  The combination of photometry, spectroscopy and spectropolarimetry of the
chemically peculiar stars often aims to study the complex physical phenomena
such as stellar pulsation, chemical inhomogeneity, magnetic field and their
interplay with stellar atmosphere and circumstellar environment. The prime
objective of the present study is to determine the atmospheric parameters of a
set of Am stars to understand their evolutionary status. Atmospheric abundances
and basic parameters are determined using full spectrum fitting technique by
comparing the high-resolution spectra to the synthetic spectra. To know the
evolutionary status we derive the effective temperature and luminosity from
different methods and compare them with the literature. The location of these
stars in the H-R diagram demonstrate that all the sample stars are evolved from
the Zero-Age-Main-Sequence towards Terminal-Age-Main-Sequence and occupy the
region of $\delta$ Sct instability strip. The abundance analysis shows that the
light elements e.g. Ca and Sc are underabundant while iron peak elements such
as Ba, Ce etc. are overabundant and these chemical properties are typical for
Am stars. The results obtained from the spectropolarimetric analysis shows that
the longitudinal magnetic fields in all the studied stars are negligible that
gives further support their Am class of peculiarity.
