GRB 110106A
GCN Circular 11593
Subject
GRB 110106A: CrAO optical observations
Date
2011-01-21T21:12:26Z (15 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
V. Rumyantsev, K. Antoniuk (CrAO), A. Pozanenko (IKI) report on behalf of
larger GRB follow-up collaboration:
We observed the field of the Swift GRB 110106A (Mangano et al., GCN 11520)
with AZT-11 telescope of CrAO starting on Jan. 06 (UT) 16:26. In the
enhanced Swift-XRT position (Osborne al., GCN 11526) we do not detect
optical afterglow candidate (Malesani et al., GCN 11524) up to R=21.9. We
clearly detect the nearby galaxy outside the error circle (Malesani et al.,
GCN 11524, Piranomonte et al., GCN 11530, Gorbovskoy et al., GCN 11542). The
photometry is based on the USNO B1.0 star 1541-0130790 (05:17:11.42
+64:10:11.0) assuming R=17.81. The finding chart can be found at
http://grb.rssi.ru/GRB110106A/grb110106a_110106_R_azt11.png
T0+ Filter, Exposure, mag.
(mid, d) (s)
0.06398 R 20x180 >21.9
GCN Circular 11580
Subject
GRB110106A, mm-radio observations
Date
2011-01-19T18:55:19Z (15 years ago)
From
Ashley Zauderer at CfA <bevinashley@gmail.com>
A. Zauderer (Harvard), D.A. Frail (NRAO), E. Berger (Harvard), and S.R.
Kulkarni (Caltech) report:
We observed the position of the intermediate-duration GRB 110106A
(GCN #11520) with the CARMA millimeter array starting on 2011 Jan.
16.827 UT (84 min after the burst) at a frequency of 92 GHz.
A total of 32 minutes were spent integrating on
source in good weather conditions (tau230 < 0.1). With baselines up
to ~1 km, we obtain a beam size of 3.3'' x 0.9'' (natural weighting).
We do not detect any sources within the revised XRT position
(GCN#11526) to a 5-sigma upper limit of 4.1 mJy/beam.
These observations are among the earliest millimeter wavelength
afterglow searches at milliJansky noise levels.
We thank the CARMA staff for their support of these observations.
GCN Circular 11542
Subject
Short GRB 110106A: MASTER OT observations
Date
2011-01-07T15:54:51Z (15 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina,
D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov,
D.Zimnukhov, M. Kornilov
Sternberg Astronomical Institute, Moscow State University
V.Krushinski, I.Zalozhnich, A. Popov
Ural State University, Kourovka
K.Ivanov, O.Chuvalaev, V.Poleschuk, E.Konstantinov, V.Lenok, O.Gres,
S.Yazev, N.M.Budnev,
Irkutsk State University
A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory
V.Yurkov, Yu.Sergienko, D.Varda, I.Kudelina
Blagoveschensk Educational State University, Blagoveschensk
MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in
Kislovodsk was pointed to the GRB110106A (Mangano et al., GCN Circ 1152) 17
sec s after notice time and 41 sec after GRB time at 2011-01-06 15:25:57.96 UT
in two polarizations+filter R (Gorbovskoy et al., GCN Circ 11523).
We marginally see OT about 16.0+-0.5 mag in XRT error box on second set
at 2011-01-06 15:26:19 (starting 69 s after trigger time with 10 sec
exposition, Gorbovskoy et al., GCN Circ 11523).
The OT positon:
RA= 05 17 13.98
DEC= 64 10 23.5
the error +-4" and coincident with late OT TNG position (Malesani
et al., GCN Circ 11524).
GRB trigger time: 15:25:16
Time UT T-T_trigger Exp Filter Mag
15:25:57 41 10 Cr >16,1
15:26:19 63 10 R+P 16,0+-0.5
15:26:40 84 20 R+P >16,6
15:27:11 115 20 R+P >16,6
15:27:42 146 30 R+P >17,0
15:28:23 187 40 R+P >17,2
15:29:14 238 50 R+P >17,4
15:30:15 299 60 R+P >17,5
15:31:26 370 70 R+P >17,7
15:32:47 451 90 R+P >17,9
15:34:28 552 110 R+P >18,0
15:36:29 673 130 R+P >18,1
15:38:51 815 160 R+P >18,3
15:41:42 986 180 R+P >18,3
15:44:53 1177 180 R+P >18,4
The more detailed data are available at
http://observ.pereplet.ru/images/GRB110106A/grb.html
We see the galaxy near (~8" distance, in our prevous Circ
11523 we not include the binning CCD scale = 4"/pix) OT on later images
with long exposition. The redshift z=0.093 (Piranomonte et al., GCN Circ
1130) is typical for short bursts.
