THE OPTICAL AND NEAR-INFRARED TRANSMISSION SPECTRUM OF THE SUPER-EARTH GJ 1214b: FURTHER EVIDENCE FOR A METAL-RICH ATMOSPHERE

Bean, Jacob L.; Désert, Jean-Michel; Kabáth, P.; Stalder, B.; Seager, Sara; Kempton, Eliza M.-R.; Berta, Zachory K.; Homeier, D.; Walsh, Shane; Seifahrt, Andreas

doi:10.1088/0004-637x/743/1/92

Cited by 216 publications

(298 citation statements)

References 33 publications

(87 reference statements)

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“…Also, day-side spectral features may be absent due to an isothermal pressuretemperature profile (Fortney et al 2006). These planets are consistent with other transiting exoplanet observations with flat spectra in optical wavelengths on TrES-3b , GJ 3470b (a hot Uranus; Biddle et al 2014), GJ 1214b (Bean et al 2011;Kreidberg et al 2014), WASP-29b (Gibson et al 2013a), and HAT-P-32b (Gibson et al 2013b).…”

Section: Wavelength Dependence On the Planetary Radiussupporting

confidence: 90%

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.

102

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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: Wavelength Dependence On the Planetary Radiussupporting

confidence: 90%

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.

102

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“…Such observations have benefited not only from advances in observing strategy, but also from the availability of new bright targets with nearby comparison stars. Similar observations have since been made in the NIR (Bean et al 2011) and with long-slit spectrographs ). Here we report Gemini observations of WASP-29 using this MOS technique.…”

Section: Introductionsupporting

confidence: 77%

A Gemini ground-based transmission spectrum of WASP-29b: a featureless spectrum from 515 to 720 nm

Gibson¹,

Aigrain²,

Barstow³

et al. 2012

Monthly Notices of the Royal Astronomical Society

137

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We report Gemini-South GMOS observations of the exoplanet system WASP-29 during primary transit as a test case for differential spectrophotometry. We use the multi-object spectrograph to observe the target star and a comparison star simultaneously to produce multiple light curves at varying wavelengths. The 'white' light curve and fifteen 'spectral' light curves are analysed to refine the system parameters and produce a transmission spectrum from ∼515 to 720 nm. All light curves exhibit time-correlated noise, which we model using a variety of techniques. These include a simple noise rescaling, a Gaussian process model, and a wavelet based method. These methods all produce consistent results, although with different uncertainties. The precision of the transmission spectrum is improved by subtracting a common signal from all the spectral light curves, reaching a typical precision of ∼1×10 −4 in transit depth. The transmission spectrum is free of spectral features, and given the non-detection of a pressure broadened Na feature, we can rule out the presence of a Na rich atmosphere free of clouds or hazes, although we cannot rule out a narrow Na core. This indicates that Na is not present in the atmosphere, and/or that clouds/hazes play a significant role in the atmosphere and mask the broad wings of the Na feature, although the former is a more likely explanation given WASP-29b's equilibrium temperature of ∼970 K, at which Na can form various compounds. We also briefly discuss the use of Gaussian process and wavelet methods to account for time correlated noise in transit light curves.

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“…If the planet is transiting and the parent star is bright, then the planetary atmosphere can be probed by transmission spectroscopy (e.g. GJ 1214 b: Croll et al 2011;Crossfield et al 2011;Bean et al 2011;Berta et al 2012;Colòn & Gaidos 2013;GJ 3470 b: Crossfield et al 2013;GJ 436 b: Pont et al 2009;Gibson et al 2011), transmission photometry (e.g. GJ 1214 b: de Mooij et al 2012;Murgas et al 2012;de Mooij et al 2013;Narita et al 2013;GJ 3470 b: Nascimbeni et al 2013) and observations of secondary eclipses A&A 562, A126 (2014) 7, 11, 20 5.14 Notes.…”

Section: Introductionmentioning

confidence: 99%

Physical properties and transmission spectrum of the WASP-80 planetary system from multi-colour photometry

Mancini

Southworth

Ciceri

et al. 2014

A&A

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WASP-80 is one of only two systems known to contain a hot Jupiter which transits its M-dwarf host star. We present eight light curves of one transit event, obtained simultaneously using two defocussed telescopes. These data were taken through the Bessell I, Sloan g r i z and near-infrared JHK passbands. We use our data to search for opacity-induced changes in the planetary radius, but find that all values agree with each other. Our data are therefore consistent with a flat transmission spectrum to within the observational uncertainties. We also measure an activity index of the host star of log R HK = −4.495, meaning that WASP-80 A shows strong chromospheric activity. The non-detection of starspots implies that, if they exist, they must be small and symmetrically distributed on the stellar surface. We model all available optical transit light curves and obtain improved physical properties and orbital ephemerides for the system.

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THE OPTICAL AND NEAR-INFRARED TRANSMISSION SPECTRUM OF THE SUPER-EARTH GJ 1214b: FURTHER EVIDENCE FOR A METAL-RICH ATMOSPHERE

Cited by 216 publications

References 33 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

A Gemini ground-based transmission spectrum of WASP-29b: a featureless spectrum from 515 to 720 nm

Physical properties and transmission spectrum of the WASP-80 planetary system from multi-colour photometry

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