The angular sizes of dwarf stars and subgiants Surface brightness relations calibrated by interferometry

By Pierre Kervella, F. Thévenin, E. D. Folco, Damien Ségransan. 2004

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The availability of a number of new interferometric measurements of Main Sequence and subgiant stars makes it possible to calibrate the surface brightness relations of these stars using exclusively direct angular diameter measurements. These empirical laws make it possible to predict the limb darkened angular diameters $\theta_{\rm LD}$ of dwarfs and subgiants using their dereddened Johnson magnitudes, or their effective temperature. The smallest intrinsic dispersions of $\sigma \le 1\%$ in $\theta_{\rm LD}$ are obtained for the relations based on the K and L magnitudes, for instance $\log \theta_{\rm LD} = 0.0502\,(B-L) + 0.5133 - 0.2\,L$ or $\log \theta_{\rm LD} = 0.0755\,(V-K) + 0.5170 - 0.2\rm \,K$. Our calibrations are valid between the spectral types A0 and M2 for dwarf stars (with a possible extension to later types when using the effective temperature), and between A0 and K0 for subgiants. Such relations are particularly useful for estimating the angular sizes of calibrators for long-baseline interferometry from readily available broadband photometry.

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

View Paper: https://www.semanticscholar.org/paper/5d1992ef0ad5ec25cdec9935cc6a6cf5f50bc36f

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In Astronomy and Astrophysics

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Citations in the corpus

• SearchCal: a Virtual Observatory tool for searching calibrators in optical long-baseline interferometry II. The faint-object case (2006, background): “Such relations exist in the literature (di Benedetto 1998; van Belle 1999; Kervella et al. 2004) but are determined only for a particular luminosity class or only for few a photometric indices.”
• THE ARAUCARIA PROJECT. THE DISTANCE TO THE SMALL MAGELLANIC CLOUD FROM LATE-TYPE ECLIPSING BINARIES (2013, background): “…over those containing early-type stars comes from utilizing well determined empirical surface brightness relation (e.g., the Barnes–Evans relation in the optical) derived for late-type stars from interferometric measurements (e.g., Barnes & Evans 1976; Kervella et al. 2004; di Benedetto 2005).”
• A new implementation of the infrared flux method using the 2MASS catalogue (2009, result): “Ramírez & Meléndez (2005a) compare their results with measured angular diameters from Richichi & Percheron (2002) and Kervella et al. (2004) for giant and dwarf stars, respectively.”
• A Low-Mass Planet with a Possible Sub-Stellar-Mass Host in Microlensing Event MOA-2007-BLG-192 (2008, methodology): “So, we use a cubic fit to the color and radius values of Kervella et al. (2004) to yield θ∗ = 0.50 ± 0.10µas for the angular source radius for the assumed source magnitude of Is = 21.44.”
• Gaia FGK benchmark stars: Effective temperatures and surface gravities (2015, methodology): “The last two are metal-poor dwarf stars with diameter values of less than 0.4 mas, which is well below the lowest value (0.7 mas) measured for the sample of stars that Kervella et al. (2004a) used for calibrating their relations.”
• Stellar and substellar companions of nearby stars from Gaia DR2 (2018, methodology): “The (K,V − K) surface brightness-color relations by Kervella et al. (2004) for the radius, and the isochrones by Girardi et al. (2000) for the masses of stars with MK 6 4.5.”
• A COLD NEPTUNE-MASS PLANET OGLE-2007-BLG-368Lb: Cold neptunes are common (2009, background): “K, K)s,0 and the empirical color/brightness-radius relation by Kervella et al. (2004), we estimate the source angular radius, θ∗ = 0.81 ± 0.07µas, where the error includes uncertainty in the color conversion and the color/brightness-radius relation.”
• MOA-2009-BLG-387Lb: a massive planet orbiting an M dwarf (2011, background): “The color determines the relation between dereddened source flux and angular source radius (Kervella et al. 2004) log 2θ∗ = 0.5170 − 0.2V0 + 0.2755(V − K)0, (3) giving θ∗ = 0.63 ± 0.06 μas.”
• FUNDAMENTAL PROPERTIES OF STARS USING ASTEROSEISMOLOGY FROM KEPLER AND CoRoT AND INTERFEROMETRY FROM THE CHARA ARRAY (2012, methodology): “Expected sizes are calculated using the V −K relation by Kervella et al. (2004) for dwarf and subgiant stars.”
• ELODIE metallicity-biased search for transiting Hot Jupiters. II. A very hot Jupiter transiting the bright K star HD 189733 (2005, methodology): “Kervella et al. (2004) have calibrated a relation between theV − K colour and radii measured from interferometry that shows very little dispersion for low-mass stars (∼1 %).”
• The Effective Temperature Scale of FGK Stars. I. Determination of Temperatures and Angular Diameters with the Infrared Flux Method (2005, neutral): “For Procyon (HD 61421) and HD 121370 more than one value is given by Kervella et al. (2004); only the more accurate VLTI measurement was considered.”
• Microlensing Surveys for Exoplanets (2012, neutral): “F or p er so na l u se o nl y. AA50CH10-Gaudi ARI 16 July 2012 12:29 stars (Kervella et al. 2004).”
• Effective temperature scale and bolometric corrections from 2MASS photometry (2006, background): “…approaches we find the remarkable work by Code et al. (1976), which is based on interferometric measurements of stellar angular semi-diameters (θ) and total fluxes (Fbol) at Earth, and the more recent works of Mozurkewich et al. (2003) and Kervella et al. (2004), also based on interferometry.”
• Accurate fundamental parameters for lower main‐sequence stars (2006, methodology): “…from https://academic.oup.com/mnras/article-abstract/373/1/13/1374497 by guest on 30 July 2018 of θ = 0.227 ± 0.003 mas is in excellent agreement with that of θ = 0.228 ± 0.004 mas (Table 12) obtained by Kervella et al. (2004) using surface brightness relations calibrated by interferometry.”
• VEGA: Visible spEctroGraph and polArimeter for the CHARA array: principle and performance (2009, methodology): “…provide a new quasi-geometrical way to calibrate the Cepheid periodluminosity relation; indeed it is now possible to determine the distance of galactic Cepheids up to 1 kpc using the Interferometric Baade-Wesselink method (Kervella et al. 2004; Sasselov & Karovska 1994; Davis et al. 2009).”
• HD 147506b: A Supermassive Planet in an Eccentric Orbit Transiting a Bright Star (2007, result): “Additionally, it implies an angular diameter for the star (φ = 0.127+0.021−0.014 mas) that is in agreement with the more direct estimate of φ = 0.117 ± 0.001 mas from the near-infrared surface-brightness relation by Kervella et al. (2004).”
• REDDENING AND EXTINCTION TOWARD THE GALACTIC BULGE FROM OGLE-III: THE INNER MILKY WAY'S RV ∼ 2.5 EXTINCTION CURVE (2012, methodology): “A combination of color-color relations (Bessell & Brett 1988) and empiricallycalibrated relations between color and surface brightness (Kervella et al. 2004) can then be used to yield the surface brightness.”
• The colours of the sun (2005, background): “These instruments have produced high-accuracy stellar diameters for about 20 mainsequence stars from ≈1.3 to ≈0.7 M (Kervella et al. 2004).”