Volume 560, December 2013
|Number of page(s)||20|
|Section||Stellar structure and evolution|
|Published online||04 December 2013|
An archive study of 18 old novae
1 INAF – Ossservatorio Astronomico di Trieste, via Tiepolo 11, 34143 Trieste, Italy
2 European Southern Observatory, Karl Schwarzschild-Str. 2, 85748 Garching, Germany
Received: 25 October 2012
Accepted: 14 September 2013
Aims. We present an overview of the UV spectral properties of old novae as a class. The data and results of this paper, together with data from the outburst phases, will be utilized in a follow-up study to determine statistical properties and to investigate correlations among the physical parameters of the quiescent and eruptive phases.
Methods. All the available IUE, HST, and FUSE archive data for 18 old novae were used to derive accurate and homogeneous estimates of the reddening from the 2175 Å extinction bump and to determine the intrinsic spectral energy distribution corresponding to the utilization of both existing extinction curves. We also measured all the emission and absorption lines.
Results. We have found good agreement between spectra taken at different epochs and by different instruments, a clear indication of the near constancy of the SED on timescales of several years. With the possible exception of GK Per, the dereddened UV continua are represented well by a single-curve power-law distribution Fλ ∝ λ− α, with α in the range 0.32–2.55 for one curve and 0.35–2.88 for the other one. The extrapolation of the various UV power laws to the optical range yields values that are in good agreement with the V magnitudes. We interpret this result as evidence that the SED is dominated by the accretion disk in the UV and optical spectral regions. A detailed study of the emission spectrum has led to measuring and identifying more than one hundred features and to detecting several lines that are rather uncommon in other CVs and whose identification is uncertain.
Key words: novae, cataclysmic variables / ultraviolet: stars / line: identification
Based on INES data from the IUE satellite. Some of the data presented in this paper were obtained from the Multimission Archive at the Space Telescope Science Institute (MAST).
Tables 2–7 and 10–14 are available in electronic form at http://www.aanda.org
The final reduced spectra (FITS files) and full Table 2 are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (188.8.131.52) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/560/A49
© ESO, 2013
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