The X-ray Reconvolution of NGC 3603

Details The X-ray Reconvolution of NGC 3603 The X-ray Reconvolution of NGC 3603

Nov 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aas...198.9503b&link_type=abstract

American Astronomical Society, 198th AAS Meeting, #95.03; Bulletin of the American Astronomical Society, Vol. 33, p.1182

Astronomy and Astrophysics

Astronomy

Scientific paper

The massive star cluster NGC 3603, the ionizing source of a Galactic supergiant HII region, has long been thought of as a nearby analog to more distant starburst galaxies. As such, it is an interesting and useful object of study for stellar and galactic astronomers alike. We have obtained a 50 ksec observation of this region using the CHANDRA X-ray observatory. The high stellar density in the core and the distance to the cluster ( 7 kpc), however, render the stars in the core unresolved even to CHANDRA. In order to properly determine the X-ray luminosities of the stars in the core, and to examine the evidence for diffuse X-ray emission near the core, we have attempted to "reconvolve" the X-ray image by simulating the expected distribution of X-ray photons. As a template, we have used an optical image of the stars in the cluster obtained by the HST Planetary Camera. We find that we can produce the observed CHANDRA image of the core of the cluster using this technique, as well as derive constrained source luminosities for all the member stars in the core. In addition, we show that the observed contribution of diffuse X-ray emission is generally small in the core, though there are some limited regions devoid of strong stellar emission where diffuse X-ray emission may be important. This work was supported by NASA and the Chandra project (award number GO0-1047Z).

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