This page describes the outputs of our applet, which fits transit and RV data using AMOEBA.

Chi^2/dof, scaling errors, RMS of residuals - The input errors are not assumed to be correct, but are scaled such that the chance of getting that chi^2 or smaller is 50%, or P(chi^2) = 0.5 (roughly chi^2/dof = 1) once the best fit is found. This is to ensure that the relative weights of RV and Transit data are appropriate.

__Stellar Parameters__

M_{*} - Stellar mass, in solar masses. In fits including
transits, this is derived from the transit plus logg and guided by the
Torres relation (see equation 24 in Eastman, et al., 2013). If
only RV is fit, we use the Torres relation alone.

R_{*} - Stellar radius, in solar radii. In fits including
transits, this is derived from the transit plus logg and guided by the
Torres relation (see equation 24 in Eastman, et al., 2013). If
only RV is fit, we use the Torres relation alone.

L_{*} - Stellar luminosity, in solar luminosity.

ρ_{*} - stellar density, in cgs. This simulateously
includes the constraints from the mass/radius of the star and the
transit.

logg_{*} - The stellar surface gravity. Constained by the
transit and/or its prior.

T_{eff} - The Stellar effective temperature, in Kelvin. This is mostly
constrained by the prior.

[Fe/H] - The stellar metallicity. This is mostly constrained by the prior.

__Planetary Parameters__

e - The eccentricity of the orbit. Not shown for circular fits.

ω_{*} - The argument of periastron of the star's orbit,
in degrees. Not shown for circular fits.

P - The period of the orbit, in days.

a - The semi-major axis of the orbit, in AU.

M_{P} - The mass of the planet, in Jupiter masses. Not shown for RV only fits.

R_{P} - The radius of the planet, in Jupiter radii. Not shown for RV only fits.

ρ_{P} - The density of the planet, in cgs. Not shown for RV only fits.

log(g_{p}) - The log of the surface gravity of the planet, in cgs. Not shown for RV only fits.

T_{eq} - The equilibrium temperature of the planet, assuming
perfect redistribution and no albedo.

Θ - The Safronov number. Not shown for RV only fits.

<F> - The time-averaged incident flux that the planet receives, in units of 10^9 ergs/s/cm^2.

__RV Parameters__

ecosω_{*} - eccentricity times the cosine of the
argument of periastron. Not shown for circular fits.

esinω_{*} - eccentricity times the sine of the argument
of periastron. Not shown for circular fits.

T_{P} - The time of periastron, in BJD_{TDB}.

K - The RV semi-amplitude, in m/s. Not shown for transit-only fits.

M_{P}sini - The minimum mass, in jupiter masses. Not shown for
Transit-only fits.

M_{P}/M_{*} - The mass ratio of the planet to the
star. Not shown for Transit-only fits.

γ - The systemic velocity (or instrumental velocity) in m/s

\dot{\gamma} - The slope in RV, in m/s/day. Only displayed if RV is fit and slope is checked.

__Primary Transit Parameters__

T_{C} - The time of transit center (or time of Conjunction), in BJD_{TDB}.

R_{P}/R_{*} - Radius of the planet in stellar
radii. Not shown for RV only fits.

a/R_{*} - Semi major axis in stellar radii.

i - inclination of the orbit, in degrees. Not shown for RV only fits.

b - the impact parameter. Not shown for RV only fits.

δ - (R_{P}/R_{*})^{2}, which is the
transit depth for non-grazing transits with no limb darkening.

T_{FWHM} - The duration of the Full Width at Half Maximum
Transit (from mid ingress to mid egress), or the time it takes for the
center of the planet to cross the entire star. For eccentric orbits,
this uses the approximations of Winn, 2010. If no transit is fit, we
assume a point planet (R_{P}=0) and a central crossing (b=0),
and therefore T_{FWHM} is not displayed because it equals
T_{14}.

τ - the duration of ingress/egrees (1st to 2nd contact or 3rd to
4th contact). For eccentric orbits, this uses the approximations of
Winn, 2010. If no transit is fit, we assume a point planet
(R_{P}=0) and a central crossing (b=0) and therefore τ is
not displayed because it is equal to 0.

T_{14} - The duration of transit (1st to 4th contact). For
eccentric orbits, this uses the approximations of Winn, 2010. If no
transit is fit, we assume a point planet (R_{P}=0) and a
central crossing (b=0).

P_{T} - The a priori non-grazing transit probability, assuming
no knowledge of the inclination. If no transit is fit, we assume a
point planet (R_{P}=0); and therefore P_{T} =
P_{T,G}. This is useful for transit searches of RV planets or
to correct for geometric biases for transiting planets.

P_{T,G} - The a priori grazing transit probability, assuming
no knowledge of the inclination.

u_{1} - The linear limb darkening coefficient.

u_{2} - The quadratic limb darkening coefficient.

F_{0} - The average out-of-transit flux. Should be
close to 1 (and in the figure, it is exactly equal to 1).

__Secondary Eclipse Parameters__

T_{S} - The time of secondary eclipse center in BJD_{TDB}.

b_{S} - The impact parameter for the secondary eclipse. Only
shown if eccentricity is free (otherwise it's identical to the
primary).

T_{S,FWHM} - The duration of the Full Width at Half Maximum of
the eclipse (from mid ingress to mid egress), or the time it takes for
the center of the planet to cross the entire star. Only shown if
eccentricity is free (otherwise it's identical to the primary). We use
the approximations of Winn, 2010. If no transit is fit, we assume a
point planet (R_{P}=0) and a central crossing (b=0).

τ_{S} - the duration of ingress/egrees (1st to 2nd contact
or 3rd to 4th contact). Only shown if eccentricity is free (otherwise
it's identical to the primary). We use the approximations of Winn,
2010. If no transit is fit, we assume a point planet (R_{P}=0)
and a central crossing (b=0).

T_{S,14} - The duration of eclipse (1st to 4th contact). Only
shown if eccentricity is free (otherwise it's identical to the
primary). We use the approximations of Winn, 2010. If no transit is
fit, we assume a point planet (R_{P}=0) and a central crossing
(b=0).

P_{S} - The a priori non-grazing eclipse probability, assuming
no knowledge of the inclination. To determine posterior eclipse
probablity: b_{S} < 1-p => eclipse. Only shown if
eccentricity is free (otherwise it's identical to the primary).

P_{S,G} - The a priori grazing eclipse probability, assuming
no knowledge of the inclination. To determine posterior eclipse
probablity: b_{S} < 1+p => eclipse. shown if eccentricity
is free (otherwise it's identical to the primary).

** NOTE:** The times are only in BJD

Copyright © Jason Eastman (jason.eastman@cfa.harvard.edu) All Rights Reserved. Questions, comments, or bug reports encouraged.