The co-evolution of star-forming galaxies and their supermassive black holes across cosmic time
Creators: name: Calhau, Joao
Publisher: name: Lancaster University
Year: 2020

description: It is now generally accepted that galaxies host supermassive black holes in their centres. Observational evidence for a correlation between the supermassive black hole and the host galaxy properties are numerous, such as the relation between the mass of the black hole and the mass of the galaxy's bulge (M<sub>BH</sub>-M<sub>bulge</sub> relation) and between the black hole mass and the velocity dispersion of a galaxy (M<sub>BH</sub>-σ relation). However, attempts at correlating the growth of galaxies (star formation rate - SFR) with the growth of their supermassive black holes (black hole accretion rate - BHAR) yield conflicting results, depending on the properties of the selected sample. Furthermore, most samples used when studying the activity of SMBHs are taken from AGN-selected populations, which may introduce biases by restricting the studies to only high luminosity/high accreting sources. This thesis takes an alternative approach and probes the relation between the SFR and BHAR for samples of star-forming galaxies across cosmic time from z~0.4 to z~6. It makes use of the High Redshift Emission Line Survey (HiZELS) and the Slicing COSMOS with 4000 Lyman-α emitters (SC4K survey) to select a large sample of line-emitting star-forming galaxies (672 Hα emitters - HAEs - at z=0.4-2 for HiZELS and 3700 Lyman-α emitters - LAEs - at z=2-6 for SC4K). Making use of stacking and SED fitting techniques, as well as direct source extraction by using the publicly available data in the X-rays, radio and FIR bands for the COSMOS field, this work estimates the BHARs and SFRs of star-forming galaxies and provides additional information on the SMBH/SF processes of star-forming galaxies across cosmic time. The results show that most star-forming galaxies at z&lt;2 do not have AGN activity of note (average BHAR=0.001-0.01 M<sub>sun</sub> yr<sup>-1</sup>) with SFRs ranging from 2 M<sub>sun</sub> yr<sup>-1</sup> at z=0.4 to 40 M<sub>sun</sub> yr<sup>-1</sup> at z=2.23, which means HAEs grow approximately 1000 times faster than their SMBHs. This BHAR/SFR ratio shows little to no evolution with redshift and has very little dependence on galaxy mass. Lyα emitters at higher redshifts (z=2-6) are also shown to be mostly star-forming galaxies with only ~6.8% being detected in the X-rays. The X-ray luminosity of LAEs correlates with Lyα luminosity, suggesting Lyα acts as a tracer of black hole accretion. However this only happens for X-ray detected LAEs and most LAEs do not show this correlation. Most LAEs (~93%) are not detected in the X-rays, even when stacking, and have BHAR&lt;0.017 M<sub>sun</sub> yr<sup>-1</sup>. Only ~3% of LAEs are detected in the radio and their 1.4 GHz luminosity is consistent with AGN sources. However, no correlation with Lyα is found. In further contrast with the X-ray results, there are significant detections (&gt;3σ) when stacking in the radio while excluding direct detections, allowing for the use of radio as an additional SFR estimator. The results from radio are found to be consistent with FIR and Lyα results (total median SFR~7.2 M<sub>sun</sub> y<sup>-1</sup>). The BHAR/SFR ratio of LAEs (log10(BHAR/SFR)&lt;-2.7) is comparable to that of lower redshift HAEs (log10(BHAR/SFR)=-3.3) and sets a trend where star-forming galaxies grow approximately 1000 times faster than their SMBHs. This thesis results are therefore consistent with a scenario of co-evolution between supermassive black holes and their host galaxies.