Elemental Abundances of Kepler Objects of Interest in APOGEE DR17

Aida Behmard, Melissa K. Ness, Emily C. Cunningham, Megan Bedell

Research output: Contribution to journalArticlepeer-review

4 Citations (Scopus)

Abstract

The elemental abundances of planet host stars can shed light on the conditions of planet forming environments. We
test if individual abundances of 130 known/candidate planet hosts in APOGEE are statistically different from
those of a reference doppelgänger sample. The reference set comprises objects selected with the same Teff,
log ,
[Fe/H], and [Mg/H] as each Kepler Object of Interest (KOI). We predict twelve individual abundances (X = C, N,
O, Na, Al, Si, Ca, Ti, V, Cr, Mn, Ni) for the KOIs and their doppelgängers using a local linear model of these four
parameters, training on ASPCAP abundance measurements for a sample of field stars with high-fidelity (signal-to
noise ratio > 200) APOGEE observations. We compare element prediction residuals (model–measurement) for the
two samples and find them to be indistinguishable, given a high-quality sample selection. We report median
intrinsic dispersions of ∼0.038 dex and ∼0.041 dex, for the KOI and doppelgänger samples, respectively, for these
g
elements. We conclude that the individual abundances at fixed Teff,
log , [Fe/H], and [Mg/H] are unremarkable
for known planet hosts. Our results establish an upper limit on the abundance precision required to uncover any
chemical signatures of planet formation in planet host stars.
Original languageEnglish
Pages (from-to)165-178
Number of pages14
JournalThe Astronomical Journal
Volume165
Issue number4
DOIs
Publication statusPublished - Apr 2023
Externally publishedYes

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