GRB 110205A
GCN Circular 11740
Subject
GRB110205A: EVLA Observations
Date
2011-02-16T17:37:36Z (15 years ago)
From
Ashley Zauderer at CfA <bevinashley@gmail.com>
A. Zauderer (Harvard), D. Frail (NRAO), and E. Berger (Harvard) report:
We observed the position of GRB 110205A (GCN 11629) with the EVLA
starting 1.2 days after the burst. Preliminary reduction of these data
gives a flux density of 182 +/-12 microJy at a frequency of 22 GHz.
Further EVLA observations are on-going.
We thank the EVLA staff for their support of these observations.
GCN Circular 11726
Subject
GRB 110205A: Konkoly optical observations
Date
2011-02-14T15:40:15Z (15 years ago)
From
Janos Kelemen at Konkoly Obs/Hungary <kelemen@konkoly.hu>
J. Kelemen (kelemen at konkoly.hu) on behalf of the GRB OT observing program
at the Konkoly Observatory.
Starting on 05/02/2011 we observed the field of GRB 110205A detected
by Swift (trigger #444643; Beardmore et al., GCN 11629)) with a 60/90 cm
Schmidt telescope located at the Mountain Station of the Konkoly Observatory
using V,R,I filters. Although the OT was visible on the frames we coadded
images to achieve better S/N ratio due to the cloudy weather.
The time column contains seconds counting from the trigger (J.D. 2455597.58520)
Time Exp Mag. Error. Filter Flag.
[s] [s] [3-sigma]
-------------------------------------------------
61782 300 19.53 0.5 V
66022 1800 18.97 0.4 R
70312 300 19.63 0.4 V
71671 1500 19.92 0.5 R
74194 1500 20.11 0.5 I
75323 300 19.67 0.4 V
159722 2700 21.52 0.6 R Upper Level
--------------------------------------------------
GCN Circular 11697
Subject
Konus-Wind observation of GRB 110205A (correction to GCN 11659)
Date
2011-02-11T11:35:08Z (15 years ago)
From
Valentin Pal'shin at Ioffe Inst <val@mail.ioffe.ru>
V. Pal'shin report on behalf of the Konus-Wind team:
The isotropic equivalent energy and peak luminosity of GRB 110205A given
in GCN Circular 11659 have been erroneously computed.
The correct values for the isotropic equivalent energy is E_iso = (4.34
+/- 0.42)x10^53 erg, and for the isotropic peak luminosity is
(L_iso)_max = (1.95 +/- 0.27)x10^52 erg/s
(assuming z = 2.22 (Cenko & Hora, GCN 11638; Vreeswijk et al. GCN 11640)
and a standard cosmology model with H_0 = 71 km/s/Mpc, Omega_M = 0.27,
Omega_Lambda = 0.73).
I thank Max De Pasquale and Takanori Sakamoto for pointing this out to
me and I apologize for the error.
GCN Circular 11696
Subject
GRB 110205A: detection of optical linear polarization from CAHA
Date
2011-02-11T11:05:19Z (15 years ago)
From
Javier Gorosabel at IAA-CSIC <jgu@iaa.es>
J. Gorosabel (IAA-CSIC), R. Duffard (IAA-CSIC), P. Kubanek (IAA-CSIC & U. of Valencia), A. Guijarro (CAHA), report on behalf of a larger collaboration:
"We carried out optical linear polarization observations of the GRB 110205A afterglow (GCN Circ. 11629, Beardmore et al.) using the 2.2m telescope of the Calar Alto Observatory equipped with CAFOS. The data were acquired in the R-band on Feb 5.19879-5.26570 UT (2.73-4.33 hours post burst) with a total exposure time of 10x500s. A preliminary analysis reveals an afterglow linear polarization at a level of P~1.4%. This value is higher than the polarization (P ~< 0.4%) measured for the bright field stars, so we conclude that most of the measured afterglow polarization has very likely an extragalactic origin."
GCN Circular 11692
Subject
GRB 110205A: Swift/BAT and Suzaku/WAM joint spectral analysis
Date
2011-02-10T18:55:44Z (15 years ago)
From
Takanori Sakamoto at NASA/GSFC <Taka.Sakamoto@nasa.gov>
T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
S. Sugita (Nagoya U.), K. Yamaoka (Aoyama Gakuin U.), N. Vasquez (Tokyo Tech.),
T. Uehara, Y. Hanabata, T. Takahashi, Y. Fukazawa (Hiroshima U.),
Y. Terada, M. Tashiro, W. Iwakiri, K. Takahara, T. Yasuda (Saitama U.),
M. Ohno, M. Suzuki, M. Kokubun, T. Takahashi (ISAS/JAXA),
Y. E. Nakagawa, T. Tamagawa (RIKEN), N. Ohmori, A. Daikyuji, Y. Nishioka,
M. Yamauchi (Univ. of Miyazaki), Y. Urata, P. Tsai (NCU),
K. Nakazawa, K. Makishima (Univ. of Tokyo), S. Hong (Nihon U.)
(i.e. the Suzaku WAM team):
We performed the Swift/BAT and the Suzaku/WAM joint spectral analysis
of GRB 110205A (Swift/BAT trigger #444643: Beardmore et al., GCN Circ.
11629, Markwardt et al. GCN Circ. 11646). The joint spectral analysis
of the Swift/BAT and the Suzaku/WAM data allows us to derive the broad-band
spectral parameters of this burst.
The time interval of the spectral data for each instrument is chosen
from T0(BAT)+20.2 to T0(BAT)+318.2 sec where T0(BAT) is the trigger time
of BAT at 02:02:41.3 UTC. The energy ranges which we used in the joint
spectral analysis are 15-150 keV and 100-3000 keV for the Swift/BAT and
the Suzaku/WAM respectively. The spectral data of two instruments are
fitted with the spectral model multiplied by the constant factor to take
into account the systematic effective area uncertainties in the response
matrices of each instrument.
