GRB 160327A
GCN Circular 19453
Subject
GRB 160327A: 15 GHz upper limits from AMI
Date
2016-05-24T15:04:33Z (10 years ago)
From
Kunal Mooley at Oxford U <kunal.mooley@physics.ox.ac.uk>
K. P. Mooley, T. D. Staley, R. P. Fender (Oxford), G. E. Anderson
(Curtin), C. Rumsey, D. Titterington, S. Carey, J. Hickish, Y. C.
Perrott, N. Razavi-Ghods, P. Scott (Cambridge), K. Grainge, A. Scaife
(Manchester)
The AMI Large Array robotically triggered on the Swift alert for GRB
160327A (Racusin et al., GCN 19235) as part of the 4pisky program, and
subsequent follow up observations were obtained up to 10 days
post-burst. Our observations at 15 GHz on 2016 Mar 27.75, Mar 28.94, Mar
30.94, Apr 04.79, and Apr 06.83 (UT) do not reveal any radio source at
the XRT location (Goad et al., GCN 19237), with 3sigma upper limits of
84 uJy, 69 uJy, 96 uJy, 102 uJy, and 93 uJy respectively.
We thank the AMI staff for scheduling these observations. The AMI-GRB
database is a log of all GRB follow up observations with the AMI, and is
available at http://4pisky.org/ami-grb/.
GCN Circular 19250
Subject
GRB 160327A: Continued RATIR Optical and NIR Observations
Date
2016-04-01T19:20:19Z (10 years ago)
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), Ori Fox (STScI), J. Xavier
Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (GSFC/STScI),
Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC),
Jos�� A. de Diego (UNAM), Leonid Georgiev (UNAM), Jes��s Gonz��lez (UNAM),
Carlos Rom��n-Z����iga (UNAM), Neil Gehrels (GSFC), Harvey Moseley (GSFC),
John Capone (UMD), V. Zach Golkhou (ASU), and Vicki Toy (UMD) report:
We observed the field of GRB 160327A (Racusin, et al., GCN 19235) for a
third epoch with the Reionization and Transients Infrared Camera (RATIR;
www.ratir.org) on the 1.5m Harold Johnson Telescope at the Observatorio
Astron��mico Nacional on Sierra San Pedro M��rtir from 2016/04 1.22 to
2016/04 1.41 UTC (115.97 to 120.62 hours after the BAT trigger), obtaining
a total of 3.18 hours exposure in the r and i bands and 1.34 hours exposure
in the Z, Y, J, and H bands.
We are able to detect two of the three sources identified by the GTC (de
Ugarte Postigo, et al., GCN 19245). The afterglow (GTC source #1 and
Golkhou, et al., GCN 19236) is detected in our night 2 observations on 28
March (Golkhou, et al., GCN 19243) but not on 1 April. The GTC source #2
is detected on 28 March and 1 April and is the dominant source in terms of
brightness. We do not detect GTC source #3 on either night.
In comparison with the SDSS DR9 and 2MASS catalogs, we obtain the following
detections and upper limits (3-sigma):
Afterglow (GTC Source #1):
28 March 1 April
r > 24.37 r > 24.41
i = 24.20 +/- 0.31 i > 24.38
Z = 22.98 +/- 0.28 Z > 23.15
Y > 22.85 Y > 22.91
J > 22.67 J > 22.61
H > 22.21 H > 22.23
GTC Source #2:
28 March 1 April
r = 23.84 +/- 0.22 r > 24.42
i = 23.33 +/- 0.14 i = 23.57 +/- 0.17
Z = 22.57 +/- 0.20 Z = 22.71 +/- 0.25
Y = 22.83 +/- 0.35 Y > 22.73
J = 22.43 +/- 0.29 J > 22.60
H = 21.75 +/- 0.24 H > 22.24
GTC Source #3:
28 March 1 April
r > 24.37 r > 24.41
i > 24.34 i > 24.39
Z > 23.19 Z > 23.11
Y > 22.86 Y > 22.76
J > 22.66 J > 22.6
H > 22.21 H > 22.25
These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.
