The Quasar Feedback Survey: Ionised Outflows in type 2 QSOs with MUSE data

A. Girdhar; C. M. Harrison; C. Ramos Almeida; D. Kakkad; E. P. Farina; F. Arrigoni Battaia; G. Venturi; J. Mullaney; L. Ulivi; M. Bianchin

REVIEW 3 major objections 5 minor 284 references

The Quasar Feedback Survey: Ionised Outflows in type 2 QSOs with MUSE data

T0 review · 3 major / 5 minor · reviewed 2026-08-12 · deepseek-v4-flash

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Pith's one-line read Measuring electron densities from the [Ar IV] doublet in 18 type 2 quasars lowers ionised outflow mass rates and kinetic powers by about an order of magnitude and reveals a positive density–velocity correlation for fast outflows.

desk verdict The 1-dex density correction is solid arithmetic; the n_e-V_out correlation is a promising hint that needs a proper fit. read the letter →

arxiv 2608.08275 v1 pith:EHMM3EBH submitted 2026-08-08 astro-ph.GA

M. Bianchin , C. M. Harrison , T. Costa , V. Mainieri , R. A. Riffel , G. Venturi , D. Kakkad , C. Ramos Almeida

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P. H. Cezar S. Ward A. Girdhar S. Molyneux L. Ulivi E. P. Farina J. Mullaney F. Arrigoni Battaia

This is my paper · ORCID

classification astro-ph.GA

keywords AGNfeedbackionisedoutflowselectrondensitytype2quasars[ArIV]doubletintegralfieldspectroscopykineticcouplingefficiencyquasar-drivenwinds

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 studies ionised gas outflows in 18 luminous, obscured quasars (type 2 QSOs) at redshifts 0.085–0.2 using MUSE integral-field spectroscopy. Its central quantitative claim is that when electron densities are measured from the [Ar IV] 4711,4740 doublet rather than assumed to be 1000 $\mathrm{cm}^{-3}$, the derived outflow mass rates (0.03–4.17 $M_\odot\,\mathrm{yr}^{-1}$) and kinetic powers ($10^{39.25}$–$10^{41.91}$ erg s$^{-1}$) fall by roughly one order of magnitude. The paper also reports a positive correlation between electron density and outflow velocity for velocities above about 630 km s$^{-1}$, which it interprets as compression of the ionised gas clouds by faster outflows. A sympathetic reader would care because outflow mass and energy are the quantities used to judge whether AGN feedback can affect galaxy evolution, and the electron density has been one of the largest uncertainties in those estimates.

What carries the argument

The load-bearing measurement is the [Ar IV] 4711,4740 Å doublet ratio, an electron-density diagnostic for fully ionised gas that is sensitive from roughly $10^2$ to $6\times10^4\,\mathrm{cm}^{-3}$ at an assumed electron temperature of 15,000 K; the ratio is converted to $n_e$ with the PyNeb routine. Because the doublet is detected only in integrated $r=1.5$ arcsecond nuclear spectra, the single resulting density is inserted into the [O III] mass formula $M = 8\times10^7 M_\odot\,(L_{\rm [OIII]}/10^{44}\,\mathrm{erg\,s}^{-1})(n_e/500\,\mathrm{cm}^{-3})^{-1}$ for every outflow spaxel. Outflow spaxels are selected with a per-galaxy $W_{80}$ threshold set from the unresolved nuclear velocity dispersion, and outflow velocities and radii are computed with flux-weighted global and radial peak methods. This chain carries the argument from line ratios to outflow energetics.

What would settle it

A spatially resolved density measurement in outflow spaxels of one of these quasars (for example, with deeper MUSE or JWST/NIRSpec observations that detect [Ar IV] or transauroral [O II]/[S II] lines outside the nuclear aperture) would settle the claim: if densities at kiloparsec radii approach $10^3\,\mathrm{cm}^{-3}$, the roughly one-dex reduction and the $n_e$–$V_{\rm out}$ correlation would not survive.

