A Caltech Library Service

TOI-1235 b: a keystone super-Earth for testing radius valley emergence models around early M dwarfs

Cloutier, Ryan and Rodriguez, Joseph E. and Irwin, Jonathan and Charbonneau, David and Stassun, Keivan G. and Mortier, Annelies and Latham, David W. and Isaacson, Howard and Howard, Andrew W. and Udry, Stéphane and Wilson, Thomas G. and Watson, Christopher A. and Pinamonti, Matteo and Lienhard, Florian and Giacobbe, Paolo and Guerra, Pere and Collins, Karen A. and Beiryla, Allyson and Esquerdo, Gilbert A. and Matthews, Elisabeth and Crossfield, Ian J. M. and Winters, Jennifer G. and Nava, Chantanelle and Ment, Kristo and Lopez, Eric D. and Ricker, George and Vanderspek, Roland and Seager, Sara and Jenkins, Jon M. and Ting, Eric B. and Tenenbaum, Peter and Sozzetti, Alessandro and Sha, Lizhou and Ségransan, Damien and Schlieder, Joshua E. and Sasselov, Dimitar and Roy, Arpita and Robertson, Paul and Rice, Ken and Poretti, Ennio and Piotto, Giampaolo and Phillips, David and Pepper, Joshua and Pepe, Francesco and Molinari, Emilio and Mocnik, Teo and Micela, Giuseppina and Mayor, Michel and Matson, Rachel A. and Martinez Fiorenzano, Aldo F. and Mallia, Franco and Lubin, Jack and Lovis, Christophe and López-Morales, Mercedes and Kosiarek, Molly R. and Kielkopf, John F. and Kane, Stephen R. and Jensen, Eric L. N. and Isopi, Giovanni and Huber, Daniel and Howell, Steve B. and Hill, Michelle L. and Harutyunyan, Avet and Gonzales, Erica J. and Giacalone, Steven and Ghedina, Adriano and Ercolino, Andrea and Dumusque, Xavier and Dressing, Courtney D. and Damasso, Mario and Dalba, Paul A. and Cosentino, Rosario and Conti, Dennis M. and Colón, Knicole D. and Collins, Kevin I. and Cameron, Andrew Collier and Ciardi, David and Christiansen, Jessie and Chontos, Ashley and Cecconi, Massimo and Caldwell, Douglas A. and Burke, Christopher and Buchhave, Lars and Beichman, Charles and Behmard, Aida and Beard, Corey and Murphy, Joseph M. Akana and Furlan, Elise (2020) TOI-1235 b: a keystone super-Earth for testing radius valley emergence models around early M dwarfs. Astronomical Journal, 160 (1). Art. No. 22. ISSN 1538-3881. doi:10.3847/1538-3881/ab9534.

[img] PDF - Published Version
See Usage Policy.

[img] PDF - Submitted Version
See Usage Policy.


Use this Persistent URL to link to this item:


