exoplanet.orbits.
KeplerianOrbit
(period=None, a=None, t0=None, t_periastron=None, incl=None, b=None, duration=None, ecc=None, omega=None, Omega=None, m_planet=0.0, m_star=None, r_star=None, rho_star=None, ror=None, m_planet_units=None, rho_star_units=None, model=None, contact_points_kwargs=None, **kwargs)¶A system of bodies on Keplerian orbits around a common central
Given the input parameters, the values of all other parameters will be
computed so a KeplerianOrbit
instance will always have attributes for
each argument. Note that the units of the computed attributes will all be
in the standard units of this class (R_sun
, M_sun
, and days
)
except for rho_star
which will be in g / cm^3
.
There are only specific combinations of input parameters that can be used:
First, either period
or a
must be given. If values are given
for both parameters, then neither m_star
or rho_star
can be
defined because the stellar density implied by each planet will be
computed in rho_star
.
Only one of incl
and b
can be given.
If a value is given for ecc
then omega
must also be given.
If no stellar parameters are given, the central body is assumed to be
the sun. If only rho_star
is defined, the radius of the central is
assumed to be 1 * R_sun
. Otherwise, at most two of m_star
,
r_star
, and rho_star
can be defined.
Either t0
(reference transit) or t_periastron
must be given,
but not both.
period – The orbital periods of the bodies in days.
a – The semimajor axes of the orbits in R_sun
.
t0 – The time of a reference transit for each orbits in days.
t_periastron – The epoch of a reference periastron passage in days.
incl – The inclinations of the orbits in radians.
b – The impact parameters of the orbits.
ecc – The eccentricities of the orbits. Must be 0 <= ecc < 1
.
omega – The arguments of periastron for the orbits in radians.
Omega – The position angles of the ascending nodes in radians.
m_planet – The masses of the planets in units of m_planet_units
.
m_star – The mass of the star in M_sun
.
r_star – The radius of the star in R_sun
.
rho_star – The density of the star in units of rho_star_units
.
m_planet_units – An astropy.units
compatible unit object giving the
units of the planet masses. If not given, the default is M_sun
.
rho_star_units – An astropy.units
compatible unit object giving the
units of the stellar density. If not given, the default is
g / cm^3
.
get_planet_position
(t, parallax=None)¶The planets’ positions in the barycentric frame
t – The times where the position should be evaluated.
The components of the position vector at t
in units of
R_sun
.
get_planet_velocity
(t)¶Get the planets’ velocity vectors
t – The times where the velocity should be evaluated.
The components of the velocity vector at t
in units of
M_sun/day
.
get_radial_velocity
(t, K=None, output_units=None)¶Get the radial velocity of the star
Note
The convention in exoplanet is that positive z points towards the observer. However, for consistency with radial velocity literature this method returns values where positive radial velocity corresponds to a redshift as expected.
t – The times where the radial velocity should be evaluated.
K (Optional) – The semi-amplitudes of the orbits. If provided, the
m_planet
and incl
parameters will be ignored and this
amplitude will be used instead.
output_units (Optional) – An AstroPy velocity unit. If not given,
the output will be evaluated in m/s
. This is ignored if a
value is given for K
.
The reflex radial velocity evaluated at t
in units of
output_units
. For multiple planets, this will have one row for
each planet.
get_relative_angles
(t, parallax=None)¶The planets’ relative position to the star in the sky plane, in separation, position angle coordinates.
Note
This treats each planet independently and does not take the other planets into account when computing the position of the star. This is fine as long as the planet masses are small.
t – The times where the position should be evaluated.
The separation (arcseconds) and position angle (radians, measured east of north) of the planet relative to the star.
get_relative_position
(t, parallax=None)¶The planets’ positions relative to the star in the X,Y,Z frame.
Note
This treats each planet independently and does not take the other planets into account when computing the position of the star. This is fine as long as the planet masses are small. In other words, the reflex motion of the star caused by the other planets is neglected when computing the relative coordinates of one of the planets.
t – The times where the position should be evaluated.
The components of the position vector at t
in units of
R_sun
.
get_relative_velocity
(t)¶The planets’ velocity relative to the star
Note
This treats each planet independently and does not take the other planets into account when computing the position of the star. This is fine as long as the planet masses are small.
t – The times where the velocity should be evaluated.
