GRB 220412A
GCN Circular 32326
Subject
GRB220412A: VIRT Optical Upper Limit
Date
2022-07-05T17:53:31Z (4 years ago)
From
Priyadarshini Gokuldass at U. of the Virgin Islands <priyadass.94@gmail.com>
K. Noonan (UVI), P. Gokuldass (Florida Institute of Technology), N. Orange
(OrangeWave Innovative Science, LLC), K. Smith (UVI), D. Morris (UVI)
report:
We observed the field of GRB220412A (N. J. Klingler et al., GCN 31881) with
the 0.5m Virgin Island Robotic Telescope (VIRT) at the University of the
Virgin Islands' Etelman Observatory on 04-13-2022 starting at 00:11:58.73
UT (T+17.30 hrs). We performed a series of exposures in the R filter with a
total exposure of 4000 s. The weather conditions were partly cloudy during
the hours of observation with an average airmass of 1.25.
We find no new source within the enhanced XRT position error circle (P. A.
Evans et al., 31887) and report the following 5-sigma upper limit:
T_mid ||Exposure ||Filter ||Limit
T+ 18.2 hrs ||4000s ||R ||>20.8
The limit is estimated from comparison to nearby USNO B1 stars and is not
corrected for Galactic extinction. The VIRT is still in the commissioning
phase.
We acknowledge financial support from NASA MUREP MIRO award 80NSSC21M0001, NASA
EPSCoR award 80NSSC19M0060, and NSF EiR award 1901296.This message can be
cited.
GCN Circular 31903
Subject
GRB 220412A: GRANDMA observations
Date
2022-04-15T12:13:31Z (4 years ago)
From
Patrice Hello at LAL <hello@lal.in2p3.fr>
Subject Line:
GRB 220412A: GRANDMA observations
Content:
S. Beradze (AbAO), U. Bhardwaj (GRAPPA), T. Culino (ESILV), P. Hello
(IJCLAB), M. Masek (FZU), G. Raaijmakers (GRAPPA), Y. Rajabov (UBAI),
T. Sadibekova (AIM/CEA-UPS), F. Z. Guo (THU), X. F. Wang (THU/BJP), Y.
Zhu (NAOC), J. Zhang (NAOC), D. A. Kann (HETH/IAA-CSIC), K. Noysena
(NARIT), A. Kaouech (OUCA/KNC) C. Rinner (OUCA), Z. Benkhaldoun (OUCA),
S. Antier (OCA/Artemis), P. A. Duverne (IJCLAB), M. Freeberg (KNC),
R. Hainich (UP), F. Runger (UP), S. Karpov (FZU), A. Simon (Kyiv Univ),
A. Baransky (Kyiv Univ) and V. Godunova (IC ICAMER)
report on behalf of GRANDMA collaboration:
The GRANDMA telescope network responded to the alert of GRB 220412A
(N. J. Klingler et al. GCNC 31881, P.A. Evans et al. GCN 31887,
A. D'Ai et al. GCN 31888, K.L. Page et al GCN 31890).
The first observations started ** h after the SWIFT BAT trigger time.
We did not detect the optical afterglow within the first 24 h.
Upper limits are given in the AB system, at 3-sigma.
T-T0(hr)| MJD������ | Observatory�� | Exposure| Filter | Upp. Lim. (AB)
_____________________________________________________
05.55 |59681.50689|Xinglong-2.16m|12*300s������ |�� R�������� |���� 19.5
14.02 |59681.86193|OST/CDK20�������� |18*180s������ |�� R�������� |���� 17.8
14.07 |59681.85977|OST/CDK20�������� |17*180s������ |�� I�������� |���� 17.0
17.36 |59681.99881|KNC-HAO������������ |5*180s�������� |�� L������ �� |���� 17.3
21.18 |59682.15807|TRT-SRO������������ |10*60s�������� |�� V ������ �� |���� 18.1
21.35 |59682.16537|TRT-SRO������������ |10*60s�������� |�� R ������ �� |���� 17.7
21.53 |59682.17271|TRT-SRO������������ |10*60s�������� |�� I ������ �� |���� 17.1
21.95 |59682.19014|KNC-T24������������ |3300s���������� |�� I ������ �� |���� 18.1
The observations were contaminated by the moon.
