Two warm Neptunes transiting HIP 9618 revealed by TESS and Cheops

H. P. Osborn; G. Nowak; G. Hébrard; T. Masseron; J. Lillo-Box; E. Pallé; A. Bekkelien; H. G. Florén; P. Guterman; A. E. Simon; V. Adibekyan; A. Bieryla; L. Borsato; A. Brandeker; D. R. Ciardi; A. Collier Cameron; K. A. Collins; J. A. Egger; D. Gandolfi; M. J. Hooton; D. W. Latham; M. Lendl; E. C. Matthews; A. Tuson; S. Ulmer-Moll; A. Vanderburg; T. G. Wilson; C. Ziegler; Y. Alibert; R. Alonso; G. Anglada; L. Arnold; J. Asquier; D. Barrado y Navascues; W. Baumjohann; T. Beck; A. A. Belinski; W. Benz; F. Biondi; I. Boisse; X. Bonfils; C. Broeg; L. A. Buchhave; T. Bárczy; S. C.C. Barros; J. Cabrera; C. Cardona Guillen; I. Carleo; A. Castro-González; S. Charnoz; J. Christiansen; P. Cortes-Zuleta; S. Csizmadia; S. Dalal; M. B. Davies; M. Deleuil; X. Delfosse; L. Delrez; B. O. Demory; A. B. Dunlavey; D. Ehrenreich; A. Erikson; R. B. Fernandes; A. Fortier; T. Forveille; L. Fossati; M. Fridlund; M. Gillon; R. F. Goeke; M. V. Goliguzova; E. J. Gonzales; M. N. Günther; M. Güdel; N. Heidari; C. E. Henze; S. Howell; S. Hoyer; J. I. Frey; K. G. Isaak; J. M. Jenkins; F. Kiefer; L. Kiss; J. Korth; P. F.L. Maxted; J. Laskar; A. Lecavelier des Etangs; C. Lovis; M. B. Lund; R. Luque; D. Magrin; J. M. Almenara; E. Martioli; M. Mecina; J. V. Medina; D. Moldovan; M. Morales-Calderón; G. Morello; C. Moutou; F. Murgas; E. L.N. Jensen; V. Nascimbeni; G. Olofsson; R. Ottensamer; I. Pagano; G. Peter; G. Piotto; D. Pollacco; D. Queloz; R. Ragazzoni; N. Rando; H. Rauer; I. Ribas; G. Ricker; O. D.S. Demangeon; A. M.S. Smith; N. Santos; G. Scandariato; S. Seager; S. G. Sousa; M. Steller; G. M. Szabó; D. Ségransan; N. Thomas; S. Udry; B. Ulmer; V. Van Grootel; R. Vanderspek; N. Walton; J. N. Winn

