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Peer-reviewedCC BY 4.0Monthly Notices of the Royal Astronomical Society

Demographics of Close-In TESS Exoplanets Orbiting FGK Main-sequence Stars – II. Spectral-Type Dependence and the Neptunian Landscape

  • Kaiming Cui1,2
  • David J Armstrong1,2
  • Andreas Hadjigeorghiou1,2
  • Marina Lafarga1,2
  • Ares Osborn1,2
  • George W King1,2
  • Tim Hallatt3
  • Vedad Kunovac1,2
  • Lauren Doyle1,2
  1. 1University of Warwick Department of Physics, , Gibbet Hill Road, Coventry CV4 7AL ,
  2. 2Centre for Exoplanets and Habitability, University of Warwick , Gibbet Hill Road, Coventry CV4 7AL ,
  3. 3MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology , Cambridge, MA 02139 ,
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Abstract

Understanding how planetary demographics depend on host star properties is essential for constraining planet formation and evolution theories. In this paper, we analyse close-in (0.5–16 d) planet occurrence rates from the TESS Science Processing Operations Center (SPOC) full-frame image data for individual F-, G-, and K-type main-sequence stellar samples. Integrated over 0.5 < P < 16 d and 2 < Rp < 20 R⊕, the occurrence rates are 12.1+3.0−2.3, 10.2+1.2−1.0, and 13.1+1.4−1.2 planets per 100 stars for F-, G-, and K-type hosts, consistent with each other at 1σ, so any spectral-type dependence is localized rather than global. For transiting hot Jupiters, we measure 0.30+0.04−0.03, 0.50 ± 0.03, and 0.67+0.08−0.07 per cent, with the rate peaking at K type; the latter being the first such measurement for K-type hosts. Modelling the Neptunian desert directly in occurrence-rate space, we find that the desert extends to longer orbital periods around hotter stars. Integrating over the desert interior gives 0.069+0.045−0.011, 0.093+0.046−0.022, and 0.150+0.033−0.026 planets per 100 stars, implying about one close-in planet in a hundred lies inside the desert, and the desert is roughly twice as populated around K- as around F-type hosts. A rigorous Bayesian model comparison for the 6–8 R⊕ strip indicates that a distinct Neptunian ridge is not required to explain the measurements.

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Cite

BibTeXRIS
BibTeX
@article{cui2026demographics,
  title = {{Demographics of Close-In TESS Exoplanets Orbiting FGK Main-sequence Stars – II. Spectral-Type Dependence and the Neptunian Landscape}},
  author = {Kaiming Cui and David J Armstrong and Andreas Hadjigeorghiou and Marina Lafarga and Ares Osborn and George W King and Tim Hallatt and Vedad Kunovac and Lauren Doyle},
  journal = {Monthly Notices of the Royal Astronomical Society},
  year = {2026},
  month = oct,
  doi = {10.1093/mnras/stag2018},
  url = {https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag2018/8979809},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - Demographics of Close-In TESS Exoplanets Orbiting FGK Main-sequence Stars – II. Spectral-Type Dependence and the Neptunian Landscape
AU  - Kaiming Cui
AU  - David J Armstrong
AU  - Andreas Hadjigeorghiou
AU  - Marina Lafarga
AU  - Ares Osborn
AU  - George W King
AU  - Tim Hallatt
AU  - Vedad Kunovac
AU  - Lauren Doyle
PY  - 2026
DA  - 2026/10/22
JO  - Monthly Notices of the Royal Astronomical Society
DO  - 10.1093/mnras/stag2018
UR  - https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stag2018/8979809
AB  - Understanding how planetary demographics depend on host star properties is essential for constraining planet formation and evolution theories. In this paper, we analyse close-in (0.5–16 d) planet occurrence rates from the TESS Science Processing Operations Center (SPOC) full-frame image data for individual F-, G-, and K-type main-sequence stellar samples. Integrated over 0.5 < P < 16 d and 2 < Rp < 20 R⊕, the occurrence rates are 12.1^+3.0_−2.3, 10.2^+1.2_−1.0, and 13.1^+1.4_−1.2 planets per 100 stars for F-, G-, and K-type hosts, consistent with each other at 1σ, so any spectral-type dependence is localized rather than global. For transiting hot Jupiters, we measure 0.30^+0.04_−0.03, 0.50 ± 0.03, and 0.67^+0.08_−0.07 per cent, with the rate peaking at K type; the latter being the first such measurement for K-type hosts. Modelling the Neptunian desert directly in occurrence-rate space, we find that the desert extends to longer orbital periods around hotter stars. Integrating over the desert interior gives 0.069^+0.045_−0.011, 0.093^+0.046_−0.022, and 0.150^+0.033_−0.026 planets per 100 stars, implying about one close-in planet in a hundred lies inside the desert, and the desert is roughly twice as populated around K- as around F-type hosts. A rigorous Bayesian model comparison for the 6–8 R⊕ strip indicates that a distinct Neptunian ridge is not required to explain the measurements.
SN  - 0035-8711
SN  - 1365-2966
ER  -