Detection of the secondary eclipse of WASP-10b in the<i>K</i>s-band

Cruz, P.; Barrado, D.; Lillo-Box, J.; Diaz, Marcos P.; Birkby, Jayne; López‐Morales, Mercedes; Hodgkin, S. T.; Fortney, Jonathan J.

doi:10.1051/0004-6361/201423509

Cited by 16 publications

(18 citation statements)

References 36 publications

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“…Our new orbital eccentricity of e = 0.0589 +0.0033 −0.0026 differs from our previous value by 4σ; this change can be attributed to the inclusion of our measured secondary eclipse times in the new fits as well as the switch to a curved radial velocity trend model. We note that a previous study reported a detection of the secondary eclipse for this planet in the Ks band at an orbital phase of 0.4972 ± 0.0005 (Cruz et al 2015); this offset differs significantly from that of our Spitzer secondary eclipse observations and is also inconsistent with the current radial velocity measurements for this system. The authors of this study note that their reported error is likely an underestimate as it does not account for additional uncertainties contributed by the removal of systematic noise sources from their light curve.…”

Section: Eclipse Model and Uncertainty Estimatescontrasting

confidence: 99%

“…It is also by far the most massive planet in our sample, a fact that we discuss in more detail below. Although we do not show it in these plots, there is a published Ks (2.1 µm) secondary eclipse measurement available for this planet with a value of 0.137% ± 0.016% (Cruz et al 2015). The measured planet-star flux ratio in this bandpass is 3 − 10× larger than the predictions of our models, and the reported center of eclipse phase differs from our measurement by 2.4 hours (54σ), comparable to the eclipse duration.…”

Section: Day-night Circulationcontrasting

confidence: 67%

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SPITZERSECONDARY ECLIPSE OBSERVATIONS OF FIVE COOL GAS GIANT PLANETS AND EMPIRICAL TRENDS IN COOL PLANET EMISSION SPECTRA

Kammer

Knutson

Line

et al. 2015

ApJ

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In this work we present Spitzer 3.6 and 4.5 µm secondary eclipse observations of five new cool (< 1200 K) transiting gas giant planets: HAT-P-19b, WASP-6b, WASP-10b, WASP-39b, and WASP-67b. We compare our measured eclipse depths to the predictions of a suite of atmosphere models and to eclipse depths for planets with previously published observations in order to constrain the temperature-and mass-dependent properties of gas giant planet atmospheres. We find that the dayside emission spectra of planets less massive than Jupiter require models with efficient circulation of energy to the night side and/or increased albedos, while those with masses greater than that of Jupiter are consistently bestmatched by models with inefficient circulation and low albedos. At these relatively low temperatures we expect the atmospheric CH 4 /CO ratio to vary as a function of metallicity, and we therefore use our observations of these planets to constrain their atmospheric metallicities. We find that the most massive planets have dayside emission spectra that are best-matched by solar metallicity atmosphere models, but we are not able to place strong constraints on metallicities of the smaller planets in our sample. Interestingly, we find that the ratio of the 3.6 and 4.5 µm brightness temperatures for these cool transiting planets is independent of planet temperature, and instead exhibits a tentative correlation with planet mass. If this trend can be confirmed, it would suggest that the shape of these planets' emission spectra depends primarily on their masses, consistent with the hypothesis that lower-mass planets are more likely to have metal-rich atmospheres.

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Section: Eclipse Model and Uncertainty Estimatescontrasting

confidence: 99%

Section: Day-night Circulationcontrasting

confidence: 67%

SPITZERSECONDARY ECLIPSE OBSERVATIONS OF FIVE COOL GAS GIANT PLANETS AND EMPIRICAL TRENDS IN COOL PLANET EMISSION SPECTRA

Kammer

Knutson

Line

et al. 2015

ApJ

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“…This survey has already confirmed the A&A 576, A88 (2015) planetary nature of Kepler-91b (KOI-2133b, Lillo-Box et al 2014c, Kepler-432b (KOI-1299b, Ciceri et al 2015, and Kepler-447b (KOI-1800b; and has detected the secondary eclipse of WASP-10b (Cruz et al 2015). In the present paper, we analyze 13 specific candidates in our sample that have shown either large RV variations or broadened spectra owing to the fast rotation of the host stars.…”