doi:10.1093/mnras/stad1319

Two warm Neptunes transiting HIP 9618 revealed by TESS and Cheops

H. P. Osborn, G. Nowak, G. Hébrard, T. Masseron, J. Lillo-Box, E. Pallé, A. Bekkelien, H. G. Florén, P. Guterman, A. E. Simon, V. Adibekyan, A. Bieryla, L. Borsato, A. Brandeker, D. R. Ciardi, A. Collier Cameron, K. A. Collins, J. A. Egger, D. Gandolfi, M. J. HootonD. W. Latham, M. Lendl, E. C. Matthews, A. Tuson, S. Ulmer-Moll, A. Vanderburg, T. G. Wilson, C. Ziegler, Y. Alibert, R. Alonso, G. Anglada, L. Arnold, J. Asquier, D. Barrado y Navascues, W. Baumjohann, T. Beck, A. A. Belinski, W. Benz, F. Biondi, I. Boisse, X. Bonfils, C. Broeg, L. A. Buchhave, T. Bárczy, S. C.C. Barros, J. Cabrera, C. Cardona Guillen, I. Carleo, A. Castro-González, S. Charnoz, J. Christiansen, P. Cortes-Zuleta, S. Csizmadia, S. Dalal, M. B. Davies, M. Deleuil, X. Delfosse, L. Delrez, B. O. Demory, A. B. Dunlavey, D. Ehrenreich, A. Erikson, R. B. Fernandes, A. Fortier, T. Forveille, L. Fossati, M. Fridlund, M. Gillon, R. F. Goeke, M. V. Goliguzova, E. J. Gonzales, M. N. Günther, M. Güdel, N. Heidari, C. E. Henze, S. Howell, S. Hoyer, J. I. Frey, K. G. Isaak, J. M. Jenkins, F. Kiefer, L. Kiss, J. Korth, P. F.L. Maxted, J. Laskar, A. Lecavelier des Etangs, C. Lovis, M. B. Lund, R. Luque, D. Magrin, J. M. Almenara, E. Martioli, M. Mecina, J. V. Medina, D. Moldovan, M. Morales-Calderón, G. Morello, C. Moutou, F. Murgas, E. L.N. Jensen, V. Nascimbeni, G. Olofsson, R. Ottensamer, I. Pagano, G. Peter, G. Piotto, D. Pollacco, D. Queloz, R. Ragazzoni, N. Rando, H. Rauer, I. Ribas, G. Ricker, O. D.S. Demangeon, A. M.S. Smith, N. Santos, G. Scandariato, S. Seager, S. G. Sousa, M. Steller, G. M. Szabó, D. Ségransan, N. Thomas, S. Udry, B. Ulmer, V. Van Grootel, R. Vanderspek, N. Walton, J. N. Winn

Astrophysical Sciences

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

4 Scopus citations

Abstract

HIP 9618 (HD 12572, TOI-1471, TIC 306263608) is a bright (G = 9.0 mag) solar analogue. TESS photometry revealed the star to have two candidate planets with radii of 3.9 ± 0.044 R (HIP 9618 b) and 3.343 ± 0.039 R (HIP 9618 c). While the 20.77291 d period of HIP 9618 b was measured unambiguously, HIP 9618 c showed only two transits separated by a 680-d gap in the time series, leaving many possibilities for the period. To solve this issue, CHEOPS performed targeted photometry of period aliases to attempt to recover the true period of planet c, and successfully determined the true period to be 52.56349 d. High-resolution spectroscopy with HARPS-N, SOPHIE, and CAFE revealed a mass of 10.0 ± 3.1M for HIP 9618 b, which, according to our interior structure models, corresponds to a 6.8 ± 1.4 per cent gas fraction. HIP 9618 c appears to have a lower mass than HIP 9618 b, with a 3-sigma upper limit of <18M. Follow-up and archival RV measurements also reveal a clear long-term trend which, when combined with imaging and astrometric information, reveal a low-mass companion (0.08⁺₋₀⁰₀₅¹²M_☉) orbiting at 26.0⁺₋₁₁¹⁹₀⁰ au. This detection makes HIP 9618 one of only five bright (K < 8 mag) transiting multiplanet systems known to host a planet with P > 50 d, opening the door for the atmospheric characterization of warm (T_eq < 750 K) sub-Neptunes.

Original language	English (US)
Pages (from-to)	3069-3089
Number of pages	21
Journal	Monthly Notices of the Royal Astronomical Society
Volume	523
Issue number	2
DOIs	https://doi.org/10.1093/mnras/stad1319
State	Published - Aug 1 2023

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

binaries: spectroscopic
eclipses
occultations
planets and satellites: detection
surveys

Access to Document

10.1093/mnras/stad1319

Cite this

Osborn, H. P., Nowak, G., Hébrard, G., Masseron, T., Lillo-Box, J., Pallé, E., Bekkelien, A., Florén, H. G., Guterman, P., Simon, A. E., Adibekyan, V., Bieryla, A., Borsato, L., Brandeker, A., Ciardi, D. R., Cameron, A. C., Collins, K. A., Egger, J. A., Gandolfi, D., ... Winn, J. N. (2023). Two warm Neptunes transiting HIP 9618 revealed by TESS and Cheops. Monthly Notices of the Royal Astronomical Society, 523(2), 3069-3089. https://doi.org/10.1093/mnras/stad1319

