collaborators

12 papers

astro-ph.SR2026

A Test of FeH Line Parameters using DR19 APOGEE spectra of Benchmark M Dwarfs

Anderson Silva-Andrade, Diogo Souto, Katia Cunha +9

Recent studies have suggested a mismatch of up to 0.20 dex between iron abundances derived from Fe I and FeH lines in the H-band spectra of M dwarfs, and in this work we investigat…

astro-ph.SR2025

Stellar characterization, Magnesium Abundances and Chromospheric Activity Analysis of Stars with Confirmed Exoplanets from the K2 mission

V. Loaiza-Tacuri, Diogo Souto, F. Quispe-Huaynasi +5

We present a homogeneous spectroscopic analysis of confirmed K2 mission exoplanet-hosting stars, comprising 301 targets with high-resolution optical spectra from HIRES and TRES tak…

astro-ph.SR2025

Chemical Abundances of M and G Dwarfs in the Hyades and Coma Berenices Open Clusters from APOGEE Spectra

Deusalete Vilar, Diogo Souto, Katia Cunha +8

Open clusters are one of the best astrophysical laboratories we have available for stellar astrophysics studies. This work presents metallicities and individual abundances for four…

astro-ph.EP2025

An Analysis of the Radius Gap in a Sample of Kepler, K2 and TESS exoplanets orbiting M Dwarf Stars

Fábio Wanderley, Katia Cunha, Verne V. Smith +11

Planetary radii are derived for 218 exoplanets orbiting 161 M dwarf stars. Stellar radii are based on an analysis of APOGEE high-resolution near-IR spectra for a subsample of the M…

astro-ph.SR2025

Metallicities of M Dwarf Planet Host Stars from Kepler, K2, and TESS observed by APOGEE: Trends with Exoplanetary Radii and Orbital Periods

Fábio Wanderley, Katia Cunha, Diogo Souto +2

One important property in studying the exoplanet population is the host star metallicity ([M/H]). In this study, we derived stellar metallicities and oxygen abundances for 48 M dwa…

astro-ph.SR2025

Abundances of P, S, and K in 58 bulge spheroid stars from APOGEE

B. Barbuy, H. Ernandes, A. C. S. Friaça +25

We have previously studied several elements in 58 selected bulge spheroid stars, based on spectral lines in the H-band. We now derive the abundances of the less-studied elements ph…