Parameterization Class Family

class model.PSBL_PhotAstromParam1(mLp, mLs, t0, xS0_E, xS0_N, beta, muL_E, muL_N, muS_E, muS_N, dL, dS, sep, alpha, b_sff, mag_src, dmag_Lp_Ls, raL=None, decL=None, obsLocation='earth', root_tol=1e-08)

Bases: PSPL_Param

Point source binary lens. Note that this is a STATIC binary lens, i.e. there is no orbital motion.

Attributes:

mLp, mLsfloat

Masses of the lenses (Msun)

t0float

Time of photometric peak, as seen from Earth (MJD.DDD)

xS0_Efloat

R.A. of source position on sky at t = t0 (arcsec) in an arbitrary ref. frame.

xS0_Nfloat

Dec. of source position on sky at t = t0 (arcsec) in an arbitrary ref. frame.

betafloat

Angular distance between the source and the GEOMETRIC center of the lenses on the plane of the sky (mas). Can be

• positive (u0_amp > 0 when u0_hat[0] > 0) or

• negative (u0_amp < 0 when u0_hat[0] < 0).

muL_Efloat

Lens system proper motion in the RA direction (mas/yr)

muL_Nfloat

Lens system proper motion in the Dec. direction (mas/yr)

muS_Efloat

Source proper motion in the RA direction (mas/yr)

muS_Nfloat

Source proper motion in the Dec. direction (mas/yr)

dLfloat

Distance from the observer to the lens system (pc)

dSfloat

Distance from the observer to the source (pc)

sepfloat

Angular separation of the two lenses (mas)

alphafloat

Angle made between the binary axis and North; measured in degrees East of North.

b_sffnumpy array or list

The ratio of the source flux to the total (source + neighbors + lenses). One for each filter.

mag_srcnumpy array or list

Source magnitude, unlensed. One in each filter.

dmag_Lp_Lsnumpy array or list

Magnitude difference of lens primary - lens secondary. If the primary lens is dark, then dmag_L1_L2 should be set to 20 (or some other large, positive number). If the secondary lens 2 is dark, then it should be set to -20. If they are both dark, then dmag_Lp_Ls=0 and b_sff=1. Note, in astrometric filters, we assume all the excess flux (i.e. 1 - b_sff) comes from the lenses, not any neighbors.

raL: float, optional

Right ascension of the lens in decimal degrees.

decL: float, optional

Declination of the lens in decimal degrees.

obsLocation: str or list[str], optional

The observers location for each photometric dataset (def=[‘earth’])

root_tolfloat

Tolerance in comparing the polynomial roots to the physical solutions. Default = 1e-8

class model.PSBL_PhotAstromParam2(t0, u0_amp, tE, thetaE, piS, piE_E, piE_N, xS0_E, xS0_N, muS_E, muS_N, q, sep, alpha, b_sff, mag_src, dmag_Lp_Ls, raL=None, decL=None, obsLocation='earth', root_tol=1e-08)

Bases: PSPL_Param

Point source binary lens. It has 3 more parameters than PSPL (additional mass term, separation, and angle of approach). Note that this is a STATIC binary lens, i.e. there is no orbital motion.

Attributes:

t0float

Time of photometric peak, as seen from Earth (MJD.DDD)

u0_ampfloat

Angular distance between the source and the GEOMETRIC center of the lenses on the plane of the sky at closest approach in units of thetaE. Can be

• positive (u0_amp > 0 when u0_hat[0] > 0) or

• negative (u0_amp < 0 when u0_hat[0] < 0).

tEfloat

Einstein crossing time (days).

thetaEfloat

The size of the Einstein radius in (mas).

piSfloat

Amplitude of the parallax (1AU/dS) of the source. (mas)

piE_Efloat

The microlensing parallax in the East direction in units of thetaE

piE_Nfloat

The microlensing parallax in the North direction in units of thetaE

xS0_Efloat

R.A. of source position on sky at t = t0 (arcsec) in an arbitrary ref. frame.

