Multiple Kepler "Terrestrial" Exoplanets are Really SuperEarths and Mini Neptunes

REVISION OF EARTH-SIZED KEPLER PLANET CANDIDATE PROPERTIES WITH HIGH-RESOLUTION IMAGING BY THE HUBBLE SPACE TELESCOPE

Authors:

Cartier et al

Abstract:

We present the results of our Hubble Space Telescope program and describe how our analysis methods were used to re-evaluate the habitability of some of the most interesting Kepler planet candidates. Our program observed 22 Kepler Object of Interest (KOI) host stars, several of which were found to be multiple star systems unresolved by Kepler. We use our high-resolution imaging to spatially resolve the stellar multiplicity of Kepler-296, KOI-2626, and KOI-3049, and develop a conversion to the Kepler photometry (Kp) from the F555W and F775W filters on WFC3/UVIS. The binary system Kepler-296 (five planets) has a projected separation of $0\buildrel{\prime\prime}\over{.} 217$ (80 AU); KOI-2626 (one planet candidate) is a triple star system with a projected separation of $0\buildrel{\prime\prime}\over{.} 201$ (70 AU) between the primary and secondary components and $0\buildrel{\prime\prime}\over{.} 161$ (55 AU) between the primary and tertiary; and the binary system KOI-3049 (one planet candidate) has a projected separation of $0\buildrel{\prime\prime}\over{.} 464$ (225 AU). We use our measured photometry to fit the separated stellar components to the latest Victoria–Regina Stellar Models with synthetic photometry to conclude that the systems are coeval. The components of the three systems range from mid-K dwarf to mid-M dwarf spectral types.We solved for the planetary properties of each system analytically and via an MCMC algorithm using our independent stellar parameters. The planets range from $\sim 1.6\;\;{\rm to}\;\sim 4.2\;{{R}_{\oplus }}$, mostly Super Earths and mini-Neptunes. As a result of the stellar multiplicity, some planets previously in the Habitable Zone are, in fact, not, and other planets may be habitable depending on their assumed stellar host.

S Type Circumbinary Exoplanetary System Kepler-296 has two SuperEarths in the Potential Habitable Zone

The Five Planets in the Kepler-296 Binary System All Orbit the Primary: A Statistical and Analytical Analysis

Authors:

Barclay et al

Abstract:

Kepler-296 is a binary star system with two M-dwarf components separated by 0.2 arcsec. Five transiting planets have been confirmed to be associated with the Kepler-296 system; given the evidence to date, however, the planets could in principle orbit either star. This ambiguity has made it difficult to constrain both the orbital and physical properties of the planets. Using both statistical and analytical arguments, this paper shows that all five planets are highly likely to orbit the primary star in this system. We performed a Markov-Chain Monte Carlo simulation using a five transiting planet model, leaving the stellar density and dilution with uniform priors. Using importance sampling, we compared the model probabilities under the priors of the planets orbiting either the brighter or the fainter component of the binary. A model where the planets orbit the brighter component, Kepler-296A, is strongly preferred by the data. Combined with our assertion that all five planets orbit the same star, the two outer planets in the system, Kepler-296 Ae and Kepler-296 Af, have radii of 1.53 +/- 0.26 and 1.80 +/- 0.31 R_earth, respectively, and receive incident stellar fluxes of 1.40 +/- 0.23 and 0.62 +/- 0.10 times the incident flux the Earth receives from the Sun. This level of irradiation places both planets within or close to the circumstellar habitable zone of their parent star.

Hubble Telescope Reexamines Some Kepler Candidates, Disputes Many Superearths in Habitable Zones

Revision of Earth-sized Kepler Planet Candidate Properties with High Resolution Imaging by Hubble Space Telescope

Authors:

Star et al

Abstract:

We present the results of our Hubble Space Telescope program and describe how our image analysis methods were used to re-evaluate the habitability of some of the most interesting Kepler planet candidates. Our program observed 22 KOI hosts, several of which were found to be multiple star systems unresolved by Kepler. We use our high-resolution imaging to provide a conversion to the Kepler photometric bandpass (Kp) from the F555W and F775W filters on WFC3/UVIS, and spatially resolve the stellar multiplicity of Kepler-296, KOI-2626, and KOI-3049. The binary system Kepler-296 has a projected separation of 0.217" (80 AU); KOI-2626 is a triple star system with a projected separation of 0.201" (70 AU) between the primary and secondary components and 0.161" (55 AU) between the primary and tertiary components; and the binary system KOI-3049 has a projected separation of 0.464" (225 AU). Using theoretical isochrones from the latest Victoria-Regina Stellar Models, we performed hierarchical fitting using our derived photometry and the synthetic photometry from the isochrones. We find that the individual components of the three systems range from mid-K dwarf to mid-M dwarf spectral types. We solved for the planetary properties in the three systems directly from the stellar and published transit parameters and from empirically derived relations. We find that the planets range in size from ~1.2Re to ~4Re, placing them in the Super Earth/mini-Neptune regime. As a result of the stellar multiplicity, we find that some planets previously in the Habitable Zone are, in fact, not, and that other planets may be in the HZ depending on their assumed stellar host.