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Extended reading notes

Core claim

The paper's central discovery is that [Ar IV]-based electron densities in the nuclear regions of these quasars are high (500 to 27,700 $\mathrm{cm}^{-3}$, median about 5,900 $\mathrm{cm}^{-3}$), and that adopting these densities instead of the customary $10^3\,\mathrm{cm}^{-3}$ lowers outflow masses, mass-loss rates, and kinetic powers by about one dex: global mass outflow rates fall to $0.03$–$4.17\,M_\odot\,\mathrm{yr}^{-1}$ and kinetic powers to $10^{39.25}$–$10^{41.91}$ erg s$^{-1}$. It further identifies a positive correlation between $n_e$ and $V_{\rm out}$ for $V_{\rm out}>630$ km s$^{-1}$, suggesting that faster gas is denser, consistent with gas compression in quasar-driven outflows. The paper also reports that the radio emission peaks coincide with the largest [O III] line widths ($W_{80}$) in most galaxies, and that mass outflow rates peak in the innermost $\sim$2 kpc and decline outward, consistent with cloud destruction or incomplete ionisation at large radii.

Load-bearing premise

The single electron density measured from the integrated nuclear spectrum is assumed to apply to all gas classified as outflowing, even tens of kiloparsecs away; if those clouds are less dense, the derived masses, rates, and the reported density–velocity correlation would all be biased.

Editorial extensions

If this is right

Outflow masses and kinetic powers published for type 2 quasars with an assumed $n_e=1000\,\mathrm{cm}^{-3}$ are likely overestimated by about an order of magnitude.
The kinetic coupling efficiencies of these outflows ($\log \varepsilon_f \approx -6.8$ to $-4.2$ of $L_{\rm bol}$) are low, and are lower limits because only one gas phase at optical wavelengths and no turbulent term are included.
The positive $n_e$–$V_{\rm out}$ correlation at $V_{\rm out}>630$ km s$^{-1}$, if confirmed, implies that faster outflows are denser, favouring models in which the outflow compresses the ionised clouds.
The decreasing radial mass-outflow profiles with a peak inside 2 kpc indicate that most of the outflowing ionised mass is released in the nuclear region, with material farther out either destroyed or not excited by the AGN.
Radio peaks spatially matching the $W_{80}$ peaks support a jet or radio-driven disturbance of the ionised gas even in radio-quiet quasars.

Reading between the lines

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

If the $n_e$–$V_{\rm out}$ correlation holds beyond this sample, unresolved single-fibre surveys could use $W_{80}$ to statistically correct outflow densities and energetics in large quasar samples where only integrated spectra exist.
The roughly one-dex drop in kinetic power brings observed outflow coupling closer to the low coupling efficiencies used in some galaxy-formation models, although the comparison is indirect because only the kinetic energy in one gas phase is measured.
A natural test is to look for the same density–velocity trend in molecular outflows of these galaxies: if the dense optical gas is a small fraction of the outflowing mass, the mass rates could be higher while the compression link between speed and density remains.
Re-observing a few of these quasars with higher spatial resolution and longer integrations could map $n_e$ directly inside the outflow cones, separating nuclear-averaged density from true outflow density — the assumption on which the current result rests.

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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

Quick take: the 1-dex reduction is real arithmetic and the paper deserves a serious referee; the n_e-V_out correlation is a promising hint, not a locked result.

What's new: first systematic [Ar IV] densities for this sample of type 2 QSOs, with a clean MUSE/VLA dataset and non-parametric W80 kinematics. The finding that densities (median ~5900 cm^-3) push outflow mass rates and kinetic powers down by ~1 dex relative to the common n_e=1000 assumption is well supported by the tables and follows directly from Eq. 1. The paper is honest about the caveats: densities come from integrated r=1.5'' spectra, no outflow-specific component, and they even flag that high-density gas may be a small fraction of the outflowing mass. That is more than many papers do.

Where it gets shaky: the correlation in Fig. 7. It is fitted after cutting V_out < 630 km/s, combining global and peak measurements from the same galaxies as if independent, and no fit uncertainties are reported. The abstract says 600, the text says 630. With 15 galaxies and two methods per galaxy, the effective number of independent points is small. The correlation may well be real, but the case is not yet made; it needs a proper covariance treatment or a split-sample check. This is the main thing I would ask for in revision.

