Two temperate earth-mass planets orbiting the nearby star GJ 1002
This work has made use of data from the European Space Agency (ESA) mission Gaia: https://www. cosmos.esa.int/gaia. The data were processed by the Gaia Data Processing and Analysis Consortium (DPAC): https://www.cosmos.esa.int/web/gaia/dpac/consortium
| Autores: | , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2023 |
| País: | España |
| Institución: | Instituto Nacional de Técnica Aeroespacial (INTA) |
| Repositorio: | DIGITAL.INTA Repositorio Digital del Instituto Nacional de Técnica Aeroespacial |
| OAI Identifier: | oai:digital.inta.es:20.500.12666/902 |
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| Palabra clave: | Techniques: spectroscopic Techniques: radial velocities Planets and satellites: terrestrial planets Stars: activity Stars: low-mass Stars: individual: GJ 1002 |
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Two temperate earth-mass planets orbiting the nearby star GJ 1002 |
| title |
Two temperate earth-mass planets orbiting the nearby star GJ 1002 |
| spellingShingle |
Two temperate earth-mass planets orbiting the nearby star GJ 1002 Suárez Mascareño, A. Techniques: spectroscopic Techniques: radial velocities Planets and satellites: terrestrial planets Stars: activity Stars: low-mass Stars: individual: GJ 1002 |
| title_short |
Two temperate earth-mass planets orbiting the nearby star GJ 1002 |
| title_full |
Two temperate earth-mass planets orbiting the nearby star GJ 1002 |
| title_fullStr |
Two temperate earth-mass planets orbiting the nearby star GJ 1002 |
| title_full_unstemmed |
Two temperate earth-mass planets orbiting the nearby star GJ 1002 |
| title_sort |
Two temperate earth-mass planets orbiting the nearby star GJ 1002 |
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Suárez Mascareño, A. González Álvarez, E. Lillo Box, J. Faria, J. P. Passegger, V. M. González Hernández, J. I. Figueira, P. Sozzetti, A. Rebolo, R. Pepe, Francesco Santos, Nuno C. Cristiani, S. Lovis, C. Silva, André Ribas, I. Amado, P. J. Caballero, J. A. Quirrenbach, A. Reiners, A. Zechmeister, M. Adibekyan, V. Alibert, Y. Béjar, V. J. S. Benatti, S. D´Odorico, V. Damasso, M. Delisle, J. B. Di Marcantonio, P. Dreizler, S. Ehrenreich, D. Hatzes, Artie Hara, N. C. Henning, T. Kaminski, A. López González, M. J. Martins, C. J. A. P. Micela, G. Montes, D. Pallé, E. Pedraz, S. Rodríguez Martínez, Eloy Rodríguez López, C. Tal Or, L. Sousa, S. G. Udry, S. Zapatero Osorio, María Rosa |
| author |
Suárez Mascareño, A. |
| author_facet |
Suárez Mascareño, A. González Álvarez, E. Lillo Box, J. Faria, J. P. Passegger, V. M. González Hernández, J. I. Figueira, P. Sozzetti, A. Rebolo, R. Pepe, Francesco Santos, Nuno C. Cristiani, S. Lovis, C. Silva, André Ribas, I. Amado, P. J. Caballero, J. A. Quirrenbach, A. Reiners, A. Zechmeister, M. Adibekyan, V. Alibert, Y. Béjar, V. J. S. Benatti, S. D´Odorico, V. Damasso, M. Delisle, J. B. Di Marcantonio, P. Dreizler, S. Ehrenreich, D. Hatzes, Artie Hara, N. C. Henning, T. Kaminski, A. López González, M. J. Martins, C. J. A. P. Micela, G. Montes, D. Pallé, E. Pedraz, S. Rodríguez Martínez, Eloy Rodríguez López, C. Tal Or, L. Sousa, S. G. Udry, S. Zapatero Osorio, María Rosa |
| author_role |
author |
| author2 |
González Álvarez, E. Lillo Box, J. Faria, J. P. Passegger, V. M. González Hernández, J. I. Figueira, P. Sozzetti, A. Rebolo, R. Pepe, Francesco Santos, Nuno C. Cristiani, S. Lovis, C. Silva, André Ribas, I. Amado, P. J. Caballero, J. A. Quirrenbach, A. Reiners, A. Zechmeister, M. Adibekyan, V. Alibert, Y. Béjar, V. J. S. Benatti, S. D´Odorico, V. Damasso, M. Delisle, J. B. Di Marcantonio, P. Dreizler, S. Ehrenreich, D. Hatzes, Artie Hara, N. C. Henning, T. Kaminski, A. López González, M. J. Martins, C. J. A. P. Micela, G. Montes, D. Pallé, E. Pedraz, S. Rodríguez Martínez, Eloy Rodríguez López, C. Tal Or, L. Sousa, S. G. Udry, S. Zapatero Osorio, María Rosa |
