TOI-836: A super-Earth and mini-Neptune transiting a nearby K-dwarf
| dc.contributor.author | Hawthorn, Faith | |
| dc.contributor.author | Bayliss, Daniel | |
| dc.contributor.author | Wilson, Thomas G. | |
| dc.contributor.author | Bonfanti, Andrea | |
| dc.contributor.author | Barclay, Thomas | |
| dc.contributor.author | et al | |
| dc.date.accessioned | 2022-09-15T16:36:59Z | |
| dc.date.available | 2022-09-15T16:36:59Z | |
| dc.date.issued | 2022-08-15 | |
| dc.description | Authors: Faith Hawthorn, Daniel Bayliss, Thomas G. Wilson, Andrea Bonfanti, Vardan Adibekyan, Yann Alibert, Sérgio G. Sousa, Karen A. Collins, Edward M. Bryant, Ares Osborn, David J. Armstrong, Lyu Abe, Jack S. Acton, Brett C. Addison, Karim Agabi, Roi Alonso, Douglas R. Alves, Guillem Anglada-Escudé, Tamas Bárczy, Thomas Barclay, David Barrado, Susana C. C. Barros, Wolfgang Baumjohann, Philippe Bendjoya, Willy Benz, Allyson Bieryla, Xavier Bonfils, François Bouchy, Alexis Brandeker, Christopher Broeg, David J.A. Brown, Matthew R. Burleigh, Marco Buttu, Juan Cabrera, Douglas A. Caldwell, Sarah L. Casewell, David Charbonneau, Sébastian Charnoz, Ryan Cloutier, Andrew Collier Cameron, Kevin I. Collins, Dennis M.Conti, Nicolas Crouzet, Szilárd Czismadia, Melvyn B. Davies, Magali Deleuil, Elisa Delgado-Mena, Laetitia Delrez, Olivier D. S. Demangeon, Brice-Olivier Demory, Georgina Dransfield, Xavier Dumusque, Jo Ann Egger, David Ehrenreich, Philipp Eigmüller, Anders Erickson, Zahra Essack, Andrea Fortier, Luca Fossati, Malcolm Fridlund, Maximilian N. Günther, Manuel Güdel, Davide Gandolfi, Harvey Gillard, Michaël Gillon, Crystal Gnilka, Michael R. Goad, Robert F. Goeke, Tristan Guillot, Andreas Hadjigeorghiou, Coel Hellier, Beth A. Henderson, Kevin Heng, Matthew J. Hooton, Keith Horne, Steve B. Howell, Sergio Hoyer, Jonathan M. Irwin, James S. Jenkins, Jon M. Jenkins, Eric L. N. Jensen, Stephen R. Kane, Alicia Kendall, John F. Kielkopf, Laszlo L. Kiss, Gaia Lacedelli, Jacques Laskar, David W. Latham, Alain Lecavalier des Etangs, Adrien Leleu, Monika Lendl, Jorge Lillo-Box, Christophe Lovis, Djamel Mékarnia, Bob Massey, Tamzin Masters, Pierre F. L. Maxted, Valerio Nascimbeni, Louise D. Nielsen, Sean M. O’Brien, Göran Olofsson, Hugh P. Osborn, Isabella Pagano, Enric Pallé, Carina M. Persson, Giampaolo Piotto, Peter Plavchan, Don Pollacco, Didier Queloz, Roberto Ragazzoni, Heike Rauer, Ignasi Ribas, George Ricker, Damien Ségransan, Sébastien Salmon, Alexandre Santerne, Nuno C. Santos, Gaetano Scandariato, François-Xavier Schmider, Richard P. Schwarz, Sara Seager, Avi Shporer, Attila E. Simon, Alexis M. S. Smith, Gregor Srdoc, Manfred Steller, Olga Suarez, Gyula M. Szabó, Johanna Teske, Nicolas Thomas, Rosanna H. Tilbrook, Amaury H. M. J. Triaud, Stéphane Udry, Valérie Van Grootel, Nicholas Walton, Sharon X. Wang, Peter J. Wheatley, Joshua N. Winn, Robert A. Wittenmyer, Hui Zhang | en_US |
| dc.description.abstract | We present the discovery of two exoplanets transiting TOI-836 (TIC 440887364) using data from TESS Sector 11 and Sector 38. TOI-836 is a bright (T = 8.5 mag), high proper motion (∼ 200 mas yr−1 ), low metallicity ([Fe/H]≈−0.28) K-dwarf with a mass of 0.68 ± 0.05 M and a radius of 0.67 ± 0.01R . We obtain photometric follow-up observations with a variety of facilities, and we use these data-sets to determine that the inner planet, TOI-836 b, is a 1.70 ± 0.07R⊕ super-Earth in a 3.82 day orbit, placing it directly within the so-called ‘radius valley’. The outer planet, TOI-836 c, is a 2.59 ± 0.09R⊕ mini-Neptune in an 8.60 day orbit. Radial velocity measurements reveal that TOI-836 b has a mass of 4.5 ± 0.9 M⊕, while TOI836 c has a mass of 9.6 ± 2.6 M⊕. Photometric observations show Transit Timing Variations (TTVs) on the order of 20 minutes for TOI-836 c, although there are no detectable TTVs for TOI-836 b. The TTVs of planet TOI-836 c may be caused by an undetected exterior planet. | en_US |
| dc.description.sponsorship | This work makes use of tpfplotter by J. Lillo-Box (publicly available in www.github.com/jlillo/tpfplotter), which also made use of the python packages astropy, lightkurve, matplotlib and numpy. This research makes use of exoplanet (Foreman-Mackey et al. 2021b) and its dependencies (Agol et al. 2020; Kumar et al. 2019; Astropy Collaboration et al. 2013, 2018; Foreman-Mackey et al. 2021b; Kipping 2013b; Luger et al. 2019b; Salvatier et al. 2016a; Theano Development Team 2016). This paper makes use of EXOFAST (Eastman et al. 2013, 2019) as provided by 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. This publication makes use of The Data & Analysis Center for Exoplanets (DACE), which is a facility based at the University of Geneva (CH) dedicated to extrasolar planets data visualisation, exchange and analysis. DACE is a platform of the Swiss National Centre of Competence in Research (NCCR) PlanetS, federating the Swiss