J/ApJS/255/6 Warm Jupiters in TESS FFIs 1st year (2018-2019 July) (Dong+, 2021)
Warm Jupiters in TESS full-frame images: a catalog and observed eccentricity
distribution for Year 1.
Dong J., Huang C.X., Dawson R.I., Foreman-Mackey D., Collins K.A.,
Quinn S.N., Lissauer J.J., Beatty T., Quarles B., Sha L., Shporer A.,
Guo Z., Kane S.R., Abe L., Barkaoui K., Benkhaldoun Z., Brahm R.,
Bouchy F., Carmichael T.W., Collins K.I., Conti D.M., Crouzet N.,
Dransfield G., Evans P., Gan T., Ghachoui M., Gillon M., Grieves N.,
Guillot T., Hellier C., Jehin E., Jensen E.L.N., Jordan A., Kamler J.,
Kielkopf J.F., Mekarnia D., Nielsen L.D., Pozuelos F.J., Radford D.J.,
Schmider F.-X., Schwarz R.P., Stockdale C., Tan T.-G., Timmermans M.,
Triaud A.H.M.J., Wang G., Ricker G., Vanderspek R., Latham D.W., Seager S.,
Winn J.N., Jenkins J.M., Mireles I., Yahalomi D.A., Morgan E.H., Vezie M.,
Quintana E.V., Rose M.E., Smith J.C., Shiao B.
<Astrophys. J. Suppl. Ser., 255, 6-6 (2021)>
=2021ApJS..255....6D 2021ApJS..255....6D (SIMBAD/NED BibCode)
ADC_Keywords: Exoplanets; Stars, diameters; Surveys
Keywords: Exoplanet catalogs
Abstract:
Warm Jupiters-defined here as planets larger than 6 Earth radii with
orbital periods of 8-200 days-are a key missing piece in our
understanding of how planetary systems form and evolve. It is
currently debated whether Warm Jupiters form in situ, undergo disk or
high-eccentricity tidal migration, or have a mixture of origin
channels. These different classes of origin channels lead to different
expectations for Warm Jupiters' properties, which are currently
difficult to evaluate due to the small sample size. We take advantage
of the Transiting Exoplanet Survey Satellite (TESS) survey and
systematically search for Warm Jupiter candidates around main-sequence
host stars brighter than the TESS-band magnitude of 12 in the
full-frame images in Year 1 of the TESS Prime Mission data. We
introduce a catalog of 55 Warm Jupiter candidates, including 19
candidates that were not originally released as TESS objects of
interest by the TESS team. We fit their TESS light curves,
characterize their eccentricities and transit-timing variations, and
prioritize a list for ground-based follow-up and TESS Extended Mission
observations. Using hierarchical Bayesian modeling, we find the
preliminary eccentricity distributions of our Warm-Jupiter-candidate
catalog using a beta distribution, a Rayleigh distribution, and a
two-component Gaussian distribution as the functional forms of the
eccentricity distribution. Additional follow-up observations will be
required to clean the sample of false positives for a full statistical
study, derive the orbital solutions to break the eccentricity
degeneracy, and provide mass measurements.
Description:
In this work, we describe a systematic search for Warm Jupiters,
defined here as planets larger than 6 Earth radii with orbital periods
of 8-200 days, around stars brighter than 12th TESS-band magnitude
(Tmag) in the Full-Frame Images (FFIs) in the first year of TESS data.
