Parameterization Class Family
- class model.BSBL_PhotParam1(t0, u0_amp, tE, piE_E, piE_N, sep_SL, sep_S, phi_S, sep_L, phi_L, mag_src_pri, mag_src_sec, b_sff, dmag_Lp_Ls, raL=None, decL=None, obsLocation='earth')
Bases:
PSPL_ParamBSBL model for photometry only
A Binary point Source Binary Lens model for microlensing.
Note the attributes, RA (raL) and Dec (decL) are required if you are calculating a model with parallax.
- Attributes:
- t0: float
Time of photometric peak, as seen from Earth (MJD.DDD)
- 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).
Note, since this is a binary source, we are expressing the nominal source position as that of the primary star in the source binary system.
- tE: float
Einstein crossing time based on the lens 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 of the lens binary (low-mass / high-mass)
- sep_SL: float
Angular separation of the source system position (defined as position of primary) from the lens system geometric center (in units of thetaE).
- sepS: float
Angular separation between the two sources in units of thetaE where thetaE is defined with the total binary lens mass.
- phiS: float
Angle made between the binary source axis and the relative proper motion vector, measured in degrees.
- sepL: float
Angular separation between the two lenses in units of theteaE where thetaE is defined with the total binary lens mass.
- phiL: float
Angle made between the binary lens axis and the relative proper motion vector, measured in degrees.
- mag_src_pri: array or list
Photometric magnitude of the first (primary) source. This must be passed in as a list or array, with one entry for each photometric filter.
- mag_src_sec: array or list
Photometric magnitude of the second (secondary) source. This must be passed in as a list or array, with one entry for each photometric filter.
- b_sff: array or list
The ratio of the source flux to the total (source + neighbors + lens) \(b_sff = (f_S1 + f_S2) / (f_S1 + f_s2 + f_L1 + f_L2 + f_N)\). 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’]) such as ‘jwst’ or ‘spitzer’. Can be a single string if all observer locations are identical. Otherwise, array of same length as mag_src or b_sff (e.g. other photometric parameters).
- class model.BSBL_PhotAstromParam1(mLp, mLs, t0, xS0_E, xS0_N, beta, muL_E, muL_N, muS_E, muS_N, dL, dS, sepL, alphaL, sepS, alphaS, mag_src_pri, mag_src_sec, b_sff, dmag_Lp_Ls, raL=None, decL=None, obsLocation='earth', root_tol=1e-08)
Bases:
PSPL_ParamBSBL model for astrometry and photometry - physical parameterization.
A binary source binary lens model for microlensing. This model uses a parameterization that depends on only physical quantities such as the lens masses and positions and proper motions. 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 closest approach between the geometric center of source and geometric center of the lens, as seen from Earth (MJD.DDD)
- xS0_Efloat
R.A. of source primary position on sky at t = t0 (arcsec) in an arbitrary ref. frame.
- xS0_Nfloat
Dec. of source primary position on sky at t = t0 (arcsec) in an arbitrary ref. frame.
- beta: float
Angular distance between the source PRIMARY position 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 system proper motion in the RA direction (mas/yr)
- muS_Nfloat
Source system 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)
- sepLfloat
Angular separation of the lens secondary from the lens primary (mas).
- alphaLfloat
Angle made between the binary lens axis and North; measured in degrees East of North. Example, alphaL = 90 will place the lens primary to the East and the lens secondary to the West.
- sepSfloat
Angular separation of the source secondary from the source primary (mas).
- alphaSfloat
Angle made between the binary source axis and North; measured in degrees East of North. Example, alphaL = 90 will place the source primary to the East and the source secondary to the West.
- mag_src_pri: array or list
Photometric magnitude of the first (primary) source. This must be passed in as a list or array, with one entry for each photometric filter.
- mag_src_sec: array or list
Photometric magnitude of the second (secondary) source. This must be passed in as a list or array, with one entry for each photometric filter.
- b_sffnumpy array or list
The ratio of the combined source flux to the total (sources + neighbors + lenses). One for 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’]) such as ‘jwst’ or ‘spitzer’. Can be a single string if all observer locations are identical. Otherwise, array of same length as mag_src or b_sff (e.g. other photometric parameters).
- root_tolfloat
Tolerance in comparing the polynomial roots to the physical solutions. Default = 1e-8
- class model.BSBL_PhotAstromParam2(mLp, mLs, t0_p, xS0_E, xS0_N, beta_p, muL_E, muL_N, muS_E, muS_N, dL, dS, sepL, alphaL, sepS, alphaS, mag_src_pri, mag_src_sec, b_sff, dmag_Lp_Ls, raL=None, decL=None, obsLocation='earth', root_tol=1e-08)
Bases:
PSPL_ParamBSBL model for astrometry and photometry - physical parameterization with primary lens and primary source center.
