The “666” collaboration on OGLE transits

Pont, F.; Moutou, C.; Gillon, M.; Udalski, A.; Bouchy, F.; Fernandes, J.; Gieren, W.; Mayor, M.; Mazeh, T.; Minniti, D.; Melo, C.; Naef, D.; Pietrzyński, G.; Queloz, D.; Ruíz, M. T.; Santos, N. C.; Udry, S.

doi:10.1051/0004-6361:20066645

Cited by 40 publications

(66 citation statements)

References 25 publications

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“…Therefore, the estimates for the decrease in the orbital period due to orbital decay range from 0.1 to 10 ms yr −1 . This value is only a few times smaller than the current error on the orbital period (86 ms from Pont et al 2007). …”

Section: Introductionmentioning

confidence: 53%

“…In Section 2, we describe the collection and analysis of the data. In Section 3, we describe the transit model fitting; we note the difference in light curve shape compared to the light curve published by Pont et al (2007) in Section 3.3. In Section 4, we present the revised transit ephemeris and discuss how the timing constrains the presence of other objects in the system.…”

Section: Introductionmentioning

confidence: 99%

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TWENTY-ONE NEW LIGHT CURVES OF OGLE-TR-56b: NEW SYSTEM PARAMETERS AND LIMITS ON TIMING VARIATIONS

Adams¹,

López‐Morales²,

Elliot³

et al. 2011

ApJ

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Although OGLE-TR-56b was the second transiting exoplanet discovered, only one light curve, observed in 2006, has been published besides the discovery data. We present 21 light curves of 19 different transits observed between 2003 July and 2009 July with the Magellan Telescopes and Gemini South. The combined analysis of the new light curves confirms a slightly inflated planetary radius relative to model predictions, with R p = 1.378 ± 0.090 R J . However, the values found for the transit duration, semimajor axis, and inclination values differ significantly from the previous result, likely due to systematic errors. The new semimajor axis and inclination, a = 0.01942 ± 0.00015 AU and i = 73.• 72 ± 0.• 18, are smaller than previously reported, while the total duration, T 14 = 7931 ± 38 s, is 18 minutes longer. The transit midtimes have errors from 23 s to several minutes, and no evidence is seen for transit midtime or duration variations. Similarly, no change is seen in the orbital period, implying a nominal stellar tidal decay factor of Q * = 10 7 , with a 3σ lower limit of 10 5.7 .

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Section: Introductionmentioning

confidence: 53%

Section: Introductionmentioning

confidence: 99%

TWENTY-ONE NEW LIGHT CURVES OF OGLE-TR-56b: NEW SYSTEM PARAMETERS AND LIMITS ON TIMING VARIATIONS

Adams¹,

López‐Morales²,

Elliot³

et al. 2011

ApJ

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“…Recent studies have clearly demonstrated that the luminosity in transiting systems can be very well constrained by the LC fitting (Pont et al 2007;Sozzetti et al 2007). However, for CoRoT-7 the shallow transit and the stellar activity result in a large uncertainty on the stellar density and further on the planet radius, so we have abandoned it.…”

Section: Mass Radius and Effective Temperaturementioning

confidence: 99%

Transiting exoplanets from the CoRoT space mission

Léger¹,

Rouan²,

Schneider³

et al. 2009

A&A

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507

378

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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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“…It was used several times in the past to obtain high-precision transit photometry (e.g. Gillon et al 2007bGillon et al , 2009aPont et al 2007). The high-resolution mode and 1×1 binning were used to optimize the spatial sampling, resulting in a 4.6 × 4.6 field of view with a pixel scale of 0.063 /pixel.…”

Section: Vlt/fors2 Transit Photometrymentioning

confidence: 99%

The thermal emission of the young and massive planet CoRoT-2b at 4.5 and 8 μm

Gillon

Lanotte²,

Barman

et al. 2010

A&A

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118

149

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We report measurements of the thermal emission of the young and massive planet CoRoT-2b at 4.5 and 8 μm with the Spitzer Infrared Array Camera (IRAC). Our measured occultation depths are 0.510±0.042% at 4.5 and 0.41±0.11% at 8 μm. In addition to the CoRoT optical measurements, these planet/star flux ratios indicate a poor heat distribution on the night side of the planet and agree better with an atmosphere free of temperature inversion layer. Still, such an inversion is not definitely ruled out by the observations and a larger wavelength coverage is required to remove the current ambiguity. Our global analysis of CoRoT, Spitzer, and ground-based data confirms the high mass and large size of the planet with slightly revised values (M p = 3.47 ± 0.22 M J , R p = 1.466 ± 0.044 R J ). We find a small but significant offset in the timing of the occultation when compared to a purely circular orbital solution, leading to e cos ω = −0.00291 ± 0.00063 where e is the orbital eccentricity and ω is the argument of periastron. Constraining the age of the system to at most a few hundred Myr and assuming that the non-zero orbital eccentricity does not come from a third undetected body, we modeled the coupled orbital-tidal evolution of the system with various tidal Q values, core sizes, and initial orbital parameters. For Q s = 10 5 −10 6 , our modeling is able to explain the large radius of CoRoT-2b if Q p ≤ 10 5.5 through a transient tidal circularization and corresponding planet tidal heating event. Under this model, the planet will reach its Roche limit within 20 Myr at most.

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The “666” collaboration on OGLE transits

Cited by 40 publications

References 25 publications

TWENTY-ONE NEW LIGHT CURVES OF OGLE-TR-56b: NEW SYSTEM PARAMETERS AND LIMITS ON TIMING VARIATIONS

TWENTY-ONE NEW LIGHT CURVES OF OGLE-TR-56b: NEW SYSTEM PARAMETERS AND LIMITS ON TIMING VARIATIONS

Transiting exoplanets from the CoRoT space mission

The thermal emission of the young and massive planet CoRoT-2b at 4.5 and 8 μm

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