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29 March 2024
 
  » arxiv » 1612.1598

 Article overview


Chemical Abundances of M-dwarfs from the APOGEE Survey. I. The Exoplanet Hosting Stars Kepler-138 and Kepler-186
Diogo Souto ; Katia Cunha ; D. A. Garcia-Hernandez ; Olga Zamora ; C. Allende Prieto ; Verne Smith ; Suvrath Mahadevan Cullen Blake ; J. A. Johnson ; Henrik Jonsson ; Marc Pinsonneault ; Jon Holtzman ; S. R. Majewski ; Matthew Shetrone ; Johanna Teske ; David Nidever ; Ricardo Schiavon ; Jennifer Sobeck ; A. E. Garcia Perez ; Y. Gomez Maqueo Chew ; Keivan Stassun ;
Date 6 Dec 2016
AbstractWe report the first detailed chemical abundance analysis of the exoplanet-hosting M-dwarf stars Kepler-138 and Kepler-186 from the analysis of high-resolution ($R$ $sim$ 22,500) $H$-band spectra from the SDSS IV - APOGEE survey. Chemical abundances of thirteen elements - C, O, Na, Mg, Al, Si, K, Ca, Ti, V, Cr, Mn, and Fe - are extracted from the APOGEE spectra of these early M-dwarfs via spectrum syntheses computed with an improved line list that takes into account H$_{2}$O and FeH lines. This paper demonstrates that APOGEE spectra can be analyzed to determine detailed chemical compositions of M-dwarfs. Both exoplanet-hosting M-dwarfs display modest sub-solar metallicities: [Fe/H]$_{Kepler-138}$ = -0.09 $pm$ 0.09 dex and [Fe/H]$_{Kepler-186}$ = -0.08 $pm$ 0.10 dex. The measured metallicities resulting from this high-resolution analysis are found to be higher by $sim$0.1-0.2 dex than previous estimates from lower-resolution spectra. The C/O ratios obtained for the two planet-hosting stars are near-solar, with values of 0.55 $pm$ 0.10 for Kepler-138 and 0.52 $pm$ 0.12 for Kepler-186. Kepler-186 exhibits a marginally enhanced [Si/Fe] ratio.
Source arXiv, 1612.1598
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