Small planets on close-in orbits tend to exhibit envelope mass fractions of either effectively zero or up to a few percent depending on their size and orbital period. Models of thermally driven atmospheric mass loss and of terrestrial planet formation in a gas-poor environment make distinct predictions regarding the location of this rocky/nonrocky transition in period–radius space. Here we present the confirmation of TOI-1235 b (P = 3.44 days, r_p=1.738^(+0.087)_(−0.076) R⊕), a planet whose size and period are intermediate between the competing model predictions, thus making the system an important test case for emergence models of the rocky/nonrocky transition around early M dwarfs (R_s = 0.630 ± 0.015 R⊙, M_s = 0.640 ± 0.016 M⊙). We confirm the TESS planet discovery using reconnaissance spectroscopy, ground-based photometry, high-resolution imaging, and a set of 38 precise radial velocities (RVs) from HARPS-N and HIRES. We measure a planet mass of 6.91^(+0.75)_(−0.85) M⊕, which implies an iron core mass fraction of 20⁺¹⁵₋₁₂% in the absence of a gaseous envelope. The bulk composition of TOI-1235 b is therefore consistent with being Earth-like, and we constrain an H/He envelope mass fraction to be <0.5% at 90% confidence. Our results are consistent with model predictions from thermally driven atmospheric mass loss but not with gas-poor formation, suggesting that the former class of processes remains efficient at sculpting close-in planets around early M dwarfs. Our RV analysis also reveals a strong periodicity close to the first harmonic of the photometrically determined stellar rotation period that we treat as stellar activity, despite other lines of evidence favoring a planetary origin (P=21.8^(+0.9)_(−0.8) days, m_p sin i=13.0^(+3.8)_(−5.3) M⊕) that cannot be firmly ruled out by our data.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Cloutier, Ryan0000-0001-5383-9393
Rodriguez, Joseph E.0000-0001-8812-0565
Charbonneau, David0000-0002-9003-484X
Stassun, Keivan G.0000-0002-3481-9052
Latham, David W.0000-0001-9911-7388
Isaacson, Howard0000-0002-0531-1073
Howard, Andrew W.0000-0001-8638-0320
Collins, Karen A.0000-0001-6588-9574
Esquerdo, Gilbert A.0000-0002-9789-5474
Crossfield, Ian J. M.0000-0002-1835-1891
Winters, Jennifer G.0000-0001-6031-9513
Ment, Kristo0000-0001-5847-9147
Vanderspek, Roland0000-0001-6763-6562
Seager, Sara0000-0002-6892-6948
Jenkins, Jon M.0000-0002-4715-9460
Ting, Eric B.0000-0002-8219-9505
Sha, Lizhou0000-0001-5401-8079
Schlieder, Joshua E.0000-0001-5347-7062
Sasselov, Dimitar0000-0001-7014-1771
Roy, Arpita0000-0001-8127-5775
Robertson, Paul0000-0003-0149-9678
Pepper, Joshua0000-0002-3827-8417
Matson, Rachel A.0000-0001-7233-7508
López-Morales, Mercedes0000-0003-3204-8183
Kosiarek, Molly R.0000-0002-6115-4359
Kane, Stephen R.0000-0002-7084-0529
Jensen, Eric L. N.0000-0002-4625-7333
Huber, Daniel0000-0001-8832-4488
Howell, Steve B.0000-0002-2532-2853
Hill, Michelle L.0000-0002-0139-4756
Gonzales, Erica J.0000-0002-9329-2190
Dressing, Courtney D.0000-0001-8189-0233
Dalba, Paul A.0000-0002-4297-5506
Colón, Knicole D.0000-0001-8020-7121
Collins, Kevin I.0000-0003-2781-3207
Cameron, Andrew Collier0000-0002-8863-7828
Ciardi, David0000-0002-5741-3047
Christiansen, Jessie0000-0002-8035-4778
Chontos, Ashley0000-0003-1125-2564
Caldwell, Douglas A.0000-0003-1963-9616
Burke, Christopher0000-0002-7754-9486
Buchhave, Lars0000-0003-1605-5666
Beichman, Charles0000-0002-5627-5471
Behmard, Aida0000-0003-0012-9093
Murphy, Joseph M. Akana0000-0001-8898-8284
Furlan, Elise0000-0001-9800-6248
Additional Information:© 2020 The American Astronomical Society. Received 2020 April 13; Accepted 2020 May 19; Published 2020 June 12. R.C. is supported by a grant from the National Aeronautics and Space Administration in support of the TESS science mission. We thank Andrew Vanderburg for enlightening discussions regarding the TESS light curves. M.P. gratefully acknowledges the support from the European Union Seventh Framework Programme (FP7/2007-2013) under grant agreement No. 313014 (ETAEARTH). J.M.A.M. gratefully acknowledges support from the National Science Foundation Graduate Research Fellowship Program under grant No. DGE-1842400. J.M.A.M. also thanks 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. This work has been partially supported by the National Aeronautics and Space Administration under grant No. NNX17AB59G issued through the Exoplanets Research Program. We acknowledge the use of public TESS Alert data from the pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. 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 on work supported by the National Science Foundation under grants AST-0807690, AST-1109468, AST-1004488 (Alan T. Waterman Award), and AST-1616624. 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 material is based on work supported by the National Aeronautics and Space Administration under grant No. 80NSSC18K0476 issued through the XRP Program. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This work has made use of data from the European Space Agency (ESA) mission Gaia (, processed by the Gaia Data Processing and Analysis Consortium (DPAC, Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This work makes use of observations from the LCOGT network. Based on observations made with the Italian Telescopio Nazionale Galileo (TNG) operated by the Fundación Galileo Galilei (FGG) of the Istituto Nazionale di Astrofisica (INAF) at the Observatorio del Roque de los Muchachos (La Palma, Canary Islands, Spain). The HARPS-N project has been funded by the Prodex Program of the Swiss Space Office (SSO), the Harvard University Origins of Life Initiative (HUOLI), the Scottish Universities Physics Alliance (SUPA), the University of Geneva, the Smithsonian Astrophysical Observatory (SAO), the Italian National Astrophysical Institute (INAF), the University of St Andrews, Queens University Belfast, and the University of Edinburgh. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. 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. Based on observations obtained at the international Gemini Observatory under the program GN-2019B-LP-101, 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 Observatory 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). Some of the observations in the paper made use of the High-Resolution Imaging instrument 'Alopeke. Facilities: TESS - , MEarth-North - , TRES - , LCOGT - , Gemini/NIRI - , TNG/HARPS-N - , Keck/HIRES. - Software: AstroImageJ (Collins et al. 2017), astropy (Astropy Collaboration et al. 2013, 2018), BANZAI (McCully et al. 2018), batman (Kreidberg 2015), BGLS (Mortier et al. 2015), celerite (Foreman-Mackey et al. 2017), emcee (Foreman-Mackey et al. 2013), EvapMass (Owen & Campos Estrada 2020), EXOFAST (Eastman et al. 2013), EXOFASTv2 (Eastman et al. 2019), exoplanet (Foreman-Mackey et al. 2019), PyMC3 (Salvatier et al. 2016), scipy (Virtanen et al. 2020), SpecMatch-Emp (Yee et al. 2017), STARRY (Luger et al. 2019), Tapir (Jensen 2013), TERRA (Anglada-Escudé & Butler 2012), triceratops (Giacalone & Dressing 2020), vespa (Morton 2012).
Group:Astronomy Department, Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
European Research Council (ERC)313014
NSF Graduate Research FellowshipDGE-1842400
Large Synoptic Survey Telescope CorporationUNSPECIFIED
Brinson FoundationUNSPECIFIED
Gordon and Betty Moore FoundationUNSPECIFIED
David and Lucile Packard FoundationUNSPECIFIED
John Templeton FoundationUNSPECIFIED
Gaia Multilateral AgreementUNSPECIFIED
W. M. Keck FoundationUNSPECIFIED
Subject Keywords:Radial velocity ; M dwarf stars ; Transit photometry ; Exoplanet formation ; Exoplanet structure
Issue or Number:1
Classification Code:Unified Astronomy Thesaurus concepts: Radial velocity (1332); M dwarf stars (982); Transit photometry (1709); Exoplanet formation (492); Exoplanet structure (495)
Record Number:CaltechAUTHORS:20200420-110205450
Persistent URL:
Official Citation:Ryan Cloutier et al 2020 AJ 160 22
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:102653
Deposited By: Tony Diaz
Deposited On:20 Apr 2020 18:57
Last Modified:16 Nov 2021 18:14

Repository Staff Only: item control page