The young HD 73583 (TOI-560) planetary system: Two 10-M⊕ mini-Neptunes transiting a 500-Myr-old, bright, and active K dwarf

Autor: O Barragán, D J Armstrong, D Gandolfi, I Carleo, A A Vidotto, C Villarreal D’Angelo, A Oklopčić, H Isaacson, D Oddo, K Collins, M Fridlund, S G Sousa, C M Persson, C Hellier, S Howell, A Howard, S Redfield, N Eisner, I Y Georgieva, D Dragomir, D Bayliss, L D Nielsen, B Klein, S Aigrain, M Zhang, J Teske, J D Twicken, J Jenkins, M Esposito, V Van Eylen, F Rodler, V Adibekyan, J Alarcon, D R Anderson, J M Akana Murphy, D Barrado, S C C Barros, B Benneke, F Bouchy, E M Bryant, R P Butler, J Burt, J Cabrera, S Casewell, P Chaturvedi, R Cloutier, W D Cochran, J Crane, I Crossfield, N Crouzet, K I Collins, F Dai, H J Deeg, A Deline, O D S Demangeon, X Dumusque, P Figueira, E Furlan, C Gnilka, M R Goad, E Goffo, F Gutiérrez-Canales, A Hadjigeorghiou, Z Hartman, A P Hatzes, M Harris, B Henderson, T Hirano, S Hojjatpanah, S Hoyer, P Kabáth, J Korth, J Lillo-Box, R Luque, M Marmier, T Močnik, A Muresan, F Murgas, E Nagel, H L M Osborne, A Osborn, H P Osborn, E Palle, M Raimbault, G R Ricker, R A Rubenzahl, C Stockdale, N C Santos, N Scott, R P Schwarz, S Shectman, S Seager, D Ségransan, L M Serrano, M Skarka, A M S Smith, J Šubjak, T G Tan, S Udry, C Watson, P J Wheatley, R West, J N Winn, S X Wang, A Wolfgang, C Ziegler
Přispěvatelé: Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Ministerio de Ciencia e Innovación (España), European Commission, European Research Council, Swiss National Science Foundation, Fondazione Cassa di Risparmio di Torino, Centre National D'Etudes Spatiales (France), Low Energy Astrophysics (API, FNWI)
Jazyk: angličtina
Rok vydání: 2022
Předmět:
Zdroj: Monthly Notices of the Royal Astronomical Society
Monthly Notices of the Royal Astronomical Society, 2022, ⟨10.1093/mnras/stac638⟩
Digital.CSIC. Repositorio Institucional del CSIC
instname
Monthly Notices of the Royal Astronomical Society, 514(2), 1606-1627. Oxford University Press
Monthly Notices of the Royal Astronomical Society, 514(2), 1606-1627
Barragán, O, Armstrong, D J, Gandolfi, D, Carleo, I, Vidotto, A A, Villarreal D’Angelo, C, Oklopčić, A, Isaacson, H, Oddo, D, Collins, K I, Fridlund, M, Sousa, S G, Persson, C M, Hellier, C, Howell, S, Howard, A, Redfield, S, Eisner, N, Georgieva, I Y, Dragomir, D, Bayliss, D, Nielsen, L D, Klein, B, Aigrain, S, Zhang, M, Teske, J, Twicken, J D, Jenkins, J, Esposito, M, Van Eylen, V, Rodler, F, Adibekyan, V, Alarcon, J, Anderson, D R, Akana Murphy, J M, Barrado, D, Barros, S C C, Benneke, B, Bouchy, F, Bryant, E M, Butler, R P, Burt, J, Cabrera, J, Casewell, S, Chaturvedi, P, Cloutier, R, Cochran, W D, Crane, J, Crossfield, I, Crouzet, N, Collins, K I, Dai, F, Deeg, H J, Deline, A, Demangeon, O D S, Dumusque, X, Figueira, P, Furlan, E, Gnilka, C, Goad, M R, Goffo, E, Gutiérrez-Canales, F, Hadjigeorghiou, A, Hartman, Z, Hatzes, A P, Harris, M, Henderson, B, Hirano, T, Hojjatpanah, S, Hoyer, S, Kabáth, P, Korth, J, Lillo-Box, J, Luque, R, Marmier, M, Močnik, T, Muresan, A, Murgas, F, Nagel, E, Osborne, H L M, Osborn, A, Osborn, H P, Palle, E, Raimbault, M, Ricker, G R, Rubenzahl, R A, Stockdale, C, Santos, N C, Scott, N, Schwarz, R P, Shectman, S, Raimbault, M, Seager, S, Ségransan, D, Serrano, L M, Skarka, M, Smith, A M S, Šubjak, J, Tan, T G, Udry, S, Watson, C, Wheatley, P J, West, R, Winn, J N, Wang, S X, Wolfgang, A & Ziegler, C 2022, ' The young HD 73583 (TOI-560) planetary system: two 10-M⊕ mini-Neptunes transiting a 500-Myr-old, bright, and active K dwarf ', Monthly Notices of the Royal Astronomical Society, vol. 514, no. 2, pp. 1606-1627 . https://doi.org/10.1093/mnras/stac638
