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Planetary System Around the Nearby M Dwarf GJ 357 Including a Transiting, Hot, Earth-Sized Planet Optimal for Atmospheric Characterization

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Planetary system around the nearby M dwarf GJ 357 including a transiting, hot, Earth-sized planet optimal for atmospheric characterization The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Luque, R., et al., "Planetary system around the nearby M dwarf GJ 357 including a transiting, hot, Earth-sized planet optimal for atmospheric characterization." Astronomy & Astrophysics 628 (2019): no. A39 doi 10.1051/0004-6361/201935801 ©2019 Author(s) As Published 10.1051/0004-6361/201935801 Publisher EDP Sciences Version Final published version Citable link https://hdl.handle.net/1721.1/125897 Terms of Use Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. A&A 628, A39 (2019) Astronomy https://doi.org/10.1051/0004-6361/201935801 & © ESO 2019 Astrophysics Planetary system around the nearby M dwarf GJ 357 including a transiting, hot, Earth-sized planet optimal for atmospheric characterization? R. Luque1,2, E. Pallé1,2, D. Kossakowski3, S. Dreizler4, J. Kemmer5, N. Espinoza3, J. Burt6,??, G. Anglada-Escudé7,8, V. J. S. Béjar1,2, J. A. Caballero9, K. A. Collins10, K. I. Collins11, M. Cortés-Contreras9, E. Díez-Alonso12,13, F. Feng14, A. Hatzes15, C. Hellier16, T. Henning3, S. V. Jeffers4, L. Kaltenegger17, M. Kürster3, J. Madden17, K. Molaverdikhani3, D. Montes12, N. Narita1,18,19,20, G. Nowak1,2, A. Ofir21, M. Oshagh4, H. Parviainen1,2, A. Quirrenbach5, S. Reffert5, A. Reiners4, C. Rodríguez-López8, M. Schlecker3, S. Stock5, T. Trifonov3, J. N. Winn22, M. R. Zapatero Osorio23, M. Zechmeister4, P. J. Amado8, D. R. Anderson16, N. E. Batalha24, F. F. Bauer8, P. Bluhm5, C. J. Burke6, R. P. Butler14, D. A. Caldwell25,26, G. Chen27, J. D. Crane28, D. Dragomir6,???, C. D. Dressing29, S. Dynes6, J. M. Jenkins26, A. Kaminski5, H. Klahr3, T. Kotani18,20, M. Lafarga30,31, D. W. Latham10, P. Lewin32, S. McDermott33, P. Montañés-Rodríguez1,2, J. C. Morales30,31, F. Murgas1,2, E. Nagel34, S. Pedraz35, I. Ribas30,31, G. R. Ricker6, P. Rowden36, S. Seager6,37,38, S. A. Shectman28, M. Tamura18,20,39, J. Teske28,???, J. D. Twicken25,26, R. Vanderspeck6, S. X. Wang14, and B. Wohler25,26 (Affiliations can be found after the references) Received 29 April 2019 / Accepted 27 June 2019 ABSTRACT We report the detection of a transiting Earth-size planet around GJ 357, a nearby M2.5 V star, using data from the Transiting Exoplanet Survey Satellite (TESS). GJ 357 b (TOI-562.01) is a transiting, hot, Earth-sized planet (Teq = 525 ± 11 K) with a radius of Rb = 1:217 ± 0:084 R⊕ and an orbital period of Pb = 3:93 d. Precise stellar radial velocities from CARMENES and PFS, as well as archival data from HIRES, UVES, and HARPS also display a 3.93-day periodicity, confirming the planetary nature and leading to a planetary mass of Mb = 1:84 ± 0:31 M⊕. In addition to the radial velocity signal for GJ 357 b, more periodicities are present in the data indicating the presence of two further planets in the system: GJ 357 c, with a minimum mass of Mc = 3:40 ± 0:46 M⊕ in a 9.12 d orbit, and GJ 357 d, with a minimum mass of Md = 6:1 ± 1:0 M⊕ in a 55.7 d orbit inside the habitable zone. The host is relatively inactive and exhibits a photometric rotation period of Prot = 78 ± 2 d. GJ 357 b is to date the second closest transiting planet to the Sun, making it a prime target for further investigations such as transmission spectroscopy. Therefore, GJ 357 b represents one of the best terrestrial planets suitable for atmospheric characterization with the upcoming