The TESS-Keck Survey. XXII. A Sub-Neptune Orbiting TOI-1437
- Creators
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Pidhorodetska, Daria1
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Gilbert, Emily A.2
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Kane, Stephen R.1
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Barclay, Thomas3
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Polanski, Alex S.4
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Hill, Michelle L.1
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Stassun, Keivan G.5
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Giacalone, Steven6
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Ciardi, David R.7
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Boyle, Andrew W.6
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Howell, Steve B.8
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Lillo-Box, Jorge9
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MacDougall, Mason G.10
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Fetherolf, Tara1, 11
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Batalha, Natalie M.12
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Crossfield, Ian J. M.4
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Dressing, Courtney13
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Fulton, Benjamin7
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Howard, Andrew W.6
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Huber, Daniel14, 15
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Isaacson, Howard13, 16
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Petigura, Erik A.10
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Robertson, Paul17
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Weiss, Lauren M.18
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Angelo, Isabel10
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Beard, Corey17
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Behmard, Aida19
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Blunt, Sarah20
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Brinkman, Casey L.14
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Chontos, Ashley21
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Dai, Fei6, 14
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Dalba, Paul A.12
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Holcomb, Rae17
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Lubin, Jack10, 17
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Mayo, Andrew W.13
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Murphy, Joseph M. Akana12
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Rice, Malena22
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Rubenzahl, Ryan6
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Scarsdale, Nicholas12
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Turtelboom, Emma V.13
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Tyler, Dakotah10
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Van Zandt, Judah10
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Schwieterman, Edward W.1
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1.
University of California, Riverside
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2.
Jet Propulsion Lab
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3.
Goddard Space Flight Center
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4.
University of Kansas
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5.
Vanderbilt University
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6.
California Institute of Technology
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7.
NASA Exoplanet Science Institute
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8.
Ames Research Center
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9.
Centro de Astrobiología
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10.
University of California, Los Angeles
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11.
California State University, San Marcos
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12.
University of California, Santa Cruz
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13.
University of California, Berkeley
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14.
University of Hawaii at Manoa
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15.
University of Sydney
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16.
University of Southern Queensland
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17.
University of California, Irvine
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18.
University of Notre Dame
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19.
American Museum of Natural History
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20.
Northwestern University
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21.
Princeton University
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22.
Yale University
Abstract
Exoplanet discoveries have revealed a dramatic diversity of planet sizes across a vast array of orbital architectures. Sub-Neptunes are of particular interest; due to their absence in our own solar system, we rely on demographics of exoplanets to better understand their bulk composition and formation scenarios. Here, we present the discovery and characterization of TOI-1437 b, a sub-Neptune with a 18.84 day orbit around a near-solar analog (M⋆ = 1.10 ± 0.10 M☉, R⋆=1.17 ± 0.12 R☉). The planet was detected using photometric data from the Transiting Exoplanet Survey Satellite (TESS) mission and radial velocity (RV) follow-up observations were carried out as a part of the TESS-Keck Survey using both the HIRES instrument at Keck Observatory and the Levy Spectrograph on the Automated Planet Finder telescope. A combined analysis of these data reveal a planet radius of Rp = 2.24 ± 0.23 R⊕ and a mass measurement of Mp = 9.6 ± 3.9 M⊕). TOI-1437 b is one of few (∼50) known transiting sub-Neptunes orbiting a solar-mass star that has a RV mass measurement. As the formation pathway of these worlds remains an unanswered question, the precise mass characterization of TOI-1437 b may provide further insight into this class of planet.
Copyright and License
© 2024. The Author(s). Published by the American Astronomical Society.
Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.
Acknowledgement
We thank the time assignment committees of the University of California, the California Institute of Technology, NASA, and the University of Hawaii for supporting the TESS-Keck Survey with observing time at Keck Observatory and on the Automated Planet Finder. We thank NASA for funding associated with our Key Strategic Mission Support project. We gratefully acknowledge the efforts and dedication of the Keck Observatory staff for support of HIRES and remote observing. We recognize and acknowledge the cultural role and reverence that the summit of Maunakea has within the indigenous Hawaiian community. We are deeply grateful to have the opportunity to conduct observations from this mountain. We thank Ken and Gloria Levy, who supported the construction of the Levy Spectrometer on the Automated Planet Finder. We thank the University of California and Google for supporting Lick Observatory and the UCO staff for their dedicated work scheduling and operating the telescopes of Lick Observatory. This paper is based on data collected by the TESS mission. Funding for the TESS mission is provided by the NASA Explorer Program. This paper includes data collected by the TESS mission that are publicly available from the Mikulski Archive for Space Telescopes (MAST). Data was taken from the TESS Input Catalog (STScI 2018).
D.P. acknowledges support from the NASA FINESST Fellowship issued via grant No. 80NSSC22K1319.
M.L.H. would like to acknowledge NASA support via the FINESST Planetary Science Division, NASA award number 80NSSC21K1536.
D.R.C. acknowledges partial support from NASA grant 18-2XRP18_2-0007.
D.H. acknowledges support from the Alfred P. Sloan Foundation, the National Aeronautics and Space Administration (80NSSC21K0652) and the Australian Research Council (FT200100871).
J.L.-B. was partly funded by the Ramón y Cajal program with code RYC2021-031640-I. and by the Spanish MCIN/AEI/10.13039/501100011033 grant PID2019-107061GB-C61.
J.M.A.M. is supported by the National Science Foundation Graduate Research Fellowship Program under grant No. DGE-1842400.
This research has made use of the Exoplanet Follow-up Observation Program (ExoFOP; DOI: 10.26134/ExoFOP5) website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program.
Some of the observations in this paper made use of the High-Resolution Imaging instrument 'Alopeke and were obtained under Gemini LLP Proposal Number: GN/S-2021A-LP-105. 'Alopeke was 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 was mounted on the Gemini North telescope of the international Gemini Observatory, 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 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 research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004).
The authors thank Eric Mamajek for helpful discussions that improved the quality of this manuscript.
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Additional details
- National Aeronautics and Space Administration
- 80NSSC22K1319
- National Aeronautics and Space Administration
- 80NSSC21K1536
- National Aeronautics and Space Administration
- 18-2XRP18_2-0007
- Alfred P. Sloan Foundation
- National Aeronautics and Space Administration
- 80NSSC21K0652
- Australian Research Council
- FT200100871
- Instituo Cajal
- RYC2021-031640-I
- Ministerio de Ciencia e Innovación
- PID2019-107061GB-C61
- National Science Foundation
- DGE-1842400
- Jet Propulsion Laboratory
- National Aeronautics and Space Administration
- 80NM0018D0004
- National Aeronautics and Space Administration
- NASA FINESST Fellowship -
- National Science Foundation
- Astronomy and Astrophysics Postdoctoral Fellowship -
- Accepted
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2024-07-23Accepted
- Available
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2024-08-30Published
- Caltech groups
- Astronomy Department, Infrared Processing and Analysis Center (IPAC)
- Publication Status
- Published