@article{89b5fbb6efaa46b9847607812971e8be,

title = "Two warm Neptunes transiting HIP 9618 revealed by TESS and Cheops",

abstract = "HIP 9618 (HD 12572, TOI-1471, TIC 306263608) is a bright (G = 9.0 mag) solar analogue. TESS photometry revealed the star to have two candidate planets with radii of 3.9 ± 0.044 R (HIP 9618 b) and 3.343 ± 0.039 R (HIP 9618 c). While the 20.77291 d period of HIP 9618 b was measured unambiguously, HIP 9618 c showed only two transits separated by a 680-d gap in the time series, leaving many possibilities for the period. To solve this issue, CHEOPS performed targeted photometry of period aliases to attempt to recover the true period of planet c, and successfully determined the true period to be 52.56349 d. High-resolution spectroscopy with HARPS-N, SOPHIE, and CAFE revealed a mass of 10.0 ± 3.1M for HIP 9618 b, which, according to our interior structure models, corresponds to a 6.8 ± 1.4 per cent gas fraction. HIP 9618 c appears to have a lower mass than HIP 9618 b, with a 3-sigma upper limit of <18M. Follow-up and archival RV measurements also reveal a clear long-term trend which, when combined with imaging and astrometric information, reveal a low-mass companion (0.08+−000512M☉) orbiting at 26.0+−111900 au. This detection makes HIP 9618 one of only five bright (K < 8 mag) transiting multiplanet systems known to host a planet with P > 50 d, opening the door for the atmospheric characterization of warm (Teq < 750 K) sub-Neptunes.",

keywords = "binaries: spectroscopic, eclipses, occultations, planets and satellites: detection, surveys",

author = "Osborn, {H. P.} and G. Nowak and G. H{\'e}brard and T. Masseron and J. Lillo-Box and E. Pall{\'e} and A. Bekkelien and Flor{\'e}n, {H. G.} and P. Guterman and Simon, {A. E.} and V. Adibekyan and A. Bieryla and L. Borsato and A. Brandeker and Ciardi, {D. R.} and Cameron, {A. Collier} and Collins, {K. A.} and Egger, {J. A.} and D. Gandolfi and Hooton, {M. J.} and Latham, {D. W.} and M. Lendl and Matthews, {E. C.} and A. Tuson and S. Ulmer-Moll and A. Vanderburg and Wilson, {T. G.} and C. Ziegler and Y. Alibert and R. Alonso and G. Anglada and L. Arnold and J. Asquier and {y Navascues}, {D. Barrado} and W. Baumjohann and T. Beck and Belinski, {A. A.} and W. Benz and F. Biondi and I. Boisse and X. Bonfils and C. Broeg and Buchhave, {L. A.} and T. B{\'a}rczy and Barros, {S. C.C.} and J. Cabrera and Guillen, {C. Cardona} and I. Carleo and A. Castro-Gonz{\'a}lez and S. Charnoz and J. Christiansen and P. Cortes-Zuleta and S. Csizmadia and S. Dalal and Davies, {M. B.} and M. Deleuil and X. Delfosse and L. Delrez and Demory, {B. O.} and Dunlavey, {A. B.} and D. Ehrenreich and A. Erikson and Fernandes, {R. B.} and A. Fortier and T. Forveille and L. Fossati and M. Fridlund and M. Gillon and Goeke, {R. F.} and Goliguzova, {M. V.} and Gonzales, {E. J.} and G{\"u}nther, {M. N.} and M. G{\"u}del and N. Heidari and Henze, {C. E.} and S. Howell and S. Hoyer and Frey, {J. I.} and Isaak, {K. G.} and Jenkins, {J. M.} and F. Kiefer and L. Kiss and J. Korth and Maxted, {P. F.L.} and J. Laskar and {des Etangs}, {A. Lecavelier} and C. Lovis and Lund, {M. B.} and R. Luque and D. Magrin and Almenara, {J. M.} and E. Martioli and M. Mecina and Medina, {J. V.} and D. Moldovan and M. Morales-Calder{\'o}n and G. Morello and C. Moutou and F. Murgas and Jensen, {E. L.N.} and V. Nascimbeni and G. Olofsson and R. Ottensamer and I. Pagano and G. Peter and G. Piotto and D. Pollacco and D. Queloz and R. Ragazzoni and N. Rando and H. Rauer and I. Ribas and G. Ricker and Demangeon, {O. D.S.} and Smith, {A. M.S.} and N. Santos and G. Scandariato and S. Seager and Sousa, {S. G.} and M. Steller and Szab{\'o}, {G. M.} and D. S{\'e}gransan and N. Thomas and S. Udry and B. Ulmer and {Van Grootel}, V. and R. Vanderspek and N. Walton and Winn, {J. N.}",