The bigger conceptual caveat is the one the stress-test note raises: an emission-line ratio in a multiphase medium is emission-measure-weighted, biased to dense clumps, while Eq. 1 needs a mass-weighted density. If the bulk of the outflowing gas is at lower density, the measured rates are not 1 dex too high relative to the truth, they are 1 dex too low relative to what n_e=1000 would give. The paper's wording is careful, but the '1 dex lower' message is easier to over-read than the caveat.

Bottom line: this is a solid, useful paper for anyone working on ionised outflows in AGN. The density set is a real addition, and the comparison with previous samples is valuable. The correlation claim needs more work, but the paper's central result holds as far as the measurements reach. I'd send it to a good referee, ask them to focus on the correlation and the density-representativeness caveat, and cite it myself for the density values. Yes, I'd bring it to reading group, mostly for the discussion of density tracer systematics.

Referee Report

3 major / 5 minor

Summary. The paper presents VLT/MUSE integral-field observations of 18 type 2 quasars from the Quasar Feedback Survey (QFeedS), characterising ionised gas kinematics via non-parametric [O III]5007 measurements and identifying outflow-dominated spaxels using a galaxy-dependent W80 threshold. The new quantitative contribution is the measurement of electron densities from the [Ar IV] 4711,4740 doublet in r=1.5 arcsec nuclear spectra, yielding 500–27700 cm^-3 (median ~5900 cm^-3), and the resulting ionised outflow masses, mass-loss rates, and kinetic powers (0.03–4.17 Msun/yr and 10^39.25–10^41.91 erg/s for the global method), which are ~1 dex lower than the commonly assumed n_e=10^3 cm^-3. A second claim is a positive correlation between n_e and V_out for V_out > 630 km/s, interpreted as gas compression at higher outflow velocities. The paper also compares radio and W80 morphologies and places the outflow energetics in the context of literature samples and coupling efficiencies.

Significance. If the density assumption holds, the paper provides a useful demonstration that using a high-density tracer such as [Ar IV] rather than an assumed n_e=10^3 cm^-3 changes ionised outflow energetics by about an order of magnitude, with direct implications for feedback coupling efficiencies and for comparisons with simulations. The homogeneous 18-object sample, consistent non-parametric analysis, and the global/peak decomposition are strengths, as is the careful comparison with earlier work on overlapping objects. However, the statistical support for the headline n_e–V_out correlation is currently weak, and the representativeness of the single nuclear density for the spatially extended outflow is not established, so the quantitative conclusions are conditional on an assumption the paper itself questions.

major comments (3)

[Sec. 4.2 and Eq. 1] The single electron density measured from the r=1.5 arcsec integrated nuclear spectrum is used in Eq. 1 for every W80-selected outflow spaxel, including gas at projected radii of tens of kpc (e.g., the 45–50 kpc features in J1356+1026). The paper itself states that the [Ar IV] density is 'likely tracing the overall density of the galaxy, not specifically the outflow density.' Since M_out scales as n_e^-1, the headline result that [Ar IV]-based rates and powers are ~1 dex lower than for n_e=10^3 cm^-3 (Table 3 vs. Table A.1) is contingent on the outflow gas having the same density as the nuclear-averaged gas. If the true outflowing phase is closer to 10^3 cm^-3, the reported values would be underestimated by up to ~0.8 dex and the '1 dex lower' message would be inverted. Please either provide a quantitative justification (e.g., spatially resolved density constraints or photoionisation-model checks) or explicitly frame the numbers as conditional on this assumption.
[Sec. 5.4 and Fig. 7] The claimed positive n_e–V_out correlation is fit only to points with V_out > 630 km/s, a threshold selected after inspecting the same plot, and the fit combines global and peak values from the same galaxies as independent measurements. The text notes that the correlation is weaker when global or peak values are considered alone. To support the 'clear positive correlation' statement, the paper should report the correlation coefficient and its significance (e.g., Spearman rank with p-value) for the combined sample and for global-only and peak-only subsamples, and should account for the non-independence of the two points per galaxy (e.g., by bootstrapping over galaxies or fitting one point per galaxy). As presented, the correlation is not statistically established.
[Sec. 5.4 and Table 2] The most extreme outflow-velocity galaxy, J1347+1217 (V_out ~2466 km/s global), is excluded from the n_e–V_out fit because its [Ar IV] doublet is not detected at 3 sigma. If its non-detection is not simply a signal-to-noise effect, the missing high-velocity point could weaken or alter the fitted correlation. Please discuss how this exclusion affects the correlation and whether the non-detection is consistent with the fitted trend.