ISSN: 0035-8711
1365-2966
DOI: 10.1093/mnras/stac638⟩
Popis: This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.--Full list of authors: Barragan, O.; Armstrong, D. J.; Gandolfi, D.; Carleo, I; Vidotto, A. A.; D'Angelo, C. Villarreal; Oklopcic, A.; Isaacson, H.; Oddo, D.; Collins, K.; Fridlund, M.; Sousa, S. G.; Persson, C. M.; Hellier, C.; Howell, S.; Howard, A.; Redfield, S.; Eisner, N.; Georgieva, I. Y.; Dragomir, D.; Bayliss, D.; Nielsen, L. D.; Klein, B.; Aigrain, S.; Zhang, M.; Teske, J.; Twicken, J. D.; Jenkins, J.; Esposito, M.; Van Eylen, V.; Rodler, F.; Adibekyan, V; Alarcon, J.; Anderson, D. R.; Murphy, J. M. Akana; Barrado, D.; Barros, S. C. C.; Benneke, B.; Bouchy, F.; Bryant, E. M.; Butler, R. P.; Burt, J.; Cabrera, J.; Casewell, S.; Chaturvedi, P.; Cloutier, R.; Cochran, W. D.; Crane, J.; Crossfield, I; Crouzet, N.; Collins, K., I; Dai, F.; Deeg, H. J.; Deline, A.; Demangeon, O. D. S.; Dumusque, X.; Figueira, P.; Furlan, E.; Gnilka, C.; Goad, M. R.; Goffo, E.; Gutierrez-Canales, F.; Hadjigeorghiou, A.; Hartman, Z.; Hatzes, A. P.; Harris, M.; Henderson, B.; Hirano, T.; Hojjatpanah, S.; Hoyer, S.; Kabath, P.; Korth, J.; Lillo-Box, J.; Luque, R.; Marmier, M.; Mocnik, T.; Muresan, A.; Murgas, F.; Nagel, E.; Osborne, H. L. M.; Osborn, A.; Osborn, H. P.; Palle, E.; Raimbault, M.; Ricker, G. R.; Rubenzahl, R. A.; Stockdale, C.; Santos, N. C.; Scott, N.; Schwarz, R. P.; Shectman, S.; Seager, S.; Segransan, D.; Serrano, L. M.; Skarka, M.; Smith, A. M. S.; Subjak, J.; Tan, T. G.; Udry, S.; Watson, C.; Wheatley, P. J.; West, R.; Winn, J. N.; Wang, S. X.; Wolfgang, A.; Ziegler, C.; KESPRINT Team.
We present the discovery and characterization of two transiting planets observed by TESS in the light curves of the young and bright (V = 9.67) star HD73583 (TOI-560). We perform an intensive spectroscopic and photometric space- and ground-based follow-up in order to confirm and characterize the system. We found that HD73583 is a young (∼500 Myr) active star with a rotational period of 12.08 ± 0.11 d, and a mass and radius of 0.73 ± 0.02 M⊙ and 0.65 ± 0.02 R⊙, respectively. HD 73583 b (Pb = 6.3980420+0.0000067−0.0000062 d) has a mass and radius of 10.2+3.4−3.1 M⊕ and 2.79 ± 0.10 R⊕, respectively, which gives a density of 2.58+0.95−0.81 gcm−3⁠. HD 73583 c (Pc = 18.87974+0.00086−0.00074 d) has a mass and radius of 9.7+1.8−1.7 M⊕ and 2.39+0.10−0.09 R⊕, respectively, which translates to a density of 3.88+0.91−0.80 gcm−3⁠. Both planets are consistent with worlds made of a solid core surrounded by a volatile envelope. Because of their youth and host star brightness, they both are excellent candidates to perform transmission spectroscopy studies. We expect ongoing atmospheric mass-loss for both planets caused by stellar irradiation. We estimate that the detection of evaporating signatures on H and He would be challenging, but doable with present and future instruments. © The Author(s) 2022. Published by Oxford University Press on behalf of Royal Astronomical Society.
