The planetary system around HD 190622 (TOI-1054): Measuring the gas content of low-mass planets orbiting F-stars

J. Cabrera; D. Gandolfi; L. M. Serrano; Sz Csizmadia; J. A. Egger; Ph Baumeister; A. Krenn; W. Benz; A. Deline; H. G. Florén; A. Collier Cameron; V. Adibekyan; Y. Alibert; S. E. Bellomo; L. Delrez; L. Fossati; A. Fortier; S. Grziwa; S. Hoyer; A. Bonfanti; S. Salmon; S. G. Sousa; T. G. Wilson; J. Alarcón; R. Alonso; G. Anglada Escudé; T. Bárczy; O. Barragán; D. Barrado; S. C.C. Barros; W. Baumjohann; M. Beck; T. Beck; L. M. Bernabò; N. Billot; X. Bonfils; L. Borsato; A. Brandeker; C. Broeg; O. Carrión-González; S. Charnoz; D. R. Ciardi; W. D. Cochran; K. A. Collins; K. I. Collins; D. M. Conti; M. B. Davies; H. J. Deeg; M. Deleuil; O. D.S. Demangeon; B. O. Demory; D. Ehrenreich; A. Erikson; M. Esposito; M. Fridlund; M. Gillon; E. Goffo; M. Güdel; E. W. Guenther; J. V. Harre; K. Heng; M. J. Hooton; K. G. Isaak; J. M. Jenkins; L. L. Kiss; E. Knudstrup; K. W.F. Lam; J. Laskar; A. Lecavelier Des Etangs; M. Lendl; C. Lovis; R. Luque; D. Magrin; P. F.L. Maxted; A. Muresan; V. Nascimbeni; G. Olofsson; H. P. Osborn; H. L.M. Osborne; R. Ottensamer; I. Pagano; E. Pallé; C. M. Persson; G. Peter; G. Piotto; D. Pollacco; D. Queloz; R. Ragazzoni; N. Rando; H. Rauer; S. Redfield; I. Ribas; G. R. Ricker; F. Rodler; N. C. Santos; G. Scandariato; S. Seager; D. Ségransan; A. E. Simon; A. M.S. Smith; M. Steller; Gy M. Szabó; N. Thomas; N. Tosi; J. D. Twicken; S. Udry; V. Van Eylen; V. Van Grootel; N. A. Walton; J. N. Winn

doi:10.1051/0004-6361/202245774

The planetary system around HD 190622 (TOI-1054): Measuring the gas content of low-mass planets orbiting F-stars

J. Cabrera, D. Gandolfi, L. M. Serrano, Sz Csizmadia, J. A. Egger, Ph Baumeister, A. Krenn, W. Benz, A. Deline, H. G. Florén, A. Collier Cameron, V. Adibekyan, Y. Alibert, S. E. Bellomo, L. Delrez, L. Fossati, A. Fortier, S. Grziwa, S. Hoyer, A. BonfantiS. Salmon, S. G. Sousa, T. G. Wilson, J. Alarcón, R. Alonso, G. Anglada Escudé, T. Bárczy, O. Barragán, D. Barrado, S. C.C. Barros, W. Baumjohann, M. Beck, T. Beck, L. M. Bernabò, N. Billot, X. Bonfils, L. Borsato, A. Brandeker, C. Broeg, O. Carrión-González, S. Charnoz, D. R. Ciardi, W. D. Cochran, K. A. Collins, K. I. Collins, D. M. Conti, M. B. Davies, H. J. Deeg, M. Deleuil, O. D.S. Demangeon, B. O. Demory, D. Ehrenreich, A. Erikson, M. Esposito, M. Fridlund, M. Gillon, E. Goffo, M. Güdel, E. W. Guenther, J. V. Harre, K. Heng, M. J. Hooton, K. G. Isaak, J. M. Jenkins, L. L. Kiss, E. Knudstrup, K. W.F. Lam, J. Laskar, A. Lecavelier Des Etangs, M. Lendl, C. Lovis, R. Luque, D. Magrin, P. F.L. Maxted, A. Muresan, V. Nascimbeni, G. Olofsson, H. P. Osborn, H. L.M. Osborne, R. Ottensamer, I. Pagano, E. Pallé, C. M. Persson, G. Peter, G. Piotto, D. Pollacco, D. Queloz, R. Ragazzoni, N. Rando, H. Rauer, S. Redfield, I. Ribas, G. R. Ricker, F. Rodler, N. C. Santos, G. Scandariato, S. Seager, D. Ségransan, A. E. Simon, A. M.S. Smith, M. Steller, Gy M. Szabó, N. Thomas, N. Tosi, J. D. Twicken, S. Udry, V. Van Eylen, V. Van Grootel, N. A. Walton, J. N. Winn