During the first year of the Transiting Exoplanet Survey Satellite
(TESS) Prime Mission (2018 July 25-2019 July 18), TESS surveyed almost
the entire southern ecliptic hemisphere. The Year 1 Prime Mission was
divided into 13 TESS sectors (Sector 1-13), with each sector
monitoring a fraction of sky for ∼27days. The TESS data release
includes 30 minute cadence FFIs and 2minute cadence for ∼200000
preselected target stars.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 279 55 Warm Jupiter candidates discovered in Year 1
TESS Full-Frame Images
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See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
IV/38 : TESS Input Catalog - v8.0 (TIC-8) (Stassun+, 2019)
J/A+A/517/L1 : Radial velocities of WASP-8b planet (Queloz+, 2010)
J/A+A/568/A81 : WASP-117b photometry and radial velocities (Lendl+, 2014)
J/ApJ/790/146 : Planets in Kepler's multi-transiting systems (Fabrycky+, 2014)
J/A+A/570/A64 : WASP-104b and WASP-106b photometry (Smith+, 2014)
J/A+A/587/A64 : Physical properties of giant exoplanets (Santerne+, 2016)
J/ApJ/831/64 : Mass-metallicity relation for giant planets (Thorngren+, 2016)
J/ApJ/834/17 : Mass & radius of planets, moons, low mass stars (Chen+, 2017)
J/MNRAS/465/3693 : 7 WASP-South transiting exoplanets (Hellier+, 2017)
J/AJ/156/18 : Binary companions of evolved stars (Price-Whelan+, 2018)
J/AJ/156/102 : TESS Input Catalog and Candidate Target List (Stassun+, 2018)
J/AJ/156/234 : KELT transit false positive catalog for TESS (Collins+, 2018)
J/AJ/157/191 : Light curve & radial velocities for TOI-172 (Rodriguez+, 2019)
J/AJ/158/25 : Automated triage and vetting of TESS candidates (Yu+, 2019)
J/AJ/158/45 : TESS light curve & radial velocities for HD 1397 (Brahm+, 2019)
J/AJ/158/239 : Metal-rich host stars abundances & EWs (Teske+, 2019)
J/AJ/159/145 : RVs & opt. photometry of the host star TOI-677 (Jordan+, 2020)
J/AJ/160/235 : Opt. photometry and RVs of TOI-481b and TOI-892b (Brahm+, 2020)
J/AJ/160/239 : Cluster difference imaging phot. survey. II. (Bouma+, 2020)
J/AJ/161/97 : Radial Velocities of TOI-811 and TOI-852 (Carmichael+, 2021)
J/AJ/161/194 : LCs & RVs of 5 exoplanets discovered by TESS (Rodriguez+, 2021)
J/AJ/161/235 : Radial velocity of TOI-201 (Hobson+, 2021)
J/ApJS/254/39 : Exoplanet candidates from TESS first 2yr obs (Guerrero+, 2021)
Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 9 I9 --- TIC [4598935/464300749] TESS Input Catalog ID
11- 17 A7 --- Pl TESS Objects of Interest name
19- 23 F5.3 Rsun Rs [0.68/2.3] Stellar radius derived from the
isochrone fitting
25- 29 F5.3 Rsun e_Rs [0.016/0.15] Rs downwards uncertainty
31- 35 F5.3 Rsun E_Rs [0.016/0.15] Rs upwards uncertainty
37- 41 F5.3 Sun Rho [0.08/2.2] Stellar mean density in solar
units derived from the isochrone fitting
43- 47 F5.3 Sun e_Rho [0.007/1.55] Rho downwards uncertainty
49- 53 F5.3 Sun E_Rho [0.007/1.55] Rho upwards uncertainty
55- 59 F5.3 Sun Rhoc [0.059/4.9] Stellar mean density inferred
from light curves (1)
61- 65 F5.3 Sun e_Rhoc [0.007/2.3] Rhoc downwards uncertainty
67- 71 F5.3 Sun E_Rhoc [0.009/2.2] Rhoc upwards uncertainty
73- 78 F6.3 10-3 delta [1.28/35.7] Transit depth in parts per
thousand, derived from the light-curve fitting
80- 85 F6.3 10-3 e_delta [0.057/17] Delta downwards uncertainty
87- 92 F6.3 10-3 E_delta [0.076/77] Delta upwards uncertainty
94- 99 F6.3 Rgeo Rp [5.83/17.75] Planet radius derived from the
light-curve fitting
