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[vsnet-grb-info 2] GRB011130 (XRF011130) Chandra Observations
TITLE: GCN GRB OBSERVATION REPORT
NUMBER: 1185
SUBJECT: GRB011130 (XRF011130) Chandra Observations
DATE: 01/12/11 07:50:50 GMT
FROM: Roland Vanderspek at MIT <roland@space.mit.edu>
GRB011130 (=XRF011130): Results of a Target of Opportunity Observation
with the Chandra X-ray Observatory
G. Ricker, P. Ford, G. Monnelly, N. Butler, R. Vanderspek (MIT); and
D. Lamb (U.Chicago)
on behalf of the Chandra ToO Team and the HETE Science Team
write:
On 10 December, from 00:38 UT - 09:27 UT, the Chandra Observatory
targeted the field of the X-ray rich gamma-ray burst XRF011130 that
was previously localized by the HETE satellite (Ricker et al.,
GCN1165). The revised error circle for XRF011130 (Ricker et al.
GCN1178) fit completely within the field-of-view of the ACIS-I array
on Chandra. The observation duration was 30 ksec.
As a result of the special arrangements made by the Chandra Science
Center to expedite the pre-processing of the data from our
observation, the TOO Science Team has been able to establish the
location and relative intensity for the 10 brightest X-ray sources
within the HETE field.
The following table lists the J2000 coordinates of the 10 brightest
sources we have established in the HETE Field:
Chandra Name RA DEC dRA(s) dDEC('') Cts
CXOU J030527.9+034657 3 5 27.88 3 46 57.04 0.061 0.96 110
CXOU J030532.5+035140 3 5 32.50 3 51 40.37 0.061 0.96 101
CXOU J030534.3+034958 3 5 34.26 3 49 58.94 0.061 0.96 33
CXOU J030514.2+034854 3 5 14.21 3 48 54.19 0.061 0.96 30
CXOU J030550.1+035009 3 5 50.10 3 50 9.38 0.064 0.99 27
CXOU J030458.7+034702 3 4 58.68 3 47 2.92 0.069 1.03 27
CXOU J030541.4+034808 3 5 41.43 3 48 8.02 0.061 0.97 26
CXOU J030534.2+034208 3 5 34.22 3 42 8.75 0.070 1.10 23
CXOU J030512.9+034936 3 5 12.91 3 49 36.35 0.062 0.97 22
CXOU J030536.0+035303 3 5 36.01 3 53 3.58 0.062 0.97 21
The astrometry was calibrated by correlating against four USNO A2
catalog stars.
In the table, delta(RA), the uncertainty in RA, and delta(DEC),the
uncertainty in DEC, were established by summing the following in
quadrature for each coordinate: the error reported by celldetect,
the error reported by the correlation code, and the error estimate
from the star reference catalog.
We gratefully acknowledge the timely assistance of the personnel
at the Chandra Science Center in the preparation of these data.
This message may be cited.
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