JWST and ground-based ELTs. Key words. planetary systems – techniques: photometric – techniques: radial velocities – stars: individual: Gl 357 – stars: late-type 1. Introduction Only six of the abovementioned eleven systems con- tain planets with masses below 10 M⊕: LHS 1140 b and c To date nearly 200 exoplanets have been discovered orbiting (GJ 3053, Dittmann et al. 2017; Ment et al. 2019), K2-3 b approximately 100 M dwarfs in the solar neighborhood (e.g., and c (PM J11293–0127, Almenara et al. 2015; Sinukoff et al. Bonfils et al. 2013; Rowe et al. 2014; Trifonov et al. 2018; Ribas 2016), K2-18 b (PM J11302+0735, Cloutier et al. 2017; Sarkis et al. 2018). Some of these orbit near to or in the habitable et al. 2018), GJ 1214 b (LHS 3275 b, Harpsøe et al. 2013), zone (e.g., Udry et al. 2007; Anglada-Escudé et al. 2013, 2016; GJ 1132 (Berta-Thompson et al. 2015; Bonfils et al. 2018), Tuomi & Anglada-Escudé 2013; Dittmann et al. 2017; Reiners and b–g planets of TRAPPIST-1 (Gillon et al. 2016, 2017). et al. 2018). However, only 11 M dwarf planet systems have been However, only three planets with masses similar to Earth orbit detected with both the transit as well as the radial velocity (RV) M dwarfs of moderate brightness (J = 9.2–9.8 mag): GJ 1132 b method, which allows us to derive their density from their mea- (1:66 ± 0:23 M⊕), LHS 1140 c (1:81 ± 0:39 M⊕), and K2-18 b sured radius and mass, informing us about its bulk properties. +2:1 (2.1−1:3 M⊕). Systems hosting small terrestrial exoplanets orbit- When transit timing variation (TTV) mass measurements are ing bright stars are ideal not only from the perspective of precise included, TRAPPIST-1 (2MUCD 12171, Gillon et al. 2017) rep- mass measurements with ground-based instruments, but also for resents the 12th M dwarf planet system with mass and radius further orbital (e.g., obliquity determination) and atmospheric measurements. characterization using current and future observatories (see, e.g., ? RV data are only available at the CDS via anonymous ftp to Batalha et al. 2018). cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc. The Transiting Exoplanet Survey Satellite (TESS, Ricker u-strasbg.fr/viz-bin/qcat?J/A+A/628/A39 et al. 2015) mission is an observatory that was launched to find ?? Torres Fellow. small planets transiting small, bright stars. Indeed, since the ??? NASA Hubble Fellow. start of scientific operations in July 2018, TESS has already Article published by EDP Sciences A39, page 1 of 18 A&A 628, A39 (2019) uncovered over 600 new planet candidates, and is quickly Li et al. 2019), for example, even-odd transits comparison, eclips- increasing the sample of known Earths and super-Earths around ing binary discrimination tests, ghost diagnostic tests to help rule small M-type stars (Vanderspek et al. 2019; Günther et al. out scattered light, or background eclipsing binaries, among oth- 2019; Kostov et al. 2019). In this paper, we present the dis- ers. The report indicates that the dimming events are associated covery of three small planets around a bright M dwarf, one with significant image motion, which is usually indicative of a of which, GJ 357 b, is an Earth-sized transiting exoplanet dis- background eclipsing binary. However, in this case, the reported covered using photometry from the TESS mission. To date, information is meaningless because the star is saturated. On the GJ 357 b is the second nearest (d = 9:44 pc) transiting planet to other hand, the transit source is coincident with the core of the the Sun after HD 219134 b (Motalebi et al. 2015, d = 6:53 pc), stellar point spread function (PSF), so the transit events happen and the closest around an M dwarf. Besides, it is