No evidence for a significant evolution of M_dot-M_star relation up to z ~ 4

Over the past two decades, tight correlations between black hole masses ($M_{\bullet}$ ) and their host galaxy properties have been firmly established at $\mathrm{low}-z$ ($z < 1$ ), indicating coevolution of supermassive black holes and galaxies. However, the situation at $\mathrm{high}-z$ , especially beyond cosmic noon ($z \gtrsim 2.5$ ), is controversial. With a combination of JWST NIRCam/wide field slitless spectroscopy (WFSS) from FRESCO, CONGRESS and deep multi-band NIRCam/image data from JADES in the GOODS fields, we study the black hole to galaxy mass relation at $z \sim 1-4$ . After identifying $18$ broad-line active galactic nuclei (BL AGNs) at $0.9 < z < 3.6$ (with $8$ at $z > 2.5$ ) from the WFSS data, we measure their black hole masses based on broad near-infrared lines ($\mathrm{Pa}\alpha$ , $\mathrm{Pa}\beta$ , and $\mathrm{HeI}\lambda10833\,\mathrm{\AA}$ ), and constrain their stellar masses ($M_{\ast}$ ) from AGN-galaxy image decomposition or SED decomposition. Taking account of the observational biases, the intrinsic scatter of the $M_{\bullet}-M_{\ast}$ relation, and the errors in mass measurements, we find no significant difference in the $M_{\bullet}/M_{\ast}$ ratio for $2.5 < z < 3.6$ compared to that at lower redshifts ($1 < z < 2.5$ ), suggesting no evolution of the $M_{\bullet}-M_{\ast}$ relation up to $z \sim 4$ .

eprint arXiv:2409.06796