In addition to our first night observations (Golkhou, et al., GCN 19236),
which show the afterglow peaking and then fading, our observations on 28
March and 1 April confirm the fading of the afterglow. The above
photometric analysis, based on PSF fitting, may still suffer from modest
contamination between sources. More detailed analyses are under way.
We thank the staff of the Observatorio Astron��mico Nacional in San Pedro
M��rtir.
GCN Circular 19247
Subject
GRB 160327A: Early RAPTOR Limits
Date
2016-03-29T22:58:53Z (10 years ago)
From
James Wren at LANL <jwren@lanl.gov>
J. Wren, W.T. Vestrand, P. Wozniak, and H. Davis,
of Los Alamos National Laboratory report:
The RAPTOR network of robotic optical telescops made observations of Swift
trigger 680655 (Racusin, et al., GCN 19235). Our Raptor-S telescope began
imaging at 09:16:27.58 UT, 19.9 s after the Swift trigger time. We do not
detect the optical counterpart reported by RATIR (Golkhou, et al., GCN 19236).
We derive the following 3-sigma limits for our unfiltered observations based
on comparison to the USNO-B1.0 catalog R-band.
t-mid(s) exp(s) mag_limit
-------------------------------
32.5 5 17.4
67.8 40 18.6
131.8 10 18.0
180.4 100 19.2
249.9 200 19.6
GCN Circular 19246
Subject
GRB 160327A: JCMT SCUBA-2 sub-mm observation
Date
2016-03-29T19:28:48Z (10 years ago)
From
Ian Smith at Rice U <ian@spacsun.rice.edu>
I.A. Smith (Rice U.), N.R. Tanvir (U. of Leicester), and Y. Urata (NCU)
report:
We observed the location of GRB 160327A (Racusin et al., GCN Circ. 19235)
using the SCUBA-2 sub-millimeter continuum camera on the James Clerk
Maxwell Telescope. The observation started at 10:24 UT on 2016-03-27,
corresponding to 68 minutes after the burst trigger. Exposures totaling
1.0 hours were made in good weather conditions. No source was detected,
with the RMS background noise being 2.0 mJy/beam at 850 microns and
26.0 mJy/beam at 450 microns.
We thank Callie Matulonis and Iain Coulson for the prompt support of
these observations that were taken under project M16AP005.
GCN Circular 19245
Subject
GRB 160327A: Imaging and spectroscopy from GTC
Date
2016-03-29T18:18:21Z (10 years ago)
From
Antonio de Ugarte Postigo at IAA-CSIC <deugarte@iaa.es>
A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), N.R. Tanvir (U. Leicester),
Z. Cano (U. Iceland), L. Izzo (U. Roma1), J.P.U. Fynbo (DARK/NBI),
R. Sanchez-Ramirez (IAA-CSIC), C.C. Thoene (IAA-CSIC), P. Pesev
(GRANTECAN, IAC, ULL) report:
We observed the field of GRB 160327A (Racusin, et al., GCN 19235) with
OSIRIS mounted on the 10.4 m GTC telescope, located at Roque de los
Muchachos Observatory (La Palma, Spain) starting at 00:26 UT on 28th
March 2016 (15.17 hr after the burst).
In the acquisition image, we identify the afterglow proposed by Golkhou
et al. (GCN 19236) and later also observed by Zheng & Filippenko (GCN
19242). At the time of our observation, the object was at a magnitude
of i(AB) = 23.89 +/-0.12 (as compared to nearby SDSS stars), with
coordinates of (J2000.0, +/-0.5"):
R.A.: 09:46:48.56
Dec.: +54:00:46.3
We also note the presence of two other sources within 2.5��� of the GRB
afterglow: The first one is located at 09:46:48.35, +54:00:47.8 and has a
magnitude of i(AB) = 23.76+/-0.11, and the second one is at 09:46:48.55,
+54:00:44.2 with a magnitude of i(AB) = 24.24+/-0.15. We suspect that
these sources may be contributing to the magnitudes given by Golkhou
et al. (GCN 19243), especially in the bluer bands.