The components of the velocity vector at t
in units of
R_sun/day
.
get_star_position
(t, parallax=None)¶The star’s position in the barycentric frame
Note
If there are multiple planets in the system, this will return one column per planet with each planet’s contribution to the motion. The star’s full position can be computed by summing over the last axis.
t – The times where the position should be evaluated.
The components of the position vector at t
in units of
R_sun
.
get_star_velocity
(t)¶Get the star’s velocity vector
Note
For a system with multiple planets, this will return one column per planet with the contributions from each planet. The total velocity can be found by summing along the last axis.
t – The times where the velocity should be evaluated.
The components of the velocity vector at t
in units of
M_sun/day
.
exoplanet.orbits.
TTVOrbit
(*args, **kwargs)¶A generalization of a Keplerian orbit with transit timing variations
Only one of the arguments ttvs
or transit_times
can be given and
the other will be computed from the one that was provided.
In practice the way this works is that the time axis is shifted to account
for the TTVs before solving for a standard Keplerian orbit. To identify
which times corrorspond to which transits, this will find the closest
labelled transit to the timestamp and adjust the timestamp accordingly.
This means that things will go very badly if the time between
neighboring transits is larger than 2*period
.
ttvs – A list (with on entry for each planet) of “O-C” vectors for each transit of each planet in units of days. “O-C” means the difference between the observed transit time and the transit time expected for a regular periodic orbit.
transit_times – A list (with on entry for each planet) of transit times
for each transit of each planet in units of days. These times will
be used to compute the implied (least squares) ttv_period
and
t0
. It is possible to supply a separate period
parameter
that will set the shape of the transits, but care should be taken
to make sure that period
and ttv_period
don’t diverge
because things will break if the time between neighboring transits
is larger than 2*period
.
transit_inds – A list of integer value tensors giving the transit
number for each transit in transit_times'' or ``ttvs
. This is
useful when not all transits are observed. This should always be
zero indexed.
delta_log_period – If using the transit_times
argument, this
parameter specifies the difference (in natural log) between the
leqast squares period and the effective period of the transit.
get_planet_position
(t, parallax=None)¶The planets’ positions in the barycentric frame
t – The times where the position should be evaluated.
The components of the position vector at t
in units of
R_sun
.
get_planet_velocity
(t)¶Get the planets’ velocity vectors
t – The times where the velocity should be evaluated.
The components of the velocity vector at t
in units of
M_sun/day
.
get_radial_velocity
(t, K=None, output_units=None)¶Get the radial velocity of the star
Note
The convention in exoplanet is that positive z points towards the observer. However, for consistency with radial velocity literature this method returns values where positive radial velocity corresponds to a redshift as expected.
t – The times where the radial velocity should be evaluated.
K (Optional) – The semi-amplitudes of the orbits. If provided, the
m_planet
and incl
parameters will be ignored and this
amplitude will be used instead.
output_units (Optional) – An AstroPy velocity unit. If not given,
the output will be evaluated in m/s
. This is ignored if a
value is given for K
.
The reflex radial velocity evaluated at t
in units of
output_units
. For multiple planets, this will have one row for
each planet.
get_relative_angles
(t, parallax=None)¶The planets’ relative position to the star in the sky plane, in separation, position angle coordinates.
Note
This treats each planet independently and does not take the other planets into account when computing the position of the star. This is fine as long as the planet masses are small.
t – The times where the position should be evaluated.
The separation (arcseconds) and position angle (radians, measured east of north) of the planet relative to the star.
get_relative_position
(t, parallax=None)¶The planets’ positions relative to the star in the X,Y,Z frame.
Note
This treats each planet independently and does not take the other planets into account when computing the position of the star. This is fine as long as the planet masses are small. In other words, the reflex motion of the star caused by the other planets is neglected when computing the relative coordinates of one of the planets.
t – The times where the position should be evaluated.
The components of the position vector at t
in units of
R_sun
.
get_relative_velocity
(t)¶The planets’ velocity relative to the star
Note
This treats each planet independently and does not take the other planets into account when computing the position of the star. This is fine as long as the planet masses are small.
t – The times where the velocity should be evaluated.
