Abstract:
Accurate wavelength calibration is an important factor for any measure ment with high resolution spectrographs. Stellar spectrum comprises of dis crete absorption or emission lines whose position is precisely determined by
calibrating the spectrographs using known reference lines generated from lab oratory sources. For the spectrograph to measure small variations in Doppler
shift, the wavelength calibration must be sufficiently stable during observa tion time. Instrument instability, mainly due to environmental factors like
temperature and pressure variations, and limitations of traditional calibration
methods, for example Th-Ar lamps, are the two challenges which limit high
precision spectroscopy.
Through proper environmental control, by maintaining pressure at 1 mbar
and temperature fluctuations at ±0.05◦C, Fabry-P´erot etalons (FP) can yield
a velocity precision of 1-10 m/s, when used for wavelength calibration. A pas sively stabilized FP based wavelength calibrator has been developed for Hanle
Echelle Spectrograph (HESP) installed on the Himalayan Chandra Telescope
(HCT). The etalon has been characterized using Fourier Transform Spectro graph (FTS) and tested with high resolution echelle spectrograph on Vainu
Bappu Telescope (VBT). Initial test runs of the entire instrument with HESP
have been conducted to study the performance of the FP instrument with the
spectrograph.
Often, curvature and tilted lines are the observed artifacts in a high res olution spectra, arising due to the design of the respective spectrographs.
Removal of these artifacts can help avoid wrong flux calculation and line cen troid position misinterpretation, which can aid in a better prediction of the
wavelength calibration model. As a part of this thesis work, a post processing
technique for the correction of the observed curvature and tilt in the spec tra has also been worked out. Curvature and tilt correction algorithm has
been tested on the FP and Th-Ar calibration spectra obtained from different
spectrographs.
