Calibration of Synthetic Photometry Using DA White Dwarfs

By J. Holberg, Pierre Bergeron. 2005

381 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/8751cbf810d6a25afb6295c28e66c4acb56d91a2

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Citations in the corpus

SEGUE: A SPECTROSCOPIC SURVEY OF 240,000 STARS WITH g = 14–20 (2009, background): “WDs are important for absolute calibration of the astrophysical temperature and flux scales, including calibration of filter systems that span ultraviolet (UV), optical and IR wavelengths (Holberg & Bergeron 2006; Bohlin 2007).”
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).”
Fundamental properties of core-collapse Supernova and GRB progenitors: predicting the look of massive stars before death (2013, methodology): “We performed synthetic photometry of our SN progenitor models using the Chorizos code (Maíz-Apellániz 2004), adopting its built-in passband and zero point definitions that were obtained from Cohen et al. (2003); Maíz Apellániz (2006); Holberg & Bergeron (2006); Maíz-Apellániz (2007).”
Three Hypervelocity White Dwarfs in Gaia DR2: Evidence for Dynamically Driven Double-degenerate Double-detonation Type Ia Supernovae (2018, methodology): “Using publicly available DB WD cooling tables1 (Holberg & Bergeron 2006; Kowalski & Saumon 2006; Tremblay et al. 2011; Bergeron et al. 2011), we find that a 0.6 (1.0)M WD that has cooled for 1 Gyr since its birth has an absolute visual magnitude of 12.9 (12.8).”
The Structure of the Local Interstellar Medium. V. Electron Densities (2007, positive): “The 74 Psc stars are inactive and relatively cool A stars, while GD659 is the coolest (∼35000 K) of the singleton white dwarfs in our sample, which are all &50000 K (Lajoie & Bergeron 2007; Holberg & Bergeron 2006).”
The Sirius System and Its Astrophysical Puzzles: Hubble Space Telescope and Ground-based Astrometry (2017, methodology): “These tables are based on evolutionary sequences and model atmospheres calculated by Holberg & Bergeron (2006), Kowalski & Saumon (2006), Tremblay et al. (2011), and Bergeron et al. (2011). measure 89.60± 0.75 km s−1.”
THE EVOLUTION OF CATACLYSMIC VARIABLES AS REVEALED BY THEIR DONOR STARS (2011, methodology): “…to system just before or after a nova outburst.27 Given M1 and Teff,1, we then estimate R1 and all photometric properties by interpolating on the Holberg & Bergeron (2006) grid of WD models.28 The predicted properties of the accreting WD are listed as a function of Porb in Tables 7 and 8.”
A COMPREHENSIVE SPECTROSCOPIC ANALYSIS OF DB WHITE DWARFS (2011, methodology): “The absolute visual magnitude (MV ) and luminosity (L) are determined with the improved calibration from Holberg & Bergeron (2006), defined with the Hubble Space Telescope absolute flux scale of Vega.”
Techniques and Review of Absolute Flux Calibration from the Ultraviolet to the Mid-Infrared (2014, background): “A set of WD models for the primary standards provides complete wavelength coverage for a system of absolute fluxes and for the zero points of the various standard magnitude systems; see for example Holberg & Bergeron (2006) and Pickles (2010).”
A SPECTROSCOPIC SURVEY AND ANALYSIS OF BRIGHT, HYDROGEN-RICH WHITE DWARFS (2011, methodology): “In addition, we list absolute visual magnitudes determined using the photometric calibrations from Holberg & Bergeron (2006).”
AN IMPROVED SPECTROSCOPIC ANALYSIS OF DA WHITE DWARFS FROM THE SLOAN DIGITAL SKY SURVEY DATA RELEASE 4 (2011, methodology): “The absolute visual magnitude MV obtained from spectroscopic measurements of Teff and log g is also given for each object following the calibration of Holberg & Bergeron (2006).”
FUNDAMENTAL PARAMETERS AND SPECTRAL ENERGY DISTRIBUTIONS OF YOUNG AND FIELD AGE OBJECTS WITH MASSES SPANNING THE STELLAR TO PLANETARY REGIME (2015, methodology): “The SDSS magnitude system (Fukugita et al. 1996) is not quite in the AB magnitude system (Oke & Gunn 1983) so we converted first to AB using the corrections of Holberg & Bergeron (2006) and then to the Vega system using the corrections of Blanton & Roweis (2007).”
SPECTROSCOPIC ANALYSIS OF DA WHITE DWARFS: STARK BROADENING OF HYDROGEN LINES INCLUDING NONIDEAL EFFECTS (2009, methodology): “We then use the calibration of Holberg & Bergeron (2006) to obtain MV (spec) from spectroscopic measurements of Teff and log g.”
Sloan Digital Sky Survey Standard Star Catalog for Stripe 82: The Dawn of Industrial 1% Optical Photometry (2007, methodology): “Similar values of mr, also based on hot white dwarfs, were obtained by Holberg & Bergeron (2006): 0.046, +0.001, +0.013, and +0.024 mag for m ¼ ugiz, respectively.”
The Milky Way Tomography with SDSS. II. Stellar Metallicity (2008, methodology): “For example, the SDSS u-band measurements are offset from the AB system by ∼0.04 mag (Eisenstein et al. 2006; Holberg & Bergeron 2006), leading to a metallicity bias of up to 0.2 dex.”
KNOW YOUR NEIGHBORHOOD: A DETAILED MODEL ATMOSPHERE ANALYSIS OF NEARBY WHITE DWARFS (2012, methodology): “Note that the Strömgren u magnitude in Table 1 of Holberg & Bergeron (2006) is erroneous and should read 1.437 instead of 1.357 (Hauck & Mermilliod 1998), which yields a corrected zero point of cu = −19.80809 (instead of −19.8882).”
Prospects for detection of detached double white dwarf binaries with Gaia, LSST and LISA (2017, methodology): “The absolute magnitudes for WDs are deduced from the WD cooling curves of pure hydrogen atmosphere models (Holberg & Bergeron 2006; Kowalski & Saumon 2006; Tremblay, Bergeron & Gianninas 2011, and references therein1).”