Astrophysical Sciences

Research output: Contribution to journal › Article › peer-review

Abstract

Context. Giant planets are known to dominate the long-term stability of planetary systems due to their prevailing gravitational interactions, but they are also thought to play an important role in planet formation. Observational constraints improve our understanding of planetary formation processes such as the delivery of volatile-rich planetesimals from beyond the ice line into the inner planetary system. Additional constraints may come from studies of the atmosphere, but almost all such studies of the atmosphere investigate the detection of certain species, and abundances are not routinely quantitatively measured. Aims. Accurate measurements of planetary bulk parameters-that is, mass and density-provide constraints on the inner structure and chemical composition of transiting planets. This information provides insight into properties such as the amounts of volatile species, which in turn can be related to formation and evolution processes. Methods. The Transiting Exoplanet Survey Satellite (TESS) reported a planetary candidate around HD 190622 (TOI-1054), which was subsequently validated and found to merit further characterization with photometric and spectroscopic facilities. The KESPRINT collaboration used data from the High Accuracy Radial Velocity Planet Searcher (HARPS) to independently confirm the planetary candidate, securing its mass, and revealing the presence of an outer giant planet in the system. The CHEOPS consortium invested telescope time in the transiting target in order to reduce the uncertainty on the radius, improving the characterization of the planet. Results. We present the discovery and characterization of the planetary system around HD 190622 (TOI-1054). This system hosts one transiting planet, which is smaller than Neptune (3.087-0.053+0.058REarth, 7.7 ± 1.0 MEarth) but has a similar bulk density (1.43 ± 0.21 g cm-3) and an orbital period of 16 days; and a giant planet, not known to be transiting, with a minimum mass of 227.0 ± 6.7 MEarth in an orbit with a period of 315 days. Conclusions. Our measurements constrain the structure and composition of the transiting planet. HD 190622b has singular properties among the known population of transiting planets, which we discuss in detail. Among the sub-Neptune-sized planets known today, this planet stands out because of its large gas content.

Original language	English (US)
Article number	A183
Journal	Astronomy and Astrophysics
Volume	675
DOIs	https://doi.org/10.1051/0004-6361/202245774
State	Published - Jul 1 2023

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

Planetary systems
Planets and satellites: detection

Access to Document

10.1051/0004-6361/202245774

Cite this

Cabrera, J., Gandolfi, D., Serrano, L. M., Csizmadia, S., Egger, J. A., Baumeister, P., Krenn, A., Benz, W., Deline, A., Florén, H. G., Collier Cameron, A., Adibekyan, V., Alibert, Y., Bellomo, S. E., Delrez, L., Fossati, L., Fortier, A., Grziwa, S., Hoyer, S., ... Winn, J. N. (2023). The planetary system around HD 190622 (TOI-1054): Measuring the gas content of low-mass planets orbiting F-stars. Astronomy and Astrophysics, 675, Article A183. https://doi.org/10.1051/0004-6361/202245774

@article{b52edf4b0760421e9b4aee825278a011,

title = "The planetary system around HD 190622 (TOI-1054): Measuring the gas content of low-mass planets orbiting F-stars",

abstract = "Context. Giant planets are known to dominate the long-term stability of planetary systems due to their prevailing gravitational interactions, but they are also thought to play an important role in planet formation. Observational constraints improve our understanding of planetary formation processes such as the delivery of volatile-rich planetesimals from beyond the ice line into the inner planetary system. Additional constraints may come from studies of the atmosphere, but almost all such studies of the atmosphere investigate the detection of certain species, and abundances are not routinely quantitatively measured. Aims. Accurate measurements of planetary bulk parameters-that is, mass and density-provide constraints on the inner structure and chemical composition of transiting planets. This information provides insight into properties such as the amounts of volatile species, which in turn can be related to formation and evolution processes. Methods. The Transiting Exoplanet Survey Satellite (TESS) reported a planetary candidate around HD 190622 (TOI-1054), which was subsequently validated and found to merit further characterization with photometric and spectroscopic facilities. The KESPRINT collaboration used data from the High Accuracy Radial Velocity Planet Searcher (HARPS) to independently confirm the planetary candidate, securing its mass, and revealing the presence of an outer giant planet in the system. The CHEOPS consortium invested telescope time in the transiting target in order to reduce the uncertainty on the radius, improving the characterization of the planet. Results. We present the discovery and characterization of the planetary system around HD 190622 (TOI-1054). This system hosts one transiting planet, which is smaller than Neptune (3.087-0.053+0.058REarth, 7.7 ± 1.0 MEarth) but has a similar bulk density (1.43 ± 0.21 g cm-3) and an orbital period of 16 days; and a giant planet, not known to be transiting, with a minimum mass of 227.0 ± 6.7 MEarth in an orbit with a period of 315 days. Conclusions. Our measurements constrain the structure and composition of the transiting planet. HD 190622b has singular properties among the known population of transiting planets, which we discuss in detail. Among the sub-Neptune-sized planets known today, this planet stands out because of its large gas content.",