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). We thank the referee for their helpful comments and suggestions that improved the quality of this manuscript. 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 NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This work uses 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. This paper is in part based on data collected under the NGTS project at the ESO La Silla Paranal Observatory. The NGTS facility is operated by the consortium institutes with support from the UK Science and Technology Facilities Council (STFC) projects ST/M001962/1 and ST/S002642/1. This research has used the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Some of the observations in the paper used the High-Resolution Imaging instrument Zorro obtained under Gemini LLP Proposal Number: GN/S-2021A-LP-105. Zorro 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. Zorro 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). OB, BK, and SA acknowledge that this publication is part of a project that has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (Grant agreement No. 865624). DG and LMS gratefully acknowledge financial support from the Cassa di Risparmio di Torino foundation under Grant No. 2018.2323 ‘Gaseous or rocky? Unveiling the nature of small worlds’. DJA acknowledges support from the STFC via an Ernest Rutherford Fellowship (ST/R00384X/1). APH and ME acknowledges grant HA 3279/12-1 within the DFG Schwerpunkt SPP 1992, ‘Exploring the Diversity of Extrasolar Planets’. JS and PK would like to acknowledge support from MSMT grant LTT-20015. We acknowledges the support 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/FISAST /28953/2017 & POCI-01-0145-FEDER-028953. AD acknowledges the financial support of the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project FOUR ACES; grant agreement No 724427). AD also acknowledges financial support of the the Swiss National Science Foundation (SNSF) through the National Centre for Competence in Research ‘PlanetS’. MF, IYG, JK, and CMP gratefully acknowledge the support of the Swedish National Space Agency (DNR 177/19, 174/18, 2020-00104, 65/19). FGC thanks the Mexican national council for science and technology (CONACYT, CVU-1005374). MS acknowledge financial support of the Inter-transfer grant no LTT-20015. JL-B acknowledges financial support received from ‘la Caixa’ Foundation (ID 100010434) and from the European Union’s Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No 847648, with fellowship code LCF/BQ/PI20/11760023. AAV acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 817540, ASTROFLOW). JMAM is supported by the National Science Foundation Graduate Research Fellowship Program under Grant No. DGE-1842400. JMAM acknowledges the LSSTC Data Science Fellowship Program, which is funded by LSSTC, NSF Cybertraining Grant No. 1829740, the Brinson Foundation, and the Moore Foundation; his participation in the program has benefited this work. RAR is supported by the NSF Graduate Research Fellowship, grant No. DGE 1745301. RL acknowledges financial support from the Spanish Ministerio de Ciencia e Innovación, through project PID2019-109522GB-C52, and the Centre of Excellence ‘Severo Ochoa’ award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). PC acknowledges the generous support from Deutsche Forschungsgemeinschaft (DFG) of the grant CH 2636/1-1. SH acknowledges CNES funding through the grant 837319. VA acknowledges the support from Fundação para a Ciência e Tecnologia (FCT) through Investigador FCT contract nr. IF/00650/2015/CP1273/CT0001. ODSD is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through Fundação para a Ciência e Tecnologia (FCT). AO is supported by an STFC studentship. XD would like to acknowledge the funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement SCORE No 851555). HJD acknowledges support from the Spanish Research Agency of the Ministry of Science and Innovation (AEI-MICINN) under the grant ‘Contribution of the IAC to the PLATO Space Mission’ with reference PID2019-107061GB-C66, DOI: 10.13039/501100011033. DD acknowledges support from the TESS Guest Investigator Program grant 80NSSC19K1727 and NASA Exoplanet Research Program grant 18-2XRP18_2-0136. AO gratefully acknowledges support from the Dutch Research Council NWO Veni grant.
Databáze: OpenAIRE
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