arxiv: 2605.02648 · v2 · submitted 2026-05-04 · 🌌 astro-ph.GA

Recognition: unknown

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE). XXI. Statistical properties of individual HII regions in perturbed galaxies

A. Boselli , M. Fossati , Y. Roehlly , M. Boquien , J. Braine , P. Cote , J.C. Cuillandre , B. Epinat

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L. Ferrarese S. Gwyn G. Hensler

Authors on Pith no claims yet

Pith reviewed 2026-05-08 17:25 UTC · model grok-4.3

classification 🌌 astro-ph.GA

keywords HII regionsVirgo clusterram pressure strippingHI deficiencyluminosity functionstar formation quenchinggalaxy evolution

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The pith

HI-deficient galaxies in the Virgo cluster have steeper HII region faint-end slopes and brighter characteristic Ha luminosities than gas-rich systems.

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

The paper uses narrow-band Halpha imaging from the VESTIGE survey to catalog over 76,000 HII regions across 322 star-forming Virgo galaxies and compares the subset in HI gas-deficient perturbed galaxies to those in unperturbed gas-rich ones. It derives luminosity functions, size and density distributions, and scaling relations, finding systematic differences that grow with HI deficiency and concentrate in the outer disks. These shifts are interpreted as the result of ram pressure stripping by the intracluster medium, which removes atomic gas from the outside inward and thereby quenches star formation in galaxy outskirts. The result matters because it supplies a statistical, observable signature of environmental quenching that can be tracked without direct gas maps.

Core claim

The statistical and physical properties of HI gas-deficient cluster galaxies are different from those of unperturbed systems, with perturbed objects having a steeper faint-end slope and a brighter characteristic Ha luminosity than gas-rich galaxies. The difference in the two distributions comes principally from the outer disc (outside the effective radius). The analysis of the scaling relations indicates that perturbed objects have a lower number of HII regions per unit stellar mass and disc surface than unperturbed systems, with differences increasing with the HI-deficiency parameter, principally in the outer disc where HII regions are less present in gas-poor systems. All these differences

What carries the argument

Composite H-alpha luminosity functions, diameter and electron density distributions, and scaling relations of HII regions identified above the completeness limit, compared between HI-deficient perturbed galaxies and gas-rich unperturbed galaxies.

If this is right

Perturbed galaxies contain fewer HII regions per unit stellar mass and per unit disk surface area.
The faint-end slope of the luminosity function steepens and the characteristic luminosity brightens as HI deficiency increases.
The strongest changes occur outside the effective radius, consistent with outside-in gas removal.
Once the outer HI is stripped, star formation activity in the outer disk drops sharply.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

HII region statistics could serve as a proxy for identifying galaxies in the process of environmental quenching even when HI data are unavailable.
The shift toward brighter characteristic luminosities may reflect more intense remaining star formation confined to the inner disk.
Repeating the analysis with molecular-gas or UV tracers would test whether the quenching affects all phases of star formation or only the ionised component.

Load-bearing premise

That selecting galaxies as perturbed solely by their HI deficiency cleanly isolates ram pressure effects without substantial contamination from galaxy mass, morphology, or internal processes.

What would settle it

Finding no difference in HII region luminosity functions or number densities between HI-deficient and gas-rich galaxies once stellar mass and morphology are matched would falsify the environmental-quenching interpretation.

Figures

Figures reproduced from arXiv: 2605.02648 by A. Boselli, B. Epinat, G. Hensler, J. Braine, J.C. Cuillandre, L. Ferrarese, M. Boquien, M. Fossati, P. Cote, S. Gwyn, Y. Roehlly.

**Figure 1.** Figure 1: Continuum-subtracted Hα images of representative galaxies in the unperturbed (upper row) and perturbed (lower row) samples in different bins of stellar mass: Mstar > 1010 M⊙ (upper left column: NGC4535-VCC1555, lower left column: NGC4548- VCC1615), 109 < Mstar ≤ 1010 M⊙ (upper central column: NGC4411b-VCC939, lower central column: IC3267-VCC697), 108 < Mstar ≤ 109 M⊙ (upper right column: VCC334; lower rig… view at source ↗

**Figure 2.** Figure 2: Comparison of the distributions of the stellar mass (left panel), i-band effective radius (central panel), and star formation rate (right panel) of the unperturbed (blue filled histogram) and perturbed (red empty histogram) samples. 3. Narrow-band Hα imaging data The data analysed in this work have been gathered during the VESTIGE Hα narrow-band imaging survey of the Virgo cluster. The details of the obser… view at source ↗