The spectrum is well fitted with a power-law with exponential cutoff
model: dN/dE ~ E^{alpha}*exp(-(2+alpha)*E/Epeak). The constant factors
of each instrument agree within 10%. No systematic residual from the
best fit model is seen in the spectral data of each instrument. The
best fit spectral parameters are: alpha = -1.59 (-0.06/+0.07) and Epeak
= 230 (-65/+135) keV (chi2/dof = 96.6/85). A simple power-law fit
shows a poor fit to the data (chi2/dof=126.4/86). The best fit spectral
parameters for the Band function fixing beta = -2.5 are:
alpha = -1.57 (-0.08/+0.10), and Epeak = 200 (-60/+130) keV (chi2/dof = 96.9/85).
Our best fit spectral parameters are consistent with the Konus-Wind
result based on the 3 channel data (Golenetskii et al. GCN Circ. 11659).
The energy fluence in the 15-3000 keV band calculated by a power-law with
exponential cutoff model for this 298 sec interval is 2.7 (-0.4/+0.7)x10^-5 erg/cm2.
Assuming z = 2.22 (Cenko et al. GCN Circ. 11638; Vreeswijk et al. GCN Circ. 11640)
and a standard cosmology model with H_0 = 71 km/s/Mpc, Omega_M = 0.27,
Omega_Lambda = 0.73, the isotropic energy release is
E_iso = 4.6 (-0.7/+0.4) x10^53 erg in 1 keV to 10 MeV at the GRB rest frame.
All the quoted errors are at the 90% confidence level.
GCN Circular 11682
Subject
GRB 110205A: Suzaku WAM observation of the prompt emission
Date
2011-02-09T15:19:09Z (15 years ago)
From
Satoshi Sugita at Aoyama Gakuin U. <sugita@phys.aoyama.ac.jp>
S. Sugita (Nagoya U.), K. Yamaoka (Aoyama Gakuin U.), N. Vasquez (Tokyo Tech.),
T. Uehara, Y. Hanabata, T. Takahashi, Y. Fukazawa (Hiroshima U.),
Y. Terada, M. Tashiro, W. Iwakiri, K. Takahara, T. Yasuda (Saitama U.),
M. Ohno, M. Suzuki, M. Kokubun, T. Takahashi (ISAS/JAXA),
Y. E. Nakagawa, T. Tamagawa (RIKEN), N. Ohmori, A. Daikyuji, Y. Nishioka,
M. Yamauchi (Univ. of Miyazaki), Y. Urata, P. Tsai (NCU),
K. Nakazawa, K. Makishima (Univ. of Tokyo),
S. Hong (Nihon U.), on behalf of the Suzaku WAM team, report:
The long GRB 110205A (Swift/BAT trigger #444643 ; Beardmore et al.,
GCN 11629; Beardmore et al., GCN 11639,; Markwardt et al., GCN 11646)
was detected by the the Suzaku Wide-band All-sky Monitor (WAM)
which covers an energy range of 50 keV - 5 MeV at 02:02:41 UT (=T0).
The observed light curve shows a multi-peaked structure starting at T0+20s,
ending at T0+318s with a duration (T90) of 248 (+/- 51) seconds.
The fluence in 100 - 1000 keV was 1.33 (+/- 0.23) x10^-5 erg/cm^2.
The 1-s peak flux measured from T0+211s was 1.15 (+/- 0.23) photons/cm^2/s in the same
energy range.
Preliminary result shows that the time-averaged spectrum from T0+20s to
T0+318s is well fitted by a single power-law with a photon index
of 2.12 (+/- 0.17) (chi^2/d.o.f = 82.1/50).
All the quoted errors are at statistical 90% confidence level.
The light curves with 1-sec time resolution for this burst is appeared at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/untrig/grb_table.html
GCN Circular 11672
Subject
GRB 110205A: optical observations in Mondy observatory
Date
2011-02-08T19:00:44Z (15 years ago)
From
Alina Volnova at SAI MSU <alinusss@gmail.com>
A. Volnova , E. Klunko (ISTP), A. Pozanenko (IKI) on behalf of larger
GRB follow up collaboration report:
We observed the Swift GRB 110205A (Beardmore et al., GCN 11629) with
AZT-33IK telescope of Sayan observatory (Mondy) on Feb.05 between (UT)
12:06:19 and 20:25:34, and we took several series in R-band with
exposures 60 - 180s.
The optical afterglow (Beardmore et al., GCN 11629) is clearly
detected on the stacked images. The photometry calibration performed
against the USNO-B1.0 star 1575-0155390 ((J2000) RA = 10:58:34.20, Dec
= +67:31:45.3), assuming R = 16.7:
T0+ Filter, Exposure, OT mag., UpperLimit
(mid, d) (s)
0.43968 R 51x60 19.88+/-0.04 21.9
0.71912 R 25x120+20x180 20.85+/-0.05 22.8
The power-law decay index during our observation is alpha ~1.8 which
is consistent with the index reported by Urata et al., GCN 11648.
[GCN OPS NOTE(08aug11): Per author's request, the spelling of the EK
author was corrected.]
GCN Circular 11670
Subject
GRB 110205A : HCT optical observations
Date
2011-02-08T09:28:45Z (15 years ago)
From
D.K. Sahu at Indian Inst of Astrophysics,Bangalore <dks@iiap.res.in>
D.K. Sahu and Pepsi Anto (Indian Institute of Astrophysics,
Bangalore) report.
Optical afterglow of the Swift GRB 110205A (Beardmore et al.,
GCN 11629) was observed with the 2m. Himalayan Chandra
Telescope of the Indian Astronomical Observatory, Hanle,
India, under poor sky condition. The optical afterglow
was observed in Bessell R filter and was detected in
all the frames.
