A Hot Mars-sized Exoplanet Transiting an M Dwarf

We validate the planetary nature of an ultra-short-period planet orbiting the M dwarf KOI-4777. We use a combination of space-based photometry from Kepler, high-precision, near-infrared Doppler spectroscopy from the Habitable-zone Planet Finder, and adaptive optics imaging to characterize this syste...

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Bibliographic Details
Published in:The Astronomical journal 2022-01, Vol.163 (1), p.3
Main Authors: Cañas, Caleb I., Mahadevan, Suvrath, Cochran, William D., Bender, Chad F., Feigelson, Eric D., Harman, C. E., Kopparapu, Ravi Kumar, Caceres, Gabriel A., Diddams, Scott A., Endl, Michael, Ford, Eric B., Halverson, Samuel, Hearty, Fred, Jones, Sinclaire, Kanodia, Shubham, Lin, Andrea S. J., Metcalf, Andrew J., Monson, Andrew, Ninan, Joe P., Ramsey, Lawrence W., Robertson, Paul, Roy, Arpita, Schwab, Christian, Stefánsson, Guđmundur
Format: Article
Language:English
Subjects:
Adaptive optics
Astronomy
Circumstellar habitable zone
Exoplanets
Extrasolar planets
Extrasolar rocky planets
Infrared photometry
Mars
Near infrared radiation
Optics
Planets
Red dwarf stars
Spectroscopy
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Summary:We validate the planetary nature of an ultra-short-period planet orbiting the M dwarf KOI-4777. We use a combination of space-based photometry from Kepler, high-precision, near-infrared Doppler spectroscopy from the Habitable-zone Planet Finder, and adaptive optics imaging to characterize this system. KOI-4777.01 is a Mars-sized exoplanet ( R p = 0.51 ± 0.03 R ⊕ ) orbiting the host star every 0.412 days (∼9.9 hr). This is the smallest validated ultra-short period planet known and we see no evidence for additional massive companions using our HPF RVs. We constrain the upper 3 σ mass to M p < 0.34 M ⊕ by assuming the planet is less dense than iron. Obtaining a mass measurement for KOI-4777.01 is beyond current instrumental capabilities.
ISSN:0004-6256
1538-3881
DOI:10.3847/1538-3881/ac3088