“School of Astronomy”
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| Paper IPM / Astronomy / 18193 |
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Galactic gas contains atomic hydrogen (HI), which is crucial to numerous astrophysical phenomena. Studying the HI atomic gas in and around galaxies is very important to investigate the physical conditions under which massive star formation is quenched throughout cosmic time and to examine the feeding and feedback scenario in the conventional models of galaxy history. The first practical chance to investigate the unexplored field of HI in higher redshift galaxies is provided by sensitive SKA measurements. We model the HI maps of high-z galaxies whose SFR and current HI emission properties resemble those of neighboring galaxies like M51. In order to explore the possibilities of suggested surveys for mapping HI at high-z in this galaxy, the simulations utilize SKA configurations and sensitivities. Furthermore, throughout the redshift range of 0.15 < z < 3, the study also models the evolution of thermal and non-thermal radio continuum (RC) emission on kpc scales. This study aims to investigate: a) the thermal and non-thermal emission structures on kpc scales; b) the evolution of the synchrotron spectrum and thermal portion at mid-radio frequencies; and c) the detection capacity of RC emitting structures using the SKA1-MID reference survey.
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