The preliminary magnitudes of the optical afterglow,
calibrated using NOMAD1 1574-0155978 (R = 16.100)
(Veli-Pekka et al., GCN11637), are as under:
Date Mid UT Exposure R mag
05-02-2011 20:50 6 x 180sec 21.11 +/- 0.05
05-02-2011 21:13 3 x 180sec 21.19 +/- 0.08
05-02-2011 22:09 1 x 600sec 21.18 +/- 0.10
This message may be cited.
GCN Circular 11666
Subject
GRB 110205A - Continued PAIRITEL NIR Observations
Date
2011-02-07T22:24:21Z (15 years ago)
From
Adam Morgan at U.C. Berkeley <qmorgan@gmail.com>
A. N. Morgan and J. S. Bloom (UC Berkeley) report:
We continued to observe the location of the NIR afterglow of GRB
110205A (Morgan et al. GCN 11636) with the 1.3m PAIRITEL located at
Mt. Hopkins, Arizona throughout the night of February 5th and again on
2011-02-06. The afterglow continued to be well detected throughout
the first night.
The preliminary photometry yields:
post burst
t_mid (hr) exp.(hr) filt mag m_err
4.63 0.64 J 17.01 0.05
4.63 0.64 H 16.26 0.06
4.63 0.64 Ks 15.43 0.07
5.63 0.64 J 17.23 0.06
5.63 0.64 H 16.37 0.07
5.63 0.64 Ks 15.71 0.09
6.63 0.64 J 17.46 0.07
6.63 0.64 H 16.71 0.09
6.63 0.64 Ks 16.0 0.1
7.64 0.64 J 17.9 0.1
7.64 0.64 H 17.0 0.1
7.64 0.64 Ks 16.3 0.2
8.64 0.64 J 17.8 0.1
8.64 0.64 H 17.3 0.2
8.64 0.64 Ks 16.3 0.2
9.64 0.64 J 18.2 0.2
9.64 0.64 H 17.5 0.3
9.64 0.64 Ks 16.8 0.3
10.6 0.64 J 18.4 0.2
10.6 0.64 H 17.6 0.3
10.6 0.64 Ks 16.7 0.3
30.7 4.45 J >20.1 3sig
30.7 4.45 H >19.0 3sig
30.7 4.45 Ks >18.3 3sig
The late time decay index is consistent with that seen in the optical
(Urata et al. GCN 11648). All magnitudes are given in the Vega
system, calibrated to 2MASS. No correction for Galactic extinction has
been made to the above reported values.
GCN Circular 11663
Subject
GRB 110205A: WSRT radio observation
Date
2011-02-07T17:35:33Z (15 years ago)
From
Alexander van der Horst at NASA/MSFC <Alexander.J.VanDerHorst@nasa.gov>
A.J. van der Horst (USRA), C. Kouveliotou (NASA/MSFC), A.P. Kamble
(U of Wisconsin Milwaukee) and R.A.M.J. Wijers (U of Amsterdam)
report on behalf of a larger collaboration:
"We observed the position of the GRB 110205A afterglow at 4.9 GHz with
the Westerbork Synthesis Radio Telescope at February 6 19.44 UT to
February 7 07.41 UT, i.e. 1.72 - 2.22 days after the burst (GCN 11629).
We do not detect a radio source at the position of the optical
counterpart (GCN 11633). The three-sigma rms noise in the map around
that position is 105 microJy per beam. The formal flux measurement for
a point source at the position of the optical counterpart is 44 +/- 35
microJy.
We would like to thank the WSRT staff for scheduling and obtaining these
observations."
GCN Circular 11661
Subject
GRB110205A: CARMA 3mm Observations
Date
2011-02-07T16:13:16Z (15 years ago)
From
Ashley Zauderer at CfA <bevinashley@gmail.com>
GRB110205A: CARMA 3mm Observations
Ashley Zauderer, Edo Berger (Harvard) and Dale Frail (NRAO) report:
We observed GRB110205A (GCN 11629) with CARMA at 3 mm (93 GHz) starting
2.1 hours after the burst for a total on-source time of 2.3 hours. No
millimeter emission is detected in coincidence with the optical
afterglow position (GCN 11629) to a 3-sigma limit of 0.6 mJy.
We thank the CARMA observatory staff for support of these observations.
GCN Circular 11659
Subject
Konus-Wind observation of GRB 110205A
Date
2011-02-07T11:34:21Z (15 years ago)
From
Valentin Pal'shin at Ioffe Inst <val@mail.ioffe.ru>
S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P.
Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind
team report:
The long GRB 110205A (Swift-BAT trigger #444643: Beardmore et al., GCN
11629; Markwardt et al., GCN 11646) was detected by Konus-Wind in the
waiting mode.
The burst light curve shows a multipeaked pulse started at ~T0(BAT) with
a total duration of ~330 s. There is a weak pulse at ~T0(BAT)-1360 s
(seen by the same detector which observed GRB 110205A; the detection
significance is ~4.5 sigma in the G1+G2 (20-360 keV) band; the pulse
duration is ~25 s), which might be a burst precursor. There is a hint of
a weak soft tail seen up to ~T0+1200 s.
As observed by Konus-Wind, the burst had a fluence of (3.66 +/-
0.35)x10^-5 erg/cm2 and a 3-s peak flux measured from T0+211.6 s
of (5.1 +/- 0.7)x10^-7 erg/cm2/s (both in the 20 - 1200 keV energy range).
Modeling the K-W 3-channel time-integrated spectrum (from T0 s to
T0+330 s) by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -1.52 +/- 0.14, and Ep = 222 +/- 74 keV.
Assuming z = 2.22 (Cenko & Hora, GCN 11638; Vreeswijk et al. GCN 11640)
and a standard cosmology model with H_0 = 71 km/s/Mpc, Omega_M = 0.27,
Omega_Lambda = 0.73, the isotropic energy release E_iso is (1.36 +/-
0.13)x10^54 erg, the peak luminosity (L_iso)_max is (5.9 +/- 0.8)x10^51
erg/s, and Ep_rest is 715 +/- 238 keV.
All the quoted errors are estimated at the 1 sigma confidence level.
