TY - JOUR
T1 - Early Results from the HUMDRUM Survey
T2 - A Small, Earth-mass Planet Orbits TOI-1450A
AU - Brady, Madison
AU - Bean, Jacob L.
AU - Seifahrt, Andreas
AU - Kasper, David
AU - Luque, Rafael
AU - Stefánsson, Guđmundur
AU - Stürmer, Julian
AU - Charbonneau, David
AU - Collins, Karen A.
AU - Doty, John P.
AU - Essack, Zahra
AU - Fukui, Akihiko
AU - Horta, Ferran Grau
AU - Hedges, Christina
AU - Hellier, Coel
AU - Jenkins, Jon M.
AU - Narita, Norio
AU - Quinn, Samuel N.
AU - Shporer, Avi
AU - Schwarz, Richard P.
AU - Seager, Sara
AU - Stassun, Keivan G.
AU - Striegel, Stephanie
AU - Watkins, Cristilyn N.
AU - Winn, Joshua N.
AU - Zambelli, Roberto
N1 - Publisher Copyright:
© 2024. The Author(s). Published by the American Astronomical Society.
PY - 2024/8/1
Y1 - 2024/8/1
N2 - M-dwarf stars provide us with an ideal opportunity to study nearby small planets. The HUnting for M Dwarf Rocky planets Using MAROON-X (HUMDRUM) survey uses the MAROON-X spectrograph, which is ideally suited to studying these stars, to measure precise masses of a volume-limited (<30 pc) sample of transiting M-dwarf planets. TOI-1450 is a nearby (22.5 pc) binary system containing a M3 dwarf with a roughly 3000 K companion. Its primary star, TOI-1450A, was identified by the Transiting Exoplanet Survey Satellite (TESS) to have a 2.04 days transit signal, and is included in the HUMDRUM sample. In this paper, we present MAROON-X radial velocities (RVs) which confirm the planetary nature of this signal and measure its mass at nearly 10% precision. The 2.04 days planet, TOI-1450A b, has R b = 1.13 ± 0.04 R ⊕ and M b = 1.26 ± 0.13 M ⊕. It is the second-lowest-mass transiting planet with a high-precision RV mass measurement. With this mass and radius, the planet’s mean density is compatible with an Earth-like composition. Given its short orbital period and slightly sub-Earth density, it may be amenable to JWST follow-up to test whether the planet has retained an atmosphere despite extreme heating from the nearby star. We also discover a nontransiting planet in the system with a period of 5.07 days and a M sin i c = 1.53 ± 0.18 M ⊕ . We also find a 2.01 days signal present in the systems’s TESS photometry that likely corresponds to the rotation period of TOI-1450A’s binary companion, TOI-1450B. TOI-1450A, meanwhile, appears to have a rotation period of approximately 40 days, which is in line with our expectations for a mid-M dwarf.
AB - M-dwarf stars provide us with an ideal opportunity to study nearby small planets. The HUnting for M Dwarf Rocky planets Using MAROON-X (HUMDRUM) survey uses the MAROON-X spectrograph, which is ideally suited to studying these stars, to measure precise masses of a volume-limited (<30 pc) sample of transiting M-dwarf planets. TOI-1450 is a nearby (22.5 pc) binary system containing a M3 dwarf with a roughly 3000 K companion. Its primary star, TOI-1450A, was identified by the Transiting Exoplanet Survey Satellite (TESS) to have a 2.04 days transit signal, and is included in the HUMDRUM sample. In this paper, we present MAROON-X radial velocities (RVs) which confirm the planetary nature of this signal and measure its mass at nearly 10% precision. The 2.04 days planet, TOI-1450A b, has R b = 1.13 ± 0.04 R ⊕ and M b = 1.26 ± 0.13 M ⊕. It is the second-lowest-mass transiting planet with a high-precision RV mass measurement. With this mass and radius, the planet’s mean density is compatible with an Earth-like composition. Given its short orbital period and slightly sub-Earth density, it may be amenable to JWST follow-up to test whether the planet has retained an atmosphere despite extreme heating from the nearby star. We also discover a nontransiting planet in the system with a period of 5.07 days and a M sin i c = 1.53 ± 0.18 M ⊕ . We also find a 2.01 days signal present in the systems’s TESS photometry that likely corresponds to the rotation period of TOI-1450A’s binary companion, TOI-1450B. TOI-1450A, meanwhile, appears to have a rotation period of approximately 40 days, which is in line with our expectations for a mid-M dwarf.
UR - https://www.scopus.com/pages/publications/85198615075
UR - https://www.scopus.com/pages/publications/85198615075#tab=citedBy
U2 - 10.3847/1538-3881/ad500a
DO - 10.3847/1538-3881/ad500a
M3 - Article
AN - SCOPUS:85198615075
SN - 0004-6256
VL - 168
JO - Astronomical Journal
JF - Astronomical Journal
IS - 2
M1 - 67
ER -