reflection from ionized material. XSpec convolution model *Experimental*.
Convolution model for reflection from ionized material according to the method of Magdziarz & Zdziarski (1995, MNRAS, 273, 837). This is a generalization of the pexrav and bexrav models. Ionization and opacities of the reflectiong medium is computewd as in the absori model. The reflection component alone can be obtained for
|rel_refl| < 0
then the actual reflection normalization is |rel_refl|. Note that you need to change then the limits of |rel_refl| excluding zero (as then the direct component appears). If
E_c = 0
, there is no cutoff in the power law. The metal and iron abundance are variable with respect to those set by the command set_xsabund.
When using this model it is essential to extend the energy range over which the model is calculated because photons at higher energies are Compton down-scattered into the target energy range. Please contact the CXC HelpDesk if you need to do this. The upper limit on the energies should be set above that for which the input spectrum has significant flux. To speed up the model, calculation of the output spectrum can be limited to energies below a given value by using set-xset to define IREFLECT_MAX_E (in units of keV). For instance, suppose that the original data extends up to 100 keV. To accurately determine the reflection it may be necessary to extend the energy range up to 500 keV. Now to avoid calculating the output spectrum between 100 and 500 keV use the command
sherpa> set_xsxset('IREFLECT_MAX_E', 100.0)
The core of this model is a Greens' function integration with one numerical integral performed for each model energy. The numerical integration is done using an adaptive method which continues until a given estimated fractional precision is reached. The precision can be changed by setting IREFLECT_PRECSION. The default precision is 0.01 (i.e. 1%).
|1||rel_refl||reflection scaling factor (1 for isotropic source above disk)|
|3||abund||abundance of elements heavier than He relative to the solar abundances|
|4||Fe_abund||iron abundance relative to the above|
|5||cosIncl||cos i, the inclination angle|
|6||T_disk||disk temperature in K|
|7||xi||disk ionization parameter, xi=4 pi F_ion / n, where F_ion is the 5 eV - 20 keV irradiating flux, n is the density of the reflector.|
For more infomration on the xi parameter see Done et al., 1992, ApJ 395, 275.
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.
- Sherpa does not have an equivalent of the extend command in X-Spec.
This information is taken from the XSpec User's Guide. Version 12.10.0e of the XSpec models is supplied with CIAO 4.11.
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_xsclumin, load_xscpflux, load_xsgsmooth, 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