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1. Planetary system LHS 1140 revisited with ESPRESSO and TESS

Author

L. Acuña, Nathan Hara, Nuno C. Santos, David Barrado, João P. Faria, Emmanuel Marcq, Nicola Astudillo-Defru, Stéphane Udry, Xavier Bonfils, Francesco Pepe, Pedro Figueira, A. Leleu, Philippe Robutel, Alexandre C. M. Correia, Jorge Lillo-Box, S. G. Sousa, C. Lovis, Magali Deleuil, O. Mousis, Jose-Manuel Almenara, Centro de Astrobiologia [Madrid] (CAB), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), European Southern Observatory [Santiago] (ESO), European Southern Observatory (ESO), Instituto de Astrofísica e Ciências do Espaço (IASTRO), Center for Space and Habitability (CSH), University of Bern, Space Research and Planetary Sciences [Bern) (WP), Physikalisches Institut [Bern], Universität Bern [Bern]-Universität Bern [Bern], National Centre of Competence in Research PlanetS (NCCR PlanetS), Universität Bern [Bern]-Universität Bern [Bern]-Swiss National Science Foundation (SNSF), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Departamento de Física e Astronomia [Porto] (DFA/FCUP), Faculdade de Ciências da Universidade do Porto (FCUP), Universidade do Porto-Universidade do Porto, Geneva Observatory, University of Geneva [Switzerland], Centro de Física da Universidade de Coimbra (CFisUC), Universidade de Coimbra [Coimbra], Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Departamento de Matemática y Fı́sica Aplicadas [Concepcion] (DMFA), Universidad Católica de la Santísima Concepción (UCSC), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Spanish StateResearch Agency (AEI) Projects No.ESP2017-87676-C5-1-R and No. MDM-2017-0737 Unidad de Excelencia 'María de Maeztu' – Centro de Astrobiología(INTA-CSIC). This work was supported by FCT – Fundação para a Ciênciae a Tecnologia through national funds and by FEDER through COM-PETE2020 – Programa Operacional Competitividade e Internacionalizaçãoby 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. N.A.-D. acknowledges thesupport of FONDECYT project 3180063. X.B. and J.M.A. acknowledge fundingfrom the European Research Council under the ERC Grant Agreement n. 337591-ExTrA. A.C. acknowledges support by CFisUC projects (UIDB/04564/2020and UIDP/04564/2020), ENGAGE SKA (POCI-01-0145-FEDER-022217), andPHOBOS (POCI-01-0145-FEDER-029932), funded by COMPETE 2020 andFCT, Portugal. J.P.F. is supported in the form of a work contract funded bynational funds through FCT with reference DL57/2016/CP1364/CT0005, European Project: 337591,EC:FP7:ERC,ERC-2013-StG,EXTRA(2014), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Universität Bern [Bern] (UNIBE)-Universität Bern [Bern] (UNIBE), Universität Bern [Bern] (UNIBE)-Universität Bern [Bern] (UNIBE)-Swiss National Science Foundation (SNSF), 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), Universidade do Porto = University of Porto-Universidade do Porto = University of Porto, Université de Genève = University of Geneva (UNIGE), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Faria, J. [0000-0002-6728-244X], Correia, A. C. M. [0000-0002-8946-8579], Leleu, A. [0000-0003-2051-7974], Lillo Box, J. [0000-0003-3742-1987], Santos, N. [0000-0003-4422-2919], Agencia Estatal de Investigación (AEI), FEDER through COMPETE2020 - Programa Operacional Competitividade e Internacionalizacao, Comisión Nacional de Investigación Científica y Tecnológica (CONICYT), European Research Council (ERC), ENGAGE SKA, PHOBOS, Portuguese Foundation for Science and Technology, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Fundacao para a Ciencia e a Tecnologia (FCT), Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT), and European Commission (EC)