keywords = "Planetary systems, Planets and satellites: detection",

author = "J. Cabrera and D. Gandolfi and Serrano, {L. M.} and Sz Csizmadia and Egger, {J. A.} and Ph Baumeister and A. Krenn and W. Benz and A. Deline and Flor{\'e}n, {H. G.} and {Collier Cameron}, A. and V. Adibekyan and Y. Alibert and Bellomo, {S. E.} and L. Delrez and L. Fossati and A. Fortier and S. Grziwa and S. Hoyer and A. Bonfanti and S. Salmon and Sousa, {S. G.} and Wilson, {T. G.} and J. Alarc{\'o}n and R. Alonso and {Anglada Escud{\'e}}, G. and T. B{\'a}rczy and O. Barrag{\'a}n and D. Barrado and Barros, {S. C.C.} and W. Baumjohann and M. Beck and T. Beck and Bernab{\`o}, {L. M.} and N. Billot and X. Bonfils and L. Borsato and A. Brandeker and C. Broeg and O. Carri{\'o}n-Gonz{\'a}lez and S. Charnoz and Ciardi, {D. R.} and Cochran, {W. D.} and Collins, {K. A.} and Collins, {K. I.} and Conti, {D. M.} and Davies, {M. B.} and Deeg, {H. J.} and M. Deleuil and Demangeon, {O. D.S.} and Demory, {B. O.} and D. Ehrenreich and A. Erikson and M. Esposito and M. Fridlund and M. Gillon and E. Goffo and M. G{\"u}del and Guenther, {E. W.} and Harre, {J. V.} and K. Heng and Hooton, {M. J.} and Isaak, {K. G.} and Jenkins, {J. M.} and Kiss, {L. L.} and E. Knudstrup and Lam, {K. W.F.} and J. Laskar and {Lecavelier Des Etangs}, A. and M. Lendl and C. Lovis and R. Luque and D. Magrin and Maxted, {P. F.L.} and A. Muresan and V. Nascimbeni and G. Olofsson and Osborn, {H. P.} and Osborne, {H. L.M.} and R. Ottensamer and I. Pagano and E. Pall{\'e} and Persson, {C. M.} and G. Peter and G. Piotto and D. Pollacco and D. Queloz and R. Ragazzoni and N. Rando and H. Rauer and S. Redfield and I. Ribas and Ricker, {G. R.} and F. Rodler and Santos, {N. C.} and G. Scandariato and S. Seager and D. S{\'e}gransan and Simon, {A. E.} and Smith, {A. M.S.} and M. Steller and Szab{\'o}, {Gy M.} and N. Thomas and N. Tosi and Twicken, {J. D.} and S. Udry and {Van Eylen}, V. and {Van Grootel}, V. and Walton, {N. A.} and Winn, {J. N.}",

