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Physical properties of the interstellar medium (ISM) such as metallicity, ionisation parameter, temperature, density and pressure regulate star-formation in galaxies, and thus are the prime drivers of galaxy evolution. In order to understand how galaxies evolved through cosmic time, it is important to study these properties better, particularly at high redshift. I will talk about the high-redshift ISM studies we performed, the challenges involved, and the possible solutions. I will present our pilot study comparing new rest-frame UV and optical emission line nebular diagnostics, for the first time, to the brightest known lensed galaxy at cosmic noon followed by the full high-redshift sample. I will demonstrate the power of rest-frame UV spectra surveys when combined with these diagnostics and unprecedented sensitivity of the upcoming space-based and late ground-based observatories. However, the spatial resolution of these surveys might impact the accuracy of measuring the distribution of metals in galaxies. I will present a suite of synthetic Integral Field Unit (IFU) data cubes, produced from simulations, to quantify the said effect of spatial resolution. I will finish by demonstrating our novel method of correcting existing measurements of nearby galaxies, for their insufficient spatial resolution and signal-to-noise levels. Our method will be crucial for planning high-redshift IFU surveys with future telescopes. |
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