The TOI-2427 system: Two close-in planets orbiting a late K-dwarf star
Artikel i vetenskaplig tidskrift, 2025
Using high-precision photometry, NASA’s TESS space mission has discovered many intriguing transiting planet candidates. These discoveries require ground-based follow-up observations, including high-precision Doppler spectroscopy, to rule out false positive scenarios and measure the mass of the transiting planets. In this study, we present an intensive Doppler follow-up campaign of the TESS object of interest TOI-2427, carried out with the High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph to determine the mass of the previously validated transiting planet (TOI-2427 b) and search for additional orbiting companions. By analyzing TESS transit photometry alongside our HARPS radial velocity measurements, we spectroscopically confirmed the transiting planet TOI-2427 b, which orbits its host star every ~1.3 d. We also discovered the presence of a second non-transiting planetary companion with an orbital period of ~5.15 d, which is very close to four times the orbital period of the inner transiting planet. We found that TOI-2427 b is a short-period, high-density super-Earth with a mass of Mb = 5.69+−005150 Mand a radius of Rb = 1.64+−001211 R, implying a mean density of b = 7.1+−1184 g cm−3. Its interior seems to be composed of a predominantly iron core and a silicate mantle and crust. Despite its high density, it is unlikely that TOI-2427 b can sustain any atmosphere composed of lighter gases; however, it could still retain heavier gases. The outer non-transiting planet TOI-2427 c has a minimum mass of Mc sin ic = 6.46+−007978 M. Assuming that TOI-2427 b and c are coplanar, a statistical analysis suggests that planets with a mass of ~6.5 M tend to have radii around 2.7+−1018 R. This would place TOI-2457 c near the sub-Neptune regime, while also leaving open the possibility of it being a super-Earth.
planets and satellites: detection
instrumentation: photometers
techniques: radial velocities
planets and satellites: interiors
planets and satellites: atmospheres
Författare
H. Schmerling
Universität zu Köln
E. Goffo
Thüringer Landessternwarte Tautenburg
Universita degli Studi di Torino
S. Grziwa
Universität zu Köln
Carina Persson
Chalmers, Rymd-, geo- och miljövetenskap, Astronomi och plasmafysik
D. Gandolfi
Universita degli Studi di Torino
Martin Pätzold
Universität zu Köln
A. Hatzes
Thüringer Landessternwarte Tautenburg
Coel Hellier
National Astronomical Observatory of Japan
J.H. Livingston
National Astronomical Observatory of Japan
National Institutes of Natural Sciences
The Graduate University for Advanced Studies (SOKENDAI)
L. Acuña
Max-Planck-Gesellschaft
Keele University
A. Aguichine
University of California
E. Costanza
Universita degli Studi di Torino
H. Deeg
Instituto de Astrofísica de Canarias
Universidad de la Laguna
T. Masseron
Instituto de Astrofísica de Canarias
Universidad de la Laguna
Enric Palle
Instituto de Astrofísica de Canarias
Universidad de la Laguna
William D. Cochran
University of Texas
G. Nowak
Uniwersytet Mikolaja Kopernika
Universidad de la Laguna
Instituto de Astrofísica de Canarias
D. Jankowski
Uniwersytet Mikolaja Kopernika
K. Goździewski
Uniwersytet Mikolaja Kopernika
R. Luque
University of Chicago
S. Mathur
Universidad de la Laguna
Instituto de Astrofísica de Canarias
Dinil B. Palakkatharappil
Université Paris-Saclay
R. A. García
Université Paris-Saclay
Astronomy and Astrophysics
0004-6361 (ISSN) 1432-0746 (eISSN)
Vol. 699 A185Ämneskategorier (SSIF 2025)
Astronomi, astrofysik och kosmologi
Meteorologi och atmosfärsvetenskap
Subatomär fysik
DOI
10.1051/0004-6361/202452620