  We study the statistical properties of O VI, C IV, and Ne VIII absorbers at
low-$z$ (i.e., $z<0.5$) using Sherwood simulations with "WIND" only and
"WIND+AGN" feedback and Massive black simulation that incorporates both "WIND"
i.e. outflows driven by stellar feedback and AGN feedbacks. For each
simulation, by considering a wide range of metagalactic ionizing UV background
(UVB), we show the statistical properties such as distribution functions of
column density ($N$), $b$-paramerer and velocity spread ($\Delta V_{90}$), the
relationship between $N$ and $b$-parameter and the fraction of Lya absorbers
showing detectable metal lines as a function of $N$(H I) are influenced by the
UVB used. This is because UVB changes the range in density, temperature, and
metallicity of gas contributing to a given absorption line. For simulations
considered here, we show the difference in some of the predicted distributions
between different simulations is similar to the one obtained by varying the UVB
for a given simulation. Most of the observed properties of O VI absorbers are
roughly matched by Sherwood simulation with "WIND+AGN" feedback when using the
UVB with a lower O VI ionization rate. However, this simulation fails to
produce observed distributions of C IV and fraction of H I absorbers with
detectable metals. Therefore, in order to constrain different feedback
processes and/or UVBs, using observed properties of H I and metal ions, it is
important to perform simultaneous analysis of various observable parameters.