xS0_Nfloat

Dec. of source position on sky at t = t0 (arcsec) in an arbitrary ref. frame.

muS_Efloat

RA Source proper motion (mas/yr)

muS_Nfloat

Dec Source proper motion (mas/yr)

qfloat

Mass ratio (M2 / M1)

sepfloat

Angular separation of the two lenses (mas)

alphafloat

Angle made between the binary axis and North; measured in degrees East of North.

b_sffnumpy array or list

The ratio of the source flux to the total (source + neighbors + lenses). One for each filter.

mag_srcnumpy array or list

Source magnitude, unlensed. One in each filter.

dmag_Lp_Lsnumpy array or list

Magnitude difference of lens primary - lens secondary. If the primary lens is dark, then dmag_Lp_Ls should be set to 20 (or some other large, positive number). If the secondary lens 2 is dark, then it should be set to -20. If they are both dark, then dmag_Lp_Ls=0 and b_sff=1. Note, in astrometric filters, we assume all the excess flux (i.e. 1 - b_sff) comes from the lenses, not any neighbors.

raL: float, optional

Right ascension of the lens in decimal degrees.

decL: float, optional

Declination of the lens in decimal degrees.

obsLocation: str or list[str], optional

The observers location for each photometric dataset (def=[‘earth’])

root_tolfloat

Tolerance in comparing the polynomial roots to the physical solutions. Default = 1e-8

class model.PSBL_PhotAstromParam3(t0, u0_amp, tE, log10_thetaE, piS, piE_E, piE_N, xS0_E, xS0_N, muS_E, muS_N, q, sep, alpha, b_sff, mag_base, dmag_Lp_Ls, raL=None, decL=None, obsLocation='earth', root_tol=1e-08)

Bases: PSPL_Param

Point source binary lens. It has 3 more parameters than PSPL (additional mass term, separation, and angle of approach). Note that this is a STATIC binary lens, i.e. there is no orbital motion.

Attributes:

t0float

Time of projected closest approach between the source and the geometric center of the lens system (before parallax is applied and in the SSB frame).

u0_ampfloat

Angular distance between the source and the GEOMETRIC center of the lenses on the plane of the sky at closest approach in units of thetaE. Can

• positive (u0_amp > 0 when u0_hat[0] > 0) or

• negative (u0_amp < 0 when u0_hat[0] < 0).

tEfloat

Einstein crossing time (days).

log10_thetaEfloat

The size of the Einstein radius in (mas).

piSfloat

Amplitude of the parallax (1AU/dS) of the source. (mas)

piE_Efloat

The microlensing parallax in the East direction in units of thetaE

piE_Nfloat

The microlensing parallax in the North direction in units of thetaE

xS0_Efloat

R.A. of source position on sky at t = t0 (arcsec) in an arbitrary ref. frame.

xS0_Nfloat

Dec. of source position on sky at t = t0 (arcsec) in an arbitrary ref. frame.

muS_Efloat

RA Source proper motion (mas/yr)

muS_Nfloat

Dec Source proper motion (mas/yr)

qfloat

Mass ratio (M2 / M1)

sepfloat

Angular separation of the two lenses (mas)

alphafloat

Angle made between the binary axis and North; measured in degrees East of North.

b_sffnumpy array or list

The ratio of the source flux to the total (source + neighbors + lenses). One for each filter.

\(b_sff = f_S / (f_S + f_L + f_N)\).

This must be passed in as a list or array, with one entry for each photometric filter.

mag_basenumpy array or list

Photometric magnitude of the base. This must be passed in as a list or array, with one entry for each photometric filter.

dmag_Lp_Lsnumpy array or list

Magnitude difference of lens primary - lens secondary. If the primary lens is dark, then dmag_L1_L2 should be set to 20 (or some other large, positive number). If the secondary lens 2 is dark, then it should be set to -20. Note, in astrometric filters, we assume all the excess flux (i.e. 1 - b_sff) comes from the lenses, not any neighbors.

raL: float, optional

Right ascension of the lens in decimal degrees.

