Basis

class orbitize.basis.Basis(stellar_or_system_mass, mass_err, plx, plx_err, num_secondary_bodies, fit_secondary_mass, angle_upperlim=6.283185307179586, hipparcos_IAD=None, rv=False, rv_instruments=None)[source]

Abstract base class for different basis sets. All new basis objects should inherit from this class. This class is meant to control how priors are assigned to various basis sets and how conversions are made from the basis sets to the standard keplarian set.

Author: Tirth, 2021

set_default_mass_priors(priors_arr, labels_arr)[source]

Adds the necessary priors for the stellar and/or companion masses.

Parameters

priors_arr (list of orbitize.priors.Prior objects) – holds the prior objects for each parameter to be fitted (updated here)
labels_arr (list of strings) – holds the name of all the parameters to be fitted (updated here)

set_hip_iad_priors(priors_arr, labels_arr)[source]

Adds the necessary priors relevant to the hipparcos data to ‘priors_arr’ and updates ‘labels_arr’ with the priors’ corresponding labels.

Parameters

priors_arr (list of orbitize.priors.Prior objects) – holds the prior objects for each parameter to be fitted (updated here)
labels_arr (list of strings) – holds the name of all the parameters to be fitted (updated here)

set_rv_priors(priors_arr, labels_arr)[source]

Adds the necessary priors if radial velocity data is supplied to ‘priors_arr’ and updates ‘labels_arr’ with the priors’ corresponding labels. This function assumes that ‘rv’ data has been supplied and a secondary mass is being fitted for.

Parameters

priors_arr (list of orbitize.priors.Prior objects) – holds the prior objects for each parameter to be fitted (updated here)
labels_arr (list of strings) – holds the name of all the parameters to be fitted (updated here)

verify_params()[source]: Displays warnings about the ‘fit_secondary_mass’ and ‘rv’ parameters for all basis sets. Can be overriden by any basis class depending on the necessary parameters that need to be checked.

class orbitize.basis.Period(stellar_or_system_mass, mass_err, plx, plx_err, num_secondary_bodies, fit_secondary_mass, angle_upperlim=6.283185307179586, hipparcos_IAD=None, rv=False, rv_instruments=None)[source]

Modification of the standard basis, swapping our sma for period: (per, ecc, inc, aop, pan, tau).

Parameters

stellar_or_system_mass (float) – mass of the primary star (if fitting for dynamical masses of both components) or total system mass (if fitting using relative astrometry only) [M_sol]
mass_err (float) – uncertainty on ‘stellar_or_system_mass’, in M_sol
plx (float) – mean parallax of the system, in mas
plx_err (float) – uncertainty on ‘plx’, in mas
num_secondary_bodies (int) – number of secondary bodies in the system, should be at least 1
fit_secondary_mass (bool) – if True, include the dynamical mass of orbitting body as fitted parameter, if False, ‘stellar_or_system_mass’ is taken to be total mass
angle_upperlim (float) – either pi or 2pi, to restrict the prior range for ‘pan’ parameter (default: 2pi)
hipparcos_IAD (orbitize.HipparcosLogProb object) – if not ‘None’, then add relevant priors to this data (default: None)
rv (bool) – if True, then there is radial velocity data and assign radial velocity priors, if False, then there is no radial velocity data and radial velocity priors are not assigned (default: False)
rv_instruments (np.array) – array of unique rv instruments from the originally supplied data (default: None)

construct_priors()[source]

Generates the parameter label array and initializes the corresponding priors for each parameter that’s to be sampled. For the standard basis, the parameters common to each companion are: per, ecc, inc, aop, pan, tau. Parallax, hipparcos (optional), rv (optional), and mass priors are added at the end.

Returns

list: list of strings (labels) that indicate the names of each parameter to sample

list: list of orbitize.priors.Prior objects that indicate the prior distribution of each label

Return type

tuple

to_period_basis(param_arr)[source]

Convert parameter array from standard basis to period basis by swapping out the semi-major axis parameter to period for each companion. This function is used primarily for testing purposes.

