A Catalog of Spectroscopically Identified White Dwarf Stars in the First Data Release of the Sloan Digital Sky Survey

Kleinman, S. J.; Harris, Hugh C.; Eisenstein, Daniel J.; Liebert, James; Nitta, A.; Krzesiński, Jurek; Munn, Jeffrey A.; Dahn, C. C.; Hawley, Suzanne L.; Pier, Jeffrey R.; Schmidt, Gary D.; Silvestri, Nicole M.; Smith, J. Allyn; Szkody, Paula; Strauss, Michael A.; Knapp, G. R.; Collinge, Matthew J.; Mukadam, Anjum S.; Koester, D.; Uomoto, Alan; Schlegel, David J.; Anderson, Scott F.; Brinkmann, J.; Lamb, D. Q.; Schneider, Donald P.; York, Donald G.

doi:10.1086/383464

Cited by 213 publications

(254 citation statements)

References 62 publications

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“…The UV observations fit well into the WD model with T eff = 30 000 K. For comparison, we show in Fig. 4 the SDSS spectrum of a (single) DAB WD with similar atmospheric parameters (SDSS J084742.22+000647.6, T eff = 30545 ± 241 K, log g = 8.49 ± 0.05; Kleinman et al 2004) along with the average spectrum of the WD in HS 0220+0603 and the DAB model. The SDSS WD and the HS 0220+0603 spectra show a good match.…”

Section: Spectral Energy Distributionmentioning

confidence: 70%

Dynamical masses of a nova-like variable on the edge of the period gap

Rodríguez‐Gil

Shahbaz

Marsh

et al. 2015

Mon. Not. R. Astron. Soc.

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We present the first dynamical determination of the binary parameters of an eclipsing SW Sextantis star in the 3-4 hour orbital period range during a low state. We obtained time-resolved optical spectroscopy and photometry of HS 0220+0603 during its 2004-2005 low brightness state, as revealed in the combined SMARTS, IAC80 and M1 Group long-term optical light curve.The optical spectra taken during primary eclipse reveal a secondary star spectral type of M5.5±0.5 as derived from molecular band-head indices. The spectra also provide the first detection of a DAB white dwarf in a cataclysmic variable. By modelling its optical spectrum we estimate a white dwarf temperature of 30 000 ± 5 000 K.By combining the results of modelling the white dwarf eclipse from ULTRA-CAM light curves with those obtained by simultaneously fitting the emission-and absorption-line radial velocity curves and I-band ellipsoidal light curves, we measure the stellar masses to be M 1 = 0.87 ± 0.09 M and M 2 = 0.47 ± 0.05 M for the white dwarf and the M dwarf, respectively, and an inclination of the orbital plane of i ≈ 79 o . A radius of 0.0103 ± 0.0007 R is obtained for the white dwarf. The secondary star in HS 0220+0603 is likely too cool and undersized for its mass.

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Section: Spectral Energy Distributionmentioning

confidence: 70%

Dynamical masses of a nova-like variable on the edge of the period gap

Rodríguez‐Gil

Shahbaz

Marsh

et al. 2015

Mon. Not. R. Astron. Soc.

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“…‡ LSPM J1107+0409N is a sdM5 dwarf binary companion to the white dwarf WD1104+044 (Kleinman et al 2004;Lépine & Shara 2005). SDSS J124739.04+064604.5 is a DQ peculiar white dwarf (Lépine & Shara 2005;Kilic et al 2010).…”

Section: Search For Wide Binary Companionsmentioning

confidence: 99%

49 new T dwarfs identified using methane imaging

Cardoso¹,

Burningham²,

Smart³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present the discovery of 49 new photometrically classified T dwarfs from the combination of large infrared and optical surveys combined with follow-up TNG photometry. We used multi-band infrared and optical photometry from the UKIRT and Sloan Digital Sky Surveys to identify possible brown dwarf candidates, which were then confirmed using methane filter photometry. We have defined a new photometric conversion between CH 4 s -CH 4 l colour and spectral type for T4 to T8 brown dwarfs based on a part of the sample that has been followed up using methane photometry and spectroscopy. Using methane differential photometry as a proxy for spectral type for T dwarfs has proved to be a very efficient technique. Of a subset of 45 methane selected brown dwarfs that were observed spectroscopically, 100% were confirmed as T dwarfs. Future deep imaging surveys will produce large samples of faint brown dwarf candidates, for which spectroscopy will not be feasible. When broad wavelength coverage is unavailable, methane imaging offers a means to efficiently classify candidates from such surveys using just a pair of near-infrared images.

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“…In addition, because white dwarf progenitors lose their outer layers -which are carbon-, nitrogen-and oxygen-rich -at the top of the asymptotic giant branch (AGB), they are significant contributors to the chemical evolution of the Galaxy. More than 10,000 spectroscopically identified white dwarfs with determined effective temperatures (T eff ) and gravities (log g) have been currently detected (Kleinman et al 2004; Kepler et al 2007), giving us the opportunity to explore the white dwarf mass distribution, which ultimately provides insights into mass-loss processes during stellar evolution and the mass budget of the Galaxy.…”

Section: Introductionmentioning

confidence: 99%

Evolutionary and pulsational properties of white dwarf stars

Althaus

Córsico

Isern

et al. 2010

Astron Astrophys Rev

379

372

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White dwarf stars are the final evolutionary stage of the vast majority of stars, including our Sun. Since the coolest white dwarfs are very old objects, the present population of white dwarfs contains a wealth of information on the evolution of stars from birth to death, and on the star formation rate throughout the history of our Galaxy. Thus, the study of white dwarfs has potential applications to different fields of astrophysics. In particular, white dwarfs can be used as independent reliable cosmic clocks, and can also provide valuable information about the fundamental parameters of a wide variety of stellar populations, like our Galaxy and open and globular clusters. In addition, the high densities and temperatures characterizing white dwarfs allow to use these stars as cosmic laboratories for studying physical processes under extreme conditions that cannot be achieved in terrestrial laboratories. Last but not least, since many white dwarf stars undergo pulsational instabilities, the study of their properties constitutes a powerful tool for applications beyond stellar astrophysics. In particular, white dwarfs can be used to constrain fundamental properties of elementary particles such as axions and neutrinos, and to study problems related to the variation of fundamental constants.These potential applications of white dwarfs have led to a renewed interest in the calculation of very detailed evolutionary and pulsational models for these stars. In this work, we review the essentials of the physics of white dwarf stars. We enumerate the reasons that make these stars excellent chronometers and we describe why white dwarfs provide tools for a wide variety of applications. Special emphasis is placed on the physical processes that lead to the formation of white dwarfs as well as on the different energy sources and processes responsible for chemical abundance changes that occur along their evolution. Moreover, in the course of their lives, white dwarfs cross different pulsational instability strips. The existence of these instability strips provides astronomers with an unique opportunity to peer into their internal structure that would otherwise remain hidden from observers. We will show that this allows to measure with unprecedented precision the stellar masses and to infer their envelope thicknesses, to probe the core chemical stratification, and to detect rotation rates and magnetic fields. Consequently, in this work, we also review the pulsational properties of white dwarfs and the most recent applications of white dwarf asteroseismology.

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A Catalog of Spectroscopically Identified White Dwarf Stars in the First Data Release of the Sloan Digital Sky Survey

Cited by 213 publications

References 62 publications

Dynamical masses of a nova-like variable on the edge of the period gap

Dynamical masses of a nova-like variable on the edge of the period gap

49 new T dwarfs identified using methane imaging

Evolutionary and pulsational properties of white dwarf stars

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