Multi-phase investigation of outflows in the circumgalactic and interstellar media of luminous quasars at z~5

Chiara Feruglio; George Becker; Guido Cupani; Manuela Bischetti; Matilde Brazzini; Roberta Tripodi; Valentina D'Odorico

REVIEW 3 major objections 5 minor 1 cited by

Multi-phase investigation of outflows in the circumgalactic and interstellar media of luminous quasars at z~5

T0 review · 3 major / 5 minor · reviewed 2026-08-16 · deepseek-v4-flash

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Pith's one-line read At $z\sim5$ the most luminous quasars still harbour overmassive black holes and drive outflows reaching roughly 48,000 km/s, indicating that the $z>6$ efficient feedback phase continued into the post-reionisation epoch.

desk verdict A solid, careful absorption+emission outflow study at z~5 with a genuinely new catalogue and correlation; the overmassive-BH claim should be treated as tentative because it rests on four marginally resolved sources and a fixed inclination. read the letter →

arxiv 2504.20136 v1 pith:HYJUBRT7 submitted 2025-04-28 astro-ph.GA

Matilde Brazzini , Valentina D'Odorico , Manuela Bischetti , Chiara Feruglio , Guido Cupani , George Becker , Roberta Tripodi This is my paper · ORCID

classification astro-ph.GA

keywords quasaroutflowsbroadabsorptionlinesnarrowCIVandNVblackhole–hostgalaxymassrelationz≈5quasars[CII]158μmemissionEddingtonratio

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

This paper aims to show that the violent black-hole-feedback regime seen in quasars at $z\gtrsim6$ was still operating at $z\sim5$, a few hundred million years later. It analyses 39 luminous quasars at $z=5\text{--}5.7$, combining narrow C IV and N V absorption doublets, broad absorption troughs, UV emission-line fits, and [C II] 158\,\text{\mu m} emission from ALMA to trace outflows and to weigh black holes against their host galaxies. The central claims are that these quasars lie above the local black-hole\,--\,host-galaxy mass relation, drive ionised outflows reaching almost 48,000 km/s, and show a statistical link between emission-side outflow indicators and absorption-side detections. If correct, the result extends the efficient early-feedback phase down to $z\sim5$ and makes narrow absorption lines usable as outflow tracers at high redshift.

What carries the argument

The argument is carried by four matched tracers. (1) Voigt-profile fits to C IV and N V narrow absorption doublets within 10,000 km/s of the systemic redshift, where N V marks the systems most likely to be intrinsic to the quasar; (2) the balnicity index, a velocity-integrated measure of broad troughs deeper than 10% of the continuum over contiguous 2000 km/s intervals, which sets the BAL outflow velocities; (3) single-epoch virial black-hole masses from Mg II and C IV, together with C IV\,--\,Mg II velocity shifts and C IV blueshifts as emission-side outflow indicators; and (4) dynamical host masses from spatially resolved [C II] 158\,\text{\mu m} emission, assuming a rotating disk inclined at $i=46^\circ$. The load-bearing link is the C IV\,--\,Mg II velocity shift: quasars with larger shifts are increasingly likely to show absorption outflows, connecting the emission and absorption sides of the same phenomenon.

What would settle it

Map the [C II] kinematics of the four detected sources at higher angular resolution and fit disk models that return the inclination directly. If the fitted inclinations cluster well below $46^\circ$, recomputing $M_{\rm dyn}\sin^2 i$ would pull the points toward the local relation and undermine the overmassive claim; if they cluster near $46^\circ$, the claim stands. Independently, monitoring the C IV+N V absorbers for time variability or partial coverage would test whether they are truly intrinsic outflows rather than intervening systems.

Watch

Extended reading notes

Core claim

On its own terms, the paper establishes that $z\sim5$ quasars behave like their $z\gtrsim6$ counterparts: their black holes are overgrown relative to their host galaxies and they drive exceptionally fast ionised winds. The four quasars with [C II]-based dynamical masses fall above the local $M_{\rm BH}$\,--\,$M_{\rm host}$ relation, with $M_{\rm BH}/M_{\rm dyn}$ between 0.007 and 0.047, compared with roughly 0.002 for local galaxies; six quasars show C IV broad absorption lines with maximum velocities up to $\sim48{,}000$ km/s; and 35 of 39 sources have C IV blueshifts above 1000 km/s, with Eddington ratios frequently near or above unity. The absorption statistics add a distinct finding: roughly a third of the quasars host C IV+N V narrow absorption systems in the proximity zone, and the fraction of quasars with any absorption outflow tracer rises above 50% for C IV\,--\,Mg II velocity shifts more negative than $-2000$ km/s. This is taken as evidence that emission and absorption features are different manifestations of the same outflow phenomenon.