Parameters

param_arr (np.array of float) – RxM array of fitting parameters in the standard basis, where R is the number of parameters being fit, and M is the number of orbits. If M=1 (for MCMC), this can be a 1D array.

Returns

modifies ‘param_arr’ to contain the period for each companion: in each orbit rather than semi-major axis. Shape of ‘param_arr’ remains the same.

Return type

np.array of float

to_standard_basis(param_arr)[source]

Convert parameter array from period basis to standard basis by swapping out the period parameter to semi-major axis for each companion.

Parameters

param_arr (np.array of float) – RxM array of fitting parameters in the period basis, where R is the number of parameters being fit, and M is the number of orbits. If M=1 (for MCMC), this can be a 1D array.

Returns

modifies ‘param_arr’ to contain the semi-major axis for each companion: in each orbit rather than period. Shape of ‘param_arr’ remains the same.

Return type

np.array of float

class orbitize.basis.SemiAmp(stellar_or_system_mass, mass_err, plx, plx_err, num_secondary_bodies, fit_secondary_mass, angle_upperlim=6.283185307179586, hipparcos_IAD=None, rv=False, rv_instruments=None)[source]

Modification of the standard basis, swapping our sma for period and additionally sampling in the stellar radial velocity semi-amplitude: (per, ecc, inc, aop, pan, tau, K).

Note

Ideally, ‘fit_secondary_mass’ is true and rv data is supplied.

Parameters

stellar_or_system_mass (float) – mass of the primary star (if fitting for dynamical masses of both components) or total system mass (if fitting using relative astrometry only) [M_sol]
mass_err (float) – uncertainty on ‘stellar_or_system_mass’, in M_sol
plx (float) – mean parallax of the system, in mas
plx_err (float) – uncertainty on ‘plx’, in mas
num_secondary_bodies (int) – number of secondary bodies in the system, should be at least 1
fit_secondary_mass (bool) – if True, include the dynamical mass of orbitting body as fitted parameter, if False, ‘stellar_or_system_mass’ is taken to be total mass
angle_upperlim (float) – either pi or 2pi, to restrict the prior range for ‘pan’ parameter (default: 2*pi)
hipparcos_IAD (orbitize.HipparcosLogProb object) – if not ‘None’, then add relevant priors to this data (default: None)
rv (bool) – if True, then there is radial velocity data and assign radial velocity priors, if False, then there is no radial velocity data and radial velocity priors are not assigned (default: False)
rv_instruments (np.array) – array of unique rv instruments from the originally supplied data (default: None)

compute_companion_mass(period, ecc, inc, semi_amp, m0)[source]

Computes a single companion’s mass given period, eccentricity, inclination, stellar rv semi-amplitude, and stellar mass. Uses scipy.fsolve to compute the masses numerically.

Parameters

period (np.array of float) – the period values for each orbit for a single companion (can be float)
ecc (np.array of float) – the eccentricity values for each orbit for a single companion (can be float)
inc (np.array of float) – the inclination values for each orbit for a single companion (can be float)
semi_amp (np.array of float) – the stellar rv-semi amp values for each orbit (can be float)
m0 (np.array of float) – the stellar mass for each orbit (can be float)

Returns

the companion mass values for each orbit (can also just be a single float)

Return type

np.array of float

compute_companion_sma(period, m0, m_n)[source]

Computes a single companion’s semi-major axis using Kepler’s Third Law for each orbit.

Parameters

period (np.array of float) – the period values for each orbit for a single companion (can be float)
m0 (np.array of float) – the stellar mass for each orbit (can be float)
m_n (np.array of float) – the companion mass for each orbit (can be float)

Returns

the semi-major axis values for each orbit

Return type

np.array of float

construct_priors()[source]

Generates the parameter label array and initializes the corresponding priors for each parameter that’s to be sampled. For the semi-amp basis, the parameters common to each companion are: per, ecc, inc, aop, pan, tau, K (stellar rv semi-amplitude). Parallax, hipparcos (optional), rv (optional), and mass priors are added at the end.

