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arxiv: 2603.28855 · v1 · pith:I4EX27PPnew · submitted 2026-03-30 · 🌌 astro-ph.GA

The CAVITY project. The spatially resolved SFR of galaxies in voids

Ana M. Conrado , Rub\'en Garc\'ia-Benito , Rosa M. Gonz\'alez Delgado , Bahar Bidaran , H\'el\`ene M. Courtois , Salvador Duarte Puertas , Daniel Espada , Andoni Jim\'enez
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Ignacio del Moral-Castro Isabel P\'erez Tom\'as Ruiz-Lara Laura S\'anchez-Menguiano Gloria Torres-R\'ios Simon Verley Mar\'ia Argudo-Fern\'andez Simon B. De Daniloff Estrella Florido Yllari K. Gonz\'alez-Koda Alejandra Z. Lugo-Aranda Javier Rom\'an Smitha Subramanian Pedro Villalba-Gonz\'alez Manuel Alc\'azar-Laynez M\'onica Hern\'andez-S\'anchez M\'onica Rodr\'iguez Mart\'inez Paulo V\'asquez-Bustos Martin Blazek
This is my paper

Pith reviewed 2026-05-21 09:18 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords void galaxiesstar formation rateradial profilescosmic voidsgalaxy evolutionintegral field spectroscopyextinctionlarge-scale structure
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The pith

Galaxies in cosmic voids tend to have higher star formation rates than similar galaxies in denser regions, especially early spirals at all radii.

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

The paper examines the impact of the void environment on star formation activity using spatially resolved observations of 220 galaxies from the CAVITY survey. Integral field unit data yield maps of star formation rate, specific star formation rate, and extinction derived from Halpha emission. These are compared to a control sample of galaxies in filaments and walls drawn from the CALIFA survey and matched in morphology and stellar mass. The analysis reveals trends of larger SFR in voids, particularly for early spirals across all distances and for late spirals in outer regions, along with lower extinction and higher gas mass fraction proxies in some cases. This pattern points to a slower evolution toward quiescence for galaxies in underdense regions.

Core claim

Void galaxies tend to have larger SFR, especially for early spirals at all galactocentric distances and in the outer parts of late-type spirals, together with lower extinction and higher extinction-normalised-by-stellar-mass-surface-density in outer regions of early spirals, indicating slower transition to quiescence.

What carries the argument

Radial profiles of extinction-corrected Halpha-derived star formation rate and specific star formation rate up to two half-light radii, contrasted against a control sample matched only in morphology and stellar mass.

If this is right

  • Early spiral galaxies in voids maintain elevated SFR at every galactocentric distance out to two half-light radii.
  • Late-type spirals in voids show higher SFR specifically in their outer disks compared to matched galaxies elsewhere.
  • Late-type void galaxies exhibit lower dust extinction across their disks.
  • Early spirals in voids display higher extinction normalized by stellar mass surface density in outer regions, consistent with larger gas reservoirs.
  • The void environment appears to slow the overall transition of galaxies from star-forming to passive states.

Where Pith is reading between the lines

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

  • The environmental signal may persist when samples are expanded to include fainter or higher-redshift void galaxies from future wide-field surveys.
  • Similar radial SFR trends could appear in hydrodynamical simulations when galaxies are binned by large-scale density rather than local density alone.
  • The higher outer-disk gas proxy might be tested directly with HI or CO observations to confirm whether voids truly retain more fuel for star formation.
  • If the slower quenching holds, it could help explain the observed excess of blue, late-type galaxies in void catalogs from photometric surveys.

Load-bearing premise

Matching the control sample solely on morphology and stellar mass from the CALIFA survey is sufficient to isolate the effect of the void environment from all other variables that could influence SFR and extinction.

What would settle it

A comparison showing identical SFR radial profiles once void galaxies and controls are additionally matched on local density or current gas content would indicate that the reported differences are not driven by the void environment.