note = "Funding Information: We would like to thank the anonymous referee for the careful reading and comments that improved the quality of the manuscript. CHEOPS is an ESA mission in partnership with Switzerland with important contributions to the payload and the ground segment from Austria, Belgium, France, Germany, Hungary, Italy, Portugal, Spain, Sweden, and the United Kingdom. The CHEOPS Consortium would like to gratefully acknowledge the support received by all the agencies, offices, universities, and industries involved. Their flexibility and willingness to explore new approaches were essential to the success of this mission. CHEOPS data analysed in this article will be made available in the CHEOPS mission archive ( https://cheops.unige.ch/archive_browser/ ) K.G.I. is the ESA CHEOPS Project Scientist and is responsible for the ESA CHEOPS Guest Observers Programme. She does not participate in, or contribute to, the definition of the Guaranteed Time Programme of the CHEOPS mission through which observations described in this paper have been taken, nor to any aspect of target selection for the programme. This work was supported by the KESPRINT collaboration, an international consortium devoted to the characterization and research of exoplanets discovered with space-based missions ( http://www.kesprint.science ). This paper includes data collected with the TESS mission, obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the TESS mission was provided by the NASA Explorer Program. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations center. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASAAdvanced Supercomputing (NAS) Division atAmes Research centre for the production of the SPOC data products. D.G. and L.M.S. gratefully acknowledge financial support from the CRT foundation under Grant No. 2018.2323 “Gaseous or rocky? Unveiling the nature of small worlds”. Ph. B. and N.T. acknowledge support by the DFG Schwerpunkt SPP 1992 “Exploring the Diversity of Extrasolar Planets” (grant TO 704/3-1) and by the DFG Research Unit FOR 2440 “Matter under planetary interior conditions” (grant PA 3689/1-1). A.C.C. and T.G.W. acknowledge support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1. This work was supported by FCT - Funda{\c c}{\~a}o para a Ci{\^e}ncia e a Tecnologia through national funds and by FEDER through COMPETE2020 -Programa Operacional Competitividade e Internacionaliza{\c c}{\~a}o by these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 & POCI-01-0145-FEDER-032113; PTDC/FIS-AST/28953/2017 and POCI-01-0145-FEDER-028953; PTDC/FIS-AST/28987/2017 and POCI-01-0145-FEDER-028987, 2022.06962.PTDC. Y.A., M.J.H. and J.A.E. acknowledge the support of the Swiss National Fund under grant 200020_172746. A.B. was supported by the SNSA. L.D. is an F.R.S.-FNRS Postdoctoral Researcher. The Belgian participation to CHEOPS has been supported by the Belgian Federal Science Policy Office (BELSPO) in the framework of the PRODEX Program, and by the University of Li{\`e}ge through an ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. E.G. gratefully acknowledges the support by the Th{\"u}ringer Ministerium f{\"u}r Wirtschaft, Wissenschaft und Digitale Gesellschaft. S.H. gratefully acknowledges CNES funding through the grant 837319. S.G.S. acknowledges support from FCT through FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC). We acknowledge support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grants ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, PGC2018-098153-B-C33, PGC2018-098153-B-C31, ESP2017-87676-C5-1-R, MDM-2017-0737 Unidad de Excelencia “Mar{\'i}a de Maeztu”- Centro de Astrobiolog{\textquoteright}ia (INTA-CSIC), as well as the support of the Generalitat de Catalunya/CERCA programme. S.C.C.B. acknowledges support from FCT through FCT contracts nr. IF/01312/2014/CP1215/CT0004. X.B., S.C.C.B., D.G., M.F. and J.L. acknowledge their role as ESA-appointed CHEOPS science team members. This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. H.J.D. acknowledges support from the Spanish Research Agency of the Ministry of Science and Innovation (AEI-MICINN) under grant PID2019-107061GB-C66, DOI: 10.13039/501100011033 . This project was supported by the CNES. O.D.S.D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through FCT. B.-O.D. acknowledges support from the Swiss National Science Foundation (PP00P2-190080). This project has received funding from the European Research Council (ERC) under the European Union{\textquoteright}s Horizon 2020 research and innovation programme (project FOUR ACES; grant agreement No 724427). It has also been carried out in the frame of the National Centre for Competence in Research PlanetS supported by the Swiss National Science Foundation (SNSF). DE acknowledges financial support from the Swiss National Science Foundation for project 200021_200726. A.De. acknowledges the financial support of the National Centre of Competence in Research PlanetS supported by the Swiss National Science Foundation under grants 51NF40_182901 and 51NF40_205606. M.F. and C.M.P. gratefully acknowledge the support of the Swedish National Space Agency (DNR 65/19, 174/19, 174/18). M.G. is an F.R.S.-FNRS Senior Research Associate. K.W.F.L. acknowledges support by DFG grants RA714/14-1 within the DFG Schwerpunkt SPP 1992, “Exploring the Diversity of Extrasolar Planets”. This work was granted access to the HPC resources of MesoPSL financed by the Region Ile de France and the project Equip@Meso (reference ANR-10-EQPX-29-01) of the programme Investissements d{\textquoteright}Avenir supervised by the Agence Nationale pour la Recherche. M.L. acknowledges support of the Swiss National Science Foundation under grant number PCEFP2_194576. R.L. acknowledges funding from University of La Laguna through the Margarita Salas Fellowship from the Spanish Ministry of Universities ref. UNI/551/2021-May 26, and under the EU Next Generation funds. P.M. acknowledges support from STFC research grant number ST/M001040/1. G.P., I.P., V.N. and R.R. acknowledge the funding support from Italian Space Agency (ASI) regulated by “Accordo ASI-INAF n. 2013-016-R.0 del 9 luglio 2013 e integrazione del 9 luglio 2015 CHEOPS Fasi A/B/C”. This work was also partially supported by a grant from the Simons Foundation (PI: Queloz, grant number 327127). I.R. acknowledges support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grant PGC2018-098153-B- C33, as well as the support of the Generalitat de Catalunya/CERCA programme. N.C.S. acknowledges support from the European Research Council through the grant agreement 101052347 (FIERCE). Gy.M.Sz. acknowledges the support of the Hungarian National Research, Development and Innovation Office (NKFIH) grant K-125015, a PRODEX Institute Agreement between the ELTE E{\"o}tv{\"o}s Lor{\'a}nd University and the European Space Agency (ESA-D/SCI-LE-2021-0025), the Lend{\"u}let LP2018-7/2021 grant of the Hungarian Academy of Science and the support of the city of Szombathely. V.V.G. is an F.R.S-FNRS Research Associate. S.S. has received funding from the European Research Council (ERC) under the European Union{\textquoteright}s Horizon 2020 research and innovation programme (grant agreement No 833925, project STAREX). N.A.W. acknowledges UKSA grant ST/R004838/1. The MOC activities have been supported by the ESA contract No. 4000124370. This work has made use of data from the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. Publisher Copyright: {\textcopyright} 2023 EDP Sciences. All rights reserved.",