| author2_role |
author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author author |
| dc.contributor.none.fl_str_mv |
European Commission (EC) Ministerio de Ciencia e Innovación (MICINN) Agencia Estatal de Investigación (AEI) Consejo Superior de Investigaciones Científicas (CSIC) Fundacao para a Ciencia e a Tecnologia (FCT) Junta de Andalucía Swiss National Science Foundation (SNSF) Cabildo de Gran Canaria |
| dc.subject.none.fl_str_mv |
Techniques: spectroscopic Techniques: radial velocities Planets and satellites: terrestrial planets Stars: activity Stars: low-mass Stars: individual: GJ 1002 |
| topic |
Techniques: spectroscopic Techniques: radial velocities Planets and satellites: terrestrial planets Stars: activity Stars: low-mass Stars: individual: GJ 1002 |
| description |
This work has made use of data from the European Space Agency (ESA) mission Gaia: https://www. cosmos.esa.int/gaia. The data were processed by the Gaia Data Processing and Analysis Consortium (DPAC): https://www.cosmos.esa.int/web/gaia/dpac/consortium |
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2023 |
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2023 2023 2023 |
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info:eu-repo/semantics/article info:eu-repo/semantics/publishedVersion http://purl.org/coar/resource_type/c_6501 |
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article |
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publishedVersion |
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https://www.aanda.org/articles/aa/full_html/2023/02/aa44991-22/aa44991-22.html http://hdl.handle.net/20.500.12666/902 |
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https://www.aanda.org/articles/aa/full_html/2023/02/aa44991-22/aa44991-22.html http://hdl.handle.net/20.500.12666/902 |
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Inglés |
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Inglés |
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info:eu-repo/grantAgreement/MICINN//CEX2021-001131-S info:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2020-117493GB-I00 |
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Attribution-NonCommercial-NoDerivatives 4.0 International Attribution-NonCommercial-NoDerivatives 4.0 Internacional © The Authors 2023 http://creativecommons.org/licenses/by-nc-nd/4.0/ info:eu-repo/semantics/openAccess |
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Attribution-NonCommercial-NoDerivatives 4.0 International Attribution-NonCommercial-NoDerivatives 4.0 Internacional © The Authors 2023 http://creativecommons.org/licenses/by-nc-nd/4.0/ |
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openAccess |
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application/pdf |
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EDP Sciences |
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EDP Sciences |
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Two temperate earth-mass planets orbiting the nearby star GJ 1002Suárez Mascareño, A.González Álvarez, E.Lillo Box, J.Faria, J. P.Passegger, V. M.González Hernández, J. I.Figueira, P.Sozzetti, A.Rebolo, R.Pepe, FrancescoSantos, Nuno C.Cristiani, S.Lovis, C.Silva, AndréRibas, I.Amado, P. J.Caballero, J. A.Quirrenbach, A.Reiners, A.Zechmeister, M.Adibekyan, V.Alibert, Y.Béjar, V. J. S.Benatti, S.D´Odorico, V.Damasso, M.Delisle, J. B.Di Marcantonio, P.Dreizler, S.Ehrenreich, D.Hatzes, Artie Hara, N. C.Henning, T.Kaminski, A.López González, M. J.Martins, C. J. A. P.Micela, G.Montes, D.Pallé, E. Pedraz, S.Rodríguez Martínez, EloyRodríguez López, C.Tal Or, L.Sousa, S. G.Udry, S.Zapatero Osorio, María RosaTechniques: spectroscopicTechniques: radial velocitiesPlanets and satellites: terrestrial planetsStars: activityStars: low-massStars: individual: GJ 1002This work has made use of data from