Michelle Kunimoto, MIT Kavli Institute for Astrophysics and Space Research
Zifan Lin, Massachusetts Institute of Technology
Sarah Millholland, Massachusetts Institute of Technology
Alexander Venner, University of Southern Queensland
Natalie R. Hinkel, Louisiana State University
Avi Shporer, MIT Kavli Institute for Astrophysics and Space Research
Andrew Vanderburg, MIT Kavli Institute for Astrophysics and Space Research
Jeremy Bailey, UNSW Sydney
Rafael Brahm, Universidad Adolfo Ibáñez
Jennifer A. Burt, California Institute of Technology
R. Paul Butler, Carnegie Institution of Washington
Brad Carter, University of Southern Queensland
David R. Ciardi, California Institute of Technology
Karen A. Collins, Harvard-Smithsonian Center for Astrophysics
Kevin I. Collins, George Mason University
Knicole D. Colón, NASA Goddard Space Flight Center
Jeffrey D. Crane, Carnegie Observatories
Tansu Daylan, McDonnell Center for the Space Sciences
Matías R. Díaz, Las Campanas Observatory
John P. Doty, Noqsi Aerospace Ltd.
Fabo Feng, Shanghai Jiao Tong University
Eike W. Guenther, Thueringer Landessternwarte Tautenburg
Jonathan Horner, University of Southern Queensland
Steve B. Howell, NASA Ames Research Center
Jan Janik, Masaryk University
Hugh R.A. Jones, University of Hertfordshire
Petr Kabáth, Astronomical Institute, Academy of Sciences of the Czech Republic v.v.i.
Shubham Kanodia, Carnegie Institution of Washington
Colin Littlefield, NASA Ames Research Center
Hugh P. Osborn, University of Bern
Simon O’Toole, Macquarie University
Martin Paegert, Harvard-Smithsonian Center for Astrophysics
Pavel Pintr, Institute of Plasma Physics, Academy of Sciences of the Czech Republic

Document Type

Article

Publication Date

1-1-2025

Abstract

We report the validation of multiple planets transiting the nearby (d = 12.8 pc) K5V dwarf HD 101581 (GJ 435, TOI-6276, TIC 397362481). This system consists of at least two Earth-size planets whose orbits are near a mutual 4:3 mean-motion resonance, HD 101581 b ( R p = 0.956 − 0.061 + 0.063 R ⊕ , P = 4.47 days) and HD 101581c ( R p = 0.990 − 0.070 + 0.070 R ⊕ , P = 6.21 days). Both planets were discovered in Sectors 63 and 64 TESS observations and statistically validated with supporting ground-based follow-up. We also identify a signal that probably originates from a third transiting planet, TOI-6276.03 ( R p = 0.982 − 0.098 + 0.114 R ⊕ , P = 7.87 days). These planets are remarkably uniform in size and their orbits are evenly spaced, representing a prime example of the “peas-in-a-pod” architecture seen in other compact multiplanet systems. At V = 7.77, HD 101581 is the brightest star known to host multiple transiting planets smaller than 1.5 R ⊕. HD 101581 is a promising system for atmospheric characterization and comparative planetology of small planets.

Publication Source (Journal or Book title)

Astronomical Journal

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