J/A+A/689/A250 Kepler DR25 cat. transit and detec. prob. (Castro-Gonzale+, 2024)
Mapping out the exo-Neptunian landscape. A ridge between the desert and savanna.
Castro-Gonzalez A., Bourrier V., Lillo-Box J., Delisle J.-B.,
Armstrong D.J., Barrado D., Correia A.C.M.
<Astron. Astrophys. 689, A250 (2024)>
=2024A&A...689A.250C 2024A&A...689A.250C (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Optical
Keywords: planets and satellites: atmospheres -
planets and satellites: dynamical evolution and stability -
planets and satellites: formation -
planets and satellites: gaseous planets -
planets and satellites: physical evolution
Abstract:
Atmospheric and dynamical processes are thought to play a major role
in shaping the distribution of close-in exoplanets. A striking feature
of such distribution is the Neptunian desert, a dearth of Neptunes on
the shortest-period orbits. We aim at delineating the Neptunian desert
boundaries and studying its transition into the savanna, a moderately
populated region at larger orbital distances. This will allow bringing
constraints to the processes that carved out the Neptunian landscape
and provide the exoplanet community with a framework to perform
studies of planet formation and evolution. We built a sample of
planets and candidates based on the Kepler DR25 catalogue and weighed
it according to the transit and detection probabilities. We used the
corrected distribution to study occurrences across the period and
period-radius spaces. We delimited the Neptunian desert as the
close-in region of the period-radius space with no planets at a
3σ level, and provide the community with simple, ready-to-use
approximate boundaries. We identified an overdensity of planets
separating the Neptunian desert and savanna (3.2d≲ Porb≲5.7d) that
stands out at a 4.7σ level above the desert and at a 3.5σ
level above the savanna, which we propose to call the Neptunian ridge.
The period range of the ridge matches that of the well-known hot
Jupiter pileup (~=3-5 days), which suggests that similar evolutionary
processes might act on both populations. We find that the occurrence
fraction between the pileup and warm Jupiters
(fpileup/warm=5.3±1.1) is about twice that between the Neptunian
ridge and savanna (fridge/savanna=2.7±0.5). This indicates either
that the processes that drive or maintain planets in the overdensity
are more efficient for Jupiters or that the processes that drive or
maintain planets in the warm region are more efficient for Neptunes.
Our revised landscape supports a previous hypothesis that a fraction
of Neptunes were brought to the edge of the desert (i.e. the newly
identified ridge) through high-eccentricity tidal migration (HEM) late
in their life, surviving the evaporation that eroded Neptunes that
arrived earlier on in the desert. The ridge thus appears as a true
physical feature illustrating the interplay between photoevaporation
and HEM processes, providing further evidence of their role in shaping
the distribution of close-in Neptunes.
Description:
Transit and detection probabilities of the Kepler DR25 catalogue.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 79 4072 Transit and detection probabilities of the
Kepler DR25 catalogue
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- KOI Kepler Object of Interest
11- 34 F24.18 --- 1/ptransit Inverse of the transit probability
36- 55 F20.16 --- 1/pdetection Inverse of the detection probability
57- 79 F23.17 --- Weight Assigned weight to correct for
non-transiting orbital inclinations and
insufficient photometric precision
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Acknowledgements:
Amadeo Castro-Gonzalez, acastro(at)cab.inta-csic.es
(End) Amadeo Castro-Gonzalez [CAB, Spain], Patricia Vannier [CDS] 15-Aug-2024