Section: Introductionmentioning

confidence: 71%

Eclipsing binaries and fast rotators in theKeplersample

Lillo-Box

Barrado

Mancini

et al. 2015

A&A

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Context. The Kepler mission has searched for planetary transits in more than two hundred thousand stars by obtaining very accurate photometric data over a long period of time. Among the thousands of detected candidates, the planetary nature of around 15% has been established or validated by different techniques. But additional data are needed to characterize the rest of the candidates and reject other possible configurations. Aims. We started a follow-up program to validate, confirm, and characterize some of the planet candidates. In this paper we present the radial velocity analysis of those that present large variations, which are compatible with being eclipsing binaries. We also study those showing high rotational velocities, which prevents us from reaching the necessary precision to detect planetary-like objects. Methods. We present new radial velocity results for 13 Kepler objects of interest (KOIs) obtained with the CAFE spectrograph at the Calar Alto Observatory and analyze their high-spatial resolution (lucky) images obtained with AstraLux and the Kepler light curves of some interesting cases. Results. We have found five spectroscopic and eclipsing binaries (group A). Among them, the case of KOI-3853 is of particular interest. This system is a new example of the so-called heartbeat stars, showing dynamic tidal distortions in the Kepler light curve. We have also detected duration and depth variations of the eclipse. We suggest possible scenarios to explain such an effect, including the presence of a third substellar body possibly detected in our radial velocity analysis. We also provide upper mass limits to the transiting companions of six other KOIs with high rotational velocities (group B). This property prevents the radial velocity method from achieving the necessary precision to detect planetary-like masses. Finally, we analyze the large radial velocity variations of two other KOIs, which are incompatible with the presence of planetary-mass objects (group C). These objects are likely to be stellar binaries. However, a longer timespan is needed to complete their characterization.

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“…−131 K (Cruz et al 2015). The maximum expected equilibrium temperature for the planet, assuming zero Bond albedo and instant reradiation (A B = 0 and f = 2/3, respectively) is T eq 1224 K. This temperature is about 25% cooler than the observed T Ks .…”

Section: Estimated Thermal Emissionmentioning

confidence: 76%

“…We fit for these systematics simultaneously by performing a multiple linear regression, where we modeled the trends only on the out-of-eclipse portions of the light curve, applied the model to the in-eclipse portion, and removed it from the light curve. The complete description of the reduction procedure and analysis performed can be found in Cruz et al (2015).…”

Section: The Case Study: Wasp-10bmentioning

confidence: 99%

Detection of secondary eclipses of WASP-10b and Qatar-1b in the Ks band and the correlation between Ks-band temperature and stellar activity.

et al. 2016

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The Calar Alto Secondary Eclipse study was a program dedicated to observe secondary eclipses in the near-IR of two known close-orbiting exoplanets around K-dwarfs: WASP-10b and Qatar-1b. Such observations reveal hints on the orbital configuration of the system and on the thermal emission of the exoplanet, which allows the study of the brightness temperature of its atmosphere. The observations were performed at the Calar Alto Observatory (Spain). We used the OMEGA2000 instrument (Ks band) at the 3.5m telescope. The data was acquired with the telescope strongly defocused. The differential light curve was corrected from systematic effects using the Principal Component Analysis (PCA) technique. The final light curve was fitted using an occultation model to find the eclipse depth and a possible phase shift by performing a MCMC analysis. The observations have revealed a secondary eclipse of WASP-10b with depth of 0.137%, and a depth of 0.196% for Qatar-1b. The observed phase offset from expected mid-eclipse was of −0.0028 for WASP-10b, and of −0.0079 for Qatar-1b. These measured offsets led to a value for |ecosω| of 0.0044 for the WASP-10b system, leading to a derived eccentricity which was too small to be of any significance. For Qatar-1b, we have derived a |ecosω| of 0.0123, however, this last result needs to be confirmed with more data. The estimated Ks-band brightness temperatures are of 1647 K and 1885 K for WASP-10b and Qatar-1b, respectively. We also found an empirical correlation between the (R′HK) activity index of planet hosts and the Ks-band brightness temperature of exoplanets, considering a small number of systems.

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Detection of the secondary eclipse of WASP-10b in theKs-band

Cited by 16 publications

References 36 publications

SPITZERSECONDARY ECLIPSE OBSERVATIONS OF FIVE COOL GAS GIANT PLANETS AND EMPIRICAL TRENDS IN COOL PLANET EMISSION SPECTRA

SPITZERSECONDARY ECLIPSE OBSERVATIONS OF FIVE COOL GAS GIANT PLANETS AND EMPIRICAL TRENDS IN COOL PLANET EMISSION SPECTRA

Eclipsing binaries and fast rotators in theKeplersample

Detection of secondary eclipses of WASP-10b and Qatar-1b in the Ks band and the correlation between Ks-band temperature and stellar activity.

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