The components of the velocity vector at t
in units of
R_sun/day
.
get_star_position
(t, parallax=None)¶The star’s position in the barycentric frame
Note
If there are multiple planets in the system, this will return one column per planet with each planet’s contribution to the motion. The star’s full position can be computed by summing over the last axis.
t – The times where the position should be evaluated.
The components of the position vector at t
in units of
R_sun
.
get_star_velocity
(t)¶Get the star’s velocity vector
Note
For a system with multiple planets, this will return one column per planet with the contributions from each planet. The total velocity can be found by summing along the last axis.
t – The times where the velocity should be evaluated.
The components of the velocity vector at t
in units of
M_sun/day
.
exoplanet.orbits.
ReboundOrbit
(*args, **kwargs)¶An N-body system powered by the rebound integrator
This takes all the same arguments as the KeplerianOrbit
, but
these arguments define the orbital elements at some reference time (given
by the rebound_t
parameter). The positions and velocities of the bodies
are then computed by numerically integrating the gravitational N-body
system.
rebound
-specific parameters can be provided as keyword arguments
prefixed by rebound_
. These will then be applied to the
rebound.Simulation
object as properties. Therefore, if you want to
change the integrator, you could use: rebound_integrator = "whfast"
,
for example. All of these parameters are passed directly through to
rebound
except rebound_t
(the reference time) which is converted
from days to years over two pi (the default time units in rebound
).
Note
exoplanet
and rebound
use different base units, but all
of the unit conversions are handled behind the scenes in this object
so that means that you should mostly use the exoplanet
units when
interacting with this class and you should be very cautious about
setting the rebound_G
argument. One example of a case where you’ll
need to use the rebound
units is when you want to set the
integrator step size using the rebound_dt
parameter.
get_planet_position
(t)¶The planets’ positions in the barycentric frame
t – The times where the position should be evaluated.
The components of the position vector at t
in units of
R_sun
.
get_planet_velocity
(t)¶Get the planets’ velocity vectors
t – The times where the velocity should be evaluated.
The components of the velocity vector at t
in units of
M_sun/day
.
get_radial_velocity
(t, output_units=None)¶Get the radial velocity of the star
Note
The convention in exoplanet is that positive z points towards the observer. However, for consistency with radial velocity literature this method returns values where positive radial velocity corresponds to a redshift as expected.
Note
Unlike the KeplerianOrbit
implementation, the
semi-amplitude K
cannot be used with the ReboundOrbit
.
Also, the contributions of each planet are not returned separately;
this will always return a single time series.
t – The times where the radial velocity should be evaluated.
output_units (Optional) – An AstroPy velocity unit. If not given,
the output will be evaluated in m/s
. This is ignored if a
value is given for K
.
The reflex radial velocity evaluated at t
in units of
output_units
.
get_relative_angles
(t, parallax=None)¶The planets’ relative position to the star in the sky plane, in separation, position angle coordinates.
Note
This treats each planet independently and does not take the other planets into account when computing the position of the star. This is fine as long as the planet masses are small.
t – The times where the position should be evaluated.
The separation (arcseconds) and position angle (radians, measured east of north) of the planet relative to the star.
get_relative_position
(t)¶The planets’ positions relative to the star in the X,Y,Z frame.
t – The times where the position should be evaluated.
The components of the position vector at t
in units of
R_sun
.
get_relative_velocity
(t)¶The planets’ velocity relative to the star
t – The times where the velocity should be evaluated.
The components of the velocity vector at t
in units of
R_sun/day
.
get_star_position
(t)¶The star’s position in the barycentric frame
Note
Unlike the KeplerianOrbit
, this will not return
the contributions from each planet separately.
t – The times where the position should be evaluated.
The components of the position vector at t
in units of
R_sun
.
get_star_velocity
(t)¶Get the star’s velocity vector
Note
Unlike the KeplerianOrbit
, this will not return
the contributions from each planet separately.
t – The times where the velocity should be evaluated.
The components of the velocity vector at t
in units of
M_sun/day
.
in_transit
(t, r=0.0, texp=None)¶This is a no-op and all points are assumed to be in transit
exoplanet.orbits.