the European Space Agency (ESA) mission Gaia: https://www. cosmos.esa.int/gaia. The data were processed by the Gaia Data Processing and Analysis Consortium (DPAC): https://www.cosmos.esa.int/web/gaia/dpac/consortiumWe report the discovery and characterisation of two Earth-mass planets orbiting in the habitable zone of the nearby M-dwarf GJ 1002 based on the analysis of the radial-velocity (RV) time series from the ESPRESSO and CARMENES spectrographs. The host star is the quiet M5.5 V star GJ 1002 (relatively faint in the optical, V ~ 13.8 mag, but brighter in the infrared, J ~ 8.3 mag), located at 4.84 pc from the Sun. We analyse 139 spectroscopic observations taken between 2017 and 2021. We performed a joint analysis of the time series of the RV and full-width half maximum (FWHM) of the cross-correlation function (CCF) to model the planetary and stellar signals present in the data, applying Gaussian process regression to deal with the stellar activity. We detect the signal of two planets orbiting GJ 1002. GJ 1002 b is a planet with a minimum mass mp sin i of 1.08 ± 0.13 M⊕ with an orbital period of 10.3465 ± 0.0027 days at a distance of 0.0457 ± 0.0013 au from its parent star, receiving an estimated stellar flux of 0.67 F⊕. GJ 1002 c is a planet with a minimum mass mp sin i of 1.36 ± 0.17 M⊕ with an orbital period of 20.202 ± 0.013 days at a distance of 0.0738 ± 0.0021 au from its parent star, receiving an estimated stellar flux of 0.257 F⊕. We also detect the rotation signature of the star, with a period of 126 ± 15 days. We find that there is a correlation between the temperature of certain optical elements in the spectrographs and changes in the instrumental profile that can affect the scientific data, showing a seasonal behaviour that creates spurious signals at periods longer than ~200 days. GJ 1002 is one of the few known nearby systems with planets that could potentially host habitable environments. The closeness of the host star to the Sun makes the angular sizes of the orbits of both planets (~9.7 mas and ~15.7 mas, respectively) large enough for their atmosphere to be studied via high-contrast high-resolution spectroscopy with instruments such as the future spectrograph ANDES for the ELT or the LIFE mission.We want to thank the anonymous referee for their insightful comments, which helped improve the manuscript. We want to thank Ravi Kopparapu and Emily Gilbert for reaching out and highlighting an error in the limits of the habitable zone. A.S.M. acknowledges financial support from the Spanish Ministry of Science and Innovation (MICINN) under 2018 Juan de la Cierva program IJC2018-035229-I. A.S.M., V.M.P., J.I.G.H., C.A.P. and R.R. acknowledge financial support from the Spanish MICINN project PID2020-117493GB-I00. A.S.M., V.M.P., J.I.G.H. and R.R. acknowledge financial support from the Government of the Canary Islands project ProID2020010129. J.P.F. is supported in the form of a work contract funded by national funds through FCT with reference DL 57/2016/CP1364/CT0005. C.J.M. acknowledges FCT and POCH/FSE (EC) support through Investigador FCT Contract 2021.01214.CEECIND/CP1658/CT0001. 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: UIDB/04434/2020; UIDP/04434/2020. A.M.S acknowledges support from the Fundação para a Ciência e a Tecnologia (FCT) through the Fellowship 2020.05387.BD. and POCH/FSE (EC). 