TY - JOUR
T1 - Ly Observations of high radial velocity low-mass stars ross 1044 and ross 825
AU - Schneider, Adam C.
AU - Shkolnik, Evgenya L.
AU - Barman, Travis S.
AU - Loyd, R. Parke
N1 - Funding Information:
the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555
PY - 2019/11/20
Y1 - 2019/11/20
N2 - The discovery of habitable zone (HZ) planets around low-mass stars has highlighted the need for a comprehensive understanding of the radiation environments in which such planets reside. Of particular importance is knowledge of the far-ultraviolet (FUV) radiation, as low-mass stars are typically much more active than solar-type stars and the proximity of their HZs can be one-tenth the distance. The vast majority of the flux emitted by low-mass stars at FUV wavelengths occurs in the Ly line at 1216. However, measuring a low-mass star's Ly emission directly is almost always impossible because of the contaminating effects of interstellar hydrogen and geocoronal airglow. We observed Ross 825 (K3) and Ross 1044 (M0), two stars with exceptional radial velocities, with the Space Telescope Imaging Spectrograph on board the Hubble Space Telescope. Their radial velocities resulted in significant line shifts, allowing for a more complete view of their Ly line profiles. We provide an updated relation between effective temperature and Ly flux using Gaia DR2 astrometry as well as updated, model-independent relationships between Ly flux and UV flux measurements from the Galaxy Evolution Explorer (GALEX) for low-mass stars. These new relations, in combination with GALEX's considerable spatial coverage, provide substantial predictive power for the Ly environments for thousands of nearby, low-mass stars.
AB - The discovery of habitable zone (HZ) planets around low-mass stars has highlighted the need for a comprehensive understanding of the radiation environments in which such planets reside. Of particular importance is knowledge of the far-ultraviolet (FUV) radiation, as low-mass stars are typically much more active than solar-type stars and the proximity of their HZs can be one-tenth the distance. The vast majority of the flux emitted by low-mass stars at FUV wavelengths occurs in the Ly line at 1216. However, measuring a low-mass star's Ly emission directly is almost always impossible because of the contaminating effects of interstellar hydrogen and geocoronal airglow. We observed Ross 825 (K3) and Ross 1044 (M0), two stars with exceptional radial velocities, with the Space Telescope Imaging Spectrograph on board the Hubble Space Telescope. Their radial velocities resulted in significant line shifts, allowing for a more complete view of their Ly line profiles. We provide an updated relation between effective temperature and Ly flux using Gaia DR2 astrometry as well as updated, model-independent relationships between Ly flux and UV flux measurements from the Galaxy Evolution Explorer (GALEX) for low-mass stars. These new relations, in combination with GALEX's considerable spatial coverage, provide substantial predictive power for the Ly environments for thousands of nearby, low-mass stars.
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U2 - 10.3847/1538-4357/ab48de
DO - 10.3847/1538-4357/ab48de
M3 - Article
AN - SCOPUS:85077344485
VL - 886
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 1
M1 - 19
ER -