year = "2023",

month = jul,

day = "1",

doi = "10.1051/0004-6361/202245774",

language = "English (US)",

volume = "675",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Cabrera, J, Gandolfi, D, Serrano, LM, Csizmadia, S, Egger, JA, Baumeister, P, Krenn, A, Benz, W, Deline, A, Florén, HG, Collier Cameron, A, Adibekyan, V, Alibert, Y, Bellomo, SE, Delrez, L, Fossati, L, Fortier, A, Grziwa, S, Hoyer, S, Bonfanti, A, Salmon, S, Sousa, SG, Wilson, TG, Alarcón, J, Alonso, R, Anglada Escudé, G, Bárczy, T, Barragán, O, Barrado, D, Barros, SCC, Baumjohann, W, Beck, M, Beck, T, Bernabò, LM, Billot, N, Bonfils, X, Borsato, L, Brandeker, A, Broeg, C, Carrión-González, O, Charnoz, S, Ciardi, DR, Cochran, WD, Collins, KA, Collins, KI, Conti, DM, Davies, MB, Deeg, HJ, Deleuil, M, Demangeon, ODS, Demory, BO, Ehrenreich, D, Erikson, A, Esposito, M, Fridlund, M, Gillon, M, Goffo, E, Güdel, M, Guenther, EW, Harre, JV, Heng, K, Hooton, MJ, Isaak, KG, Jenkins, JM, Kiss, LL, Knudstrup, E, Lam, KWF, Laskar, J, Lecavelier Des Etangs, A, Lendl, M, Lovis, C, Luque, R, Magrin, D, Maxted, PFL, Muresan, A, Nascimbeni, V, Olofsson, G, Osborn, HP, Osborne, HLM, Ottensamer, R, Pagano, I, Pallé, E, Persson, CM, Peter, G, Piotto, G, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Rauer, H, Redfield, S, Ribas, I, Ricker, GR, Rodler, F, Santos, NC, Scandariato, G, Seager, S, Ségransan, D, Simon, AE, Smith, AMS, Steller, M, Szabó, GM, Thomas, N, Tosi, N, Twicken, JD, Udry, S, Van Eylen, V, Van Grootel, V, Walton, NA & Winn, JN 2023, 'The planetary system around HD 190622 (TOI-1054): Measuring the gas content of low-mass planets orbiting F-stars', Astronomy and Astrophysics, vol. 675, A183. https://doi.org/10.1051/0004-6361/202245774

TY - JOUR

T1 - The planetary system around HD 190622 (TOI-1054)

T2 - Measuring the gas content of low-mass planets orbiting F-stars

AU - Cabrera, J.

AU - Gandolfi, D.

AU - Serrano, L. M.

AU - Csizmadia, Sz

AU - Egger, J. A.

AU - Baumeister, Ph

AU - Krenn, A.

AU - Benz, W.

AU - Deline, A.

AU - Florén, H. G.

AU - Collier Cameron, A.

AU - Adibekyan, V.

AU - Alibert, Y.

AU - Bellomo, S. E.

AU - Delrez, L.

AU - Fossati, L.

AU - Fortier, A.

