GRB 100219A
GCN Circular 10527
Subject
GRB 100219A: MASTER-Net optical alert observations
Date
2010-03-19T19:50:44Z (16 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
V.Yurkov, Yu.Sergienko, D.Varda, A.Garusina
Blagoveschensk Educational State University, Blagoveschensk
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.Zemnukhov,
M. Kornilov
Sternberg Astronomical Institute, Moscow State University
A. Tlatov, A.V. Parhomenko, D. Dormidontov
Kislovodsk Solar Station of the Pulkovo Observatory
V.Krushinski, I.Zalozhnih, T.Kopytova, A. Popov Ural State University, Kourovka
K.Ivanov, S.Yazev, N.M.Budnev, E.Konstantinov, V.Lenok
Irkutsk State University
MASTER robotic telescope (MASTER-Net: http://observ.pereplet.ru, 200
mm, FOV=8 square degrees (testing telescope) and Very Wide Field Camera (D=50
mm, 1000 square degrees, 11 Mpx, 36" per pix, mounted on telescope)
located at Blagoveschensk was responted to the GRB 100219A (Swift Bat
alert,
Gelbord et al, GCN CIRC 10526) 64 sec after Notice time and 78 s
after
the GRB time.
There is now OT on the first 20-s exposition time image inside Swift XRT
error box (Gelbord et al., GCN CIRC 10526) brighter 16.0.
The message may be cited.
mailto: lipunov@sai.msu.ru
GCN Circular 10522
Subject
GRB 100219A: optical upper limit
Date
2010-03-18T01:35:33Z (16 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
A. Volnova (SAI MSU), E. Klunko (ISTP), and A. Pozanenko (IKI) report on
behalf of larger GRB follow-up collaboration:
We observed the field of the Swift GRB 100219A (Rowlinson et al. GCN 10438)
with AZT-33IK telescope of Sayan observatory (Mondy) starting on Feb.19 (UT)
16:16:18, i.e. 1.0 hours after the burst. Observations were carried out up
to (UT) 16:59:26. We do not detect any objects in enhanced XRT error circle
(Evans et al. GCN 10437). The upper limit (3 sigma) of stacked image of the
first series is based on several USNO-B1.0 nearby stars:
T0+ Filter Exposure mag.
(mid, d) (s)
0.0431 R 3x60 > 19.00
GCN Circular 10453
Subject
GRB 100219A: optical observations
Date
2010-02-26T02:48:20Z (16 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
V. Rumyantsev, D. Shakhovskoy (CrAO), A. Pozanenko (IKI) report on behalf
of larger GRB follow-up collaboration:
We observed the field of the Swift GRB 100219A (Rowlinson et al. GCN 10438)
with AZT-11 telescope of CrAO starting (UT) Feb. 19 22:54 (7.6 hours after
burst onset). We detect the galaxy (previously reported by Holland &
Rowlinson (GCN 10436), Bloom & Nugent (GCN 10437)). The coordinates of the
galaxy are (J2000) RA= 10 16 48.61, Dec= -12 33 57.15 (with uncertainties
0.5 arcsec in both coordinates). We do not detect optical afterglow
(Jakobsson et al. GCN 10430, Kruehler et al. GCN 10439). The photometry is
based on USNO-B1.0 star 0774-0276292 (assuming R=16.90):
T0+ Filter, Exposure, mag. Object
(mid, d) (s)
0.3364 R 20x180 21.3 +/- 0.25 galaxy
0.3364 R 20x180 > 21.8 OT
GCN Circular 10452
Subject
GRB 100219A: GAO 150cm telescope Optical Observation
Date
2010-02-26T01:01:58Z (16 years ago)
From
Kenzo Kinugasa at Gunma Astro. Obs/Japan <kinugasa@astron.pref.gunma.jp>
K. Kinugasa, S. Honda, H. Takahashi, H. Taguchi, O. Hashimoto
(Gunma Astronomical Observatory) report:
The position of GRB 100219A (Rowlinson et al., GCN 10430) was observed
with the 150 cm telescope of Gunma Astronomical Observatory. Starting at
16:06:16 UT on Feb.19 (0.84 hour after the trigger), both Rc and Ic
frames were acquired for sets of 5 x 3-min exposures.