note = "Funding Information: ACC acknowledges support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1. Funding Information: We thank the TESS-Keck Survey team for their open coordination on this target, especially Joey Murphy, Howard Isaacson, Erik Petigura, Andrew Howard, & Natalie Batalha. This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by the NASA Explorer Program. We acknowledge the use of public TOI Release 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 NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This research has made use of the Exoplanet Follow-up Observation Program (ExoFOP; DOI: 10.26134/ExoFOP5) website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. 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. Some of the observations in the paper made use of the High-Resolution Imaging instrument {\textquoteleft}Alopeke obtained under Gemini LLP Proposal Number: GN/S-2021A-LP-105. {\textquoteleft}Alopeke was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. Alopeke was mounted on the Gemini North (and/or South) telescope of the international Gemini Observatory, a program of NSF{\textquoteright}s OIR Lab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigaci{\'o}n y Desarrollo (Chile), Ministerio de Ciencia, Tecnolog{\'i}a e Innovaci{\'o}n (Argentina), Minist{\'e}rio da Ci{\^e}ncia, Tecnologia, Inova{\c c}{\~o}es e Comunica{\c c}{\~o}es (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). 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. The Digitized Sky Surveys were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. The National Geographic Society – Palomar Observatory Sky Atlas (POSS-I) was made by the California Institute of Technology with grants from the National Geographic Society. The Second Palomar Observatory Sky Survey (POSS-II) was made by the California Institute of Technology with funds from the National Science Foundation, the National Geographic Society, the Sloan Foundation, the Samuel Oschin Foundation, and the Eastman Kodak Corporation. Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundaci{\'o}n Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias under programs ITP19_1 and CAT21B_39. Based on observations collected at the Centro Astron{\'o}mico Hispano en Andaluc{\'i}a (CAHA) at Calar Alto, operated jointly by Junta de Andaluc{\'i}a and Consejo Superior de Investigaciones Cient{\'i}ficas (IAA-CSIC). This work has been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation under grants 51NF40_182901 and 51NF40_205606. Funding Information: MF and CMP gratefully acknowledge the support of the Swedish National Space Agency (DNR 65/19, 174/18). Funding Information: 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 Funding Information: DG gratefully acknowledges financial support from the CRT foundation under Grant No. 2018.2323 {\textquoteleft}Gaseousor rocky? Unveiling the nature of small worlds{\textquoteright}. Funding Information: NCSa acknowledges funding by the European Union (ERC, FIERCE, 101052347). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. Funding Information: ACC and TW acknowledge support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1. Funding Information: SGS acknowledge support from FCT through FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC) Funding Information: JAEg acknowledges support from the Swiss National Science Foundation (SNSF) under grant 200020_192038. Funding Information: IRI 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. Funding Information: This work was also partially supported by a grant from the Simons Foundation (PI Queloz, grant number 327127). Funding Information: ML acknowledges support of the Swiss National Science Foundation under grant number PCEFP2_194576. Funding Information: 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; LD is an F.R.S.-FNRS Postdoctoral Researcher. Funding Information: We warmly thank the OHP staff for their support on the observations. XB, IB, and TF received funding from the French Programme National de Physique Stellaire (PNPS) and the Programme National de Plan{\'e}tologie (PNP) of CNRS (INSU). Funding Information: 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 Internacionalizac{\~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 & POCI-01-0145-FEDER-028953, PTDC/FIS-AST/28987/2017 & POCI-01-0145-FEDER-028987, ODSD is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through FCT. Funding Information: B-OD acknowledges support from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00046. Funding Information: 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. Funding Information: AAB and MVG acknowledge the support of Ministry of Science and Higher Education of the Russian Federation under the grant 075-15-2020-780 (N13.1902.21.0039) Funding Information: GN thanks for the research funding from the Ministry of Education and Science programme the {\textquoteleft}Excellence Initiative – Research University{\textquoteright} conducted at the Centre of Excellence in Astrophysics and Astrochemistry of the Nicolaus Copernicus University in Toru{\'n}, Poland. Funding Information: SH gratefully acknowledges CNES funding through the grant 837319. Funding Information: EM acknowledges funding from the French National Research Agency (ANR) under contract number ANR18CE310019 (SPlaSH) and funding from Funda{\c c}{\~a}o de Amparo {\`a} Pesquisa do Estado de Minas Gerais (FAPEMIG) under the project number APQ0249322. Funding Information: GyMSz acknowledges the support of the Hungarian National Research, Development and Innovation Office (NKFIH) grant K-125015, a PRODEX Experiment Agreement No. 4000137122, the Lend{\"u}let LP2018-7/2021 grant of the Hungarian Academy of Science and the support of the city of Szombathely. Funding Information: 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 Maria de Maeztu-Centro de Astrobiolog{\'i}a (INTA-CSIC), as well as the support of the Generalitat de Catalunya/CERCA programme. The MOC activities have been supported by the ESA contract No. 4000124370. Funding Information: PM acknowledges support from STFC research grant number ST/M001040/1. Funding Information: JK gratefully acknowledges the support of the Swedish National Space Agency (SNSA; DNR 2020–00104) and of the Swedish Research Council (VR: Etableringsbidrag 2017–04945) Funding Information: LBo, GBr, VNa, IPa, GPi, RRa, GSc, VSi, and TZi acknowledge support from CHEOPS ASI-INAF agreement n. 2019-29-HH.0. Publisher Copyright: {\textcopyright} 2023 The Author(s).",

