Long-term study of variable stars and asteroids lightcurves using a 25cm Meade
Schmidt-Cassegrain optical reflecting telescope driven by an altazimuth Mount and along with a
SBIG ST-7E CCD camera. B,V and R standard filters attached to a CFW-9 Filter wheel are
used. The telescope is also used for observing very close bright extended objects such as planets,
comets, nebulae and galaxies.


Imaging and monitoring of solar phenomena such as solar flares, sunspots, solar prominences and
and granulation. The telescope used is a 10cm H-Alpha Solar Telescope by the manufacturer
”Lunt Solar System” and is equipped with a CCD Camera, ZWO ASI120MM.

Experimental Radio Astronomy

Experiments involving small radio telescopes (SRT) that offer students, researchers and amateur
radio astronomers a great opportunity to acquaint themselves with techniques used in radio
astronomy observation, data acquisition and analysis. Design and construction of low cost and
effective antennas and receiver system used in these SRTs with design and functionality that
look similar to professional telescopes except that dish size and sensitivity are more restricted.
Antenna types include parabolic dish, dipole, Yagi-Uda and pyramidal horn. For the parabolic
dishes, we have a fully steerable mesh dish of diameter of 3m used for undergraduate and
graduate teaching, three solid dishes of diameter of 2m used as a phased array interferometer to
demonstrate the techniques of interferometer, locally made solid dishes of 6m and 10m used for
transit observations of nearby radio sources. Other antennas include a locally made Yagi-Uda
antenna and pyramidal horn antennas operating at 1420 MHz and both dedicated for 21cm
astronomy, a dual-dipole antenna used in the simple low cost CBSS’s Radio Jove Telescope that
brings the sounds of Jupiter, Sun and the Milky-way to students, researchers and the general

Extragalactic Astrophysics

Modelling of spectral energy distribution of observed star forming galaxies with the aim of
deriving their physical properties such as star formation rate, stellar and dust mass. We mainly
use the state-of-the-art SED fitting fortran and python codes respectively, GRASIL (GRAsil and
SILicates) and CIGALE (Code Investigating GALaxy Emission).

Close Menu