SimpleTransitOrbit
(period=None, t0=0.0, b=0.0, duration=None, r_star=1.0)¶An orbit representing a set of planets transiting a common central
This orbit is parameterized by the observables of a transiting system, period, phase, duration, and impact parameter.
period – The orbital period of the planets in days.
t0 – The midpoint time of a reference transit for each planet in days.
b – The impact parameters of the orbits.
duration – The durations of the transits in days.
r_star – The radius of the star in R_sun
.
get_relative_position
(t)¶The planets’ positions relative to the star
t – The times where the position should be evaluated.
The components of the position vector at t
in units of
R_sun
.
exoplanet.
LimbDarkLightCurve
(u, model=None)¶A limb darkened light curve computed using starry
u (vector) – A vector of limb darkening coefficients.
get_light_curve
(orbit=None, r=None, t=None, texp=None, oversample=7, order=0, use_in_transit=True)¶Get the light curve for an orbit at a set of times
orbit – An object with a get_relative_position
method that
takes a tensor of times and returns a list of Cartesian
coordinates of a set of bodies relative to the central source.
This method should return three tensors (one for each
coordinate dimension) and each tensor should have the shape
append(t.shape, r.shape)
or append(t.shape, oversample,
r.shape)
when texp
is given. The first two coordinate
dimensions are treated as being in the plane of the sky and the
third coordinate is the line of sight with positive values
pointing away from the observer. For an example, take a look
at orbits.KeplerianOrbit
.
r (tensor) – The radius of the transiting body in the same units as
r_star
. This should have a shape that is consistent with
the coordinates returned by orbit
. In general, this means
that it should probably be a scalar or a vector with one entry
for each body in orbit
.
t (tensor) – The times where the light curve should be evaluated.
texp (Optional[tensor]) – The exposure time of each observation.
This can be a scalar or a tensor with the same shape as t
.
If texp
is provided, t
is assumed to indicate the
timestamp at the middle of an exposure of length texp
.
oversample (Optional[int]) – The number of function evaluations to use when numerically integrating the exposure time.
order (Optional[int]) – The order of the numerical integration
scheme. This must be one of the following: 0
for a
centered Riemann sum (equivalent to the “resampling” procedure
suggested by Kipping 2010), 1
for the trapezoid rule, or
2
for Simpson’s rule.
use_in_transit (Optional[bool]) – If True
, the model will only
be evaluated for the data points expected to be in transit
as computed using the in_transit
method on orbit
.
exoplanet.gp.
GP
(kernel, x, diag=None, mean=<exoplanet.gp.means.Zero object>, J=-1, model=None)¶The interface for computing Gaussian Process models with celerite
This class implements the method described in Foreman-Mackey et al. (2017) and Foreman-Mackey (2018) for scalable evaluation of Gaussian Process (GP) models in 1D.
Note
The input coordinates x
must be sorted in ascending order,
but this is not checked in the code. If the values are not sorted, the
behavior of the algorithm is undefined.
kernel – A exoplanet.gp.terms.Term
object the specifies the
GP kernel.
x – The input coordinates. This should be a 1D array and the elements must be sorted. Otherwise the results are undefined.
diag (Optional) – The extra diagonal to add to the covariance matrix.
This should have the same length as x
and correspond to the
excess variance for each data point. Note: this is different
from the usage in the celerite
package where the standard
deviation (instead of variance) is provided.
mean (Optional) – The mean function for the GP. This can be a constant scalar value or a callable that will be called with a single, one dimensional tensor argument specifying the input coordinates where the mean should be evaluated.
J (Optional) –
The width of the system. This is the J
parameter
from Foreman-Mackey (2018)
(not the original paper) so a real term contributes J += 1
and
a complex term contributes J += 2
. If you know this value in
advance, you can provide it. Otherwise, the code will try to work
it out.
marginal
(name, **kwargs)¶The marginal likelihood
name – The name of the node
observed – The observed data
A pymc3.DensityDist
with the likelihood
predict
(t=None, return_var=False, return_cov=False, predict_mean=False, kernel=None, _fast_mean=True)¶Compute the conditional distribution
t (optional) – The independent coordinates where the prediction should be evaluated. If not provided, this will be evaluated at the observations.
return_var (bool, optional) – Return the variance of the conditional distribution.
return_cov (bool, optional) – Return the full covariance matrix of the conditional distribution.
predict_mean (bool, optional) – Include the mean function in the prediction.
kernel (optional) – If provided, compute the conditional distribution using a different kernel. This is generally used to separate the contributions from different model components.