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 Inter-nacionalização by these grants: 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. The INAF authors acknowledge financial support of the Italian Ministry of Education, University, and Research with PRIN 201278X4FL and the “Progetti Premiali” funding scheme. J.B.D. acknowledges financial support from the Swiss National Science Foundation (SNSF). This work has, in part, been carried out within the framework of the National Centre for Competence in Research PlanetS supported by SNSF. CARMENES is an instrument for the Centro Astronómico Hispano en Andalucía (CAHA) at Calar Alto (Almería, Spain), operated jointly by the Junta de Andalucía and the Instituto de Astrofísica de Andalucía (CSIC). CARMENES was funded by the Max-Planck-Gesellschaft (MPG), the Consejo Superior de Investigaciones Científicas (CSIC), the Ministerio de Economía y Competitividad (MINECO) and the European Regional Development Fund (ERDF) through projects FICTS-2011-02, ICTS-2017-07-CAHA-4, and CAHA16-CE-3978, and the members of the CARMENES Consortium (Max-Planck-Institut für Astronomie, Instituto de Astrofísica de Andalucía, Landessternwarte Königstuhl, Institut de Ciències de l’Espai, Institut für Astrophysik Göttingen, Universidad Complutense de Madrid, Thüringer Landessternwarte Tautenburg, Instituto de Astrofísica de Canarias, Hamburger Sternwarte, Centro de Astrobiología and Centro Astronómico Hispano en Andalucía), with additional contributions by the MINECO, the Deutsche Forschungsgemeinschaft through the Major Research Instrumentation Programme and Research Unit FOR2544 “Blue Planets around Red Stars”, the Klaus Tschira Stiftung, the states of Baden-Württemberg and Niedersachsen, and by the Junta de Andalucía. 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. Manuscript written using Overleaf. Main analysis performed in Python3 (Van Rossum & Drake 2009) running on Ubuntu (Sobell 2015) systems and MS. Windows running the Windows subsystem for Linux (WLS). Radial velocities and selected activity indicators extracted with SERVAL (Zechmeister et al. 2018). Second RV extraction with S-BART (Silva et al. 2022). Extensive use of the DACE platform https://dace.unige.ch/ Extensive usage of Numpy (van der Walt et al. 2011). Extensive usage of Scipy (Virtanen et al. 2020). All figures built with Matplotlib (Hunter 2007). Periodograms and phase folded curves built using Pyastronomy (Czesla et al. 2019). Gaussian processes modelled with S+LEAF (Delisle et al. 2022), Celerite2 (Foreman-Mackey et al. 2017) and George (Foreman-Mackey et al. 2013). Nested sampling with Dynesty (Speagle 2020). Selected operations accelerated with Numba (Lam et al. 2015). Keplerian function adapted from Pytransit (Parviainen 2015). Selected calculations made in Excel (Microsoft Corporation 2018). TESS target pixel file plot done with tpfplotter (Aller et al. 2020). Aperture photometry performed with AstroImageJ (Collins et al. 2017). The bulk of the analysis was performed on desktop PC with an AMD RyzenTM 9 3950X (16 cores, 2 threads per core, 3.5–4.7 GHz) and a server hosting 2 x Intel(R) Xeon(R) Gold 5218 (2x16 cores, 2 threads per core, 2.3-3.9 GHz).With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).PeerreviewEDP SciencesEuropean Commission (EC)Ministerio de Ciencia e Innovación (MICINN)Agencia Estatal de Investigación (AEI)Consejo Superior de Investigaciones Científicas (CSIC)Fundacao para a Ciencia e a Tecnologia (FCT)Junta de AndalucíaSwiss National Science Foundation (SNSF)Cabildo de Gran Canaria202320232023info:eu-repo/semantics/articleinfo:eu-repo/semantics/publishedVersionhttp://purl.org/coar/resource_type/c_6501application/pdfhttps://www.aanda.org/articles/aa/full_html/2023/02/aa44991-22/aa44991-22.htmlhttp://hdl.handle.net/20.500.12666/902reponame:DIGITAL.INTA Repositorio Digital del Instituto Nacional de Técnica Aeroespacialinstname:Instituto Nacional de Técnica Aeroespacial (INTA)Inglésinfo:eu-repo/grantAgreement/MICINN//CEX2021-001131-Sinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PID2020-117493GB-I00Attribution-NonCommercial-NoDerivatives 4.0 InternationalAttribution-NonCommercial-NoDerivatives 4.0 Internacional© The Authors 2023http://creativecommons.org/licenses/by-nc-nd/4.0/info:eu-repo/semantics/openAccessoai:digital.inta.es:20.500.12666/9022026-06-23T12:46:37Z |
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15.300724 |