decL: float, optional

Declination of the lens in decimal degrees.

obsLocation: str or list[str], optional

The observers location for each photometric dataset (def=[‘earth’])

root_tolfloat

Tolerance in comparing the polynomial roots to the physical solutions. Default = 1e-8

class model.PSBL_PhotAstromParam4(t0_com, u0_amp_com, tE, thetaE, piS, piE_E, piE_N, xS0_E, xS0_N, muS_E, muS_N, q, sep, alpha, b_sff, mag_src, dmag_Lp_Ls, raL=None, decL=None, obsLocation='earth', root_tol=1e-08)

Bases: PSPL_Param

Point source binary lens. It has 3 more parameters than PSPL (additional mass term, separation, and angle of approach). Note that this is a STATIC binary lens, i.e. there is no orbital motion.

Attributes:

t0_comfloat

Time of projected closest approach between the source and the geometric center of the lens system (before parallax is applied and in the SSB frame).

u0_amp_comfloat

Angular distance between the source and the binary lens COM on the plane of the sky at closest approach in units of thetaE. Can be

• positive (u0_amp > 0 when u0_hat[0] > 0) or

• negative (u0_amp < 0 when u0_hat[0] < 0).

tEfloat

Einstein crossing time (days).

thetaEfloat

The size of the Einstein radius in (mas).

piSfloat

Amplitude of the parallax (1AU/dS) of the source. (mas)

piE_Efloat

The microlensing parallax in the East direction in units of thetaE

piE_Nfloat

The microlensing parallax in the North direction in units of thetaE

xS0_Efloat

R.A. of source position on sky at t = t0 (arcsec) in an arbitrary ref. frame.

xS0_Nfloat

Dec. of source position on sky at t = t0 (arcsec) in an arbitrary ref. frame.

muS_Efloat

RA Source proper motion (mas/yr)

muS_Nfloat

Dec Source proper motion (mas/yr)

qfloat

Mass ratio (M2 / M1)

sepfloat

Angular separation of the two lenses (mas)

alphafloat

Angle made between the binary axis and North; measured in degrees East of North.

b_sffnumpy array or list

The ratio of the source flux to the total (source + neighbors + lenses). One for each filter.

\(b_sff = f_S / (f_S + f_L + f_N)\).

This must be passed in as a list or array, with one entry for each photometric filter.

mag_basenumpy array or list

Photometric magnitude of the base. This must be passed in as a list or array, with one entry for each photometric filter.

dmag_Lp_Lsnumpy array or list

Magnitude difference of lens primary - lens secondary. If the primary lens is dark, then dmag_L1_L2 should be set to 20 (or some other large, positive number). If the secondary lens 2 is dark, then it should be set to -20. Note, in astrometric filters, we assume all the excess flux (i.e. 1 - b_sff) comes from the lenses, not any neighbors.

raL: float, optional

Right ascension of the lens in decimal degrees.

decL: float, optional

Declination of the lens in decimal degrees.

obsLocation: str or list[str], optional

The observers location for each photometric dataset (def=[‘earth’])

root_tolfloat

Tolerance in comparing the polynomial roots to the physical solutions. Default = 1e-8

class model.PSBL_PhotAstromParam5(t0_prim, u0_amp_prim, tE, thetaE, piS, piE_E, piEN_piEE, xS0_E, xS0_N, muS_E, muS_N, q, sep, alpha, b_sff, mag_base, dmag_Lp_Ls, raL=None, decL=None, obsLocation='earth', root_tol=1e-08)

Bases: PSPL_Param

Point source binary lens. It has 3 more parameters than PSPL (additional mass term, separation, and angle of approach). Note that this is a STATIC binary lens, i.e. there is no orbital motion.

