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TESS Spots a Compact System of Super-Earths around the Naked-eye Star HR 858

Vanderburg, Andrew and Fulton, Benjamin J. (2019) TESS Spots a Compact System of Super-Earths around the Naked-eye Star HR 858. Astrophysical Journal Letters, 881 (1). Art. No. L19. ISSN 2041-8213.

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Transiting Exoplanet Survey Satellite (TESS) observations have revealed a compact multiplanet system around the sixth-magnitude star HR 858 (TIC 178155732, TOI 396), located 32 pc away. Three planets, each about twice the size of Earth, transit this slightly evolved, late F-type star, which is also a member of a visual binary. Two of the planets may be in mean motion resonance. We analyze the TESS observations, using novel methods to model and remove instrumental systematic errors, and combine these data with follow-up observations taken from a suite of ground-based telescopes to characterize the planetary system. The HR 858 planets are enticing targets for precise radial velocity observations, secondary eclipse spectroscopy, and measurements of the Rossiter–McLaughlin effect.

Item Type:Article
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URLURL TypeDescription Paper
Vanderburg, Andrew0000-0001-7246-5438
Fulton, Benjamin J.0000-0003-3504-5316
Additional Information:© 2019 The American Astronomical Society. Received 2019 May 7; revised 2019 July 11; accepted 2019 July 12; published 2019 August 9. We thank Jen Winters and Michael Fausnaugh for helpful discussions. We acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Funding for the TESS mission is provided by NASA's Science Mission directorate. 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. AV's work was performed under contract with the California Institute of Technology/Jet Propulsion Laboratory funded by NASA through the Sagan Fellowship Program executed by the NASA Exoplanet Science Institute. C.X.H. and J.B. acknowledge support from MIT's Kavli Institute as Torres postdoctoral fellows. J.A.D. and J.N.W. acknowledge support from the Heising–Simons Foundation. J.E.R. is supported by the Harvard Future Faculty Leaders Postdoctoral fellowship. J.C.B is supported by the NSF Graduate Research Fellowship grants No. DGE 1256260 and a graduate fellowship from the Leinweber Center for Theoretical Physics. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5–26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts. 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. MINERVA-Australis is supported by Australian Research Council LIEF grant LE160100001, Discovery grant DP180100972, Mount Cuba Astronomical Foundation, and institutional partners University of Southern Queensland, UNSW Australia, MIT, Nanjing University, George Mason University, University of Louisville, University of California Riverside, University of Florida, and University of Texas at Austin. This work makes use of observations from the LCOGT network. This research has made use of NASA's Astrophysics Data System and 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. The National Geographic Society–Palomar Observatory Sky Atlas (POSS-I) was made by the California Institute of Technology with grants from the National Geographic Society. The Oschin Schmidt Telescope is operated by the California Institute of Technology and Palomar Observatory. Facilities: TESS - , FLWO:1.5 m (TRES) - , SOAR (HRCAM) - , LCO:1 m (NRES) - , ATT (echelle) - , CTIO:1.5 m (CHIRON). - Software: IDL Astronomy Library (Landsman 1993), EXOFASTv2 (Eastman et al. 2013; Eastman 2017), Mercury6 (Chambers 1999), vespa (Morton 2012, 2015), Orbits for the Impatient (Blunt et al. 2017, L. A. Pearce et al. 2019, in preparation), RadVel (Fulton et al. 2018), numpy (Oliphant 2006), pandas (McKinney et al. 2010), matplotlib (Hunter 2007), Pandexo (Batalha et al. 2017).
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
Massachusetts Institute of Technology (MIT)UNSPECIFIED
Heising-Simons FoundationUNSPECIFIED
Harvard UniversityUNSPECIFIED
NSF Graduate Research FellowshipDGE-1256260
Leinweber Center for Theoretical PhysicsUNSPECIFIED
Gaia Multilateral AgreementUNSPECIFIED
Australian Research CouncilLE160100001
Australian Research CouncilDP180100972
Mt. Cuba Astronomical FoundationUNSPECIFIED
National Geographic SocietyUNSPECIFIED
Subject Keywords:planetary systems – planets and satellites: detection – stars: individual (HR 858, TIC 178155732)
Issue or Number:1
Record Number:CaltechAUTHORS:20190809-144205741
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Official Citation:Andrew Vanderburg et al 2019 ApJL 881 L19
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:97729
Deposited By: Tony Diaz
Deposited On:09 Aug 2019 21:57
Last Modified:03 Oct 2019 21:34

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