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A prevalent population of normal-mass central black holes in high-redshift massive galaxies

T0 review · 3 major / 5 minor · reviewed 2026-08-08 · deepseek-v4-flash

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Pith's one-line read A galaxy-based search at z~3-5 finds thirteen broad-line AGNs whose black holes average about 0.1% of their host stellar mass, matching local galaxies and showing that normal-mass black holes were common in the early Universe.

desk verdict First direct sample of normal-mass BHs at z~3-5, but the prevalence claim outstrips the unquantified selection function. read the letter →

arxiv 2502.05048 v1 pith:RANZ2VFA submitted 2025-02-07 astro-ph.GA

Junyao Li , Yue Shen , Ming-Yang Zhuang This is my paper · ORCID
classification astro-ph.GA
keywords supermassiveblackholeshole-hostgalaxyscalingrelationsbroad-lineAGNshigh-redshiftgalaxiesgalaxy-basedselectionvirialholemassestimatorquiescentseeding
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

Previous high-redshift black hole samples were mostly found by first spotting a bright active nucleus, which skews the census toward overmassive black holes. This paper reports thirteen broad-line active galactic nuclei discovered by starting from 52 massive galaxies at $z\sim3-5$, without requiring the black hole to outshine its host. These black holes have masses of about 0.1% of their host stellar mass, matching the local ratio, and their hosts are mostly already quenched. The paper concludes that normal-mass black holes were already common in the early Universe, so the early Universe contained both overmassive and ordinary black holes.

What carries the argument

The load-bearing measurement chain is the galaxy-based selection combined with the H$\alpha$ single-epoch virial estimator, a mass formula that converts the width and luminosity of a single broad emission line into a black hole mass using local calibrations. The selection inverts the usual approach: instead of picking AGNs by luminosity, which biases toward overmassive black holes, it starts with massive galaxies and searches for broad H$\alpha$ with FWHM $>1000$ km s$^{-1}$, ruling out outflow broadening with fits to [O III] and [S II]. Black hole masses come from Eq. (1), $\log (M_{\rm BH}/M_\odot)=6.57+0.47\log(L_{H\alpha}/10^{42}\,{\rm erg\,s^{-1}})+2.06\log({\rm FWHM}/1000\,{\rm km\,s^{-1}})$, and bolometric luminosities from the H$\alpha$-to-5100 Å continuum relation. Star formation histories reconstructed from SED fitting allow the authors to back-trace stellar masses to higher redshift and place upper limits on $M_{\rm BH}/M_\star$ at $z\sim5.7$, connecting the sample to the first billion years.

What would settle it

Reverberation-map or spectroastrometrically measure the broad-line region size in a few of these $z\sim3-5$ AGNs; if the H$\alpha$ radius-luminosity relation differs from the local calibration by more than about 0.3 dex, the virial masses from Eq. (1) would shift systematically and the 0.1% mean ratio could move away from the local value.

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Extended reading notes

Core claim

Starting from a galaxy-based parent sample of 52 spectroscopically confirmed massive galaxies ($M_\star > 10^{10}\,M_\odot$) at $z\sim3-5$ across six deep fields, the authors identify 14 broad-line AGNs, 13 of which are moderate-luminosity with black hole masses $\log (M_{\rm BH}/M_\odot)\sim6.6-8.1$. Using the H$\alpha$ single-epoch virial estimator, they find a mean black-hole-to-stellar mass ratio of about 0.1%, consistent with the local $M_{\rm BH}-M_\star$ relation, and a lower limit of about 27% (14/52) for the broad-line AGN fraction in their massive galaxy sample. Because most hosts assembled most of their stars before $z\sim5$ and are now quenched, the authors argue that this normal-mass black hole population was already in place when the Universe was roughly one billion years old, coexisting with the overmassive black holes seen in little red dots (compact, AGN-dominated galaxies) and luminous quasars. The paper therefore claims that the high-redshift black hole population is diverse and that previous overmassive-only samples were biased by AGN luminosity selection.

Load-bearing premise

The load-bearing premise is that the locally calibrated H$\alpha$ black-hole mass formula applies to these $z\sim3-5$ sources without a systematic offset, a point the paper itself flags as uncertain.

