GRB 100213B
GCN Circular 10913
Subject
GRB 100213B: Detection of Fading Optical Afterglow
Date
2010-06-30T23:03:00Z (16 years ago)
From
Jules Halpern at Columbia U. <jules@astro.columbia.edu>
Y. Li, J. Weston, X. Fernandez, A. Brown, J. H. Yoon, A. P. S. Crotts,
and J. P. Halpern (Columbia U.) report on behalf of the graduate
Observational Astronomy class:
"We obtained R-band images of the field of Swift GRB 100213B (Vetere et al.,
GCN 10412) on two consecutive, photometric nights using the MDM 1.3m
telescope, for total exposure times of 30 and 40 minutes, respectively.
Within 3.8" of the enhanced Swift XRT afterglow position (of 90% confidence
radius 3.5", Evans, GCN 10423), we find a fading object at
(J2000) R.A. = 08h 17m 07.94s, Decl. = +43d 26' 54.94"
with positional uncertainty ~0.5", and the following magnitudes:
----------------------------------------------------------
Date(UT) Mid-time(UT) t-t0(hr) Exp(min) R(mag)
----------------------------------------------------------
Feb. 14 03:44 4.8 30 22.00+/-0.14
Feb. 15 03:35 28.6 40 23.01+/-0.24
----------------------------------------------------------
Magnitudes are referenced to Landolt (1992) standard stars, and are not
corrected for Galactic extinction.
The position of the afterglow coincides with the R ~ 21.5 object detected by
Malesani et al. (GCN 10413) 19 minutes after the GRB, and whose redshift
z = 0.604 was measured by Cucchiara et al. (GCN 10422). We conclude that the
observed variability and positional coincidence with an emission-line object
establishes the optical afterglow and host galaxy redshift of GRB 100213B.
Further observations of the host galaxy are encouraged.
MDM images of the field are posted at
http://www.astro.columbia.edu/~jules/grb/100213b/
This message may be cited."
GCN Circular 10454
Subject
GRB 100213B: Mondy optical observations
Date
2010-02-26T02:54:05Z (17 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
E. Klunko (ISTP), A. Volnova (SAI MSU), A. Pozanenko (IKI) on behalf of
larger GRB follow up collaboration report:
We observed the field of GRB 100213B (Vetere et al., GCN 10412) with
AZT-33IK telescope of Sayan observatory (Mondy) starting Feb. 14 (UT)
14:54:31. We do not detect any sources in enhanced XRT error circle (Evans,
GCN 10423). The upper limit (3 sigma) of stacked image is based on
USNO-B1.0 nearby stars:
T0+ Filter, Exposure, mag.
(mid, d) (s)
0.6801 R 94x30 > 20.80
GCN Circular 10426
Subject
GRB 100213B: GRT Optical Observation
Date
2010-02-15T20:34:15Z (17 years ago)
From
Takanori Sakamoto at NASA/GSFC <takanori@milkyway.gsfc.nasa.gov>
T. Sakamoto (UMBC/GSFC), D. Donato (ORAU/GSFC), N. Gehrels (GSFC),
T. Okajima (JHU/GSFC), Y. Urata (NCU), C.A. Wallace (FGCU)
We observed the field of GRB 100213B detected by Swift
(trigger #412220; Vetere et al., GCN Circ. 10412) with the 14-inch
Goddard Robotic Telescope (GRT) located at the Goddard Geophysical
and Astronomical Observatory (http://cddisa.gsfc.nasa.gov/ggao/).
Total 59 images of 60 sec exposures were taken in the R filter
starting from February 13 23:55:15 (UT) about 0.94 hours after
the trigger and stopped on February 14 01:50:46 (UT). We do
not detect the optical afterglow both in the individual images
and the combined image inside the XRT position (Evans, GCN #10423).
The estimated three sigma upper limit of the combined image
(total exposure of 3540 sec) is ~18.7 mag using the USNO-B1 catalog.
GCN Circular 10423
Subject
GRB 100213B: Enhanced Swift-XRT position
Date
2010-02-14T17:42:01Z (17 years ago)
From
Phil Evans at U of Leicester <pae9@star.le.ac.uk>
P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team.
Using 819 s of XRT Photon Counting mode data and 1 UVOT
image for GRB 100213B, 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 = 124.28226, +43.44773 which is equivalent
to:
RA (J2000): 08h 17m 7.74s
Dec (J2000): +43d 26' 51.8"
with an uncertainty of 3.5 arcsec (radius, 90% confidence). This position
is 3.7" from the object reported by Malesani et al. (GCN Circ. 10413) and
Cucchiara et al (GCN Circ. 10422).
Position enhancement is described by Goad et al. (2007, A&A, 476, 1401) and
Evans et al. (2009, MNRAS, 397, 1177).
This circular is an official product of the Swift-XRT team.
