TY - JOUR
T1 - Properties of F Stars with Stable Radial Velocity Timeseries
T2 - A Useful Metric for Selecting Low-jitter F Stars
AU - Luhn, Jacob K.
AU - Wright, Jason T.
AU - Isaacson, Howard
N1 - Publisher Copyright:
© 2020. The American Astronomical Society. All rights reserved.
PY - 2020/5
Y1 - 2020/5
N2 - In a companion paper, we have conducted an in-depth analysis of radial velocity jitter of over 600 stars, examining the astrophysical origins including stellar granulation, oscillation, and magnetic activity. In this paper, we highlight a subsample of those stars, specifically the main sequence and "retired" F stars - which we refer to as "MSRF" stars - that show low levels of RV jitter (<10 m s-1). We describe the observational signatures of these stars that allow them to be identified in radial velocity planet programs, for instance, those performing follow-up of transiting planets discovered by TESS. We introduce a "jitter metric" that combines the two competing effects of RV jitter with age: activity and convection. Using thresholds in the jitter metric, we can select both "complete" and "pure" samples of low jitter F stars. We also provide recipes for identifying these stars using only Gaia colors and magnitudes. Finally, we describe a region in the Gaia color-magnitude diagram where low jitter F stars are most highly concentrated. By fitting a ninth-order polynomial to the Gaia main sequence, we use the height above the main sequence as a proxy for evolution, allowing for a crude selection of low jitter MSRF stars when activity measurements are otherwise unavailable.
AB - In a companion paper, we have conducted an in-depth analysis of radial velocity jitter of over 600 stars, examining the astrophysical origins including stellar granulation, oscillation, and magnetic activity. In this paper, we highlight a subsample of those stars, specifically the main sequence and "retired" F stars - which we refer to as "MSRF" stars - that show low levels of RV jitter (<10 m s-1). We describe the observational signatures of these stars that allow them to be identified in radial velocity planet programs, for instance, those performing follow-up of transiting planets discovered by TESS. We introduce a "jitter metric" that combines the two competing effects of RV jitter with age: activity and convection. Using thresholds in the jitter metric, we can select both "complete" and "pure" samples of low jitter F stars. We also provide recipes for identifying these stars using only Gaia colors and magnitudes. Finally, we describe a region in the Gaia color-magnitude diagram where low jitter F stars are most highly concentrated. By fitting a ninth-order polynomial to the Gaia main sequence, we use the height above the main sequence as a proxy for evolution, allowing for a crude selection of low jitter MSRF stars when activity measurements are otherwise unavailable.
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U2 - 10.3847/1538-3881/ab775c
DO - 10.3847/1538-3881/ab775c
M3 - Article
AN - SCOPUS:85106824952
VL - 159
JO - Astronomical Journal
JF - Astronomical Journal
SN - 0004-6256
IS - 5
M1 - 234
ER -