Inside the XRT error circle (Evans et al., GCN 10437), we detected the
optical counterpart reported by Jakobsson et al. (GCN 10438), Kruehler
et al. (GCN 10439), and Kuroda et al. (GCN 10440) in Rc and Ic stacked
images. We estimated the Rc and Ic magnitudes relative to USNO-B1.0 R2
and I magnitudes, respectively.
mid-UT T0+(d) exp mag.
-----------------------------------------------------
16:15:24 0.0414 5x3min Rc=20.5+-0.2
16:34:45 0.0549 5x3min Ic=19.6+-0.3
-----------------------------------------------------
GCN Circular 10445
Subject
GRB 100219A: X-shooter refined analysis
Date
2010-02-20T21:32:41Z (16 years ago)
From
Antonio Deugarte at IAA-CSIC <deugarte@iaa.es>
A. de Ugarte Postigo, C.C. Thoene (INAF/OAB), S.D. Vergani
(APC/Univ. Paris 7), B. Milvang-Jensen, J. Fynbo (DARK/NBI)
report on behalf of the X-shooter GRB collaboration:
We continued with the analysis of X-shooter's spectrum
(Groot et al. GCN 10441) obtained for the afterglow of
GRB 100219A (Rowlinson et al. GCN 10430). Additionally to
the strong Ly-alpha absorption reported in the previous GCN
and the SiII and SiII* absorptions suggested by Cenko et al.
(GCN 10443) we detect several other absorption features,
including SII, OI, OI*, CII, CII*, SiIV, CIV, FeII, AlII and
AlIII at a redshift of 4.6667 +/- 0.0005. We also detect an
intervening system at z = 2.1810 +/- 0.0005 through the
identification of FeII, MgII and MgI. A second intervening
system might be present at z = 1.7980 +/- 0.0005 identified
by faint MgII and MgI absorptions. Further analysis is ongoing.
GCN Circular 10444
Subject
GRB 100219A: XRT refined analysis
Date
2010-02-20T07:11:16Z (16 years ago)
From
Antonia Rowlinson at U.of Leicester <bar7@star.le.ac.uk>
A. Rowlinson (U Leicester) reports on behalf of the Swift-XRT team:
We have analysed 3.8 ks of XRT data for GRB 100219A (Rowlinson et al.
GCN Circ. 10430), from 207 s to 28.4 ks after the BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position for
this burst was given by Evans et al. (GCN. Circ 10437).
The light curve can be modelled with an initial power-law decay with an
index of alpha=1.53 (+0.28, -0.22), followed by a break at T+785 s to an
alpha of 0.57 (+/-0.06).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.72 (+0.16, -0.13). The
best-fitting absorption column is 8.8 (+4.2, -0.0) x 10^20 cm^-2, in
excess of the Galactic value of 6.5 x 10^20 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum is 4.5 x 10^-11 (5.3 x 10^-11) erg
cm^-2 count^-1.
If the light curve continues to decay with a power-law decay index of
0.57, the count rate at T+24 hours will be 0.035 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.6 x
10^-12 (1.8 x 10^-12) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00412982.
This circular is an official product of the Swift-XRT team.
GCN Circular 10443
Subject
GRB 100219A - Gemini South Spectroscopy
Date
2010-02-20T06:58:52Z (16 years ago)
From
S. Bradley Cenko at Caltech <cenko@srl.caltech.edu>
S. B. Cenko, J. S. Bloom, D. A. Perley, and B. E. Cobb (UC Berkeley)
report on behalf of a larger collaboration:
We have obtained spectra of the proposed host galaxy (Bloom and
Nugent, GCN 10433; Holland et al., GCN 10436) and the optical afterglow
(Jakobsson et al., GCN 10438; Kruehler et al., GCN 10439) of
GRB100219A (Rowlinson et al., GCN 10430) with the Gemini Multi-Object
Spectrograph mounted on the 8-m Gemini South telescope. Our first
sequence of 2 x 900 s observations started at 2:44 UT on 20 February
2010 and cover the range from 6500 - 9500 A. Only the proposed host
galaxy was contained on the slit for these spectra. Our second set,
starting immediately afterward, cover the wavelength range from 4500 -
7500 A and both the proposed host and afterglow are positioned on the
slit.