The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB110205A/
GCN Circular 11655
Subject
GRB 110205A: Lightbuckets Optical Observations
Date
2011-02-06T22:19:34Z (15 years ago)
From
Tilan Ukwatta at GSFC/GWU <tilan.ukwatta@gmail.com>
T. N. Ukwatta (MSU), E. Sonbas (GSFC/USRA/Adiyaman Univ.),
N. Gehrels (GSFC), J. Linnemann (MSU), K. Tollefson (MSU),
and U. Abeysekara (MSU)
We observed the Swift GRB 110205A (Beardmore et al., GCN 11629)
with the Lightbuckets 0.61m rental telescope LB-0001 in Rodeo,
NM, USA. Under good weather conditions, two observations
were carried out in the Luminance and R filter starting
2011-02-05 at 07:45:58 UT (~ 5.7 hours after the GRB trigger)
and 09:39:21 UT (~7.6 hours after the GRB trigger). Another
followup observation was performed on R filter starting
2011-02-06 at 09:29:04 UT (~1.31 days after the trigger)
under acceptable weather conditions.
The burst afterglow is clearly detected in the first two
observations and estimated magnitudes are given below:
Time after trigger Exposure (s) Filter Magnitude
5.7 hours (0.24 days) 1 x 300 Lum 19.0 +/- 0.1
7.6 hours (0.31 days) 1 x 300 R 19.6 +/- 0.2
31.4 hours (1.31 days) 2 x 300 R > 20.1
The afterglow, not corrected for Galactic extinction, is
calibrated against the USNO-B1.0 catalog.
We acknowledge the helpful assistance of the Lightbuckets staff,
in particular Stephen G. Cullen.
GCN Circular 11653
Subject
GRB 110205A : Lulin optical observation
Date
2011-02-06T17:09:26Z (15 years ago)
From
Yuji Urata at Nat. Central U. <urata@astro.ncu.edu.tw>
Yuji Urata, Chia-Jung Chuang (NCU) and Kuiyun Huang (ASIAA)
on behalf of EAFON report
"We made a further optical afterglow observation with r'-band using
the Lulin 1m telescope. The stacked image made from 7 frames with 600s
exposure shows the afterglow clearly. The brightness calibrated
against with the SDSS catalog is r'=22.49+/-0.12 at 1.53 days after
the burst. This is consistent with the extrapolation of the simple
power-law decay with the temporal index of about 1.9 from our previous
report (GCN 11648)."
GCN Circular 11652
Subject
GRB110205A: MITSuME Ishigakijima Optical Observation
Date
2011-02-06T16:23:27Z (15 years ago)
From
Daisuke Kuroda at OAO/NAOJ <dikuroda@oao.nao.ac.jp>
D. Kuroda (OAO, NAOJ), H. Hanayama, T. Miyaji, J. Watanabe (IAO, NAOJ),
K. Yanagisawa (OAO, 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 110205A (Beardmore et al., GCNC 11629)
with the optical three color (g', Rc and Ic) CCD camera attached
to the Murikabushi 1m telescope of Ishigakijima Astronomical
Observatory.
The observation started on 2011-02-05 12:15:24 UT (~10.2 hours after
the burst). We detected the previously reported afterglow
(Klotz et al., GCNC 11630; Schaefer et al., GCNC 11631) in all the
three bands.
Photometric results are listed below. We used SDSS catalog for flux
calibration.
#T0+[day] MID-UT T-EXP[sec] g' g'_err Rc Rc_err Ic Ic_err
----------------------------------------------------------------------
0.45691 13:00:38 4500.0 21.0 0.2 20.2 0.1 19.8 0.2
0.76876 20:29:42 4620.0 21.5 0.2 20.8 0.1 20.2 0.2
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]
GCN Circular 11651
Subject
GRB110205A: MITSuME Okayama Optical Observation
Date
2011-02-06T16:19:56Z (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 110205A (Beardmore et al., GCNC 11629)
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 2011-02-05 10:37:55 UT (~8.6 hours after
the burst). We detected the previously reported afterglow
(Klotz et al., GCNC 11630; Schaefer et al., GCNC 11631) in all the
three bands.
Photometric results and are listed below. We used SDSS catalog for flux
calibration.
#T0+[day] MID-UT T-EXP[sec] g' g'_err Rc Rc_err Ic Ic_err
----------------------------------------------------------------------
0.39965 11:38:11 6120.0 >20.1 19.4 0.2 18.5 0.2
0.48327 13:38:36 6300.0 20.6 0.3 20.4 0.3 19.7 0.3
0.56675 15:38:49 6300.0 21.2 0.4 19.8 0.2 19.7 0.2
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]
GCN Circular 11650
Subject
GRB110205A: SMA 1.3mm Observations
Date
2011-02-06T01:03:33Z (15 years ago)
From
Ashley Zauderer at CfA <bevinashley@gmail.com>
Glen Petitpas (SMA), Ashley Zauderer, Edo Berger, Nimesh Patel, Erin
Brassfield (Harvard/CfA), Jen Miller, Anil Dosaj (SMA) report:
We observed GRB110205A (GCN #11629) with the Submillimeter Array (SMA)
at 1.3 mm (225 GHz) starting 1.3 hours after the burst for a duration of
6 hours. No source is detected in coincidence with the optical
afterglow (GCN #11629). With a combined 8 GHz of bandwidth, the
resulting 3-sigma upper limit is 1.65 mJy.
GCN Circular 11649
Subject
GRB 110205A: Swift/UVOT Continuing Observations
Date
2011-02-05T17:55:39Z (15 years ago)
From
Margaret Chester at PSU <chester@astro.psu.edu>
M. M. Chester (PSU) and A. P. Beardmore (U Leicester) report on
behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 110205A
164 s after the BAT trigger (Beardmore et al., GCN Circ. 11629).
