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We study the statistical properties of O VI, C IV, and Ne VIII absorbers atlow-$z$ (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 eachsimulation, by considering a wide range of metagalactic ionizing UV background(UVB), we show the statistical properties such as distribution functions ofcolumn density ($N$), $b$-paramerer and velocity spread ($\Delta V_{90}$), therelationship between $N$ and $b$-parameter and the fraction of Lya absorbersshowing detectable metal lines as a function of $N$(H I) are influenced by theUVB used. This is because UVB changes the range in density, temperature, andmetallicity of gas contributing to a given absorption line. For simulationsconsidered here, we show the difference in some of the predicted distributionsbetween different simulations is similar to the one obtained by varying the UVBfor a given simulation. Most of the observed properties of O VI absorbers areroughly matched by Sherwood simulation with "WIND+AGN" feedback when using theUVB with a lower O VI ionization rate. However, this simulation fails toproduce observed distributions of C IV and fraction of H I absorbers withdetectable metals. Therefore, in order to constrain different feedbackprocesses and/or UVBs, using observed properties of H I and metal ions, it isimportant to perform simultaneous analysis of various observable parameters.

Role of ionizing background on the statistics of metal absorbers in hydrodynamical simulations