J/AJ/167/210 <200Myr planet's hosts TESS parameters (Vach+, 2024)
The Occurrence of Small, Short-period Planets Younger than 200 Myr with TESS.
Vach S., Zhou G., Huang C.X., Rogers J.G., Bouma L.G., Douglas S.T.,
Kunimoto M., Mann A.W., Barber M.G., Quinn S.N., Latham D.W., Bieryla A.,
Collins K.
<Astron. J., 167, 210 (2024)>
=2024AJ....167..210V 2024AJ....167..210V
ADC_Keywords: Exoplanets; YSOs; Clusters, open; Optical; Effective temperatures;
Parallaxes, trigonometric; Stars, ages
Keywords: Exoplanets ; Mini Neptunes ; Transit photometry ; Exoplanet
evolution ; Planetary system evolution ; Young star clusters ;
Exoplanet astronomy
Abstract:
Within the first few hundreds of millions of years, many physical
processes sculpt the eventual properties of young planets. NASA's
Transiting Exoplanet Survey Satellite (TESS) mission has surveyed
young stellar associations across the entire sky for transiting
planets, providing glimpses into the various stages of planetary
evolution. Using our own detection pipeline, we search a
magnitude-limited sample of 7219 young stars (≲200Myr) observed in
the first 4 yr of TESS for small (2-8R⊕), short period
(1.6-20days) transiting planets. The completeness of our survey is
characterized by a series of injection and recovery simulations. Our
analysis of TESS 2minute cadence and Full Frame Image (FFI) light
curves recover all known TESS Objects of Interest (TOIs), as well as
four new planet candidates not previously identified as TOIs. We
derive an occurrence rate of 35-10+13% for mini-Neptunes and
27-8+10% for super-Neptunes from the 2 minute cadence data, and
22-6.8+8.6% for mini-Neptunes and 13-4.9+3.9% for
super-Neptunes from the FFI data. To independently validate our
results, we compare our survey yield with the predicted planet yield
assuming Kepler planet statistics. We consistently find a mild
increase in the occurrence of super-Neptunes and a significant
increase in the occurrence of Neptune-sized planets with orbital
periods of 6.2-12days when compared to their mature counterparts. The
young planet distribution from our study is most consistent with
evolution models describing the early contraction of
hydrogen-dominated atmospheres undergoing atmospheric escape and
inconsistent with heavier atmosphere models offering only mild radial
contraction early on.
Description:
TESS observations are conducted via four individual cameras covering a
24x96deg area of the sky, with each sector of observations lasting an
average of 27days. TESS samples the light curves of preselected target
stars at 2minute and 20s cadences via target pixel stamp observations.
Additionally, TESS observes its entire field of view via Full-Frame
Images (FFIs). FFIs were taken every 30 minutes in the TESS primary
mission and then every 10 minutes in the first extended mission.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 85 7219 Parent stellar population
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See also:
I/337 : Gaia DR1 (Gaia Collaboration, 2016)
IV/34 : K2 Ecliptic Plane Input Catalog (EPIC) (Huber+, 2017)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
IV/38 : TESS Input Catalog - v8.0 (TIC-8) (Stassun+, 2019)
I/350 : Gaia EDR3 (Gaia Collaboration, 2020)
J/MNRAS/422/2024 : Xray-age relation and exoplanet evaporation (Jackson+, 2012)
J/A+A/560/A13 : Stellar rotation in h Per (Moraux+, 2013)
J/AJ/147/119 : Catalog of sources in Kepler field of view (Coughlin+, 2014)
J/ApJ/810/95 : Kepler pipeline S/N studies. II. 2011 (Christiansen+, 2015)
J/MNRAS/448/1044 : Simulation data 50 planetary model systems (Hansen+, 2015)
J/AJ/152/113 : Pleiades members with K2 light curves I. Per (Rebull+, 2016)
J/A+A/600/A30 : Limb-darkening for TESS satellite (Claret, 2017)
J/AJ/154/109 : California-Kepler Survey. III. Planet radii (Fulton+, 2017)
J/ApJS/229/30 : Revised stellar properties of Q1-17 Kepler (Mathur+, 2017)
J/AJ/154/224 : Transiting planets young clusters from K2 (Rizzuto+, 2017)
J/ApJ/856/23 : BANYAN. XI. The BANYAN Σ algorithm (Gagne+, 2018)
J/AJ/155/196 : Analysis K2 LCs members of USco & ρ Oph (Rebull+, 2018)
J/ApJS/235/38 : Kepler planetary cand. VIII. DR25 reliab (Thompson+, 2018)
J/AJ/158/77 : Cand & members of the Pisces-Eridanus stream (Curtis+, 2019)
J/AJ/158/109 : Occurrence rates of planets orbiting FGK stars (Hsu+, 2019)
J/A+A/622/L13 : Stellar stream in Gaia DR2 discovery (Meingast+, 2019)
J/AJ/159/211 : Exoplanets parameters from Kepler and K2 (Cloutier+, 2020)
J/ApJS/247/28 : K2 star parameters Gaia & LAMOST (Hardegree-Ullman+, 2020)
J/MNRAS/495/4924 : Exoplanets in Southern open clusters (Nardiello+, 2020)
J/AJ/159/166 : Membership & prop of moving groups with Gaia (Ujjwal+, 2020)
J/other/ExA/51.109 : Transit KELT-11b observed by CHEOPS (Benz+, 2021)
J/AJ/161/265 : Compared rot periods for 1189 CKS host stars (David+, 2021)
J/AJ/161/24 : TRICERATOPS predictions for 384 TOIs (Giacalone+, 2021)
J/ApJS/257/46 : Membership & rotational for clusters (Godoy-Rivera+, 2021)
J/AJ/161/65 : THYME. IV. 3 Exoplanets around TOI-451 B (Newton+, 2021)
J/AJ/164/88 : THYME. VIII. MELANGE-3 candidate members (Barber+, 2022)
J/AJ/164/215 : Candidate members of Cep-Her, RSG-5 and CH-2 (Bouma+, 2022)
J/A+A/657/A7 : Star &substellar companions from Gaia EDR3 (Kervella+, 2022)
J/ApJS/259/33 : Faint-star TOIs from TESS Primary Mission (Kunimoto+, 2022)
J/other/Sci/377.1211 : RV and LC of 8 M dwarf stars with planets (Luque+, 2022)
J/AJ/166/175 : Pre- and main sequence stars properties (Fernandes+, 2023)
J/AJ/165/85 : THYME. IX. MELANGE-4 association members (Wood+, 2023)
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 10 I10 --- Name TIC ID
12- 20 F9.5 deg RAdeg [0/360] Right ascension (J2000)
22- 30 F9.5 deg DEdeg [-88/88] Declination (J2000)
32- 37 F6.1 K Teff [3000/7000] Stellar effective temperature
39- 43 F5.2 mas plx [1.12/90.17]? Gaia parallax
45- 48 F4.2 solMass Mass [0.26/1.54] Stellar mass
50- 53 F4.2 solRad Rad [0.29/2.0] Stellar radius
55- 58 F4.1 mag Tmag [5.0/12.0] Tess band magnitude
60- 64 F5.1 Myr Age [1/200] Stellar age
66- 80 A15 --- Assoc Name of stellar association
82- 85 F4.1 d Prot [0.4/11.9]? Measured rotation period from FFI
light curves
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 11-Jun-2024