The peak near 1000s reported by Klotz et al. (GCN Circ. 11632) and
Andreev et al. (GCN Circ. 11641) is seen in the UVOT optical filters
and one of the UV filters (uvw1), consistent with the reported
redshift z=2.22 (Cenko et al., GCN Circ. 11638 and Vreeswijk et al.,
GCN Circ. 11640). The weak detections (2-3 sigma) in uvw2 are
probably due to the filter's extended sensitivity in the red.
After 5000s, the estimated temporal slope in the white filter is 1.6.
Preliminary photometry using the UVOT photometric system (Poole et al.
2008, MNRAS, 383, 627) for the finding chart (FC) and subsequent
exposures is:
FILTER TSTART TSTOP MAG +/- UL(2o)
white_FC 164.0 313.8 18.79 0.07
white 601.9 621.7 17.01 0.08
white 774.6 794.4 15.74 0.06
white_FC 875.4 1025.1 15.36 0.04
white 1181.0 1375.8 15.39 0.05
v 652.0 671.8 15.76 0.11
v 824.3 844.1 14.98 0.08
v 1056.5 1251.8 14.68 0.06
b 577.5 597.3 17.10 0.12
b 750.3 770.1 15.77 0.07
b 1154.7 1351.5 15.33 0.05
u_FC 321.9 571.7 18.24 0.09
u 725.4 745.2 15.59 0.09
u 1130.5 1325.1 15.02 0.06
uvw1 701.0 720.8 18.23 0.41
uvw1 1106.0 1300.8 17.09 0.17
uvm2 676.3 1276.1 19.89
uvm2 1430.1 1795.8 19.60
uvw2 627.4 1226.2 19.89 0.49
uvw2 1381.4 1747.0 19.28 0.41
The values quoted above 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 11648
Subject
GRB 110205A: Lulin optical observations and temporal decay index
Date
2011-02-05T17:33:40Z (15 years ago)
From
Yuji Urata at Nat. Central U. <urata@astro.ncu.edu.tw>
Yuji Urata, Chia-Jung Chuang (NCU) and Kuiyun Huang (ASIAA)
on behalf of EAFON
"We are monitoring the optical afterglow of GRB110205A (GCN 11630,
11631) in g', r' and i' filters using the 1.0m telescope at Mt. Lulin,
Taiwan. The observations are started at 2011 February 5, 13:02 UT.
Based on our r'-band photometry against with the SDSS catalog, the
temporal decay index between 40000 and 52740 sec after the burst is
about 1.9. The brightness in r'-band at 52740 sec after the burst is
20.64 +/-0.05 mag.
The further monitoring observation and analysis are ongoing.
GCN Circular 11647
Subject
Observations GRB 110205A
Date
2011-02-05T16:39:26Z (15 years ago)
From
Francois Kugel at Obs.Chante-Perdix,04 Banon,Fr <fkugel@wanadoo.fr>
Francois Kugel at Obs.Chante-Perdix,04 Banon,Fr
Observer : C. RINNER; F. KUGEL
We imaged the field of GRB 110205A detected by SWIFT(trigger 444643) with the
0.5-m F/3 reflector + ccd kai 11k (No filter).
The observations started at 04:30:52 (UT)
The elevation of the field decreased from 54 degrees above horizon and weather
conditions were good.
We clearly identify the afterglow and the flux decreases slowly.
USNO-SA 2.0 R
Exp : hh:mm:ss
180s : 04:32:22 (UT) = 10h58m31.149s +67��31'30.89'' 17.44 +/-0.08
180s : 04:48:32 (UT) = 10h58m31.173s +67��31'30.88'' 17.84 +/-0.16
120s : 05:38:46 (UT) = 10h58m31.173s +67��31'30.86'' 18.09 +/-0.35
120s : 05:51:26 (UT) = 10h58m31.169s +67��31'30.71'' 17.99 +/-0.64
Image & measurement : http://astrosurf.com/obsdauban/pages/GRB110205A.html
GCN Circular 11646
Subject
GRB 110205A: Swift-BAT refined analysis
Date
2011-02-05T16:32:29Z (15 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@lheamail.gsfc.nasa.gov>
GRB 110205A: Swift-BAT refined analysis
C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
Using the data set from T-239 to ~T+2000 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 110205A (trigger #444643)
(Beardmore, et al., GCN Circ. 11629). The BAT ground-calculated position is
RA, Dec = 164.603, 67.533 deg, which is
RA(J2000) = 10h 58m 24.8s
Dec(J2000) = +67d 31' 57.1"
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 29%.
The mask-weighted light curve shows many overlapping peaks with a general
slow rise starting at ~T-120 sec, with the tallest peak at ~T+210 sec, and
ending at ~T+1500 sec. T90 (15-350 keV) is 257 +- 25 sec
(estimated error including systematics).
The time-averaged spectrum from T-129 to T+377 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.80 +- 0.04. The fluence in the 15-150 keV band is 1.7 +- 0.0 x 10^-5 erg/cm2.
The 1-sec peak photon flux measured from T+210.44 sec in the 15-150 keV band
is 3.6 +- 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/444643/BA/
GCN Circular 11645
Subject
GRB 110205A: Newcastle Observatory Optical Observations
Date
2011-02-05T15:37:38Z (15 years ago)
From
Michael Cook at Newcastle Obs. <michaeljcook@rogers.com>
Michael J. Cook, Newcastle Observatory report:
On 5 February UT, the field of GRB 110205A detected by SWIFT (trigger 444643)
was observed, beginning approximately 49 minutes after the GRB trigger, with the
Newcastle Observatory 0.4 meter robotic telescope, located in Newcastle,
Ontario, Canada (Bortle Class 4-5 sky).
Observations were made under transparent skies, but with poor seeing. Weather
was good with an ambient temperature of -4C. No Moon was present.
Automatic imaging in the V-band detected the afterglow candidate reported by
Beardmore et al., Klotz et al. (GCN 11630) at:
RA 10: 58: 31.34 DEC +67 31 31.4 (J2000)
A 180s calibrated image gives a preliminary magnitude of 15.41 (V-band).
