Empirically Constrained Color-Temperature Relations. I. BV(RI)C

By D. VandenBerg, J. Clem. 2003

164 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/19400aec92c25d466ae7f51bfbb512b5038a4552

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Citations in the corpus

Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs (2005, methodology): “We obtained a bolometric correction, V , for each star by interpolating in the ‘‘high-temperature’’ grid of VandenBerg & Clem (2003), using our spectroscopically determined TeA, log g, and [M/H] from Table 8.”
The ACS Survey of Galactic Globular Clusters. I. Overview and Clusters without Previous Hubble Space Telescope Photometry (2006, methodology): “The semiempirical transformation uses the B, V, and I magnitudes from VandenBerg & Clem (2003) and the relevant equations to convert from Vand I to F606Wand F814W in Appendix D of Sirianni et al. (2005).”
New companions to nearby low-mass stars (2013, methodology): “Companion masses can be determined from the magnitude difference between primary and secondary in the SDSS i band ( I) using isochrones from evolutionary models (Chabrier et al. 2000; Vandenberg & Clem 2003; Marigo et al. 2008).”
Accurate fundamental parameters for 23 bright solar-type stars (2010, methodology): “Both VandenBerg & Clem (2003) and Girardi et al. (2002) include the changes in BC withlog g and [Fe/H].”
An absolutely calibrated T eff scale from the infrared flux method. Dwarfs and subgiants (2010, background): “Effective temperature calibrations are also crucial in the context of deriving reliable colours for theor tical stellar models, which apart from few notable exceptions(e.g. VandenBerg & Clem 2003) have to resort entirely to theoretical flux libraries.”
The ACS Survey of Galactic Globular Clusters. II. Stellar Evolution Tracks, Isochrones, Luminosity Functions, and Synthetic Horizontal-Branch Models (2007, methodology): “One is based on the semi-empirical colors and bolometric corrections of Vandenberg & Clem (2003) and the transformation equations found in Appendix D of Sirianni et al. (2005), specifically those in Tables 22 and 24, hereafter referred to as the Empirical transformation.”
STELLAR DIAMETERS AND TEMPERATURES. II. MAIN-SEQUENCE K- AND M-STARS (2012, methodology): “The (B − V)–radius plot also shows the Dartmouth isochrones under the same conditions, but with the semi-empirical BV (RI )C color-transformations (VandenBerg & Clem 2003, blue lines).”
AN EMPIRICAL UBV RI JHK COLOR–TEMPERATURE CALIBRATION FOR STARS (2006, methodology): “We check our results for cool stars against VandenBerg & Clem (2003), Lejeune et al. (1998), an update of the Green (1988) color table used in the Yonsei–Yale isochrones (Yi et al. 2001), and, for good measure, the synthetic colors of Worthey (1994) in Figure 11.”
The Milky Way Tomography with SDSS. II. Stellar Metallicity (2008, methodology): “17 from VandenBerg & Clem (2003): for B−V =(1.2, 1.3, 1.4), corresponding to g−i=(1.51, 1.70, 1.93), we adopt MV =(7.5, 8.0, 8.5).”
The Adequacy of Stellar Evolution Models for the Interpretation of the Color-Magnitude Diagrams of Resolved Stellar Populations (2005, background): “Example of such transformations are given in Lejeune, Cuisinier & Buser (1998) and VandenBerg & Clem (2003).”
SPECTRAL PROPERTIES OF COOL STARS: EXTENDED ABUNDANCE ANALYSIS OF 1,617 PLANET-SEARCH STARS (2016, methodology): “Using those parameters, the bolometric correction of VandenBerg & Clem (2003) and our values of Teff and log g we calculated the 23 luminosity, radius, mass and their uncertainties in Columns (35)-(37).”
A Transiting Planet of a Sun-like Star (2006, methodology): “We used our spectroscopic effective temperature, spectroscopic gravity, and an assumed distance to derive a bolometric correction by interpolating the “high temperature” table from VandenBerg & Clem (2003).”
ROTATIONAL AND RADIAL VELOCITIES FOR A SAMPLE OF 761 HIPPARCOS GIANTS AND THE ROLE OF BINARITY (2007, methodology): “Next, we took advantage of the fact that all our stars had parallaxes measured by Hipparcos to derive bolometric luminosities, L/L , from the absolute V magnitudes using the bolometric corrections from VandenBerg & Clem (2003).”
An Assessment of Dynamical Mass Constraints on Pre-Main-Sequence Evolutionary Tracks (2003, background): “A hint provided in VandenBerg & Clem (2003) suggests that more may be coming from this group on pre–main-sequence evolution, including realistic atmospheres, with the most recent description of main-sequence and post–main-sequence evolution appearing in VandenBerg et al. (2000).”
First stars VII - Lithium in extremely metal poor dwarfs (2006, methodology): “For B−V we determined Teff using both the Alonso et al. (1996) calibration and the theoretical colours of VandenBerg & Clem (2003).”
PROSPECTING IN LATE-TYPE DWARFS: A CALIBRATION OF INFRARED AND VISIBLE SPECTROSCOPIC METALLICITIES OF LATE K AND M DWARFS SPANNING 1.5 dex (2012, methodology): “Bolometric corrections are obtained by interpolating in the high temperature grid of VandenBerg & Clem (2003), and B, V magnitudes were drawn from Hipparcos (van Leeuwen & Fantino 2005).”
Ground-based CCD astrometry with wide-field imagers - II. A star catalog for M 67: WFI@2.2 m MPG/ESO astrometry, FLAMES@VLT radial velocities (2008, methodology): “This deficiency is corrected for VictoriaRegina isochrones by applying semi-empirical color transformations (VandenBerg & Clem 2003).”