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Virgo Filaments V: Disrupting the Baryon Cycle in the NGC 5364 Galaxy Group

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Pith's one-line read Ram pressure stripping, tides, and starvation are jointly disrupting gas in the low-mass NGC 5364 group.

desk verdict Solid first Hα+MeerKAT look at a low-mass group, with a quantitative RPS claim that is plausible but rides on an unmeasured IGM density. read the letter →

arxiv 2505.09782 v1 pith:T5HWKZQA submitted 2025-05-14 astro-ph.GA

Rose A. Finn , Gregory Rudnick , Pascale Jablonka , Mpati Ramatsoku , Gautam Nagaraj , Benedetta Vulcani , Rebecca A. Koopmann , Matteo Fossati
show 15 more authors
James Agostino Yannick Bahe Santiago Garcia-Burillo Gianluca Castignani Francoise Combes Kim Conger Gabriella De Lucia Vandana Desai John Moustakas Dara Norman Damien Sperone-Longin Melinda Townsend Lizhi Xie Daria Zakharova Dennis Zaritsky
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classification astro-ph.GA
keywords galaxygroupsquenchingenvironmentslarge-scalestructurecosmicwebrampressurestrippingH-alphaimagingHIobservations
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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 tries to show that even a very low-mass galaxy group can disrupt the baryon cycle—the flow of gas into galaxies, its conversion into stars, and its return to the intergalactic medium—through the group environment rather than through internal processes alone. Using narrowband H$\alpha$ imaging from the Virgo Filament Survey and resolved H I maps from MeerKAT for eight members of the NGC 5364 group, the authors find a range of damage: lopsided stellar and gas disks, truncated H I and H$\alpha$ disks, H I tails, extraplanar star formation, and two gas-poor dwarfs. They compare the gravitational restoring force at each galaxy's truncation radius with the classical ram pressure from the intragroup medium, and conclude that ram pressure can explain the observed truncation and tails for all but one of the disk-dominated galaxies. If correct, this extends cluster-scale environmental quenching down to groups of about $10^{12.7}$ solar masses and implies that tidal interactions, ram pressure, and starvation act together even in quite small groups.

What carries the argument

The argument is carried by spatially resolved maps of two gas phases—narrowband H$\alpha$ imaging from the Virgo Filament Survey-H$\alpha$ (a 34-arcminute field from the Wide Field Camera on the Isaac Newton Telescope) and MeerKAT H I cubes with a $1\sigma$ column density limit of $3.4\times 10^{19}$ cm$^{-2}$—placed against stellar mass maps built from Legacy Surveys $g$ and $r$ images. The quantitative engine is the classical Gunn and Gott ram-pressure criterion: ram pressure $P = \rho_{\rm IGM} \Delta v^2$ is compared with the disk's restoring force per area $2\pi G \Sigma_\star \Sigma_g$, with exponential stellar and gas profiles used to evaluate the surface densities at each galaxy's observed truncation radius. This comparison turns an observed truncation radius into a required intragroup medium density for each galaxy, which is then judged against the density range measured for more massive groups and the group's velocity dispersion.

What would settle it

A deep X-ray observation of the NGC 5364 group that measures the density of the intragroup medium at about 0.4 times the group's virial radius would settle the central claim, since the ram-pressure explanation requires that density to fall in the range $2.5\times10^{-28}$ to $4.4\times10^{-28}$ g cm$^{-3}$; a measured density below that band would leave ram pressure unable to explain more than one of the truncated disks.

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Extended reading notes

Core claim

The central claim is that combining resolved H$\alpha$ star-formation maps with MeerKAT H I imaging reveals the baryon cycle being disrupted in the NGC 5364 group, a system with dynamical mass $\log_{10}(M_{\rm halo}/M_\odot) = 12.7$ at the western edge of the Virgo III filament, more than 6 Mpc from the center of Virgo. Eight group members show a range of signatures: the two most massive disk galaxies have lopsided stars and gas, one shows truncated H I and H$\alpha$ with no tidal signature, two have H I tails and compressed leading gas consistent with ram pressure, one has extraplanar H$\alpha$ and H I, and two dwarfs are undetected in both H$\alpha$ and H I but appear in the NUV. The authors quantify ram pressure using the classical Gunn and Gott criterion, equating $\rho_{\rm IGM} \Delta v^2$ with the restoring force per area $2\pi G \Sigma_\star \Sigma_g$ at the observed truncation radius, and find that the required pressures are consistent with the expected intragroup medium density and group velocity dispersion for three of the four disk-dominated galaxies, with VFID5842 requiring conditions at the upper edge of expectations. They conclude that ram pressure stripping, tidal interactions, and starvation are all operating, and that the group's passive fraction of 3/8 is far above the field value, so environmental quenching is not confined to clusters and massive groups.

Load-bearing premise

The ram-pressure argument assumes the hot gas between the galaxies in this low-mass group is about as dense as the gas measured in heavier groups; the paper presents no direct X-ray measurement of that gas.

Editorial extensions

If this is right

  • Low-mass groups of $\log_{10}(M_{\rm halo}/M_\odot) = 12.7$ can host the same kind of environmental gas removal and star-formation truncation previously seen in clusters and more massive groups.
  • Intragroup medium ram pressure is quantitatively sufficient to explain the H I tails and truncated H$\alpha$ disks in three of the four disk-dominated galaxies studied.
  • A passive fraction of 3/8 among the imaged members, against field passive fractions of at most a few percent, means groups of this mass can quench a substantial fraction of their galaxies.
  • The correlation between the H I-to-stellar-mass ratio and the size ratio of the H$\alpha$ disk to the stellar disk will be testable with the full VFS-H$\alpha$ sample of over 600 galaxies.