Load-bearing premise

The host-galaxy dynamical masses assume every [C II]-emitting disk is inclined at $46^\circ$ to the line of sight, because the sources are only marginally resolved; if the true inclinations are much smaller, the inferred masses rise by up to an order of magnitude and the claimed deviation from the local black-hole\,--\,host relation could shrink or disappear.

Editorial extensions

If this is right

The overmassive-black-hole offset measured at $z\gtrsim6$ persists at $z\sim5$, so black-hole growth outpaced host-galaxy growth over a prolonged early epoch.
Ionised outflows with velocities up to $\sim48{,}000$ km/s were already present in $z\sim5$ quasars, implying feedback energy injection comparable to the most extreme $z>6$ sources.
Absorption-line statistics can serve as outflow tracers at high redshift: the detection fraction in absorption exceeds 50% when the C IV\,--\,Mg II velocity shift is more negative than $-2000$ km/s.
C IV+N V narrow absorption systems are preferentially found at small velocity separations and around stronger C IV systems, consistent with an intrinsic, highly ionised outflow origin.
The four [C II]-detected hosts have dynamical masses and sizes consistent with $z\gtrsim6$ quasar hosts, supporting continuity of the host-galaxy population across this redshift gap.

Reading between the lines

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

If the emission\,--\,absorption link is causal, narrow absorption-line statistics could replace expensive emission-line outflow measurements for faint high-redshift AGNs, extending feedback studies to the low-luminosity population.
The apparent deficit of N V absorbers at the highest bolometric luminosities may mean the most powerful quasars over-ionise or clear their circumgalactic gas; a larger sample could turn this hint into a test.
Because the dynamical masses assume a single inclination, the overmassive conclusion is statistically robust only if the true inclination distribution is not dominated by near-face-on disks; higher-resolution kinematics of these four sources would decide.
The rising C IV\,--\,Mg II shift with redshift could partly reflect selection of hyper-luminous quasars, so the claimed evolutionary trend should be re-tested once fainter $z\sim6$ quasars are observed spectroscopically.

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Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note

read the letter

You should know two things about this paper. First, it delivers a genuinely useful new catalogue: 50 associated C IV and 22 N V absorption systems in 39 z~5 quasars, plus BAL identifications and emission-line properties, in a redshift range that has been thinly sampled before. Second, the strongest astrophysical claim—that these quasars lie above the local MBH–Mhost relation—should be read as tentative, because it depends on four [C II]-detected sources with fixed inclination i=46°, and that assumption can be nudged in ways that shrink the offset.

What the paper does well: the absorption-line work is careful and reproducible in spirit. The authors check completeness limits, group components at 200 km/s, compare with XQ-100 and XQR-30, validate their [C II] measurements against independent reductions, and are transparent about systematic uncertainties (0.5 dex on MBH and Mdyn). The new correlation between absorption outflow detection fraction and C IV–Mg II velocity shift is interesting and, as far as I can tell, not an artifact of prior definitions. The sample overlap with XQz5 is handled honestly, and the mass comparison to Lai et al. is a fair sanity check. None of this is revolutionary, but it is solid work in an under-explored regime.

Soft spots, in order of concern. First, the 48,000 km/s BAL velocity comes from one object where the SDSS composite template is a poor match to the quasar's extreme C IV wing. The authors acknowledge the mismatch but do not test whether the maximum velocity survives a different continuum choice. That should be checked before the number enters the literature as fact. Second, the key correlation plot (Fig. 13) has no error bars on the binned absorption fractions; a Poisson interval or a simple significance test would make the trend persuasive rather than suggestive. Third, the inclination issue. The paper's defense—that erasing the offset would require all quasars to be nearly face-on—is too strong. The stress-test note is right: under a random-disk prior, you expect roughly one of four sources to have i below ~20°, and that alone moves a point by 0.5–0.8 dex in dynamical mass. With the paper's own 0.5 dex systematic, the offset could be substantially weakened. This does not kill the paper, but it means the z~5 version of the 'overmassive black hole' claim is currently a suggestion, not a measurement. The paper itself says 'tentatively claim' in Sec. 6.2; the abstract states it more firmly, and that mismatch should be reconciled.

Citation pattern: abundant self-citations, but to the same program's earlier work (Bischetti, D'Odorico, Perrotta, Davies), and the central statistics are computed directly from the data. No circularity worries.