From the nearby galaxy, we detect strong emissions features corresponding
to H-alpha, H-beta, and [O III] at a common redshift of z = 0.217.
The spectrum of the afterglow shows a strong break at ~ 6880 A, with
only faint continuum blueward of this feature. Interpreting this as
the Lyman-alpha break, this correponds to a redshift of z ~ 4.7. We
find marginal evidence for narrow absorption features corresponding to Si
II and Si II* at z = 4.65 redward of the break - however the relatively
low signal-to-noise ratio of our spectrum in this regime makes this result
somewhat uncertain.
Our derived redshifts for both objects are similar to, though slightly
less than, the values derived by Groot et al. (GCN 10441) from the
VLT/X-shooter. They are also consistent with the photometric redshift of
z ~ 4.5 derived by Kruehler et al. (GCN 10439) from GROND.
GCN Circular 10441
Subject
GRB 100219A: VLT/X-shooter redshift
Date
2010-02-20T04:48:54Z (16 years ago)
From
Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst <malesani@dark-cosmology.dk>
P. Groot (Radboud Univ. Nijmegen), L. Kaper, L. Ellerbroek (Univ.
Amsterdam), D. Malesani (DARK/NBI), P. Jakobsson (Univ. Iceland), J. P.
U. Fynbo, J. Hjorth, D. J. Watson (DARK/NBI), and E. Mason (ESO), report
on behalf of a larger collaboration:
We observed the optical objects associated to GRB 100219A (Rowlinson et
al., GCN 10430; Holland & Rowlinson, GCN 10432; Bloom & Nugent, GCN
10433; Jakobsson et al., GCN 10438; Kruehler et al., GCN 10439) with the
VLT equipped with the X-shooter spectrograph. The slit was oriented so
to include both the pre-existing object and the candidate afterglow.
Observations started on 2010 Feb 20.105 UT (0.47 days after the GRB),
for a total exposure time of 4x1200 s.
In a preliminary analysis of the spectra, we detect a clear signal from
both objects. The continuum from the candidate afterglow is only
detected redward of ~5310 AA. A further spectral break is recognised at
~7060 AA. This is consistent with the onset of the Lyman limits and of
the Lyman alpha forest at a common redshift z = 4.8. Our observations
are consistent with the photometric redshift indicated by the GROND
observations (Kruehler et al., GCN 10439).
The high luminosity of the object and its spectral shape indicate that
this is indeed the afterglow of GRB 100219A.
The spectrum of the nearby galaxy implies a significantly lower
redshift, around z=0.25, hence it is unrelated to the GRB.
We caution that the above analysis (particularly the wavelength
solution) is preliminary. Reduction with updated calibrations is
underway. We would like to thank Alain Smette (ESO) for his kind assistance.
GCN Circular 10440
Subject
GRB100219A Akeno and Okayama MITSuME Optical Observation
Date
2010-02-20T03:43:34Z (16 years ago)
From
Daisuke Kuroda at OAO/NAOJ <dikuroda@oao.nao.ac.jp>
D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ), H. Nakajima,
Y.Yatsu, Y.A.Mori, A.Endo, T. Shimokawabe, and N. Kawai(Tokyo Tech),
S. Nagayama (NAOJ), M. Yoshida (Hiroshima) and K. Ohta (Kyoto)
report on behalf of the MITSuME collaboration:
We observed the field of GRB 100219A (Rowlinson et al. GCN 10430)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Akeno Observatory and Okayama
Astrophysical Observatory. We found the afterglow at the XRT
position (Holland et al. GCN 10432, Rowlinson et al. GCN 10435
and Evans et al. GCN 10437) in Rc and Ic band.
The coordinates of the object are:
RA(J2000.0) 10:16:48.50 (+- 0.5 arcsec)
DEC(J2000.0) -12:34:00.6 (+- 0.3 arcsec)
But we could not detect the optical afterglow previously
reported by Holland and Rowlinson (GCN 10436)
Photometric results and three sigma upper limits of the OT are
listed below. We used GSC2.3 catalog for flux calibration.
