Planetary transit candidates in Corot-IRa01 field

Carpano, S.; Cabrera, J.; Alonso, R.; Barge, P.; Aigrain, S.; Almenara, J. M.; Bordé, P.; Bouchy, F.; Carone, L.; Deeg, H. J.; Reza, R. de la; Deleuil, M.; Dvořák, R.; Erikson, A.; Fressin, François; Fridlund, M.; Gondoin, P.; Guillot, T.; Hatzes, A. P.; Jordá, L.; Lämmer, H.; Léger, Alain; Llebaria, A.; Magain, Pierre; Moutou, C.; Ofir, A.; Ollivier, M.; Janot-Pacheco, E.; Pätzold, M.; Pont, F.; Queloz, D.; Rauer, H.; Régulo, C.; Renner, S.; Rouan, D.; Samuel, B.; Schneider, Jodi; Wuchterl, G.

doi:10.1051/0004-6361/200911882

Cited by 38 publications

(65 citation statements)

References 23 publications

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“…Whenever transits are detected in a CoRoT LC and when the candidate survives the set of tests performed to rule out obvious stellar systems (see Carpano et al 2009) a ground based followup programme is initiated. The goal is to check further for possible contaminating eclipsing binaries (EBs) whose point spread function (PSF) could fall within the CoRoT photometric mask.…”

Section: Photometric and Imaging Follow-upmentioning

confidence: 99%

Transiting exoplanets from the CoRoT space mission

Léger¹,

Rouan²,

Schneider³

et al. 2009

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Aims. We report the discovery of very shallow (ΔF/F ≈ 3.4× 10 −4 ), periodic dips in the light curve of an active V = 11.7 G9V star observed by the CoRoT satellite, which we interpret as caused by a transiting companion. We describe the 3-colour CoRoT data and complementary ground-based observations that support the planetary nature of the companion. Methods. We used CoRoT colours information, good angular resolution ground-based photometric observations in-and out-of transit, adaptive optics imaging, near-infrared spectroscopy, and preliminary results from radial velocity measurements, to test the diluted eclipsing binary scenarios. The parameters of the host star were derived from optical spectra, which were then combined with the CoRoT light curve to derive parameters of the companion. Results. We examined all conceivable cases of false positives carefully, and all the tests support the planetary hypothesis. Blends with separation >0.40 or triple systems are almost excluded with a 8 × 10 −4 risk left. We conclude that, inasmuch we have been exhaustive, we have discovered a planetary companion, named CoRoT-7b, for which we derive a period of 0.853 59 ± 3 × 10 −5 day and a radius of R p = 1.68 ± 0.09 R Earth . Analysis of preliminary radial velocity data yields an upper limit of 21 M Earth for the companion mass, supporting the finding. Conclusions. CoRoT-7b is very likely the first Super-Earth with a measured radius. This object illustrates what will probably become a common situation with missions such as Kepler, namely the need to establish the planetary origin of transits in the absence of a firm radial velocity detection and mass measurement. The composition of CoRoT-7b remains loosely constrained without a precise mass. A very high surface temperature on its irradiated face, ≈1800-2600 K at the substellar point, and a very low one, ≈50 K, on its dark face assuming no atmosphere, have been derived.

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Section: Photometric and Imaging Follow-upmentioning

confidence: 99%

Transiting exoplanets from the CoRoT space mission

Léger¹,

Rouan²,

Schneider³

et al. 2009

A&A

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513

378

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“…If all close-in planets of A stars would induce oscillations, it would be easy to understand why only one has been found. It is also interesting to note that there are transit candidates of early-type stars published by the CoRoT (Carpano et al 2009) and Kepler space-missions (Borucki et al 2011). Since the spectral types of these candidates are not well known, none of these candidates were confirmed as planets of an intermediate-mass star so far.…”

