Parameterization Class Family - BSPL
BSPL Models
- class model.BSPL_PhotParam1(t0, u0_amp, tE, piE_E, piE_N, sep, phi, mag_src_pri, mag_src_sec, b_sff, raL=None, decL=None)
Bases:
PSPL_ParamBSPL model for photometry only
A Binary point Source Point 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. [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
- sep: float
Angular separation of the source scondary from the source primary (in units of thetaE).
- phi: float
Angle made between the binary 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) \(b_sff = (f_S1 + f_S2) / (f_S1 + f_s2 + f_L + f_N)\). 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.
- class model.BSPL_PhotAstromParam1(mL, t0, beta, dL, dL_dS, xS0_E, xS0_N, muL_E, muL_N, muS_E, muS_N, sep, alpha, mag_src_pri, mag_src_sec, b_sff, raL=None, decL=None)
Bases:
PSPL_ParamBSPL model for astrometry and photometry - physical parameterization.
A Binary point Source Point Lens model for microlensing. This model uses a parameterization that depends on only physical quantities such as the lens mass and positions and proper motions of both the lens and source.
Note the attributes, RA (raL) and Dec (decL) are required if you are calculating a model with parallax.
- Attributes
- mL: float
Mass of the lens (Msun)
- t0: float
Time of photometric peak, as seen from Earth (MJD.DDD)
- beta: float
Angular distance between the lens and primary source 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).
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.
- dL: float
Distance from the observer to the lens (pc)
- dL_dS: float
Ratio of Distance from the obersver to the lens to Distance from the observer to the source
- xS0_E: float
RA Source position on sky at t = t0 (arcsec) in an arbitrary ref. frame. This should be the position of the source primary.
- xS0_N: float
Dec source position on sky at t = t0 (arcsec) in an arbitrary ref. frame. This should be the position of the source primary.
- muL_E: float
RA Lens proper motion (mas/yr)
- muL_N: float
Dec Lens proper motion (mas/yr)
- muS_E: float
RA Source proper motion (mas/yr) Identical proper motions are assumed for the source primary and secondary.
- muS_N: float
Dec Source proper motion (mas/yr) Identical proper motions are assumed for the source primary and secondary.
- sep: float
Angular separation of the source scondary from the source primary (mas).
- alpha: float
Angle made between the binary source axis and North; measured in degrees East of North.
- 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) \(b_sff = (f_S1 + f_S2) / (f_S1 + f_s2 + f_L + f_N)\). 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.
- class model.BSPL_PhotAstromParam2(t0, u0_amp, tE, thetaE, piS, piE_E, piE_N, xS0_E, xS0_N, muS_E, muS_N, sep, alpha, fratio_bin, mag_base, b_sff, raL=None, decL=None)
Bases:
PSPL_ParamBSPL model for astrometry and photometry - physical parameterization.
A Binary point Source Point Lens model for microlensing. This model uses a parameterization that depends on only physical quantities such as the lens mass and positions and proper motions of both the lens and source.
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_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).
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.
- 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. This should be the position of the source primary.
- 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) Identical proper motions are assumed for the source primary and secondary.
- muS_Nfloat
Dec Source proper motion (mas/yr) Identical proper motions are assumed for the source primary and secondary.
- sep: float
Angular separation of the source scondary from the source primary (mas).
- alpha: float
Angle made between the binary source axis and North; measured in degrees East of North.
- 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) \(b_sff = (f_{S1} + f_{S2}) / (f_{S1} + f_{s2} + f_L + f_N)\). This must be passed in as a list or array, with one entry for each photometric filter.
- raL: float, optional
Right ascension of the lens in decimal degrees.
- decL: float, optional
Declination of the lens in decimal degrees.
- class model.BSPL_PhotAstromParam3(t0, u0_amp, tE, log10_thetaE, piS, piE_E, piE_N, xS0_E, xS0_N, muS_E, muS_N, sep, alpha, fratio_bin, mag_base, b_sff, raL=None, decL=None)
Bases:
PSPL_ParamBSPL model for astrometry and photometry - physical parameterization.