A binary source binary lens model for microlensing. This model uses a parameterization that depends on only physical quantities such as the lens masses and positions and proper motions. Note that this is a STATIC binary lens, i.e. there is no orbital motion.
- Attributes:
- mLp, mLsfloat
Masses of the lenses (Msun)
- t0_pfloat
Time of closest approach between source and PRIMARY LENS (MJD.DDD)
- xS0_Efloat
R.A. of source primary position on sky at t = t0 (arcsec) in an arbitrary ref. frame.
- xS0_Nfloat
Dec. of source primary position on sky at t = t0 (arcsec) in an arbitrary ref. frame.
- beta_pfloat
Angular distance between the source PRIMARY position and the PRIMARY 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 system proper motion in the RA direction (mas/yr)
- muS_Nfloat
Source system 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)
- sepLfloat
Angular separation of the lens secondary from the lens primary (mas).
- alphaLfloat
Angle made between the binary lens axis and North; measured in degrees East of North. Example, alphaL = 90 will place the lens primary to the East and the lens secondary to the West.
- sepSfloat
Angular separation of the source secondary from the source primary (mas).
- alphaSfloat
Angle made between the binary source axis and North; measured in degrees East of North. Example, alphaL = 90 will place the source primary to the East and the source secondary to the West.
- mag_src_pri: array or list
Photometric magnitude of the first (primary) source. This must be passed in as a list or array, with one entry for each photometric filter.
- mag_src_sec: array or list
Photometric magnitude of the second (secondary) source. This must be passed in as a list or array, with one entry for each photometric filter.
- b_sffnumpy array or list
The ratio of the combined source flux to the total (sources + neighbors + lenses). One for 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.
- root_tolfloat
Tolerance in comparing the polynomial roots to the physical solutions. Default = 1e-8
- 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’]) such as ‘jwst’ or ‘spitzer’. Can be a single string if all observer locations are identical. Otherwise, array of same length as mag_src or b_sff (e.g. other photometric parameters).
- class model.BSBL_PhotAstrom_CircOrbs_Param1(mLp, mLs, t0_com, xS0_E, xS0_N, beta, muL_E, muL_N, muS_E, muS_N, dL, dS, omegaL_pri, big_omegaL_sec, iL, tpL, sepL, omegaS_pri, big_omegaS_sec, iS, pS, tpS, alephS, aleph_secS, mag_src_pri, mag_src_sec, b_sff, dmag_Lp_Ls, raL=None, decL=None, obsLocation='earth', root_tol=1e-08)
Bases:
BSBL_PhotAstrom_EllOrbs_Param1BSBL model for astrometry and photometry - physical parameterization.
A binary source binary lens model for microlensing. This model uses a parameterization that depends on only physical quantities such as the lens masses and positions and proper motions.
Note that this is a non-STATIC binary lens, i.e. there is no orbital motion.
- Attributes:
- mLp, mLsfloat
Masses of the lenses (Msun)
- t0_comfloat
Time of closest approach between source COM and Lens COM (MJD.DDD)
- xS0_Efloat
R.A. of source COM position on sky at t = t0 (arcsec) in an arbitrary ref. frame.
- xS0_Nfloat
Dec. of source COM position on sky at t = t0 (arcsec) in an arbitrary ref. frame.
- beta: float
Angular distance between the source PRIMARY position 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 system proper motion in the RA direction (mas/yr)
- muS_Nfloat
Source system 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)
- omegaL_pri: float
The argument of periastron of the primary lens’s orbit in degrees.
- big_omegaL_sec: float
The longitude of the ascending node of the secondary lens’s orbit in degrees.
- iL: float
Inclination angle of the system in degrees.
- tpL: float
This is the time of the periastron of the system in days.
- sepL: float
This is the angular separation between the lenses (mas)
- omegaS_pri: float
The argument of periastron of the primary source’s orbit in degrees.
- big_omegaS_sec: float
The longitude of the ascending node of the secondary source’s orbit in degrees.
- is: float
Inclination angle of the system in degrees.
- pS: float
Orbital period of the system in days.
- tpS: float
This is the time of the periastron of the system in days.
- alephS: float
This is the semi-major axis of the primary source in mas.
- aleph_secS: float
This is the semi-major axis of the secondary source in mas.
