MulensModel.model module¶
 class MulensModel.model.Model(parameters=None, coords=None, ra=None, dec=None, ephemerides_file=None)¶
Bases:
object
A Model for a microlensing event with the specified parameters.
 Arguments :
parameters: dictionary,
ModelParameters
coords
: str, astropy.SkyCoords, MulensModel.Coordinates, optionalSky coordinates of the event. If type is str, then it is assumed that the units are hour angle and degrees for RA and Dec, respectively.
 ra, dec: str, optional
Sky coordinates of the event.
 ephemerides_file: str, optional
Specify name of the file with satellite ephemerides. See
MulensData
for more details. Note that if you provide file name here, then it will affect all calculations for this model. In most cases, you want to combine groundbased and satellite data and in those cases set ephemerides_file for specificMulensData
instance to pass satellite information.
 Attributes :
 ephemerides_file: str
Name of file with satellite ephemerides.
Default values for parallax are all True. Use
parallax()
to turn different parallax effects ON/OFF. If using satellite parallax, you may also specify an ephemerides_file (seeMulensData
).Note that you can print an instance of Model, which shows you parameters in a nice way, e.g.,
model = Model(parameters={'t_0': 2456789.0, ....}) print(model)
This will provide information on parameter values, coordinates, methods used for magnification calculations, and limbdarkening coefficients.
 plot_magnification(times=None, t_range=None, t_start=None, t_stop=None, dt=None, n_epochs=None, subtract_2450000=False, subtract_2460000=False, satellite_skycoord=None, gamma=None, source_flux_ratio=None, flux_ratio_constraint=None, **kwargs)¶
Plot the model magnification curve.
 Keywords :
see
plot_lc()
 gamma:
 satellite_skycoord:
 source_flux_ratio: float
If the model has two sources, source_flux_ratio is the ratio of source_flux_2 / source_flux_1
flux_ratio_constraint: DEPRECATED. Use source_flux_ratio instead.
**kwargs
:any arguments accepted by
matplotlib.pyplot.plot()
.
 get_lc(times=None, t_range=None, t_start=None, t_stop=None, dt=None, n_epochs=None, source_flux=None, blend_flux=None, source_flux_ratio=None, gamma=None, bandpass=None)¶
Calculate model light curve in magnitudes.
 Keywords :
 times: [float, list, numpy.ndarray]
a list of times at which to plot the magnifications
t_range, t_start, t_stop, dt, n_epochs: see
set_times()
 source_flux: float or list
Explicitly specify the source flux(es) in a system where flux = 1 corresponds to
MulensModel.utils.MAG_ZEROPOINT
(= 22 mag). If the model has n_source > 1, source_flux may be specified as a list: one value for each source. Alternatively, if source_flux is specified as a float, source_flux_ratio should also be specified. Then, source_flux is taken to be the flux of the first source, and the other source fluxes are derived using source_flux_ratio. blend_flux: float
Explicitly specify the blend flux in a system where flux = 1 corresponds to
MulensModel.utils.MAG_ZEROPOINT
(= 22 mag). source_flux_ratio: float, Optional
If the model has two sources, source_flux_ratio is the ratio of source_flux_2 / source_flux_1.
 gamma, bandpass:
 Returns :
 magnification: numpy.ndarray
Magnification values for each epoch.
 plot_lc(times=None, t_range=None, t_start=None, t_stop=None, dt=None, n_epochs=None, source_flux=None, blend_flux=None, source_flux_ratio=None, gamma=None, bandpass=None, subtract_2450000=False, subtract_2460000=False, data_ref=None, flux_ratio_constraint=None, fit_blending=None, f_source=None, f_blend=None, phot_fmt='mag', **kwargs)¶
Plot the model light curve in magnitudes.
