| Issue |
A&A
Volume 464, Number 1, March II 2007
AMBER: Instrument description and first astrophysical results
|
|
|---|---|---|
| Page(s) | 299 - 307 | |
| Section | Stellar atmospheres | |
| DOI | https://doi.org/10.1051/0004-6361:20066098 | |
| Published online | 19 December 2006 | |
The hot subdwarf B + white dwarf binary KPD 1930+2752*,**,***,****
A supernova type Ia progenitor candidate
1
Dr.-Remeis-Sternwarte, Institute for Astronomy, University Erlangen-Nuremberg, Sternwartstr. 7, 96049 Bamberg, Germany e-mail: geier@sternwarte.uni-erlangen.de
2
Centre of Astrophysics Research, University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK
3
Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA
Received:
25
July
2006
Accepted:
27
October
2006
Context.The nature of the progenitors of type Ia supernovae is still under
debate. KPD 1930+2752 is one of the best SN Ia progenitor candidates known
today. The object is a double degenerate system consisting of a
subluminous B star (sdB) and a massive white dwarf (WD). Maxted et al. ([CITE])
conclude that the system mass exceeds the Chandrasekhar mass. This
conclusion, however, rests on the assumption that the sdB mass is
. However, recent binary population synthesis calculations
suggest that the mass of an sdB star may range from 
to more
than 
.
Aims. It is therefore important to measure the mass of the sdB star simultaneously with that of the white dwarf. Since the rotation of the sdB star is tidally locked to the orbit, the inclination of the system can be constrained if the sdB radius and the projected rotational velocity can be measured with high precision. An analysis of the ellipsoidal variations in the light curve allows the constraints derived from spectroscopy to be tightened.
Methods.We derived the mass-radius relation for the sdB star from a quantitative spectral analysis of 150 low-resolution spectra obtained with the Calar Alto 2.2 m telescope using metal-rich, line-blanketed LTE model atmospheres with and without NLTE line formation. The projected rotational velocity was determined for the first time from 200 high-resolution spectra obtained with the Keck I 10 m and with the ESO-VLT 8.2 m telescopes. In addition a reanalysis of the published light curve was performed.
Results.The atmospheric and orbital parameters were measured with unprecedented accuracy. In particular the projected rotational velocity 
was determined.
Assuming the companion to be a white dwarf, the mass of the sdB is limited
between 
and 
and the corresponding total
mass of the system ranges from 
to 
. This
constrains the inclination to 
. The photometric analysis allows the parameters to be constrained even more.
A neutron star companion can be ruled out and the mass of the sdB is limited to the range between
and 
. The total mass of the system ranges from
to 
and hence is likely to exceed the Chandrasekhar mass. The inclination angle is
and the light curve shows weak and shallow signs of eclipses. A high-precision light curve is needed in order to accurately measure these eclipses.
So KPD 1930+2752 qualifies as an excellent double degenerate supernova Ia progenitor candidate.
Some of the data presented here were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation.
Based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut für Astronomie and the Instituto de Astrofísica de Andalucía (CSIC).
© ESO, 2007
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