Three irradiated and bloated hot Jupiters:

West, R. G.; Hellier, C.; Almenara, J. M.; Anderson, D. R.; Barros, S. C. C.; Bouchy, F.; Brown, D. J. A.; Cameron, A. Collier; Deleuil, M.; Delrez, Laetitia; Doyle, A. P.; Faedi, F.; Fumel, A.; Gillon, M.; Chew, Y. Gómez Maqueo; Hébrard, G.; Jehin, Emmanuël; Lendl, M.; Maxted, P. F. L.; Pepe, F.; Pollacco, D.; Queloz, D.; Ségransan, D.; Smalley, B.; Smith, A. M. S.; Southworth, J.; Triaud, A. H. M. J.; Udry, S.

doi:10.1051/0004-6361/201527276

Cited by 110 publications

(86 citation statements)

References 36 publications

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“…With a revised stellar radius of 1.969 ± 0.035 R (compared to 1.7 ± 0.03 R , Brown et al 2017), we find a ∼20% larger planetary radius of 2.078 +0.036 −0.044 R J (compared to 1.73 ± 0.03 R J ). As already suggested by Brown et al (2017), we find a larger impact parameter compared to that stated in the discovery paper (West et al 2016). A full list of the derived stellar and planetary parameters is given in Fig.…”

Section: Simultaneous Photometry With Eulercamsupporting

confidence: 83%

Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS)

Seidel

Ehrenreich

Wyttenbach

et al. 2019

A&A

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High-resolution optical spectroscopy is a powerful tool to characterise exoplanetary atmospheres from the ground. The sodium D lines, with their large cross sections, are especially suited to studying the upper layers of atmospheres in this context. We report on the results from Hot Exoplanet Atmosphere Resolved with Transit Spectroscopy survey (HEARTS), a spectroscopic survey of exoplanet atmospheres, performing a comparative study of hot gas giants to determine the effects of stellar irradiation. In this second installation of the series, we highlight the detection of neutral sodium on the ultra-hot giant WASP-76b. We observed three transits of the planet using the High-Accuracy Radial-velocity Planet Searcher (HARPS) high-resolution spectrograph at the European Southern Observatory (ESO) 3.6 m telescope and collected 175 spectra of WASP-76. We repeatedly detect the absorption signature of neutral sodium in the planet atmosphere (0.371 ± 0.034%; 10.75σ in a 0.75 Å passband). The sodium lines have a Gaussian profile with full width at half maximum (FWHM) of 27.6 ± 2.8 km s−1. This is significantly broader than the line spread function of HARPS (2.7 km s−1). We surmise that the observed broadening could trace the super-rotation in the upper atmosphere of this ultra-hot gas giant.

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Section: Simultaneous Photometry With Eulercamsupporting

confidence: 83%

Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS)

Seidel

Ehrenreich

Wyttenbach

et al. 2019

A&A

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132

173

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“…Our derived distances are listed in Table 4, available electronically from the CDS, and are generally within 2σ of the previously reported values. Notably different distances are those for WASP-66 and WASP-67, for which we find 520±30 pc and 184 ± 6 pc respectively, compared to 380 ± 100 and 255 ± 45 given by Hellier et al (2012); WASP-90, which we find to be at 211 ± 10 compared to 340 ± 60 by West et al (2016); and OGLE-TR-113, which we place at 358±19 pc, much closer than the previously reported distances of 600 pc by Konacki et al (2004) and 553 pc by Santos et al (2006).…”

Section: Host Star Distancescontrasting

confidence: 65%

High-resolution Imaging of Transiting Extrasolar Planetary systems (HITEP)

Evans

Southworth

Maxted

et al. 2016

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Context. Wide binaries are a potential pathway for the formation of hot Jupiters. The binary fraction among host stars is an important discriminator between competing formation theories, but has not been well characterised. Additionally, contaminating light from unresolved stars can significantly affect the accuracy of photometric and spectroscopic measurements in studies of transiting exoplanets. Aims. We observed 101 transiting exoplanet host systems in the Southern hemisphere in order to create a homogeneous catalogue of both bound companion stars and contaminating background stars, in an area of the sky where transiting exoplanetary systems have not been systematically searched for stellar companions. We investigate the binary fraction among the host stars in order to test theories for the formation of hot Jupiters. Methods. Lucky imaging observations from the Two Colour Instrument on the Danish 1.54 m telescope at La Silla were used to search for previously unresolved stars at small angular separations. The separations and relative magnitudes of all detected stars were measured. For 12 candidate companions to 10 host stars, previous astrometric measurements were used to evaluate how likely the companions are to be physically associated. Results. We provide measurements of 499 candidate companions within 20 arcsec of our sample of 101 planet host stars. 51 candidates are located within 5 arcsec of a host star, and we provide the first published measurements for 27 of these. Calibrations for the plate scale and colour performance of the Two Colour Instrument are presented. Conclusions. We find that the overall multiplicity rate of the host stars is 38 +17 −13 %, consistent with the rate among solar-type stars in our sensitivity range, suggesting that planet formation does not preferentially occur in long period binaries compared to a random sample of field stars. Long period stellar companions (P > 10 yr) appear to occur independently of short period companions, and so the population of close-in stellar companions is unconstrained by our study.

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“…We looked at the confirmed planets list from the NASA Exoplanet Archive 3 , and found that EPIC 229426032 b falls into a region of highly inflated hot Jupiters that is as yet not very well populated. We also compared the planet with other cases of highly inflated hot Jupiters, like WASP-17 b (Anderson et al 2010), WASP-82 b (West et al 2016), and WASP-12 b (Hebb et al 2009). These planets have shown to be good cases to perform atmospheric studies, which makes EPIC 229426032 b a good laboratory for studying the atmospheres of highly inflated planets as well.…”

Section: Discussionmentioning

confidence: 99%

K2-237 b and K2-238 b: discovery and characterization of two new transiting hot Jupiters from K2

Soto

Díaz

Jenkins

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We report the discovery of two hot Jupiters orbiting the stars EPIC229426032 and EPIC246067459. We used photometric data from Campaign 11 and 12 of the Kepler K2 Mission and radial velocity data obtained using the HARPS, FEROS, and CORALIE spectrographs. EPIC229426032 b and EPIC246067459 b have masses of 1.60 +0.11 −0.11 and 0.86 +0.13 −0.12 M Jup , radii of 1.65 +0.07 −0.08 and 1.30 +0.15 −0.14 R Jup , and are orbiting their host stars in 2.18 and 3.20-day orbits, respectively. The large radius of EPIC229426032 b leads us to conclude that this candidate corresponds to a highly inflated hot Jupiter. EPIC2460674559 b has a radius consistent with theoretical models, considering the high incident flux falling on the planet. We consider EPIC229426032 b to be a excellent system for follow-up studies, since not only is it very inflated, but it also orbits a relatively bright star (V = 11.6).

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Three irradiated and bloated hot Jupiters:

Cited by 110 publications

References 36 publications

Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS)

Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS)

High-resolution Imaging of Transiting Extrasolar Planetary systems (HITEP)

K2-237 b and K2-238 b: discovery and characterization of two new transiting hot Jupiters from K2

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