 Keywords :
 times: [float, list, numpy.ndarray]
a list of times at which to plot the magnifications
 t_range, t_start, t_stop, dt, n_epochs:
see
set_times()
 source_flux, blend_flux, source_flux_ratio:
see
get_lc()
 gamma, bandpass:
 subtract_2450000, subtract_2460000: boolean, optional
If True, subtracts 2450000 or 2460000 from the time axis to get more humanscale numbers. If using, make sure to also set the same settings for all other plotting calls (e.g.
plot_data()
) data_ref: DEPRECATED
Specify source_flux and blend_flux instead or use plotting functions in py:class:~MulensModel.Event()
 flux_ratio_constraint: DEPRECATED
Use source_flux_ratio instead
 fit_blending: DEPRECATED
Use py:class:~MulensModel.Event() for fitting.
 f_source, f_blend: DEPRECATED
use source_flux or blend_flux instead.
 phot_fmt: str
Specifies whether the photometry is plotted in magnitude or flux space. Accepts either ‘mag’ or ‘flux’. Default = ‘mag’.
**kwargs
:any arguments accepted by
matplotlib.pyplot.plot()
.
 plot_caustics(n_points=5000, epoch=None, **kwargs)¶
Plot the caustic structure. See
MulensModel.caustics.Caustics.plot()
for binary lenses. For a single lens it just marks (0, 0) point and the first two parameters are ignored. Additional parameters :
 n_points: int, optional
The number of points to calculate along the caustic. Defaults to 5000.
 epoch: float, optional
Epoch for which separation s will be used. Important for models with orbital motion. Defaults to t_0_kep, which defaults to t_0.
**kwargs
:keywords accepted by
matplotlib.pyplot.scatter()
 update_caustics(epoch=None)¶
Updates
caustics
property for given epoch. Parameters :
 epoch: float
For orbital motion models, epoch for which separation s is calculated to calculate
caustics
. Defaults to t_0_kep, which defaults to t_0.
 plot_trajectory(times=None, t_range=None, t_start=None, t_stop=None, dt=None, n_epochs=None, caustics=False, arrow=True, satellite_skycoord=None, arrow_kwargs=None, show_data=None, **kwargs)¶
Plot the source trajectory.
Keywords (all optional) :
 times, t_range, t_start, t_stop, dt, n_epochs:
May all be used to specify exactly when to plot the source trajectory. See also
plot_lc()
andset_times()
. caustics: boolean
plot the caustic structure in addition to the source trajectory. default=False (off). For finer control of plotting features, e.g. color, use
plot_caustics()
instead. arrow: boolean
Show the direction of the source motion. Default is True.
satellite_skycoord: astropy.SkyCoord or
MulensModel.satelliteskycoord.SatelliteSkyCoord
Allows the user to specify that the trajectory is calculated for a satellite. If astropy.SkyCoord object is provided, then these are satellite positions for all epochs. See also
get_satellite_coords()
 arrow_kwargs: dict
Kwargs that are passed to
pyplot.arrow()
. If no color is given here, then we use one specified in**kwargs
and if nothing is there, then we use black. The size of the arrow is determined based on limits of current axis. If those are not adequate, then change the size by specifying width keyword and maybe other as well. Note that arrow_kwargs are of dict type and are different than**kwargs
. show_data: DEPRECATED
Use py:class:~MulensModel.Event() for plotting data with models.
**kwargs
Controls plotting features of the trajectory. It’s passed to
pyplot.plot()
.
Note that in order to have equal scaling of both axis (i.e., make circles look circular), you have to call appropriate pyplot command. This can be one of these commands:
pyplot.axis('equal') pyplot.axis('scaled') pyplot.axis('square') pyplot.gca().set_aspect('equal')
They have slightly different behavior.
 plot_source(times=None, **kwargs)¶
Plot source: circles of the radius rho at positions corresponding to source positions at times. When the rho is not defined, then X symbols are plotted.
 Parameters:
 times: float or np.ndarray
epochs for which source positions will be plotted
**kwargs
:Keyword arguments passed to matplotlib.Circle. Examples:
color='red'
,fill=False
,linewidth=3
,alpha=0.5
. When the rho is not defined, then keyword arguments are passed to matplotlib.plot.
Note that it is likely that with default axis scaling, the circles may be plotted as ellipses. To mitigate it, use:
plt.gca().set_aspect('equal')
orplt.axis('equal')
(the other possible options are'scaled'
or'square'
).
 get_trajectory(times, satellite_skycoord=None)¶
Get the source trajectory for the given set of times.
