Table 2.
Overview of various literature studies on SMBH masses MBH at high redshift.
| Study | Sample | Line | Calibration | Virial | Width | Dust- | Redshift |
|---|---|---|---|---|---|---|---|
| size | factor f | definition | corr.? | range | |||
| Maiolino et al. (2024) | 12 | Hα | Reines & Volonteri (2015) | 4.3 | Broad FWHM | Yes | 4 < z < 7 |
| Harikane et al. (2023) | 10 | Hα | Greene & Ho (2005) | 0.75 | Broad FWHM | Yes | 4 < z < 7 |
| Farina et al. (2022) | 38 | Mostly Mg II | Shen et al. (2011) | 1.4 | Total FWHM | No | 5.8 < z < 7.5 |
| Yue et al. (2024a) | 6 | Hβ | Vestergaard & Peterson (2006) | 1.4 | Total FWHM | No | 5.9 < z < 7.1 |
| Stone et al. (2024)(a) | 5 | Hβ | Vestergaard & Peterson (2006) | 1.4 | Total FWHM | No | z ∼ 5 − 7 |
| Übler et al. (2023) | 1 | Hα | Reines et al. (2013) | 1.075 | Broad FWHM | No | z ∼ 5.6 |
| Juodžbalis et al. (2024) | 1 | Hα | Reines et al. (2013) | 1.075 | Broad FWHM | Both | z ∼ 6.7 |
| Pensabene et al. (2020)(b) | 10 (c) | Mostly Mg II | Bongiorno et al. (2014) | Various | 2 < z < 7 | ||
| Willott et al. (2017)(b) | 21 (c) | Mostly Mg II | Various (literature compilation) | z > 5.7 | |||
| Kocevski et al. (2023) | 2 | Hα | (1) Modified Kaspi et al. (2000)(d) | 0.75 | Broad FWHM | No | z > 5 |
| (2) Greene & Ho (2005) | 0.75 | Broad FWHM | Both | ||||
| Ding et al. (2023) | 2 | Mostly Hβ | Vestergaard & Peterson (2006) | 1.4 | Broad FWHM | No | z > 6 |
| SHELLQs (e,a,b) | 5 (f) | Mg II | Vestergaard & Osmer (2009) | 1.4 | Total FWHM | No | z ∼ 6 |
Notes. For each study, we list the number of sources, the broad line used as a tracer, the underlying virial MBH calibration, and the adopted value for the virial factor f (accounting for the BLR geometry). Columns 6 and 7 specify whether the line width was evaluated based on the FWHM of the total line profile or the broad component, and whether a dust correction has been applied (affecting the luminosity-inferred BLR size). In the last column, we list the redshift range probed. The three parts of the table group together studies finding evidence for over-massive BHs with respect to their hosts, mixed results, or BH masses in line with local scaling relations.
One source, J2239+0207, was included both in Stone et al. (2024) and the SHELLQs sample in Izumi et al. (2019).
Evaluated w.r.t. the relation between BH mass and [C II]-inferred host dynamical mass, rather than stellar mass. See also Willott et al. (2017).
One source, PSO J167-13, was studied both in Willott et al. (2017) and Pensabene et al. (2020).
Substituting Hβ for Hα and using the FWHM of the broad component rather than the total line profile.
Izumi et al. (2018, 019, 2021). Izumi et al. (2021) also presents a literature compilation of ∼20 higher-luminosity AGNs with Mg II-based virial MBH and [C II]-based dynamical mass measurements, which favour an offset from local scaling relations.
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