synthesizer.emission_models.stellar.pacman_model¶

A module defining the Pacman emission models.

This module defines the PacmanEmission and BimodalPacmanEmission classes which are used to define the emission models for the Pacman model. Both these models combine various differen spectra together to produce a final total emission spectrum.

The PacmanEmission model is used to define the emission model for a single population of stars. Including both intrinsic and attenuate emission, and if a dust emission model is given also dust emission. It includes the option to include escaped emission for a given escape fraction, and if a lyman alpha escape fraction is given, a more sophisticated nebular emission model is used, including line and nebuluar continuum emission.

The BimodalPacmanEmission model is similar to the PacmanEmission model but splits the emission into a young and old population.

The Charlot & Fall (2000) model if a special of the BimodalPacmanEmission model and is also included. This model is identical to the BimodalPacmanEmission model but with a fixed age pivot of 10^7 Myr and no escaped emission.

Example:

To create a PacmanEmission model for a grid with a V-band optical depth of
0.1 and a dust curve, one would do the following:

dust_curve = PowerLaw(...)
model = PacmanEmission(grid, 0.1, dust_curve)

To create a CharlotFall2000 model, you can use the following code:

tau_v_ism = 0.33
tau_v_birth = 0.67
dust_curve_ism = PowerLaw(...)
dust_curve_birth = PowerLaw(...)
age_pivot = 7 * dimensionless
dust_emission_ism = BlackBody(...)
dust_emission_birth = GreyBody(...)
model = CharlotFall2000(
    grid,
    tau_v_ism,
    tau_v_birth,
    dust_curve_ism,
    dust_curve_birth,
    age_pivot,
    dust_emission_ism,
    dust_emission_birth,
)

Classes

class synthesizer.emission_models.stellar.pacman_model.BimodalPacmanEmission(grid, tau_v_ism='tau_v_ism', tau_v_birth='tau_v_birth', dust_curve_ism=<synthesizer.emission_models.transformers.dust_attenuation.Calzetti2000 object>, dust_curve_birth=<synthesizer.emission_models.transformers.dust_attenuation.Calzetti2000 object>, age_pivot=unyt_quantity(7, 'dimensionless'), dust_emission_ism=None, dust_emission_birth=None, fesc='fesc', fesc_ly_alpha='fesc_ly_alpha', label=None, stellar_dust=True, **kwargs)[source]¶

A class defining the Bimodal Pacman model.

This model defines both intrinsic and attenuated stellar emission with or without dust emission. It also includes the option to include escaped emission for a given escape fraction. If a lyman alpha escape fraction is given, a more sophisticated nebular emission model is used, including line and nebular continuum emission.

All spectra produced have a young, old and combined component. The split between young and old is by default 10 ^ 7 Myr but can be changed with the age_pivot argument.

This model will always produce:

young_incident: the stellar emission incident onto the ISM for the
young population.
old_incident: the stellar emission incident onto the ISM for the old
population.
incident: the stellar emission incident onto the ISM for the
combined population.
young_attenuated_nebular: the nebular emission attenuated by dust
for the young population.
young_attenuated_ism: the intrinsic emission attenuated by dust for
the young population.
young_attenuated: the intrinsic emission attenuated by dust for the
young population.
old_attenuated: the intrinsic emission attenuated by dust for the old
population.
young_transmitted: the stellar emission transmitted through the ISM
for the young population.
old_transmitted: the stellar emission transmitted through the ISM for
the old population.
transmitted: the stellar emission transmitted through the ISM for the
combined population.
young_nebular: the stellar emission from nebulae for the young
population.
old_nebular: the stellar emission from nebulae for the old
population.
nebular: the stellar emission from nebulae for the combined
population.
young_reprocessed: the stellar emission reprocessed by the ISM for
the young population.
old_reprocessed: the stellar emission reprocessed by the ISM for the
old population.
reprocessed: the stellar emission reprocessed by the ISM for the
combined population.