- mag_src_pri: array or list
Photometric magnitude of the first (primary) source. This must be passed in as a list or array, with one entry for each photometric filter.
- mag_src_sec: array or list
Photometric magnitude of the second (secondary) source. This must be passed in as a list or array, with one entry for each photometric filter.
- b_sffnumpy array or list
The ratio of the combined source flux to the total (sources + neighbors + lenses). One for 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.BSBL_PhotAstrom_CircOrbs_Param2(t0_com, u0_amp_com, tE, thetaE, piS, piE_E, piE_N, q, xS0_E, xS0_N, muS_E, muS_N, omegaL_pri, big_omegaL_sec, iL, tpL, sepL, omegaS_pri, big_omegaS_sec, iS, pS, tpS, alephS, aleph_secS, fratio_bin, mag_base, b_sff, dmag_Lp_Ls, raL=None, decL=None, obsLocation='earth', root_tol=1e-08)
Bases:
BSBL_PhotAstrom_EllOrbs_Param2BSBL model for astrometry and photometry - physical parameterization.
A binary source binary lens model for microlensing. This model uses a parameterization that depends on only physical quantities such as the lens masses and positions and proper motions.
Note that this is a non-STATIC binary lens, i.e. there is no orbital motion.
- Attributes:
- t0_comfloat
Time of closest approach between the primary source and lens COM (MJD.DDD)
- u0_amp_com: float
Angular distance between the primary source and the binary lens center of mass 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
- qfloat
Mass ratio (M2 / M1)
- xS0_Efloat
R.A. of primary source position on sky at t = t0_com (arcsec) in an arbitrary ref. frame.
- xS0_Nfloat
Dec. of primary source position on sky at t = to_com (arcsec) in an arbitrary ref. frame.
- muS_Efloat
Source system proper motion in the RA direction (mas/yr)
- muS_Nfloat
Source system proper motion in the Dec. direction (mas/yr)
- omegaL_pri: float
The argument of periastron of the primary lens’s orbit in degrees.
- big_omegaL_sec: float
The longitude of the ascending node of the secondary lens’s orbit in degrees.
- iL: float
Inclination angle of the system in degrees.
- tpL: float
This is the time of the periastron of the system in days.
- sepL: float
This is the angular separation between the lenses (mas)
- omegaS_pri: float
The argument of periastron of the primary source’s orbit in degrees.
- big_omegaS_sec: float
The longitude of the ascending node of the secondary source’s orbit in degrees.
- is: float
Inclination angle of the system in degrees.
- pS: float
Orbital period of the system in days.
- tpS: float
This is the time of the periastron of the system in days.
- alephS: float
This is the semi-major axis of the primary source in mas.
- aleph_secS: float
This is the semi-major axis of the secondary source in mas.
- fratio_bin: float
Flux ratio of secondary flux / primary flux.
- mag_basearray or list
Photometric magnitude of the base. This must be passed in as a list or array, with one entry for each photometric filter. Note that \(flux_{base} = f_{src1} + f_{src2} + f_{blend}\) such that \(b_sff = (f_{src1}+ f_{src2}) / ( f_{src1} + f_{src2} + f_{blend} )\)
- b_sff: array or list
The ratio of the source flux to the total (source + neighbors + lens):math:b_sff = (f_{S1} + f_{S2}) / (f_{S1} + f_{s2} + f_L + f_N). 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.BSBL_PhotAstrom_EllOrbs_Param1(mLp, mLs, t0_com, xS0_E, xS0_N, beta, muL_E, muL_N, muS_E, muS_N, dL, dS, omegaL_pri, big_omegaL_sec, iL, eL, tpL, aL, omegaS_pri, big_omegaS_sec, iS, eS, pS, tpS, alephS, aleph_secS, mag_src_pri, mag_src_sec, b_sff, dmag_Lp_Ls, raL=None, decL=None, obsLocation='earth', root_tol=1e-08)
Bases:
PSPL_ParamBSBL model for astrometry and photometry - physical parameterization.
A binary source binary lens model for microlensing. This model uses a parameterization that depends on only physical quantities such as the lens masses and positions and proper motions.
Note that this is a non-STATIC binary lens, i.e. there is no orbital motion.
- Attributes:
- mLp, mLsfloat
Masses of the lenses (Msun)
- t0_comfloat
Time of closest approach between source COM and Lens COM (MJD.DDD)
- xS0_Efloat
R.A. of source COM position on sky at t = t0 (arcsec) in an arbitrary ref. frame.
- xS0_Nfloat
Dec. of source COM position on sky at t = t0 (arcsec) in an arbitrary ref. frame.