Figures

Figures reproduced from arXiv: 2603.28855 by Alejandra Z. Lugo-Aranda, Ana M. Conrado, Andoni Jim\'enez, Bahar Bidaran, Daniel Espada, Estrella Florido, Gloria Torres-R\'ios, H\'el\`ene M. Courtois, Ignacio del Moral-Castro, Isabel P\'erez, Javier Rom\'an, Laura S\'anchez-Menguiano, Manuel Alc\'azar-Laynez, Mar\'ia Argudo-Fern\'andez, Martin Blazek, M\'onica Hern\'andez-S\'anchez, M\'onica Rodr\'iguez Mart\'inez, Paulo V\'asquez-Bustos, Pedro Villalba-Gonz\'alez, Rosa M. Gonz\'alez Delgado, Rub\'en Garc\'ia-Benito, Salvador Duarte Puertas, Simon B. De Daniloff, Simon Verley, Smitha Subramanian, Tom\'as Ruiz-Lara, Yllari K. Gonz\'alez-Koda.

Figure 2
Figure 2. Figure 2: shows the colour-magnitude diagram of the parent sample and the selection for this work. It can be seen that our analysed sample covers the same area as the parent sample, with a smaller population at the fainter end. This is a result of the selection criteria: we select the brightest galaxies to ensure a sufficient signal-to-noise ratio (S/N) for reliable fitting at large galactocentric distances and to o… view at source ↗
Figure 3
Figure 3. Figure 3: Radial profiles and maps of some physical properties of CAVITY54706, one of the Sc galaxies in our sample. The shaded area around them mark the uncertainty, calculated as the standard deviation divided by the square root of the number of pixels taken into account. The red ellipse indicates its half-light radius. The colour bars share scale with their corresponding profile’s y-axis. In the left, from top to… view at source ↗
Figure 4
Figure 4. Figure 4: BPT (top, Baldwin et al. 1981) and WHaN (bottom, Cid Fernandes et al. 2010, 2011) diagnostic diagrams. The dots represent the flux values at the centre (left) or median values at a galactocentric distance of R = 1 HLR (right), coloured by the measurements of EW(Hα) (top) or by morphological type (bottom). The grey shadow in the left shows the distribution of the values of all pixels of all galaxies. On the… view at source ↗
Figure 5
Figure 5. Figure 5: Global properties coloured by morphological type. Each row shows a different property of each galaxy against their total stellar mass at the left, calculated in Conrado et al. (2024), and the density distri￾bution of each morphological type convolved with a gaussian kernel at the right, in the y-axis. The grey straight lines in the top left panel show the SFMS calculated by fitting the Sc and Sd galaxies o… view at source ↗
Figure 6
Figure 6. Figure 6: Radial profiles of different emission line properties, stacked by morphological type. Each point represents the median value of the un￾masked profiles at a given galactocentric distance, in bins of 0.3 HLR. Elliptical and lenticular galaxies are not represented given that most of the values of their profiles are masked. The shaded area marks the un￾certainty, calculated as the standard deviation divided by… view at source ↗
Figure 7
Figure 7. Figure 7: Distribution of the total stellar mass by morphological types, for CAVITY void galaxies (in dark blue) and for CALIFA galaxies in filament or walls, matched in morphological type and total stellar mass (in red). The black and white lines mark the location of the median of each distribution, and the dotted lines their first and third quartiles. The edges of the distributions are cut to show the minimum and … view at source ↗
Figure 8
Figure 8. Figure 8: Violin plots of the distributions of the global properties for void galaxies (in dark blue) and filament and wall galaxies (in red). From top to bottom, SFR, sSFR, and AV . See [PITH_FULL_IMAGE:figures/full_fig_p009_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Radial profiles of the sSFR (top row) and AV (bottom row) for spiral galaxies in voids and in filaments and walls, stacked by morphological type. Shaded areas mark the uncertainty (see [PITH_FULL_IMAGE:figures/full_fig_p011_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Global values (left) and radial profiles (three right panels) of the AV /Σ⋆ for the LTG in voids and in filaments and walls. Each dot represent the median value of the unmasked profiles at each galactocentric distance, and shaded areas around the radial profiles mark the uncertainty (see [PITH_FULL_IMAGE:figures/full_fig_p012_10.png] view at source ↗
read the original abstract