Akeno Observatory:
The observation started on 2010-02-19 15:17:30 UT (104s after the
trigger).
PDAY MID-UT T-EXP g' Rc Ic
-----------------------------------------------------
0.00471 15:22:34 540.0 19.8+-0.3 18.5+-0.3
----------------------------------------------------
Okayama Astrophysical Observatory:
The observation started on 2010-02-19 15:20:08 UT (262 sec after
the trigger).
PDAY MID-UT T-EXP g' Rc Ic
-----------------------------------------------------
0.00675 15:25:30 540.0 >19.1 >19.0 17.8+-0.2
0.01428 15:36:21 540.0 >19.1 >19.1 17.5+-0.1
0.02177 15:47:07 540.0 >19.1 18.4+-0.2 18.1+-0.3
0.06589 16:50:40 3000.0 >19.4 >19.7 18.9+-0.3
-----------------------------------------------------
GCN Circular 10439
Subject
GRB 100219A: GROND observations
Date
2010-02-20T02:53:11Z (16 years ago)
From
Thomas Kruehler at MPE/MPI <kruehler@mpe.mpg.de>
T. Kruehler (MPE), A. Nicuesa (Tautenburg Obs.), S. Klose (Tautenburg
Obs.), J. Greiner and P. Afonso (both MPE Garching) report on behalf of
the GROND team:
We observed the field of GRB 100219A (Swift trigger #412982; Rowlinson et
al., GCN #10430) simultaneously in g'r'i'z'JHK with GROND (Greiner et al.
2008, PASP 120, 405) mounted at the 2.2 m MPI/ESO telescope at LaSilla
Observatory (Chile).
Observations started on 20 February 2010 at 00:30 UT, 8.7 hours after the
GRB trigger.
Inside the XRT error circle (Evans et al., GCN #10437), we detect the
source mentioned in Jakobsson et al. GCN #10438, spatially separated by 3"
from the object mentioned in Holland et al. GCN#10432 and Bloom & Nugent
GCN #10433.
The object inside the XRT error circle is well detected in the r' band and
redder, but not in g'. Preliminary photometry yields an AB magnitude of
i'=21.5 calibrated against the GROND zeropoint at 9.0 hours after the
trigger. At the moment no statement about variability can be made.
However, if this is the afterglow of GRB 100219A, its colors indicate a
relatively high redshift event (z around 4.5).
GCN Circular 10438
Subject
GRB 100219A: NOT OA observations
Date
2010-02-20T02:40:12Z (16 years ago)
From
Pall Jakobsson at U of Iceland <pja@raunvis.hi.is>
P. Jakobsson (U. Iceland), D. Malesani (DARK, NBI),
C. Villforth (Tuorla Observatory), J. Hjorth,
D. J. Watson (DARK, NBI) and N. R. Tanvir (U. Leicester)
report on behalf of a larger collaboration:
Using StanCam on the Nordic Optical Telescope (NOT) we have
obtained R-band imaging of the GRB 100219A field
(Rowlinson et al., GCN 10430) on Feb 20.02 (9.25 hours after
the burst). Right in the middle of the revised XRT error circle
(Evans et al., GCN 10437) we detect an object at the following
coordinates:
RA(J2000) = 10:16:48.49
Dec(J2000) = -12:34:00.5
Its magnitude is R = 22.2 +- 0.1 based on USNO-B1 calibration. The
object first noticed by Holland & Rowlinson (GCN 10436) and found in
pre-explosion images by Bloom & Nugent (GCN 10437) is well detected in
our images, and is located 3.1" NNE of the above object.
An image of the field is shown at:
http://www.astro.ku.dk/~malesani/GRB/100219A/finder_100219A.png
GCN Circular 10437
Subject
GRB 100219A: Enhanced Swift-XRT position
Date
2010-02-20T00:49:00Z (16 years ago)
From
Phil Evans at U of Leicester <pae9@star.le.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 1938 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 100219A, 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 = 154.20206, -12.56671 which is equivalent
to:
RA (J2000): 10h 16m 48.49s
Dec (J2000): -12d 34' 00.2"
with an uncertainty of 1.4 arcsec (radius, 90% confidence).