These upper limits are consistent with previous reports of detections by
RATIR (Alan M. Watson et al., GCN 31882 & GCN 31902) and the upper limits
provided by UVOT (A. Breeveld and N. Klingler, GCN 31885), MITSuME Akeno
(K. L. Murata et al., GCN 31891).
The Xinglong-2.16m and TRT-SRO data have been calibrated using nearby stars
from the Pan-STARRS catalog. The measurements for�� Xinglong-2.16m provided
by the STDPipe pipeline (Karpov 2022). The OST data have been using CDK
filter and calibrated with USNO-B1.0 Catalog (Monet+ 2003). The KNC-T24 and
KNC-HAO images have been calibrated using field stars from the
PanSTARRS-DR1
catalog, measured with the MUPHOTEN pipeline (Duverne et al. 2021).
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 31902
Subject
GRB 220412A: Continued RATIR Observations and Steepening of the Light Curve
Date
2022-04-14T20:00:57Z (4 years ago)
From
Alan M Watson at UNAM <alan@astro.unam.mx>
Alan M. Watson (UNAM), Nat Butler (ASU), Eleonora Troja (UTV), Alexander Kutyrev
(GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM), Ori Fox (STScI), J.
Xavier Prochaska (UCSC), Josh Bloom (UCB), Enrico Ramirez-Ruiz (UCSC), Jes��s
Gonz��lez (UNAM), Carlos Rom��n-Z����iga (UNAM), Harvey Moseley (GSFC), Rosa L.
Becerra (UNAM), Simone Dichiara (PSU), and Oc��lotl L��pez (UNAM) report:
We observed the field of GRB 220412A (Klingler et al. GCN 31881) with the
Reionization and Transients Infrared Camera (RATIR) on the 1.5m Harold Johnson
Telescope at the Observatorio Astron��mico Nacional on Sierra San Pedro M��rtir
from 2022-04-14 03:28 to 07:30 UTC (44.9 to 48.9 hours after the trigger)
obtaining 2.31 hours of exposure in the i band.
In comparison with the SDSS DR9 catalog, the afterglow candidate reported by
Watson et al. (GCN Circ. 31882, 31898) is detected at i = 21.51 +/- 0.10.
We note that the optical light curve appears to have steepened. The temporal
index between our observations at 21 hours (Watson et al., GCN Circ 31898) and
47 hours is close to -1.0.
Further observations are continuing.
We thank the staff of the Observatorio Astron��mico Nacional in San Pedro M��rtir.
GCN Circular 31901
Subject
GRB 220412A: BOOTES-network optical upper limits
Date
2022-04-14T00:05:31Z (4 years ago)
From
Youdong HU at IAA-CSIC <huyoudong072@hotmail.com>
Y.-D. Hu, E. Fernandez-Garcia, A. J. Castro-Tirado, T.-R. Sun, M. D. Caballero-Garcia, R. Sanchez-Ramirez (IAA-CSIC), D. Hiriart and W. H. Lee (UNAM), C. Perez del Pulgar, A. Castellon, I. Carrasco, A. Reina (Univ. de Malaga), I. H. Park (SKKU) and F. Rendon (IAA-CSIC and INTA-CEDEA) on behalf of a larger collaboration, report:
Following the detection of GRB 220412A by Swift (Klingler et al., GCNC 31881), the 0.3m BOOTES-1B robotic telescope in Mazagon (Huelva), southern Spain, automatically responded to this burst on Apr 12 at 22:41 UT (i.e. ~16.1 hours after trigger). In the co-added frame (52 x 60 s, clear filter), no source is detected within the enhanced XRT position (Evans et al., GCNC 31887) down to 19.2 mag.
Later on, the 60cm BOOTES-5/JGT robotic telescope at Observatorio Astronomico Nacional in San Pedro Martir (Mexico) automatically responded to this burst on Apr 13 at 03:33 UT (i.e. ~ 21 hrs after trigger). In the co-added image (45 x 60 s, clear filter), no optical afterglow is detected within the enhanced XRT position (Evans et al., GCNC 31887) down to 20.3 mag.