 Parameters :
 times: np.ndarray, list of floats, or float
Epochs for which source positions are requested.
 satellite_skycoord: astropy.SkyCoord
Allows the user to specify that the trajectory is calculated for a satellite. If astropy.SkyCoord object is provided, then these are satellite positions for all epochs. See also
get_satellite_coords()
 ReturnsA :py:class:`~MulensModel.trajectory.Trajectory object. If
n_sources > 1, returns a tuple of `:py:class:`~MulensModel.trajectory.Trajectory`s
 set_times(t_range=None, t_start=None, t_stop=None, dt=None, n_epochs=1000)¶
Return a list of times. If no keywords are specified, default is 1000 epochs from [\(t_0  1.5 * t_E\), \(t_0 + 1.5 * t_E\)] range. For binary source models, respectively, smaller and larger of t_0_1/t_0_2 values are used.
 Parameters (all optional):
 t_range: [list, tuple]
A range of times of the form [t_start, t_stop]
 t_start, t_stop: float
a start or stop time.
 dt: float
the interval spacing between successive points
 n_epochs: int
the number of epochs (evenly spaced)
 Returns :
 times: np.ndarray
Vector of epochs.
 set_magnification_methods(methods, source=None)¶
Sets methods used for magnification calculation. See
MagnificationCurve
for a list of implemented methods. Parameters :
 methods: list
List that specifies which methods (str) should be used when (float values for Julian dates). Given method will be used for times between the times between which it is on the list, e.g.,
methods = [ 2455746., 'Quadrupole', 2455746.6, 'Hexadecapole', 2455746.7, 'VBBL', 2455747., 'Hexadecapole', 2455747.15, 'Quadrupole', 2455748.]
 source: int or None, optional
Which source do the given methods apply to? Accepts 1, 2, or None (i.e., all sources). Default is None
 get_magnification_methods(source=None)¶
Gets methods used for magnification calculation. See
set_magnification_methods()
 Parameters :
 source: int or None, optional
Which source do the given methods apply to? Accepts 1, 2, or None (i.e., all sources). Default is None.
 property methods¶
list of methods used for magnification calculation or dict of lists if there are multiple sources.
 set_default_magnification_method(method)¶
Stores information on method to be used, when no method is directly specified. See
MagnificationCurve
for a list of implemented methods. Parameters:
 method: str
Name of the method to be used.
 property default_magnification_method¶
Stores information on method to be used, when no method is directly specified. See
MagnificationCurve
for a list of implemented methods. Parameters:
 method: str
Name of the method to be used.
 set_magnification_methods_parameters(methods_parameters)¶
Set additional parameters for magnification calculation methods.
 Parameters :
 methods_parameters: dict
Dictionary that for method names (keys) returns dictionary in the form of
**kwargs
that are passed to given method, e.g.,{'VBBL': {'accuracy': 0.005}}
.
 get_magnification_methods_parameters(method)¶
Get additional parameters for a specific magnification calculation method or methods.
 Parameters :
 method: str, list
Name of method or a list of the names for which parameters will be returned.
 Returns :
 method_parameters: dict
 set_limb_coeff_gamma(bandpass, coeff)¶
Store gamma limb darkening coefficient for given band. See also
LimbDarkeningCoeffs
. Parameters :
 bandpass: str
Bandpass for the coefficient you provide.
 coeff: float
Value of the coefficient.
 get_limb_coeff_gamma(bandpass)¶
Get gamma limb darkening coefficient for given band.
 Parameters :
 bandpass: str
Bandpass for which coefficient will be provided.
 Returns :
 gamma: float
limb darkening coefficient
 set_limb_coeff_u(bandpass, coeff)¶
Store u limb darkening coefficient for given band. See also
MulensModel.limbdarkeningcoeffs.LimbDarkeningCoeffs
. Parameters :
 bandpass: str
Bandpass for which coefficient you provide.
 coeff: float
Value of the coefficient.
 get_limb_coeff_u(bandpass)¶
Get u limb darkening coefficient for given band.
 Parameters :
 bandpass: str
Bandpass for which coefficient will be provided.
 Returns :
 u: float
limb darkening coefficient
 parallax(earth_orbital=None, satellite=None, topocentric=None)¶
Specifies the types of the microlensing parallax that will be included in calculations.