A Binary point Source Point Lens model for microlensing. This model uses a parameterization that depends on only physical quantities such as the lens mass and positions and proper motions of both the lens and source.
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_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).
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.
- 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. This should be the position of the source primary.
- 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) Identical proper motions are assumed for the source primary and secondary.
- muS_Nfloat
Dec Source proper motion (mas/yr) Identical proper motions are assumed for the source primary and secondary.
- sep: float
Angular separation of the source scondary from the source primary (mas).
- alpha: float
Angle made between the binary source axis and North; measured in degrees East of North.
- 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) \(b_sff = (f_{S1} + f_{S2}) / (f_{S1} + f_{s2} + f_L + f_N)\). This must be passed in as a list or array, with one entry for each photometric filter.
- raL: float, optional
Right ascension of the lens in decimal degrees.
- decL: float, optional
Declination of the lens in decimal degrees.
GP Models
- class model.BSPL_GP_PhotParam1(t0, u0_amp, tE, piE_E, piE_N, sep, phi, mag_src_pri, mag_src_sec, b_sff, gp_log_sigma, gp_rho, gp_log_omega04_S0, gp_log_omega0, raL=None, decL=None)
Bases:
BSPL_PhotParam1BSPL model for photometry only, with GP.
A Binary point Source Point Lens model for microlensing.
Note the attributes, RA (raL) and Dec (decL) are required if you are calculating a model with parallax.
- Parameters
- 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. [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
- sep: float
Angular separation of the source scondary from the source primary (in units of thetaE).
- phi: float
Angle made between the binary 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) \(b_sff = (f_{S1} + f_{S2}) / (f_{S1} + f_{s2} + f_L + f_N).\) This must be passed in as a list or array, with one entry for each photometric filter.
- gp_log_sigma: float
Guassian process \(log(\sigma)\) for the Matern 3/2 kernel.
- gp_rho: float
Guassian process \({\rho}\) for the Matern 3/2 kernel.
- gp_log_omega04_S0: float
Guassian process \(log(\omega_0^4 * S_0)\) from the SHO kernel.
- gp_log_omega0: float
Guassian process \(log(\omega_0)\) from the SHO kernel.
- raL: float, optional
Right ascension of the lens in decimal degrees.
- decL: float, optional
Declination of the lens in decimal degrees.
- class model.BSPL_GP_PhotAstromParam1(mL, t0, beta, dL, dL_dS, xS0_E, xS0_N, muL_E, muL_N, muS_E, muS_N, sep, alpha, mag_src_pri, mag_src_sec, b_sff, gp_log_sigma, gp_rho, gp_log_omega04_S0, gp_log_omega0, raL=None, decL=None)
Bases:
BSPL_PhotAstromParam1BSPL model for astrometry and photometry with GP - physical parameterization.
A Binary point Source Point Lens model for microlensing. This model uses a parameterization that depends on only physical quantities such as the lens mass and positions and proper motions of both the lens and source.
Note the attributes, RA (raL) and Dec (decL) are required if you are calculating a model with parallax.
- Attributes
- mL: float
Mass of the lens (Msun)
- t0: float
Time of photometric peak, as seen from Earth (MJD.DDD)
- beta: float
Angular distance between the lens and primary source 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).
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.
- dL: float
Distance from the observer to the lens (pc)
- dL_dS: float
Ratio of Distance from the obersver to the lens to Distance from the observer to the source
- xS0_E: float
RA Source position on sky at t = t0 (arcsec) in an arbitrary ref. frame. This should be the position of the source primary.
- xS0_N: float
Dec source position on sky at t = t0 (arcsec) in an arbitrary ref. frame. This should be the position of the source primary.
- muL_E: float
RA Lens proper motion (mas/yr)
- muL_N: float
Dec Lens proper motion (mas/yr)
- muS_E: float
RA Source proper motion (mas/yr) Identical proper motions are assumed for the source primary and secondary.
- muS_N: float
Dec Source proper motion (mas/yr) Identical proper motions are assumed for the source primary and secondary.
- sep: float
Angular separation of the source scondary from the source primary (mas).
- alpha: float
Angle made between the binary source axis and North; measured in degrees East of North.