Although the candidate reported by RATIR (Watson et al. GCNC 31882, GCNC 31898) is not detected, those non-detections are consistent with the reports from Swift/UVOT (Klingler et al., GCNC 31881, Breeveld et al. GCNC 31885), MITSuME (Murata et al. GCNC 31891) and MASTER-Net (Lipunov et al., GCNC 31880).
We thank the staff at INTA-CEDEA and San Pedro Martir Observatory for their excellent support.
GCN Circular 31899
Subject
GRB 220412A: Swift-BAT refined analysis
Date
2022-04-13T21:01:24Z (4 years ago)
From
Tyler Parsotan at UMBC/GSFC/CRESST II <parsotat@umbc.edu>
T. Parsotan (GSFC/UMBC), S. D. Barthelmy (GSFC),
H. A. Krimm (NSF), S. Laha (GSFC/UMBC),
A. Y. Lien (U Tampa), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU) (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 220412A (trigger #1102281)
(Klingler et al. GCN Circ. 31881). The BAT ground-calculated position is
RA, Dec = 123.975, 30.336 deg which is
RA(J2000) = 08h 15m 54.0s
Dec(J2000) = +30d 20' 08.5"
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 92%.
The BAT light curve showed a complex
structure with a duration of about 20 sec. The peak count rate
was ~900 counts/sec (15-350 keV), at ~1 sec after the trigger.
T90 (15-350 keV) is 41.66 +- 7.00 sec (estimated error including systematics).
The time-averaged spectrum from T-11.07 to T+38.00 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.53 +- 0.21. The fluence in the 15-150 keV band is 5.9 +- 0.9 x 10^-07 erg/cm2.
The 1-sec peak photon flux measured from T+6.88 sec in the 15-150 keV band
is 0.5 +- 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/1102281/BA/
GCN Circular 31898
Subject
GRB 220412A: RATIR Observations of the Fading Afterglow
Date
2022-04-13T20:05:34Z (4 years ago)
From
Alan M Watson at UNAM <alan@astro.unam.mx>
Alan M. Watson (UNAM), Nat Butler (ASU), Eleonora Troja (UTV), Alexander
Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM), Ori Fox
(STScI), J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Enrico Ramirez-Ruiz
(UCSC), Jes��s Gonz��lez (UNAM), Carlos Rom��n-Z����iga (UNAM), Harvey Moseley
(GSFC), Rosa L. Becerra (UNAM), Simone Dichiara (PSU), and Oc��lotl L��pez (UNAM)
report:
We observed the field of GRB 220412A (Klingler et al. GCN 31881) with the
Reionization and Transients Infrared Camera (RATIR) on the 1.5m Harold Johnson
Telescope at the Observatorio Astron��mico Nacional on Sierra San Pedro M��rtir
from 2022-04-12 06:39 to 06:56 UTC (0.04 to 0.33 hours after the trigger) and
2022-04-13 03:16 to 04:38 UTC (20.65 to 22.00 hours after the trigger) obtaining
totals of 0.21 and 1.07 hours of exposure in the i band.
In comparison with the SDSS DR9 catalog, the afterglow candidate reported by
Watson et al. (GCN Circ. 31882) has faded from i = 19.27 +/- 0.10 to i = 20.64
+/- 0.08. This photometry for the first night supersedes the preliminary
photometry reported by Watson et al.
We note that the optical light curve does not seem to show the same steep
decline as the XRT light curve reported by the UKSSDC. From 0.33 to 21 hours,
the XRT light curve falls by a factor of about 50, whereas our photometry only
falls by a factor of about 3.5.
We have checked the SDSS DR9 i image, and there is no apparent host galaxy
present at the position of the afterglow bright enough to explain the
apparent slow decline.
Further observations are planned.
We thank the staff of the Observatorio Astron��mico Nacional in San Pedro M��rtir.