Spectroscopy of the GRB afterglow and the first of the two other objects
was obtained by exposing 3x1200 s with grism R1000R, which covers
between 5100 and 10100 Angstrom. We detect a trace of the GRB
afterglow above 7300 AA, below which the emission drops abruptly. The
other object shows a continuum over the complete spectral range,
suggesting that this object is unrelated to the GRB. The afterglow
spectrum is indicative of a Lyman-alpha drop at a redshift between 4.90
and 5.01, with a most probable value at z = 4.99, although even lower
redshifts could not be discarded for unusually large Hydrogen column
densities. Due to the low S/N of the spectrum we are not able to confirm
any other absorption lines at this time.
GCN Circular 19243
Subject
GRB 160327A: Continued RATIR Optical and NIR Observations
Date
2016-03-28T20:27:50Z (10 years ago)
From
V. Zach Golkhou at ASU/RATIR <golkhou@gmail.com>
V. Zach Golkhou (ASU), Nat Butler (ASU), Alan M. Watson (UNAM), Alexander
Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM), Ori Fox
(STScI), J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara
(GSFC/STScI), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), Jos�� A. de Diego (UNAM), Leonid Georgiev (UNAM), Jes��s
Gonz��lez (UNAM), Carlos Rom��n-Z����iga (UNAM), Neil Gehrels (GSFC), Harvey
Moseley (GSFC), John Capone (UMD), and Vicki Toy (UMD) report:
We observed the field of GRB 160327A (Racusin, et al., GCN 19235) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astron��mico Nacional on
Sierra San Pedro M��rtir from 2016/03 28.14 to 2016/03 28.39 UTC (17.98 to
24.15 hours after the BAT trigger), obtaining a total of 4.21 hours
exposure in the r and i bands and 1.76 hours exposure in the Z, Y, J, and H
bands.
For a source within the Swift-XRT error circle (Goad, et al., GCN 19237),
in comparison with the SDSS DR9 and 2MASS catalogs, we obtain the following
detections:
r 23.84 +/- 0.22
i 23.29 +/- 0.14
Z 22.57 +/- 0.20
Y 22.83 +/- 0.35
J 22.43 +/- 0.29
H 21.75 +/- 0.23
These magnitudes are in the AB system and are not corrected for
Galactic extinction
in the direction of the GRB. Compared to our previous night of observations
(Golkhou et al., GCN 19236), the source flux has decayed substantially in
all bands. The source r - i color changes from 2.1 +/- 0.1 to 0.6 +/-
0.3 between our first and the second night observations. The strong color
change suggests the possibility of contamination by the GRB host galaxy at
late-time.
We thank the staff of the Observatorio Astron��mico Nacional in San Pedro
M��rtir.
GCN Circular 19242
Subject
GRB 160327A: KAIT optical afterglow confirmation
Date
2016-03-28T19:36:40Z (10 years ago)
From
Weikang Zheng at UC Berkeley <weikang@berkeley.edu>
WeiKang Zheng and Alexei V. Filippenko (UC Berkeley) report
on behalf of the KAIT GRB team:
The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, responded to Swift GRB 151027A (Racusin et al.,
GCN 19235) starting at 09:17:37 UT, 90 s after the burst under
fair condition. Observations were performed with an automatic
sequence in the clear (roughly R), V, and I filters, and the
exposure time was 20 s per image.
The afterglow reported by Golkhou et al. (GCN 19236) was not detected
in any of our single images, however, it is detected in the
co-added images in both clear and I band, except V band. We report
the follow detection magnitude or upper limit:
Filter co-add Mid-time Detection_Mag Upper_limit
clear 20s x 10 549s 19.8 +/- 0.3 -
clear 20s x 10 1495s 20.2 +/- 0.4 -
clear 20s x 10 2162s - 20.0
I 20s x 10 615s 18.1 +/- 0.2 -
I 20s x 10 1541s 18.8 +/- 0.4 -
I 20s x 10 2195s - 18.7
V 20s x 15 781s - 18.9
[GCN OPS NOTE(30mar16): Per author's request, the second reference
was changed from Zach to Golkhou.]
