calculate luminosity. XSpec convolution model *Experimental*.
A convolution model to calculate the luminosity of other model components.
The Sherpa commands calc_energy_flux, calc_photon_flux, and sample_flux, as well as the Calculating Model Flux and Flux Uncertainty thread can also be used. These would then need to be converted to a luminosity using your favorite Cosmology. See also the calc_kcorr function for applying a K correction to a spectral model.
|1||Emin||Minimum source-frame energy over which luminosity is calculated (keV)|
|2||Emax||Maximum source-frame energy over which luminosity is calculated (keV)|
|3||Redshift||Redshift of the source|
|4||lg10Lum||log (base 10) of the luminosity in erg/s|
Loading the X-Spec convolution models
Please see ahelp xsconvolve for information on how to load the model.
- This is an experimental release of the convolution models; please take care when using this model.
- When lumin is used with multiple additive models, the normalization of one of the additive models must be fixed to a non-zero value.
- The energy range defined by the Emin and Emax parameters must lie inside the energy range of the response matrix.
- If the model to which lumin is applied integrates to zero then a divide-by-zero error will occur and the fit will likely fail due to the presence of NaN values.
This information is taken from the XSpec User's Guide. Version 12.10.0e of the XSpec models is supplied with CIAO 4.11.
sherpa> from sherpa_contrib.xspec.xsconvolve import load_xsclumin sherpa> load_xsclumin("clumin") sherpa> xsphabs.gal() sherpa> xspowerlaw.pl() sherpa> xsgaussian.gs() sherpa> clumin.emin = 0.5 sherpa> clumin.emax = 7 sherpa> clumin.redshift = 0.2 sherpa> set_source(clumin(gal * (pl + gs)))
Luminosity of the absorbed model
If the power-law or gaussian normalization is fixed to a non-zero value then the above will calculate the luminosity and error on the entire model (absorbed). The redshift and energy range range are 0.2 and 0.5 to 7 keV respectively.
sherpa> set_source(gal * clumin(pl + gs)))
Luminosity of the un-absorbed model
If the power-law or gaussian normalization is fixed to a non-zero value then this calculates the unabsorbed luminosity and error.
sherpa> set_source(gal * (pl + clumin(gs)))
Luminosity of a component
If the gaussian normalization is fixed to a non-zero value then this calculates the unabsorbed luminosity and error of the gaussian component.
About Contributed Software
This script is not an official part of the CIAO release but is made available as "contributed" software via the CIAO scripts page. Please see this page for installation instructions - such as how to ensure that the parameter file is available.
For a list of known bugs and issues with the XSPEC models, please visit the XSPEC bugs page.
- list_model_components, list_models, load_xscflux, load_xscpflux, load_xsgsmooth, load_xsireflect, load_xskdblur, load_xskdblur2, load_xskerrconv, load_xslsmooth, load_xspartcov, load_xsrdblur, load_xsreflect, load_xsrfxconv, load_xsrgsxsrc, load_xssimpl, load_xsvashift, load_xsvmshift, load_xsxilconv, load_xszashift, load_xszmshift, models, tablemodel, xs, xsconvolve