GCN Circular 31891
Subject
GRB 220412A: MITSuME Akeno optical upper limits
Date
2022-04-13T05:35:44Z (4 years ago)
From
Katsuhiro L. Murata at Nagoya U <murata@u.phys.nagoya-u.ac.jp>
K. L. Murata, M. Niwano, Y. Imai, N. Ito, Y. Takamatsu, S. Sato, R.
Hosokawa, M. Sasada, Y. Yatsu, and N. Kawai (Tokyo Tech) report on behalf
of the MITSuME collaboration:
We observed the field of GRB 220412A (Klingler et al. GCN Circular #31881,
Watson et al. GCN Circular #31882, Breeveld and Klingler et al. GCN
Circular #31885, Evans et al. GCN Circular #31887, D'Ai et al. GCN Circular
#31888) with the optical three color (g', Rc, and Ic) CCD cameras attached
to the MITSuME 50 cm telescope Akeno. The observation with a series of 60
sec exposures started at 2022-04-12 10:10:00 UT (214 minutes after the
Swift/BAT trigger). We stacked the images with good conditions. We did not
detect any uncatalogued sources within the enhanced XRT error region (Evans
et al. GCN Circular #31887). We obtained the 5-sigma limits of the stacked
images as follows.
T0+[min] MID-UT T-EXP[sec] 5-sigma limits
------------------------------------------------------------------------------------------------
214 2022-04-12 10:53:37 3960 g'>19.0, Rc>19.3, Ic>18.8
------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used the PS1 catalog for flux calibration. The magnitudes are expressed
in the AB system. The images were processed in real-time through the
MITSuME GPU reduction pipeline (Niwano et al. 2021, PASJ, Vol.73, Issue 1,
Pages 4-24; https://github.com/MNiwano/Eclaire).
GCN Circular 31890
Subject
Correction to GCN 31888: GRB 220412A: Swift-XRT refined Analysis
Date
2022-04-13T05:34:52Z (4 years ago)
From
Kim Page at U.of Leicester <klp5@leicester.ac.uk>
K.L. Page (U. Leicester) reports on behalf of the Swift-XRT team:
In GCN 31888, the fit to the XRT light curve was stated incorrectly. There
correct details are as follows:
The light curve can be modelled with an initial power-law decay with an
index of alpha=2.10 (+0.08, -0.07), followed by a break at T+1330 s to
an alpha of 0.98 (+0.13, -0.28).
If the light curve continues to decay with a power-law decay index of
0.98, the count rate at T+24 hours will be 1.9e-03 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 7.4 x 10^-14
(8.1 x 10^-14) erg cm^-2 s^-1.
The remaining details in GCN 31888 were correct. We apologise for any
inconveniece.
This circular is an official product of the Swift-XRT team.
GCN Circular 31888
Subject
GRB 220412A: Swift-XRT refined Analysis
Date
2022-04-13T03:20:26Z (4 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
A. D'Ai (INAF-IASFPA), J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto),
B. Sbarufatti (PSU), A.P. Beardmore (U. Leicester), P.A. Evans (U.
Leicester), J.P. Osborne (U. Leicester), A. Melandri (INAF-OAB), T.
Sbarrato (INAF-OAB) and N.J. Klingler report on behalf of the Swift-XRT
team:
We have analysed 8.6 ks of XRT data for GRB 220412A (Klingler et al.
GCN Circ. 31881), from 106 s to 68.7 ks after the BAT trigger. The
data comprise 158 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 enhanced XRT position for this burst was given by Evans
et al. (GCN Circ. 31887).
The light curve can be modelled with an initial power-law decay with an
index of alpha=2.10 (+0.08, -0.07), followed by a break at T+4017 s to
an alpha of 0.0 (+0.0, -1.1).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.02 (+0.18, -0.09). The
best-fitting absorption column is consistent with the Galactic value
of 3.7 x 10^20 cm^-2 (Willingale et al. 2013). The PC mode spectrum has
a photon index of 1.68 (+0.22, -0.18) and a best-fitting absorption
column of 5.7 (+5.9, -2.0) x 10^20 cm^-2. The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum is 3.9 x 10^-11 (4.3 x 10^-11) erg cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 5.7 (+5.9, -2.0) x 10^20 cm^-2
Galactic foreground: 3.7 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index: 1.68 (+0.22, -0.18)
If the light curve continues to decay with a power-law decay index of
0.0, the count rate at T+24 hours will be 0.011 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.4 x
10^-13 (4.7 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/01102281.
This circular is an official product of the Swift-XRT team.
GCN Circular 31887
Subject
GRB 220412A: Enhanced Swift-XRT position
Date
2022-04-12T18:40:00Z (4 years ago)
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 1814 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 220412A, 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 = 123.96809, +30.34259 which is equivalent
to:
RA (J2000): 08h 15m 52.34s
Dec (J2000): +30d 20' 33.3"
with an uncertainty of 3.7 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.