- 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) \(b_sff = (f_{S1} + f_{S2}) / (f_{S1} + f_{s2} + f_L + f_N)\). This must be passed in as a list or array, with one entry for each photometric filter.
- gp_log_sigma: float
Guassian process \(log(\sigma)\) for the Matern 3/2 kernel.
- gp_rho: float
Guassian process \({\rho}\) for the Matern 3/2 kernel.
- gp_log_omega04_S0: float
Guassian process \(log(\omega_0^4 * S_0)\) from the SHO kernel.
- gp_log_omega0: float
Guassian process \(log(\omega_0)\) from the SHO kernel.
- raL: float, optional
Right ascension of the lens in decimal degrees.
- decL: float, optional
Declination of the lens in decimal degrees.
- class model.BSPL_GP_PhotAstromParam2(t0, u0_amp, tE, thetaE, piS, piE_E, piE_N, xS0_E, xS0_N, muS_E, muS_N, sep, alpha, fratio_bin, mag_base, b_sff, gp_log_sigma, gp_rho, gp_log_omega04_S0, gp_log_omega0, raL=None, decL=None)
Bases:
BSPL_PhotAstromParam2BSPL model for astrometry and photometry with GP - physical parameterization.
A Binary point Source Point Lens model for microlensing. This model uses a parameterization that depends on only physical quantities such as the lens mass and positions and proper motions of both the lens and source.
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_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).
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.
- 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. This should be the position of the source primary.
- 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) Identical proper motions are assumed for the source primary and secondary.
- muS_Nfloat
Dec Source proper motion (mas/yr) Identical proper motions are assumed for the source primary and secondary.
- sep: float
Angular separation of the source scondary from the source primary (mas).
- alpha: float
Angle made between the binary source axis and North; measured in degrees East of North.
- 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.
- gp_log_sigma: float
Guassian process \(log(\sigma)\) for the Matern 3/2 kernel.
- gp_rho: float
Guassian process \({\rho}\) for the Matern 3/2 kernel.
- gp_log_omega04_S0: float
Guassian process \(log(\omega_0^4 * S_0)\) from the SHO kernel.
- gp_log_omega0: float
Guassian process \(log(\omega_0)\) from the SHO kernel.
- raL: float, optional
Right ascension of the lens in decimal degrees.
- decL: float, optional
Declination of the lens in decimal degrees.
- class model.BSPL_GP_PhotAstromParam3(t0, u0_amp, tE, log10_thetaE, piS, piE_E, piE_N, xS0_E, xS0_N, muS_E, muS_N, sep, alpha, fratio_bin, mag_base, b_sff, gp_log_sigma, gp_rho, gp_log_omega04_S0, gp_log_omega0, raL=None, decL=None)
Bases:
BSPL_PhotAstromParam3Point Source Point Lens with GP model for microlensing. This model includes proper motions of the source and the source position on the sky. It is the same as PSPL_PhotAstromParam4 except it fits for log10(thetaE) instead of thetaE.
- 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. 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 (days).
- log10_thetaE: float
log10 of the size of the Einstein radius in (mas).
- piS: float
Amplitude of the parallax (1AU/dS) of the source. (mas)
- 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
- xS0_E: float
RA Source position on sky at t = t0 (arcsec) in an arbitrary ref. frame.
- xS0_N: float
Dec source position on sky at t = t0 (arcsec) in an arbitrary ref. frame.
- muS_E: float
RA Source proper motion (mas/yr)
- muS_N: float
Dec Source proper motion (mas/yr)
- sep: float
Angular separation of the source scondary from the source primary (mas).
- alpha: float
Angle made between the binary source axis and North; measured in degrees East of North.
- 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.
- gp_log_sigma: float
Guassian process \(log(\sigma)\) for the Matern 3/2 kernel.
- gp_rho: float
Guassian process \({\rho}\) for the Matern 3/2 kernel.
- gp_log_omega04_S0: float
Guassian process \(log(\omega_0^4 * S_0)\) from the SHO kernel.
- gp_log_omega0: float
Guassian process \(log(\omega_0)\) from the SHO kernel.