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Orbital periods of cataclysmic variables identified by the SDSS. V, VLT, NTT and Magellan observations of nine equatorial systems

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Southworth, J. (John), Gänsicke, B. T. (Boris T.), Marsh, T. R., Torres, M. A. P., Steeghs, D. (Danny), 1972-, Hakala, P., Copperwheat, C. M., Aungwerojwit, A. (Amornrat) and Mukadam, Anjum S.. (2008) Orbital periods of cataclysmic variables identified by the SDSS. V, VLT, NTT and Magellan observations of nine equatorial systems. Monthly Notices of the Royal Astronomical Society, Vol.391 (No.2). pp. 591-606. ISSN 0035-8711

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Official URL: http://dx.doi.org/10.1111/j.1365-2966.2008.13932.x

Abstract

We present Very Large Telescope (VLT) and Magellan spectroscopy and New Technology Telescope photometry of nine faint cataclysmic variables (CVs) which were spectroscopically identified by the Sloan Digital Sky Survey (SDSS). We measure orbital periods for five of these from the velocity variations of the cores and wings of their H alpha emission lines. Four of the five have orbital periods shorter than the 2-3 h period gap observed in the known population of CVs. SDSS J004335.14-003729.8 has an orbital period of P-orb = 82.325 +/- 0.088 min; Doppler maps show emission from the accretion disc, bright spot and the irradiated inner face of the secondary star. In its light curve, we find a periodicity which may be attributable to pulsations of the white dwarf. SDSS J163722.21-001957.1 has P-orb = 99.75 +/- 0.86 min. By combining this new measurement with a published superhump period, we estimate a mass ratio of q approximate to 0.16 and infer the physical properties and orbital inclination of the system. For SDSS J164248.52+134751.4, we find P-orb = 113.60 +/- 1.5 min. The Doppler map of this CV shows an unusual brightness distribution in the accretion disc which would benefit from further observations. SDSS J165837.70+184727.4 had spectroscopic characteristics which were very different between the SDSS spectrum and our own VLT observations, despite only a small change in brightness. We measure P-orb = 98.012 +/- 0.065 min from its narrow H alpha emission line. Finally, SDSS J223843.84+ 010820.7 has a comparatively longer period of P-orb = 194.30 +/- 0.16 min. It contains a magnetic white dwarf and, with g = 18.15, is brighter than the other objects studied here. These results continue the trend for the fainter CVs identified by the SDSS to be almost exclusively shorter period objects with low mass transfer rates.

Item Type:	Journal Article
Subjects:	Q Science > QB Astronomy
Divisions:	Faculty of Science > Physics
Library of Congress Subject Headings (LCSH):	Double stars -- Spectra, White dwarf stars, Cataclysmic variable stars, Dwarf novae, Stars, New
Journal or Publication Title:	Monthly Notices of the Royal Astronomical Society
Publisher:	Wiley-Blackwell Publishing, Inc
ISSN:	0035-8711
Date:	1 December 2008
Volume:	Vol.391
Number:	No.2
Number of Pages:	16
Page Range:	pp. 591-606
Identification Number:	10.1111/j.1365-2966.2008.13932.x
Status:	Peer Reviewed
Publication Status:	Published
Access rights to Published version:	Restricted or Subscription Access
Funder:	Particle Physics and Astronomy Research Council (Great Britain) (PPARC), Science and Technology Facilities Council (Great Britain) (STFC), Alfred P. Sloan Foundation, United States. National Aeronautics and Space Administration (NASA), National Science Foundation (U.S.) (NSF), United States. Dept. of Energy, Japan. Monbushō, Max-Planck-Gesellschaft zur Förderung der Wissenschaften [Max Planck Society for the Advancement of Science]
Related URLs:	Other Repository
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URI:	http://wrap.warwick.ac.uk/id/eprint/28967