XSTAR Home Page

Two component XSTAR model fit to the 800 ks Chandra HETG observation of NGC 3783. Model fit performed in xspec11 using the warmabs analytic model.

What is XSTAR?

XSTAR is a computer program for calculating the physical conditions and emission spectra of photoionized gases.

How Do I Get XSTAR?

Xstar is avaible in several different ways.

The XSTAR package is now integrated and distributed with the HEASARC's standard HEADAS package, so if your facility has this package installed then you already have access to xstar. Xstar Version 2.2 is part of the HEADAS release, November 2009.

XSTAR is also available as a standalone package. The standalone XSTAR (or the full HEADAS), is available in either source or binary versions and it can be downloaded from here .

Version 2.2 of xstar is available. It contains many updates and enhancements which are described in the manual

The release version of xstar is now available on hera. To use it, you must install fv and set up your environment to use it (fv is part of the standard heasoft software distribution or it can be installed standalone), and type 'fv -r xstar'. Input parameters are specified by prompting or else on the command line. Currently the output is buffered in large blocks, rather than printing each line of output as processing progresses. Thus it may appear that nothing is happening for a while until the buffer fills and is sent to your screen. It's also possible to start up the xstar task in hera, and then retrieve the results later, without having to keep the command window open. One would need to specify all the parameters directly on the command line, and also add a "-nowait " flag. For example: "fv -r -nowait me@milkyway.gsfc.nasa.gov xstar cfrac=1. temperature=400. ..." You will then receive an email message when the job is finished, with instructions on how to retrieve the output.

A utility has been created for extracting atomic data and rates from the xstar database. This utility is a standalone fortran program, which calls many of the xstar routines, and returns the rate (forward and reverse) and raw atomic data for a single type of rate for a single ion. It can be found here

An analytic model for calculating warm absorber and emitter spectra within xspec is available. This has the advantage that it avoids the intrinsic approximations associated with use of tables for absorption with variable abundances treated as multiplicative parameters, and the intrinsic clumsiness of the use of tables. It also allows the use of arbitrary spectral resolution, not limited by the internal xstar spectral resolution. To use it, download the tarfile, unzip and untar in your user area, and follow the installation instructions contained in the README. This includes the analogous routine which simulates the absorption (and emission) by a gas in coronal equilibrium. Scattered emission can be modeled using the 'windabs' model. These routines are still in the testing phase, so please send reports of bugs and problems.

A version of xstar which allows for parallel computation of a grid of models has been developed by Michael Noble of MIT. pvm_xstar fosters parallel execution of XSTAR over large, time-consuming sets of parameters.

Online Documentation

XSTAR documentation is included as part of the standard source distribution and is also viewable online or can be downloaded as a PostScript file or HTML.

Sample xstar output from optically thin photoionized model, alpha=1 power law, line opacities

Sample xstar output from optically thin photoionized model, alpha=1 power law, RRC emissivities

Sample xstar output from optically thin photoionized model, alpha=1 power law, RRC opacities

Sample XSPEC table models

Postscript plots of atomic rates(42 Mbytes).

An ascii version of the xstar database (28 Mbytes).

An ascii version of the xstar database, version 2.1ln2, containing up-to-date K shell cross sections (63 Mbytes).

The xstar database sorted according to process. (16 Mbytes).