minor comments (5)

[Sec. 3.1] The sentence 'the amplitude of unnecessary components components tends to zero' contains a duplicated word.
[Sec. 5.2] The text 'clouds of cool emitting gas are are eventually destroyed' has a duplicated 'are'.
[Fig. A.2–A.16 captions] The captions use 'colobars' instead of 'colorbars'.
[Sec. 5.4 / Fig. 7 caption] The text says the grey region contains points with V_out < 630 km/s, while the body text says 'We exclude the 4 galaxies at the lower V_out end'; please make the description of the threshold and the excluded points consistent.
[Table 2] The entries for J1114+1939 and J1347+1217 would be clearer with explicit 'not detected' notes rather than a dash, especially since the notes below the table already explain the reason.

Circularity Check

0 steps flagged · score 2.0 of 10

No significant circularity: the electron densities are measured observables, the outflow velocities are W80-based and independent of n_e, and the ~1 dex comparison follows from inserting measured densities into Eq. 1.

full rationale

The derivation chain is self-contained against external benchmarks. The [Ar IV] densities (Table 2) are measured from the integrated r=1.5 arcsec spectra and inserted into the standard mass formula Eq. 1, where M is proportional to n_e^-1; the comparison with n_e=1000 cm^-3 is a direct arithmetic consequence, not a fitted-input prediction. V_out is defined from W80 (Eq. 4), which has no n_e dependence, and outflow spaxels are selected via W80 thresholds from the unresolved nuclear spectrum (Sec. 4.4), so the n_e-V_out correlation is not built in. The compression interpretation is a post-hoc physical explanation, not a circular derivation. Self-citations to QFeedS papers (Jarvis et al. 2019, 2021; Girdhar et al. 2022; Ulivi et al. 2024) and to simulations with overlapping authors (Ward et al. 2024; Almeida et al. 2026) provide sample context and consistency checks but do not determine the measured values or the correlation. The paper itself flags the main limitation in Sec. 4.2: 'the derived electron density is likely tracing the overall density of the galaxy, not specifically the outflow density,' and in Sec. 5.3 that high-density gas 'might be a small fraction of the total mass that is outflowing.' These are acknowledged assumptions about representativeness, not circular reasoning, and they do not reduce any result to its inputs by construction.

Assumptions & free parameters 5 free parameters · 5 assumptions · 0 invented entities

No new physical entities are introduced. The main free parameters are astrophysical assumptions (T_e, W80 threshold factor, Balmer ratio) typical for this kind of work, plus the post-hoc 630 km/s cut used for the correlation fit. The most consequential unverified assumption is that a single integrated-aperture density represents the outflowing gas across the whole galaxy.

free parameters (5)

Electron temperature T_e for [Ar IV] density = 15000 K
Assumed for Pyneb getTemDen; at 10000 K densities are lower by a median of about 500 cm^-3 (Section 4.2). Affects all derived densities and outflow rates.
V_out threshold for correlation fit = 630 km/s
Chosen post hoc to exclude four low-velocity galaxies from the n_e-V_out fit (Section 5.4, Fig. 7). Directly shapes the reported correlation.
W80 to sigma conversion factor = 2.563
Taken from Liu et al. (2013) to define the outflow threshold from the narrowest nuclear Gaussian component (Section 4.4).
Intrinsic Balmer decrement = Halpha/Hbeta = 2.86
Used for extinction correction with case B recombination at T=10^4 K (Section 4.1).
Assumed density for comparison runs = 1000 cm^-3
Used in Table A.1 and literature comparisons; not fitted but a central benchmark against which the 1-dex difference is defined.