The origin of the GRB110106A is no connected with massive star core
collapse because long distance from center of the host galaxy
(independently of the host galaxy type!). The
origin of the GRB connected with the NS+NS or NS+BH merging
(Lipunov et al.,1995, "Evolution of the Double Neutron Star Merging Rate
and the Cosmological Origin of Gamma-Ray Burst Sources", Astrophysical Journal
v.454, p.593.; Lipunov, 1997, Relativistic
Binary Merging Rates, The Invited Review on Joint Discussion "High
Energy Transients" on XXIIIrd General Assembly of IAU, Kioto, 1997,
http://adsabs.harvard.edu/abs/1997astro.ph.11270L).
The message may be cited.
mailto: lipunov@sai.msu.ru
GCN Circular 11539
Subject
GRB 110106A: TNG NIR observations
Date
2011-01-07T12:51:41Z (15 years ago)
From
Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst <malesani@dark-cosmology.dk>
D. Malesani (DARK/NBI), D. Fugazza (INAF/Brera), S. Covino (INAF/Brera),
L. Angelo Antonelli (INAF/Roma), A. Harutyunyan (INAF/TNG), G. Tessicini
(INAF/TNG), G. Andreuzzi (INAF/TNG), report on behalf of a larger
collaboration:
We observed the field of GRB 110106A (Mangano et al., GCN 11520) in the
K band with the 3.6m TNG equipped with NICS. A total of 60 min
integrations were obtained with a mean time Jan 7.07 UT (10.33 hr after
the GRB).
We detect no sources within the refined X-ray position (Osborne et al.,
GCN 11526; see also http://www.swift.ac.uk/xrt_positions), down to a
3-sigma limiting magnitude K > 20.3. We clearly detect the z=0.093
galaxy just outside the error circle (Malesani et al., GCN 11524;
Piranomonte et al., GCN 11530), with a magnitude K=14.90 +- 0.06
(calibration against 2MASS stars in the field).
GCN Circular 11536
Subject
GRB 110106A: ISAS-Kanazawa optical upper limit
Date
2011-01-07T05:48:17Z (15 years ago)
From
Daisuke Yonetoku at Kanazawa U <gcn@astro.s.kanazawa-u.ac.jp>
T. Yatsu, Y. Nishikawa, D. Yonetoku, T. Murakami and S. Gima (Kanazawa University)
on behalf of the ISAS-Kanazawa collaboration, report:
We observed the field of GRB 110106A (Mangano et al., GCN 11520) in Rc-band,
using the 1.3m ISAS-Kanazawa telescope, located at Sagamihara.
The observation started on Jan 6.64375 UT at ~2 min after the burst.
No any new source was found within the revised position of X-ray
counterpart (Osborne et al., GCN 11526), down to the 3 sigma upper limit
of Rc~17.6 mag.
GCN Circular 11535
Subject
GRB 110106A: MITSuME Okayama optical upper limits
Date
2011-01-07T04:51:09Z (15 years ago)
From
Daisuke Kuroda at OAO/NAOJ <dikuroda@oao.nao.ac.jp>
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 the MITSuME collaboration:
We observed the field of GRB 110106A (Mangano et al., GCN 11520)
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 2011-01-06 15:26:22 UT (~65 sec after
the burst). We did not find any new point source within the
enhanced XRT error circle (Osborne et al., GCNC 11526) in all
the three bands.
Three sigma upper limits of the OT are listed below. We used
GSC2.3 catalog for flux calibration.
