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Stellar Diameters and Temperatures. III. Main-sequence A, F, G, and K Stars: Additional High-precision Measurements and Empirical Relations

Boyajian, Tabetha S. and von Braun, Kaspar and van Belle, Gerard and Farrington, Chris and Schaefer, Gail and Jones, Jeremy and White, Russel and McAlister, Harold A. and ten Brummelaar, Theo A. and Ridgway, Stephen and Gies, Douglas and Sturmann, Laszlo and Sturmann, Judit and Turner, Nils H. and Goldfinger, P. J. and Vargas, Norm (2013) Stellar Diameters and Temperatures. III. Main-sequence A, F, G, and K Stars: Additional High-precision Measurements and Empirical Relations. Astrophysical Journal, 771 (1). Art. No. 40. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20130816-160949360

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Abstract

Based on CHARA Array measurements, we present the angular diameters of 23 nearby, main-sequence stars, ranging from spectral types A7 to K0, 5 of which are exoplanet host stars. We derive linear radii, effective temperatures, and absolute luminosities of the stars using Hipparcos parallaxes and measured bolometric fluxes. The new data are combined with previously published values to create an Angular Diameter Anthology of measured angular diameters to main-sequence stars (luminosity classes V and IV). This compilation consists of 125 stars with diameter uncertainties of less than 5%, ranging in spectral types from A to M. The large quantity of empirical data is used to derive color-temperature relations to an assortment of color indices in the Johnson (BVR_(J)I_(J)JHK), Cousins (R_(C)I_(C)), Kron (R_(K)I_(K)), Sloan (griz), and WISE (W_(3)W_(4)) photometric systems. These relations have an average standard deviation of ~3% and are valid for stars with spectral types A0-M4. To derive even more accurate relations for Sun-like stars, we also determined these temperature relations omitting early-type stars (T_eff > 6750 K) that may have biased luminosity estimates because of rapid rotation; for this subset the dispersion is only ~2.5%. We find effective temperatures in agreement within a couple of percent for the interferometrically characterized sample of main-sequence stars compared to those derived via the infrared flux method and spectroscopic analysis.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/771/1/40DOIArticle
http://iopscience.iop.org/0004-637X/771/1/40PublisherArticle
http://arxiv.org/abs/1306.2974arXivDiscussion Paper
http://dx.doi.org/10.1088/0004-637X/787/1/92ErrataErratum
ORCID:
AuthorORCID
Boyajian, Tabetha S.0000-0001-9879-9313
von Braun, Kaspar0000-0002-5823-4630
van Belle, Gerard0000-0002-8552-158X
Farrington, Chris0000-0001-9939-2830
White, Russel0000-0001-5313-7498
ten Brummelaar, Theo A.0000-0002-0114-7915
Additional Information:© 2013 American Astronomical Society. Received 2013 February 14; accepted 2013 May 10; published 2013 June 13. T.S.B. acknowledges support provided through NASA grant ADAP12-0172. S.T.R. acknowledges partial support from NASA grant NNH09AK731. We thank the referee for many helpful comments to improve the paper.We thank Mike Bessell for his helpful advice on photometric transformations.We thank Mike Ireland, Tim White, Vincente Maestro, and Daniel Huber for enlightening discussions on precision bolometric flux measurements. The CHARA Array is funded by the National Science Foundation through NSF grants AST-0908253 and AST 1211129, and by Georgia State University through the College of Arts and Sciences. This research has made use of the SIMBAD literature database, operated at CDS, Strasbourg, France, and of NASA’s Astrophysics Data System. This research has made use of the VizieR catalog access tool, CDS, Strasbourg, France. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This publicationmakes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. This research has made use of the JSDC Jean-Marie Mariotti Center database, available at http://www.jmmc.fr/jsdc.
Funders:
Funding AgencyGrant Number
NASAADAP12-0172
NASANNH09AK731
NSFAST-0908253
NSFAST 1211129
Georgia State UniversityUNSPECIFIED
NASAUNSPECIFIED
NSFUNSPECIFIED
Subject Keywords:Hertzsprung-Russell and C-M diagrams; infrared: stars; planetary systems; stars: atmospheres; stars: fundamental parameters; stars: general; stars: solar-type; techniques: high angular resolution; techniques: interferometric
Issue or Number:1
Record Number:CaltechAUTHORS:20130816-160949360
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20130816-160949360
Official Citation:Stellar Diameters and Temperatures. III. Main-sequence A, F, G, and K Stars: Additional High-precision Measurements and Empirical Relations Tabetha S. Boyajian et al. 2013 ApJ 771 40
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:40715
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:19 Aug 2013 14:42
Last Modified:09 Mar 2020 13:19

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