**Figure 3.** Figure 3: Composite luminosity function of the H ii regions detected by HIIphot on the selected galaxies for unperturbed (HI − de f ≤ 0.4; blue dots) and perturbed (HI − de f > 0.4; red dots) galaxies. The Hα luminosities of individual H ii regions have been corrected for dust attenuation and [N ii] contamination. The solid and dotted lines indicate the best-fit and 1σ confidence regions for the Schechter luminos… view at source ↗

**Figure 4.** Figure 4: Composite luminosity function of the H ii regions detected within (filled dots, solid lines) and outside (empty dots, dashed lines) the i-band effective radius of the target galaxies normalised to the total number of H ii regions with L(Hα) ≥ 1037 erg s−1 within (Ntot=4 194; 9 292) and outside (Ntot=9 084; 11 788) the effective radius for unperturbed (HI−de f ≤ 0.4; blue dots and lines) and perturbed (HI−… view at source ↗

**Figure 5.** Figure 5: Left: relation between the faint end slope α of the luminosity function and the characteristic luminosity L ∗ (Hα) of individual galaxies with more than 20 H ii regions brighter than L(Hα) ≥ 1037 erg s−1 . Right: relation between the characteristic number of objects Φ∗ and the faint end slope α of the luminosity function. Different colours are used for galaxies belonging to different cluster substructures:… view at source ↗

**Figure 6.** Figure 6: Normalised distribution of the observed (empty dots) equivalent diameters for H ii regions with L(Hα) ≥ 1037 erg s−1 for unperturbed (HI − de f ≤ 0.4; blue symbols) and perturbed (HI − de f > 0.4; red symbols) galaxies. Empty symbols show the normalised distribution of equivalent diameters corrected for seeing effects whenever the correction is less than 50%. The dashed vertical line shows the equivalent d… view at source ↗

**Figure 8.** Figure 8: Normalised distribution of the electron density derived using equivalent diameters corrected for seeing effects for H ii regions with L(Hα) ≥ 1037 erg s−1 and a diameter correction factor ≤ 50% detected within (filled dots, solid lines) and outside (empty dots, dashed lines) the i-band effective radius for unperturbed (HI − de f ≤ 0.4; blue symbols) and perturbed (HI − de f > 0.4; red symbols) galaxies view at source ↗

**Figure 9.** Figure 9: Relation between the Hα luminosity of individual H ii regions corrected for [N ii] contamination and dust attenuation and the equivalent diameter corrected for seeing effects. Blue and red filled dots are for H ii regions with a diameter correction factor ≤ 50% for unperturbed (HI − de f ≤ 0.4; blue symbols) and perturbed (HI−de f > 0.4; red symbols) galaxies, respectively. Grey dots are for all H ii reg… view at source ↗

**Figure 12.** Figure 12: Relation between the Hα luminosity of the brightest H ii region corrected for dust attenuation and [N ii] contamination and the total star formation rate (upper left panel) and total stellar mass (lower left) surface densities of the host galaxies. Blue filled dots are for unperturbed systems with a normal H i gas content (HI − de f ≤ 0.4), red empty circles gas-deficient perturbed galaxies (HI−de f > 0… view at source ↗

**Figure 14.** Figure 14: Relation between the number of H ii regions of luminosity L(Hα) ≥ 1037 erg s−1 corrected for dust attenuation and [N ii] contamination per unit stellar mass disc, (upper panel) stellar disc surface (measured up to the 25.5 B-band isophotal diameter; central panel), and the ratio of total number of H ii regions located inside and outside the i-band effective radius (in log scale; lower panel) and the H… view at source ↗

**Figure 15.** Figure 15: Relation between the output parameters (α, upper panel; L ∗ (Hα), central panel; Φ∗ , lower panel) of the best fit Schechter function on individual galaxies with more than 20 H ii regions of Hα luminosity brighter than L(Hα) ≥ 1037 erg s−1 and the H i- -deficiency parameter. Blue filled dots are for unperturbed systems with a normal H i gas content (HI − de f ≤ 0.4), red empty circles gas-deficient pertu… view at source ↗

read the original abstract

We use narrow-band Halpha+[NII] imaging data gathered during VESTIGE, a blind survey of the Virgo cluster carried out with MegaCam at the CFHT, to identify HII regions in 385 galaxies showing ionised gas emission. We identify 76645 HII regions in 322 star-forming galaxies and study their physical properties for those above the completeness limit (L(Ha)>=10^37 erg s-1). The present work is focused on perturbed cluster galaxies, identified as those having a reduced amount of HI when compared to similar objects in the field. We derive composite luminosity functions, diameter and electron density distributions, and several scaling relations, and compare them to those already derived for gas-rich, unperturbed systems identified during the VESTIGE survey. The analysis shows that the statistical and physical properties of HI gas-deficient cluster galaxies are different from those of unperturbed systems, with perturbed objects having a steeper faint-end slope and a brighter characteristic Ha luminosity than gas-rich galaxies. The difference in the two distributions comes principally from the outer disc (outside the effective radius). The analysis of the scaling relations indicates that perturbed objects have a lower number of HII regions per unit stellar mass and disc surface than unperturbed systems, with differences increasing with the HI-deficiency parameter, principally in the outer disc where HII regions are less present in gas-poor systems. All these differences can be explained in the framework of galaxy evolution in rich environments, where their hydrodynamic interaction with the surrounding ICM (ram pressure) removes the gas outside-in quenching the star formation activity in the outer disc once the HI is removed.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Desk Editor's Note private letter to a colleague