If an escape fraction is given, the following additional models will be produced:

young_intrinsic: the intrinsic emission for the young population.

old_intrinsic: the intrinsic emission for the old population.

intrinsic: the intrinsic emission for the combined population.

young_escaped: the incident emission that completely escapes the ISM
for the young population.

old_escaped: the incident emission that completely escapes the ISM
for the old population.

escaped: the incident emission that completely escapes the ISM for
the combined population.

young_emergent: the emission which emerges from the stellar
population, including any escaped emission for the young population.

old_emergent: the emission which emerges from the stellar population,
including any escaped emission for the old population.

emergent: the emission which emerges from the stellar population,
including any escaped emission for the combined population.

if dust_emission is not None:

young_dust_emission_birth: the emission from dust for the young
population.
young_dust_emission_ism: the emission from dust for the young
population.
young_dust_emission: the emission from dust for the young population.
old_dust_emission: the emission from dust for the old population.
dust_emission: the emission from dust for the combined population.
young_total: the final total combined emission for the young
population.
old_total: the final total combined emission for the old population.
total: the final total combined emission for the combined population.

Examples using `synthesizer.emission_models.stellar.pacman_model.BimodalPacmanEmission`¶

Camels example

Generate parametric galaxy SED

class synthesizer.emission_models.stellar.pacman_model.BimodalPacmanEmissionNoEscapedNoDust(grid, tau_v_ism='tau_v_ism', tau_v_birth='tau_v_birth', dust_curve_ism=<synthesizer.emission_models.transformers.dust_attenuation.Calzetti2000 object>, dust_curve_birth=<synthesizer.emission_models.transformers.dust_attenuation.Calzetti2000 object>, age_pivot=unyt_quantity(7, 'dimensionless'), fesc_ly_alpha='fesc_ly_alpha', label=None, **kwargs)[source]¶

A class defining the Bimodal Pacman model without fesc or dust emission.

This model defines both intrinsic and attenuated stellar emission without dust emission, split into young and old populations. If a lyman alpha escape fraction is given, a more sophisticated nebular emission model is used, including line and nebular continuum emission with the amount of lyman alpha emission scaled by the escape fraction.

This model will produce:

young_incident: the stellar emission incident onto the ISM for the
young population.
old_incident: the stellar emission incident onto the ISM for the old
population.
incident: the stellar emission incident onto the ISM for the
combined population.
young_transmitted: the stellar emission transmitted through the ISM
for the young population.
old_transmitted: the stellar emission transmitted through the ISM for
the old population.
transmitted: the stellar emission transmitted through the ISM for the
combined population.
young_nebular: the stellar emission from nebulae for the young
population.
old_nebular: the stellar emission from nebulae for the old
population.
nebular: the stellar emission from nebulae for the combined
population.
young_reprocessed: the stellar emission reprocessed by the ISM for
the young population.
old_reprocessed: the stellar emission reprocessed by the ISM for the
old population.
reprocessed: the stellar emission reprocessed by the ISM for the
combined population.
young_intrinsic: the intrinsic emission for the young population.
old_intrinsic: the intrinsic emission for the old population.
intrinsic: the intrinsic emission for the combined population.
young_attenuated_nebular: the nebular emission attenuated by dust
for the young population.
young_attenuated_ism: the intrinsic emission attenuated by dust for
the young population.
young_attenuated: the intrinsic emission attenuated by dust for the
young population.
old_attenuated: the intrinsic emission attenuated by dust for the old
population.
attenuated: the intrinsic emission attenuated by dust for the
combined population.

class synthesizer.emission_models.stellar.pacman_model.BimodalPacmanEmissionNoEscapedWithDust(grid, tau_v_ism='tau_v_ism', tau_v_birth='tau_v_birth', dust_curve_ism=<synthesizer.emission_models.transformers.dust_attenuation.Calzetti2000 object>, dust_curve_birth=<synthesizer.emission_models.transformers.dust_attenuation.Calzetti2000 object>, age_pivot=unyt_quantity(7, 'dimensionless'), dust_emission_ism=None, dust_emission_birth=None, fesc_ly_alpha='fesc_ly_alpha', label=None, stellar_dust=True, **kwargs)[source]¶

A class defining the Bimodal Pacman model without fesc + dust emission.

This model defines both intrinsic and attenuated stellar emission with dust emission, split into young and old populations. If a lyman alpha escape fraction is given, a more sophisticated nebular emission model is used, including line and nebular continuum emission with the amount of lyman alpha emission scaled by the escape fraction.