assumptions (5)

domain assumption [Ar IV] line ratio probes electron density of the same ionized gas traced by [O III]
Invoked in Section 4.2; the paper notes Ar3+ and O++ have similar ionization potentials, but the [Ar IV] density is measured from the integrated r=1.5 arcsec spectrum and assumed applicable to outflow spaxels.
domain assumption The W80 > 2.563 sigma_n threshold separates outflow-dominated from non-outflow gas
Section 4.4; based on literature (Riffel et al. 2023, Liu et al. 2013). All outflow properties depend on this definition.
domain assumption Mass outflow rate is constant over time and density decreases with radius
Section 4.4 and Eqs. 2 and 6, following Lutz et al. (2020); the authors state this adds a factor of 3 not accounted for in the calculations.
standard math The [O III] luminosity to gas mass relation (Eq. 1) is valid
Eq. 1 from Carniani et al. (2015), assuming fully ionized gas at 10^4 K and solar oxygen abundance.
standard math Case B recombination and Cardelli extinction curve apply
Section 4.1: used to correct [O III] fluxes for dust extinction before mass and rate estimates.

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Cite this review

Pith. "Pith review of The Quasar Feedback Survey: Ionised Outflows in type 2 QSOs with MUSE data." pith.science (2026). https://pith.science/paper/EHMM3EBH

@misc{pith2026260808275,
  author       = {Pith},
  title        = {Pith review of: The Quasar Feedback Survey: Ionised Outflows in type 2 QSOs with MUSE data},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/EHMM3EBH}},
  note         = {Machine review of arXiv:2608.08275}
}

abstract

We study ionised gas properties in a sample of 18 luminous (log L$_{\rm bol}\geq45$ erg/s) obscured QSOs at 0.085<z<0.2 observed with VLT/MUSE as part of the multi-wavelength Quasar Feedback Survey (QFeedS) and with VLA at low- and high-resolution data. We compare the outflow-related quantities with values reported in the literature and investigate possible correlations between the outflows and other properties of the ionised gas such as the electron density. We adopt a non-parametric approach to characterise the ionised gas kinematics, traced by the [O III]5007 emission line, and use $W_{80}$ measured from the unresolved nuclear spectra as a threshold to identify outflow-dominated spaxels. A qualitative comparison between the radio and the $W_{80}$ maps shows that, in general, the peak of the radio coincides with the peak of the $W_{80}$. The [O III]5007 is used as a proxy for the ionised gas mass, and the outflow-related properties are obtained in two different ways: the global, which uses flux-weighted velocities and radii; and the peak, relying on radial profiles. We correct the [O III]5007 flux for extinction using the Balmer decrement. We take advantage of the MUSE sensitivity and use the [Ar IV]4711,4740 doublet, only observable in the integrated r=1.5'' spectra, to measure the electron density in each galaxy. We obtain $500<n_{e}{\rm[ cm^{-3}]}<27700$, leading to 0.03$<\dot{M}_{\rm out}/{\rm (M_{\odot} yr^{-1})}<$4.17 and $39<\dot{E}_{\rm kin}/{\rm [erg/s]}<42$. Our results emphasise the importance of accurate n$_e$ determination, leading to a difference of ~1 dex in the outflow rates and kinetic powers. We observe a positive correlation between $n_e$ and $V_{\rm out}$, interpreted as compression of the gas at higher velocities. This correlation should be further investigated at other luminosity and redshift ranges, but it can inform future outflow simulation studies.

Figures

Figures reproduced from arXiv: 2608.08275 by the authors.

**Figure 2.** Pseudo narrow-band image constructed from the MUSE data cube accounting for the emission of Hβ [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗

**Figure 3.** Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗

Figures from the paper (4 more)

**Figure 4.** Figure 4: Fitting example of the [O iii]5007Å for nuclear spaxel of J0945+1737. The linear continuum fit is subtracted from both modelled and observed spectra. The green-dotted lines represent the individual Gaussian components. The shaded yellow area corresponds to the W80 whe…

**Figure 5.** Figure 5: Top panel: Outflow velocity radial profile. Bottom panel: mass of the gas in the outflow radial profile assuming a density of ne = 103 cm−3 . The velocities are insensitive to our choice of electron density. the destruction of [O iii] emitting clouds; ii) differences i…

**Figure 6.** Figure 6: Mass outflow rates and kinetic power versus AGN [PITH_FULL_IMAGE:figures/full_fig_p012_6.png]

**Figure 7.** Figure 7: shows ne based on [Ar iv] lines we measure in this work versus Vout for the global and peak methods. The grey shaded area corresponds to galaxies with Vout < 630 km s−1 , where there is clear scatter of the electron density values. When considering only the values with…

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