Who this is for: anyone working on high-redshift quasar outflows, absorption systems, or BH-host coevolution. It deserves a serious referee. My recommendation: send it to peer review, but ask for (1) a robustness test of the extreme BAL velocity against an alternative continuum template, (2) error bars or a significance statement on the binned correlation, and (3) a revised discussion of how inclination uncertainty affects the mass-offset conclusion—preferably folding the inclination prior into the plotted Mdyn scatter.

Referee Report

3 major / 5 minor

Summary. This paper presents a multi-phase outflow study of 39 luminous quasars at z=5–5.7 using VLT/X-Shooter UV/optical spectra and archival ALMA [C ii] data for six objects. The authors build a catalogue of associated C iv and N v narrow absorption line systems within 10,000 km/s of the systemic redshift, identify six C iv BAL quasars with maximum outflow velocities up to ~49,000 km/s, derive black hole masses, bolometric luminosities, and Eddington ratios from Mg ii and C iv emission, and use the four [C ii]-detected sources to estimate dynamical masses. They report that z~5 quasars lie above the local MBH–Mhost relation, similar to z>6 quasars, and that the fraction of quasars with absorption-line outflow tracers increases with the C iv–Mg ii velocity shift, suggesting a link between emission- and absorption-selected outflows.

Significance. If the results hold, the paper extends the overmassive-black-hole and powerful-outflow phenomena from z>6 down to z~5, a redshift range that is still sparsely sampled. The associated absorber catalogue is a valuable resource, and the comparison with XQ-100 and XQR-30 samples is informative. The paper is careful in validating redshifts against [C ii] where possible, cross-checking ALMA reductions with independent analyses, and propagating systematic uncertainties on black hole masses. The absorption-line statistics are computed directly from the data, and the correlation between absorption-line outflow tracers and the C iv–Mg ii velocity shift is a new, testable result.

major comments (3)

[Sec. 5.2, Eq. (6); Sec. 6.2] The claim that the four z~5 quasars lie above the local MBH–Mhost relation rests on dynamical masses computed with a fixed inclination i=46° for sources that are only marginally resolved. The robustness argument in Sec. 6.2 is too strong: it envisions erasing the offset only if all high-redshift disks are nearly face-on, but with a random-disk prior the probability that at least one of four sources has i<21° is about 24%, and for i=15–20° Mdyn increases by 0.6–0.9 dex, comparable to the 0.5 dex systematic uncertainty assigned to Mdyn. This is enough to move at least one or two of the four points onto or within the scatter of the local relation. The paper should present the MBH–Mdyn offset as a function of inclination (e.g., a Monte Carlo drawing inclinations from a random-disk prior and from the Wang et al. 2024 resolved-sample distribution) and state how many sources remain inconsistent with the local relation under plausible inclination values. Without this, the Sec. 7 conclusion about efficient feedback at z~5 is not yet supported.
[Sec. 5.2, Table 5] The relation between the tabulated Mdyn and Mdyn sin^2 i columns is internally inconsistent. For i=46°, sin^2(46°)=0.517, so Mdyn/(Mdyn sin^2 i) should equal 1.93 for every source; the reported ratios are 1.37 (J0131-0321), 2.14 (J0306+1853), 1.26 (J2207-0416), and 1.15 (J1335-0328). This suggests either different inclination values were used, a numerical error in one column, or an inconsistency in the conversion from Eq. (6). Since Fig. 12 and Sec. 6.2 use these Mdyn values, the authors must correct or clarify this before the dynamical-mass comparison can be assessed.
[Sec. 2.5 and Table 2] The headline maximum BAL velocity of 48,670 km/s for J1004+2025 is derived by comparing the observed spectrum with an SDSS composite template matched to quasars with relatively normal C iv profiles. For an object with an extreme C iv blueshift and a prominent blue wing, the template may not reproduce the intrinsic continuum at the wavelengths of the BAL trough; the paper asserts that the mismatch lies outside the absorption region, but no quantitative sensitivity test is shown. I request an explicit check of how vmax and BI for J1004+2025 (and J1601-1828) change under alternative continuum models, for example power-law continua of varying slope or templates selected to include stronger C iv blueshifts. Without such a test, the 'up to 48,000 km/s' claim is not fully quantified.

minor comments (5)

