This page describes the inputs required to run our applet, which fits transit and RV data using AMOEBA.

__ BJD_{TDB} | Flux | Error | D0 | ... | DN __ - A
list of times, fluxes, and errors and (optionally) an arbitrary number
of detrending variables for each data point. These must be in
whitespace delimited columns. For a description of BJD

__ Select Planet__ - This is a drop down menu populated by
all of the transiting planets in the exoplanets.org database, which is
updated once per day from their site. If a planet is selected, the
values from their site are used to begin the fit and any user input
"priors" not be used to begin the fit, but will be used to calculate a
chi^2 penalty, as outlined below.

__ Prior__ - This is the parameter value that the amoeba fit
will start at. These starting values for RV parameters are ignored
during the RV fit.

__ Prior Width__ - This is the uncertainty in the prior. A
penalty term will be added to the chi^2 equal to ((value -
prior)/prior_width)^2. If you do not want the prior to influence the
fit, leave it at "inf". This assumes the errors are Gaussian and
uncorrelated.

__ T_{C}__ - The time of central transit (may be an
integer number of periods off). If only fitting a transit and none is
specified, the mean of the input times will be used. If your light
curve covers a large fraction of out of transit time (or multiple
transits) this default is likely to fail and will have to be refined
by hand.

__ R_{p}/R_{*}__ - The radius of the planet,
in stellar radii (roughly the square root of the depth of transit).

__ i__ - The orbital inclination, in degrees.

__ a/R_{*}__ - The semi-major axis of the orbit, in stellar radii.

__ F_{0}__ - The baseline flux of the transit light curve.

__ u_{1}__ - The linear limb darkening coefficient.

__ u_{2}__ - The quadratic limb darkening coefficient.

__ logg_{*}__ - The stellar surface gravity. If
fitting just the RV, this must be specified, including width (unless
it is a known planet and "Spec Priors?" is set).

__ T_{eff}__ - The stellar effective
temperature. This must be specified, including width (unless it is a
known planet and "Spec Priors?" is set). If this is wrong, none of the
stellar properties, anything derived from the stellar properties,
should be trusted.

__ [Fe/H]__ - The stellar metalicity. This must be specified,
including width (unless it is a known planet and "Spec Priors?" is
set). If this is wrong, none of the stellar properties, anything
derived from the stellar properties, should be trusted.

**Why do I need logg, Teff, and [Fe/H] at all?**

logg,
Teff, and [Fe/H] are used to derive the stellar mass and radius via
the Torres
relations. If there is no transit data, we use these both to
derive additional information (e.g., msini). If we have transit data
(alone or with RV data), we can derive the stellar mass and radius
from logg by itself. However, since that constraint is poor, we add a
penalty to the chi^2 equal to ((mass_derived -
mass_torres)/err_torres)^2 + ((radius_derived -
radius_torres)/err_torres)^2. The stellar parameters are required to
fit RV+transit data simultaneously. If you really don't care about
these, do the fits seperately, enter a large width on the priors, and
then simply ignore the stellar properties and anything derived from
them.

__ P__ - If RV data is not used, you must specify a precise
period. If the transit data do not span multiple periods, you must
specify a prior width, too. Otherwise, the starting value will be
determined from the RV data.

__ e__ - The eccentricity of the orbit. If fitting the
transit only, it is strongly recommended that you fix the orbit to be
circular by checking the "Circular?" box. The photometry alone provide
very little constraint on these parameters, but they appreciably
affect the derived physical parameters.

__ ω_{*}__ - The argument of periastron of the
orbit. If fitting the transit only, it is strongly recommended that
you fix the orbit to be circular by checking the "Circular?" box. The
photometry alone provide very little constraint on these parameters,
but they appreciably affect the derived physical parameters.

__ K__ - The RV semi-amplitude, in m/s.

__ γ__ - The RV systemic velocity (zero point), in m/s.

__ Slope__ - The slope in the RV (m/s/day).

__ Circular?__ - Check this box to force the orbit to be circular.

__ RV Slope?__ - Check this box to fit a slope to the RV (m/s/day).

__ Spec Priors?__ - Check this box to use the logg, Teff,
[Fe/H] and their uncertainties from exoplanets.org as the priors in
the fit. Note that many uncertainties neglect large systematic
uncertainties. We impose a minimum uncertainty of 0.05 in logg, 80 K
in Teff, and 0.08 in [Fe/H], when automatically taken from
exoplanets.org.

__ Long Cadence?__ - Check this box for Long Cadence Kepler
data to generate the model by resampling the light curve 10 times
uniformly spaced over 29.5 minutes for each data point and
averaging.

__ Debug?__ - Check this box to redirect stderr to the
screen. This may give you some insight into any problems that are
occurring. If you think you've found a bug, please copy the output of
the program with "Debug?" checked when you email me.

__ Minimum Period__ - The minimum period for the Lomb-Scargle
periodogram. Use this to explore other periods that are only slightly
disfavored. This is not influenced by and does not influence the
period prior.

__ Maximum Period__ - The maximum period for the Lomb-Scargle
periodogram. Use this to explore other periods that are only slightly
disfavored. This is not influenced by and does not influence the
period prior. The default is the range of input times.

__ N Min__ - The number of minimums in the Lomb-Scargle
periodogram to fit with a full, Keplerian orbit. The actual number of
peaks will be the lesser of this number or the number of local
minimums within the range P

__ Test Input?__ - If a fit doesn't work, it will help to
refine your input values. Check this box to avoid fitting, and just
plot the input parameters over your data.

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