101- 105 F5.3 Rgeo e_Rp [0.18/3.9] Rp downwards uncertainty
107- 112 F6.3 Rgeo E_Rp [0.2/11.3] Rp upwards uncertainty
114- 118 F5.3 --- b [0.13/0.99] Impact parameter, b, derived from
the light-curve fitting
120- 124 F5.3 --- e_b [0.05/0.4] B downwards uncertainty
126- 130 F5.3 --- E_b [0.033/0.31] B upwards uncertainty
132- 138 F7.3 d Per [7.87/139.31] Orbital period derived from the
light-curve fitting
140- 144 F5.3 d e_Per [0/1.5] Per downwards uncertainty
146- 150 F5.3 d E_Per [0/1.5] Per upwards uncertainty
152- 159 F8.3 d Tc [1243.91/1652.83] Conjunction time, Tc,
derived from the light-curve fitting
161- 165 F5.3 d e_Tc [0/0.019] Tc downwards uncertainty
167- 171 F5.3 d E_Tc [0/0.019] Tc upwards uncertainty
173- 177 F5.3 --- ecc [0.052/0.78] Eccentricity inferred from light
curves
179- 183 F5.3 --- e_ecc [0.05/0.3] 68% lower HPD interval in ecc
185- 189 F5.3 --- E_ecc [0.09/0.4] 68% upper HPD interval in ecc
191- 210 A20 deg omega The 68% highest posterior density (HPD)
argument of periapse inferred from light curves
212- 217 F6.4 --- elit [0.0046/0.43]? Median eccentricity from
literature (see Ref)
219- 224 F6.4 --- e_elit [0.001/0.065]? 68% lower interval in elit
226- 231 F6.4 --- E_elit [0.0027/0.04]? 68% upper interval in elit
233- 235 I3 --- olit [35/358]? Median of the argument of periapse
from literature (see Ref)
237- 239 I3 --- e_olit [0/130]? 68% lower interval in olit
241- 243 I3 --- E_olit [0/120]? 68% upper interval in olit
245- 248 F4.1 --- Sig [0.1/27.1]? Significance level of the TTV
signal (2)
250- 252 I3 --- TSM [1/100]? Transmission Spectroscopy Metric score
(3)
254- 262 A9 --- OName Other name (4)
264- 279 A16 --- Ref Reference(s) (5)
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Note (1): Stellar density inferred from light curves, assuming a circular-orbit
planet in the mean solar density, ρcirc
Note (2): Te significance level of the TTV signal using the metric discussed
in Section 3.2 for candidates with 3+ transits.
Note (3): Scores the candidate gets from the transmission spectroscopy metric
(TSM; Kempton+ 2018PASP..130k4401K 2018PASP..130k4401K), scaled between 1-100.
Note (4): Some of the non-TOI targets have been independently vetted by other
groups (e.g., Montalto+ 2020MNRAS.498.1726M 2020MNRAS.498.1726M) and reported as Community
TOIs (CTOIs). See Section 4.1.
Note (5): References as follows:
Br19 = Brahm et al. (2019, J/AJ/158/45)
Ni9 = Nielsen et al. (2019A&A...623A.100N 2019A&A...623A.100N)
Ro19 = Rodriguez et al. (2019, J/AJ/157/191)
Le14 = Lendl et al. (2014, J/A+A/568/A81)
Qu10 = Queloz et al. (2010, J/A+A/517/L1)
Ne19 = Newton et al. (2019ApJ...880L..17N 2019ApJ...880L..17N)
Ho21 = Hobson et al. (2021, J/AJ/161/235)
Da21 = Dawson et al. (2021AJ....161..161D 2021AJ....161..161D)
Da19 = Dawson et al. (2019AJ....158...65D 2019AJ....158...65D)
Ki19 = Kipping et al. (2019MNRAS.486.4980K 2019MNRAS.486.4980K)
Ad20 = Addison et al. (2021MNRAS.502.3704A 2021MNRAS.502.3704A)
Br20 = Brahm et al. (2020, J/AJ/160/235)
Sm14 = Smith et al. (2014, J/A+A/570/A64)
Jo20 = Jordan et al. (2020, J/AJ/159/145)
He17 = Hellier et al. (2017, J/MNRAS/465/3693)
Hu20 = Huang et al. (2020ApJ...892L...7H 2020ApJ...892L...7H)
He19 = Hellier et al. (2019MNRAS.482.1379H 2019MNRAS.482.1379H)
Mo20 = Montalto et al. (2020MNRAS.498.1726M 2020MNRAS.498.1726M)
Ro21 = Rodriguez et al. (2021, J/AJ/161/194)
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 25-Oct-2021