud Univ.), and L. Izzo (INAF-OACn and DARK/NBI) report:
We observed the field of GRB 250114A (Klingler et al., GCN #38927) with the Sinistro instrument mounted on the 1-m telescope of the LCO network, located at the Cerro Tololo, Chile. Observations started on 2025 January 14 at 07:48:10 UT (14.85 minutes after the GRB trigger). We obtained a series of 3x180 s images in the SDSS-r filter.
At the location of the Swift-UVOT afterglow, we detect a faint source. We measure a preliminary magnitude of r = 20.18 +/- 0.15 mag (AB), calibrated against nearby stars from the Pan-STARRS catalog. This value is consistent with TRT observations obtained at a similar epoch (An et al., GCN #38929).
This project has received funding from the European Union's Horizon 2020 research and innovation program under grant agreement No 101004719.
GCN Circular 38929
Subject
GRB 250114A: TRT optical observations
Date
2025-01-14T08:35:39Z (2 years ago)
From
Dong Xu at NAOC/CAS <dxu@nao.cas.cn>
Via
Web form
J. An (NAOC), S. Tinyanont, R. Anutarawiramkul, P. Butpan (NARIT), X. Liu, Z.P. Zhu, S.Y. Fu, S.Q. Jiang, D. Xu (NAOC) report on behalf of a large collaboration:
We observed the field of GRB 250114A detected by Swift (Klingler et al., GCN 38927), using the 0.7-m telescope of the Thai Robotic Telescope network (TRT), located at Cerro Tololo, Chile. Observations started at 07:46:08.50 UTC on 2025-01-14, i.e., 13 mins after the Swift trigger, and a series of R-band frames were obtained.
The optical afterglow by Swift/UVOT (Klingler et al., GCN 38927) is clearly detected in the stacked images. Its brightness is decaying and has r ~ 20.2 mag at a median time 14.5 mins after the Swift trigger, calibrated with PanSTARRS and not corrected for Galactic extinction.
GCN Circular 38928
Subject
Swift GRB 250114A: Global MASTER-Net observations report
Date
2025-01-14T08:25:08Z (2 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
Via
email
V.Lipunov, E.Gorbovskoy, N.Tiurina, P.Balanutsa, , D.Vlasenko, I.Panchenko,
A.Kuznetsov, G.Antipov, A.Sankovich, A.Sosnovskij, Yu.Tselik, M.Gulyaev, Ya.Kechin,
V.Senik, A.Chasovnikov, K.Labsina, I. Gorbunov (Lomonosov MSU),
O.Gress, N.Budnev (ISU),
C.Francile, F. Podesta, R.Podesta, E. Gonzalez (Observatorio Astronomico Felix Aguilar (OAFA),
A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),
A. Gabovich, V.Yurkov (Blagoveschensk Educational StateUniversity)
D.Buckley (SAAO),
R.Rebolo (The Instituto de Astrofisica de Canarias),
L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez,
A.R.Corella, L.H.Rodriguez (INAOE, Guillermo Haro Astrophysics Observatory)
MASTER-OAFA robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Argentina (OAFA observatory of San Juan National University) was pointed to the Swift GRB 250114A ( N. J. Klingler et al., GCN 38927) errorbox 18 sec after notice time and 63 sec after trigger time at 2025-01-14 07:34:22 UT, with upper limit up to 18.2 mag. The observations began at zenith distance = 18 deg. The sun altitude is -23.6 deg.
The galactic latitude b = 41 deg., longitude l = 270 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=2742671
We obtain a following upper limits.
Tmid-T0 | Site |Filt.| Expt. | Limit| Comment
_________|_____________________|_____|_______|______|________
68 | MASTER-OAFA | C | 10 | 18.2 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
GCN Circular 38927
Subject
GRB 250114A: Swift detection of a burst with an optical counterpart
Date
2025-01-14T07:50:30Z (2 years ago)
From
K.L. Page at U Leicester <klp5@leicester.ac.uk>
Via
email
N. J. Klingler (GSFC/UMBC/CRESSTII), R. Brivio (INAF-OAB),
J. J. DeLaunay (PSU), K. L. Page (U Leicester),
C. Salvaggio (INAF-OAB), T. Sbarrato (INAF-OAB), M. H. Siegel (PSU)
and A. Tohuvavohu (Caltech) report on behalf of the Neil Gehrels Swift
Observatory Team:
At 07:33:19 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 250114A (trigger=1281241). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 166.590, -15.143 which is
RA(J2000) = 11h 06m 22s
Dec(J2000) = -15d 08' 34"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a multi-peaked
structure with a duration of about 50 sec. The peak count rate
was ~875 counts/sec (15-350 keV), at ~3 sec after the trigger.
The XRT began observing the field at 07:35:27.7 UT, 128.3 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 166.57673, -15.11138 which
is equivalent to:
RA(J2000) = 11h 06m 18.42s
Dec(J2000) = -15d 06' 41.0"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 122 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
https://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 (5.06 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 3.9
(+3.65/-3.04) x 10^21 cm^-2 (90% confidence).
The initial flux in the 2.5 s image was 4.84e-09 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 136 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
RA(J2000) = 11:06:18.43 = 166.57679
DEC(J2000) = -15:06:41.7 = -15.11159
with a 90%-confidence error radius of about 0.74 arc sec. This position is 3.2
arc sec. from the center of the XRT error circle. The estimated magnitude is
20.35 with a 1-sigma error of about 0.20. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.056.
Burst Advocate for this burst is N. J. Klingler (noelklin AT umbc.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/)