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Figure 1: From top to bottom: distribution functions for the radii, masses and effective temperatures for our fiducial stellar population corresponding to the simulated OGLE Carina field. The black line represents the ensemble of stars in the field. The filled red region is a subset for dwarf stars with stellar type F4 and later, as these are the only stars for which a transiting planet has a reasonnable chance of being detected by present-day transit surveys. |
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Figure 2: Upper panel: probability for a solar-type star to possess a giant planet companion as a function of the stellar metallicity (from Santos et al. 2004). Lower panel: relative normalised distributions of stellar metallicities for stars in the field (black line), and for stars with a giant planet companion (red line). |
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Figure 3: From top to bottom, distributions of orbital periods, masses and radii, respectively, of the planets observed by radial velocimetry (black lines), simulated as part of the mass-period "carbon copy'' model (red lines), and simulated as part of the analytical model (dotted blue lines) (see text). |
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Figure 4:
Mass of heavy elements in transiting Pegasids known by 2006
as a function of the metal content of the parent star relative to
the Sun. The mass of heavy elements required to fit the measured
radii is calculated on the basis of evolution models including an
additional heat source slowing the cooling of the planet. This heat
source is assumed equal to ![]() ![]() |
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Figure 5:
Theoretical and observed mass-radius relations. The black
line is applicable to the evolution of solar composition planets,
brown dwarfs, and stars, when isolated or nearly isolated (as
Jupiter, Saturn, Uranus, and Neptune, defined by diamonds and their
respective symbols), after 5 Ga of evolution. The dotted line shows
the effect of a
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Figure 6:
Logarithm of the probability that a simulated
detection event occurs in each one of the
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Figure 7:
Depth of the planetary transit events versus magnitude of the
parent star in the V band. The five confirmed OGLE detections are shown
as circles. Model results are shown as black plusses for detectable
events and orange crosses for events that are considered
undetectable based on the photometric signal (see text). Blue diamonds
correspond to events that would be detectable by photometry
alone but that cannot be confirmed by radial velocimetry. Note that
the model results correspond to 3 times the full OGLE campaign
for more statistical significance. The OGLE planets depth-magnitude
distribution is at
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Figure 8:
Mass versus period of transiting giant planets.
(OGLE planets are red circles, other transit surveys in orange, planets from
radial velocity surveys in blue. Simulated planets detected: black plusses, under threshold: orange crosses).
The OGLE planets mass-period distribution is at
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Figure 9: Distribution of the crowding index (see text) of target stars in Carina (black) and in the bulge (red). |
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Figure 10:
Deviations from a maximum likelihood obtained as a function
of
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Figure 11:
Period of transiting exoplanets versus metallicity of their
parent star. The model is based on analytic relations for the mass
and period distributions of planetary companions (see
Sect. 2.4.2). (OGLE planets are red circles, other transit surveys in orange, planets from radial velocity surveys in blue. Simulated planets detected: black plusses, under threshold: orange crosses).
The OGLE planets period-metallicity
distribution is at
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Figure 12:
Period of transiting exoplanets versus metallicity of their
parent star. The figure differs from
Fig. 11 in that our fiducial model,
i.e. the mass-period-metallicity "carbon-copy'' model is used (see
Sect. 2.4.2).
(OGLE planets are red circles, other transit surveys in orange, planets from
radial velocitiy surveys in
blue. Simulated planets detected: black plusses, under threshold: orange crosses).
The OGLE planets period-metallicity
distribution is at
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Figure 13:
Potential energy per unit mass (Ep=GM/R) versus orbital period of
transiting planets. (OGLE planets are red circles, other transit surveys in orange, planets from radial velocity surveys in
blue. Simulated planets detected: black plusses, under threshold: orange crosses).
Observations are compared to models based on the
analytical relations for the mass and period distribution of
planetary companions (see Sect. 2.4.2).
The OGLE planets' energy-period distribution is at
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Figure 14:
Potential energy per unit mass versus orbital period of
transiting planets. The figure is similar to
Fig. 13, except for the fact that our
fiducial model is used (see Sect. 2.4.2).
(OGLE planets are red circles, other transit surveys in orange, planets from radial velocity surveys in
blue. Simulated planets detected: black plusses, under threshold: orange crosses).
The OGLE planets energy-period distribution is at
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Figure 15:
Radius as a function of equilibrium temperature of transiting
exoplanets.
(OGLE planets are red circles, other transit surveys in orange, planets from radial velocity surveys in
blue. Simulated planets detected: black plusses, under threshold: orange crosses).
The OGLE planets
equilibrium temperature-radius distribution is at
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Figure 16:
Mass-radius relation for transiting extrasolar giant
planets.
(OGLE planets are red circles, other transit surveys in orange, planets from radial velocity surveys
in blue. Simulated planets detected: black plusses, under threshold: orange crosses).
The OGLE planets mass-radius distribution is at 0.67![]() ![]() ![]() |
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Figure 17:
Mass-radius relation for a very large number of Monte-Carlo
trials using the fiducial model. The curves show the ensemble of
planets with masses of heavy elements between 0 and 25, 25 and 50,
50 and 75, 75 and 100 ![]() |
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Figure 18:
Mass-radius relation obtained for an alternative model with
70% of "standard'' planets with no extra-energy source, and 30%
planets receiving an additional
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