This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).
This circular was automatically generated, and is an official product of the
Swift-XRT team.
GCN Circular 10436
Subject
GRB 100219A: Swift/UVOT Detection of the Optical Afterglow
Date
2010-02-20T00:18:39Z (16 years ago)
From
Stephen Holland at USRA/NASA/GSFC/SSC <Stephen.T.Holland@nasa.gov>
S. T. Holland (CRESST/GSFC/USRA) and
A. Rowlinson (U. Leicester) report
on the behalf of the Swift UVOT team:
Swift/UVOT began settled observations of the field of GRB
100219A starting 161 s after the BAT trigger (Rowlinson, et al. 2010,
GCN Circ. 10430). Settled exposures started at T+183 s. The source
reported by Holland, et al. (2010, GCN Circ. 104322) is seen in the
white and u-band exposures. Preliminary 3-sigma magnitudes and upper
limits are
Filter T_start T_stop Exp(s) Mag Err
------------------------------------------------------
white 183 333 150 20.91 0.28
white 875 1718 225 >21.6 3-sigma UL
v 673 1767 136 >19.7 3-sigma UL
b 598 1693 117 >20.5 3-sigma UL
u 341 1668 343 20.35 0.35
uvw1 722 1812 113 >19.9 3-sigma UL
uvm2 697 1792 39 >18.3 3-sigma UL
uvw2 648 1297 78 >19.5 3-sigma UL
------------------------------------------------------
The fading observed between T+183 s and T+875 s suggests that
this is the afterglow of GRB 100219A superimposed on the host galaxy
candidate of Bloom and Nugent (2010, GCN Circ. 10433). The weak
detection in the u band suggests that this source has a redshift of
less than approximately 2.8.
The quoted magnitudes have not been corrected for the expected
Galactic extinction along the line of sight corresponding to a
reddening of E_{B-V} = 0.08 mag (Schlegel, et al., 1998, ApJS, 500,
525). All photometry is on the UVOT photometric system described in
Poole et al. (2008, MNRAS, 383, 627).
GCN Circular 10434
Subject
GRB 100219A: Swift-BAT refined analysis
Date
2010-02-19T21:13:35Z (16 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@lheamail.gsfc.nasa.gov>
W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC/UMD),
D. M. Palmer (LANL), A. Rowlinson (U Leicester), T. Sakamoto (GSFC/UMBC),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
Using the data set from T-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 100219A (trigger #412982)
(Rowlinson, et al., GCN Circ. 10430). The BAT ground-calculated position is
RA, Dec = 154.202, -12.555 deg which is
RA(J2000) = 10h 16m 48.4s
Dec(J2000) = -12d 33' 19.4"
with an uncertainty of 2.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 71%.
The mask-weighted light curve shows a roughly triangular shaped peak
starting at ~T-10sec, peaking at ~T+30 sec, and ending at ~T+50 sec
(possibly out to ~T+100 sec). T90 (15-350 keV) is 18.8 +- 5.0 sec
(estimated error including systematics).
The time-averaged spectrum from T+19 to T+45 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.34 +- 0.25. The fluence in the 15-150 keV band is 3.7 +- 0.6 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+31.89 sec in the 15-150 keV band
is 0.4 +- 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/412982/BA/
GCN Circular 10433
Subject
GRB 100219A: Pre-explosion imaging and host candidate
Date
2010-02-19T17:55:52Z (16 years ago)
From
Josh Bloom at UC Berkeley <jbloom@astron.berkeley.edu>
J. S. Bloom (UC Berkeley) and P. E. Nugent (LBNL) report:
"We co-added 27 archival images from the DeepSky* project at Palomar Observatory covering the field of GRB 100219A (Rowlinson et al. 2010, GCN Circ. 10430). The images were obtained between 2004-2007 from the Palomar-Quest Consortium at the Oschin Schmidt telescope. The limiting magnitude of the stack is approximately R ~ 22.5 mag.