T0+[day] MID-UT T-EXP[sec] g' Rc Ic
------------------------------------------------------
0.00424 15:31:23 540.0 >20.0 >19.7 >18.8
0.09936 17:48:21 5040.0 >20.8 >20.4 >19.5
------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]
GCN Circular 11531
Subject
GRB 110106A: Swift/UVOT Upper Limits
Date
2011-01-07T00:53:06Z (15 years ago)
From
Stephen Holland at USRA/NASA/GSFC/SSC <Stephen.T.Holland@nasa.gov>
S. T. Holland (CRESST/USRA/GSFC) and
V. Mangano (INAF-IASFP)
report on behalf of the Swift/UVOT team:
The Swift/UVOT observed the field of GRB 110106A starting 92 s
after the BAT trigger (Mangano, et al., 2011, GCN Circ. 11520).
Settled observations started at 110 s. We do no detect an optical
afterglow in any of the UVOT filters. Preliminary 3-sigma upper
limits for detecting a source in the finding charts and in the
co-added images, are
Filter T_start T_stop Exp(s) Mag
-----------------------------------------------
white (fc) 110 162 52 >20.2
3530 3680 150 >20.3
v 3687 16,046 1278 >20.3
b 4508 10,281 1082 >21.1
u 4302 5939 393 >20.4
uvw1 4097 5734 393 >20.2
uvm2 3892 5529 393 >20.1
uvw2 4918 11,717 706 >20.9
white 110 11,194 1280 >22.0
-----------------------------------------------
The quoted magnitudes and upper limits have not been corrected
for the expected Galactic extinction along the line of sight
corresponding to a reddening of E_{B-V} = 0.24 mag (Schlegel, et al.,
1998, ApJS, 500, 525). All photometry is on the UVOT photometry
system described in Poole et al. (2008, MNRAS, 383, 627).
GCN Circular 11530
Subject
GRB 110106A: TNG redshift of the closeby galaxy
Date
2011-01-07T00:43:11Z (15 years ago)
From
Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst <malesani@dark-cosmology.dk>
S. Piranomonte (INAF/Roma), D. Malesani (DARK/NBI), V. D'Elia (ASDC and
INAF/Roma), S. Covino (INAF/Brera), L.A. Antonelli (INAF/Roma), D.
Fugazza (INAF/Brera), A. Harutyunyan (INAF/TNG), G. Tessicini
(INAF/TNG), report on behalf of a larger collaboration:
Following the release of the refined X-ray position (Osborne et al., GCN
11526) of the afterglow of GRB 110106A (Mangano et al., GCN 11520), we
further inspected our TNG images. The faint object reported by Malesani
et al. (GCN 11524) is significantly outside the revised error circle,
and is thus likely unrelated to the GRB.
The new X-ray position however partially covers the outskirts of the
extended object mentioned in GCN 11520.
A 1-hr TNG spectrum of this galaxy, starting on Jan 6.878 UT (5.64 hr
after the GRB) and covering the wavelength range 3800-8000 AA, reveals
the presence of a few emission features, which we interpret as Halpha,
[NII] 6583, [SII] 6730, and weak Hbeta at a common redshift z=0.093. At
the same redshift, we also see Ca H and K in absorption.
While the XRT error circle (1.7" radius) overlaps the stellar light from
the galaxy, its center lies 4.3" away of the galaxy nucleus (7.3 kpc in
projection at z=0.093). Such large offset would be more typical of
short-duration GRBs, although the duration of GRB 110106A (T90 =
4.3+-1.1 s; Stamatikos et al., GCN 11527) seems to exclude this
hypothesis. The relation between the galaxy and the GRB cannot be
conclusively established at this point.
GCN Circular 11529
Subject
GRB 110106A: Swift-XRT refined Analysis
Date
2011-01-07T00:29:39Z (15 years ago)
From
Vanessa Mangano at INAF-IASFPA <vanessa@ifc.inaf.it>
V. Mangano (INAF-IASFPA) and B. Sbarufatti (INAF-OAB/INAF-IASFPA)
report on behalf of the Swift-XRT team:
We have analysed 7.0 ks of XRT data for GRB 110106A (Mangano et al.
GCN Circ. 11520), from 91 s to 17.3 ks after the BAT trigger. The data
comprise 8 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 Osborne et al. (GCN. Circ
11526).