This VESTIGE paper adds new HII region luminosity functions and scaling relations for HI-deficient Virgo galaxies that differ from the unperturbed sample mainly in the outer disk, but the HI-deficiency selection leaves room for mass or morphology confounds.

read the letter

The main thing to know is that the team measured HII regions in 322 star-forming Virgo galaxies and found the HI-deficient subset has a steeper faint-end H-alpha luminosity function, a brighter characteristic luminosity, and fewer regions per unit stellar mass than the gas-rich ones, with the gaps largest outside the effective radius. They attribute this to ram-pressure stripping removing gas from the outside in and quenching star formation there once the HI is gone. The work ships composite distributions for luminosity, diameter, and electron density plus several scaling relations, all built from the same MegaCam narrow-band imaging and restricted to the completeness limit above 10^37 erg/s. That gives a clean set of numbers for the perturbed population that extends the earlier VESTIGE results on unperturbed systems. The sample size is large, over 76,000 regions total, and the outer-disk emphasis matches the expected hydrodynamic picture. The differences also scale with the HI-deficiency parameter, which adds some internal consistency. The soft spot is that selecting on HI deficiency relative to field analogs may not fully separate environmental effects from differences in stellar mass or morphology that could alter HII statistics on their own. The abstract mentions comparisons to similar objects but does not spell out the matching procedure or how errors were propagated in the fits, so it is hard to judge how much those choices drive the reported slopes and normalizations. If the full text shows only loose controls, the interpretation would need tightening. This paper is aimed at people who already track environmental quenching in clusters or who use HII region statistics as model constraints. Readers working on Virgo or ram-pressure models would pick up usable benchmarks from the new distributions. It has enough fresh data and a coherent observational story to warrant peer review, though the methods section will probably need more detail on selection and fitting before it is ready for publication.

Referee Report

3 major / 2 minor

Summary. The manuscript uses VESTIGE narrow-band Hα+[NII] imaging to identify 76,645 HII regions in 322 star-forming Virgo galaxies (385 total with emission), focusing on HI-deficient perturbed systems above the L(Hα) ≥ 10^37 erg s^{-1} completeness limit. It constructs composite luminosity functions, diameter and electron density distributions, and scaling relations, comparing them to unperturbed gas-rich galaxies from the same survey. Perturbed galaxies show a steeper faint-end slope and brighter characteristic Hα luminosity, with differences concentrated in the outer disc; they also exhibit fewer HII regions per unit stellar mass and disc surface area, increasing with HI deficiency. These are interpreted as signatures of outside-in quenching via ram-pressure stripping by the ICM.

Significance. The large sample from a blind cluster survey enables statistically meaningful composite distributions that, if robust, would strengthen evidence for environmental quenching mechanisms in dense environments. The focus on outer-disc differences and scaling with HI deficiency directly tests the ram-pressure scenario. However, the overall significance depends on confirming that the reported differences are not driven by unaccounted sample biases.

major comments (3)

[§3] §3 (sample definition): The selection of perturbed galaxies via HI deficiency relative to 'similar objects' in the field, and any explicit matching on stellar mass, morphology, or other properties, must be described in detail. The central claim that differences in the faint-end slope, characteristic luminosity, and outer-disc HII region counts arise from ram pressure requires that this selection isolates environmental effects; without it, residual composition differences could produce the observed trends.
[§4.2] §4.2 (luminosity functions): The fitting procedure for the composite Hα luminosity functions—including the adopted functional form, incorporation of the stated completeness limit, and propagation of uncertainties on the faint-end slope and characteristic luminosity—must be provided. The reported steeper slope and brighter L* in perturbed galaxies are load-bearing for the quenching interpretation, yet the current description does not allow assessment of whether these differences are statistically significant or sensitive to analysis choices.
[§4.3] §4.3 (radial analysis): The definition of the effective radius used to separate inner and outer discs, and the quantitative method for measuring the reduced number of HII regions per unit stellar mass in the outer disc, require explicit description. This radial dependence is central to the outside-in quenching claim and must be shown to be independent of how galaxies are binned by HI deficiency.

minor comments (2)