GCN Circular 19241
Subject
GRB 160327A: Mondy optical upper limit
Date
2016-03-28T15:43:01Z (10 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
E. Mazaeva (IKI), A. Volnova (IKI), E. Klunko (ISTP), I. Korobtsev
(ISTP), A. Pozanenko (IKI) report on behalf of larger GRB follow-up
collaboration:
We observed the field of the GRB 160327A (Racusin et al., GCN 19235)
with AZT-33IK telescope of Sayan observatory (Mondy) starting on March,
27 (UT) 13:48:49. We do not detect any source within enhanced Swift-XRT
position (Goad et al., GCN 19237). In particular we do not detect the
source reported in GCN 19236 and it could confirm the source (Zach
Golkhou et al., GCN 19236) is an afterglow of the GRB 160327A.
Preliminary photometry of the combined image is following
Date UT start t-T0 Filter Exp. UpperLimit (3 sigma)
(mid, days) (s)
2016-03-27 13:48:49 0.20675 R 25*120 23.0
Photometry is based on nearby SDSS-DR9 stars, Lupton transformations
into R.
GCN Circular 19240
Subject
GRB 160327A: Swift-BAT refined analysis
Date
2016-03-28T14:30:02Z (10 years ago)
From
Tilan Ukwatta at LANL <tilan.ukwatta@gmail.com>
C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Y. Lien (GSFC/UMBC),
D. M. Palmer (LANL), J. L. Racusin (NASA/GSFC)
T. Sakamoto (AGU), M. Stamatikos (OSU),
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 160327A (trigger #680655) (Racusin, et al.,
GCN Circ. 19235). The BAT ground-calculated position is
RA, Dec = 146.698, 54.018 deg which is
RA(J2000) = 09h 46m 47.5s
Dec(J2000) = +54d 01' 04.0"
with an uncertainty of 1.0 arcmin, (radius, sys+stat,
90% containment). The partial coding was 82%.
BAT light curve shows a single peak starting around
T-10 sec, peaking around T+5 sec and ending around
T+22 sec. T90 (15-350 keV) is 28 +- 9 sec (estimated
error including systematics).
The time-averaged spectrum from T-6.30 to T+42.80 sec
is best fit by a simple power-law model. The power
law index of the time-averaged spectrum is 1.84 +- 0.11.
The fluence in the 15-150 keV band is
1.4 +- 0.1 x 10^-06 erg/cm2. The 1-sec peak photon flux
measured from T+4.14 sec in the 15-150 keV band
is 1.8 +- 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/680655/BA/
GCN Circular 19239
Subject
GRB 160327A: Swift/UVOT Upper Limits
Date
2016-03-28T13:55:52Z (10 years ago)
From
Marissa McCaule at PSU <marissamc@swift.psu.edu>
L. M. McCauley (PSU) and J. L. Racusin (NASA/GSFC)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 160327A
71 s after the BAT trigger (Racusin et al., GCN Circ. 19235).
No optical afterglow consistent with the XRT position
(Goad et al. GCN Circ. 19237) 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 71 221 147 >21.06
u_FC 284 534 246 >20.52
white 71 5902 535 >21.50
v 613 6310 451 >19.66
b 539 5702 254 >20.38
u 283 6918 670 >20.66
uvw1 662 6721 412 >20.21
uvm2 637 1088 58 >18.49
uvw2 589 1039 38 >18.61
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).
GCN Circular 19238
Subject
GRB 160327A: Swift-XRT refined Analysis
Date
2016-03-27T20:13:31Z (10 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
P. D'Avanzo (INAF-OAB), T.G.R. Roegiers (PSU), L.M. McCauley (PSU),
J.A. Kennea (PSU), P.A. Evans (U. Leicester), S.L. Gibson (U.
Leicester), J.P. Osborne (U. Leicester), V. D'Elia (ASDC), A. D'Ai
(INAF-IASFPA) and J.L. Racusin report on behalf of the Swift-XRT team:
We have analysed 6.0 ks of XRT data for GRB 160327A (Racusin et al. GCN
Circ. 19235), from 51 s to 22.1 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 Goad et al. (GCN Circ. 19237).