The mass parameter will always be m0.

Returns

list: list of strings (labels) that indicate the names of each parameter to sample

list: list of orbitize.priors.Prior objects that indicate the prior distribution of each label

Return type

tuple

func(x, lhs, m0)[source]

Define function for scipy.fsolve to use when computing companion mass.

Parameters

x (float) – the companion mass to be calculated (Msol)
lhs (float) – the left hand side of the rv semi-amplitude equation (Msol^(1/3))
m0 (float) – the stellar mass (Msol)

Returns

the difference between the rhs and lhs of the rv semi-amplitude equation, ‘x’ is a: good companion mass when this difference is very close to zero

Return type

float

to_semi_amp_basis(param_arr)[source]

Convert parameter array from standard basis to semi-amp basis by swapping out the semi-major axis parameter to period for each companion and computing the stellar rv semi-amplitudes for each companion.

Parameters

param_arr (np.array of float) – RxM array of fitting parameters in the period basis, where R is the number of parameters being fit, and M is the number of orbits. If M=1 (for MCMC), this can be a 1D array.

Returns

modifies ‘param_arr’ to contain the semi-major axis for each companion: in each orbit rather than period, appends stellar rv semi-amplitude parameters, and removes companion masses

Return type

np.array of float

to_standard_basis(param_arr)[source]

Convert parameter array from semi-amp basis to standard basis by swapping out the period parameter to semi-major axis for each companion and computing the masses of each companion.

Parameters

param_arr (np.array of float) – RxM array of fitting parameters in the period basis, where R is the number of parameters being fit, and M is the number of orbits. If M=1 (for MCMC), this can be a 1D array.

Returns

modifies ‘param_arr’ to contain the semi-major axis for each companion: in each orbit rather than period, removes stellar rv semi-amplitude parameters for each companion, and appends the companion masses to ‘param_arr’

Return type

np.array of float

verify_params()[source]: Additionally warns that this basis will sample stellar mass rather than sample mass regardless of whether ‘fit_secondary_mass’ is True or not.

class orbitize.basis.Standard(stellar_or_system_mass, mass_err, plx, plx_err, num_secondary_bodies, fit_secondary_mass, angle_upperlim=6.283185307179586, hipparcos_IAD=None, rv=False, rv_instruments=None)[source]

Standard basis set based upon the 6 standard Keplarian elements: (sma, ecc, inc, aop, pan, tau).

Parameters

stellar_or_system_mass (float) – mass of the primary star (if fitting for dynamical masses of both components) or total system mass (if fitting using relative astrometry only) [M_sol]
mass_err (float) – uncertainty on ‘stellar_or_system_mass’, in M_sol
plx (float) – mean parallax of the system, in mas
plx_err (float) – uncertainty on ‘plx’, in mas
num_secondary_bodies (int) – number of secondary bodies in the system, should be at least 1
fit_secondary_mass (bool) – if True, include the dynamical mass of orbitting body as fitted parameter, if False, ‘stellar_or_system_mass’ is taken to be total mass
angle_upperlim (float) – either pi or 2pi, to restrict the prior range for ‘pan’ parameter (default: 2pi)
hipparcos_IAD (orbitize.HipparcosLogProb object) – if not ‘None’, then add relevant priors to this data (default: None)
rv (bool) – if True, then there is radial velocity data and assign radial velocity priors, if False, then there is no radial velocity data and radial velocity priors are not assigned (default: False)
rv_instruments (np.array) – array of unique rv instruments from the originally supplied data (default: None)

construct_priors()[source]

Generates the parameter label array and initializes the corresponding priors for each parameter that’s to be sampled. For the standard basis, the parameters common to each companion are: sma, ecc, inc, aop, pan, tau. Parallax, hipparcos (optional), rv (optional), and mass priors are added at the end.