RuntimeError – if GP.condition()
or marginal()
are not
called first.
exoplanet.gp.terms.
Term
(**kwargs)¶The abstract base “term” that is the superclass of all other terms
Subclasses should overload the terms.Term.get_real_coefficients()
and terms.Term.get_complex_coefficients()
methods.
exoplanet.gp.terms.
RealTerm
(**kwargs)¶The simplest celerite term
This term has the form
with the parameters a
and c
.
Strictly speaking, for a sum of terms, the parameter a
could be
allowed to go negative but since it is somewhat subtle to ensure positive
definiteness, we recommend keeping both parameters strictly positive.
Advanced users can build a custom term that has negative coefficients but
care should be taken to ensure positivity.
a or log_a (tensor) – The amplitude of the term.
c or log_c (tensor) – The exponent of the term.
exoplanet.gp.terms.
ComplexTerm
(**kwargs)¶A general celerite term
This term has the form
with the parameters a
, b
, c
, and d
.
This term will only correspond to a positive definite kernel (on its own) if \(a_j\,c_j \ge b_j\,d_j\).
a or log_a (tensor) – The real part of amplitude.
b or log_b (tensor) – The imaginary part of amplitude.
c or log_c (tensor) – The real part of the exponent.
d or log_d (tensor) – The imaginary part of exponent.
exoplanet.gp.terms.
SHOTerm
(*args, **kwargs)¶A term representing a stochastically-driven, damped harmonic oscillator
The PSD of this term is
with the parameters S0
, Q
, and w0
.
S0 or log_S0 (tensor) – The parameter \(S_0\).
Q or log_Q (tensor) – The parameter \(Q\).
w0 or log_w0 (tensor) – The parameter \(\omega_0\).
Sw4 or log_Sw4 (tensor) – It can sometimes be more efficient to
parameterize the amplitude of a SHO kernel using
\(S_0\,{\omega_0}^4\) instead of \(S_0\) directly since
\(S_0\) and \(\omega_0\) are strongly correlated. If
provided, S0
will be computed from Sw4
and w0
.
exoplanet.gp.terms.
Matern32Term
(**kwargs)¶A term that approximates a Matern-3/2 function
This term is defined as
with the parameters sigma
and rho
. The parameter eps
controls the quality of the approximation since, in the limit
\(\epsilon \to 0\) this becomes the Matern-3/2 function
sigma or log_sigma (tensor) – The parameter \(\sigma\).
rho or log_rho (tensor) – The parameter \(\rho\).
eps (Optional[float]) – The value of the parameter \(\epsilon\). (default: 0.01)
exoplanet.gp.terms.
RotationTerm
(**kwargs)¶A mixture of two SHO terms that can be used to model stellar rotation
This term has two modes in Fourier space: one at period
and one at
0.5 * period
. This can be a good descriptive model for a wide range of
stochastic variability in stellar time series from rotation to pulsations.
amp or log_amp (tensor) – The amplitude of the variability.
period or log_period (tensor) – The primary period of variability.
Q0 or log_Q0 (tensor) – The quality factor (or really the quality factor minus one half) for the secondary oscillation.
deltaQ or log_deltaQ (tensor) – The difference between the quality factors
of the first and the second modes. This parameterization (if
deltaQ > 0
) ensures that the primary mode alway has higher
quality.
mix – The fractional amplitude of the secondary mode compared to the
primary. This should probably always be 0 < mix < 1
.
exoplanet.
estimate_semi_amplitude
(periods, x, y, yerr=None, t0s=None)¶Estimate the RV semi-amplitudes for planets in an RV series
periods – The periods of the planets. Assumed to be in days
if not
an AstroPy Quantity.
x – The observation times. Assumed to be in days
if not an AstroPy
Quantity.
y – The radial velocities. Assumed to be in m/s
if not an AstroPy
Quantity.
yerr (Optional) – The uncertainty on y
.
t0s (Optional) – The time of a reference transit for each planet, if known.