year = "2023",

month = aug,

day = "1",

doi = "10.1093/mnras/stad1319",

language = "English (US)",

volume = "523",

pages = "3069--3089",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "2",

}

Osborn, HP, Nowak, G, Hébrard, G, Masseron, T, Lillo-Box, J, Pallé, E, Bekkelien, A, Florén, HG, Guterman, P, Simon, AE, Adibekyan, V, Bieryla, A, Borsato, L, Brandeker, A, Ciardi, DR, Cameron, AC, Collins, KA, Egger, JA, Gandolfi, D, Hooton, MJ, Latham, DW, Lendl, M, Matthews, EC, Tuson, A, Ulmer-Moll, S, Vanderburg, A, Wilson, TG, Ziegler, C, Alibert, Y, Alonso, R, Anglada, G, Arnold, L, Asquier, J, y Navascues, DB, Baumjohann, W, Beck, T, Belinski, AA, Benz, W, Biondi, F, Boisse, I, Bonfils, X, Broeg, C, Buchhave, LA, Bárczy, T, Barros, SCC, Cabrera, J, Guillen, CC, Carleo, I, Castro-González, A, Charnoz, S, Christiansen, J, Cortes-Zuleta, P, Csizmadia, S, Dalal, S, Davies, MB, Deleuil, M, Delfosse, X, Delrez, L, Demory, BO, Dunlavey, AB, Ehrenreich, D, Erikson, A, Fernandes, RB, Fortier, A, Forveille, T, Fossati, L, Fridlund, M, Gillon, M, Goeke, RF, Goliguzova, MV, Gonzales, EJ, Günther, MN, Güdel, M, Heidari, N, Henze, CE, Howell, S, Hoyer, S, Frey, JI, Isaak, KG, Jenkins, JM, Kiefer, F, Kiss, L, Korth, J, Maxted, PFL, Laskar, J, des Etangs, AL, Lovis, C, Lund, MB, Luque, R, Magrin, D, Almenara, JM, Martioli, E, Mecina, M, Medina, JV, Moldovan, D, Morales-Calderón, M, Morello, G, Moutou, C, Murgas, F, Jensen, ELN, Nascimbeni, V, Olofsson, G, Ottensamer, R, Pagano, I, Peter, G, Piotto, G, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Rauer, H, Ribas, I, Ricker, G, Demangeon, ODS, Smith, AMS, Santos, N, Scandariato, G, Seager, S, Sousa, SG, Steller, M, Szabó, GM, Ségransan, D, Thomas, N, Udry, S, Ulmer, B, Van Grootel, V, Vanderspek, R, Walton, N & Winn, JN 2023, 'Two warm Neptunes transiting HIP 9618 revealed by TESS and Cheops', Monthly Notices of the Royal Astronomical Society, vol. 523, no. 2, pp. 3069-3089. https://doi.org/10.1093/mnras/stad1319

