The software made available on this website is provided "as is." Use at your own risk. All software is made available under the terms of the GNU Public License (version 2). Software is Copyright (C) 2000-2007 David Strickland.
Proteus is a library of the basic data structures and functions necessesary to efficiently and simply manage 2 or 3-dimensional hydrodynamic data. It is used by other tools to calculate interesting astronomical observables, e.g. X-ray images, spectra, multi-wavelength long-slit emission or absorption line spectra, as well as quantify the basic physical properties of the data.
A gzipped tar file of the current version of Proteus is available here.
coolcurve_create is a set of tcl and csh scripts that enable the creation of cooling functions (the emissivity per unit density per volume per unit elemental abundance, as a function of plasma temperature) using the modern hot plasma codes available within the XSPEC spectral fitting code.
It is particularly useful for calculating the broad-band or line-specific Far-UV or X-ray emissivities needed to predict the observable UV or X-ray emission from diffuse hot plasmas in galaxies, galaxy halos and the Warm/Hot IGM. These can be used in hydrodynamical simulations to assess the total cooling rate, calculate the luminosity in a specific wavelength/energy range, or more generally to calculate X-ray or UV line diagnostics.
PAPFIP is a FITS image plotter based on the python bindings to the pgplot graphics library. PAPFIP is an acronym for "Python and PGPLOT-based FITS image plotter". It is intended as a non-interactive (command-line or script-driven) astronomical image plotter intended for the automated or repeated production of finalized publication-quality postscipt files, rather than a method of inspecting or visualizing the data.