On the Metal Richness of M Dwarfs with Planets
- Creators
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Johnson, John Asher
- Apps, Kevin
Abstract
Knowledge of the metallicities of M dwarfs rests predominantly on the photometric calibration of Bonfils and collaborators, which predicts that M dwarfs in the solar neighborhood, including those with known planets, are systematically metal poor compared to their higher-mass counterparts. We test this prediction using a volume-limited sample of low-mass stars, together with a subset of M dwarfs with high-metallicity, F, G, and K wide binary companions. We find that the Bonfils et al. photometric calibration systematically underestimates the metallicities of our high-metallicity M dwarfs by an average of 0.32 dex. We derive a new photometric metallicity calibration and show that M dwarfs with planets appear to be systematically metal rich, a result that is consistent with the metallicity distribution of FGK dwarfs with planets.
Additional Information
© 2009 American Astronomical Society. Received 2009 February 12; accepted 2009 April 21; published 2009 June 17. We gratefully acknowledge Geoff Marcy, Jon Swift, Mike Liu, Mike Cushing, Andrew West, Debra Fischer and Jeff Valenti for their helpful conversations and feedback. We also thank the anonymous referee for their helpful feedback. J.A.J. is an NSF Astronomy and Astrophysics Postdoctoral Fellow with support from the NSF grant AST-0702821. This publication makes use of data from the Two Micron All Sky Survey (2MASS), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center; the SIMBAD database operated at CDS, Strasbourge, France; and NASA's Astrophysics Data System Bibliographic Services.Attached Files
Published - 0004-637X_699_2_933.pdf
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Additional details
- Eprint ID
- 36191
- Resolver ID
- CaltechAUTHORS:20130107-085104917
- AST-0702821
- NSF
- Created
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2013-01-07Created from EPrint's datestamp field
- Updated
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2021-11-09Created from EPrint's last_modified field