Returns

list: list of strings (labels) that indicate the names of each parameter to sample

list: list of orbitize.priors.Prior objects that indicate the prior distribution of each label

Return type

tuple

to_standard_basis(param_arr)[source]

For standard basis, no conversion needs to be made.

Parameters: param_arr (np.array of float) – RxM array of fitting parameters in the standard basis, where R is the number of parameters being fit, and M is the number of orbits. If M=1 (for MCMC), this can be a 1d array.
Returns: param_arr without any modification
Return type: np.array of float

class orbitize.basis.XYZ(stellar_or_system_mass, mass_err, plx, plx_err, num_secondary_bodies, fit_secondary_mass, data_table, best_epoch_idx, epochs, angle_upperlim=6.283185307179586, hipparcos_IAD=None, rv=False, rv_instruments=None)[source]

Defines an orbit using the companion’s position and velocity components in XYZ space (x, y, z, xdot, ydot, zdot). The conversion algorithms used for this basis are defined in the following paper: http://www.dept.aoe.vt.edu/~lutze/AOE4134/9OrbitInSpace.pdf

Note

Does not have support with sep,pa data yet.

Note

Does not work for all multi-body data.

Parameters

stellar_or_system_mass (float) – mass of the primary star (if fitting for dynamical masses of both components) or total system mass (if fitting using relative astrometry only) [M_sol]
mass_err (float) – uncertainty on ‘stellar_or_system_mass’, in M_sol
plx (float) – mean parallax of the system, in mas
plx_err (float) – uncertainty on ‘plx’, in mas
num_secondary_bodies (int) – number of secondary bodies in the system, should be at least 1
fit_secondary_mass (bool) – if True, include the dynamical mass of orbitting body as fitted parameter, if False, ‘stellar_or_system_mass’ is taken to be total mass
input_table (astropy.table.Table) – output from ‘orbitize.read_input.read_file()’
best_epoch_idx (list) – indices of the epochs corresponding to the smallest uncertainties
epochs (list) – all of the astrometric epochs from ‘input_table’
angle_upperlim (float) – either pi or 2pi, to restrict the prior range for ‘pan’ parameter (default: 2*pi)
hipparcos_IAD (orbitize.HipparcosLogProb object) – if not ‘None’, then add relevant priors to this data (default: None)
rv (bool) – if True, then there is radial velocity data and assign radial velocity priors, if False, then there is no radial velocity data and radial velocity priors are not assigned (default: False)
rv_instruments (np.array) – array of unique rv instruments from the originally supplied data (default: None)

Author: Rodrigo

construct_priors()[source]

Generates the parameter label array and initializes the corresponding priors for each parameter that’s to be sampled. For the xyz basis, the parameters common to each companion are: x, y, z, xdot, ydot, zdot. Parallax, hipparcos (optional), rv (optional), and mass priors are added at the end.

The xyz basis describes the position and velocity vectors with reference to the local coordinate system (the origin of the system is star).

Returns

list: list of strings (labels) that indicate the names of each parameter to sample

list: list of orbitize.priors.Prior objects that indicate the prior distribution of each label

Return type

tuple

standard_to_xyz(epoch, elems, tau_ref_epoch=58849, tolerance=1e-09, max_iter=100)[source]

Converts array of orbital elements from the regular base of Keplerian orbits to positions and velocities in xyz Uses code from orbitize.kepler

Parameters

epoch (float) – Date in MJD of observation to calculate time of periastron passage (tau).
elems (np.array of floats) – Orbital elements (sma, ecc, inc, aop, pan, tau, plx, mtot). If more than 1 set of parameters is passed, the first dimension must be the number of orbital parameter sets, and the second the orbital elements.

Returns

Orbital elements in xyz (x-coordinate [au], y-coordinate [au], z-coordinate [au], velocity in x [km/s], velocity in y [km/s], velocity in z [km/s], parallax [mas], total mass of the two-body orbit

(M_* + M_planet) [Solar masses])

Return type

np.array

to_standard_basis(param_arr)[source]

Makes a call to ‘xyz_to_standard’ to convert each companion’s xyz parameters to the standard parameters an returns the updated array for conversion.

