2025ApJ...978...98S

Over the past two decades, tight correlations between black hole masses (M_•) and their host galaxy properties have been firmly established for massive galaxies (with stellar mass $\mathrm{log}({M}_{* }/{M}_{\odot })\gtrsim 10$) at low-z (z < 1), indicating coevolution of supermassive black holes and galaxies. However, the situation at high-z, especially beyond cosmic noon (z ≳ 2.5), is controversial. With a combination of JWST Near Infrared Camera (NIRCam)/wide field slitless spectroscopy (WFSS) from FRESCO, CONGRESS and deep multiband NIRCam/image data from JADES in the GOODS fields, we study the black-hole-to-galaxy mass relation at z ∼ 1-4. After identifying 18 broad-line active galactic nuclei (AGNs) at 1 < z < 4 (with 8 at z > 2.5) from the WFSS data, we measure their black hole masses based on broad near-infrared lines (Paα, Paβ, and He Iλ10833 Å), and constrain their stellar masses from AGN-galaxy image decomposition or spectral energy distribution decomposition. Taking account of the observational biases, the intrinsic scatter of the M_•-M_* relation, and the errors in mass measurements, we find no significant difference in the M_•/M_* ratio for 2.5 < z < 4 compared to that at lower redshifts (1 < z < 2.5), suggesting no evolution of the M_•-M_* relation at $\mathrm{log}({M}_{* }/{M}_{\odot })\gtrsim 10$ up to z ∼ 4.