Subjects
010504 meteorology & atmospheric sciences, FOS: Physical sciences, Context (language use), Astrophysics, polarimetric [Techniques], 01 natural sciences, Photometry (optics), planets and satellites: terrestrial planets, Planet, 0103 physical sciences, techniques: radial velocities, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [PHYS]Physics [physics], radial velocities [Techniques], planets and satellites: composition, Astronomy and Astrophysics, Planetary system, Orbital period, interiors [Planets and satellites], Exoplanet, planets and satellites: interiors, planets and satellites: individual: LHS1140, Radial velocity, techniques: polarimetric, 13. Climate action, Space and Planetary Science, terrestrial planets [Planets and satellites], composition [Planets and satellites], individual: LHS1140 [Planets and satellites], [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Circumstellar habitable zone, Astrophysics - Earth and Planetary Astrophysics
Abstract

Context. LHS 1140 is an M dwarf known to host two transiting planets at orbital periods of 3.77 and 24.7 days. They were detected with HARPS and Spitzer. The external planet (LHS 1140 b) is a rocky super-Earth that is located in the middle of the habitable zone of this low-mass star. All these properties place this system at the forefront of the habitable exoplanet exploration, and it therefore constitutes a relevant case for further astrobiological studies, including atmospheric observations. Aims. We further characterize this system by improving the physical and orbital properties of the known planets, search for additional planetary-mass components in the system, and explore the possibility of co-orbitals. Methods. We collected 113 new high-precision radial velocity observations with ESPRESSO over a 1.5-yr time span with an average photon-noise precision of 1.07 m s-1. We performed an extensive analysis of the HARPS and ESPRESSO datasets and also analyzed them together with the new TESS photometry. We analyzed the Bayesian evidence of several models with different numbers of planets and orbital configurations. Results. We significantly improve our knowledge of the properties of the known planets LHS 1140 b (Pb ∼ 24.7 days) and LHS 1140 c (Pc ∼ 3.77 days). We determine new masses with a precision of 6% for LHS 1140 b (6.48 ± 0.46 Mpdbl) and 9% for LHS 1140 c (mc = 1.78 ± 0.17 Mpdbl). This reduces the uncertainties relative to previously published values by half. Although both planets have Earth-like bulk compositions, the internal structure analysis suggests that LHS 1140 b might be iron-enriched and LHS 1140 c might be a true Earth twin. In both cases, the water content is compatible to a maximum fraction of 10-12% in mass, which is equivalent to a deep ocean layer of 779 ± 650 km for the habitable-zone planet LHS 1140 b. Our results also provide evidence for a new planet candidate in the system (md = 4.8 ± 1.1Mpdbl) on a 78.9-day orbital period, which is detected through three independent methods. The analysis also allows us to discard other planets above 0.5 Mpdbl for periods shorter than 10 days and above 2 Mpdbl for periods up to one year. Finally, our co-orbital analysis discards co-orbital planets in the tadpole and horseshoe configurations of LHS 1140 b down to 1 Mpdbl with a 95% confidence level (twice better than with the previous HARPS dataset). Indications for a possible co-orbital signal in LHS 1140 c are detected in both radial velocity (alternatively explained by a high eccentricity) and photometric data (alternatively explained by systematics), however. Conclusions. The new precise measurements of the planet properties of the two transiting planets in LHS 1140 as well as the detection of the planet candidate LHS 1140 d make this system a key target for atmospheric studies of rocky worlds at different stellar irradiations., With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)

Published
2020

2. HORuS transmission spectroscopy of 55 Cnc e

Author

A. Diaz Torres, J. Peñate Castro, C. Allende Prieto, H. D. Viera Martín, F. Gracia-Témich, J. Calvo Tovar, C. del Burgo, F. Tenegi, Rafael Rebolo, M. R. Zapatero Osorio, R. J. García López, R. Barreto, M. Abril-Abril, Hugo M. Tabernero, S. Santana-Tschudi, M. F. Gómez-Reñasco, J. I. González Hernández, E. Joven, P. Fernández Izquierdo, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Tabernero, H. M. [https://orcid.org/0000-0002-8087-4298], Fundacao para a Ciencia e a Tecnologia (FCT), Agencia Estatal de Investigación (AEI), Mexican National Council on Science and Technology (CONACYT), Ministerio de Economía y Competitividad (MINECO), Fundacao para a Ciencia e a Tecnologia (FCT), UID/FIS/04434/2019 UIDB/04434/2020 UIDP/04434/2020 PTDC/FIS-AST/28953/2017, Spanish Ministerio de Ciencia Innovacion y Universidades, Fundo Europeu de Desenvolvimento Regional (FEDER) through Programa Operacional Competitividade e Internacionalizacao, and Spanish Ministry of Science Innovation and Universities (MICIU) under the 2013 Ramon y Cajal program