AU - Grziwa, S.

AU - Hoyer, S.

AU - Bonfanti, A.

AU - Salmon, S.

AU - Sousa, S. G.

AU - Wilson, T. G.

AU - Alarcón, J.

AU - Alonso, R.

AU - Anglada Escudé, G.

AU - Bárczy, T.

AU - Barragán, O.

AU - Barrado, D.

AU - Barros, S. C.C.

AU - Baumjohann, W.

AU - Beck, M.

AU - Beck, T.

AU - Bernabò, L. M.

AU - Billot, N.

AU - Bonfils, X.

AU - Borsato, L.

AU - Brandeker, A.

AU - Broeg, C.

AU - Carrión-González, O.

AU - Charnoz, S.

AU - Ciardi, D. R.

AU - Cochran, W. D.

AU - Collins, K. A.

AU - Collins, K. I.

AU - Conti, D. M.

AU - Davies, M. B.

AU - Deeg, H. J.

AU - Deleuil, M.

AU - Demangeon, O. D.S.

AU - Demory, B. O.

AU - Ehrenreich, D.

AU - Erikson, A.

AU - Esposito, M.

AU - Fridlund, M.

AU - Gillon, M.

AU - Goffo, E.

AU - Güdel, M.

AU - Guenther, E. W.

AU - Harre, J. V.

AU - Heng, K.

AU - Hooton, M. J.

AU - Isaak, K. G.

AU - Jenkins, J. M.

AU - Kiss, L. L.

AU - Knudstrup, E.

AU - Lam, K. W.F.

AU - Laskar, J.

AU - Lecavelier Des Etangs, A.

AU - Lendl, M.

AU - Lovis, C.

AU - Luque, R.

AU - Magrin, D.

AU - Maxted, P. F.L.

AU - Muresan, A.

AU - Nascimbeni, V.

AU - Olofsson, G.

AU - Osborn, H. P.

AU - Osborne, H. L.M.

AU - Ottensamer, R.

AU - Pagano, I.

AU - Pallé, E.

AU - Persson, C. M.

AU - Peter, G.

AU - Piotto, G.

AU - Pollacco, D.

AU - Queloz, D.

AU - Ragazzoni, R.

AU - Rando, N.

AU - Rauer, H.

AU - Redfield, S.

AU - Ribas, I.

AU - Ricker, G. R.

AU - Rodler, F.

AU - Santos, N. C.

AU - Scandariato, G.

AU - Seager, S.

AU - Ségransan, D.

AU - Simon, A. E.

AU - Smith, A. M.S.

AU - Steller, M.

AU - Szabó, Gy M.

AU - Thomas, N.

AU - Tosi, N.

AU - Twicken, J. D.

AU - Udry, S.

AU - Van Eylen, V.

AU - Van Grootel, V.

AU - Walton, N. A.

AU - Winn, J. N.