GCN Circular 31885
Subject
GRB 220412A: Swift/UVOT Upper Limits
Date
2022-04-12T16:20:20Z (4 years ago)
From
Alice Breeveld at MSSL-UCL <a.breeveld@ucl.ac.uk>
A. Breeveld (UCL-MSSL) and N. Klingler (GSFC/UMBC/CRESSTII) report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 220412A 127 s after the BAT trigger
(Klingler et al., GCN Circ. 31881).
No optical afterglow consistent with the RATIR position (Watson et al., GCN Circ. 31882) 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) exposures and subsequent exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
white_FC 127 276 147 >20.5
u_FC 285 479 191 >19.6
white 566 758 34 >19.7
b 542 734 34 >18.97
v 616 1059 53 >18.18
uvw1 665 857 34 >18.25
uvw2 592 1039 58 >18.64
uvm2 813 833 20 >17.37
The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of
E(B-V) = 0.0373 in the direction of the burst (Schlegel et al. 1998).
GCN Circular 31882
Subject
GRB 220412A: RATIR Afterglow Candidate
Date
2022-04-12T07:25:10Z (4 years ago)
From
Alan M Watson at UNAM <alan@astro.unam.mx>
Alan M. Watson (UNAM), Eleonora Troja (UTV), Nat Butler (ASU), Alexander
Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM), Ori Fox
(STScI), J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Enrico Ramirez-Ruiz
(UCSC), Jes��s Gonz��lez (UNAM), Carlos Rom��n-Z����iga (UNAM), Harvey Moseley
(GSFC), Rosa L. Becerra (UNAM), Simone Dichiara (PSU), and Oc��lotl L��pez (UNAM)
report:
We observed the field of GRB 220412A (Klingler et al. GCN 31881) with the
Reionization and Transients Infrared Camera (RATIR) on the 1.5m Harold Johnson
Telescope at the Observatorio Astron��mico Nacional on Sierra San Pedro M��rtir
from 2022/04 12.28 to 2022/04 12.29 UTC (0.1 to 0.5 hours after the BAT
trigger), obtaining a total of 0.21 hours exposure in the r and i bands and 0.08
hours exposure in the Z, Y, J, and H bands.
We detect a bright, uncataloged source at RA = 123.967275 and declination =
30.342693 degrees (J2000), about 5.5 arcsec to the east of the current Swift XRT
SPER position. In comparison with the SDSS DR9 and 2MASS catalogs, we obtain the
following magnitudes:
r = 19.41 +/- 0.12
i = 19.26 +/- 0.10
Y = 19.11 +/- 0.23
These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.
Despite being slightly outside the current XRT error region, we suggest that
this source is likely to be the afterglow. Observations are continuing.
We thank the staff of the Observatorio Astron��mico Nacional in San Pedro M��rtir.
GCN Circular 31881
Subject
GRB 220412A: Swift detection of a burst
Date
2022-04-12T06:53:12Z (4 years ago)
From
Noel Klingler at NASA-GSFC / UMBC <njk5441@psu.edu>
N. J. Klingler (GSFC/UMBC/CRESSTII), J.D. Gropp (PSU),
K. L. Page (U Leicester), D. M. Palmer (LANL),
T. M. Parsotan (GSFC/UMBC/CRESSTII), B. Sbarufatti (PSU) and
A. Tohuvavohu (U Toronto) report on behalf of the Neil Gehrels Swift
Observatory Team:
At 06:36:50 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 220412A (trigger=1102281). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 123.968, +30.322 which is
RA(J2000) = 08h 15m 52s
Dec(J2000) = +30d 19' 19"
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 20 sec. The peak count rate
was ~900 counts/sec (15-350 keV), at ~1 sec after the trigger.
The XRT began observing the field at 06:38:52.9 UT, 122.7 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 123.96470, 30.34319 which is equivalent
to:
RA(J2000) = 08h 15m 51.53s
Dec(J2000) = +30d 20' 35.5"
with an uncertainty of 4.5 arcseconds (radius, 90% containment). This
location is 76 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. No
spectrum from the promptly downlinked event data is yet available to
determine the column density.
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 126 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
0.037.
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/)