  In this paper, we present the first results of spectral and timing properties
of the atoll source 4U 1705-44 using $\sim$ 100 ks data obtained with Large
Area X-ray Proportional Counter (LAXPC) onboard {\it AstroSat}. The source was
in the high-soft state during our observations and traced out a {\it banana
track} in the Hardness Intensity Diagram (HID). We study {\bf the} evolution of
the Power Density Spectra (PDS) and the energy spectra along the HID. PDS show
presence of a broad Lorentzian feature (Peaked Noise or PN) centered at $1-13$
Hz and a very low frequency noise (VLFN). The energy spectra can be described
by sum of a thermal Comptonized component, a power-law and a broad iron line.
The hard tail seen in the energy spectra is variable and contribute $4-30$\% of
the total flux. The iron line seen in this source is broad (FWHM $\sim$ 2 keV)
and strong (EW $\sim$ $369-512$ eV). Only relativistic smearing in the
accretion disc can not explain the origin of this feature and requires other
mechanism such as broadening by Comptonization process in the external part of
the `Comptonized Corona'. A subtle and systematic evolution of the spectral
parameters (optical depth, electron temperature etc.) is seen as the source
moves along the HID. We study the correlation between frequency of the PN and
the spectral parameters. PN frequency seems to be correlated with the strength
of the corona. We discuss the implication of the results in the paper.
