Optical novae: the major class of supersoft X-ray sources in M 31
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, 85741 Garching, Germany e-mail: email@example.com
2 Universitätssternwarte München, Scheinerstraße, 81679 München, Germany
3 Institut d'Estudis Espacials de Catalunya (ICE-CSIC), Campus UAB, Facultat de Ciencies, 08193 Bellaterra, Spain
Accepted: 19 June 2005
We searched for X-ray counterparts of optical novae detected in M 31 and M 33. We combined an optical nova catalogue from the WeCAPP survey with optical novae reported in the literature and correlated them with the most recent X-ray catalogues from ROSAT, XMM-Newton, and Chandra, and – in addition – searched for nova correlations in archival data. We report 21 X-ray counterparts for novae in M 31 – mostly identified as supersoft sources (SSS) by their hardness ratios – and two in M 33. Our sample more than triples the number of known optical novae with a supersoft X-ray phase. Most of the counterparts are covered in several observations allowing us to constrain their X-ray light curves. Selected brighter sources were classified by their XMM-Newton EPIC spectra. We use the well-determined start time of the SSS state in two novae to estimate the hydrogen mass ejected in the outburst to ~ and ~, respectively. The supersoft X-ray phase of at least 15% of the novae starts within a year. At least one of the novae shows a SSS state lasting 6.1 years after the optical outburst. Six of the SSSs turned on between 3 and 9 years after the optical discovery of the outburst and may be interpreted as recurrent novae. If confirmed, the detection of a delayed SSS phase turn-on may be used as a new method to classify novae as recurrent. At the moment, the new method yields a ratio of recurrent novae to classical novae of 0.3, which is in agreement (within the errors) with previous works.
Key words: galaxies: individual: M 31 / galaxies: individual: M 33 / stars: novae, cataclysmic variables / X-rays: galaxies / X-rays: binaries
© ESO, 2005