The magnitude is estimated with the nearby NOMAD1 star 1574-0155894 (Vmag
15.240)
A time-series was taken from 02:52:09 to 07:23:05 and further analysis is in
progress.
This message is quotable in publications.
GCN Circular 11644
Subject
GRB 110205A: Swift-XRT refined Analysis
Date
2011-02-05T13:47:05Z (15 years ago)
From
Kim Page at U.of Leicester <kpa@star.le.ac.uk>
A. P. Beardmore (U Leicester) reports on behalf of the Swift-XRT team:
We have analysed 14 ks of XRT data for GRB 110205A (Beardmore et al.
GCN Circ. 11629), from 145 s to 30.7 ks after the BAT trigger. The
data comprise 737 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
Beardmore et al. (GCN. Circ 11639).
The light curve comprises a number of flares (at ~T0+145 s, T0+175 s to
T0+275 s, T0+615 s) followed by a power-law decay. The late-time light
curve (from T0+5.1 ks) can be modelled with a power-law decay with a
decay index of alpha=1.63 (+/-0.10).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.420 (+/-0.020). The
best-fitting absorption column is 4.2 (+/-0.6) x 10^21 cm^-2, at a
redshift of 2.22, in addition to the Galactic value of 1.6 x 10^20
cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a photon index
of 1.99 (+0.08, -0.07) and a best-fitting absorption column of 3.5
(+1.6, -1.5) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10
keV flux conversion factor deduced from this spectrum is 3.7 x 10^-11
(4.2 x 10^-11) erg cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Galactic foreground: 1.6 x 10^20 cm^-2
Intrinsic column: 3.5 (+1.6, -1.5) x 10^21 cm^-2 at z=2.22
Photon index: 1.99 (+0.08, -0.07)
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00444643.
This circular is an official product of the Swift-XRT team.
GCN Circular 11643
Subject
GRB 110205A: LOAO B/R Observation
Date
2011-02-05T11:53:19Z (15 years ago)
From
Myungshin Im at Seoul Nat U <mim@astro.snu.ac.kr>
Myungshin Im (CEOU/SNU), and Yuji Urata (NCU) on behalf
of a larger collaboration
We are taking images of the field around GRB 110205A (GCN 11629)
in B and R filters using the 1.0m telescope at Mt. Lemmon, AZ, USA,
starting at 2011 February 5, 05:19:11 UT (roughly 3.28 hrs
after the burst alert).
We clearly identify the afterglow (GCN 11630 et al.) in all the
image taken so far..
The first image of the observation shows that the afterglow
is at R = 18.0 +- 0.1 (Vega), calibrated against a star in the
USNO B-1 catalog at RA=10:58:34.2 and Dec=+67:31:45.3.
The observation and the further analysis of the data are
onging. We thank the LOAO operator, Jae-Hyuck Youn, for his assitance
of the observation.
GCN Circular 11641
Subject
GRB 110205A: optical flare confirmation
Date
2011-02-05T08:54:23Z (15 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
M. Andreev, A. Sergeev (Terskol Branch of Institute of Astronomy), A.
Pozanenko (IKI) on behalf of larger GRB follow up collaboration report:
We observed field of the Swift GRB 110205A (Beardmore et al, GCN 11629)
with Zeiss-600 telescope of Mt.Terskol observatory in R,V filters starting
on Feb. 05 (UT) 02:16. We clearly detect optical afterglow (Beardmore et
al, GCN 11629, Klotz et al, GCN 11630, Schaefer et al, GCN 11631, Mundell
et al, GCN 11633) and confirm the optical flare at ~ 1140 s (Schaefer et
al, GCN 11631, Klotz et al, GCN 11632, Chester et al, GCN 11634) with
maximal brightness R ~ 13.7.
The finding chart and preliminary light curves can be found at
http://grb.rssi.ru/GRB110205A/
GCN Circular 11640
Subject
GRB 110205A: NOT redshift confirmation
Date
2011-02-05T08:49:25Z (15 years ago)
From
Annalisa De Cia at U of Iceland <annalisa@raunvis.hi.is>
Paul Vreeswijk (U. Iceland), Paul Groot (Radboud U. Nijmegen),
Philip Carter (U. Warwick), Dong Xu (WIS), Annalisa De Cia, P.
Jakobsson (U. Iceland) and Johan Fynbo (DARK) report on behalf
of a larger collaboration:
We have observed the field of GRB 110205A (Beardmore et al., GCN
11629) with the 2.5m NOT telescope at Roque de los Muchachos
Observatory (La Palma, Spain) equipped with ALFOSC starting at
3:25 UT (1.4h after the burst). Despite thick clouds, the
optical afterglow is clearly detected at R ~ 16.7 (as compared
to nearby USNO-B1.0 stars).
Preliminary reduction of the subsequent spectroscopic
observations shows a clear DLA and several metal absorption
lines (OI/OI*, CII/CII*, CIV, AlII, FeII) at a common redshift
z=2.22, confirming the redshift measurement by Cenko et al. (GCN
11638).
GCN Circular 11639
Subject
GRB 110205A: Enhanced Swift-XRT position
Date
2011-02-05T08:44:48Z (15 years ago)
From
Phil Evans at U of Leicester <pae9@star.le.ac.uk>
A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester)
report on behalf of the Swift-XRT team.
Using 3847 s of XRT Photon Counting mode data and 7 UVOT
images for GRB 110205A, 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 = 164.62969, +67.52521 which is equivalent
to:
RA (J2000): 10h 58m 31.13s
Dec (J2000): +67d 31' 30.8"
with an uncertainty of 1.5 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 11638
Subject
GRB 110205A: FAST Redshift
Date
2011-02-05T07:57:29Z (15 years ago)
From
S. Bradley Cenko at Caltech <cenko@srl.caltech.edu>
S. B. Cenko (UC Berkeley), J. L. Hora (CfA), and J. S. Bloom (UC Berkeley)
report on behalf of a larger collaboration:
We obtained a pair of spectra of the optical afterglow of GRB 110205A
(Beardmore et al., GCN 11629) with the FAST spectrograph mounted on the
FLWO 1.5 m telescope. Observations began at 6:27 UT (~ 4.5 hours after
the burst) and cover the wavelength range from 3500-7400 A.