Parameters :
 earth_orbital: boolean, optional
Do you want to include the effect of Earth motion about the Sun? Default is False.
 satellite: boolean, optional
Do you want to include the effect of difference due to separation between the Earth and satellite? Note that this separation changes over time. Default is False.
 topocentric: boolean, optional
Do you want to include the effect of different positions of observatories on the Earth? Default is False. Note that this is significant only for very high magnification events and if high quality datasets are analyzed. Hence, this effect is rarely needed. Not Implemented yet.
 get_parallax()¶
Returns dict that specifies the types of the microlensing parallax that are included in calculations.
 Returns :
 parallax: dict
For keys
'earth_orbital'
,'satellite'
, and'topocentric'
returns bool.
 get_satellite_coords(times)¶
Get astropy.SkyCoord object that gives satellite positions for given times. see also
MulensModel.satelliteskycoord.SatelliteSkyCoord
 Parameters :
 times: np.ndarray or list
Epochs for which satellite position is requested.
 Returns :
 satellite_skycoord: astropy.SkyCoord
SkyCoord giving satellite positions. The parameter representation is set to ‘spherical’. If ephemerides_file is not set, returns None.
 get_magnification(time, satellite_skycoord=None, gamma=None, bandpass=None, source_flux_ratio=None, separate=False, flux_ratio_constraint=None)¶
Calculate the model magnification for the given time(s).
 Parameters :
 time: np.ndarray, list of floats, or float
Times for which magnification values are requested.
 satellite_skycoord: astropy.coordinates.SkyCoord, optional
SkyCoord object that gives satellite positions. Must be the same length as time parameter. Use only for satellite parallax calculations.
 gamma: float, optional
The limbdarkening coefficient in gamma convention. Default is 0 which means no limb darkening effect.
 bandpass: str, optional
The bandpass for setting the limbdarkening coefficient. Expects that you have used
set_limb_coeff_gamma()
orset_limb_coeff_u()
. Only ONE of ‘gamma’ or ‘bandpass’ may be specified. source_flux_ratio: float
If the model has two sources, source_flux_ratio is the ratio of source_flux_2 / source_flux_1
 separate: boolean, optional
For binary source models, return magnification of each source separately. Default is False and then only effective magnification is returned.
 flux_ratio_constraint: DEPRECATED
Use source_flux_ratio instead.
 Returns :
 magnification: np.ndarray
A vector of calculated magnification values. For binary source models, the effective magnification is returned (unless separate=True).
 magnification(*args, **kwargs)¶
DEPRECATED
Use
get_magnification()
instead.
 property parameters¶

Model parameters.
 property n_lenses¶
int
number of objects in the lens system
 property n_sources¶
int
number of luminous sources; it’s possible to be 1 for xallarap model
 is_static()¶
 property coords¶
see
Coordinates
 property bandpasses¶
list
List of all bandpasses for which limb darkening coefficients are set.
 reset_plot_properties()¶
DEPRECATED
Resets internal plotting properties of all attached datasets.
 plot_data(data_ref=None, show_errorbars=None, show_bad=None, color_list=None, marker_list=None, size_list=None, label_list=None, alpha_list=None, zorder_list=None, subtract_2450000=False, subtract_2460000=False, **kwargs)¶
DEPRECATED
Plot the data scaled to the model.
 Keywords (all optional):
 data_ref: see
get_ref_fluxes()
If data_ref is not specified, uses the first dataset as the reference for flux scale.
 show_errorbars: boolean or None
Do you want errorbars to be shown for all datasets? Default is None, which means the option is taken from each dataset plotting properties (for which default is True). If True, then data are plotted using matplotlib.errorbar(). If False, then data are plotted using matplotlib.scatter().
 show_bad: boolean or None
Do you want data marked as bad to be shown? Default is None, which means the option is taken from each dataset plotting properties (for which default is False). If bad data are shown, then they are plotted with ‘x’ marker.
 subtract_2450000, subtract_2460000: boolean
If True, subtracts 2450000 or 2460000 from the time axis to get more humanscale numbers. If using, make sure to also set the same settings for all other plotting calls (e.g.
plot_lc()
).**kwargs
:Passed to matplotlib plotting functions. Contrary to previous behavior,
**kwargs
are no longer remembered.
 data_ref: see
 plot_residuals(show_errorbars=None, color_list=None, marker_list=None, size_list=None, label_list=None, alpha_list=None, zorder_list=None, data_ref=None, subtract_2450000=False, subtract_2460000=False, show_bad=None, **kwargs)¶
DEPRECATED
Plot the residuals (in magnitudes) of the model.
