SDSS Dr7 White Dwarf Catalog

Kleinman, S. J.; Kepler, S. O.; Koester, D.; Pelisoli, Ingrid; Peçanha, Viviane; Nitta, A.; Costa, J. E. S.; Krzesiński, Jurek; Dufour, Patrick; Lachapelle, F. R.; Bergeron, P.; Yip, C. W.; Harris, Hugh C.; Eisenstein, Daniel J.; Althaus, Leandro Gabriel; Córsico, Alejandro H.

doi:10.1088/0067-0049/204/1/5

Cited by 405 publications

(514 citation statements)

References 86 publications

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“…Hügelmeyer et al (2006) already noted that the mean value of their sample of 20 DOs from the SDSS DR4 was somewhat larger (0.69 M ), although some of the difference could be due to the calibration problem reported in Kleinman et al (2009Kleinman et al ( , 2013 Reindl et al 2014). In conclusion, there is no significant difference in the mean masses of the three considered H-deficient spectral classes.…”

Section: Discussionmentioning

confidence: 98%

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New hydrogen-deficient (pre-) white dwarfs in the Sloan Digital Sky Survey Data Release 10

Werner¹,

Rauch²,

Kepler

2014

A&A

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We have detected 21 new, very hot hydrogen-deficient (pre-) white dwarfs (spectral types O(He), hot DO, PG1159) in the Data Release 10 of the Sloan Digital Sky Survey. We present the results of non-local thermodynamic equilibrium (non-LTE) model-atmosphere analyses. The seven PG1159 stars have effective temperatures and surface gravities in the ranges T eff = 100 000-140 000 K and log g = 6-7.5. The hottest one is a new member of the rare hybrid-PG1159 subtype, indicating the presence of residual hydrogen. The ten new hot DOs span T eff = 65 000-120 000 K and log g = 7.5-8. Carbon abundances were derived and it is found that the PG1159 star values (C/He = 0.33-0.03 by number) and the DO values (<0.0004-0.01) cover distinct but adjacent ranges. With the discovery of four new O(He) stars (T eff = 80 000-100 000 K, log g = 5-5.5, C/He = 0.002-0.01), we double the number of known members of this rare spectral class. One of them is particularly interesting because it is unusually rich in C, N, O, and Si. Unexpected problems arose with the DOs because many He ii lines of every other star are so deep that they cannot be matched by any model. This is most conspicuous in the case of one object which exhibits the occurrence of ultrahigh-ionization metal features, a hitherto unexplained phenomenon that is known from a disquieting large fraction of hot DOs.

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Section: Discussionmentioning

confidence: 98%

“…Here we present a similar study for the DR 10. Kleinman et al (2013) already announced the identification of a number of new DOs and PG 1159s in DR 7. In addition, we have now searched DR 10 for such hitherto unidentified stars.…”

Section: Introductionmentioning

confidence: 99%

New hydrogen-deficient (pre-) white dwarfs in the Sloan Digital Sky Survey Data Release 10

Werner¹,

Rauch²,

Kepler

2014

A&A

Self Cite

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“…Despite the all sky capacity of WISE, there is not yet a commensurate catalog of white dwarfs (pending GAIA results). Thus the WIRED team opted to cross-correlate the infrared database with each of the two largest available white dwarf catalogs: a preliminary version of the SDSS DR7 (spectroscopic) white dwarf catalog (Kleinman et al, 2013), and the older but historically invaluable catalog of McCook & Sion (1999).…”

Section: Independent Studies and Infrared Statisticsmentioning

confidence: 99%

Circumstellar debris and pollution at white dwarf stars

Farihi

2016

New Astronomy Reviews

300

265

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Circumstellar disks of planetary debris are now known or suspected to closely orbit hundreds of white dwarf stars. To date, both data and theory support disks that are entirely contained within the preceding giant stellar radii, and hence must have been produced during the white dwarf phase. This picture is strengthened by the signature of material falling onto the pristine stellar surfaces; disks are always detected together with atmospheric heavy elements. The physical link between this debris and the white dwarf host abundances enables unique insight into the bulk chemistry of extrasolar planetary systems via their remnants. This review summarizes the body of evidence supporting dynamically active planetary systems at a large fraction of all white dwarfs, the remnants of first generation, main-sequence planetary systems, and hence provide insight into initial conditions as well as long-term dynamics and evolution.

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“…10 shows the distribution of gravitational settling timescales for calcium in the sample, taken from Table 5 and 6 of Koester (2009), based on the stellar effective temperature and atmospheric composition. The stellar type classification are taken from Kleinman et al (2013) for the Debes et al (2011a) sample.…”

Section: A: Dust Disc Fully Accreted (Green Region)mentioning

confidence: 99%

Infrared observations of white dwarfs and the implications for the accretion of dusty planetary material

Bonsor

Farihi

Wyatt

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Infrared excesses around metal polluted white dwarfs have been associated with the accretion of dusty, planetary material. This work analyses the available infrared data for an unbiased sample of white dwarfs and demonstrates that no more than 3.3% can have a wide, flat, opaque dust disc, extending to the Roche radius, with a temperature at the disc inner edge of T in = 1, 400K, the standard model for the observed excesses. This is in stark contrast to the incidence of pollution of about 30%. We present four potential reasons for the absence of an infrared excess in polluted white dwarfs, depending on their stellar properties and inferred accretion rates: i) their dust discs are opaque, but narrow, thus evading detection if more than 85% of polluted white dwarfs have dust discs narrower than δr < 0.04r, ii) their dust discs have been fully consumed, which only works for the oldest white dwarfs with sinking timescales longer than hundreds of years, iii) their dust is optically thin, which can supply low accretion rates of < 10 7 gs −1 if dominated by PR-drag, and higher accretion rates, if inwards transport of material is enhanced, for example due to the presence of gas, iv) their accretion is supplied by a pure gas disc, which could result from the sublimation of optically thin dust for T * > 20, 000K. Future observations sensitive to faint infrared excesses or the presence of gas, can test the scenarios presented here, thereby better constraining the nature of the material fuelling accretion in polluted white dwarfs.

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SDSS Dr7 White Dwarf Catalog

Cited by 405 publications

References 86 publications

New hydrogen-deficient (pre-) white dwarfs in the Sloan Digital Sky Survey Data Release 10

New hydrogen-deficient (pre-) white dwarfs in the Sloan Digital Sky Survey Data Release 10

Circumstellar debris and pollution at white dwarf stars

Infrared observations of white dwarfs and the implications for the accretion of dusty planetary material

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