An estimate of the semi-amplitude of each planet in units of m/s
.
exoplanet.
estimate_minimum_mass
(periods, x, y, yerr=None, t0s=None, m_star=1)¶Estimate the minimum mass(es) for planets in an RV series
periods – The periods of the planets. Assumed to be in days
if not
an AstroPy Quantity.
x – The observation times. Assumed to be in days
if not an AstroPy
Quantity.
y – The radial velocities. Assumed to be in m/s
if not an AstroPy
Quantity.
yerr (Optional) – The uncertainty on y
.
t0s (Optional) – The time of a reference transit for each planet, if known.
m_star (Optional) – The mass of the star. Assumed to be in M_sun
if not an AstroPy Quantity.
An estimate of the minimum mass of each planet as an AstroPy Quantity
with units of M_jupiter
.
exoplanet.
lomb_scargle_estimator
(x, y, yerr=None, min_period=None, max_period=None, filter_period=None, max_peaks=2, **kwargs)¶Estimate period of a time series using the periodogram
x (ndarray[N]) – The times of the observations
y (ndarray[N]) – The observations at times x
yerr (Optional[ndarray[N]]) – The uncertainties on y
min_period (Optional[float]) – The minimum period to consider
max_period (Optional[float]) – The maximum period to consider
filter_period (Optional[float]) – If given, use a high-pass filter to down-weight period longer than this
max_peaks (Optional[int]) – The maximum number of peaks to return (default: 2)
A dictionary with the computed periodogram
and the parameters for
up to max_peaks
peaks in the periodogram.
exoplanet.
autocorr_estimator
(x, y, yerr=None, min_period=None, max_period=None, oversample=2.0, smooth=2.0, max_peaks=10)¶Estimate the period of a time series using the autocorrelation function
Note
The signal is interpolated onto a uniform grid in time so that the autocorrelation function can be computed.
x (ndarray[N]) – The times of the observations
y (ndarray[N]) – The observations at times x
yerr (Optional[ndarray[N]]) – The uncertainties on y
min_period (Optional[float]) – The minimum period to consider
max_period (Optional[float]) – The maximum period to consider
oversample (Optional[float]) – When interpolating, oversample the times by this factor (default: 2.0)
smooth (Optional[float]) – Smooth the autocorrelation function by this factor times the minimum period (default: 2.0)
max_peaks (Optional[int]) – The maximum number of peaks to identify in the autocorrelation function (default: 10)
A dictionary with the computed autocorrelation function and the
estimated period. For compatibility with the
lomb_scargle_estimator()
, the period is returned as a list with
the key peaks
.
exoplanet.
bls_estimator
(x, y, yerr=None, duration=0.2, min_period=None, max_period=None, objective=None, method=None, oversample=10, **kwargs)¶Estimate the period of a time series using box least squares
All extra keyword arguments are passed directly to
astropy.timeseries.BoxLeastSquares.autopower()
.
A dictionary with the computed autocorrelation function and the
estimated period. For compatibility with the
lomb_scargle_estimator()
, the period is returned as a list with
the key peaks
.
exoplanet.distributions.
UnitUniform
(*args, **kwargs)¶A uniform distribution between zero and one
This can sometimes get better performance than pm.Uniform.dist(0, 1)
.
exoplanet.distributions.
UnitVector
(*args, **kwargs)¶A vector where the sum of squares is fixed to unity
For a multidimensional shape, the normalization is performed along the last dimension.
exoplanet.distributions.
Angle
(*args, **kwargs)¶An angle constrained to be in the range -pi to pi
The actual sampling is performed in the two dimensional vector space
(sin(theta), cos(theta))
so that the sampler doesn’t see a
discontinuity at pi.
exoplanet.distributions.
Periodic
(lower=0, upper=1, **kwargs)¶An periodic parameter in a given range
Like the Angle
distribution, the actual sampling is performed in
a two dimensional vector space (sin(theta), cos(theta))
and then
transformed into the range [lower, upper)
.
lower – The lower bound on the range.
upper – The upper bound on the range.
exoplanet.distributions.
QuadLimbDark
(*args, **kwargs)¶An uninformative prior for quadratic limb darkening parameters
This is an implementation of the Kipping (2013) reparameterization of the two-parameter limb darkening model to allow for efficient and uninformative sampling.
exoplanet.distributions.
