ON THE METAL RICHNESS OF M DWARFS WITH PLANETS

By J. Johnson, K. Apps. 2009

146 citations recorded by the source corpus.

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.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/356150e0473afbf97bf0e66db3dfbdb5a91a6b3f

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. D. Charbonneau
2. E. Gaidos
3. Timothy Morton
4. J. Johnson
5. A. Mann
6. Andrew W. Howard
7. G. Marcy
8. Jon Fortney

In Instrumentation

1. D. Charbonneau
2. E. Gaidos
3. Timothy Morton
4. A. Mann
5. J. Johnson
6. Andrew W. Howard
7. G. Marcy
8. S. Lépine

In Statistical and Nonlinear Physics

1. Timothy Morton
2. D. Charbonneau
3. J. Johnson
4. Andrew W. Howard
5. E. Gaidos
6. G. Marcy
7. S. Lépine
8. A. Mann

Citations in the corpus

• THE ULTRAVIOLET RADIATION ENVIRONMENT AROUND M DWARF EXOPLANET HOST STARS (2012, background): “It has a 45 day rotation period, a relatively old age (∼ 6+4 −5 Gyr; Torres 2007), and may have a super-solar metallicity ([Fe/H] = 0.00 – 0.25; Johnson & Apps 2009; Rojas-Ayala et al. 2010).”
• CHARACTERIZING THE COOL KOIs. II. THE M DWARF KOI-254 AND ITS HOT JUPITER (2011, methodology): “This in turn agrees with observations to date that suggest that the formation of a Jupiter-mass planet around a low-mass star requires high metallicity (Johnson & Apps 2009; Schlaufman & Laughlin 2010; Rojas-Ayala et al. 2010).”
• 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): “The major difference between our fit and that of Johnson et al. (2012) is that they fix the constant term to -0.05 in order to keep [Fe/H] = -0.05 at ∆(J −K) = 0, consistent with a volume limited sample of stars from Johnson & Apps (2009), whereas we make no such restrictions.”
• NEAR-INFRARED METALLICITIES, RADIAL VELOCITIES, AND SPECTRAL TYPES FOR 447 NEARBY M DWARFS (2013, methodology): “Johnson & Apps (2009), finding the calibration of Bonfils et al. (2005) to systematically underestimate the metallicities of metal-rich stars, update the relation by considering the offset from the mean main se- quence (MS), assuming the mean MS defined an isometallicity contour with[Fe/H] = −0.05…”
• METALLICITY AND TEMPERATURE INDICATORS IN M DWARF K-BAND SPECTRA: TESTING NEW AND UPDATED CALIBRATIONS WITH OBSERVATIONS OF 133 SOLAR NEIGHBORHOOD M DWARFS (2011, methodology): “K band [Fe/H] Estimates Compared with Other [Fe/H] Techniques Supersolar metallicities for most of the M dwarf planet hosts are predicted by the K band [Fe/H] fit as well as the photometric calibrations by Johnson & Apps (2009) and Schlaufman & Laughlin (2010).”
• THE CALIFORNIA PLANET SURVEY. I. FOUR NEW GIANT EXOPLANETS (2010, methodology): “Johnson & Apps (2009) estimate [Fe/H] = +0.3 and +0.37 for Gl 179 and Gl 876, respectively.”
• PARTICLE CLUMPING AND PLANETESIMAL FORMATION DEPEND STRONGLY ON METALLICITY (2009, background): “Thus planetesimal formation may help explain the high probability of finding giant exoplanets around stars rich in heavy elements (Gonzalez 1997; Santos et al. 2001; Fischer & Valenti 2005; Johnson & Apps 2009).”
• AN ALL-SKY CATALOG OF BRIGHT M DWARFS (2011, background): “…and the presence of giant planets found among solar-mass stars (Gonzalez 1997; Fischer, & Valenti 2005) has been recently extended to M dwarf stars (Johnson & Apps 2009; Johnson et al. 2010a), and metal-rich M dwarfs, if they can be identified (Bonfils et al. 2005; Schlaufman & Laughlin 2010;…”
• Trumpeting M dwarfs with CONCH-SHELL: a catalogue of nearby cool host-stars for habitable exoplanets and life (2014, background): “This is consistent with previous estimates of volume-limited M dwarf samples (Johnson & Apps 2009; Schlaufman & Laughlin 2010), and very similar to the distribution of FGK stars in the solar neighborhood (median metallicity = -0.06, standard deviation = 0.21 dex, Casagrande et al. 2011).”
• SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs - I. New atmospheric parameters and masses for 48 stars with planets (2013, background): “…2005; Bean et al. 2006; Önehag et al. 2012), most determinations of their values are based on calibrations using colors (Bonfilset al. 2005a; Johnson & Apps 2009; Casagrande et al. 2008; Schlaufman & Laughlin 2010; Neves et al. 2012) or spectroscopic indices (e.g. Terrien et al. 2012;…”
• THE LICK–CARNEGIE EXOPLANET SURVEY: A 3.1 M⊕ PLANET IN THE HABITABLE ZONE OF THE NEARBY M3V STAR GLIESE 581 (2010, background): “Johnson & Apps (2009) presented a broadband (V-K) photometric metallicity calibration for M dwarfs that, in conjunction with the star’s broadband magnitudes implies a metallicity of [Fe/H] = -0.049.”
• The Habitability of Planets Orbiting M-dwarf Stars (2016, background): “…the empirical color-magnitude relationship among the M dwarfs that successfully traced the metallicities of the more massive companions, although subsequent studies refined this relationship and placed it on an absolute scale (Johnson & Apps, 2009; Schlaufman & Laughlin, 2010; Neves et al., 2014).”
• CHARACTERIZING THE COOL KOIs. III. KOI 961: A SMALL STAR WITH LARGE PROPER MOTION AND THREE SMALL PLANETS (2012, methodology): “Recently developed methods for estimating the metallicities of M dwarfs have shown that M-dwarf planet-hosts are also systematically metalrich (Johnson & Apps 2009; Rojas-Ayala et al. 2010; Schlaufman & Laughlin 2010; Neves et al. 2011).”
• THE LICK-CARNEGIE EXOPLANET SURVEY: A URANUS-MASS FOURTH PLANET FOR GJ 876 IN AN EXTRASOLAR LAPLACE CONFIGURATION (2010, background): “The Johnson & Apps (2009) calibration indicates that the planetbearing M dwarfs do appear to be systematically metal-rich, suggesting that there is no breakdown of the planet-metallicity correlation as one progresses into the red dwarf regime.”
• AN EFFICIENT AUTOMATED VALIDATION PROCEDURE FOR EXOPLANET TRANSIT CANDIDATES (2012, methodology): “…and we constrain our representative populations of HEB and EB scenarios to conform to the observed total g − r and J −K colors, to within 0.1 mag (I choose these two colors in particular, and not g − K, for example, to avoid being too sensitive to metallicity effects (Johnson & Apps 2009)).”
• New constraints on the chemical evolution of the solar neighbourhood and galactic disc(s) - improved astrophysical parameters for the Geneva-Copenhagen Survey (2011, background): “In all cases stars withMVT < 2 are excluded, their effect being responsible for the bump (green dotted line) around 1 Gyr. around solar metallicity if the recent spectroscopic findings of Johnson & Apps (2009) are confirmed and photometric determinations for those stars are recalibrated accordingly.”