CONSTRAINTS ON THE ATMOSPHERIC CIRCULATION AND VARIABILITY OF THE ECCENTRIC HOT JUPITER XO-3b

Wong, Ian; Knutson, Heather A.; Cowan, Nicolas B.; Lewis, Nikole K.; Agol, Eric; Burrows, Adam; Deming, Drake; Fortney, Jonathan J.; Fulton, Benjamin J.; Langton, Jonathan; Laughlin, Gregory; Showman, Adam P.

doi:10.1088/0004-637x/794/2/134

Cited by 66 publications

(72 citation statements)

References 48 publications

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“…−4 days −1 (Wong et al 2014). Here we compare our results with the ones reported in Wong et al (2014).…”

Section: -+ ×10mentioning

confidence: 95%

“…The eclipse depth is defined as the (unseen) planetʼs flux at the center of eclipse, in units of stellar flux (see Figure 1). When fitting the eclipse models, the orbital parameters are fixed to the values reported in Table 2, taken from Wong et al (2014), while the center of eclipse, eclipse depth, and phase constant are free parameters to determine. We also considered models with zero phase curveʼs slope (see Appendix A.5).…”

Section: The Eclipse Modelmentioning

confidence: 99%

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Repeatability of Spitzer/Irac Exoplanetary Eclipses With Independent Component Analysis

Morello

Waldmann

Tinetti

2016

ApJ

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The research of effective and reliable detrending methods for Spitzer data is of paramount importance for the characterization of exoplanetary atmospheres. To date, the totality of exoplanetary observations in the mid-and farinfrared, at wavelengths >3 μm, have been taken with Spitzer. In some cases, in past years, repeated observations and multiple reanalyses of the same data sets led to discrepant results, raising questions about the accuracy and reproducibility of such measurements. Morello et al. (2014Morello et al. ( , 2015 proposed a blind-source separation method based on the Independent Component Analysis of pixel time series (pixel-ICA) to analyze InfraRed Array Camera (IRAC) data, obtaining coherent results when applied to repeated transit observations previously debated in the literature. Here we introduce a variant to the pixel-ICA through the use of wavelet transform, wavelet pixel-ICA, which extends its applicability to low-signal-to-noise-ratio cases. We describe the method and discuss the results obtained over 12 eclipses of the exoplanet XO3b observed during the "Warm Spitzer" era in the 4.5 μm band. The final results are reported, in part, also in Ingalls et al. ), which appeared on arXiv while this paper was under review. Based on many statistical tests discussed in Ingalls et al. (2016), the wavelet pixel-ICA method performs as well as or better than other state-of-art methods recently developed by other teams to analyze Spitzer/IRAC data, and, in particular, it appears to be the most repeatable and the most reliable, while reaching the photon noise limit, at least for the particular data set analyzed. Another strength of the ICA approach is its highest objectivity, as it does not use prior information about the instrument systematics, making it a promising method to analyze data from other observatories. The selfconsistency of individual measurements of eclipse depth and phase curve slope over a span of more than three years proves the stability of Warm Spitzer/IRAC photometry within the error bars, at the level of 1 part in 10 4 in stellar flux.

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“…−4 days −1 (Wong et al 2014). Here we compare our results with the ones reported in Wong et al (2014).…”

Section: -+ ×10mentioning

confidence: 95%

Section: The Eclipse Modelmentioning

confidence: 99%

Repeatability of Spitzer/Irac Exoplanetary Eclipses With Independent Component Analysis

Morello

Waldmann

Tinetti

2016

ApJ

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“…We also tried decorrelating instrumental noise in our data using pixel mapping (e.g., Ballard et al 2010;Lewis et al 2013;Wong et al 2014). This nonparametric technique constructs an empirical map of the pixel response across the chip by comparing the measured flux from each image to those of other images with similar stellar positions.…”