- beta: float
Angular distance between the primary source and the lens geometric center 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 system proper motion in the RA direction (mas/yr)
- muS_Nfloat
Source system 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)
- omegaL_pri: float
The argument of periastron of the primary lens’s orbit in degrees.
- big_omegaL_sec: float
The longitude of the ascending node of the secondary lens’s orbit in degrees.
- iL: float
Inclination angle of the system in degrees.
- eL: float
Eccentricity of the Lens System
- tpL: float
This is the time of the periastron of the system in days.
- aL: float
This is the semi-major axis of the binary lens system (mas)
- omegaS_pri: float
The argument of periastron of the primary source’s orbit in degrees.
- big_omegaS_sec: float
The longitude of the ascending node of the secondary source’s orbit in degrees.
- is: float
Inclination angle of the system in degrees.
- eS: float
Eccentricity of the Source System
- pS: float
Orbital period of the system in days.
- tpS: float
This is the time of the periastron of the system in days.
- alephS: float
This is the semi-major axis of the primary source in mas.
- aleph_secS: float
This is the semi-major axis of the secondary source in mas.
- mag_src_pri: array or list
Photometric magnitude of the first (primary) source. This must be passed in as a list or array, with one entry for each photometric filter.
- mag_src_sec: array or list
Photometric magnitude of the second (secondary) source. This must be passed in as a list or array, with one entry for each photometric filter.
- b_sffnumpy array or list
The ratio of the combined source flux to the total (sources + neighbors + lenses). One for 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.BSBL_PhotAstrom_EllOrbs_Param2(t0_com, u0_amp_com, tE, thetaE, piS, piE_E, piE_N, q, xS0_E, xS0_N, muS_E, muS_N, omegaL_pri, big_omegaL_sec, iL, eL, tpL, aL, omegaS_pri, big_omegaS_sec, iS, eS, pS, tpS, alephS, aleph_secS, fratio_bin, mag_base, b_sff, dmag_Lp_Ls, raL=None, decL=None, obsLocation='earth', root_tol=1e-08)
Bases:
PSPL_ParamBSBL model for astrometry and photometry - physical parameterization.
A binary source binary lens model for microlensing. This model uses a parameterization that depends on only physical quantities such as the lens masses and positions and proper motions.
Note that this is a non-STATIC binary lens, i.e. there is no orbital motion.
- Attributes:
- t0_comfloat
Time of closest approach between the primary source and lens COM (MJD.DDD)
- u0_amp_com: float
Angular distance between the primary source and the binary lens center of mass 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
- qfloat
Mass ratio (M2 / M1)
- xS0_Efloat
R.A. of primary source position on sky at t = t0_com (arcsec) in an arbitrary ref. frame.
- xS0_Nfloat
Dec. of primary source position on sky at t = to_com (arcsec) in an arbitrary ref. frame.
- muS_Efloat
Source system proper motion in the RA direction (mas/yr)
- muS_Nfloat
Source system proper motion in the Dec. direction (mas/yr)
- omegaL_pri: float
The argument of periastron of the primary lens’s orbit in degrees.
- big_omegaL_sec: float
The longitude of the ascending node of the secondary lens’s orbit in degrees.
- iL: float
Inclination angle of the system in degrees.
- eL: float
Eccentricity of the Lens System
- tpL: float
This is the time of the periastron of the system in days.
- aL: float
This is the semi-major axis of the binary lens system (mas)
- omegaS_pri: float
The argument of periastron of the primary source’s orbit in degrees.
- big_omegaS_sec: float
The longitude of the ascending node of the secondary source’s orbit in degrees.
- is: float
Inclination angle of the system in degrees.
- eS: float
Eccentricity of the Source System
- pS: float
Orbital period of the system in days.
- tpS: float
This is the time of the periastron of the system in days.
- alephS: float
This is the semi-major axis of the primary source in mas.
- aleph_secS: float
This is the semi-major axis of the secondary source in mas.
- fratio_bin: float
Flux ratio of secondary flux / primary flux.
- mag_basearray or list
Photometric magnitude of the base. This must be passed in as a list or array, with one entry for each photometric filter. Note that \(flux_{base} = f_{src1} + f_{src2} + f_{blend}\) such that \(b_sff = (f_{src1}+ f_{src2}) / ( f_{src1} + f_{src2} + f_{blend} )\)
- b_sffarray or list
The ratio of the source flux to the total (source + neighbors + lens):math:b_sff = (f_{S1} + f_{S2}) / (f_{S1} + f_{s2} + f_L + f_N). 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