This model will produce:

young_incident: the stellar emission incident onto the ISM for the
young population.
old_incident: the stellar emission incident onto the ISM for the old
population.
incident: the stellar emission incident onto the ISM for the
combined population.
young_transmitted: the stellar emission transmitted through the ISM
for the young population.
old_transmitted: the stellar emission transmitted through the ISM for
the old population.
transmitted: the stellar emission transmitted through the ISM for the
combined population.
young_nebular: the stellar emission from nebulae for the young
population.
old_nebular: the stellar emission from nebulae for the old
population.
nebular: the stellar emission from nebulae for the combined
population.
young_reprocessed: the stellar emission reprocessed by the ISM for
the young population.
old_reprocessed: the stellar emission reprocessed by the ISM for the
old population.
reprocessed: the stellar emission reprocessed by the ISM for the
combined population.
young_intrinsic: the intrinsic emission for the young population.
old_intrinsic: the intrinsic emission for the old population.
intrinsic: the intrinsic emission for the combined population.
young_attenuated_nebular: the nebular emission attenuated by dust
for the young population.
young_attenuated_ism: the intrinsic emission attenuated by dust for
the young population.
young_attenuated: the intrinsic emission attenuated by dust for the
young population.
old_attenuated: the intrinsic emission attenuated by dust for the old
population.
attenuated: the intrinsic emission attenuated by dust for the
combined population.
young_emergent: the emission which emerges from the young stellar
population.
old_emergent: the emission which emerges from the old stellar
population.
emergent: the emission which emerges from the stellar population.
young_dust_emission_birth: the emission from dust for the young
population.
young_dust_emission_ism: the emission from dust for the young
population.
young_dust_emission: the emission from dust for the young population.
old_dust_emission: the emission from dust for the old population.
dust_emission: the emission from dust for the combined population.
young_total: the final total combined emission for the young
population.
old_total: the final total combined emission for the old population.
total: the final total combined emission for the combined population.

class synthesizer.emission_models.stellar.pacman_model.BimodalPacmanEmissionWithEscapedNoDust(grid, tau_v_ism='tau_v_ism', tau_v_birth='tau_v_birth', dust_curve_ism=<synthesizer.emission_models.transformers.dust_attenuation.Calzetti2000 object>, dust_curve_birth=<synthesizer.emission_models.transformers.dust_attenuation.Calzetti2000 object>, age_pivot=unyt_quantity(7, 'dimensionless'), fesc='fesc', fesc_ly_alpha='fesc_ly_alpha', label=None, **kwargs)[source]¶

A class defining the BimodalPacman model with fesc but no dust emission.

This model will produce:

young_incident: the stellar emission incident onto the ISM for the
young population.
old_incident: the stellar emission incident onto the ISM for the old
population.
incident: the stellar emission incident onto the ISM for the
combined population.
young_transmitted: the stellar emission transmitted through the ISM
for the young population.
old_transmitted: the stellar emission transmitted through the ISM for
the old population.
transmitted: the stellar emission transmitted through the ISM for the
combined population.
young_escaped: the incident emission that completely escapes the ISM
for the young population.
old_escaped: the incident emission that completely escapes the ISM
for the old population.
escaped: the incident emission that completely escapes the ISM for
the combined population.
young_nebular: the stellar emission from nebulae for the young
population.
old_nebular: the stellar emission from nebulae for the old
population.
nebular: the stellar emission from nebulae for the combined
population.
young_reprocessed: the stellar emission reprocessed by the ISM for
the young population.
old_reprocessed: the stellar emission reprocessed by the ISM for the
old population.
reprocessed: the stellar emission reprocessed by the ISM for the
combined population.
young_intrinsic: the intrinsic emission for the young population.
old_intrinsic: the intrinsic emission for the old population.
intrinsic: the intrinsic emission for the combined population.
young_attenuated_nebular: the nebular emission attenuated by dust
for the young population.
young_attenuated_ism: the intrinsic emission attenuated by dust for
the young population.
young_attenuated: the intrinsic emission attenuated by dust for the
young population.
old_attenuated: the intrinsic emission attenuated by dust for the old
population.
attenuated: the intrinsic emission attenuated by dust for the
combined population.
young_emergent: the emission which emerges from the young stellar
population, including any escaped emission.
old_emergent: the emission which emerges from the old stellar
population, including any escaped emission.
emergent: the emission which emerges from the stellar population,
including any escaped emission.

