Astron. Astrophys. 344, 459-471 (1999)

The M31 population of supersoft sources

P. Kahabka

Astronomical Institute and Center for High Energy Astrophysics, University of Amsterdam, Kruislaan 403, 1098 SJ, Amsterdam, The Netherlands

Received 9 February 1998 / Accepted 11 January 1999

Abstract

The 1991 ROSAT PSPC M31 X-ray point source catalog has been screened in order to set up a sample of candidate supersoft sources in this galaxy, additional to the 16 supersoft sources already known in M31 (Supper et al. 1997). Selection criteria used were based on hardness ratios ("X-ray colors"), as developed in an earlier paper (Kahabka 1998). An additional criterion to be fulfilled was that the observed count rate is in agreement with the expected steady-state luminosity for a source with these hardness ratios. This condition constrained mainly the hydrogen absorbing column towards the source. 26 candidates not correlating with foreground stars and M31 supernova remnants have been found to fulfil one of the selection criteria. They can be considered to be candidate supersoft sources in M31. This comprises 6% of all point sources in this galaxy. For these candidates absorbing hydrogen column densities, effective temperatures and white dwarf masses (assuming the sources are on the stability line of surface nuclear burning) are derived. An observed white dwarf mass distribution is derived which indicates that the masses are constrained to 0.90 .

The entire population of supersoft sources in M31 is estimated taking a theoretical white dwarf mass distribution into account and under the assumption that the observationally derived sample is restricted to white dwarf masses above . Taking into account that the gas and the source population have different scale heights a total number of at least 200-500 and at most 6,000-15,000 sources is deduced (depending on the used galaxy model), making use of the population synthesis calculation of Yungelson et al. (1996).

The spatial distribution favors a disk (or spiral-arm) dominated young stellar population with a ratio of 1/(4-7) of bulge/disk systems, very similar to what has been found for novae in the Milky Way but lower than favored for novae in M31 (1/2). Supersoft sources and Cepheids both show association with the M31 spiral arms and may belong to a younger stellar population. A mean space density of is inferred for the supersoft sources. Assuming that all supersoft sources with masses in excess of are progenitors of supernovae of type Ia, a SN Ia rate of is derived for M31 based on these progenitors. Supersoft sources might be able to account for 20-100% of the total SN Ia rate in a galaxy like M31.

Key words: stars: evolution stars: white dwarfs galaxies: individual: M 31 X-rays: stars

Send offprint requests to: ptk@astro.uva.nl

SIMBAD Objects

Contents

• 1. Introduction
• 2. The sample of supersoft sources in M31
  • 2.1. The SW-sample
  • 2.2. The complimentary sample (C-sample)
• 3. Estimating the total population
  • 3.1. The observation derived distribution
  • 3.2. The derived white dwarf mass distribution
  • 3.3. Correcting for the and distribution
• 4. Constraining the scale height ratio and the total population from the normalized histogram
  • 4.1. Possible -models
    • 4.1.1. The Supper- model
    • 4.1.2. The Urwin- model
  • 4.2. Expected incompleteness of coverage as a function of hydrogen column density and white dwarf mass
  • 4.3. Number of supersoft sources expected for the Supper- model
  • 4.4. Number of sources expected with the Urwin- model
  • 4.5. Comparison with the galactic population
• 5. The spatial distribution
• 6. Estimating a SN Ia rate inferred from the population of supersoft sources in M31
• 7. Conclusions
• Acknowledgements
• References

© European Southern Observatory (ESO) 1999

Online publication: March 18, 1999
helpdesk.link@springer.de