Elemental Abundances of the Super-Neptune WASP-107b’s Host Star Using High-resolution, Near-infrared Spectroscopy

We present the first elemental abundance measurements of the K dwarf (K7V) exoplanet-host star WASP-107 using high-resolution ( R ≃45,000), near-infrared ( H - and K -band) spectra taken from Gemini-S/IGRINS. We use the previously determined physical parameters of the star from the literature and in...

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Bibliographic Details
Published in:The Astrophysical journal 2023-06, Vol.949 (2), p.79
Main Authors: Hejazi, Neda, Crossfield, Ian J. M., Nordlander, Thomas, Mansfield, Megan, Souto, Diogo, Marfil, Emilio, Coria, David R., Brande, Jonathan, Polanski, Alex S., Hand, Joseph E., Wienke, Kate F.
Format: Article
Language:English
Subjects:
Abundance
Aluminum
Astrophysics
Chemical composition
Chromium
Extrasolar planets
High resolution
Infrared spectra
Infrared spectroscopy
Jupiter
K dwarf stars
Magnesium
Manganese
Near infrared radiation
Near infrared spectroscopy
Neptune
Oxygen
Physical properties
Planets
Silicon
Spectrum analysis
Stars
Stars & galaxies
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Summary:We present the first elemental abundance measurements of the K dwarf (K7V) exoplanet-host star WASP-107 using high-resolution ( R ≃45,000), near-infrared ( H - and K -band) spectra taken from Gemini-S/IGRINS. We use the previously determined physical parameters of the star from the literature and infer the abundances of 15 elements—C, N, O, Na, Mg, Al, Si, K, Ca, Ti, V, Cr, Mn, Fe, and Ni, all with precision < 0.1 dex—based on model fitting using MARCS model atmospheres and the Turbospectrum spectral synthesis code. Our results show near-solar abundances and a carbon-to-oxygen ratio (C/O) of 0.50 ± 0.10, which is consistent with the solar value of 0.54 ± 0.09. The orbiting planet, WASP-107b, is a super-Neptune with a mass in the Neptune regime (=1.8 M Nep ) and a radius close to Jupiter's (=0.94 R Jup ). This planet is also being targeted by four JWST Cycle 1 programs in transit and eclipse, which should provide highly precise measurements of atmospheric abundances. This will enable us to properly compare the planetary and stellar chemical abundances, which is essential in understanding the formation mechanisms, internal structure, and chemical composition of exoplanets. Our study is a proof-of-concept that will pave the way for such measurements to be made for all of JWST’s cooler exoplanet-host stars.
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/accb97