The late-time light curve (from T0+3.5 ks) can be modelled with a
power-law decay with a decay index of alpha=1.2 (+0.4, -0.3).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.7 (+0.4, -0.5). The
best-fitting absorption column is 4.0 (+1.6, -1.4) x 10^21 cm^-2, in
excess of the Galactic value of 1.3 x 10^21 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum is 3.4 x 10^-11 (1.0 x 10^-10) erg
cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 4.0 (+1.6, -1.4) x 10^21 cm^-2
Galactic foreground: 1.3 x 10^21 cm^-2
Excess significance: 4.8 sigma
Photon index: 2.7 (+0.4, -0.5)
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00441664.
This circular is an official product of the Swift-XRT team.
GCN Circular 11527
Subject
GRB 110106A: Swift-BAT refined analysis
Date
2011-01-06T23:36:30Z (15 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@lheamail.gsfc.nasa.gov>
M. Stamatikos (OSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), V. Mangano (INAF-IASFPA),
D. M. Palmer (LANL), A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC),
G. Sato (ISAS), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
Using the data set from T-61 to T+242 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 110106A (trigger #441664)
(Mangano, et al., GCN Circ. 11520). The BAT ground-calculated position is
RA, Dec = 79.295, 64.199 deg, which is
RA(J2000) = 05h 17m 10.8s
Dec(J2000) = +64d 11' 56.4"
with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 34%.
The mask-weighted light curve shows a pulse starting at ~T-1 sec and
lasting about 6 sec. T90 (15-350 keV) is 4.3 +- 1.1 sec
(estimated error including systematics).
The time-averaged spectrum from T-1.0 to T+3.9 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.71 +- 0.28. The fluence in the 15-150 keV band is 3.0 +- 0.5 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.32 sec in the 15-150 keV band
is 1.9 +- 0.3 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/441664/BA/
GCN Circular 11526
Subject
GRB 110106A: Enhanced Swift-XRT position
Date
2011-01-06T21:53:09Z (15 years ago)
From
Phil Evans at U of Leicester <pae9@star.le.ac.uk>
J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester)
report on behalf of the Swift-XRT team.
Using 3088 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 110106A, 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 = 79.30578, +64.17349 which is equivalent
to:
RA (J2000): 05h 17m 13.39s
Dec (J2000): +64d 10' 24.6"
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 11524
Subject
GRB 110106A: TNG optical observations and candidate counterparts
Date
2011-01-06T21:38:53Z (15 years ago)
From
Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst <malesani@dark-cosmology.dk>
D. Malesani (DARK/NBI), S. Covino (INAF/Brera), L.A. Antonelli
(INAF/Roma), D. Fugazza (INAF/Brera), A. Harutyunyan (INAF/TNG),
G. Tessicini (INAF/TNG) on behalf of the CIBO collaboration, report:
We observed the field of GRB 110106A (Mangano et al., GCN 11520) using
the 3.6m TNG telescope, located in the Canary Islands. A set of R- and
I-band images were acquired starting on Jan 6.8265 UT (4.41 hr after the
GRB) for a total exposure time of 20 minutes per filter. The seeing was
1.5" in the R band.
Within the XRT error circle (Mangano et al., GCN 11520), we marginally
detect a source in both R and I. Its coordinates are (J2000):
RA = 05:17:14.14
Dec = 64:10:28.1
and its magnitude is R ~ 24.5. In addition, we note the presence of a
galaxy just outside the current X-ray error circle (its centroid being
7.3+-3.6" away of the XRT position). It is visible also in the DSS
images and has a magnitude R = 18.2 (assuming R = 17.54 for the star at
RA=05:17:11.43, Dec=+64:10:10.88).
We cannot assess whether any of the sources are variable, and so their
relation to GRB 110106A remains to be proven.
Further observations are in progress.
[GCN OPS NOTE(06jan11): Per author's request, GT was added to the author list.]