expertise in Exoplanet research. The DACE platform is available at https://dace.unige.ch. This work makes 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. This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by the NASA Explorer Program. Resources supporting this work were provided by the NASA MNRAS 000, 1–21 (2022) 16 F. Hawthorn et al. High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. The TESS team shall assure that the masses of fifty (50) planets with radii less than 4 REarth are determined. We acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research makes use of the Exoplanet Follow-up Observation Program 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 paper includes data collected by the TESS mission that are publicly available from the Mikulski Archive for Space Telescopes (MAST). CHEOPS is an ESA mission in partnership with Switzerland with important contributions to the payload and the ground segment from Austria, Belgium, France, Germany, Hungary, Italy, Portugal, Spain, Sweden, and the United Kingdom. The CHEOPS Consortium would like to gratefully acknowledge the support received by all the agencies, offices, universities, and industries involved. Their flexibility and willingness to explore new approaches were essential to the success of this mission. 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. The MEarth Team gratefully acknowledges funding from the David and Lucile Packard Fellowship for Science and Engineering (awarded to D.C.). This material is based upon work supported by the National Science Foundation under grants AST-0807690, AST-1109468, AST-1004488 (Alan T. Waterman Award), and AST1616624, and upon work supported by the National Aeronautics and Space Administration under Grant No. 80NSSC18K0476 issued through the XRP Program. This work is made possible by a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. 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. The ASTEP project was funded by the Agence Nationale de la Recherche (ANR), the Institut National des Sciences de l’Univers (INSU), the Programme National de Planétologie (PNP), and the Idex UCAJEDI (ANR-15-IDEX-01). The logistics at Concordia is handled by the French Institut Paul-Emile Victor (IPEV) and the Italian Programma Nazionale di Ricerche in Antartide (PNRA). We acknowledge support from the European Space Agency SCI-S Faculty Research Project Programme. This research is supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement n◦ 803193/BEBOP), and from the Science and Technology Facilities Council (STFC; grant n◦ ST/S00193X/1). WASP-South is hosted by the South African Astronomical Observatory and we are grateful for their ongoing support and assistance. Funding for WASP comes from consortium universities and from the UK’s Science and Technology Facilities Council. This study is based on observations collected at the European Southern Observatory under ESO programme 1102.C-0249 (PI: Armstrong). This paper includes data gathered with the 6.5-m Magellan Telescopes located at Las Campanas Observatory, Chile. MINERVA-Australis is supported by Australian Research Council LIEF Grant LE160100001, Discovery Grants DP180100972 and DP220100365, Mount Cuba Astronomical Foundation, and institutional partners University of Southern Queensland, UNSW Sydney, MIT, Nanjing University, George Mason University, University of Louisville, University of California Riverside, University of Florida, and The University of Texas at Austin. We respectfully acknowledge the traditional custodians of all lands throughout Australia, and recognise their continued cultural and spiritual connection to the land, waterways, cosmos, and community. We pay our deepest respects to all Elders, ancestors and descendants of the Giabal, Jarowair, and Kambuwal nations, upon whose lands the MINERVA-Australis facility at Mt Kent is situated. Supported by the international Gemini Observatory, a program of NSF’s NOIRLab, 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 of Argentina, Brazil, Canada, Chile, the Republic of Korea, and the United States of America. Some of the observations in the paper make use of the HighResolution Imaging instrument(s) ‘Alopeke and Zorro. ‘Alopeke and Zorro were 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 and Zorro were mounted on the Gemini North and South telescopes of the international Gemini Observatory, a program of NSF’s NOIRLab, 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 been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation. FH is supported by an STFC studentship. The French group acknowledges financial support from the French Programme National de Planétologie (PNP, INSU). AO is supported by an STFC studentship. This work has been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation. MNG acknowledges support from the European Space Agency (ESA) as an ESA