Attributes:

t0_primfloat

Time of closest approach between source and primary lens (MJD.DDD).

u0_amp_primfloat

Angular distance between the source and the PRIMARY lens on the plane of the sky at closest approach in units of thetaE. Can be

• positive (u0_amp > 0 when u0_hat[0] > 0) or

• negative (u0_amp < 0 when u0_hat[0] < 0).

tEfloat

Einstein crossing time (days).

thetaEfloat

The size of the Einstein radius in (mas).

piSfloat

Amplitude of the parallax (1AU/dS) of the source. (mas)

piE_Efloat

The microlensing parallax in the East direction in units of thetaE

piEN_piEEfloat

The ratio of piE_E / piE_N.

xS0_Efloat

R.A. of source position on sky at t = t0 (arcsec) in an arbitrary ref. frame.

xS0_Nfloat

Dec. of source position on sky at t = t0 (arcsec) in an arbitrary ref. frame.

muS_Efloat

RA Source proper motion (mas/yr)

muS_Nfloat

Dec Source proper motion (mas/yr)

betafloat

Angular distance between the source and the GEOMETRIC center of the lenses on the plane of the sky (mas).

qfloat

Mass ratio (M2 / M1)

sepfloat

Angular separation of the two lenses (mas)

alphafloat

Angle made between the binary axis and North; measured in degrees East of North.

b_sffnumpy array or list

The ratio of the source flux to the total (source + neighbors + lenses). One for each filter.

mag_srcnumpy array or list

Source magnitude, unlensed. One in each filter.

dmag_Lp_Lsnumpy array or list

Magnitude difference of lens primary - lens secondary. If the primary lens is dark, then dmag_L1_L2 should be set to 20 (or some other large, positive number). If the secondary lens 2 is dark, then it should be set to -20. Note, in astrometric filters, we assume all the excess flux (i.e. 1 - b_sff) comes from the lenses, not any neighbors.

raL: float, optional

Right ascension of the lens in decimal degrees.

decL: float, optional

Declination of the lens in decimal degrees.

obsLocation: str or list[str], optional

The observers location for each photometric dataset (def=[‘earth’])

root_tolfloat

Tolerance in comparing the polynomial roots to the physical solutions. Default = 1e-8

class model.PSBL_PhotAstromParam6(t0, u0_amp, tE, thetaE, piS, piE_E, piE_N, xS0_E, xS0_N, muS_E, muS_N, q, sep, alpha, b_sff, mag_src, dmag_Lp_Ls, raL=None, decL=None, obsLocation='earth', root_tol=1e-08)

Bases: PSPL_Param

Point source binary lens. It has 3 more parameters than PSPL (additional mass term, separation, and angle of approach). Note that this is a STATIC binary lens, i.e. there is no orbital motion.

Attributes:

t0_primfloat

Time of projected closest approach between the source and the primary lens (before parallax is applied and in the SSB frame).

u0_amp_primfloat

Angular distance between the source and the PRIMARY lens on the plane of the sky at closest approach in units of thetaE. Can be

• positive (u0_amp > 0 when u0_hat[0] > 0) or

• negative (u0_amp < 0 when u0_hat[0] < 0).

tEfloat

Einstein crossing time (days).

thetaEfloat

The size of the Einstein radius in (mas).

piSfloat

Amplitude of the parallax (1AU/dS) of the source. (mas)

piE_Efloat

The microlensing parallax in the East direction in units of thetaE

piE_Nfloat

The microlensing parallax in the North direction in units of thetaE

xS0_Efloat

R.A. of source position on sky at t = t0 (arcsec) in an arbitrary ref. frame.

xS0_Nfloat

Dec. of source position on sky at t = t0 (arcsec) in an arbitrary ref. frame.

muS_Efloat

RA Source proper motion (mas/yr)

muS_Nfloat

Dec Source proper motion (mas/yr)

betafloat

Angular distance between the source and the GEOMETRIC center of the lenses on the plane of the sky (mas).

qfloat

Mass ratio (M2 / M1)

sepfloat

Angular separation of the two lenses (mas)

alphafloat

Angle made between the binary axis and North; measured in degrees East of North.

b_sffnumpy array or list

The ratio of the source flux to the total (source + neighbors + lenses). One for each filter.

mag_srcnumpy array or list

Source magnitude, unlensed. One in each filter.

