Transiting exoplanets from the CoRoT space mission

Barge, P.; Baglin, A.; Auvergne, M.; Rauer, H.; Léger, Alain; Schneider, Jodi; Pont, F.; Aigrain, S.; Almenara, J. M.; Alonso, R.; Barbieri, M.; Bordé, P.; Bouchy, F.; Deeg, H. J.; Reza, R. de la; Deleuil, M.; Dvořák, R.; Erikson, A.; Fridlund, M.; Gillon, M.; Gondoin, P.; Guillot, T.; Hatzes, A. P.; Hébrard, G.; Jordá, L.; Kabáth, P.; Lämmer, H.; Llebaria, A.; Loeillet, B.; Magain, Pierre; Mazeh, T.; Moutou, C.; Ollivier, M.; Pätzold, M.; Queloz, D.; Rouan, D.; Shporer, Avi; Wuchterl, G.

doi:10.1051/0004-6361:200809353

Cited by 174 publications

(86 citation statements)

References 12 publications

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“…The findings presented herein are the result of more than 15 years of high-precision Doppler monitoring of nearby stars. Additional information will soon pour in from other surveys using techniques such as microlensing (e.g., Dong et al 2009;Gould et al 2010), astrometry (Boss et al 2009), transits (Borucki et al 2004;Barge et al 2008;Irwin et al 2009), and direct imaging (Claudi et al 2006;Artigau et al 2008;Macintosh et al 2008).…”

Section: Summary and Discussionmentioning

confidence: 99%

Giant Planet Occurrence in the Stellar Mass-Metallicity Plane

Johnson¹,

Aller²,

Howard³

et al. 2010

PUBL ASTRON SOC PAC

767

824

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ABSTRACT. Correlations between stellar properties and the occurrence rate of exoplanets can be used to inform the target selection of future planet-search efforts and provide valuable clues about the planet-formation process. We analyze a sample of 1266 stars drawn from the California Planet Survey targets to determine the empirical functional form describing the likelihood of a star harboring a giant planet as a function of its mass and metallicity. Our stellar sample ranges from M dwarfs with masses as low as 0:2 M ⊙ to intermediate-mass subgiants with masses as high as 1:9 M ⊙ . In agreement with previous studies, our sample exhibits a planet-metallicity correlation at all stellar masses; the fraction of stars that harbor giant planets scales as f ∝ 10 1:2½Fe=H . We can rule out a flat metallicity relationship among our evolved stars (at 98% confidence), which argues that the high metallicities of stars with planets is not likely due to convective envelope "pollution." Our data also rule out a constant planet occurrence rate for ½Fe=H < 0, indicating that giant planets continue to become rarer at sub-Solar metallicities. We also find that planet occurrence increases with stellar mass (f ∝ M ⋆ ), characterized by a rise from 3% around M dwarfs (0:5 M ⊙ ) to 14% around A stars (2 M ⊙ ), at Solar metallicity. We argue that the correlation between stellar properties and giant planet occurrence is strong supporting evidence of the core-accretion model of planet formation.

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Section: Summary and Discussionmentioning

confidence: 99%

Giant Planet Occurrence in the Stellar Mass-Metallicity Plane

Johnson¹,

Aller²,

Howard³

et al. 2010

PUBL ASTRON SOC PAC

767

824

View full text Add to dashboard Cite

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“…From the ashes of Kepler rose the K2 mission, which continues to find exoplanets in addition to a whole host of astrophysics enabled by its observations of fields in the ecliptic (Howell et al 2014;Van Cleve et al 2016b). While not the first to obtain high-precision, long-baseline photometry to look for transiting exoplanets (see, e.g., O'Donovan et al 2006;Barge et al 2008), Kepler and its plethora of planet candidates revolutionized exoplanet science. The large number of Kepler planet detections from the same telescope opened the door for occurrence rate studies and has enabled some of the first measurements of the frequency of planets similar to Earth in our Galaxy.…”

Section: Introductionmentioning

confidence: 99%

Planetary Candidates Observed by Kepler. VIII. A Fully Automated Catalog with Measured Completeness and Reliability Based on Data Release 25