Research Fellow. DJA acknowledges support from the STFC via an Ernest Rutherford Fellowship (ST/R00384X/1). PJW acknowledges support from STFC consolidated grant ST/T000406/1. JSJ greatfully acknowledges support by FONDECYT grant 1201371 and from the ANID BASAL projects ACE210002 and FB210003. JL-B acknowledges financial support received from "la Caixa" Foundation (ID 100010434) with fellowship code LCF/BQ/PI20/11760023, and the Projects No. PID2019- 107061GB-C61 and No. MDM-2017-0737. EDM acknowledges the support from Fundação para a Ciência e a Tecnologia (FCT) by the Investigador FCT contract IF/00849/2015/CP1273/CT0003. SH acknowledges CNES funding through the grant 837319. We acknowledge the support by FCT – Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 – Programa Operacional Competitividade e InternacionalizaMNRAS 000, 1–21 (2022) TOI-836 17 ção 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. S.G.S acknowledges the support from FCT through Investigador FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC). SMO is supported by an STFC studentship. VA acknowledges the support from FCT by the Investigador FCT contract IF/00650/2015/CP1273/CT0001. TGW, ACC, and KH acknowledge support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant ST/R003203/1. YA and MJH acknowledge the support of the Swiss National Fund under grant 200020_172746. SCCB acknowledges support from FCT through FCT contracts nr. IF/01312/2014/CP1215/CT0004. XB and SC acknowledge their role as ESA-appointed CHEOPS science team members. ABr was supported by the SNSA. This project was supported by the CNES. 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. ODSD is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through FCT. B-OD acknowledges support from the Swiss National Science Foundation (PP00P2-190080). 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. MF and CMP gratefully acknowledge the support of the Swedish National Space Agency (DNR 65/19, 174/18). MF acknowledges their role as ESA-appointed CHEOPS science team members. DG gratefully acknowledges financial support from the CRT foundation under Grant No. 2018.2323 “Gaseousor rocky? Unveiling the nature of small worlds”. DG acknowledges their role as ESA-appointed CHEOPS science team members. MG is an F.R.S.-FNRS Senior Research Associate. 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. JL acknowledges their role as ESAappointed CHEOPS science team members. ML acknowledges support of the Swiss National Science Foundation under grant number PCEFP2_194576. PM acknowledges support from STFC research grant number ST/M001040/1. VNa, Ipa, GPi, RRa, and GSc, acknowledge the funding support from Italian Space Agency (ASI) regulated by “Accordo ASI-INAF n. 2013-016-R.0 del 9 luglio 2013 e integrazione del 9 luglio 2015 CHEOPS Fasi A/B/C”. This work was also partially supported by a grant from the Simons Foundation (PI Queloz, grant number 327127). 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. S.S. has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 833925, project STAREX). GyMSz acknowledges the support of the Hungarian National Research, Development and Innovation Office (NKFIH) grant K-125015, a PRODEX Institute Agreement between the ELTE Eötvös Loránd University and the European Space Agency (ESA-D/SCI-LE-2021-0025), the Lendület LP2018-7/2021 grant of the Hungarian Academy of Science and the support of the city of Szombathely. VVG is an F.R.S-FNRS Research Associate. DB has been funded by the Spanish State Research Agency (AEI) Projects No. PID2019-107061GB-C61 and No. MDM-2017-0737 Unidad de Excelencia “María de Maeztu”- Centro de Astrobiología (CSIC/INTA). | en_US |
| dc.description.uri | https://arxiv.org/abs/2208.07328 | en_US |
| dc.format.extent | 21 pages | en_US |
| dc.genre | journal articles | en_US |
| dc.genre | preprints | en_US |
| dc.identifier | doi:10.13016/m2d8jy-qnkv | |
| dc.identifier.uri | https://doi.org/10.48550/arXiv.2208.07328 | |
| dc.identifier.uri | http://hdl.handle.net/11603/25670 | |
| dc.language.iso | en_US | en_US |
| dc.relation.isAvailableAt | The University of Maryland, Baltimore County (UMBC) | |
| dc.relation.ispartof | UMBC Center for Space Sciences and Technology | |
| dc.relation.ispartof | UMBC Faculty Collection | |
| dc.rights | This work was written as part of one of the author's official duties as an Employee of the United States Government and is therefore a work of the United States Government. In accordance with 17 U.S.C. 105, no copyright protection is available for such works under U.S. Law. | en_US |
| dc.rights | Public Domain Mark 1.0 | * |
| dc.rights.uri | http://creativecommons.org/publicdomain/mark/1.0/ | * |
| dc.title | TOI-836: A super-Earth and mini-Neptune transiting a nearby K-dwarf | en_US |
| dc.type | Text | en_US |
| dcterms.creator | https://orcid.org/0000-0001-7139-2724 | en_US |