Thermal and Dynamical Properties of CIV Absorbers
Adviser: Dr. Tae-Sun Kim
The spectra of Quasi-Stellar Objects (QSOs) provide a unique labratory for studying the properties of
the intergalactic medium (IGM). As the QSO light propegates through the IGM, gas clouds leave their
mark on the spectra. By analyzing the breadth, depth, shape, and position of these absorption lines,
many key properties can be determined about the gas clouds in the IGM. This study looked at the clouds
rich in triply ionized Carbon (CIV) to determine their thermal and dynamical properties at redshifts
between 1.5 and 3.5.
A lot is unknown about the IGM at these redshifts. It is important to study because at this stage of
the universe, 90% of all of the Baryons are found in the IGM. In order to determine the total Baryonic
density, the IGM must be well defined. The QSO spectra also give us clues about the evolution of
galaxies. It is believed that the CIV absorbers are located in circumgalactic clouds reaching beyond
the galaxy halos and are enriched by the supernovae within the galaxies.
The Data comes from high resolution spectra taken from 17 QSOs using the Ultraviolet and Visible Echelle
Spectrograph (UVES) on the VLT at the European Southern Observatory. These spectra have a resolution of
6.7 km/s and a signal-to-noise of 80-120 in the CIV region and 20-60 in the forest region. They were
reduced and normalized using the UVES data reduction pipeline. The absorption lines were then fitted
by hand using Voigt profiles.
The VLT at ESO.
The following links are very useful for looking up info on UNIX, web page making, and astrophysical data and journals.
SIMBAD (Stellar/Galactic database)
NED (Extragalactic database)
Web page basics
NASA Astrophysics Data Service