Section: The Frequency Of Planets Orbiting A-type Starsmentioning

confidence: 99%

Multi-object spectroscopy of stars in the CoRoT fields

Sebastian

Guenther

Schaffenroth

et al. 2012

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Context. Observations of giant stars indicate that the frequency of giant planets is much higher for intermediate-mass stars than for solar-like stars. Up to now all known planets of giant stars orbit at relatively far distances from their host stars. It is not known whether intermediate-mass stars also had many close-in planets when they were on the main sequence, which were then engulfed when the star became a giant star. To understand the formation and evolution of planets it is therefore important to find out whether main-sequence stars of intermediate-mass have close-in planets or not. Aims. A survey for transiting planets of intermediate-mass stars would be ideal to solve this question, because the detection of transiting planets is not affected by the rapid rotation of these stars. With CoRoT it is possible to detect transiting planets around stars up to a spectral type B4V. As a first step for an efficient survey we need to identify intermediate-mass stars in the CoRoT-fields, which can then be used as an input list. Methods. To compile the input list we derived the spectral types of essentially all O, B and A stars down to 14.5 mag in the CoRoT fields IRa01, LRa01, LRa02 taken with the multi-object spectrograph AAOmega. We determined the spectral types by comparing the spectra with template spectra from a library. Results. In total we identify 1856 A and B stars that have been observed with CoRoT. Using multiple spectra of these stars, we find that the accuracy of the resulting spectral classification is 1.61 ± 0.14 sub-classes for A and B stars. Conclusions. Given the number of planets that have been detected in these fields amongst late-type stars, we estimate that there are one to four transiting planets of intermediate-mass stars waiting to be discovered. Our survey not only allows us to carry out a dedicated planet search programme but is also essential for any types of studies of the light curves of early-type stars in the CoRoT database. We also show that it would be possible to extend the survey to all fields that CoRoT has observed using photometrically determined spectral types.

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“…A description of this detection effort and the properties of the entire sample will be given by Barge et al (in prep.). Detection results are also described in more detail by Carpano et al (2009) for the IRa01 observing run data and by Cabrera et al (2009) for the LRc01 data, descriptions of the later runs being in preparation. All detections from the light-curves (planets and EBs) are included in a common detection list.…”

Section: The Sample Of Candidatesmentioning

confidence: 99%

“…All detections from the light-curves (planets and EBs) are included in a common detection list. Most of these detections are then rejected by means of an analysis of the light-curves, taking into account the depth, duration, shape and color signature, among others, and become classified as unspecified binary systems (for details of this procedure see Carpano et al 2009). The remaining candidates are classified in terms of their "planet-likeliness", and forwarded to the observational followup.…”

Section: The Sample Of Candidatesmentioning

confidence: 99%

Rate and nature of false positives in the CoRoT exoplanet search

Almenara

Deeg

Aigrain

et al. 2009

A&A

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Context. The CoRoT satellite searches for planets by applying the transit method, monitoring up to 12 000 stars in the galactic plane for 150 days in each observing run. This search is contaminated by a large fraction of false positives, caused by different eclipsing binary configurations that might be confused with a transiting planet. Aims. We evaluate the rates and nature of false positives in the CoRoT exoplanets search and compare our results with semiempirical predictions. Methods. We consider the detected binary and planet candidates in the first three extended CoRoT runs, and classify the results of the follow-up observations completed to verify their planetary nature. We group the follow-up results into undiluted binaries, diluted binaries, and planets and compare their abundances with predictions from the literature. Results. 83% of the initial detections are classified as false positives using only the CoRoT light-curves, the remaining 17% require follow-up observations. Finally, 12% of the candidates in the follow-up program are planets. The shape of the overall distribution of the false positive rate follows previous predictions, except for candidates with transit depths below about 0.4%. For candidates with transit depths in the range from 0.1-0.4%, CoRoT detections are nearly complete, and this difference from predictions is probably real and dominated by a lower than expected abundance of diluted eclipsing binaries.

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Planetary transit candidates in Corot-IRa01 field

Cited by 38 publications

References 23 publications

Transiting exoplanets from the CoRoT space mission

Transiting exoplanets from the CoRoT space mission

Multi-object spectroscopy of stars in the CoRoT fields

Rate and nature of false positives in the CoRoT exoplanet search

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