GCN Circular 10422
Subject
GRB 100213B: Gemini-N Observations
Date
2010-02-14T13:52:00Z (17 years ago)
From
Antonino Cucchiara at PSU <cucchiara@astro.psu.edu>
A. Cucchiara (PSU), R. Chornock (Harvard),D. B. Fox (PSU),
E. Berger (Harvard), report on behalf of a larger collaboration:
"We observed the field of GRB 100213B (Vetere et al., GCN 10412)
with GMOS on the Gemini-North 8-m telescope starting on 2010
Feb 14.24 (~7 hours after the burst).
Inside the refined XRT error circle (GCN #10416) we detect
no new sources in a 2 min r-band acquisition image.
Outside the XRT error circle we clearly detect the source
reported by Malesani et al. (GCN #10413).
We then obtain 2x1200s spectra on this source at central
wavelength 8000A. We detect [OII]3727, H-beta and [OIII]5007
at the common redshift of z =0.604.
At this point is not clear whether this object is related to
GRB 100213B.
We thank the Gemini staff for performing this observation, in
particular Tom Geballe."
GCN Circular 10421
Subject
GRB 100213B: Swift/UVOT Upper Limits
Date
2010-02-14T12:39:59Z (17 years ago)
From
Peter Curran at MSSL <pac@mssl.ucl.ac.uk>
P.A. Curran (MSSL-UCL) and L. Vetere (PSU) report on behalf of the
Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 100213B
158 s after the BAT trigger (Vetere et al., GCN 10412). No optical
afterglow consistent with the XRT position (Vetere et al., GCN 10416) or
the NOT R-band position (Malesani et al., GCN 10413) is detected in the
initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) for the initial exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
--------------------------------------------------
white 158 4654 273 >21.17
v 3430 5065 393 >19.64
b 4250 5722 233 >20.38
u 4044 5679 393 >20.38
w1 3840 5475 393 >20.31
m2 3634 5269 393 >21.10
w2 4660 4860 197 >20.00
The values quoted above are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.08 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 10419
Subject
GRB 100213B: PAIRITEL NIR Upper Limits
Date
2010-02-14T08:57:49Z (17 years ago)
From
Adam Morgan at U.C. Berkeley <qmorgan@gmail.com>
A. N. Morgan, B. E. Cobb, C. R. Klein, J. S. Bloom (UC Berkeley), report:
We observed the field of GRB 100213B (Vetere et al., GCN 10412) with
the 1.3m PAIRITEL located at Mt. Hopkins, Arizona. Observations began
under good weather conditions at 2010-02-14 02:53:48 UT, ~3.92 hours
after the Swift trigger. In mosaics (effective exposure time of ~2387
seconds) taken simultaneously in the J, H, and Ks filters, we do not
detect any sources within the XRT error circle, nor at the potential
NOT position (Malesani et al., GCN 10413).
The preliminary photometry yields:
post_burst
t_mid(h) exp(s) filt U. Limit (3 sig)
4.44 2387 J > 19.2
4.44 2387 H > 18.2
4.44 2387 Ks > 17.1
Observations are ongoing. All magnitudes given in the Vega system,
calibrated to 2MASS. No correction for Galactic extinction has been
made to the above reported values.
GCN Circular 10417
Subject
GRB 100213B: Swift-BAT refined analysis
Date
2010-02-14T05:56:33Z (17 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@lheamail.gsfc.nasa.gov>
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/UMD), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU),
L. Vetere (PSU) (i.e. the Swift-BAT team):
Using the data set from T-61 to T+242 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 100213B (trigger #412220)
(Vetere, et al., GCN Circ. 10412). The BAT ground-calculated position is
RA, Dec = 124.320, 43.464 deg which is
RA(J2000) = 08h 17m 16.8s
Dec(J2000) = +43d 27' 51.7"
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 56%.
The mask-weighted light curve shows a FRED-like pulse starting at ~T-5 sec,
peaking at ~T+5 sec, and ending at ~T+150 sec. Because the burst goes out
of the BAT FOV at T+250 sec (due to an observing constraint), we can not tell
if there if any detectable activity past T+250 sec. T90 (15-350 keV) is
48.0 +- 16.0 sec (estimated error including systematics).
The time-averaged spectrum from T-12.7 to T+35.3 sec is best fit by a power law
with an exponential cutoff. This fit gives a photon index 1.13 +- 0.61,
and Epeak of 39.1 +- 8.8 keV (chi squared 58.8 for 56 d.o.f.). The 1-sec
peak flux measured from T+10.76 sec in the 15-150 keV band is
0.5 +- 0.2 ph/cm2/sec. A fit to a simple power law gives a photon index
of 2.04 +- 0.13 (chi squared 67.0 for 57 d.o.f.). 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/412220/BA/
GCN Circular 10416
Subject
GRB 100213B: Swift XRT refined analysis
Date
2010-02-14T05:07:53Z (17 years ago)
From
Loredana Vetere at PSU <vetere@astro.psu.edu>
L. Vetere (PSU) reports on behalf of the Swift-XRT team:
We have analysed 1.7 ks of XRT data for GRB 100213B (Vetere et al.