Thompson

Coughlin

Hoffman

et al. 2018

ApJS

402

344

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We present the Kepler Object of Interest (KOI) catalog of transiting exoplanets based on searching 4 yr of Kepler time series photometry (Data Release 25, Q1-Q17). The catalog contains 8054 KOIs, of which 4034 are planet candidates with periods between 0.25and 632days. Of these candidates, 219 are new, including two in multiplanet systems (KOI-82.06 and KOI-2926.05) and 10 high-reliability, terrestrial-size, habitable zone candidates. This catalog was created using a tool called the Robovetter, which automatically vets the DR25 threshold crossing events (TCEs). The Robovetter also vetted simulated data sets and measured how well it was able to separate TCEs caused by noise from those caused by low signal-to-noise transits. We discuss the Robovetter and the metrics it uses to sort TCEs. For orbital periods less than 100 days the Robovetter completeness (the fraction of simulated transits that are determined to be planet candidates) across all observed stars is greater 1 than 85%. For the same period range, the catalog reliability (the fraction of candidates that are not due to instrumental or stellar noise) is greater than 98%. However, for low signal-to-noise candidates between 200 and 500 days around FGK-dwarf stars, the Robovetter is 76.7% complete and the catalog is 50.5% reliable. The KOI catalog, the transit fits, and all of the simulated data used to characterize this catalog are available at the NASA Exoplanet Archive.

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“…Fortunately, VHJs have high transit probabilities, and 10 Miller Research Fellow. 11 Currently CIERA Fellow. are represented by transiting planets such as WASP-12 (Hebb et al 2009), WASP-19 (Hebb et al 2010), CoRoT-1 (Barge et al 2008), and CoRoT-2 (Alonso et al 2008).…”

Section: Introductionmentioning

confidence: 99%

WARMSPITZERPHOTOMETRY OF THE TRANSITING EXOPLANETS CoRoT-1 AND CoRoT-2 AT SECONDARY ECLIPSE

Deming

Knutson

Agol

et al. 2010

ApJ

101

121

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We measure secondary eclipses of the hot giant exoplanets CoRoT-1 at 3.6 and 4.5 μm, and CoRoT-2 at 3.6 μm, both using Warm Spitzer. We find that the Warm Spitzer mission is working very well for exoplanet science. For consistency of our analysis we also re-analyze archival cryogenic Spitzer data for secondary eclipses of CoRoT-2 at 4.5 and 8 μm. We compare the total data for both planets, including optical eclipse measurements by the CoRoT mission, and ground-based eclipse measurements at 2 μm, to existing models. Both planets exhibit stronger eclipses at 4.5 than at 3.6 μm, which is often indicative of an atmospheric temperature inversion. The spectrum of CoRoT-1 is best reproduced by a 2460 K blackbody, due either to a high altitude layer that strongly absorbs stellar irradiance, or an isothermal region in the planetary atmosphere. The spectrum of CoRoT-2 is unusual because the 8 μm contrast is anomalously low. Non-inverted atmospheres could potentially produce the CoRoT-2 spectrum if the planet exhibits line emission from CO at 4.5 μm, caused by tidal-induced mass loss. However, the viability of that hypothesis is questionable because the emitting region cannot be more than about 30% larger than the planet's transit radius, based on the ingress and egress times at eclipse. An alternative possibility to account for the spectrum of CoRoT-2 is an additional opacity source that acts strongly at wavelengths less than 5 μm, heating the upper atmosphere while allowing the deeper atmosphere seen at 8 μm to remain cooler. We obtain a similar result as Gillon et al. for the phase of the secondary eclipse of CoRoT-2, implying an eccentric orbit with e cos(ω) = −0.0030 ± 0.0004.

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Transiting exoplanets from the CoRoT space mission

Cited by 174 publications

References 12 publications

Giant Planet Occurrence in the Stellar Mass-Metallicity Plane

Giant Planet Occurrence in the Stellar Mass-Metallicity Plane

Planetary Candidates Observed by Kepler. VIII. A Fully Automated Catalog with Measured Completeness and Reliability Based on Data Release 25

WARMSPITZERPHOTOMETRY OF THE TRANSITING EXOPLANETS CoRoT-1 AND CoRoT-2 AT SECONDARY ECLIPSE

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