Comprehensive time series analysis of the transiting extrasolar planet WASP-33b

Kovács, G.; Hartman, J. D.; Bakos, G. Á.; Bieryla, Allyson; Latham, David W.; Noyes, R. W.; Regály, Zs.; Esquerdo, Gilbert A.

doi:10.1051/0004-6361/201219642

Cited by 45 publications

(70 citation statements)

References 51 publications

(65 reference statements)

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“…The light-curve solution (Table 9) and derived physical parameters (Table 14) are consistent with previous studies (e.g. Collier Cameron et al 2010;Kovács et al 2013;von Essen et al 2014). We find a near-UV R p /R * = 0.1086 +0.0022 −0.0007 , which is consistent with its optical R p /R * = 0.1066±0.0009 (Collier Cameron et al 2010).…”

Section: Wasp-33bsupporting

confidence: 91%

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Ground-based near-UV observations of 15 transiting exoplanets: constraints on their atmospheres and no evidence for asymmetrical transits

Turner

Pearson

Biddle

et al. 2016

Mon. Not. R. Astron. Soc.

107

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Transits of exoplanets observed in the near-UV have been used to study the scattering properties of their atmospheres and possible star-planet interactions. We observed the primary transits of 15 exoplanets (CoRoT-1b, GJ436b, HAT-P-1b, HAT-P-13b, HAT-P-16b, HAT-P-22b, TrES2b, in the near-UV and several optical photometric bands to update their planetary parameters, ephemerides, search for a wavelength dependence in their transit depths to constrain their atmospheres, and determine if asymmetries are visible in their light curves. Here, we present the first ground-based near-UV light curves for 12 of the targets (CoRoT1b, GJ436b, HAT-P-1b, HAT-P-13b, HAT-P-22b, TrES-2b, TrES-4b, WASP-1b, WASP-33b, WASP-36b, WASP-48b, and WASP-77Ab). We find that none of the near-UV transits exhibit any non-spherical asymmetries, this result is consistent with recent theoretical predictions by Ben-Jaffel et al. and Turner et al. The multiwavelength photometry indicates a constant transit depth from near-UV to optical wavelengths in 10 targets (suggestive of clouds), and a varying transit depth with wavelength in 5 targets (hinting at Rayleigh or aerosol scattering in their atmospheres). We also present the first detection of a smaller near-UV transit depth than that measured in the optical in WASP-1b and a possible opacity source that can cause such radius variations is currently unknown. WASP-36b also exhibits a smaller near-UV transit depth at

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Section: Wasp-33bsupporting

confidence: 91%

“…References. -(1) Gillon et al (2009) Kovács et al (2013); (12) Smith et al (2012); (13) Mancini et al (2013); (14) Enoch et al (2011); (15) Maxted et al (2013). …”

Section: Exomop Analysis Of the Systemsmentioning

confidence: 99%

Ground-based near-UV observations of 15 transiting exoplanets: constraints on their atmospheres and no evidence for asymmetrical transits

Turner

Pearson

Biddle

et al. 2016

Mon. Not. R. Astron. Soc.

107

View full text Add to dashboard Cite

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“…While our residuals clearly show unaccounted pulsations, we do not see any such hump recurring at the same phase. Therefore we find no evidence for a persistent structure on the stellar surface like, e.g., a spot belt as suggested by Kovács et al (2013).…”

Section: Transit Modelingcontrasting

confidence: 53%

“…We caution, however, that the observed trend may be feigned by an inappropriate transit normalization because many transits lack full observational coverage. Kovács et al (2013) also notice a substantial difference in the transit depth derived from an observation in Hα and a simultaneously obtained J-band light curve (their Fig. 9).…”

Section: Wavelength Dependence Of the Planet-to-star Radius Ratiomentioning

confidence: 91%

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Pulsation analysis and its impact on primary transit modeling in WASP-33

Essen

Czesla

Wolter

et al. 2013

A&A

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Aims. To date, WASP-33 is the only δ Scuti star known to be orbited by a hot Jupiter. The pronounced stellar pulsations, showing periods comparable to the primary transit duration, interfere with the transit modeling. Therefore our main goal is to study the pulsation spectrum of the host star to redetermine the orbital parameters of the system by means of pulsation-cleaned primary transit light curves. Methods. Between August 2010 and October 2012 we obtained 457 h of photometry of WASP-33 using small and middle-class telescopes located mostly in Spain and in Germany. Our observations comprise the wavelength range between the blue and the red, and provide full phase coverage of the planetary orbit. After a careful detrend, we focus our pulsation studies in the high frequency regime, where the pulsations that mostly deform the primary transit exist. Results. The data allow us to identify, for the first time in the system, eight significant pulsation frequencies. The pulsations are likely associated with low-order p-modes. Furthermore, we find that pulsation phases evolve in time. We use our knowledge of the pulsations to clean the primary transit light curves and carry out an improved transit modeling. Surprisingly, taking into account the pulsations in the modeling has little influence on the derived orbital parameters. However, the uncertainties in the best-fit parameters decrease. Additionally, we find indications for a possible dependence between wavelength and transit depth, but only with marginal significance. A clear pulsation solution, in combination with an accurate orbital period, allows us to extend our studies and search for star-planet interactions (SPI). Although we find no conclusive evidence of SPI, we believe that the pulsation nature of the host star and the proximity between members make WASP-33 a promising system for further SPI studies.

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A lower radius and mass for the transiting extrasolar planet HAT-P-8 b

Mancini

Southworth

Ciceri

et al. 2013

A&A

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Context. The extrasolar planet HAT-P-8 b was thought to be one of the more inflated transiting hot Jupiters. Aims. By using new and existing photometric data, we computed precise estimates of the physical properties of the system. Methods. We present photometric observations comprising eleven light curves covering six transit events, obtained using five mediumclass telescopes and telescope-defocussing technique. One transit was simultaneously obtained through four optical filters, and two transits were followed contemporaneously from two observatories. We modelled these and seven published datasets using the jktebop code. The physical parameters of the system were obtained from these results and from published spectroscopic measurements. In addition, we investigated the theoretically-predicted variation of the apparent planetary radius as a function of wavelength, covering the range 330-960 nm. Results. We find that HAT-P-8 b has a significantly lower radius (1.321 ± 0.037 R Jup ) and mass (1.275 ± 0.053 M Jup ) compared to previous estimates (1.50 +0.08 −0.06 R Jup and 1.52 +0.18 −0.16 M Jup respectively). We also detect a radius variation in the optical bands that, when compared with synthetic spectra of the planet, may indicate the presence of a strong optical absorber, perhaps TiO and VO gases, near the terminator of HAT-P-8 b.Conclusions. These new results imply that HAT-P-8 b is not significantly inflated, and that its position in the planetary mass-radius diagram is congruent with those of many other transiting extrasolar planets.

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Comprehensive time series analysis of the transiting extrasolar planet WASP-33b

Cited by 45 publications

References 51 publications

Ground-based near-UV observations of 15 transiting exoplanets: constraints on their atmospheres and no evidence for asymmetrical transits

Ground-based near-UV observations of 15 transiting exoplanets: constraints on their atmospheres and no evidence for asymmetrical transits

Pulsation analysis and its impact on primary transit modeling in WASP-33

A lower radius and mass for the transiting extrasolar planet HAT-P-8 b

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