Editorial extensions

If this is right

  • A census of black holes at $z\sim3-5$ based purely on AGN luminosity misses the majority of the population, since these normal-mass AGNs are faint in the continuum but dominate in line emission.
  • The mean black-hole-to-stellar mass ratio shows limited evolution from $z\sim6$ to the local Universe, suggesting the local scaling relation was largely in place within the first billion years.
  • The diversity between overmassive little red dots and quasars on one side and these normal-mass black holes on the other requires multiple formation pathways for early black holes.
  • Massive quiescent galaxies at $z\sim3-5$ can form without an overmassive black hole, since most of the quenched hosts in this sample have $M_{\rm BH}<10^{8.5}\,M_\odot$ and $M_{\rm BH}/M_\star\sim0.1\%$.
  • The normal-mass population sits on the intrinsic relation derived from forward-model bias corrections, supporting the view that the overmassive samples were inflated by selection effects.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If the lower limit of 27% broad-line AGN fraction holds across the full massive-galaxy population, the co-moving number density of active black holes at $z\sim3-5$ is much higher than luminous quasar surveys imply, so seeding and growth models will need to reproduce a more abundant low-luminosity population.
  • The quenched hosts with low-mass black holes imply that quenching can precede or occur without substantial black hole growth; a direct test would measure outflow kinematics and radio-mode feedback in these galaxies.
  • The back-tracing argument predicts an observable population of normal- or undermassive black holes at $z>6$ inside actively star-forming hosts, where the AGN and stellar light are harder to separate; deeper rest-frame optical spectroscopy could find them.
  • A joint demographic fit of the overmassive and normal-mass populations could constrain the fraction of heavy-seed versus light-seed formation channels, rather than interpreting either population alone as representative of early black hole growth.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 5 minor

Summary. The paper presents a galaxy-selected search for broad-line AGNs among 52 massive (M* > 10^10 M_sun) spectroscopically confirmed galaxies at z~3-5 drawn from six JWST deep fields. Fourteen BLAGNs are identified through a careful decomposition of the H-alpha + [NII] + [SII] region, with outflow alternatives explicitly tested. For the 13 relatively faint BLAGNs, the authors derive black hole masses from the single-epoch H-alpha virial estimator and stellar masses from CIGALE SED fitting that includes AGN components. They report a mean MBH/M* ratio of ~0.1%, consistent with the local relation, and a prevalence of post-starburst/quiescent hosts. The paper argues that previous AGN-selected samples were affected by the Lauer bias, that a significant population of normal-mass BHs existed at z~3-5 and likely at z~6, and that massive galaxy quenching does not require overmassive BHs. It also compares the sample with cosmological simulations and discusses diverse BH seeding pathways.

Significance. If the result holds, it is an important and timely contribution: it provides a galaxy-selected census in the high-stellar-mass, low-BH-mass regime, exactly where the Lauer bias has made previous samples incomplete. The strengths of the paper are substantial: the spectral decomposition is detailed, with quantitative BIC comparison of BLR versus outflow models; the two independent Lbol estimates agree well; literature samples are recalibrated to the same virial recipe; and the authors state their caveats explicitly and test SED modeling choices. The core existence claim—that normal-mass BHs exist in massive galaxies at z~3-5—is well supported. The more ambitious prevalence claim, however, rests on the representativeness of a heterogeneous parent sample whose selection function is acknowledged to be unquantified. This is the main load-bearing weakness and prevents the title's 'prevalent' from being fully established.

