Issue |
A&A
Volume 475, Number 2, November IV 2007
|
|
---|---|---|
Page(s) | 729 - 746 | |
Section | Planets and planetary systems | |
DOI | https://doi.org/10.1051/0004-6361:20077138 | |
Published online | 18 June 2007 |
Interpreting and predicting the yield of transit surveys: giant planets in the OGLE fields
1
Observatoire de la Côte d'Azur, Laboratoire Gemini, CNRS UMR 6203, BP 4229, 06304 Nice Cedex 4, France e-mail: fressin@obs-nice.fr
2
Observatoire de la Côte d'Azur, Laboratoire Cassiopée, CNRS UMR 6202, BP 4229, 06304 Nice Cedex 4, France
3
Geneva University Observatory, Switzerland
Received:
19
January
2007
Accepted:
8
April
2007
Transiting extrasolar planets are now discovered jointly by
photometric surveys and by radial velocimetry, allowing measurements
of their radius and mass.
We want to determine whether the different data sets are compatible
between themselves and with models of the evolution of extrasolar
planets. We further want to determine whether to expect a population
of dense Jupiter-mass planets to be detected by future more sensitive
transit surveys.
We directly simulate a population of stars corresponding to the OGLE
transit survey and assign them planetary companions based on a list of 153
extrasolar planets discovered by radial velocimetry. We use a model
of the evolution and structure of giant planets that assumes that
they are made of hydrogen and helium and of a variable fraction of
heavy elements (between 0 and 100 ).
The output list of detectable planets of the
simulations is compared to the real detections.
We confirm that the radial velocimetry and photometric survey data
sets are compatible within the statistical errors, assuming that
planets with periods between 1 and 2 days are approximately 5 times less
frequent than planets with periods between 2 and 5 days. We show
that evolution models fitting present observational constraints
predict a lack of small giant planets with large masses.
As a side result of the study, we identify two distinct populations of
planets: those with short periods (
d),
which are found in orbit only around metal-rich stars with [Fe/H]>~-0.07, and
those on longer orbits (
d),
for which the metallicity bias is less marked. We further confirm the relative absence of
low-mass giant planets at small orbital distances.
Testing these results and the underlying
planetary evolution models requires the detection of a statistically significant
number of transiting planets, which should be provided over the next few years by
continued ground-based photometric
surveys, the space missions CoRoT and Kepler, and combined radial
velocity measurements.
Key words: stars: planetary systems: formation / surveys / techniques: photometric / methods: data analysis / stars: planetary systems
© ESO, 2007
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