The light curve can be modelled with an initial power-law decay with an
index of alpha=2.53 (+0.14, -0.13), followed by a break at T+291 s to
an alpha of 0.59 (+/-0.06).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.97 (+0.15, -0.09). The
best-fitting absorption column is consistent with the Galactic value
of 1.2 x 10^20 cm^-2 (Willingale et al. 2013). The PC mode spectrum has
a photon index of 1.90 (+0.16, -0.15) and a best-fitting absorption
column of 4.2 (+3.5, -3.0) x 10^20 cm^-2. The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum is 3.4 x 10^-11 (3.7 x 10^-11) erg cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 4.2 (+3.5, -3.0) x 10^20 cm^-2
Galactic foreground: 1.2 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index: 1.90 (+0.16, -0.15)
If the light curve continues to decay with a power-law decay index of
0.59, 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 7.7 x
10^-13 (8.5 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/00680655.
This circular is an official product of the Swift-XRT team.
GCN Circular 19237
Subject
GRB 160327A: Enhanced Swift-XRT position
Date
2016-03-27T12:23:41Z (10 years ago)
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 1040 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 160327A, 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 = 146.70264, +54.01278 which is equivalent
to:
RA (J2000): 09h 46m 48.63s
Dec (J2000): +54d 00' 46.0"
with an uncertainty of 1.8 arcsec (radius, 90% confidence).
This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).
This circular was automatically generated, and is an official product of the
Swift-XRT team.
GCN Circular 19236
Subject
GRB 160327A: RATIR Optical and NIR Afterglow Detection
Date
2016-03-27T11:52:25Z (10 years ago)
From
V. Zach Golkhou at ASU/RATIR <golkhou@gmail.com>
V. Zach Golkhou (ASU), Nat Butler (ASU), Alan M. Watson (UNAM), Alexander
Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM), Ori Fox
(STScI), J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara
(GSFC/STScI), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), Jos�� A. de Diego (UNAM), Leonid Georgiev (UNAM), Jes��s
Gonz��lez (UNAM), Carlos Rom��n-Z����iga (UNAM), Neil Gehrels (GSFC), Harvey
Moseley (GSFC), John Capone (UMD), and Vicki Toy (UMD) report:
We observed the field of GRB 160327A (Racusin, et al., GCN 19235) with the
Reionization and Transients Infrared Camera (RATIR;www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astron��mico Nacional on
Sierra San Pedro M��rtir from 2016/03 27.39 to 2016/03 27.41 UTC (3.6
minutes to 0.58 hours after the BAT trigger), obtaining a total of 0.36
hours exposure in the r and i bands and 0.15 hours exposure in the Z, Y, J,
and H bands.
For a source within the Swift-XRT error circle, in comparison with the SDSS
DR9 and 2MASS catalogs, we obtain the following detections:
r 21.78 +/- 0.13
i 19.68 +/- 0.02
Z 18.55 +/- 0.02
Y 17.75 +/- 0.01
J 17.56 +/- 0.01
H 16.74 +/- 0.01
These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB. The source is located at RA, Dec =
9:46:48.54, +54:0:46.4 (J2000, +/-0.5").
Further observations are planned.
We thank the staff of the Observatorio Astron��mico Nacional in San Pedro
M��rtir.
GCN Circular 19235
Subject
GRB 160327A: Swift detection of a burst
Date
2016-03-27T09:35:51Z (10 years ago)
From
David Palmer at LANL <palmer@lanl.gov>
J. L. Racusin (NASA/GSFC), A. P. Beardmore (U Leicester),
K. L. Page (U Leicester) and D. M. Palmer (LANL) report on behalf of
the Swift Team:
At 09:16:07 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 160327A (trigger=680655). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 146.689, +54.017 which is
RA(J2000) = 09h 46m 45s
Dec(J2000) = +54d 01' 00"
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 ~3000 counts/sec (15-350 keV), at ~4 sec after the trigger.
The XRT began observing the field at 09:17:08.2 UT, 60.5 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
146.7019, 54.0131 which is equivalent to:
RA(J2000) = 09h 46m 48.45s
Dec(J2000) = +54d 00' 47.0"
with an uncertainty of 2.2 arcseconds (radius, 90% containment). This
location is 30 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 1.17
x 10^20 cm^-2 (Willingale et al. 2013).
The initial flux in the 2.5 s image was 1.01e-09 erg cm^-2 s^-1 (0.2-10
keV).
The prompt automatic UVOT analysis is not available at this time.
However, there appears to be no credible afterglow candidate in the
initial data.
Burst Advocate for this burst is J. L. Racusin (judith.racusin AT nasa.gov).
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)