No Evidence for a Significant Evolution of M<sub>•</sub>–M. Relation in Massive Galaxies up to z ∼ 4
Yang Sun, Jianwei Lyu, G. H. Rieke, Zhiyuan Ji, Fengwu Sun, Yongda Zhu, Andrew J. Bunker, Phillip A. Cargile, Chiara Circosta, Francesco D’Eugenio, Eiichi Egami, Kevin Hainline, Jakob M. Helton, Pierluigi Rinaldi, Brant Robertson, Jan Scholtz, Irene Shivaei, Meredith A. Stone, Sandro Tacchella, Christina C. Williams, Christopher N. A. Willmer, Chris J. Willott
Abstract
Abstract 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 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>log</mml:mi> <mml:mo stretchy="false">(</mml:mo> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>*</mml:mo> </mml:mrow> </mml:msub> <mml:mrow> <mml:mo stretchy="true">/</mml:mo> </mml:mrow> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> <mml:mo stretchy="false">)</mml:mo> <mml:mo>≳</mml:mo> <mml:mn>10</mml:mn> </mml:math> ) 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 (Pa α , Pa β , and He i λ 10833 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 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>log</mml:mi> <mml:mo stretchy="false">(</mml:mo> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>*</mml:mo> </mml:mrow> </mml:msub> <mml:mrow> <mml:mo stretchy="true">/</mml:mo> </mml:mrow> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>⊙</mml:mo> </mml:mrow> </mml:msub> <mml:mo stretchy="false">)</mml:mo> <mml:mo>≳</mml:mo> <mml:mn>10</mml:mn> </mml:math> up to z ∼ 4.