GCN Circ. 10412), from 155 s to 5.7 ks after the BAT trigger. The
data comprise 500 s in Windowed Timing (WT) mode with the remainder
in Photon Counting (PC) mode. Using 1.2ks of XRT Photon Counting
mode data we find a refined XRT position: RA, Dec = 124.28384,
43.44683 which is equivalent to:
RA (J2000): 08h 17m 08.12s
Dec (J2000): +43d 26' 48.6"
with an uncertainty of 4.9 arcsec (radius, 90% confidence).
The light curve can be modelled with a power-law decay with a decay
index of alpha=2.06 (+0.10, -0.08). A spectrum formed from the WT
mode data can be fitted with an absorbed power-law with a photon
spectral index of 1.47 (+/-0.12). The best-fitting absorption column
is 1.3 (+0.4, -0.3) x 10^21 cm^-2, in excess of the Galactic value of
5.9 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 4.9 x 10^-11 (5.6 x 10^-11) erg cm^-2 count^-1.
If the light curve continues to decay with a power-law decay index
of 2.06, the count rate at T+24 hours will be 6.9 x 10^-5 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of
3.4 x 10^-15 (3.9 x 10^-15) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00412220.
This circular is an official product of the Swift-XRT team.
GCN Circular 10413
Subject
GRB 100213B: NOT optical observations
Date
2010-02-14T00:44:21Z (17 years ago)
From
Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst <malesani@dark-cosmology.dk>
D. Malesani (DARK/NBI), N.R. Tanvir (Univ. Leicester), D. Xu (WIS,
DARK/NBI), G. Leloudas (DARK/NBI), P. Jakobsson (Univ. Iceland), A.
Somero, and S. Katajainen (Tuorla Obs.), report on behalf of a larger
collaboration:
We observed the field of GRB 100213B (Vetere et al., GCN 10412) with the
NOT equipped with ALFOSC. Due to adverse weather, we could only obtain
one 5-min R-band exposure, starting on Feb 13.970 UT (19 min after the GRB).
We find an object with R ~ 21.5 located just outside the edge of the
XRT error circle, at coordinates RA = 08:17:07.97, Dec = +43:26:54.6.
This location is 8 arcsec away of the X-ray position, which has a
reported error radius of 5.2" (Vetere et al., GCN 10412). The object
seems elongated in our image. However, it is not visible in the SDSS
data of this field, and may therefore be the afterglow of GRB 100213B.
Inside the XRT error circle, there is also a possible source close to
our image detection limit (R ~ 22.2), at coordinates RA = 08:17:08.48,
Dec = +43:26:50.3 (0.8" uncertainty). Given the low S/N, the reality of
this source cannot be confirmed.
Further observations are encouraged. The NOT may attempt again later
tonight depending on the weather conditions.
GCN Circular 10412
Subject
GRB 100213B: Swift detection of a burst
Date
2010-02-13T23:12:15Z (17 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@lheamail.gsfc.nasa.gov>
L. Vetere (PSU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU),
J. M. Gelbord (PSU), D. Grupe (PSU), S. T. Holland (CRESST/USRA/GSFC),
E. A. Hoversten (PSU), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), C. B. Markwardt (CRESST/GSFC/UMD),
F. E. Marshall (NASA/GSFC), C. Pagani (PSU), D. M. Palmer (LANL),
T. Sakamoto (NASA/UMBC), M. H. Siegel (PSU), M. C. Stroh (PSU) and
T. N. Ukwatta (GSFC/GWU) report on behalf of the Swift Team:
At 22:58:34 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 100213B (trigger=412220). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 124.338, +43.455 which is
RA(J2000) = 08h 17m 21s
Dec(J2000) = +43d 27' 19"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve shows a FRED-like pulse
structure with a duration of about 30 sec. The peak count rate
was ~1000 counts/sec (15-350 keV), at ~2 sec after the trigger.
The XRT began observing the field at 23:01:03.7 UT, 149.5 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 124.2858, +43.4473 which is equivalent to:
RA(J2000) = 08h 17m 08.59s
Dec(J2000) = +43d 26' 50.2"
with an uncertainty of 5.2 arcseconds (radius, 90% containment). No
event data are yet available to determine the column density using
X-ray spectroscopy.
The initial flux in the 2.5 s image was 1.75e-09 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 77 seconds with the White filter
starting 157 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 3-sigma upper limit is about 20.5 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 L. Vetere (vetere AT astro.psu.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/too.html.)