N1 - Funding Information: We would like to thank the anonymous referee for the careful reading and comments that improved the quality of the manuscript. CHEOPS is an ESA mission in partnership with Switzerland with important contributions to the payload and the ground segment from Austria, Belgium, France, Germany, Hungary, Italy, Portugal, Spain, Sweden, and the United Kingdom. The CHEOPS Consortium would like to gratefully acknowledge the support received by all the agencies, offices, universities, and industries involved. Their flexibility and willingness to explore new approaches were essential to the success of this mission. CHEOPS data analysed in this article will be made available in the CHEOPS mission archive ( https://cheops.unige.ch/archive_browser/ ) K.G.I. is the ESA CHEOPS Project Scientist and is responsible for the ESA CHEOPS Guest Observers Programme. She does not participate in, or contribute to, the definition of the Guaranteed Time Programme of the CHEOPS mission through which observations described in this paper have been taken, nor to any aspect of target selection for the programme. This work was supported by the KESPRINT collaboration, an international consortium devoted to the characterization and research of exoplanets discovered with space-based missions ( http://www.kesprint.science ). This paper includes data collected with the TESS mission, obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the TESS mission was provided by the NASA Explorer Program. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations center. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASAAdvanced Supercomputing (NAS) Division atAmes Research centre for the production of the SPOC data products. D.G. and L.M.S. gratefully acknowledge financial support from the CRT foundation under Grant No. 2018.2323 “Gaseous or rocky? Unveiling the nature of small worlds”. Ph. B. and N.T. acknowledge support by the DFG Schwerpunkt SPP 1992 “Exploring the Diversity of Extrasolar Planets” (grant TO 704/3-1) and by the DFG Research Unit FOR 2440 “Matter under planetary interior conditions” (grant PA 3689/1-1). A.C.C. and T.G.W. acknowledge support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1. This work was supported by FCT - Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 -Programa Operacional Competitividade e Internacionalização by these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 & POCI-01-0145-FEDER-032113; PTDC/FIS-AST/28953/2017 and POCI-01-0145-FEDER-028953; PTDC/FIS-AST/28987/2017 and POCI-01-0145-FEDER-028987, 2022.06962.PTDC. Y.A., M.J.H. and J.A.E. acknowledge the support of the Swiss National Fund under grant 200020_172746. A.B. was supported by the SNSA. L.D. is an F.R.S.-FNRS Postdoctoral Researcher. The Belgian participation to CHEOPS has been supported by the Belgian Federal Science Policy Office (BELSPO) in the framework of the PRODEX Program, and by the University of Liège through an ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. E.G. gratefully acknowledges the support by the Thüringer Ministerium für Wirtschaft, Wissenschaft und Digitale Gesellschaft. S.H. gratefully acknowledges CNES funding through the grant 837319. S.G.S. acknowledges support from FCT through FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC). We acknowledge support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grants ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, PGC2018-098153-B-C33, PGC2018-098153-B-C31, ESP2017-87676-C5-1-R, MDM-2017-0737 Unidad de Excelencia “María de Maeztu”- Centro de Astrobiolog’ia (INTA-CSIC), as well as the support of the Generalitat de Catalunya/CERCA programme. S.C.C.B. acknowledges support from FCT through FCT contracts nr. IF/01312/2014/CP1215/CT0004. X.B., S.C.C.B., D.G., M.F. and J.L. acknowledge their role as ESA-appointed CHEOPS science team members. This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. H.J.D. acknowledges support from the Spanish Research Agency of the Ministry of Science and Innovation (AEI-MICINN) under grant PID2019-107061GB-C66, DOI: 10.13039/501100011033 . This project was supported by the CNES. O.D.S.D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through FCT. B.-O.D. acknowledges support from the Swiss National Science Foundation (PP00P2-190080). This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project FOUR ACES; grant agreement No 724427). It has also been carried out in the frame of the National Centre for Competence in Research PlanetS supported by the Swiss National Science Foundation (SNSF). DE acknowledges financial support from the Swiss National Science Foundation for project 200021_200726. A.De. acknowledges the financial support of the National Centre of Competence in Research PlanetS supported by the Swiss National Science Foundation under grants 51NF40_182901 and 51NF40_205606. M.F. and C.M.P. gratefully acknowledge the support of the Swedish National Space Agency (DNR 65/19, 174/19, 174/18). M.G. is an F.R.S.-FNRS Senior Research Associate. K.W.F.L. acknowledges support by DFG grants RA714/14-1 within the DFG Schwerpunkt SPP 1992, “Exploring the Diversity of Extrasolar Planets”. This work was granted access to the HPC resources of MesoPSL financed by the Region Ile de France and the project Equip@Meso (reference ANR-10-EQPX-29-01) of the programme Investissements d’Avenir supervised by the Agence Nationale pour la Recherche. M.L. acknowledges support of the Swiss National Science Foundation under grant number PCEFP2_194576. R.L. acknowledges funding from University of La Laguna through the Margarita Salas Fellowship from the Spanish Ministry of Universities ref. UNI/551/2021-May 26, and under the EU Next Generation funds. P.M. acknowledges support from STFC research grant number ST/M001040/1. G.P., I.P., V.N. and R.R. acknowledge the funding support from Italian Space Agency (ASI) regulated by “Accordo ASI-INAF n. 2013-016-R.0 del 9 luglio 2013 e integrazione del 9 luglio 2015 CHEOPS Fasi A/B/C”. This work was also partially supported by a grant from the Simons Foundation (PI: Queloz, grant number 327127). I.R. acknowledges support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grant PGC2018-098153-B- C33, as well as the support of the Generalitat de Catalunya/CERCA programme. N.C.S. acknowledges support from the European Research Council through the grant agreement 101052347 (FIERCE). Gy.M.Sz. acknowledges the support of the Hungarian National Research, Development and Innovation Office (NKFIH) grant K-125015, a PRODEX Institute Agreement between the ELTE Eötvös Loránd University and the European Space Agency (ESA-D/SCI-LE-2021-0025), the Lendület LP2018-7/2021 grant of the Hungarian Academy of Science and the support of the city of Szombathely. V.V.G. is an F.R.S-FNRS Research Associate. S.S. has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 833925, project STAREX). N.A.W. acknowledges UKSA grant ST/R004838/1. The MOC activities have been supported by the ESA contract No. 4000124370. This work has made use of data from the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. Publisher Copyright: © 2023 EDP Sciences. All rights reserved.