dmag_Lp_Lsnumpy array or list

Magnitude difference of lens primary - lens secondary. If the primary lens is dark, then dmag_L1_L2 should be set to 20 (or some other large, positive number). If the secondary lens 2 is dark, then it should be set to -20. Note, in astrometric filters, we assume all the excess flux (i.e. 1 - b_sff) comes from the lenses, not any neighbors.

raL: float, optional

Right ascension of the lens in decimal degrees.

decL: float, optional

Declination of the lens in decimal degrees.

obsLocation: str or list[str], optional

The observers location for each photometric dataset (def=[‘earth’])

root_tolfloat

Tolerance in comparing the polynomial roots to the physical solutions. Default = 1e-8

class model.PSBL_PhotParam1(t0, u0_amp, tE, piE_E, piE_N, q, sep, phi, b_sff, mag_src, raL=None, decL=None, obsLocation='earth', root_tol=1e-08)

Bases: PSPL_Param

Point source binary lens, photometry only.

It has 3 more parameters than PSPL_PhotParam1:

• mass ratio

• separation – in units of thetaE

• angle of approach

Note that this is a STATIC binary lens, i.e. there is no orbital motion.

Attributes:

t0: float

Time (MJD.DDD) of closest projected approach between source and lens as seen in Solar System barycentric coordinates. This should be close, but not exactly aligned with the photometric peak, as seen from Earth or a Solar System satellite.

u0_amp: float

Angular distance between the lens and source on the plane of the sky at closest approach in units of thetaE. It can be

• positive (u0_amp > 0 when u0_hat[0] > 0) or

• negative (u0_amp < 0 when u0_hat[0] < 0).

tE: float

Einstein crossing time based on the system mass. [MJD]

piE_E: float

The microlensing parallax in the East direction in units of thetaE

piE_N: float

The microlensing parallax in the North direction in units of thetaE

q: float

Mass ratio (low-mass / high-mass)

sep: float

Angular separation of the two lenses in units of thetaE where thetaE is defined with the total binary mass.

phi: float

Angle made between the binary axis and the relative proper motion vector, measured in degrees.

b_sff: array or list

The ratio of the source flux to the total (source + neighbors + lens) \(b_sff = f_S / (f_S + f_L + f_N)\). This must be passed in as a list or array, with one entry for each photometric filter.

mag_src: array or list

Photometric magnitude of the source. This must be passed in as a list or array, with one entry for each photometric filter.

raL: float, optional

Right ascension of the lens in decimal degrees.

decL: float, optional

Declination of the lens in decimal degrees.

obsLocation: str or list[str], optional

The observers location for each photometric dataset (def=[‘earth’])

root_tolfloat

Tolerance in comparing the polynomial roots to the physical solutions. Default = 1e-8

class model.PSBL_GP_PhotParam1(t0, u0_amp, tE, piE_E, piE_N, q, sep, phi, b_sff, mag_src, gp_log_sigma, gp_log_rho, gp_log_S0, gp_log_omega0, raL=None, decL=None, obsLocation='earth', root_tol=1e-08)

Bases: PSBL_PhotParam1

class model.PSBL_GP_PhotAstromParam1(mLp, mLs, t0, xS0_E, xS0_N, beta, muL_E, muL_N, muS_E, muS_N, dL, dS, sep, alpha, b_sff, mag_src, dmag_Lp_Ls, gp_log_sigma, gp_log_rho, gp_log_S0, gp_log_omega0, raL=None, decL=None, obsLocation='earth', root_tol=1e-08)

Bases: PSBL_PhotAstromParam1

class model.PSBL_GP_PhotAstromParam2(t0, u0_amp, tE, thetaE, piS, piE_E, piE_N, xS0_E, xS0_N, muS_E, muS_N, q, sep, alpha, b_sff, mag_src, dmag_Lp_Ls, gp_log_sigma, gp_log_rho, gp_log_S0, gp_log_omega0, raL=None, decL=None, obsLocation='earth', root_tol=1e-08)

Bases: PSBL_PhotAstromParam2