major comments (3)
  1. [Methods, 'Identifying massive galaxies with SED fitting'; main text 'Although our sample...'] The parent sample of 52 galaxies is an amalgam of more than 20 NIRSpec programs with heterogeneous target selection, and the paper states that 'quantifying the sample selection function is highly challenging.' Because programs such as RUBIES and JADES prioritize red, bright, and rare objects during shutter allocation, the observed BLAGN fraction (14/52, or 13/52 for the normal-mass subset) and the mean MBH/M* of the detected AGNs cannot be assumed to represent the full population of massive galaxies at z~3-5. The abstract's 'prevalent population' and the body's 'significant population' claims require this representativeness step. I request either (a) a quantitative bracketing of the selection effect, for example by comparing the photometric colors and stellar masses of the 52 galaxies with the full ASTRODEEP massive-galaxy sample and reweighting by known target-selection rules, or (b) a clear reframing of the headline claim to existence of normal BHs and their occurrence in quiescent massive galaxies, rather than prevalence. This point is not merely cosmetic: a parent sample biased toward red, quenched, or post-starburst galaxies could systematically favor low-MBH/M* AGNs, as the paper itself entertains.
  2. [Methods, 'Black hole mass and bolometric luminosity of AGNs'; Eq. (1)] The single-epoch H-alpha virial estimator is calibrated on local reverberation-mapped AGNs, and the paper acknowledges that its applicability at z~3-5 is uncertain. The authors correctly note that two alternative recipes would lower MBH by 0.17-0.27 dex, which would not change the qualitative conclusion that these BHs are not overmassive. However, the central quantitative claim—that the mean MBH/M* is 'consistent with the local value'—is stated without a full sensitivity analysis. I ask the authors to recompute the mean MBH/M* and its offset from the local relation under each of the alternative calibrations (e.g., the Dalla Bontà et al. 2024 and Greene & Ho 2005 recipes) and to state whether the 'consistent with local' statement survives the full calibration range. This would bound the systematic error rather than merely noting that it exists.
  3. [Main text, 'Several factors would complicate...' and Fig. 2] The back-tracing of MBH/M* to z=5.7 assumes constant BH mass and uses SFHs from a delayed-tau model, but the quoted change in M* (~0.15 dex) is comparable to the stellar-mass uncertainties from SED fitting (~0.05-0.2 dex for these objects). The statement that the evolution is 'minimal' would be more convincing if the SFH fitting uncertainties were propagated into the back-traced MBH/M* upper limits. As written, the z~6 inference is suggestive but not quantitatively demonstrated at the same level as the z~3-5 result.
minor comments (5)
  1. [Main text, near 'relations bewteen SMBHs and galaxies'] There is a typo: 'bewteen' should be 'between'.
  2. [Methods, 'Spectroscopic data'] The phrase 'In additional to the standard JWST pipeline calibration steps' should read 'In addition to'.
  3. [Methods, 'Photometric data and slit loss correction'] The median correction factors are listed as '1.05, 1.13, 1.08, and 1.31 in F115W, F150W, F277W, and F444W, respectively'; this is fine, but the sentence would be clearer if 'respectively' were placed immediately after the filter list.
  4. [Abstract and main text, 'The derived SMBH masses...'] The abstract reports a mean MBH/M* of ~0.1% without specifying that this is the mean of the 13 faint BLAGNs and excludes 16713-CEERS, which has MBH/M*~10%. The main text is clear, but the abstract could be misread as applying to the full sample; please state the 13-object basis explicitly.
  5. [Fig. 2 caption] The caption says 'T op:' with a stray space; please correct to 'Top:'.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: black hole masses are measured with an external virial estimator and compared against, not fitted to, the local MBH-Mstar relation.

full rationale

The central claim is built from two independently measured quantities: MBH from the H-alpha single-epoch virial estimator (Eq. 1, externally calibrated on local reverberation-mapped AGNs) and Mstar from CIGALE SED fitting of NIRSpec prism spectra plus multi-band photometry. The local MBH-Mstar relation is used only as a comparison baseline, never as a fitting constraint, so the derived mean MBH/Mstar ~ 0.1% is not forced by construction. The paper explicitly tests alternative virial recipes, which lower MBH by 0.17-0.27 dex, and validates the bolometric luminosity decomposition against the CIGALE AGN continuum; these checks bound the main systematic without importing the target result. The only notable self-citation, the authors' prior forward-modeling work (ref. 6), is used as a comparison curve ('our sample aligns with the high-redshift mass relation reported by [6]'), and the present 13 BLAGNs stand as independent data; that citation is neither a uniqueness theorem nor a required input to the mass measurements. The acknowledged non-uniform parent sample and the statement that 'quantifying the sample selection function is highly challenging' limit the prevalence inference, but this is a completeness and representativeness caveat, not a circularity: the existence of normal-mass BHs and their measured mass ratios do not reduce by definition to the paper's conclusions. No equation in the paper sets MBH/Mstar to a fitted value or defines the derived population in terms of the local relation being tested.

