SWEET-Cat 2.0: The Cat just got SWEETer

Sousa, S. G.; Adibekyan, V.; Delgado-Mena, E.; Santos, N. C.; Rojas-Ayala, Bárbara; Soares, B. M. T. B.; Legoinha, H.; Ulmer-Moll, S.; Camacho, J. D.; Barros, S. C. C.; Demangeon, O.; Hoyer, S.; Israelian, G.; Mortier, A.; Tsantaki, M.; Monteiro, M. A.

doi:10.1051/0004-6361/202141584

Cited by 58 publications

(48 citation statements)

References 71 publications

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“…We are able to reproduce the oxygen abundance reported in Kolecki & Wang (2021) using their photospheric stellar parameters, our equivalent width measurements, and 3D non-LTE abundance corrections from Amarsi et al (2019). We are therefore confident that the tension between our oxygen abundances results from the photospheric stellar parameters Kolecki & Wang (2021) derived for WASP-77 A that are hotter and more metal-poor than those derived by us, Maxted et al (2013), andMortier et al (2013) as updated by Sousa et al (2021).…”

Section: Elemental Abundancessupporting

confidence: 56%

“…found T eff = 5605 ± 41 K, log g = 4.37 ± 0.09, [Fe/H] = 0.07 ± 0.03, and M * = 0.96 ± 0.07 M . Updated parameters from the same group presented inSousa et al (2021) found T eff = 5595 ± 16 K, log g = 4.41 ± 0.03, [Fe/H] = 0.01 ± 0.01, and M * = 0.915 ± 0.004 M Kolecki & Wang (2021). found T eff = 5660 ± 30 K, log g = 4.49 ± 0.01, and [Fe/H] = −0.15 ± 0.06.…”

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confidence: 99%

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Evidence that the Hot Jupiter WASP-77 A b Formed Beyond Its Parent Protoplanetary Disk's H2O Ice Line

Reggiani,

Schlaufman,

Healy

et al. 2022

Preprint

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Idealized protoplanetary disk and giant planet formation models have been interpreted to suggest that a giant planet's atmospheric abundances can be used to infer its formation location in its parent protoplanetary disk. It has recently been reported that the hot Jupiter WASP-77 A b has sub-solar atmospheric carbon and oxygen abundances with a solar C/O abundance ratio. Assuming solar carbon and oxygen abundances for its host star WASP-77 A, WASP-77 A b's atmospheric carbon and oxygen abundances possibly indicate that it accreted its envelope interior to its parent protoplanetary disk's H 2 O ice line from carbon-depleted gas with little subsequent planetesimal accretion or core erosion. We comprehensively model WASP-77 A and use our results to better characterize WASP-77 A b. We show that the photospheric abundances of carbon and oxygen in WASP-77 A are super-solar with a sub-solar C/O abundance ratio, implying that WASP-77 A b's atmosphere has significantly sub-stellar carbon and oxygen abundances with a super-stellar C/O ratio. Our result possibly indicates that WASP-77 A b's envelope was accreted by the planet beyond its parent protoplanetary disk's H 2 O ice line. While numerous theoretical complications to these idealized models have now been identified, the possibility of non-solar protoplanetary disk abundance ratios confound even the most sophisticated protoplanetary disk and giant planet formation models. We therefore argue that giant planet atmospheric abundance ratios can only be meaningfully interpreted relative to the possibly non-solar mean compositions of their parent protoplanetary disks as recorded in the photospheric abundances of their solar-type dwarf host stars.

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Section: Elemental Abundancessupporting

confidence: 56%

mentioning

confidence: 99%

Evidence that the Hot Jupiter WASP-77 A b Formed Beyond Its Parent Protoplanetary Disk's H2O Ice Line

Reggiani,

Schlaufman,

Healy

et al. 2022

Preprint

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“…For the Northern targets, we used HARPS-N. at TNG (Cosentino et al 2012) for the brightest targets (V<12.5), complementing it with PEPSI at LBT (Strassmeier et al 2003) for fainter targets. Brucalassi et al (2021) The sample presented in B21 was produced by cross-matching the Ariel Reference Sample with the spectra available in the 2020 version of SWEET-Cat (Stars With ExoplanETs Catalogue 2 ), and by selecting all targets in common with parameters' source "flag=1", which are the stars analysed homogeneously (see Santos et al 2013;Sousa et al 2021). The aim of B21 was to re-determine the stellar parameters of the Ariel-SWEET-Cat cross-matched sub-sample using two different methods (FAMA, Fast Automatic MOOG Analysis, Magrini et al 2013), based on the equivalent width, and FASMA (Fast Analysis of Spectra Made Automatically, Tsantaki et al 2018), based on spectral synthesis, and to compare them with the original results of SWEET-Cat.…”

Section: The Samplesmentioning

confidence: 99%

Ariel stellar characterisation

Magrini

Danielski

Bossini

et al. 2022

A&A

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Context. In 2020 the European Space Agency selected Ariel as the next mission to join the space fleet of observatories to study planets outside our Solar System. Ariel will be devoted to the characterisation of a thousand planetary atmospheres, for understanding what exoplanets are made of, how they formed and how they evolve. To achieve the last two goals all planets need to be studied within the context of their own host stars, which in turn have to be analysed with the same technique, in a uniform way. Aims. We present the spectro-photometric method we have developed to infer the atmospheric parameters of the known host stars in the Tier 1 of the Ariel Reference Sample. Methods. Our method is based on an iterative approach, which combines spectral analysis, the determination of the surface gravity from Gaia data, and the determination of stellar masses from isochrone fitting. We validated our approach with the analysis of a control sample, composed by members of three open clusters with well-known ages and metallicities. Results. We measured effective temperature, T eff , surface gravity, log g, and the metallicity, [Fe/H], of 187 F-G-K stars within the Ariel Reference Sample. We presented the general properties of the sample, including their kinematics which allows us to separate them between thin and thick disc populations. Conclusions. A homogeneous determination of the parameters of the host stars is fundamental in the study of the stars themselves and their planetary systems. Our analysis systematically improves agreement with theoretical models and decreases uncertainties in the mass estimate (from 0.21±0.30 to 0.10±0.02 M ), providing useful data for the Ariel consortium and the astronomical community at large.

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“…scaled to that of the star (close to the solar value at [Fe/H] = 0.04 ± 0.01;Sousa et al 2021). This yielded the input elemental abundances of carbon, oxygen, and nitrogen: C/H = 2.69 × 10 −4 , O/H = 5.37 × 10 −4 , and N/H = 7.41 × Article number, page 3 of 9 A&A proofs: manuscript no.…”

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confidence: 92%

CHEOPS geometric albedo of the hot Jupiter HD 209458b

Brandeker,

Heng,

Lendl

et al. 2022

Preprint

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We report the detection of the secondary eclipse of the hot Jupiter HD 209458 b in optical/visible light using the CHEOPS space telescope. Our measurement of 20.4 +3.2 −3.3 parts per million translates into a geometric albedo of A g = 0.096 ± 0.016. The previously estimated dayside temperature of about 1500 K implies that our geometric albedo measurement consists predominantly of reflected starlight and is largely uncontaminated by thermal emission. This makes the present result one of the most robust measurements of A g for any exoplanet. Our calculations of the bandpassintegrated geometric albedo demonstrate that the measured value of A g is consistent with a cloud-free atmosphere, where starlight is reflected via Rayleigh scattering by hydrogen molecules, and the water and sodium abundances are consistent with stellar metallicity. We predict that the bandpass-integrated TESS geometric albedo is too faint to detect and that a phase curve of HD 209458 b observed by CHEOPS would have a distinct shape associated with Rayleigh scattering if the atmosphere is indeed cloud free.

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SWEET-Cat 2.0: The Cat just got SWEETer

Cited by 58 publications

References 71 publications

Evidence that the Hot Jupiter WASP-77 A b Formed Beyond Its Parent Protoplanetary Disk's H2O Ice Line

Evidence that the Hot Jupiter WASP-77 A b Formed Beyond Its Parent Protoplanetary Disk's H2O Ice Line

Ariel stellar characterisation

CHEOPS geometric albedo of the hot Jupiter HD 209458b

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