ImpactParameter
(ror=None, **kwargs)¶The impact parameter distribution for a transiting planet
ror – A scalar, tensor, or PyMC3 distribution representing the radius
ratio between the planet and star. Conditioned on a value of
ror
, this will be uniformly distributed between 0
and
1+ror
.
exoplanet.distributions.eccentricity.
kipping13
(name, fixed=False, long=None, model=None, **kwargs)¶The beta eccentricity distribution fit by Kipping (2013)
The beta distribution parameters fit by Kipping (2013).
name (str) – The name of the eccentricity variable.
fixed (bool, optional) – If True
, use the posterior median
hyperparameters. Otherwise, marginalize over the parameters.
long (bool, optional) – If True
, use the parameters for the long
period fit. If False
, use the parameters for the short period
fit. If not given, the parameters fit using the full dataset are
used.
The eccentricity distribution.
exoplanet.distributions.eccentricity.
vaneylen19
(name, fixed=False, multi=False, model=None, **kwargs)¶The eccentricity distribution for small planets
The mixture distribution fit by Van Eylen et al. (2019) to a population of well-characterized small transiting planets observed by Kepler.
name (str) – The name of the eccentricity variable.
fixed (bool, optional) – If True
, use the posterior median
hyperparameters. Otherwise, marginalize over the parameters.
multi (bool, optional) – If True
, use the distribution for systems
with multiple transiting planets. If False
(default), use the
distribution for systems with only one detected transiting planet.
The eccentricity distribution.
exoplanet.
optimize
(start=None, vars=None, model=None, return_info=False, verbose=True, **kwargs)¶Maximize the log prob of a PyMC3 model using scipy
All extra arguments are passed directly to the scipy.optimize.minimize
function.
start – The PyMC3 coordinate dictionary of the starting position
vars – The variables to optimize
model – The PyMC3 model
return_info – Return both the coordinate dictionary and the result of
scipy.optimize.minimize
verbose – Print the success flag and log probability to the screen
exoplanet.
eval_in_model
(var, point=None, return_func=False, model=None, **kwargs)¶Evaluate a Theano tensor or PyMC3 variable in a PyMC3 model
This method builds a Theano function for evaluating a node in the graph
given the required parameters. This will also cache the compiled Theano
function in the current pymc3.Model
to reduce the overhead of calling
this function many times.
var – The variable or tensor to evaluate.
point (Optional) – A dict
of input parameter values. This can be
model.test_point
(default), the result of pymc3.find_MAP
,
a point in a pymc3.MultiTrace
or any other representation of
the input parameters.
return_func (Optional[bool]) – If False
(default), return the
evaluated variable. If True
, return the result, the Theano
function and the list of arguments for that function.
Depending on return_func
, either the value of var
at point
,
or this value, the Theano function, and the input arguments.
exoplanet.
get_samples_from_trace
(trace, size=1)¶Generate random samples from a PyMC3 MultiTrace
trace – The MultiTrace
.
size – The number of samples to generate.
exoplanet.
get_dense_nuts_step
(start=None, adaptation_window=101, doubling=True, model=None, **kwargs)¶Get a NUTS step function with a dense mass matrix
The entries in the mass matrix will be tuned based on the sample
covariances during tuning. All extra arguments are passed directly to
pymc3.NUTS
.
start (dict, optional) – A starting point in parameter space. If not
provided, the model’s test_point
is used.
adaptation_window (int, optional) – The (initial) size of the window used for sample covariance estimation.
doubling (bool, optional) – If True
(default) the adaptation window
is doubled each time the matrix is updated.
exoplanet.orbits.ttv.
compute_expected_transit_times
(min_time, max_time, period, t0)¶Compute the expected transit times within a dataset
exoplanet.units.
with_unit
(obj, unit)¶Decorate a Theano tensor with Astropy units
obj – The Theano tensor
unit (astropy.Unit) – The units for this object
TypeError – If the tensor already has units
exoplanet.units.
has_unit
(obj)¶Does an object have units as defined by exoplanet?
exoplanet.units.
to_unit
(obj, target)¶Convert a Theano tensor with units to a target set of units
obj – The Theano tensor
target (astropy.Unit) – The target units
A Theano tensor in the right units