Dust attenuation#

Base class

class pixSED.misc.cigaleModules.ATTENUATIONmodule(name: Any, filters: str = 'V_B90 & FUV')[source]#

Bases: ABC

Code author: Wilfried Mercier - IRAP/LAM <wilfried.mercier@lam.fr>

Base class implementing a module to deal with dust attenuation.

Parameters:: name – identifier for the class

Keyword arguments

Parameters:: filters (str) – filters for which the attenuation will be computed and added to the SED information dictionary. You can give several filter names separated by a & (don’t use commas).

abstract __str__(*args, **kwargs) → str[source]#

Code author: Wilfried Mercier - IRAP/LAM <wilfried.mercier@lam.fr>

Implement a string representation of the class used to make Cigale parameter files.

abstract property spec: str#

Code author: Wilfried Mercier - IRAP/LAM <wilfried.mercier@lam.fr>

Implement a string representation for the .spec file of Cigale parameters.

Powerlaw

class pixSED.misc.cigaleModules.DUSTATT_POWERLAWmodule(filters: str = 'V_B90 & FUV', Av_young: List[float] = [1.0], Av_old_factor: List[float] = [0.44], uv_bump_wavelength: List[float] = [217.5], uv_bump_width: List[float] = [35.0], uv_bump_amplitude: List[float] = [0.0], powerlaw_slope: List[float] = [- 0.7])[source]#

Bases: ATTENUATIONmodule

Code author: Wilfried Mercier - IRAP/LAM <wilfried.mercier@lam.fr>

Class implementing a single powerlaw attenuation law module.

Keyword arguments

Parameters:

filters (str) – filters for which the attenuation will be computed and added to the SED information dictionary. You can give several filter names separated by a & (don’t use commas).
Av_young (list[float]) – V-band attenuation of the young stellar population
Av_old_factor (list[float]) – reduction factor for the V-band attenuation of the old population compared to the young one. It must be between 0 and 1.
uv_bump_wavelength (list[float]) – central wavelength of the UV bump in \(\rm nm\)
uv_bump_width (list[float]) – width (FWHM) of the UV bump in \(\rm nm\)
uv_bump_amplitude (list[float]) – amplitude of the UV bump. For the Milky Way: 0.75.
powerlaw_slope (list[float]) – slope delta of the power law modifying the attenuation curve

__str__(*args, **kwargs) → str[source]#

Code author: Wilfried Mercier - IRAP/LAM <wilfried.mercier@lam.fr>

Implement a string representation of the class used to make Cigale parameter files.

property spec: str#

Code author: Wilfried Mercier - IRAP/LAM <wilfried.mercier@lam.fr>

Implement a string representation for the .spec file of Cigale parameters.

Two powerlaws

class pixSED.misc.cigaleModules.DUSTATT_2POWERLAWSmodule(filters: str = 'V_B90 & FUV', Av_BC: List[float] = [1.0], slope_BC: List[float] = [- 1.3], BC_to_ISM_factor: List[float] = [0.44], slope_ISM: List[float] = [- 0.7])[source]#

Bases: ATTENUATIONmodule

Code author: Wilfried Mercier - IRAP/LAM <wilfried.mercier@lam.fr>

Class implementing a double powerlaw attenuation law module: a birth cloud power law applied only to the young star population and an ISM power law applied to both the young and the old stellar populations.

Keyword arguments

Parameters:

filters (str) – filters for which the attenuation will be computed and added to the SED information dictionary. You can give several filter names separated by a & (don’t use commas).
Av_BC (list[float]) – V-band attenuation in the birth clouds. Minimum is 0.
slope_BC (list[float]) – power law slope of the attenuation in the birth clouds
BC_to_ISM_factor (list[float]) – Av ISM / Av BC. Must be between 0 and 1.
slope_ISM (list[float]) – power law slope of the attenuation in the ISM

__str__(*args, **kwargs) → str[source]#

Code author: Wilfried Mercier - IRAP/LAM <wilfried.mercier@lam.fr>

Implement a string representation of the class used to make Cigale parameter files.

property spec: str#

Code author: Wilfried Mercier - IRAP/LAM <wilfried.mercier@lam.fr>

Implement a string representation for the .spec file of Cigale parameters.

Calzetti et al. (2000)

class pixSED.misc.cigaleModules.DUSTATT_CALZLETTImodule(filters: str = 'B_B90 & V_B90 & FUV', E_BVs_young: List[float] = [0.3], E_BVs_old_factor: List[float] = [1.0], uv_bump_wavelength: List[float] = [217.5], uv_bump_width: List[float] = [35.0], uv_bump_amplitude: List[float] = [0.0], powerlaw_slope: List[float] = [0.0])[source]#

Bases: ATTENUATIONmodule

Code author: Wilfried Mercier - IRAP/LAM <wilfried.mercier@lam.fr>

Class implementing a Calzetti et al. (2000) and Leitherer et al. (2002) attenuation law module.