GCN Circular 11523
Subject
GRB 110106A: MASTER optical observations
Date
2011-01-06T21:14:51Z (15 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina,
D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov,
D.Zimnukhov, M. Kornilov
Sternberg Astronomical Institute, Moscow State University
V.Krushinski, I.Zalozhnich, A. Popov
Ural State University, Kourovka
K.Ivanov, O.Chuvalaev, V.Poleschuk, E.Konstantinov, V.Lenok, O.Gres,
S.Yazev, N.M.Budnev,
Irkutsk State University
A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory
V.Yurkov, Yu.Sergienko, D.Varda, I.Kudelina
Blagoveschensk Educational State University, Blagoveschensk
MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Kislovodsk was pointed to the GRB110106A (Mangano et al., GCN
Circ 1152) 17 sec s after notice time and 41 sec after GRB time at
2011-01-06 15:25:57.96 UT in two polarizations+filter R. On our
first (10s exposure) set we haven`t found optical transient within SWIFT
XRT error-box.
The 5-sigma upper limit has been about 16.0mag
We marginally see OT about 15.5 mag in XRT error box on second set at
2011-01-06 15:26:19 (starting 69 s after trigger time with 10 sec
exposition).
We see the like galaxy object near (~15" distance) XRT error box ~19-20
mag on later images. But, there is no object in NASA/IPAC EXTRAGALACTIC
DATABASE.
The same object is presented at DSS image.
The redaction is continueted.
The message may be cited.
mailto: lipunov@sai.msu.ru
GCN Circular 11521
Subject
GRB110106A: Xinglong TNT upper limit
Date
2011-01-06T17:05:02Z (15 years ago)
From
L.P. Xin at NAOC <xlp@bao.ac.cn>
L.P. Xin, Z. X. Ling, Y.L. Qiu, J.Y. Wei, J. Wang, J.S. Deng,
C. Wu, X. H. Han on behalf of EAFON report:
We began to observe GRB110106A (Mangano et al., GCN 11520 )
with Xinglong TNT telescope at 15:35:15.946 (UT), 10min after
the burst. A series of white and R-band images were obtained.
No any new source was found within the errorbox of X-ray
counterpart (Mangano et al., GCN 11520 ), down to 3 sigma
upper limit of R~19.8 mag at the mean time of 11 min after
the burst.
This message may be cited.
For more information about Xinglong GRBs Follow-up
observations, please visit the website:
http://www.xinglong-naoc.org/grb/
GCN Circular 11520
Subject
GRB 110106A: Swift detection of a burst
Date
2011-01-06T15:37:15Z (15 years ago)
From
David Palmer at LANL <palmer@lanl.gov>
V. Mangano (INAF-IASFPA), A. P. Beardmore (U Leicester),
D. N. Burrows (PSU), P. A. Evans (U Leicester),
N. Gehrels (NASA/GSFC), J. M. Gelbord (PSU), C. Gronwall (PSU),
C. Guidorzi (U Ferrara), S. T. Holland (CRESST/USRA/GSFC),
J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA),
O. M. Littlejohns (U Leicester), C. B. Markwardt (NASA/GSFC),
F. E. Marshall (NASA/GSFC), P. T. O'Brien (U Leicester),
C. Pagani (U Leicester), K. L. Page (U Leicester),
D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/IASFPA),
M. H. Siegel (PSU), M. Stamatikos (OSU/NASA/GSFC),
R. L. C. Starling (U Leicester), M. C. Stroh (PSU),
E. Troja (NASA/GSFC/ORAU) and T. N. Ukwatta (GSFC/GWU) report on
behalf of the Swift Team:
At 15:25:16 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 110106A (trigger=441664). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 79.285, +64.184 which is
RA(J2000) = 05h 17m 08s
Dec(J2000) = +64d 11' 02"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a double-peaked
structure with a total duration of about 4 sec. The peak count rate
was ~1000 counts/sec (15-350 keV), at ~0 sec after the trigger.
The XRT began observing the field at 15:27:02.4 UT, 106.2 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 79.30730, 64.17394 which is equivalent
to:
RA(J2000) = 05h 17m 13.75s
Dec(J2000) = +64d 10' 26.2"
with an uncertainty of 4.8 arcseconds (radius, 90% containment). This
location is 49 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. 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 (1.27 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 4.3
(+4.88/-3.82) x 10^21 cm^-2 (90% confidence).
UVOT took a finding chart exposure of 52 seconds with the White filter
starting 109 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
BAT 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
0.24.
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.)