Examples using `synthesizer.emission_models.stellar.pacman_model.BimodalPacmanEmissionWithEscapedNoDust`¶

Camels example

Generate parametric galaxy SED

class synthesizer.emission_models.stellar.pacman_model.BimodalPacmanEmissionWithEscapedWithDust(grid, tau_v_ism='tau_v_ism', tau_v_birth='tau_v_birth', dust_curve_ism=<synthesizer.emission_models.transformers.dust_attenuation.Calzetti2000 object>, dust_curve_birth=<synthesizer.emission_models.transformers.dust_attenuation.Calzetti2000 object>, age_pivot=unyt_quantity(7, 'dimensionless'), dust_emission_ism=None, dust_emission_birth=None, fesc='fesc', fesc_ly_alpha='fesc_ly_alpha', label=None, stellar_dust=True, **kwargs)[source]¶

A class defining the Bimodal Pacman model with fesc and dust emission.

This model will produce:

young_incident: the stellar emission incident onto the ISM for the
young population.
old_incident: the stellar emission incident onto the ISM for the old
population.
incident: the stellar emission incident onto the ISM for the
combined population.
young_transmitted: the stellar emission transmitted through the ISM
for the young population.
old_transmitted: the stellar emission transmitted through the ISM for
the old population.
transmitted: the stellar emission transmitted through the ISM for the
combined population.
young_escaped: the incident emission that completely escapes the ISM
for the young population.
old_escaped: the incident emission that completely escapes the ISM
for the old population.
escaped: the incident emission that completely escapes the ISM for
the combined population.
young_nebular: the stellar emission from nebulae for the young
population.
old_nebular: the stellar emission from nebulae for the old
population.
nebular: the stellar emission from nebulae for the combined
population.
young_reprocessed: the stellar emission reprocessed by the ISM for
the young population.
old_reprocessed: the stellar emission reprocessed by the ISM for the
old population.
reprocessed: the stellar emission reprocessed by the ISM for the
combined population.
young_intrinsic: the intrinsic emission for the young population.
old_intrinsic: the intrinsic emission for the old population.
intrinsic: the intrinsic emission for the combined population.
young_attenuated_nebular: the nebular emission attenuated by dust
for the young population.
young_attenuated_ism: the intrinsic emission attenuated by dust for
the young population.
young_attenuated: the intrinsic emission attenuated by dust for the
young population.
old_attenuated: the intrinsic emission attenuated by dust for the old
population.
attenuated: the intrinsic emission attenuated by dust for the
combined population.
young_emergent: the emission which emerges from the young stellar
population, including any escaped emission.
old_emergent: the emission which emerges from the old stellar
population, including any escaped emission.
emergent: the emission which emerges from the stellar population,
including any escaped emission.
young_dust_emission_birth: the emission from dust for the young
population.
young_dust_emission_ism: the emission from dust for the young
population.
young_dust_emission: the emission from dust for the young population.
old_dust_emission: the emission from dust for the old population.
dust_emission: the emission from dust for the combined population.
young_total: the final total combined emission for the young
population.
old_total: the final total combined emission for the old population.
total: the final total combined emission for the combined population.

class synthesizer.emission_models.stellar.pacman_model.CharlotFall2000(grid, tau_v_ism='tau_v_ism', tau_v_birth='tau_v_birth', dust_curve_ism=<synthesizer.emission_models.transformers.dust_attenuation.Calzetti2000 object>, dust_curve_birth=<synthesizer.emission_models.transformers.dust_attenuation.Calzetti2000 object>, age_pivot=unyt_quantity(7, 'dimensionless'), dust_emission_ism=None, dust_emission_birth=None, fesc='fesc', fesc_ly_alpha='fesc_ly_alpha', label=None, stellar_dust=True, **kwargs)[source]¶

The Charlot & Fall(2000) emission model.

This emission model is based on the Charlot & Fall(2000) model, which describes the emission from a galaxy as a combination of emission from a young stellar population and an old stellar population. The dust attenuation for each population can be different, and dust emission can be optionally included.

This model is a simplified version of the BimodalPacmanEmission model, so in reality is just a wrapper around that model. The only difference is that there is no option to specify an escape fraction.

grid¶

The grid object.

Type:: synthesizer.grid.Grid

tau_v_ism¶

The V-band optical depth for the ISM.

Type:: float

tau_v_birth¶

The V-band optical depth for the nebular.

Type:: float

dust_curve_ism¶

The dust curve for the ISM.

Type:: AttenuationLaw

dust_curve_birth¶

The dust curve for the nebular.

