CHARACTERIZING THE COOL KOIs. II. THE M DWARF KOI-254 AND ITS HOT JUPITER

By J. Johnson, J. Gazak, K. Apps, P. Muirhead, J. Crepp, I. Crossfield, T. Boyajian, K. von Braun, B. Rojas-Ayala, Andrew W. Howard and 6 more. 2011

146 citations recorded by the source corpus.

We report the confirmation and characterization of a transiting gas giant planet orbiting the M dwarf KOI-254 every 2.455239 days, which was originally discovered by the Kepler mission. We use radial velocity measurements, adaptive optics imaging, and near-infrared spectroscopy to confirm the planetary nature of the transit events. KOI-254 b is the first hot Jupiter discovered around an M-type dwarf star. We also present a new model-independent method of using broadband photometry to estimate the mass and metallicity of an M dwarf without relying on a direct distance measurement. Included in this methodology is a new photometric metallicity calibration based on J − K colors. We use this technique to measure the physical properties of KOI-254 and its planet. We measure a planet mass of MP  =  0.505 MJup, radius RP = 0.96 RJup, and semimajor axis a  =  0.030 AU, based on our measured stellar mass M⋆  =  0.59 M☉ and radius R⋆  =  0.55 R☉. We also find that the host star is metal-rich, which is consistent with the sample of M-type stars known to harbor giant planets.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/52f0c94242c013b527976bfe099f7c8b7a7cc985

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In Astronomy and Astrophysics

1. A. Mann
2. E. Gaidos
3. D. Charbonneau
4. Timothy Morton
5. J. Johnson
6. A. Kraus
7. C. Dressing
8. Michael J. Ireland

In Instrumentation

1. A. Mann
2. E. Gaidos
3. D. Charbonneau
4. Timothy Morton
5. C. Dressing
6. J. Johnson
7. A. Kraus
8. Jon Fortney

Citations in the corpus

• SPECTRO-THERMOMETRY OF M DWARFS AND THEIR CANDIDATE PLANETS: TOO HOT, TOO COOL, OR JUST RIGHT? (2013, unknown): “…in the online journal. a Error on Teff 58 K for all stars (see Section 5.1). b Consistent with Teff = 3820±90 K R∗ = 0.55± 0.11 and M∗ = 0.59± 0.06 from Johnson et al. (2012). c Consistent with R∗ = 0.54± 0.05, M∗ = 0.57± 0.05 from Pineda et al. (2013). d KOI 940 and KOI 2704 have Teff values…”
• They are small worlds after all: revised properties of Kepler M dwarf stars and their planets (2015, methodology): “Dilution was included as an additional parameter following the method from Johnson et al. (2011).”
• The TRAPPIST survey of southern transiting planets. I. Thirty eclipses of the ultra-short period planet WASP-43 b (2012, background): “Furthermore, it orbits arounda very cool K7-type dwarf that has the lowest mass among all the stars orbited by a hot Jupiter (0.58±0.05M⊙, Te f f = 4400±200 K, H11), except for the recently announced M0 dwarf KOI-254 (0.59 ± 0.06M⊙, Te f f = 3820± 90 K, Johnson et al. 2011).”
• PROSPECTING IN LATE-TYPE DWARFS: A CALIBRATION OF INFRARED AND VISIBLE SPECTROSCOPIC METALLICITIES OF LATE K AND M DWARFS SPANNING 1.5 dex (2012, methodology): “K-band Metallicities R10 have shown that one could derive M dwarf metallicities from K-band spectra using the Na I and Ca I lines (at 2.21µm and 2.26µm).”
• THE OCCURRENCE OF POTENTIALLY HABITABLE PLANETS ORBITING M DWARFS ESTIMATED FROM THE FULL KEPLER DATASET AND AN EMPIRICAL MEASUREMENT OF THE DETECTION SENSITIVITY (2015, background): “Other authors further constrained the properties of particular planet host stars and associated planet candidates by acquiring followup spectroscopic and high resolution imaging observations (Johnson et al. 2012; Muirhead et al. 2012a,b; Ballard et al. 2013; Muirhead et al. 2013; Swift et al. 2013).”
• NEAR-INFRARED METALLICITIES, RADIAL VELOCITIES, AND SPECTRAL TYPES FOR 447 NEARBY M DWARFS (2013, background): “Johnson et al. (2012) combined existing photometric relations to estimate the stellar properties of KOI-254, one of the few M dwarfs known to host a hot Jupiter.”
• THE OCCURRENCE RATE OF SMALL PLANETS AROUND SMALL STARS (2013, methodology): “…the transit parameters for KOIs 248.03, 248.04, and 886.03 from Steffen et al. (2012a), KOI 250.03 from Steffen et al. (2012b), KOIs 952.03 and 952.04 from Fabrycky et al. (2012a), and KOI 254.01 from Johnson et al. (2012) because the authors com- pleted extensive modeling of their light curves.”
• HOW TO CONSTRAIN YOUR M DWARF: MEASURING EFFECTIVE TEMPERATURE, BOLOMETRIC LUMINOSITY, MASS, AND RADIUS (2015, background): “(6)eff 2 3 4 In the case that metallically is not known, JHKS colors can be used to approximate metallicity (Leggett 1992; Johnson et al. 2012; Mann et al. 2013a; Newton et al. 2014).”
• CHARACTERIZING THE COOL KOIs. IV. KEPLER-32 AS A PROTOTYPE FOR THE FORMATION OF COMPACT PLANETARY SYSTEMS THROUGHOUT THE GALAXY (2012, methodology): “Aside from a single outlier—the hot Jupiter system around KOI-254 (Johnson et al. 2012)—the ensemble of 100 planet candidates around these M dwarfs have radii ranging from ∼ 0.5 to 3R⊕ and semimajor axes within about a few tenths of an astronomical unit (Muirhead et al. 2012a).”
• FUNDAMENTAL PROPERTIES OF KEPLER PLANET-CANDIDATE HOST STARS USING ASTEROSEISMOLOGY (2013, unknown): “This revision (hereafter referred to as YY values) was justified since KIC surface gravities for some stars, in particular for cool M-dwarfs and for G-type dwarfs, seemed unphysical compared to predictions from stellar evolutionary theory.”