The mass in the Universe is distributed non-uniformly, originating the Large Scale Structure (LSS), characterised by clusters, filaments, walls and voids. Galaxies in voids are bluer, later type, less massive, and have slower evolution than galaxies in denser environments. The effect of the void environment on properties such as star formation rate (SFR) is still under discussion. We tackle this by estimating spatially-resolved SFR from extinction-corrected Halpha luminosities of 220 void galaxies from the CAVITY survey. These observations consist of optical integral field unit data cubes from the PMAS/PPaK spectrograph at Calar Alto Observatory. We measure the continuum-subtracted emission lines to obtain maps of SFR, specific star formation rate (sSFR) and extinction. We assess global properties and radial profiles up to 2 half-light radii. We compare with galaxies in filaments and walls from the CALIFA survey using the same methodology, building a control sample matched in morphology and stellar mass. We find no significant differences in SFR and sSFR, although void galaxies tend to have larger SFR, especially for early spirals. This effect is present for Sa galaxies at all galactocentric distances, and in the outer parts of late-type spirals, evidencing slower transition to quiescence and less evolved discs. Void late-type galaxies have lower extinction. Using extinction normalised by stellar mass surface density as a proxy for gas mass fraction, we find it larger for void early spirals, especially in outer regions. This indicates the effect of the void environment on the transition from star forming to passive.

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.

Referee Report

2 major / 2 minor

Summary. The manuscript analyzes spatially resolved star formation rates (SFR) derived from extinction-corrected Hα luminosities in 220 void galaxies from the CAVITY survey using PMAS/PPaK integral-field spectroscopy. Radial profiles of SFR, specific SFR, and extinction are constructed out to 2 half-light radii and compared to a control sample of CALIFA galaxies in filaments/walls, matched in morphology and stellar mass using the same methodology. The central claims are that there are no statistically significant global differences in SFR or sSFR, yet void early spirals (especially Sa) exhibit higher SFR at all radii, late-type spirals show elevated SFR in outer regions, void late-types have lower extinction, and void early spirals display higher extinction normalized by stellar-mass surface density (as a gas-mass-fraction proxy) in outer disks, interpreted as slower transition to quiescence in voids.

Significance. If the reported radial trends survive improved control-sample validation, the work would add spatially resolved evidence that large-scale underdensity slows disk evolution and quenching, particularly in outer regions. The consistent Hα methodology across surveys and the use of an extinction-based gas proxy are constructive elements that go beyond global comparisons. The modest overall significance (explicitly “no significant differences”) and subsample-specific tendencies limit the immediate impact unless the effect sizes and robustness are quantified more precisely.

major comments (2)
  1. [§3 (control-sample construction)] §3 (control-sample construction): the matching is performed solely on morphology and stellar mass. To isolate the void environment as the driver of the claimed radial SFR and extinction trends, the manuscript must demonstrate that the matched distributions are statistically indistinguishable in redshift, effective radius, and inclination (all of which affect Hα-derived SFR and extinction). Without Kolmogorov-Smirnov or similar tests on these observables, residual selection differences between CAVITY and CALIFA remain a plausible alternative explanation for the reported early-spiral trends at all radii.
  2. [§4–5 (radial-profile results)] §4–5 (radial-profile results): the abstract states “no significant differences” yet highlights tendencies “especially for early spirals at all galactocentric distances.” The paper should report quantitative median offsets, uncertainties, and p-values (or equivalent) for the Sa and late-type subsamples in each radial bin. Absent these statistics, it is unclear whether the outer-disk gas-proxy elevation in early spirals is load-bearing for the environmental interpretation or merely suggestive.
minor comments (2)
  1. [Abstract] Abstract: replace the vague “tend to have larger SFR” with a brief statement of the typical fractional difference or effect size for the Sa subsample.
  2. [Figures and tables] Figure captions and tables: confirm that all radial profiles display both the median trend and the 16–84 percentile range or bootstrap uncertainties so that the strength of the outer-disk differences can be visually assessed.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive and detailed report. The comments highlight important aspects of control-sample validation and statistical quantification that will improve the clarity and robustness of the manuscript. We respond point by point below and indicate the revisions we will implement.