Type:: AttenuationLaw

age_pivot¶

The age pivot between young and old populations, expressed in terms of log10(age) in Myr.

Type:: unyt.unyt_quantity

dust_emission_ism¶

The dust emission model for the ISM.

Type:: synthesizer.dust.EmissionModel

dust_emission_birth¶

The dust emission model for the nebular.

Type:: synthesizer.dust.EmissionModel

Examples using `synthesizer.emission_models.stellar.pacman_model.CharlotFall2000`¶

Camels example

Generate parametric galaxy SED

class synthesizer.emission_models.stellar.pacman_model.PacmanEmission(grid, tau_v='tau_v', dust_curve=<synthesizer.emission_models.transformers.dust_attenuation.PowerLaw object>, dust_emission=None, fesc='fesc', fesc_ly_alpha='fesc_ly_alpha', label=None, stellar_dust=True, **kwargs)[source]¶

A class defining the Pacman model.

This model defines both intrinsic and attenuated steller emission with or without dust emission. It also includes the option to include escaped emission for a given escape fraction. If a lyman alpha escape fraction is given, a more sophisticated nebular emission model is used, including line and nebuluar continuum emission.

This model will always produce:

incident: the stellar emission incident onto the ISM.
nebular: the stellar emission from nebulae.
transmitted: the stellar emission transmitted through the ISM.
reprocessed: the stellar emission reprocessed by the ISM.
attenuated: the intrinsic emission attenuated by dust.

If an escape fraction is given, it will also produce:

intrinsic: the intrinsic emission which is reprocessed + escaped.
escaped: the incident emission that completely escapes the ISM.
emergent: the emission which emerges from the stellar population,
including any escaped emission (i.e. attenuated + escaped).

If a dust emission model is given, it will also produce:

dust_emission: the emission from dust.
total: the final total combined emission.

Examples using `synthesizer.emission_models.stellar.pacman_model.PacmanEmission`¶

SC-SAM example

Photometry example

Plot spectra example

Generate parametric observed SED

An example showing how to scale a galaxy’s mass by luminosity/flux.

An example showing how to scale a galaxy's mass by luminosity/flux.

Generate parametric galaxy SED

class synthesizer.emission_models.stellar.pacman_model.PacmanEmissionNoEscapedNoDust(grid, tau_v='tau_v', dust_curve=<synthesizer.emission_models.transformers.dust_attenuation.PowerLaw object>, fesc_ly_alpha='fesc_ly_alpha', label=None, **kwargs)[source]¶

A class defining the Pacman model without escape fraction.

This model defines both intrinsic and attenuated steller emission without dust emission. If a lyman alpha escape fraction is given, a more sophisticated nebular emission model is used, including line and nebuluar continuum emission with the amount of lyman alpha emission scaled by the escape fraction.

This model will produce

incident: the stellar emission incident onto the ISM.
nebular: the stellar emission from nebulae.
transmitted: the stellar emission transmitted through the ISM.
reprocessed: the stellar emission reprocessed by the ISM.
attenuated: the intrinsic emission attenuated by dust.

Examples using `synthesizer.emission_models.stellar.pacman_model.PacmanEmissionNoEscapedNoDust`¶

Plot spectra example

Generate parametric galaxy SED

class synthesizer.emission_models.stellar.pacman_model.PacmanEmissionNoEscapedWithDust(grid, tau_v='tau_v', dust_curve=<synthesizer.emission_models.transformers.dust_attenuation.PowerLaw object>, dust_emission=None, fesc_ly_alpha='fesc_ly_alpha', label=None, stellar_dust=True, **kwargs)[source]¶

A class defining the Pacman model with escape fraction + dust emission.

This model defines both intrinsic and attenuated steller emission with dust emission. If a lyman alpha escape fraction is given, a more sophisticated nebular emission model is used, including line and nebuluar continuum emission with the amount of lyman alpha emission scaled by the escape fraction.

This model will produce:

incident: the stellar emission incident onto the ISM.
nebular: the stellar emission from nebulae.
transmitted: the stellar emission transmitted through the ISM.
reprocessed: the stellar emission reprocessed by the ISM.
attenuated: the intrinsic emission attenuated by dust.
dust_emission: the emission from dust.
total: the final total combined emission.

class synthesizer.emission_models.stellar.pacman_model.PacmanEmissionWithEscapedNoDust(grid, tau_v='tau_v', fesc='fesc', fesc_ly_alpha='fesc_ly_alpha', label=None, **kwargs)[source]¶

A class defining the Pacman model with fesc and no dust emission.

