Remote Telescope System (RTS2) is an integrated system for remote observatory control. It is designed to keep an observatory running, protect it from elements, take images, ensure that pointing is good, react to TOOs, keep track of what was done, send you data, and help you to do science. It picks targets from a database table, stores image meta-data in a database, processes images, and stores WCS coordinates in the database. An abstract device layer enables control of all possible combinations of mounts, CCDs, photometers, and roof and cupola controllers.
ccurve_create.tcl is a TCL script (plus associated csh scripts) that makes it is possible to calculate cooling curves (plasma emissivities, in units of erg cm^3 s^-1) as a function of plasma temperature using the hot plasma codes available in the XSPEC spectral fitting program. Element-or-line-specific cooling functions can also be created. 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 (Python And PGPLOT-based FITS Image Plotter) is a FITS image plotter based on the Python bindings to the pgplot graphics library. 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.
Henry is an educational astrometry utility for performing calculations based on a Hertzsprung-Russel (H-R) diagram, such as spectroscopic parallax for working out the distance to a given star. Unlike many other solutions that use in-built images for their H-R diagrams, Henry plots data directly from the European Space Agency's HIPPARCOS catalog, allowing increased accuracy while also giving students greater room to experiment by exploring the catalogue themselves.
SAOTrace is a suite of software designed to simulate the as-built performance of grazing-angle X-ray optics using the ray-tracing approach. It is derived from portions of the NASA OSAC (Optical Surface Analysis Code) software suite. It can model nested conical as well as flat optical designs, and includes the ability to model arbitrary support structures and baffles. It can model non-ideal multi-layer reflective coatings as well as scattering from the optical surfaces.
AstroBuffer is a CCD astrophotography image manipulation application. It can open FITS and SBIG (st9) files. Contrast is adjustable to view different backgrounds and ranges of an image. It can scale, shift, rotate, and zoom in and out. Images can be aligned based on two star alignment, and can be summed, subtracted, averaged, and divided. RGB color images can be created from three images. Images can be saved as FITS or as any format that QT supports.
Extrema, originally developed in the fields of nuclear and particle physics, is a powerful visualization and data analysis tool that enables researchers to quickly distill their large, complex data sets into meaningful information. Its flexibility, sophistication, and power allow you to easily develop your own commands and create highly customized graphs.