read point-by-point responses

  1. Referee: §3 (control-sample construction): the matching is performed solely on morphology and stellar mass. To isolate the void environment as the driver of the claimed radial SFR and extinction trends, the manuscript must demonstrate that the matched distributions are statistically indistinguishable in redshift, effective radius, and inclination (all of which affect Hα-derived SFR and extinction). Without Kolmogorov-Smirnov or similar tests on these observables, residual selection differences between CAVITY and CALIFA remain a plausible alternative explanation for the reported early-spiral trends at all radii.

    Authors: We agree that demonstrating statistical indistinguishability in additional parameters is necessary to isolate the environmental effect. In the revised manuscript we will add Kolmogorov-Smirnov tests (and, where appropriate, other two-sample tests) comparing the distributions of redshift, effective radius, and inclination between the void sample and the morphology- and mass-matched control sample. We will report the test statistics, p-values, and a brief discussion of any marginal differences and their possible impact on the Hα-derived quantities. This addition will be placed in §3 alongside the existing matching description. revision: yes

  2. Referee: §4–5 (radial-profile results): the abstract states “no significant differences” yet highlights tendencies “especially for early spirals at all galactocentric distances.” The paper should report quantitative median offsets, uncertainties, and p-values (or equivalent) for the Sa and late-type subsamples in each radial bin. Absent these statistics, it is unclear whether the outer-disk gas-proxy elevation in early spirals is load-bearing for the environmental interpretation or merely suggestive.

    Authors: We accept that the presentation would be strengthened by explicit quantitative measures. In the revised version we will add, for the Sa and late-type subsamples separately, the median offsets (void minus control) in SFR, sSFR, extinction, and the extinction-normalised-by-stellar-mass-surface-density proxy, together with their uncertainties and p-values from suitable non-parametric tests, for each radial bin out to 2 R_e. These numbers will be included in the text of §§4–5 and, where space permits, in an updated version of the relevant figures or a new table. This will allow a clearer assessment of which trends are statistically supported. revision: yes

Circularity Check

0 steps flagged

Direct observational comparison with no self-referential derivations or fitted predictions

full rationale

The paper reports empirical measurements of spatially resolved SFR from extinction-corrected Hα luminosities in CAVITY void galaxies, constructs radial profiles, and performs a direct statistical comparison against a CALIFA control sample matched on morphology and stellar mass. No equations, ansatzes, or derivations are presented that reduce the reported SFR, sSFR, extinction, or gas-mass-fraction proxy to parameters fitted from the same dataset by construction. The central claims rest on observed differences after matching, with no load-bearing self-citations or uniqueness theorems invoked to force the result. This is a standard observational analysis whose conclusions are falsifiable against external data and therefore self-contained.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claims rest on two standard domain assumptions in extragalactic astronomy plus the validity of the sample-matching procedure; no free parameters or new entities are introduced.

axioms (2)
  • domain assumption Extinction-corrected H-alpha luminosity provides a reliable tracer of recent star formation rate
    Invoked when converting emission-line maps to SFR maps; standard conversion used throughout the field.
  • domain assumption Extinction normalised by stellar mass surface density serves as a proxy for gas mass fraction
    Explicitly adopted in the abstract to interpret outer-disk differences.

pith-pipeline@v0.9.0 · 6001 in / 1402 out tokens · 60516 ms · 2026-05-21T09:18:52.680922+00:00 · methodology

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