amenable to on the target and not, for example, on a nearby bright star. future detailed atmospheric characterization, opening the door to We also performed an independent analysis of the TESS light new studies for atmospheric characterization of Earth-like planet curve in order to confirm the DVR analysis and search for addi- atmospheres (Pallé et al. 2009). tional transit signals. An iterative approach was employed: in The paper is structured as follows. Section2 presents the each iteration the same raw data were detrended and outliers- TESS photometry used for the discovery of GJ 357 b. Section3 rejected, a signal was identified and then modeled, and that presents ground-based observations of the star including seeing- model was temporarily divided-out during the detrending of the limited photometric monitoring, high-resolution imaging, and next iteration to produce a succession of improving models, until precise RVs. Section4 presents a detailed analysis of the stellar the χ2 converges. The raw photometry was detrended by fitting properties of GJ 357. Section5 presents an analysis of the avail- a truncated Fourier series, starting from the natural period of able data in order to constrain the planetary properties of the sys- twice the data span, and all of its harmonics, down to some tem, including precise mass constraints on GJ 357 b along with “protected” time span to make sure the filter does not modify the a detection and characterization of two additional planets in the shape of the transit itself. We used a protected time span of 0.5 d, system, GJ 357 c and GJ 357 d. Section6 presents a discussion and this series was iteratively fitted with 4σ rejection. Finally, of our results and, finally, Sect.7 presents our conclusions. OptimalBLS (Ofir 2014) is used to identify the transit signal, which is then modeled using the Mandel & Agol(2002) model and the differential evolution Markov chain Monte Carlo algo- 2.
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    Astronomy & Astrophysics manuscript no. HD219134˙published © ESO 2019 October 31, 2019 From the stellar properties of HD 219134 to the internal compositions of its transiting exoplanets. R. Ligi1, C. Dorn2, A. Crida3;4, Y. Lebreton5;6, O. Creevey3, F. Borsa1, D. Mourard3, N. Nardetto3, I. Tallon-Bosc7, F. Morand3, E. Poretti1. 1 INAF-Osservatorio Astronomico di Brera, Via E. Bianchi 46, I-23807 Merate, Italy e-mail: [email protected] 2 University of Zurich, Institut of Computational Sciences, University of Zurich, Winterthurerstrasse 190, CH-8057, Zurich, Switzerland 3 Universite´ Coteˆ d’Azur, Observatoire de la Coteˆ d’Azur, CNRS, Laboratoire Lagrange, Bd de l’Observatoire, CS 34229, 06304 Nice cedex 4, France 4 Institut Universitaire de France, 103 Boulevard Saint-Michel, 75005 Paris, France 5 LESIA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universites,´ UPMC Univ. Paris 06, Univ. Paris Diderot, Sorbonne Paris Cite,´ 92195 Meudon Cedex, France 6 Univ. Rennes, CNRS, IPR (Institut de Physique de Rennes) - UMR 6251, F-35000 Rennes, France 7 Univ. Lyon, Univ. Lyon1, Ens de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574, F-69230 Saint-Genis- Laval, France Received 5 July 2019 / Accepted 20 September 2019 ABSTRACT Context. The harvest of exoplanet discoveries has opened the area of exoplanet characterisation. But this cannot be achieved without a careful analysis of the host star parameters. Aims. The system of HD 219134 hosts two transiting exoplanets and at least two additional non-transiting exoplanets. We revisit the properties of this system using direct measurements of the stellar parameters to investigate the composition of the two transiting exoplanets.