Assumptions & free parameters 6 free parameters · 4 assumptions · 0 invented entities

The central claim rests on the virial mass estimator, SED-fitting model choices, and a heterogeneous parent sample. No new physical entities are introduced. The free parameters are measurement pipeline choices, not theory parameters.

free parameters (6)
  • Polar dust extinction AV_polar = 0.44-0.71 mag per object
    Fitted by CIGALE for each source; used to deredden LHα before BH mass calculation, directly affecting MBH.
  • AGN fraction fAGN at 5100 Å = 0.01-0.99 grid, best-fit per object
    Controls the AGN/galaxy decomposition in SED fitting; affects stellar mass and thus MBH/M*.
  • Delayed-τ SFH parameters (e-folding time τ, stellar age) = τ: 0.1-7.0 Gyr, age: 0.1-2.2 Gyr grid
    Used to reconstruct star formation histories and back-trace MBH/M* to z~5.7.
  • Additional error parameter = 15%
    Added to flux errors in CIGALE to absorb systematics; chosen by hand.
  • Polynomial order for prism flux calibration = n=3 default, 0-5 as needed
    Chosen per object to match synthetic photometry; affects stellar continuum shape.
  • Broad-line FWHM threshold = 1000 km/s
    Defines a detection as broad; chosen following prior work.
assumptions (4)
  • domain assumption The broad-line region gas is virialized and the single-epoch Hα mass estimator (Eq. 1) is valid at z~3-5.
    The paper states this is the only consistent approach but notes its high-z applicability is uncertain (Methods, Black hole mass section).
  • domain assumption The SKIRTOR clumpy torus model plus polar dust extinction adequately represent the AGN contribution to the SED.
    CIGALE fitting assumes these templates; a wrong AGN model would bias stellar masses and fAGN.
  • domain assumption The parent galaxy sample, though heterogeneously selected, permits a lower-limit prevalence estimate (14/52) and the existence claim is independent of completeness.
    The paper acknowledges the selection function is hard to quantify (Methods), so prevalence is a lower limit.
  • domain assumption BC03 stellar population models with Chabrier IMF and Calzetti extinction recover stellar masses for these galaxies.
    Standard SED fitting choices; the paper verifies robustness with model variations.

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Cite this review

Pith. "Pith review of A prevalent population of normal-mass central black holes in high-redshift massive galaxies." pith.science (2026). https://pith.science/paper/RANZ2VFA

@misc{pith2026250205048,
  author       = {Pith},
  title        = {Pith review of: A prevalent population of normal-mass central black holes in high-redshift massive galaxies},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/RANZ2VFA}},
  note         = {Machine review of arXiv:2502.05048}
}
read the original abstract

Understanding the co-evolution between supermassive black holes (SMBHs) and their host galaxies provides crucial insights into SMBH formation and galaxy assembly in these cosmic ecosystems. However, measuring this co-evolution, as traced by the black hole mass - stellar mass relation towards the early Universe, often suffers from significant sample selection biases. Samples selected based on the luminosity of the SMBH would preferentially find overly massive black holes relative to their host stellar mass, missing the population of lower-mass SMBHs that are underrepresented. Here we report the discovery of 13 moderate-luminosity broad-line Active Galactic Nuclei from a galaxy-based selection of 52 massive galaxies at z~3-5. The derived SMBH masses for these AGNs yield a mean SMBH-to-stellar mass ratio of ~0.1%, consistent with the local value. There is limited evolution in this mean mass ratio traced back to z~6, indicating that a significant population of ''normal'' SMBHs already existed within the first billion years of the Universe. Combined with the previous sample of overmassive black holes, there must be diverse pathways for SMBH formation in high-redshift galaxies. Most of these galaxies are experiencing star formation quenching by the observed epoch, suggesting the formation of massive quiescent galaxies does not necessarily require an overly massive black hole, contrary to some theoretical predictions.

Discussion (0). Continue with ORCID to comment.

Forward citations

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