Keyword arguments

Parameters:

filters (str) – filters for which the attenuation will be computed and added to the SED information dictionary. You can give several filter names separated by a & (don’t use commas).
E_BVs_young (list[float]) – E(B-V)*, the colour excess of the stellar continuum light for the young population. Minimum is 0.
E_BVs_old_factor (list[float]) – reduction factor for the E(B-V)* of the old population compared to the young one. Must be between 0 and 1.
uv_bump_wavelength (list[float]) – central wavelength of the UV bump in \(\rm nm\). Minimum is \(0\,\rm nm\).
uv_bump_width (list[float]) – width (FWHM) of the UV bump in \(\rm nm\). Minimum is \(0\,\rm nm\).
uv_bump_amplitude (list[float]) – amplitude of the UV bump. For the Milky Way: 3. Minimum is 0.
powerlaw_slope (list[float]) – slope delta of the power law modifying the attenuation curve.

__str__(*args, **kwargs) → str[source]#

Code author: Wilfried Mercier - IRAP/LAM <wilfried.mercier@lam.fr>

Implement a string representation of the class used to make Cigale parameter files.

property spec: str#

Code author: Wilfried Mercier - IRAP/LAM <wilfried.mercier@lam.fr>

Implement a string representation for the .spec file of Cigale parameters.

Charlot & Fall (2000)

class pixSED.misc.cigaleModules.DUSTATT_MODIFIED_CF00module(filters: str = 'V_B90 & FUV', Av_ISM: List[float] = [1.0], mu: List[float] = [0.44], slope_ISM: List[float] = [- 0.7], slope_BC: List[float] = [- 1.3])[source]#

Bases: ATTENUATIONmodule

Code author: Wilfried Mercier - IRAP/LAM <wilfried.mercier@lam.fr>

Class implementing a modified Charlot & Fall 2000 attenuation law module.

Keyword arguments

Parameters:

filters (str) – filters for which the attenuation will be computed and added to the SED information dictionary. You can give several filter names separated by a & (don’t use commas).
Av_ISM (list[float]) – V-band attenuation in the interstellar medium. Minimum is 0.
mu (list[float]) – Av_ISM / (Av_BC+Av_ISM). Must be between 0.0001 and 1.
slope_ISM (list[float]) – power law slope of the attenuation in the ISM
slope_BC (list[float]) – power law slope of the attenuation in the birth clouds

__str__(*args, **kwargs) → str[source]#

Code author: Wilfried Mercier - IRAP/LAM <wilfried.mercier@lam.fr>

Implement a string representation of the class used to make Cigale parameter files.

property spec: str#

Code author: Wilfried Mercier - IRAP/LAM <wilfried.mercier@lam.fr>

Implement a string representation for the .spec file of Cigale parameters.

Starburst

class pixSED.misc.cigaleModules.DUSTATT_MODIFIED_STARBURSTmodule(filters: str = 'B_B90 & V_B90 & FUV', E_BV_lines: List[float] = [0.3], E_BV_factor: List[float] = [0.44], uv_bump_wavelength: List[float] = [217.5], uv_bump_width: List[float] = [35.0], uv_bump_amplitude: List[float] = [0.0], powerlaw_slope: List[float] = [0.0], Ext_law_emission_lines: List[int] = 1, Rv: List[float] = 3.1)[source]#

Bases: ATTENUATIONmodule

Code author: Wilfried Mercier - IRAP/LAM <wilfried.mercier@lam.fr>

Class implementing a modified Calzetti 2000 attenuation law module.

Keyword arguments

Parameters:

filters (str) – filters for which the attenuation will be computed and added to the SED information dictionary. You can give several filter names separated by a & (don’t use commas).
E_BV_lines (list[float]) – E(B-V)l, the colour excess of the nebular lines light for both the young and old stellar population. Minimum is 0.
E_BV_factor (list[float]) – reduction factor to apply on E_BV_lines to compute E(B-V)s the stellar continuum attenuation. Both young and old population are attenuated with E(B-V)s. Must be between 0 and 1.
uv_bump_wavelength (list[float]) – central wavelength of the UV bump in \(\rm nm\). Minimum is \(0\,\rm nm\).
uv_bump_width (list[float]) – width (FWHM) of the UV bump in \(\rm nm\). Minimum is \(0\,\rm nm\).
uv_bump_amplitude (list[float]) – amplitude of the UV bump. For the Milky Way: 3. Minimum is 0.
powerlaw_slope (list[float]) – slope delta of the power law modifying the attenuation curve
Ext_law_emission_lines (list[int]) – extinction law to use for attenuating the emission lines flux. Possible values are: 1, 2, 3. 1: Milky Way, 2: Large Magellanic Cloud, 3: Small Magellanic Cloud. MW is modelled using CCM89, SMC and LMC using Pei92.
Rv (list[float]) – ratio of total to selective extinction, A_V / E(B-V), for the extinction curve applied to emission lines. Standard value is 3.1 for MW using CCM89, but can be changed. For SMC and LMC, using Pei92, the value is automatically set to 2.93 and 3.16 respectively, no matter the value you provide.

__str__(*args, **kwargs) → str[source]#

Code author: Wilfried Mercier - IRAP/LAM <wilfried.mercier@lam.fr>

Implement a string representation of the class used to make Cigale parameter files.

property spec: str#

Code author: Wilfried Mercier - IRAP/LAM <wilfried.mercier@lam.fr>

Implement a string representation for the .spec file of Cigale parameters.