A Catalog of Spectroscopically Confirmed White Dwarfs from the Sloan Digital Sky Survey Data Release 4

By D. Eisenstein, J. Liebert, H. Harris, S. Kleinman, A. Nitta, N. Silvestri, S. Anderson, John C. Barentine, H. Brewington, J. Brinkmann and 6 more. 2006

333 citations recorded by the source corpus.

We present a catalog of 9316 spectroscopically confirmed white dwarfs from the Sloan Digital Sky Survey Data Release 4. We have selected the stars through photometric cuts and spectroscopic modeling, backed up by a set of visual inspections. About 6000 of the stars are new discoveries, roughly doubling the number of spectroscopically confirmed white dwarfs. We analyze the stars by performing temperature and surface gravity fits to grids of pure hydrogen and helium atmospheres. Among the rare outliers are a set of presumed helium-core DA white dwarfs with estimated masses below 0.3 M☉, including two candidates that may be the lowest-mass yet found. We also present a list of 928 hot subdwarfs.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/905d5f61de56da8b5526d662aef4bb0f7a1528a9

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Citations in the corpus

On the Spectral Evolution of Cool, Helium-Atmosphere White Dwarfs: Detailed Spectroscopic and Photometric Analysis of DZ Stars (2007, methodology): “The absence of cool stars can also be explained by the fact that most of our stars come from the DR4 catalog of Eisenstein et al. (2006).”
Spectroscopic analysis of DA white dwarfs with 3D model atmospheres (2013, methodology): “In addition to possible issues with the data calibration, the samples have significantly different selection criteria and completeness levels (Eisenstein et al. 2006; GB11).”
THE BARYON OSCILLATION SPECTROSCOPIC SURVEY OF SDSS-III (2012, background): “Special target classes in SDSS 43 produced the largest spectroscopic samples of white dwarfs (Kleinman et al. 2004; Eisenstein et al. 2006).”
Stellar SEDs from 0.3 to 2.5 μm: Tracing the Stellar Locus and Searching for Color Outliers in the SDSS and 2MASS (2007, methodology): “Note, however, that the AB offsets assumed here differ slightly from those adopted by Eisenstein et al. (2006) TABLE 1 Analytic Fits to the Stellar Locus Max.”
FIRST RESULTS FROM THE CATALINA REAL-TIME TRANSIENT SURVEY (2008, background): “The (u − g) colours are consistent with those expected for white dwarfs (Eisenstein et al. 2006) and CVs discovered in SDSS data (Szkody et al. 2007).”
New white dwarf and subdwarf stars in the Sloan Digital Sky Survey Data Release 12 (2015, methodology): “As an independent check, and to be consistent with the earlier SDSS white catalogues, we also fitted all DA and DB white dwarf spectra and colours with the AUTOFIT code described in Kleinman et al. (2004), Eisenstein et al. (2006) and Kleinman et al. (2013).”
Evolutionary and pulsational properties of white dwarf stars (2010, background): “The transition from DO to the cooler DB stage is interrupted by the non-DA gap(that occurs at 30 000 K < Teff < 45000 K) where few objects with H-deficient atmospheres havebeen observed (Eisenstein et al. 2006).”
Sloan Digital Sky Survey Standard Star Catalog for Stripe 82: The Dawn of Industrial 1% Optical Photometry (2007, methodology): “Fitting the SDSS spectra of hot white dwarfs to models, Eisenstein et al. (2006) determined theAB color corrections mr to be 0.040, +0.000, +0.015, and +0.030 mag for m ¼ ugiz, respectively, with an uncertainty of 0.01Y0.”
New white dwarf stars in the Sloan Digital Sky Survey Data Release 10 (2014, methodology): “However, much of SDSS white dwarf targeting required that the objects be unblended, which caused many brighter white dwarfs to be skipped (for a detailed discussion, see Section 5.6 of Eisenstein et al. 2006).”
White dwarf mass distribution in the SDSS (2006, methodology): “We excluded all stars classified by Eisenstein et al. (2006) as having either a detectable magnetic field or a companion, metal lines, DABs, and DBAs.”
ANCIENT PLANETARY SYSTEMS ARE ORBITING A LARGE FRACTION OF WHITE DWARF STARS (2010, background): “…cooler than 10,000 K. Investigations of substantial samples of cool He white dwarfs in classes DC, DQ and DZ have been carried out by Bergeron et al. (2001), Tremblay & Bergeron (2008), Eisenstein et al. (2006), and Dufour et al. (2007), where the latter two studies relied on the SDSS data base.”
Kinematics of SDSS subdwarfs: structure and substructure of the Milky Way halo (2009, background): “Although the Eisenstein et al. (2006) catalogue contains only DR4 data, we know that ∼ 60 per cent of our subdwarf spectra were included in DR4 and so, assuming the fraction of white dwarfs does not vary with SDSS data releases, we can expect .”
SPECTROSCOPIC ANALYSIS OF DA WHITE DWARFS: STARK BROADENING OF HYDROGEN LINES INCLUDING NONIDEAL EFFECTS (2009, unknown): “…technique coupled with high signal-to-noise spectroscopic observations of the Balmer lines for large samples of DA stars (Gianninas et al. 2005; Eisenstein et al. 2006) can reveal important details about the luminosity function and the evolution and the formation rate of DA white dwarfs…”
On the Spectral Evolution of Hot White Dwarf Stars. I. A Detailed Model Atmosphere Analysis of Hot White Dwarfs from SDSS DR12 (2020, methodology): “On the basis of a model atmosphere analysis of the Data Release (DR) 4 sample, Eisenstein et al. (2006b) reported the striking discovery of a small number of helium-rich objects in the DB gap, indicating that not all DO stars inevitably evolved into DA stars.”
Synthetic stellar photometry – I. General considerations and new transformations for broad-band systems (2014, background): “2.10 Sloan Digital Sky Survey ugriz SDSS photometry is defined to be on the AB system, although small post-facto zero-point corrections are necessary (Eisenstein et al. 2006; Holberg & Bergeron 2006).”
A SPECTROSCOPIC SURVEY AND ANALYSIS OF BRIGHT, HYDROGEN-RICH WHITE DWARFS (2011, result): “This is higher than the value of 0.613 M⊙ obtained by Tremblay et al. (2011a) for the SDSS DR4 sample.”
The Milky Way Tomography with SDSS. I. Stellar Number Density Distribution (2005, background): “…as they pointed out, their study was not based on SDSS data, and thus, even small differences between different photometric systems may have a significant effect on derived metallicities (especially since the SDSS u-band photometry is not precisely on the AB system; see Eisenstein et al. 2006).”
AN IMPROVED SPECTROSCOPIC ANALYSIS OF DA WHITE DWARFS FROM THE SLOAN DIGITAL SKY SURVEY DATA RELEASE 4 (2011, methodology): “In Figure 16, we compare our atmospheric parameters with those obtained by Eisenstein et al. (2006).”
The chemical diversity of exo-terrestrial planetary debris around white dwarfs (2012, methodology): “Eisenstein et al. (2006) identified this DA white dwarf in Data Release 4 of the Sloan Digital Sky Survey, and found Teff = 22 125 ± 136K, log g = 8.22 ± 0.02 from a fit to the SDSS spectrum.”