GJ 1252 b: A 1.2 R ⊕ planet transiting an M3 dwarf at 20.4 pc
Files
Accepted manuscript
Date
Authors
Shporer, Avi
Collins, Karen A.
Astudillo-Defru, Nicola
Irwin, Jonathan
Bonfils, Xavier
Collins, Kevin I.
Matthews, Elisabeth
Winters, Jennifer G.
Anderson, David R.
Armstrong, James D.
Version
Accepted manuscript
OA Version
Citation
Avi Shporer, Karen A Collins, Nicola Astudillo-Defru, Jonathan Irwin, Xavier Bonfils, Kevin I Collins, Elisabeth Matthews, Jennifer G Winters, David R Anderson, James D Armstrong, David Charbonneau, Ryan Cloutier, Tansu Daylan, Tianjun Gan, Maximilian N Günther, Coel Hellier, Keith Horne, Chelsea X Huang, Eric LN Jensen, John Kielkopf, Enric Palle, Ramotholo Sefako, Keivan G Stassun, Thiam-Guan Tan, Andrew Vanderburg, George R Ricker, David W Latham, Roland Vanderspek, Sara Seager, Joshua N Winn, Jon M Jenkins, Knicole Colon, Courtney D Dressing, Sébastien Léepine, Philip S Muirhead, Mark E Rose, Joseph D Twicken, Jesus Noel Villasenor. "GJ 1252 b: A 1.2 R ⊕ Planet Transiting an M3 Dwarf at 20.4 pc." The Astrophysical Journal, Volume 890, Issue 1, 15 pages. https://doi.org/10.3847/2041-8213/ab7020
Abstract
We report the discovery of GJ 1252 b, a planet with a radius of 1.193 ± 0.074 R⊕ and an orbital
period of 0.52 days around an M3-type star (0.381 ± 0.019 M⊙, 0.391 ± 0.020 R⊙) located 20.385 ±
0.019 pc away. We use TESS data, ground-based photometry and spectroscopy, Gaia astrometry, and
high angular resolution imaging to show that the transit signal seen in the TESS data must originate from a transiting planet. We do so by ruling out all false positive scenarios that attempt to explain the transit signal as originating from an eclipsing stellar binary. Precise Doppler monitoring also leads to a tentative mass measurement of 2.09 ± 0.56 M⊕. The host star proximity, brightness (V = 12.19 mag, K = 7.92 mag), low stellar activity, and the system’s short orbital period make this planet an attractive target for detailed characterization, including precise mass measurement, looking for other objects in the system, and planet atmosphere characterization.