PY - 2023/7/1

Y1 - 2023/7/1

N2 - Context. Giant planets are known to dominate the long-term stability of planetary systems due to their prevailing gravitational interactions, but they are also thought to play an important role in planet formation. Observational constraints improve our understanding of planetary formation processes such as the delivery of volatile-rich planetesimals from beyond the ice line into the inner planetary system. Additional constraints may come from studies of the atmosphere, but almost all such studies of the atmosphere investigate the detection of certain species, and abundances are not routinely quantitatively measured. Aims. Accurate measurements of planetary bulk parameters-that is, mass and density-provide constraints on the inner structure and chemical composition of transiting planets. This information provides insight into properties such as the amounts of volatile species, which in turn can be related to formation and evolution processes. Methods. The Transiting Exoplanet Survey Satellite (TESS) reported a planetary candidate around HD 190622 (TOI-1054), which was subsequently validated and found to merit further characterization with photometric and spectroscopic facilities. The KESPRINT collaboration used data from the High Accuracy Radial Velocity Planet Searcher (HARPS) to independently confirm the planetary candidate, securing its mass, and revealing the presence of an outer giant planet in the system. The CHEOPS consortium invested telescope time in the transiting target in order to reduce the uncertainty on the radius, improving the characterization of the planet. Results. We present the discovery and characterization of the planetary system around HD 190622 (TOI-1054). This system hosts one transiting planet, which is smaller than Neptune (3.087-0.053+0.058REarth, 7.7 ± 1.0 MEarth) but has a similar bulk density (1.43 ± 0.21 g cm-3) and an orbital period of 16 days; and a giant planet, not known to be transiting, with a minimum mass of 227.0 ± 6.7 MEarth in an orbit with a period of 315 days. Conclusions. Our measurements constrain the structure and composition of the transiting planet. HD 190622b has singular properties among the known population of transiting planets, which we discuss in detail. Among the sub-Neptune-sized planets known today, this planet stands out because of its large gas content.

AB - Context. Giant planets are known to dominate the long-term stability of planetary systems due to their prevailing gravitational interactions, but they are also thought to play an important role in planet formation. Observational constraints improve our understanding of planetary formation processes such as the delivery of volatile-rich planetesimals from beyond the ice line into the inner planetary system. Additional constraints may come from studies of the atmosphere, but almost all such studies of the atmosphere investigate the detection of certain species, and abundances are not routinely quantitatively measured. Aims. Accurate measurements of planetary bulk parameters-that is, mass and density-provide constraints on the inner structure and chemical composition of transiting planets. This information provides insight into properties such as the amounts of volatile species, which in turn can be related to formation and evolution processes. Methods. The Transiting Exoplanet Survey Satellite (TESS) reported a planetary candidate around HD 190622 (TOI-1054), which was subsequently validated and found to merit further characterization with photometric and spectroscopic facilities. The KESPRINT collaboration used data from the High Accuracy Radial Velocity Planet Searcher (HARPS) to independently confirm the planetary candidate, securing its mass, and revealing the presence of an outer giant planet in the system. The CHEOPS consortium invested telescope time in the transiting target in order to reduce the uncertainty on the radius, improving the characterization of the planet. Results. We present the discovery and characterization of the planetary system around HD 190622 (TOI-1054). This system hosts one transiting planet, which is smaller than Neptune (3.087-0.053+0.058REarth, 7.7 ± 1.0 MEarth) but has a similar bulk density (1.43 ± 0.21 g cm-3) and an orbital period of 16 days; and a giant planet, not known to be transiting, with a minimum mass of 227.0 ± 6.7 MEarth in an orbit with a period of 315 days. Conclusions. Our measurements constrain the structure and composition of the transiting planet. HD 190622b has singular properties among the known population of transiting planets, which we discuss in detail. Among the sub-Neptune-sized planets known today, this planet stands out because of its large gas content.

KW - Planetary systems

KW - Planets and satellites: detection

UR - http://www.scopus.com/inward/record.url?scp=85166229075&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85166229075&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/202245774

DO - 10.1051/0004-6361/202245774

M3 - Article

AN - SCOPUS:85166229075

SN - 0004-6361

VL - 675

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A183

ER -

The planetary system around HD 190622 (TOI-1054): Measuring the gas content of low-mass planets orbiting F-stars

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