J/A+A/703/A8 TIC low mass stars radius (Parashivamurthy+, 2025)
Radius valley scaling among low mass stars with TESS.
Parashivamurthy H.M., Mulders G.D.
<Astron. Astrophys. 703, A8 (2025)>
=2025A&A...703A...8P 2025A&A...703A...8P (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets
Keywords: catalogs - planets and satellites: composition -
planets and satellites: dynamical evolution and stability -
planets and satellites: formation -
planets and satellites: physical evolution -
planets and satellites: terrestrial planets
Abstract:
The Transiting Exoplanet Survey Satellite (TESS) has been highly
successful in detecting planets in close orbits around low-mass stars,
particularly M dwarfs. This presents a valuable opportunity to conduct
detailed population studies to understand how these planets depend on
the properties of their host stars. The previously observed radius
valley in Sun-like stars has also been observed among M dwarfs;
however, how its properties vary when compared with more massive stars
remains uncertain. We select the volume limited Bioverse stellar
catalog, with precise photometric stellar parameters, which was
cross-matched with the planet catalog consisting of TESS objects of
interests (TOI) candidates and confirmed planets. We detect the radius
valley around M dwarfs at a location of 1.64±0.03 R⊕ and
with a depth of approximately 45%. The radius valley among GKM stars
scales with stellar mass as Rp{prop.to M*0.15±0.04. The slope is
consistent, within 0.3σ, with those around Sun-like stars. For M
dwarfs, the discrepancy is 3.6σ with the extrapolated slope from
the Kepler FGK sample, marking the point where the deviation from
previous results begins. Moreover, we do not see a clear shift in the
radius valley between early and mid M dwarfs. The flatter scaling of
the radius valley for lower-mass stars suggests that mechanisms other
than atmospheric mass loss through photoevaporation may shape the
radius distribution of planets around M dwarfs. A comparison of the
slope with various planet formation and evolution models leads to a
good match with pebble accretion models including water worlds,
indicating a potentially different regime of planet formation that can
be probed with exoplanets around the lowest-mass stars.
Description:
This catalog contains stellar and planetary parameters for 843 TESS
targets around GKM stars.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 100 843 *Stellar and planetary parameters
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Note on table2.dat: Stellar parameters are from the Bioverse catalog
(Hardegree-Ullman et al. (2023AJ....165..267H 2023AJ....165..267H, Cat. J/AJ/165/267).
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See also:
IV/39 : TESS Input Catalog version 8.2 (TIC v8.2) (Paegert+, 2021)
J/AJ/165/267 : O2 levels in Nearby Transiting Exoplanets
(Hardegree-Ullman+, 2023)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 19 I19 --- GaiaDR3 Gaia DR3 Identifier (erroneous identifiers)
21- 30 I10 --- TIC TESS Input Catalog (TIC) identifier
32 I1 --- Planet Number of planet candidates in the system
34- 37 I4 K Teff Stellar effective temperature
39- 43 F5.3 Rsun Radius Stellar radius
45- 49 F5.3 Msun Mass Stellar mass
51- 57 F7.3 pc Dist Stellar distance
59- 70 F12.7 d Per ? Planet orbital period
72- 90 F19.16 Rgeo Rp ? Planet radius
92- 94 A3 --- TFOPWGdisp TESS Follow-up Observing Program Working
Group (TFOPWG) disposition (1)
96-100 F5.2 --- RUWE ? Gaia DR3 renormalised unit weight error
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Note (1): TESS Follow-up Observing Program Working Group (TFOPWG) disposition
as follows:
APC = ambiguous planetary candidate
CP = confirmed planet
FA = false alarm
FP = false positive
KP = known planet
PC = planetary candidate
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Acknowledgements:
Mysore Parashivamurthy,, harshitha(at)das.uchile.cl
(End) Patricia Vannier [CDS] 01-Sep-2025