This model will produce:

incident: the stellar emission incident onto the ISM.
nebular: the stellar emission from nebulae.
transmitted: the stellar emission transmitted through the ISM.
reprocessed: the stellar emission reprocessed by the ISM.
intrinsic: the intrinsic emission which is reprocessed + escaped.
escaped: the incident emission that completely escapes the ISM.
attenuated: the intrinsic emission attenuated by dust.
emergent: the emission which emerges from the stellar population,
including any escaped emission (i.e. attenuated + escaped).

Examples using `synthesizer.emission_models.stellar.pacman_model.PacmanEmissionWithEscapedNoDust`¶

SC-SAM example

Photometry example

Generate parametric observed SED

An example showing how to scale a galaxy’s mass by luminosity/flux.

An example showing how to scale a galaxy's mass by luminosity/flux.

Generate parametric galaxy SED

class synthesizer.emission_models.stellar.pacman_model.PacmanEmissionWithEscapedWithDust(grid, tau_v='tau_v', dust_curve=<synthesizer.emission_models.transformers.dust_attenuation.PowerLaw object>, dust_emission=None, fesc='fesc', fesc_ly_alpha='fesc_ly_alpha', label=None, stellar_dust=True, **kwargs)[source]¶

A class defining the Pacman model with fesc and dust emission.

This model will produce:

incident: the stellar emission incident onto the ISM.
nebular: the stellar emission from nebulae.
transmitted: the stellar emission transmitted through the ISM.
reprocessed: the stellar emission reprocessed by the ISM.
intrinsic: the intrinsic emission which is reprocessed + escaped.
escaped: the incident emission that completely escapes the ISM.
attenuated: the intrinsic emission attenuated by dust.
emergent: the emission which emerges from the stellar population,
including any escaped emission (i.e. attenuated + escaped).
dust_emission: the emission from dust.
total: the final total combined emission.

class synthesizer.emission_models.stellar.pacman_model.ScreenEmission(grid, tau_v='tau_v', dust_curve=<synthesizer.emission_models.transformers.dust_attenuation.PowerLaw object>, dust_emission=None, fesc='fesc', fesc_ly_alpha='fesc_ly_alpha', label=None, stellar_dust=True, **kwargs)[source]¶

The ScreenEmission model.

This emission model is a simple dust screen model, where the dust is assumed to be in a screen in front of the stars. The dust curve and emission model can be specified, but the escape fraction is always zero.

This model is a simplified version of the PacmanEmission model, so in reality is just a wrapper around that model. The only difference is that fesc and fesc_ly_alpha are zero by definition.

grid¶

The grid object.

Type:: synthesizer.grid.Grid

dust_curve¶

The dust curve.

Type:: AttenuationLaw

dust_emission¶

The dust emission model.

Type:: synthesizer.dust.EmissionModel

synthesizer.emission_models.stellar.pacman_model¶

Examples using synthesizer.emission_models.stellar.pacman_model.BimodalPacmanEmission¶

Examples using synthesizer.emission_models.stellar.pacman_model.BimodalPacmanEmissionWithEscapedNoDust¶

Examples using synthesizer.emission_models.stellar.pacman_model.CharlotFall2000¶

Examples using synthesizer.emission_models.stellar.pacman_model.PacmanEmission¶

Examples using synthesizer.emission_models.stellar.pacman_model.PacmanEmissionNoEscapedNoDust¶

Examples using synthesizer.emission_models.stellar.pacman_model.PacmanEmissionWithEscapedNoDust¶

Examples using `synthesizer.emission_models.stellar.pacman_model.BimodalPacmanEmission`¶

Examples using `synthesizer.emission_models.stellar.pacman_model.BimodalPacmanEmissionWithEscapedNoDust`¶

Examples using `synthesizer.emission_models.stellar.pacman_model.CharlotFall2000`¶

Examples using `synthesizer.emission_models.stellar.pacman_model.PacmanEmission`¶

Examples using `synthesizer.emission_models.stellar.pacman_model.PacmanEmissionNoEscapedNoDust`¶

Examples using `synthesizer.emission_models.stellar.pacman_model.PacmanEmissionWithEscapedNoDust`¶