Parameters: param_arr (np.array of float) – RxM array of fitting parameters in the period basis, where R is the number of parameters being fit, and M is the number of orbits. If M=1 (for MCMC), this can be a 1D array.
Returns: Orbital elements in the standard basis for all companions.
Return type: np.array

to_xyz_basis(param_arr)[source]

Makes a call to ‘standard_to_xyz’ to convert each companion’s standard keplerian parameters to the xyz parameters an returns the updated array for conversion.

Parameters: param_arr (np.array of float) – RxM array of fitting parameters in the period basis, where R is the number of parameters being fit, and M is the number of orbits. If M=1 (for MCMC), this can be a 1D array.
Returns: Orbital elements in the xyz for all companions.
Return type: np.array

verify_params()[source]: For now, additionally throws exceptions if data is supplied in sep/pa or if the best epoch for each body is one of the last two (which would inevtably mess up how the priors are imposed).

xyz_to_standard(epoch, elems, tau_ref_epoch=58849)[source]

Converts array of orbital elements in terms of position and velocity in xyz to the standard basis.

Parameters

epoch (float) – Date in MJD of observation to calculate time of periastron passage (tau).
elems (np.array of floats) – Orbital elements in xyz basis (x-coordinate [au], y-coordinate [au], z-coordinate [au], velocity in x [km/s], velocity in y [km/s], velocity in z [km/s], parallax [mas], total mass of the two-body orbit (M_* + M_planet) [Solar masses]). If more than 1 set of parameters is passed, the first dimension must be the number of orbital parameter sets, and the second the orbital elements.

Returns

Orbital elements in the standard basis: (sma, ecc, inc, aop, pan, tau, plx, mtot)

Return type

np.array

orbitize.basis.switch_tau_epoch(old_tau, old_epoch, new_epoch, period)[source]

Convert tau to another tau that uses a different referench epoch

Parameters

old_tau (float or np.array) – old tau to convert
old_epoch (float or np.array) – old reference epoch (days, typically MJD)
new_epoch (float or np.array) – new reference epoch (days, same system as old_epoch)
period (float or np.array) – orbital period (years)

Returns

new taus

Return type

float or np.array

orbitize.basis.tau_to_manom(date, sma, mtot, tau, tau_ref_epoch)[source]

Gets the mean anomlay. Wrapper for kepler.tau_to_manom, kept here for backwards compatibility.

Parameters

date (float or np.array) – MJD
sma (float) – semi major axis (AU)
mtot (float) – total mass (M_sun)
tau (float) – epoch of periastron, in units of the orbital period
tau_ref_epoch (float) – reference epoch for tau

Returns

mean anomaly on that date [0, 2pi)

Return type

float or np.array

orbitize.basis.tau_to_tp(tau, ref_epoch, period, after_date=None)[source]

Convert tau (epoch of periastron in fractional orbital period after ref epoch) to t_p (date in days, usually MJD, but works with whatever system ref_epoch is given in)

Parameters

tau (float or np.array) – value of tau to convert
ref_epoch (float or np.array) – date (in days, typically MJD) that tau is defined relative to
period (float or np.array) – period (in years) that tau is noralized with
after_date (float) – tp will be the first periastron after this date. If None, use ref_epoch.

Returns

corresponding t_p of the taus

Return type

float or np.array

orbitize.basis.tp_to_tau(tp, ref_epoch, period)[source]

Convert t_p to tau

Parameters

tp (float or np.array) – value to t_p to convert (days, typically MJD)
ref_epoch (float or np.array) – reference epoch (in days) that tau is defined from. Same system as tp (e.g., MJD)
period (float or np.array) – period (in years) that tau is defined by

Returns

corresponding taus

Return type

float or np.array