Subjects
Gran Telescopio Canarias, individual: 55 Cnc e [Planets and satellites], FOS: Physical sciences, Astrophysics, 01 natural sciences, Spectral line, 010309 optics, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Absorption (electromagnetic radiation), 010303 astronomy & astrophysics, Spectrograph, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Line (formation), Physics, Earth and Planetary Astrophysics (astro-ph.EP), Astronomy and Astrophysics, Transmission (telecommunications), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, atmospheres [Planets and satellites], Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Order of magnitude, Astrophysics - Earth and Planetary Astrophysics
Abstract

The High Optical Resolution Spectrograph (HORuS) is a new high-resolution echelle spectrograph available on the 10.4 m Gran Telescopio Canarias (GTC). We report on the first HORuS observations of a transit of the super-Earth planet 55 Cnc e. We investigate the presence of Na I and H$\alpha$ in its transmission spectrum and explore the capabilities of HORuS for planetary transmission spectroscopy. Our methodology leads to residuals in the difference spectrum between the in-transit and out-of-transit spectra for the Na I doublet lines of (3.4 $\pm$ 0.4) $\times$ 10$^{-4}$, which sets an upper limit to the detection of line absorption from the planetary atmosphere that is one order of magnitude more stringent that those reported in the literature. We demonstrate that we are able to reach the photon-noise limit in the residual spectra using HORuS to a degree that we would be able to easily detect giant planets with larger atmospheres. In addition, we modelled the structure, chemistry and transmission spectrum of 55 Cnc e using state-of-the-art open source tools., Comment: Accepted for publication in MNRAS

Published
2020

3. A precise architecture characterization of the π Mensae planetary system

Author

Giorgio Pariani, A. Fragoso, Andrea Modigliani, Paolo Molaro, Yann Alibert, Jose Luis Rasilla, Giuseppina Micela, S. Santana Tschudi, David Ehrenreich, Antonino Bianco, Paolo Conconi, Hans Dekker, P. Figueira, Denis Mégevand, Luca Pasquini, Matteo Aliverti, B. Delabre, Filippo Maria Zerbi, T. Bandy, M. A. Monteiro, E. Mueller, R. Génova Santos, C. Maire, A. Suárez Mascareño, Edoardo Maria Alberto Redaelli, Manuel Abreu, Giorgio Calderone, Luca Oggioni, G. Avila, C. Allende Prieto, L. Genolet, Mahmoudreza Oshagh, Nelson J. Nunes, M. Affolter, Stéphane Udry, Vardan Adibekyan, Ennio Poretti, Alessandro Sozzetti, G. Lo Curto, David Alves, Danuta Sosnowska, Alexandre Cabral, Andrea Mehner, J. Knudstrup, Romain Allart, F. Tenegi, Nuno C. Santos, Stefano Cristiani, Marco Riva, Florian Kerber, José Manuel Rebordão, Rafael Rebolo, Olivier Demangeon, C. Lovis, Enric Palle, Damien Ségransan, I. Hughes, Mário J. P. F. G. Monteiro, Vincent Bourrier, J. I. González Hernández, G. Cupani, M. Amate, J. L. Lizon, Roberto Cirami, M. R. Zapatero Osorio, Antonio Gouveia Oliveira, Paolo Santin, João P. Faria, François Bouchy, Baptiste Lavie, S. G. Sousa, Hugo M. Tabernero, Willy Benz, D. Álvarez, Francesco Borsa, T. M. Schmidt, P. Di Marcantonio, Diego Bossini, Francesco Pepe, P. Spano, Pedro Santos, Marco Landoni, S. C. C. Barros, Xavier Dumusque, Olaf Iwert, Cristina Martins, Michael T. Murphy, V. Baldini, C. Broeg, Matteo Genoni, Claudio Cumani, A. Segovia, M. Moschetti, João Coelho, Valentina D'Odorico, Alessio Zanutta, S. Deiries, Igor Coretti, Jorge Lillo-Box, Mario Damasso, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Swiss National Science Foundation (SNSF), Agenzia Spaziale Italiana (ASI), Fundação para a Ciência e a Tecnologia (FCT), Australian Research Council (ARC), Istituto Nazionale Astrofisica (INAF), Pallé, E. [0000-0003-0987-1593], Progetto Premiale 2015 FRONTIERA funding scheme of the Italian Ministry of Education University and Research, ESPRESSO through the SNSF 140649 152721 166227 184618 University and Research OB.FU. 1.05.06.11, SNSF's FLARE Programme, FEDER through COMPETE2020 -Programa Operacional Competitividade e Internacionalizacao 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, Fundação para a Ciência e a Tecnologia (FCT) IF/01312/2014/CP1215/CT0004 IF/00650/2015/CP1273/CT0001 IF/00028/2014/CP1215/CT0002 DL 57/2016/CP1364/CT0005, Spanish Government, Ministerio de Ciencia e Innovación (MICINN) under the 2013 Ramon y Cajal program RYC-2013-14875, Australian Research Council, Istituto Nazionale Astrofisica (INAF) Agenzia Spaziale Italiana (ASI) n.2018-16-HH.0, and Unidad de Excelencia María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC

Subjects
Orbital plane, Brown dwarf, Orbital eccentricity, Context (language use), Astrophysics, 01 natural sciences, Planet, pi Men, individual: π Men [Stars], 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Stars: individual: π Men, radial velocities [Techniques], 010308 nuclear & particles physics, photometric [Techniques], individual: [stars], Astronomy and Astrophysics, Astrometry, Planetary system, Radial velocity, Planetary systems, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Techniques: radial velocities, Astrophysics::Earth and Planetary Astrophysics, Techniques: photometric, Astrophysics - Earth and Planetary Astrophysics
Abstract

Damasso, M. et al., Context. The bright star π Men was chosen as the first target for a radial velocity follow-up to test the performance of ESPRESSO, the new high-resolution spectrograph at the European Southern Observatory's Very Large Telescope. The star hosts a multi-planet system (a transiting 4 M· planet at ∼0.07 au and a sub-stellar companion on a ∼2100-day eccentric orbit), which is particularly suitable for a precise multi-technique characterization. Aims. With the new ESPRESSO observations, which cover a time span of 200 days, we aim to improve the precision and accuracy of the planet parameters and search for additional low-mass companions. We also take advantage of the new photometric transits of π Men c observed by TESS over a time span that overlaps with that of the ESPRESSO follow-up campaign. Methods. We analysed the enlarged spectroscopic and photometric datasets and compared the results to those in the literature. We further characterized the system by means of absolute astrometry with HIPPARCOS and Gaia. We used the high-resolution spectra of ESPRESSO for an independent determination of the stellar fundamental parameters. Results. We present a precise characterization of the planetary system around π Men. The ESPRESSO radial velocities alone (37 nightly binned data with typical uncertainty of 10 cm s-1) allow for a precise retrieval of the Doppler signal induced by π Men c. The residuals show a root mean square of 1.2 m s-1, which is half that of the HARPS data; based on the residuals, we put limits on the presence of additional low-mass planets (e.g. we can exclude companions with a minimum mass less than ∼2 M· within the orbit of π Men c). We improve the ephemeris of π Men c using 18 additional TESS transits, and, in combination with the astrometric measurements, we determine the inclination of the orbital plane of π Men b with high precision (ib =45.8-1.1+1.4 deg). This leads to the precise measurement of its absolute mass mb =14.1-0.4+0.5 MJup, indicating that π Men b can be classified as a brown dwarf. Conclusions. The π Men system represents a nice example of the extreme precision radial velocities that can be obtained with ESPRESSO for bright targets. Our determination of the 3D architecture of the π Men planetary system and the high relative misalignment of the planetary orbital planes put constraints on and challenge the theories of the formation and dynamical evolution of planetary systems. The accurate measurement of the mass of π Men b contributes to make the brown dwarf desert a bit greener., With funding from the Spanish government through the "María de Maeztu Unit of Excellence" accreditation (MDM-2017-0737)

Published
2020

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