[Abstract] The abstract refers to 'several scaling relations' without naming them; listing the specific relations (e.g., N_HII vs. M*, surface density) would improve readability.
Ensure uniform terminology between 'perturbed', 'HI gas-deficient', and 'gas-poor' throughout the text and figures.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their detailed and constructive comments on our manuscript. These have prompted us to clarify several aspects of our analysis. We address each major comment below and indicate the revisions we will make to the manuscript.

read point-by-point responses

Referee: [§3] §3 (sample definition): The selection of perturbed galaxies via HI deficiency relative to 'similar objects' in the field, and any explicit matching on stellar mass, morphology, or other properties, must be described in detail. The central claim that differences in the faint-end slope, characteristic luminosity, and outer-disc HII region counts arise from ram pressure requires that this selection isolates environmental effects; without it, residual composition differences could produce the observed trends.

Authors: We agree that a more detailed description of the sample selection is essential to support our interpretation. In the revised manuscript, we will expand Section 3 to explicitly describe: the calculation of the HI deficiency parameter using the reference field sample from the literature; the criteria used to identify 'similar objects' including any matching on stellar mass, morphological type, and other relevant properties; and an assessment of potential residual biases in the sample composition. This will help demonstrate that the observed differences are attributable to environmental effects such as ram-pressure stripping. revision: yes
Referee: [§4.2] §4.2 (luminosity functions): The fitting procedure for the composite Hα luminosity functions—including the adopted functional form, incorporation of the stated completeness limit, and propagation of uncertainties on the faint-end slope and characteristic luminosity—must be provided. The reported steeper slope and brighter L* in perturbed galaxies are load-bearing for the quenching interpretation, yet the current description does not allow assessment of whether these differences are statistically significant or sensitive to analysis choices.

Authors: We acknowledge that the description of the luminosity function fitting was insufficient. The composite LFs were constructed by stacking the HII regions from the respective samples and fitted with a Schechter function for luminosities above the completeness limit of 10^37 erg s^{-1}. In the revised version, we will detail the fitting procedure, including the functional form, how the completeness limit is accounted for (by restricting the fit to L(Hα) ≥ 10^37 erg s^{-1} and using maximum likelihood estimation), and the uncertainty estimation method (via bootstrap resampling of the galaxy samples to propagate errors on the faint-end slope α and characteristic luminosity L*). We will also include a statistical comparison (e.g., likelihood ratio test) to confirm the significance of the differences between perturbed and unperturbed galaxies. revision: yes
Referee: [§4.3] §4.3 (radial analysis): The definition of the effective radius used to separate inner and outer discs, and the quantitative method for measuring the reduced number of HII regions per unit stellar mass in the outer disc, require explicit description. This radial dependence is central to the outside-in quenching claim and must be shown to be independent of how galaxies are binned by HI deficiency.

Authors: We thank the referee for pointing out the need for clarity in the radial analysis. The effective radius is taken from the literature or derived from the stellar mass distribution as the radius enclosing 50% of the total stellar light. The number of HII regions per unit stellar mass in the outer disc is computed by summing HII regions beyond the effective radius and normalizing by the stellar mass within the outer disc (or total stellar mass, as appropriate). In the revised manuscript, we will provide explicit definitions and formulas for these quantities, describe the binning by HI deficiency parameter, and present checks demonstrating that the trends are robust to different binning schemes. This will reinforce the outside-in quenching scenario. revision: yes

Circularity Check

0 steps flagged

No significant circularity in derivation chain

full rationale

The paper presents independent measurements of HII region properties (luminosity functions, diameters, densities, scaling relations) from new VESTIGE narrow-band imaging of 322 star-forming galaxies, focusing on the HI-deficient perturbed subsample. These are compared to previously published results for unperturbed galaxies from the same survey series, but the new data and derivations stand alone without any reduction to fitted parameters, self-definitions, or ansatzes imported via citation. The interpretive framework invoking ram-pressure stripping is explanatory rather than a mathematical derivation that loops back to the inputs. No self-definitional, fitted-input-as-prediction, uniqueness-theorem, or renaming patterns appear in the provided derivation steps.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The analysis is observational and relies on standard domain assumptions in astrophysics rather than new free parameters or postulated entities. The completeness threshold and HI-deficiency classification are taken from prior literature.

axioms (2)

domain assumption HI deficiency parameter reliably flags galaxies experiencing ram-pressure perturbation by the intracluster medium.
Used to define the perturbed sample and to correlate trends with increasing deficiency.
domain assumption Narrow-band H-alpha+[NII] emission primarily traces ionization by young stars in HII regions with limited contamination.
Foundation for identifying and characterizing the 76,645 regions.

pith-pipeline@v0.9.0 · 5658 in / 1496 out tokens · 52018 ms · 2026-05-08T17:25:37.717941+00:00 · methodology

discussion (0)

Reference graph

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