As reported by da Silva et al (GCN 11635), the spectrum exhibits a
prominent DLA absorption feature; however, we observe this feature at a
slightly larger wavelength (~ 3900 A). We further identify a series of
narrow absorption features, including Si II, Si II*, C IV, and Al II, at a
common redshift of z=2.22. The detection of Si II*, together with the DLA
system, strongly suggest this is the host galaxy of GRB 110205A.
GCN Circular 11637
Subject
GRB 110205A: GRAS005 optical observations
Date
2011-02-05T07:29:33Z (15 years ago)
From
Veli-Pekka Hentunen at Taurus Hill Obs,A95 <veli-pekka.hentunen@kassiopeia.net>
Veli-Pekka Hentunen, Markku Nissinen and Tuomo Salmi (Taurus Hill
Observatory, Varkaus, Finland) report:
GRAS 005 (Global-Rent-a-Scope, Mayhill, New Mexico) Takahashi Epsilon
250 10" FL 850 mm and SBIG ST-10XME camera were used to detect
GRB 110205A optical afterglow. The observations were started at
2011-02-05 02:56:38 (UT) and stopped at 2011-02-05 04:24:38 (UT). Four
unfiltered and four photometric R observations with 300s and 600s exposure
times were made. The afterglow was detected at following position
RA 10 58 31.16 and DEC +67 31 31.1 consistent those given by Klotz A.
et al. (GCN 11630) to within positional errors.
The following magnitudes were obtained from the observations using
NOMAD1 1574-0155978 (R = 16.100) as the comparison:
Tmid(s)+T0 Filter Exp (sec) Mag Mag err Limit
3537 unfilt 600 16.3 0.1 19.7
4249 Rc 600 16.5 0.1 18.9
5327 unfilt 300 16.8 0.1 19.7
5858 Rc 600 17.0 0.1 18.9
6379 Rc 300 17.3 0.1 18.9
6903 unfilt 600 17.3 0.1 19.7
7993 Rc 300 17.6 0.1 18.9
8367 unfilt 300 17.6 0.1 19.7
A jpg image of the 600sec clear filter observation is available at the following URL link:
http://cutenews.kassiopeia.net/data/upimages/GRB110205A.jpg
GCN Circular 11636
Subject
GRB 110205A: PAIRITEL NIR Afterglow Detection
Date
2011-02-05T06:30:31Z (15 years ago)
From
Adam Morgan at U.C. Berkeley <qmorgan@gmail.com>
A. N. Morgan, C. R. Klein, and J. S. Bloom (UC Berkeley) report:
We observed the field of GRB 110205A (Beardmore et al., GCN 11629)
with the 1.3m PAIRITEL located at Mt. Hopkins, Arizona. Observations
began at 2011-Feb-05 05h14m03s UT, ~3.2 hours after the Swift trigger.
In mosaics (effective exposure time of 0.50 hours) taken
simultaneously in the J, H, and Ks filters, we detect a source at the
position of the optical afterglow (Klotz et al., GCN 11630; Schaefer
et al., GCN 11631; Mundell et al., GCN 11633).
The preliminary photometry yields:
post burst
t_mid (hr) exp.(hr) filt mag m_err
3.59 0.50 J 16.74 0.05
3.59 0.50 H 15.81 0.05
3.59 0.50 Ks 15.19 0.07
All magnitudes are given in the Vega system, calibrated to 2MASS. No
correction for Galactic extinction has been made to the above reported
values. Observations are continuing.
GCN Circular 11635
Subject
GRB 110205A: Possible Lick/Kast redshift
Date
2011-02-05T06:30:21Z (15 years ago)
From
Jason Prochaska at UCO/Lick Obs <xavier@ucolick.org>
R. da Silva (UCO/Lick), M. Fumagalli (UCO/Lick), G. Worseck
(UCO/Lick), and X. Prochaska (UCO/Lick) report on behalf of GRAASP:
"We have observed GRB 110205A with the Kast
dual spectrometer on the 3m Lick telescope for a series of
three 1800s exposures starting at UT 04:47 under variable
conditions and at high air mass.
We observe a significant absorption feature (EW > 100mA) at
~3600Ang which we interpret as a z~1.98 DLA associated with
the GRB host. We identify additional absorption features at
~3875A and 3980A which are roughly consistent with OI 1302
and CII 1334 transitions at the coincident redshift.
On the other hand, we do not detect a significant feature at CIV
nor any significant features redward of ~6000Ang where we
would expect FeII 2344, 2374, and 2382 absorption."
Further analysis is in progress.
GCN Circular 11634
Subject
GRB 110205A: Swift/UVOT Confirmation of Flaring Afterglow
Date
2011-02-05T05:06:33Z (15 years ago)
From
Margaret Chester at PSU <chester@astro.psu.edu>
M. M. Chester(PSU) and A. P. Beardmore report on behalf of the
Swift/UVOT team:
The Swift/UVOT obtained three finding chart exposures of the field of
GRB 110205A (A. P. Beardmore et al., GCN Circ. 11629) which show the
brightening reported by Klotz et al. (GCN Circ. 11630 and 11632) and
Schaefer et al. (GCN Circ. 11631). Preliminary magnitudes using the
UVOT photometric system (Poole et al. 2008, MNRAS, 383, 627) are:
Filter T_start(s) T_stop(s) Exp(s) Mag Mag_err
white_FC 164 314 150 18.71 0.15
u_FC 321 571 250 18.17 0.15
white_FC 875 1025 150 15.4 0.4
Observations are continuing.