TY - JOUR

T1 - Two warm Neptunes transiting HIP 9618 revealed by TESS and Cheops

AU - Osborn, H. P.

AU - Nowak, G.

AU - Hébrard, G.

AU - Masseron, T.

AU - Lillo-Box, J.

AU - Pallé, E.

AU - Bekkelien, A.

AU - Florén, H. G.

AU - Guterman, P.

AU - Simon, A. E.

AU - Adibekyan, V.

AU - Bieryla, A.

AU - Borsato, L.

AU - Brandeker, A.

AU - Ciardi, D. R.

AU - Cameron, A. Collier

AU - Collins, K. A.

AU - Egger, J. A.

AU - Gandolfi, D.

AU - Hooton, M. J.

AU - Latham, D. W.

AU - Lendl, M.

AU - Matthews, E. C.

AU - Tuson, A.

AU - Ulmer-Moll, S.

AU - Vanderburg, A.

AU - Wilson, T. G.

AU - Ziegler, C.

AU - Alibert, Y.

AU - Alonso, R.

AU - Anglada, G.

AU - Arnold, L.

AU - Asquier, J.

AU - y Navascues, D. Barrado

AU - Baumjohann, W.

AU - Beck, T.

AU - Belinski, A. A.

AU - Benz, W.

AU - Biondi, F.

AU - Boisse, I.

AU - Bonfils, X.

AU - Broeg, C.

AU - Buchhave, L. A.

AU - Bárczy, T.

AU - Barros, S. C.C.

AU - Cabrera, J.

AU - Guillen, C. Cardona

AU - Carleo, I.

AU - Castro-González, A.

AU - Charnoz, S.

AU - Christiansen, J.

AU - Cortes-Zuleta, P.

AU - Csizmadia, S.

AU - Dalal, S.

AU - Davies, M. B.

AU - Deleuil, M.

AU - Delfosse, X.

AU - Delrez, L.

AU - Demory, B. O.

AU - Dunlavey, A. B.

AU - Ehrenreich, D.

AU - Erikson, A.

AU - Fernandes, R. B.

AU - Fortier, A.

AU - Forveille, T.

AU - Fossati, L.

AU - Fridlund, M.

AU - Gillon, M.

AU - Goeke, R. F.

AU - Goliguzova, M. V.

AU - Gonzales, E. J.

AU - Günther, M. N.

AU - Güdel, M.

AU - Heidari, N.

AU - Henze, C. E.

AU - Howell, S.

AU - Hoyer, S.

AU - Frey, J. I.

AU - Isaak, K. G.

AU - Jenkins, J. M.

