XMM-Newton Observations of GRB020322



  • On March 22, 2002, the XMM-Newton SOC received a Target of Opportunity notification after the BeppoSAX detection of GRB020322.
  • This GRB was immediately approved by the XMM-Newton SOC for ToO observation. The observation was started on 2002-03-22T18:18:00Z under ObsId=0128530801 during XMM-Newton's revolution number 0418.
  • The pointing coordinates were RA = 18:00:49.4 and Dec = +81:06:10.8 (Gandolfi et al.)
  • A source was shortly identified in EPIC, ~20 arcsec off the reported coordinates, well away from inter-CCD gaps.
  • On Mar 22, 2002 20:46, GCN1293 was issued, reporting a first estimate of the coordinates of that bright source and its count rate.
  • The images and light curves presented here are based on a preliminary processing without the re-constituted XMM-Newton Attitude History File. Therefore, the positions quoted are subject to an uncertainty of 4 arcsec.


Data (Re-processing)

  • The Observation Data File (ODF) for GRB020322 was re-generated on 03-Apr-2003 in order to eliminate information contained in the old ODF (with id: 0110980301) belonging to the previous observation. This was preventing the nominal Pipeline processing of the data.
    The new ODF (with id: 0128530801) now contains only the GRB020322 data and has been successfully processed by the Pipeline.
    The new ODF is available here as 0128530801.tar.gz.
  • The Pipeline Products are also available in the ftp area. Details of the Pipeline process can be found here



Preview of XMM-Newton images

Full pn image in sky coordinates.
Full PN
pn contour levels (blue) onto the Gunn r-band image from Bloom et al.
PN Contour Levels
The image is centered at the "b" source in GCN1296 from Bloom et al. which has been suggested to be the optical after-glow of GRB020322 (GCN1298).
Full OM image in sky coordinates.
Full OM
The extended blob and ring-like features near the center of the image are due to stray light.
Expanded OM-UVW1 view near source "b".


Quick Look Analysis

Light curves for the two brightest pn sources within 2arcmin of the reported BeppoSax position (labelled as #1 and #2 in the image above). Only pixels within 30arcsec of the sources peak have been considered for the light curves.

Count Rates
The total count rate from the brightest source decreased by a factor ~2 in ~12ks.