[Sec. 4 and Table 4] The text states '35 C iv absorption systems with vabs ≤ 5500 km/s', but Table 4 gives 25+9=34 systems in this range; the corresponding N v fraction is therefore 19/34≈56%, not ~54%.
[Table 1] The Mg ii transition wavelength should read λ2803.531 Å; as printed, 'λ280.531 Å' is missing a digit.
[Table B.1 and Sec. 5.1] For J1335-0328 the text says the redshift comes from the [C ii] line, while the table note (b) attributes the redshift to the Lyα forest; please make these consistent.
[Sec. 2.1] The phrase 'S/N per pixel of 10 km/s' should be rephrased as 'S/N per 10 km/s pixel' for clarity.
[Abstract and Sec. 2.5] The abstract quotes '48,000 km/s' while Sec. 2.5 and Table 2 report '~49,000 km/s' (48,670 km/s); please standardize the rounding.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the absorption statistics, BAL velocities, and black-hole/host comparison are measured from the data using externally published calibrations; the fixed i=46° assumption is a stated systematic limitation, not a fitted input.

full rationale

The claimed derivation chain is not circular. NAL identification uses doublet detection, Voigt-profile fitting, and 3σ column-density limits (Eqs. 2–3) directly on the X-Shooter spectra. BAL identification uses the balnicity index (Eq. 4) with empirical SDSS composite templates (Bischetti et al. 2022, 2023); those templates are external, data-based, and are not re-fit to force the BAL velocities. Black-hole masses and bolometric luminosities use published single-epoch virial relations and bolometric corrections (Vestergaard & Osmer 2009; Vestergaard & Peterson 2006; Richards et al. 2006) with stated 0.5 dex and 0.3 dex systematics. Dynamical masses use Eq. 6 with i=46° adopted from the resolved z>6 host sample of Wang et al. (2024); this is an externally motivated assumption, not a parameter chosen to make the four sources lie above the local relation. The paper explicitly flags the resulting systematic uncertainty and discusses the inclination sensitivity in Sec. 6.2, so the overmassive claim is a robustness-sensitive measurement, not a definitional artefact. The absorption–emission correlation in Sec. 6.3 and Fig. 13 is computed from measured C iv–Mg ii velocity shifts and detected absorption systems; the 'intrinsic' classification of C iv+N v NALs is an assumption supported by the independent XQ-100/XQR-30 catalogues (Perrotta et al. 2016, 2018; Davies et al. 2023), not by a circular fit. Self-citations are present, but they supply methods and calibrations validated on independent data and do not carry the target claims by themselves. No predicted quantity is equal by construction to an input quantity.

Assumptions & free parameters 1 free parameters · 6 assumptions · 0 invented entities

The paper adopts standard scaling relations and templates from the literature. The only parameter central to the results that is not directly measured is the inclination angle, which strongly affects dynamical masses. The key domain assumptions (virial relations at z~5, intrinsic NAL classification, template-based BAL continuum) are explicitly stated and are the main sources of systematic uncertainty.

free parameters (1)

Inclination angle i = 46 degrees (adopted)
Used in Eq. 6 for Mdyn sin^2 i; directly affects the claimed offset from the local MBH-Mhost relation. The value is a median from z>6 resolved quasars (Wang et al. 2024), not fitted to these data.

assumptions (6)

domain assumption Virial scaling relations for Mg II and C IV (Vestergaard & Osmer 2009; Vestergaard & Peterson 2006) are valid at z~5
Used to derive MBH from line FWHM and continuum luminosity (Sec 5.1); these relations are calibrated locally and may evolve with redshift.
domain assumption The bolometric correction from Richards et al. (2006) applies to z~5 quasars
Used to convert L3000 to Lbol (Sec 5.1); a mean SED is assumed, with 0.3 dex systematic.
domain assumption [C II] emission traces a rotating disk whose dynamical mass follows Eq. 6 with a single fixed inclination
Sec 5.2; used for Mdyn and the MBH-Mdyn comparison. The sources are marginally resolved, so inclination cannot be measured directly.
domain assumption SDSS non-BAL composite templates represent the intrinsic quasar continuum for BAL identification
Sec 2.5; BAL troughs and velocities (including the 48,000 km/s extreme) are defined relative to these templates.
domain assumption Associated CIV+N V NALs within 10,000 km/s are intrinsic to the quasar and trace outflows
Sec 6.3; only three of nineteen systems show partial coverage; the rest are classified intrinsic by proximity and high ionization.
standard math Standard ΛCDM cosmology from Planck
Used for distances and luminosities.

