FSPL User Class

FSPL_parallax

class model.FSPL_PhotAstrom_Par_Param1(*args, **kwargs)

Bases: ModelClassABC, FSPL_PhotAstrom, FSPL_Parallax, FSPL_PhotAstromParam1

Helper class that provides a standard way to create an ABC using inheritance.

Methods

animate(tE, time_steps, frame_time, name, ...)	Produces animation of microlensing event.
calc_piE_ecliptic()	Parallax: Get piE_ecliptic
get_amplification(t)	Parallax: Get the photometric amplification term at a set of times, t.
get_astrometry(t_obs[, ast_filt_idx])	Parallax: Get astrometry
get_astrometry_unlensed(t)	Outputs position of source unlensed.
get_centroid_shift(t[, ast_filt_idx])	Parallax: Get the centroid shift (in mas) for a list of observation times (in MJD).
get_geoproj_ast_params(t0par)
get_geoproj_params(t0par)
get_lens_astrometry(t_obs)	Parallax: Get lens astrometry
get_photometry(t_obs[, filt_idx, amp_arr, ...])	Get the photometry for each of the lensed source images.
get_resolved_amplification(t)	Parallax: Get the photometric amplification term at a set of times, t for both the plus and minus images.
get_source_outline_astrometry(r, n, center)	Return astrometric points that outline the outer circumference of the source star.

get_chi2_astrometry
get_chi2_photometry
get_lnL_constant
get_resolved_astrometry
log_likely_astrometry
log_likely_astrometry_each
log_likely_photometry
log_likely_photometry_each
start

animate(tE, time_steps, frame_time, name, size, zoom, astrometry)

Produces animation of microlensing event. This function takes the PSPL and makes an animation, the input variables are as follows

Parameters

tE:

number of einstein crossings times before/after the peak you want the animation to plot

e.g tE = 2 => graph will go from -2 tE to 2 tE

time_steps:

number of time steps before/after peak, so total number of time steps will be 2 times this value

frame_time:

times in ms of each frame in the animation

name: string

the animation will be saved as name.html

size: list

[horizontal, vertical] cm’s

zoom:

# of einstein radii plotted in vertical direction

calc_piE_ecliptic()

Parallax: Get piE_ecliptic

get_amplification(t)

Parallax: Get the photometric amplification term at a set of times, t.

Parameters

t:

Array of times in MJD.DDD

get_astrometry(t_obs, ast_filt_idx=0)

Parallax: Get astrometry

get_astrometry_unlensed(t)

Outputs position of source unlensed.

Input a list of times and it will output the position of the source had it not been lensed at each of the times in the list

e.g if n = 4, and say v = [1,0] & the times are [0,1,2] in years.

This will return

((( (1,0),(0,1),(-1,0),(0,-1) ), ( (2,0),(1,1),(0,0),(1,-1) ), ( (3,0),(2,1),(1,0),(2,-1) ))...

= (positions at t=0), (positions at t=1), (positions at t=2)

so np.array(positions) is an array which contains an array for each time step with the positions of all the points on the boundary of the source.

get_centroid_shift(t, ast_filt_idx=0)

Parallax: Get the centroid shift (in mas) for a list of observation times (in MJD).

get_lens_astrometry(t_obs)

Parallax: Get lens astrometry

get_photometry(t_obs, filt_idx=0, amp_arr=None, print_warning=True)

Get the photometry for each of the lensed source images.

Parameters

t_obsarray_like

Array of times to model.

Other Parameters

———-

amp_arrarray_like

Amplifications of each individual image at each time, i.e. amp_arr.shape = (len(t_obs), number of images at each t_obs).

This will over-ride t_obs; but is more efficient when calculating both photometry and astrometry. If None, then just use t_obs.

Returns

mag_modelarray_like

Magnitude of the centroid at t_obs.

get_resolved_amplification(t)

Parallax: Get the photometric amplification term at a set of times, t for both the plus and minus images.

Parameters

t:

Array of times in MJD.DDD

get_resolved_astrometry(t)

Parallax: Get the x, y astrometry for each of the two source images, which we label plus and minus.

Returns

[xS_plus, xS_minus]list of numpy arrays

• xS_plus is the vector position of the plus image.

• xS_minus is the vector position of the plus image.

get_source_outline_astrometry(r, n, center)

Return astrometric points that outline the outer circumference of the source star.

The outline is described as a circle of radius self.radius and is evaluated at self.n_outline number of points.

takes in the radius of the circle, centre position and number of points we are approximating the circle by and returns a numpy array of positions

e.g: ( ((1,0), (0,1), (-1,0), (0,-1)) ) if n = 4 and radius = 1

Returns

source_pointsnumpy array

Returns an array of shape = [2, self.n_outline, len(time)]