In the combined image we detect a faint (R = 21.0 +/- 0.3 mag relative to nearby USNO catalog stars) slightly extended source, outside the current XRT error circle to the North by ~3.7". The approximate (+/- 1") coordinates of the source are:
RA = 10:16:48.52, DEC = -12:33:57.5 (J2000)
Within the errors, this is coincident with the UVOT source reported by Holland et al. (GCN 10432). This is a potential (lowish redshift) host candidate of the event and we encourage spectroscopic follow-up."
* http://supernova.lbl.gov/~nugent/deepsky.html
GCN Circular 10432
Subject
GRB 100219A: Swift/UVOT Detection of a Source near the XRT Position
Date
2010-02-19T17:29:24Z (16 years ago)
From
Stephen Holland at USRA/NASA/GSFC/SSC <Stephen.T.Holland@nasa.gov>
S. T. Holland (CRESST/GSFC/USRA),
N. P. M. Kuin (UCL-MSSL), and
A. Rowlinson (U Leicester)
report on the behalf of the Swift/UVOT team:
The Swift/UVOT observed the field of GRB 100219A (Rowlinson et
al. 2010, GCN Circ. 10430) starting 183 s after the BAT detection. We
do not detect any source inside the XRT error circle, but we do detect
a source 3.8 arcsec north of the centre of the 2.1 arcsec XRT error
circle. This source is not present in the SDSS DR7, USNO B1.0, or
2MASS point source catalogues. It is at the detection limit of the
DSS, so it is unclear if this is a new source. The preliminary UVOT
position is
RA (J2000) 10:16:48.54 = 154.20225 (deg)
Dec (J2000) -12:33:57.9 = -12.56608 (deg)
with an estimated uncertainty of 1.0 arcsec (radius, 90% confidence,
statistical + systematic).
Preliminary magnitudes for this source are
Filter TSTART TSTOP Exposure Mag Err Sigma
---------------------------------------------------------------
white 183 333 150 20.70 0.34 3.2
white 875 1025 150 >20.9 3-sigma UL
u 341 591 250 21.00 0.56 2.0
---------------------------------------------------------------
It is not clear if this source is fading, or if it is associated with
GRB 100219A.
The quoted magnitudes have not been corrected for the expected
Galactic extinction along the line of sight corresponding to a
reddening of E_{B-V} = 0.08 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 10430
Subject
GRB 100219A: Swift detection of a burst
Date
2010-02-19T15:32:18Z (16 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@lheamail.gsfc.nasa.gov>
A. Rowlinson (U Leicester), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
D. N. Burrows (PSU), V. D'Elia (ASDC), P. A. Evans (U Leicester),
N. Gehrels (NASA/GSFC), O. Godet (U Leicester),
S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), N. P. M. Kuin (UCL-MSSL),
O. M. Littlejohns (U Leicester), V. Mangano (INAF-IASFPA),
J. Mao (INAF-OAB), F. E. Marshall (NASA/GSFC),
P. T. O'Brien (U Leicester), C. Pagani (U. Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL),
P. Romano (INAF-IASFPA), T. Sakamoto (NASA/UMBC),
B. Sbarufatti (INAF-OAB/IASFPA), M. H. Siegel (PSU),
M. Stamatikos (OSU/NASA/GSFC), M. A. Stark (PSU), M. C. Stroh (PSU)
and L. Vetere (PSU) report on behalf of the Swift Team:
At 15:15:46 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 100219A (trigger=412982). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 154.221, -12.559 which is
RA(J2000) = 10h 16m 53s
Dec(J2000) = -12d 33' 31"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). As is usual for an image trigger, the BAT light
curve shows nothing of interest.
The XRT began observing the field at 15:18:45.0 UT, 178.5 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 154.2024,
-12.5671 which is equivalent to:
RA(J2000) = 10h 16m 48.58s
Dec(J2000) = -12d 34' 01.7"
with an uncertainty of 2.1 arcseconds (radius, 90% containment). This
location is 71 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
6.51e+20 cm^-2 (Kalberla et al. 2005).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 183 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
0.08.
Burst Advocate for this burst is A. Rowlinson (bar7 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.)