GCN Circular 11633
Subject
GRB 110205A: Liverpool Telescope Afterglow Confirmation
Date
2011-02-05T02:54:32Z (15 years ago)
From
Carole Mundell at ARI, JMU,Liverpool <cgm@astro.livjm.ac.uk>
C.G. Mundell, R.J. Smith, Z. Cano (ARI, LJMU) report on behalf of a larger
collaboration:
The Liverpool Telescope began automatically observing Swift GRB 110205A
(Beardmore et al. GCN 11629) with the RINGO2 polarimeter.
Subsequent automatic imaging detects the afterglow candidate reported by
Beardmore et al., Klotz et al. (GCN 11630) and Schaefer et al. (GCN 11631) at:
RA=10:58:31.1 , Dec=+67:31:30.9 (J2000) +/-0.2"
with preliminary magnitude R=16.06 mag (wrt USNO B1) at t=924 secs.
Observations have stopped due to bad weather.
GCN Circular 11632
Subject
GRB 110205A: TAROT Calern observatory detection of an optical flare
Date
2011-02-05T02:47:49Z (15 years ago)
From
Alain Klotz at CESR-CNRS <Alain.Klotz@free.fr>
Klotz A. (CESR-OMP), Gendre B. (ASDC), Lass M. (UWA),
Boer M. (OHP-OAMP), Atteia J.L. (LATT-OMP) report:
We continue to acquire images the field of GRB 110205A
(cf. Klotz et al. GCNC 11630). After a first peak of
brightness R~16.7 at t~225s, the flux decreased at R~18
about 360s after the trigger.
Then, the brightness increased dramatically and
reached R~14.1 at t~1150s. Now the flux decreases
slowly: R~15.0 at t~1800s.
GCN Circular 11631
Subject
GRB 110205A: ROTSE-III, Optical Counterpart is flaring to ~14 mag
Date
2011-02-05T02:39:21Z (15 years ago)
From
Brad Schaefer at LSU <schaefer@grb.phys.lsu.edu>
B. E. Schaefer (Louisiana State), H. Flewelling (IfA/Hawaii), W.
Rujopakarn (Steward), T. Guver (U Arizona), report on behalf of the ROTSE
collaboration:
ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB
110205A (Swift trigger 444643). The first image was at 02:04:03.4 UT, 82.0
s after the burst (8.4 s after the GCN notice time). The unfiltered images
are calibrated relative to USNO A2.0. On the first images, we detect a
17.0 magnitude source with coordinates:
10:58:31.11 +67:31:31.91 (J2000), with positional uncertainty
of 1" or better
start UT mag mlim(of image)
----------------------------------
02:06:00.5 17.0 17.6
This source is at the position of the Swift XRT and UVOT transients, and
not visible in DSS (second epoch), 2MASS or the MPChecker database. On
our first two sets of ten images, the source is faint, near our limit,
while for our third and fourth coadded images the source has significnatly
brightened by over two magnitudes, apparently to magnitude around 13.9.
Continuing observations are in progress.
GCN Circular 11630
Subject
GRB 110205A: TAROT Calern observatory optical detection
Date
2011-02-05T02:21:42Z (15 years ago)
From
Alain Klotz at CESR-CNRS <Alain.Klotz@free.fr>
Klotz A. (CESR-OMP), Gendre B. (ASDC), Lass M. (UWA),
Boer M. (OHP-OAMP), Atteia J.L. (LATT-OMP) report:
We imaged the field of GRB 110205A detected by SWIFT
(trigger 444643) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.
The observations started 90.6s after the GRB trigger.
The elevation of the field decreased from
65 degrees above horizon and weather conditions
were good.
We detect a new source in the error box given by SWIFT
We detected the candidate couterpart mentioned
by Beardmore et al. (GCNC 11629) at the following
position (+/- 1 arcsec):
RA(J2000.0) = 10h 58m 31.25s
DEC(J2000.0) +67d 31' 31.4"
OT optical brightness increased until R~16.7
about 225s after GRB. Then it decreases.
Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.
This message may be cited.
GCN Circular 11629
Subject
GRB 110205A: Swift detection of a burst with an optical candidate
Date
2011-02-05T02:17:32Z (15 years ago)
From
David Palmer at LANL <palmer@lanl.gov>
A. P. Beardmore (U Leicester), W. H. Baumgartner (GSFC/UMBC),
D. N. Burrows (PSU), M. M. Chester (PSU), J. M. Gelbord (PSU),
S. T. Holland (CRESST/USRA/GSFC), N. P. M. Kuin (UCL-MSSL),
O. M. Littlejohns (U Leicester), C. B. Markwardt (NASA/GSFC),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester),
D. M. Palmer (LANL), T. Sakamoto (NASA/UMBC), C. J. Saxton (UCL-MSSL),
M. H. Siegel (PSU), E. Sonbas (GSFC/USRA/Adiyaman Univ.),
M. Stamatikos (OSU/NASA/GSFC), C. A. Swenson (PSU) and
T. N. Ukwatta (MSU) report on behalf of the Swift Team:
At 02:02:41 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 110205A (trigger=444643). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 164.589, +67.516 which is
RA(J2000) = 10h 58m 21s
Dec(J2000) = +67d 30' 58"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT lightcurve shows activity
with multiple peaks until at least T+300 seconds, with a
peak count rate of 4500 counts/s (15-150 keV) at T+210 s.
The XRT began observing the field at 02:05:16.8 UT, 155.4 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 164.6321, +67.5230 which is equivalent to:
RA(J2000) = 10h 58m 31.70s
Dec(J2000) = +67d 31' 22.7"
with an uncertainty of 6.2 arcseconds (radius, 90% containment). This
location is 64 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy.
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 164 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
RA(J2000) = 10:58:31.12 = 164.62965
DEC(J2000) = +67:31:31.2 = 67.52532
with a 90%-confidence error radius of about 0.63 arc sec. This position is 9.0
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.71 with a 1-sigma error of about 0.15. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.01.
Burst Advocate for this burst is A. P. Beardmore (apb AT star.le.ac.uk).
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.)