  • L0 and M0 Photometry of Ultracool Dwarfs D

    L0 and M0 Photometry of Ultracool Dwarfs D

    The Astronomical Journal, 127:3516–3536, 2004 June # 2004. The American Astronomical Society. All rights reserved. Printed in U.S.A. L0 AND M0 PHOTOMETRY OF ULTRACOOL DWARFS D. A. Golimowski,1 S. K. Leggett,2 M. S. Marley,3 X. Fan,4 T. R. Geballe,5 G. R. Knapp,6 F. J. Vrba,7 A. A. Henden,7 C. B. Luginbuhl,7 H. H. Guetter,7 J. A. Munn,7 B. Canzian,7 W. Zheng,1 Z. I. Tsvetanov,8 K. Chiu,1 K. Glazebrook,1 E. A. Hoversten,1 D. P. Schneider,9,10 and J. Brinkmann10, 11 Received 2003 November 13; accepted 2004 February 18 ABSTRACT We have compiled L0 (3.4–4.1 m) and M0 (4.6–4.8 m) photometry of 63 single and binary M, L, and T dwarfs obtained at the United Kingdom Infrared Telescope using the Mauna Kea Observatory filter set. This compilation includes new L0 measurements of eight L dwarfs and 13 T dwarfs and new M0 measurements of seven L dwarfs, five T dwarfs, and the M1 dwarf Gl 229A. These new data increase by factors of 0.6 and 1.6, 0 0 respectively, the numbers of ultracool dwarfs (Teff P 2400 K) for which L and M measurements have been 0 reported. We compute Lbol,BCK ,andTeff for 42 dwarfs whose flux-calibrated JHK spectra, L photometry, and trigonometric parallaxes are available, and we estimate these quantities for nine other dwarfs whose parallaxes and flux-calibrated spectra have been obtained. BCK is a well-behaved function of near-infrared spectral type with a dispersion of 0.1 mag for types M6–T5; it is significantly more scattered for types T5–T9.
  • Stellar Encounters with the Oort Cloud Based on Hipparcos Data Joan Garciça-Saçnchez, 1 Robert A. Preston, Dayton L. Jones, and Paul R

    Stellar Encounters with the Oort Cloud Based on Hipparcos Data Joan Garciça-Saçnchez, 1 Robert A. Preston, Dayton L. Jones, and Paul R

    THE ASTRONOMICAL JOURNAL, 117:1042È1055, 1999 February ( 1999. The American Astronomical Society. All rights reserved. Printed in U.S.A. STELLAR ENCOUNTERS WITH THE OORT CLOUD BASED ON HIPPARCOS DATA JOAN GARCI A-SA NCHEZ,1 ROBERT A. PRESTON,DAYTON L. JONES, AND PAUL R. WEISSMAN Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109 JEAN-FRANCÓ OIS LESTRADE Observatoire de Paris-Section de Meudon, Place Jules Janssen, F-92195 Meudon, Principal Cedex, France AND DAVID W. LATHAM AND ROBERT P. STEFANIK Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 Received 1998 May 15; accepted 1998 September 4 ABSTRACT We have combined Hipparcos proper-motion and parallax data for nearby stars with ground-based radial velocity measurements to Ðnd stars that may have passed (or will pass) close enough to the Sun to perturb the Oort cloud. Close stellar encounters could deÑect large numbers of comets into the inner solar system, which would increase the impact hazard at Earth. We Ðnd that the rate of close approaches by star systems (single or multiple stars) within a distance D (in parsecs) from the Sun is given by N \ 3.5D2.12 Myr~1, less than the number predicted by a simple stellar dynamics model. However, this value is clearly a lower limit because of observational incompleteness in the Hipparcos data set. One star, Gliese 710, is estimated to have a closest approach of less than 0.4 pc 1.4 Myr in the future, and several stars come within 1 pc during a ^10 Myr interval.