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Cite this review

Pith. "Pith review of Multi-phase investigation of outflows in the circumgalactic and interstellar media of luminous quasars at z~5." pith.science (2026). https://pith.science/paper/HYJUBRT7

@misc{pith2026250420136,
  author       = {Pith},
  title        = {Pith review of: Multi-phase investigation of outflows in the circumgalactic and interstellar media of luminous quasars at z~5},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/HYJUBRT7}},
  note         = {Machine review of arXiv:2504.20136}
}

abstract

Aims. Outflows from active galactic nuclei are invoked as the principal feedback process regulating the co-evolution of supermassive black holes and their host galaxies. Because of their multi-phase and multi-scale nature, an exhaustive description of these winds should exploit multiple tracers. However, connecting various outflow features remains a challenge. The aim of this work is to provide a complete characterisation of outflows in a sample of z$\sim$5 quasars, by exploiting the combination of different emission and absorption tracers. Methods. We analysed the UV/optical and FIR continuum, line emission, and absorption in a sample of 39 z$\sim$5 quasars observed with VLT/X-Shooter and ALMA (available for six objects). We identified broad and narrow absorption lines associated with the quasar and emission lines to determine black hole masses and bolometric luminosities. Results. Our sample encompasses massive (log($M_{\text{BH,MgII}}/M_\odot$) = 8.5-10) and luminous (log($L_{\text{bol}}$/(erg/s)) = 46.9-48) quasars at redshift 5-5.7. They display powerful ionised outflows detected in both emission and absorption, with velocities exceeding 48,000 km/s in some cases, and lie above the local black hole - host galaxy mass relation, exhibiting a behaviour similar to that of z$\gtrsim$6 quasars. These findings suggest a phase of efficient black hole feedback occurring at redshift z$\gtrsim$6 and likely persisting down to z$\sim$5, characterised by rapid black hole growth exceeding that of the host galaxy. The fraction of quasars with outflow detections in absorption is higher for larger CIV-MgII velocity shifts, suggesting that while the physical mechanisms powering the two outflow phenomena detected in emission and absorption may differ, a correlation exists between them.

Figures

Figures reproduced from arXiv: 2504.20136 by the authors.

**Figure 1.** Example of a typical X-Shooter spectrum from our quasar sample, covering the 560–1850 nm observed range, reported in [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗

**Figure 2.** Best-fit decomposition of Civ (upper panel) and Mg ii (lower panel) spectral regions for J2226-0618. The blue line is the power law continuum, the orange line is the Fe ii template, green dashed lines show Gaussian components. The Si iv emission line at ∼ 1400 Å is masked during the fitting procedure. velocity at which two absorbers are assumed to be physically bound or, in other words, part of the same physical sy… view at source ↗

**Figure 3.** Spectra of the six BAL quasars in our sample and two non-BAL quasars (bottom panels) reported for comparison. Quasar [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗

Figures from the paper (9 more)

**Figure 4.** Figure 4: Two-dimensional velocity-integrated [Cii] line emission maps (upper panels) and spectral profiles (lower panels) for the six analysed sources from [PITH_FULL_IMAGE:figures/full_fig_p007_4.png]

**Figure 5.** Figure 5: For each quasar of the sample, the C iv forest (light blue) and proximity zone (dark blue) are shown. Intrinsic absorbers are reported in different colours according to the different transitions. In particular, we highlight C iv+N v absorbers in yellow, Civ absorbers i…

**Figure 6.** Figure 6: Properties of Civ (red histograms) and Civ+N v (golden histograms) absorption systems. From top to bottom, distribution of absorber velocities, C iv column densities, Civ equivalent widths. confirming that the Si iv doublet alone is not a reliable tracer of ionised ou…

**Figure 8.** Figure 8: Bolometric luminosity versus redshift distribution for our [PITH_FULL_IMAGE:figures/full_fig_p010_8.png]

**Figure 10.** Figure 10: Black hole masses versus bolometric luminosities. The [PITH_FULL_IMAGE:figures/full_fig_p011_10.png]

**Figure 11.** Figure 11: Distribution of the logarithmic Eddington ratio, [PITH_FULL_IMAGE:figures/full_fig_p011_11.png]

**Figure 12.** Figure 12: Black hole mass from Mg ii versus dynamical mass for our four quasars with [C ii] S/N ≥ 5 detections (teal data points) and for other high-redshift quasars from various literature works (golden data points; Feruglio et al. 2018; Pensabene et al. 2020; Neeleman et al. …

**Figure 13.** Figure 13: Comparison of Civ FWHM and C iv-Mg ii velocity shift for our sample, for the z > 5.8 quasars from Schindler et al. (2020), and for the SDSS DR7 quasars from Shen et al. (2011), for which the Civ-Mg ii velocity shifts are calculated in Shen et al. (2016). The quantitie…

**Figure 14.** Figure 14: Mean Civ-Mg ii velocity shift as a function of redshift from Mg ii for our quasar sample (teal diamond), for the z > 5.8 dataset from Schindler et al. (2020), further divided into two redshift bins at z ≷ 6.35, and for a compilation of different samples collected in …

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