For explanation of keywords, see doctrings in
plot_data()
. Note different order of keywords.
 get_residuals(data_ref=None, type='mag', data=None)¶
DEPRECATED
Calculate the residuals from the model for each dataset at once, or just a single dataset.
Note: if residuals are returned in magnitudes, they are transformed to the magnitude system specified by data_ref, so only suitable for plotting.
 Keywords :
 data_ref: optional
see
get_ref_fluxes()
 type: str, optional
specify whether the residuals should be returned in magnitudes (‘mag’) or in flux (‘flux’). Default is ‘mag’.
 data:
MulensData
, optional dataset for which residuals are returned. If specified, then returned lists are single element.
 Returns :
 residuals: list
each element of the list is a np.ndarray with the residuals for the corresponding dataset.
 errorbars: list
the scaled errorbars for each point. For plotting errorbars for the residuals.
 plot_source_for_datasets(**kwargs)¶
DEPRECATED
Plot source positions for all linked datasets. Colors used for each dataset are the same used for plotting photometry.
 Parameters:
**kwargs
:see
plot_source()
 get_ref_fluxes(data_ref=None, fit_blending=None)¶
DEPRECATED
Get source and blending fluxes for the model by finding the bestfit values compared to data_ref.
 Parameters :
 data_ref:
MulensData
or int Reference dataset. If int, corresponds to the index of the dataset in self.datasets. If None, than the first dataset will be used.
 fit_blending: boolean
True if blending flux is going to be fitted (default), False if blending flux is fixed at 0.
 data_ref:
 Returns :
 f_source: np.ndarray
Sources’ flux; normally of size (1). If it is of size (1) for a double source model, then it is a sum of fluxes of both sources.
 f_blend: float
blending flux
Determine the reference flux system from the datasets. The data_ref may either be a dataset or the index of a dataset (if
Model.set_datasets()
was previously called). If data_ref is not set, it will use the first dataset. If you call this without callingset_datasets()
first, there will be an exception and that’s on you.
 set_source_flux_ratio(ratio)¶
DEPRECATED
Sets flux ratio of sources for binary source models. If you also call
set_source_flux_ratio_for_band()
, then the value set here will be used when: 1) no band is specified, or 2) band is specified but flux ratio for given band was not specified. Parameters :
 ratio: float or None
The ratio of fluxes of source no. 2 to source no. 1, i.e., flux_source_2/flux_source_1. Setting it to None removes the internal information, i.e., flux ratio will be fitted via regression (unless specific value is provided for bandpass).
 set_source_flux_ratio_for_band(band, ratio)¶
DEPRECATED
Sets flux ratio for binary source models for given band.
 Parameters :
 band: str
Band for which constraint is given.
 ratio: float
ratio of fluxes of source no. 2 to source no. 1, i.e., flux_source_band_2/flux_source_band_1
 property data_magnification¶
DEPRECATED
list
A list of magnifications calculated for every dataset in
datasets
.
 get_data_magnification(dataset)¶
DEPRECATED
Get the model magnification for a dataset.
 Parameters :
 dataset:
MulensData
Dataset with epochs for which magnification will be given. Satellite and limb darkening information is taken into account.
 dataset:
 Returns :
 magnification_vector: np.ndarray
Values on magnification.
 property datasets¶
DEPRECATED
list of
MulensData
Datasets linked to given model. Note that these can be changed by
Event
instances. This happens when the same model is linked to multipleEvent
instances.
 set_datasets(datasets, data_ref=0)¶
DEPRECATED
Set
datasets
property Parameters :
 datasets: list of
MulensData
Datasets to be stored.
data_ref: int or,
MulensData
, optionalReference dataset.
 datasets: list of