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N1 - Funding Information: ACC acknowledges support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1. Funding Information: We thank the TESS-Keck Survey team for their open coordination on this target, especially Joey Murphy, Howard Isaacson, Erik Petigura, Andrew Howard, & Natalie Batalha. This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by the NASA Explorer Program. We acknowledge the use of public TOI Release 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 NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This research has made use of the Exoplanet Follow-up Observation Program (ExoFOP; DOI: 10.26134/ExoFOP5) website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. 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. Some of the observations in the paper made use of the High-Resolution Imaging instrument ‘Alopeke obtained under Gemini LLP Proposal Number: GN/S-2021A-LP-105. ‘Alopeke was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. Alopeke was mounted on the Gemini North (and/or South) telescope of the international Gemini Observatory, a program of NSF’s OIR Lab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). 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. The Digitized Sky Surveys were produced at the Space Telescope Science Institute under U.S. Government grant NAG W-2166. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. The National Geographic Society – Palomar Observatory Sky Atlas (POSS-I) was made by the California Institute of Technology with grants from the National Geographic Society. The Second Palomar Observatory Sky Survey (POSS-II) was made by the California Institute of Technology with funds from the National Science Foundation, the National Geographic Society, the Sloan Foundation, the Samuel Oschin Foundation, and the Eastman Kodak Corporation. Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated on the island of La Palma by the Fundación Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias under programs ITP19_1 and CAT21B_39. Based on observations collected at the Centro Astronómico Hispano en Andalucía (CAHA) at Calar Alto, operated jointly by Junta de Andalucía and Consejo Superior de Investigaciones Científicas (IAA-CSIC). This work has been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation under grants 51NF40_182901 and 51NF40_205606. Funding Information: MF and CMP gratefully acknowledge the support of the Swedish National Space Agency (DNR 65/19, 174/18). Funding Information: 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 Funding Information: DG gratefully acknowledges financial support from the CRT foundation under Grant No. 2018.2323 ‘Gaseousor rocky? Unveiling the nature of small worlds’. Funding Information: NCSa acknowledges funding by the European Union (ERC, FIERCE, 101052347). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. Funding Information: ACC and TW acknowledge support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1. Funding Information: SGS acknowledge support from FCT through FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC) Funding Information: JAEg acknowledges support from the Swiss National Science Foundation (SNSF) under grant 200020_192038. Funding Information: IRI 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. Funding Information: This work was also partially supported by a grant from the Simons Foundation (PI Queloz, grant number 327127). Funding Information: ML acknowledges support of the Swiss National Science Foundation under grant number PCEFP2_194576. Funding Information: 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; LD is an F.R.S.-FNRS Postdoctoral Researcher. Funding Information: We warmly thank the OHP staff for their support on the observations. XB, IB, and TF received funding from the French Programme National de Physique Stellaire (PNPS) and the Programme National de Planétologie (PNP) of CNRS (INSU). Funding Information: 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 Internacionalizacã 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 & POCI-01-0145-FEDER-028953, PTDC/FIS-AST/28987/2017 & POCI-01-0145-FEDER-028987, ODSD is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through FCT. Funding Information: B-OD acknowledges support from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number MB22.00046. Funding Information: 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. Funding Information: AAB and MVG acknowledge the support of Ministry of Science and Higher Education of the Russian Federation under the grant 075-15-2020-780 (N13.1902.21.0039) Funding Information: GN thanks for the research funding from the Ministry of Education and Science programme the ‘Excellence Initiative – Research University’ conducted at the Centre of Excellence in Astrophysics and Astrochemistry of the Nicolaus Copernicus University in Toruń, Poland. Funding Information: SH gratefully acknowledges CNES funding through the grant 837319. Funding Information: EM acknowledges funding from the French National Research Agency (ANR) under contract number ANR18CE310019 (SPlaSH) and funding from Fundação de Amparo à Pesquisa do Estado de Minas Gerais (FAPEMIG) under the project number APQ0249322. Funding Information: GyMSz acknowledges the support of the Hungarian National Research, Development and Innovation Office (NKFIH) grant K-125015, a PRODEX Experiment Agreement No. 4000137122, the Lendület LP2018-7/2021 grant of the Hungarian Academy of Science and the support of the city of Szombathely. Funding Information: 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 Maria de Maeztu-Centro de Astrobiología (INTA-CSIC), as well as the support of the Generalitat de Catalunya/CERCA programme. The MOC activities have been supported by the ESA contract No. 4000124370. Funding Information: PM acknowledges support from STFC research grant number ST/M001040/1. Funding Information: JK gratefully acknowledges the support of the Swedish National Space Agency (SNSA; DNR 2020–00104) and of the Swedish Research Council (VR: Etableringsbidrag 2017–04945) Funding Information: LBo, GBr, VNa, IPa, GPi, RRa, GSc, VSi, and TZi acknowledge support from CHEOPS ASI-INAF agreement n. 2019-29-HH.0. Publisher Copyright: © 2023 The Author(s).

