grb040106 - XMM-Newton
XMM-Newton Observation of GRB040106
- GRB040106 was discovered by INTEGRAL on January 06, 2004 at 17:55 UTC in the field of view of the IBIS telescope, GCN/INTEGRAL NOTICE (see also Mereghetti et al., GCN2505).
- Following a quick evaluation, the GRB was approved by the XMM-Newton Project Scientist for a ToO observation at the beginning of revolution 747.
- The observation was manually started on 2004-01-06 at 23:10 UT under ObsId=0158160401 just 5 Hrs 15 mins. after the occurrence of the burst, and lasting for a total of 45 ksec. This has been the fastest XMM-Newton ToO response to date. The pointing coordinates were RA=11:52:18.0, Dec=-46:47:14 as reported in the GCN/INTEGRAL NOTICE of January 06, 2004, 19:25:02 UT.
- Quick-Look-Analysis of the first 30 ksec of the XMM-Newton observation of the GRB040106 field showed the presence of a bright source in the EPIC-pn and MOS cameras within the INTEGRAL error circle, XMMU J115213.1-464713 (Ehle, Gonzalez-Riestra and Gonzalez-Garcia, GCN2508) at a position of R.A. (J2000) = 11h 52m 13.1s, Dec. (J2000) = -46deg 47' 13", with a positional accuracy of better than 10 arcsec.
- The EPIC-pn count rate decreased from 0.7 to 0.2 counts/sec during the first 30 ksec of the observation.
- The Observation Data File (ODF) is available in both the XSA and the ftp server.
- The Pipeline Products are available in the XSA here.
- Details of the Pipeline process are available here
Quick analysis of preliminary XMM-Newton data
The images are centered at the IBAS position of GRB040106 and its reported uncertainty is indicated by the black circle.
A minimum event filtering has been selected to generate this image.
PN light curve
PN light curve of XMMU J115213.1-464713 (background subtracted).
The pn spectrum ofÂ XMMU J115213.1-464713 is absorbed below 1keV, consistent with an Hydrogen column density of ~8.6 1020 cm-2, consistant with the galactic value in this direction. The flux in the 2-10 keV band is approximately 9.9 10 -13 erg cm-2 s-1
XMMU J115213.1-464713 was also clearly detected in RGS as shown in the images and spectra below: