TOI-220 <i>b</i>: a warm sub-Neptune discovered by<i>TESS</i>

Hoyer, S.; Deleuil, M.; Acuña, L.; Medeiros, J. R. De; Goffo, E.; Lillo-Box, J.; Delgado-Mena, E.; Lopez, T.; Santerne, A.; Sousa, S. G.; Fridlund, M.; Adibekyan, V.; Collins, Karen A.; Serrano, L. M.; Cortés-Zuleta, P.; Howell, Steve B.; Deeg, H. J.; Aguichine, Artyom; Barragán, Oscar; Bryant, Edward M.; Martins, B. L. Canto; Collins, Kevin I.; Cooke, Benjamin F.; Díaz, R. F.; Esposito, M.; Furlan, Elise; Hojjatpanah, S.; Jackman, James A. G.; Jenkins, Jon M.; Jensen, Eric L. N.; Latham, David W.; Leão, I. C.; Matson, Rachel A.; Nielsen, L. D.; Osborn, Ares; Otegi, J. F.; Rodler, F.; Sabotta, S.; Scott, Nicholas J.; Seager, Sara; Stockdale, Chris; Strøm, Paul A.; Vanderspek, R.; Eylen, Vincent Van; Wheatley, P. J.; Winn, Joshua N.; Almenara, J. M.; Barrado, D.; Barros, S. C. C.; Bayliss, Daniel; Bouchy, F.; Boyd, Patricia T.; Cabrera, J.; Cochran, William D.; Doty, J.; Dumusque, X.; Figueira, P.; Fong, William; Grziwa, S.; Hatzes, A. P.; Kabáth, P.; Knudstrup, Emil; Korth, J.; Livingston, John H.; Luque, R.; Mousis, O.; Mullally, Susan E.; Osborn, H.; Πάλλη, Ε.; Persson, C. M.; Redfield, Seth; Santos, N. C.; Smith, Jeffrey C.; Šubjak, J.; Twicken, Joseph D.; Udry, S.; Yahalomi, Daniel A.

doi:10.1093/mnras/stab1427

Monthly Notices of the Royal Astronomical Society

2021

DOI: 10.1093/mnras/stab1427

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TOI-220 b: a warm sub-Neptune discovered byTESS

S. Hoyer

M. Deleuil

L. Acuña

et al.

Abstract: In this paper we report the discovery of TOI-220 b, a new sub-Neptune detected by the Transiting Exoplanet Survey Satellite (TESS) and confirmed by radial velocity follow-up observations with the HARPS spectrograph. Based on the combined analysis of TESS transit photometry and high precision radial velocity measurements we estimate a planetary mass of 13.8 ± 1.0 M⊕ and radius of 3.03 ± 0.15 R⊕, implying a bulk density of 2.73 ± 0.47 g cm−3. TOI-220 b orbits a relative bright (V=10.4) and old (10.1±1.4 Gyr) K … Show more

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Cited by 8 publications

References 91 publications

(79 reference statements)

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SWEET-Cat 2.0: The Cat just got SWEETer

Sousa

Adibekyan

Delgado-Mena

et al. 2021

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Aims. The catalog of Stars With ExoplanETs (SWEET-Cat) was originally introduced in 2013. Since then many more exoplanets have been confirmed, increasing significantly the number of host stars listed there. A crucial step toward a comprehensive understanding of these new worlds is the precise and homogeneous characterization of their host stars. Better spectroscopic stellar parameters along with new results from Gaia eDR3 provide updated and precise parameters for the discovered planets. A new version of the catalog, whose homogeneity in the derivation of the parameters is key to unraveling star-planet connections, is available to the community. Methods. We made use of high-resolution spectra for planet-host stars, either observed by our team or collected through public archives. The spectroscopic stellar parameters were derived for the spectra following the same homogeneous process using ARES and MOOG (ARES+MOOG) as for the previous SWEET-Cat releases. We re-derived parameters for the stars in the catalog using better quality spectra and/or using the most recent versions of the codes. Moreover, the new SWEET-Cat table can now be more easily combined with the planet properties listed both at the Extrasolar Planets Encyclopedia and at the NASA exoplanet archive to perform statistical analyses of exoplanets. We also made use of the recent GAIA eDR3 parallaxes and respective photometry to derive consistent and accurate surface gravity values for the host stars.Results. We increased the number of stars with homogeneous parameters by more than 40% (from 645 to 928). We reviewed and updated the metallicity distributions of stars hosting planets with different mass regimes comparing the low-mass planets (< 30M ⊕ ) with the high-mass planets. The new data strengthen previous results showing the possible trend in the metallicity-period-mass diagram for low-mass planets.

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SWEET-Cat 2.0: The Cat just got SWEETer

Sousa

Adibekyan

Delgado-Mena

et al. 2021

A&A

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The CARMENES search for exoplanets around M dwarfs

Ribas

Reiners

Zechmeister

et al. 2023

A&A

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Context. The CARMENES instrument, installed at the 3.5 m telescope of the Calar Alto Observatory in Almería, Spain, was conceived to deliver high-accuracy radial velocity (RV) measurements with long-term stability to search for temperate rocky planets around a sample of nearby cool stars. Moreover, the broad wavelength coverage was designed to provide a range of stellar activity indicators to assess the nature of potential RV signals and to provide valuable spectral information to help characterise the stellar targets. Aims. We describe the CARMENES guaranteed time observations (GTO), spanning from 2016 to 2020, during which 19 633 spectra for a sample of 362 targets were collected. We present the CARMENES Data Release 1 (DR1), which makes public all observations obtained during the GTO of the CARMENES survey. Methods. The CARMENES survey target selection was aimed at minimising biases, and about 70% of all known M dwarfs within 10 pc and accessible from Calar Alto were included. The data were pipeline-processed, and high-level data products, including 18 642 precise RVs for 345 targets, were derived. Time series data of spectroscopic activity indicators were also obtained. Results. We discuss the characteristics of the CARMENES data, the statistical properties of the stellar sample, and the spectroscopic measurements. We show examples of the use of CARMENES data and provide a contextual view of the exoplanet population revealed by the survey, including 33 new planets, 17 re-analysed planets, and 26 confirmed planets from transiting candidate follow-up. A subsample of 238 targets was used to derive updated planet occurrence rates, yielding an overall average of 1.44 ± 0.20 planets with 1 M⊕ < Mpl sin i < 1000 M⊕ and 1 day < Porb < 1000 days per star, and indicating that nearly every M dwarf hosts at least one planet. All the DR1 raw data, pipeline-processed data, and high-level data products are publicly available online. Conclusions. CARMENES data have proven very useful for identifying and measuring planetary companions. They are also suitable for a variety of additional applications, such as the determination of stellar fundamental and atmospheric properties, the characterisation of stellar activity, and the study of exoplanet atmospheres.

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Interior–atmosphere modelling to assess the observability of rocky planets with JWST

Acuña¹,

Deleuil²,

Mousis³

2023

A&A

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Context. Super-Earths present compositions dominated by refractory materials. However, there is a degeneracy in their interior structure between a planet that has no atmosphere and a small Fe content, and a planet that has a thin atmosphere and a higher core mass fraction. To break this degeneracy, atmospheric characterisation observations are required. Aims. We present a self-consistent interior–atmosphere model to constrain the volatile mass fraction, surface pressure, and temperature of rocky planets with water and CO2 atmospheres. The parameters obtained in our analysis can be used to predict observations in emission spectroscopy and photometry with JWST, which can determine the presence of an atmosphere and, if present, its composition. Methods. We coupled a 1D interior model with a supercritical water layer to an atmospheric model. In order to obtain the bolometric emission and Bond albedo for an atmosphere in radiative-convective equilibrium, we used a low-resolution k-correlated atmospheric model. We generated emission spectra with the same atmospheric model at a higher resolution (R = 200–300). An adaptive Markov chain Monte Carlo was employed for an efficient sampling of the parameter space at low volatile mass fractions. Results. From our interior structure retrieval, we conclude that TRAPPIST-1 c most likely has a bare surface, although the presence of an atmosphere cannot be ruled out. We estimate a 1σ confidence interval of the surface pressure for a water-dominated atmosphere of Psurf = 40 ± 40 bar. We generated spectra for these two scenarios to compare with the emission flux of TRAPPIST-1 c recently observed in the MIRI F1500W filter. This is compatible with bare rock surfaces or a thin atmosphere with little or no CO2. In the case of 55 Cancri e, a combined spectrum with NIRCam and MIRI LRS may present high uncertainties at wavelengths between 3 and 3.7 µm. However, this does not affect the identification of H2O because it does not present spectral features in this wavelength range.

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TOI-220 b: a warm sub-Neptune discovered byTESS

Cited by 8 publications

References 91 publications

SWEET-Cat 2.0: The Cat just got SWEETer

SWEET-Cat 2.0: The Cat just got SWEETer

The CARMENES search for exoplanets around M dwarfs

Interior–atmosphere modelling to assess the observability of rocky planets with JWST

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