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Collection of embedded softwares to control a telescope mount.
EQ Track purpose is to provide amateur telescope makers (ATM) with electronic board schematics and embedded software to control their telescope mount via stepping motors.
EQ Track comes in different "flavors" :
- "Basic" controls the right ascension and declination motors of an equatorial mount.
- "Go To" controls the motors of a mount in any orientation (ie. equatorial, altazimuth, alt-alt), to point and track equatorial coordinates.
INDI is an instrument neutral distributed interface control protocol that aims to provide backend driver support and automation for a wide range of Astronomical devices (telescopes, focusers, CCDs..etc).
Project migrated to Github: https://github.com/indilib/indi
Multi-SETI@home Monitor. This program was written to monitor SETI@home and BOINC activity that may be running on multiple computers over a network without having to cross mount file systems. Runs on Windows/Linux/Unix.
PARAMESH is a package of Fortran 90 subroutines designed to provide an
application developer with an easy route to extend an existing serial
code which uses a logically cartesian structured mesh into a parallel
code with adaptive mesh refinement(AMR).
ephem68k is an astronomy software the TI-92 and TI Voyage 200 CAS systems. It calculates astronomical data like julian date, local sidereal time, full/new moons, ephemerides of fixed and solar objects and more. ephem68k is based on ephem 4.29 code.
GIRAFFE Base Line Data Reduction Software is a set of python scripts and modules
and a C library to reduce FITS images produced by the Very Large Telescope (VLT)
FLAMES instrument.
KTelescope is a robust Server/Client control library for Meade's LX200 based telescopes. The library is divided into two components: A Low level modulo that allows access to the LX200 command set, and a Client/Server skeleton for remote control.
OpenWD is a scientific project to develop state-of-the-art models of white dwarf stars, to draw upon the collective expertise of astronomers around the world, and to facilitate comparisons between evolutionary and pulsational studies of white dwarf stars