Section: Instrumental Noise Model and Optimal Aperture Selectionmentioning

confidence: 99%

“…We also directly compare the performance of PLD for cases where we fit to either the unbinned or optimally binned photometry, as well as to the fit acquired from photometry using the Wong et al (2014) pixel mapping technique described in the previous paragraph. We find thatthe optimally binned PLD haslower levels of correlated noise than the other methods ( Figure 1).…”

Section: Instrumental Noise Model and Optimal Aperture Selectionmentioning

confidence: 99%

Dynamical Constraints on the Core Mass of Hot Jupiter Hat-P-13b

Buhler

Knutson

Batygin

et al. 2016

ApJ

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HAT-P-13b is a Jupiter-mass transiting exoplanet that has settled onto a stable, short-period, and mildly eccentric orbit as a consequence of the action of tidal dissipation and perturbations from a second, highly eccentric, outer companion. Owingto the special orbital configuration of the HAT-P-13 system, the magnitude of HAT-P-13bʼs eccentricity (e b ) is in part dictated by its Love number (k 2 b ), which is in turn a proxy for the degree of central mass concentration in its interior. Thus, the measurement of e b constrains k 2 b and allows us to place otherwise elusive constraints on the mass of HAT-P-13bʼs core (M core,b ). In this study we derive new constraints on the value of e b by observing two secondary eclipses of HAT-P-13b with the Infrared Array Camera on board the Spitzer Space Telescope. We fit the measured secondary eclipse times simultaneously with radial velocity measurements and find that e b =0.00700±0.00100. We then use octupole-order secular perturbation theory to find the corresponding = Applying structural evolution models, we then find, with 68% confidence, that M core,b is less than 25 Earth masses (M ⊕ ). The most likely value isM core,b =11 M ⊕ , which is similar to the core mass theoretically required for runaway gas accretion. This is the tightest constraint to date on the core mass of a hot Jupiter. Additionally, we find that the measured secondary eclipse depths, which are in the 3.6 and 4.5 μm bands, best match atmospheric model predictions with a dayside temperature inversion and relatively efficient day-night circulation.

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“…Thus they can tell us about the dynamics of giant-planet atmospheres (e.g., Wong et al 2014 and references therein).…”

Section: A Massive Planet In An Eccentric Orbitmentioning

confidence: 99%

THREE WASP-SOUTH TRANSITING EXOPLANETS: WASP-74b, WASP-83b, AND WASP-89b

Hellier

Anderson

Cameron

et al. 2015

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We report the discovery of three new transiting hot Jupiters by WASP-South together with the TRAPPIST photometer and the Euler/CORALIE spectrograph. WASP-74b orbits a star of V = 9.7, making it one of the brighter systems accessible to southern telescopes. It is a 0.95M Jup planet with a moderately bloated radius of 1.5 R Jup in a 2 day orbit around a slightly evolved F9 star. WASP-83b is a Saturn-mass planet at 0.3 M Jup with a radius of 1.0 R Jup . It is in a 5 day orbit around a fainter (V = 12.9) G8 star. WASP-89b is a 6 M Jup planet in a 3 day orbit with an eccentricity of e = 0.2. It is thus similar to massive, eccentric planets such as XO-3b and HAT-P-2b, except that those planets orbit F stars whereas WASP-89 is a K star. The V = 13.1 host star is magnetically active, showing a rotation period of 20.2 days, while star spots are visible in the transits. There are indications that the planet's orbit is aligned with the stellar spin. WASP-89 is a good target for an extensive study of transits of star spots.

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CONSTRAINTS ON THE ATMOSPHERIC CIRCULATION AND VARIABILITY OF THE ECCENTRIC HOT JUPITER XO-3b

Cited by 66 publications

References 48 publications

Repeatability of Spitzer/Irac Exoplanetary Eclipses With Independent Component Analysis

Repeatability of Spitzer/Irac Exoplanetary Eclipses With Independent Component Analysis

Dynamical Constraints on the Core Mass of Hot Jupiter Hat-P-13b

THREE WASP-SOUTH TRANSITING EXOPLANETS: WASP-74b, WASP-83b, AND WASP-89b

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