Detection of a transit of the super-Earth 55 Cancri e with warm Spitzer

By B. Demory, M. Gillon, D. Deming, Diana Valencia, S. Seager, Björn Benneke, C. Lovis, P. Cubillos, J. Harrington, Kevin B. Stevenson and 5 more. 2011

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We report on the detection of a transit of the super-Earth 55 Cnc e with warm Spitzer in IRAC’s 4.5 μm band. Our MCMC analysis includes an extensive modeling of the systematic effects affecting warm Spitzer photometry, and yields a transit depth of 410±63 ppm, which translates to a planetary radius of 2.08 +0.16 −0.17 R⊕ as measured in IRAC 4.5 μm channel. A planetary mass of 7.81 +0.58 −0.53 M⊕ is derived from an extensive set of radial-velocity data, yielding a mean planetary density of 4.78 +1.31 −1.20 gc m −3 . Thanks to the brightness of its host star (V = 6, K = 4), 55 Cnc e is a unique target for the thorough characterization of a super-Earth orbiting around a solar-type star.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/b6e77648098e002c44ee09ee5a471bc1388f98bc

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Citations in the corpus

DETECTION OF AN ATMOSPHERE AROUND THE SUPER-EARTH 55 CANCRI E (2015, methodology): “Transits from space of 55 Cancri e were observed with the Spitzer Space Telescope (Demory et al. 2011) and MOST space telescope (Winn et al. 2011), confirming its small size (∼ 2R⊕).”
A STUDY OF THE SHORTEST-PERIOD PLANETS FOUND WITH KEPLER (2014, background): “Among the best known USP planets are 55 Cnc e (Dawson & Fabrycky 2010; Winn et al. 2011; Demory et al. 2011a), CoRoT-7b (Léger et al. 2009; Queloz et al. 2009), and Kepler-10b (Batalha et al. 2011).”
ALL SIX PLANETS KNOWN TO ORBIT KEPLER-11 HAVE LOW DENSITIES (2013, background): “The three planets that lie above this threshold in the upper right are Kepler-10 b (Batalha et al. 2011), CoRoT-7 b (Léger et al. 2009; Queloz et al. 2009; Hatzes et al. 2011), and 55 Cancri e (Winn et al. 2011; Demory et al. 2011), none of which are expected to have H/He envelopes.”
A POSSIBLE CARBON-RICH INTERIOR IN SUPER-EARTH 55 Cancri e (2012, methodology): “However, the recent discovery of its transits across the host star (Winn et al. 2011; Demory et al. 2011) has made possible accurate measurements of its mass (8.37 ± 0.38 M⊕; Endl et al. 2012) and radius (2.04 ± 0.15 R⊕; Gillon et al. 2012), and, hence, constraints on its interior composition.”
PHOTOCHEMISTRY IN TERRESTRIAL EXOPLANET ATMOSPHERES. I. PHOTOCHEMISTRY MODEL AND BENCHMARK CASES (2012, background): “…et al. 2009; Mayor et al. 2009; Vogt et al. 2010; Rivera et al. 2010; Dawson & Fabrycky 2010; Holman et al. 2010; Howard et al. 2011; Bonfils et al. 2011; Winn et al. 2011; Demory et al. 2011; Batalha et al. 2011; Lissauer et al., 2011; Borucki et al. 2011; Fressin et al 2012; Cochran et al. 2012).”
Compositional Imprints in Density–Distance–Time: A Rocky Composition for Close-in Low-mass Exoplanets from the Location of the Valley of Evaporation (2017, result): “For it, a fice,mean=20% with an interval between 4 to 34% ice was found, in agreement with Demory et al. (2011).”
HOW THERMAL EVOLUTION AND MASS-LOSS SCULPT POPULATIONS OF SUPER-EARTHS AND SUB-NEPTUNES: APPLICATION TO THE KEPLER-11 SYSTEM AND BEYOND (2012, unknown): “…2009; Hatzes et al. 2011), Kepler-20b (Fressin et al. 2012; Gautier et al. 2012), Kepler-18b (Cochran et al. 2011), 55 Cancri e (Winn et al. 2011; Demory et al. 2011), GJ 1214b (Charbonneau et al. 2009), Kepler-36c (Carter et al. 2012), Kepler-30b (Fabrycky et al. 2012; Sanchis-Ojeda et al.…”
HUBBLE SPACE TELESCOPE NEAR-IR TRANSMISSION SPECTROSCOPY OF THE SUPER-EARTH HD 97658B (2014, background): “There are currently three superEarths known to transit relatively bright stars, including: GJ 1214b (mK = 8.8; Charbonneau et al. 2009), 55 Cancri e (mK = 4.0; Winn et al. 2011; Demory et al. 2011), and HD 97658b (mK = 5.7; Dragomir et al. 2013).”
INFERENCE OF INHOMOGENEOUS CLOUDS IN AN EXOPLANET ATMOSPHERE (2013, methodology): “Its relatively low mass Mp = 0.44 ± 0.04MJup and large radius Rp = 1.61 ± 0.02RJup result in a very low density ρp = 0.14g cm−3 (Demory et al. 2011b, hereafter D11).”