PY - 2023/8/1

Y1 - 2023/8/1

N2 - HIP 9618 (HD 12572, TOI-1471, TIC 306263608) is a bright (G = 9.0 mag) solar analogue. TESS photometry revealed the star to have two candidate planets with radii of 3.9 ± 0.044 R (HIP 9618 b) and 3.343 ± 0.039 R (HIP 9618 c). While the 20.77291 d period of HIP 9618 b was measured unambiguously, HIP 9618 c showed only two transits separated by a 680-d gap in the time series, leaving many possibilities for the period. To solve this issue, CHEOPS performed targeted photometry of period aliases to attempt to recover the true period of planet c, and successfully determined the true period to be 52.56349 d. High-resolution spectroscopy with HARPS-N, SOPHIE, and CAFE revealed a mass of 10.0 ± 3.1M for HIP 9618 b, which, according to our interior structure models, corresponds to a 6.8 ± 1.4 per cent gas fraction. HIP 9618 c appears to have a lower mass than HIP 9618 b, with a 3-sigma upper limit of <18M. Follow-up and archival RV measurements also reveal a clear long-term trend which, when combined with imaging and astrometric information, reveal a low-mass companion (0.08+−000512M☉) orbiting at 26.0+−111900 au. This detection makes HIP 9618 one of only five bright (K < 8 mag) transiting multiplanet systems known to host a planet with P > 50 d, opening the door for the atmospheric characterization of warm (Teq < 750 K) sub-Neptunes.

AB - HIP 9618 (HD 12572, TOI-1471, TIC 306263608) is a bright (G = 9.0 mag) solar analogue. TESS photometry revealed the star to have two candidate planets with radii of 3.9 ± 0.044 R (HIP 9618 b) and 3.343 ± 0.039 R (HIP 9618 c). While the 20.77291 d period of HIP 9618 b was measured unambiguously, HIP 9618 c showed only two transits separated by a 680-d gap in the time series, leaving many possibilities for the period. To solve this issue, CHEOPS performed targeted photometry of period aliases to attempt to recover the true period of planet c, and successfully determined the true period to be 52.56349 d. High-resolution spectroscopy with HARPS-N, SOPHIE, and CAFE revealed a mass of 10.0 ± 3.1M for HIP 9618 b, which, according to our interior structure models, corresponds to a 6.8 ± 1.4 per cent gas fraction. HIP 9618 c appears to have a lower mass than HIP 9618 b, with a 3-sigma upper limit of <18M. Follow-up and archival RV measurements also reveal a clear long-term trend which, when combined with imaging and astrometric information, reveal a low-mass companion (0.08+−000512M☉) orbiting at 26.0+−111900 au. This detection makes HIP 9618 one of only five bright (K < 8 mag) transiting multiplanet systems known to host a planet with P > 50 d, opening the door for the atmospheric characterization of warm (Teq < 750 K) sub-Neptunes.

KW - binaries: spectroscopic

KW - eclipses

KW - occultations

KW - planets and satellites: detection

KW - surveys

UR - http://www.scopus.com/inward/record.url?scp=85162768259&partnerID=8YFLogxK

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U2 - 10.1093/mnras/stad1319

DO - 10.1093/mnras/stad1319

M3 - Article

AN - SCOPUS:85162768259

SN - 0035-8711

VL - 523

SP - 3069

EP - 3089

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 2

ER -

Two warm Neptunes transiting HIP 9618 revealed by TESS and Cheops

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