Reading between the lines

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

  • A direct X-ray measurement of the group's hot gas would either confirm or refute the assumed intragroup medium density; if confirmed, this group would become a benchmark for ram-pressure stripping in the lowest-mass halos where the process has been claimed.
  • The two dwarfs with NUV emission but no H$\alpha$ or H I may be recently quenched, and follow-up optical spectroscopy could distinguish rapid ram-pressure quenching from slower starvation by their stellar ages and emission-line ratios.
  • VFID5842, the one disk galaxy that ram pressure cannot easily explain, is a clean test case for starvation or tidally assisted stripping because its stellar disk is symmetric while its gas is truncated.
  • Because the group sits inside a filament, the effective ram pressure could exceed what the group halo alone provides; comparing this group with similar-mass groups away from filaments would separate the group and filament contributions.
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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

2 major / 4 minor

Summary. This paper presents the first results from the Virgo Filament Survey-Hα for the low-mass NGC 5364 group (log10(Mhalo/Msun)=12.7), combining Isaac Newton Telescope WFC Hα narrowband imaging with Legacy Surveys g/r stellar mass maps and MeerKAT H I data for eight group members. The authors find a wide range of environmental signatures: truncated Hα and H I disks (VFID5842, VFID5892), H I tails and extraplanar Hα (VFID5855, VFID5859), tidal distortions (VFID5889, VFID5892), and gas-poor dwarfs (VFID5879, VFID5844). Using the Gunn & Gott (1972) criterion [Eq. (4)], they compare the pressure needed to explain each truncation radius with the expected intragroup medium density at ~0.4 R_vir and conclude that ram pressure stripping can explain the H I tails and truncated Hα/H I for all but one of the disk-dominated galaxies, with multiple mechanisms ('tidal interactions, ram pressure stripping, and starvation') disrupting the baryon cycle.

Significance. The observational core of the paper is strong and timely. The combination of resolved H I and Hα reveals morphological signatures that are directly visible in the figures and internally consistent, and the use of GALEX NUV and WISE 12 µm data to rule out dust as the cause of the truncated Hα disks is a careful check. The paper is also honest about the approximate nature of the ram-pressure calculation. If the quantitative claim holds, it would extend ram-pressure stripping to group halos with log M_halo ~12.7, significantly below the ~13-14 systems previously studied, and it would support the emerging picture that groups embedded in filaments are the main agents of preprocessing. The qualitative multi-mechanism interpretation does not depend on the borrowed intragroup-medium density, and the quantitative comparison is not circular: the relative velocities come from the group velocity dispersion and the density range comes from an external sample of more massive groups.

major comments (2)
  1. [Section 5.3, Figure 11, Eq. (4)] The quantitative claim that ram pressure stripping can explain the observed truncations for 'all but one' disk galaxies rests on comparing the required pressure with the cyan band of intragroup-medium densities from Sun et al. (2009), whose groups have 13 < log10(M/Msun) < 14; no X-ray detection or upper limit for the NGC 5364 intragroup medium is presented, and the authors themselves note the mass mismatch. Because Equation (4) sets the required density-velocity combination from the observed truncation radius, any factor-of-few downward shift of rho_IGM at ~0.4 R_vir in this log M_halo=12.7 group would move the VFID5892, VFID5855, and VFID5889 curves to relative velocities above the 3σ range shown in Figure 11, so the 'all but one' conclusion would reduce to a morphology-only statement. I recommend either providing an X-ray-derived density or upper limit for this system or explicitly reframing the conclusion as a consistency test rather than a quantitative explanation.
  2. [Section 5.3, Eqs. (5)-(6)] The restoring-force calculation adopts a fixed gas-to-stellar scale-length ratio of 1.7 and truncation radii determined by eye from the Hα/H I images, but no uncertainties are propagated into the curves in Figure 11; the VFID5842 curve is judged to lie at the upper edge of the expected region, and the three 'consistent' curves are not accompanied by error bars that would show whether such a conclusion is robust to realistic changes in Rd,gas and R_trunc. Please add a quantitative sensitivity test (e.g., varying Rd,gas/Rd,stars between 1.2 and 2.5 and assigning conservative uncertainties to R_trunc) or state the precision limits of the comparison.
minor comments (4)
  1. [Sections 2 and 3.1] The text refers to the 'NGC 5346 Group' in two places, while the paper is about the NGC 5364 group; please correct the name consistently.
  2. [Section 5.3] The sentence listing 'four disk-dominated galaxies (VFID5842, VFID5855, VFID5851, VFID5892)' is inconsistent with Section 4.1.1, where VFID5851 is described as an elliptical; if the intended galaxy is VFID5889, please correct the list and the accompanying 'all but one' counting.
  3. [Figure 11 caption] The caption says 'the gray shaded region shows +3σV,' which is not a full sentence; please specify which axis the 3σ region spans and what value of σV is used.
  4. [Table 1] The Hα flux correction column is headed '3d' with a note describing '1/T(z)', which is confusing; a clearer column header would help readers understand the correction.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the RPS consistency check uses independent velocity-dispersion and external IGM-density inputs.

full rationale

The quantitative ram-pressure analysis is not circular. The required pressure is computed from observed truncation radii via Eq. (4) with stellar and gas surface densities from Eqs. (5)-(6), and is then compared against two independently measured quantities: the group velocity dispersion (from Kourkchi & Tully 2017, sigma_V = 155 km/s, and the authors' own biweight estimate of 164 km/s) and the intragroup medium density range for more massive groups from Sun et al. (2009) as compiled by Boselli et al. (2022). Neither the velocity dispersion nor the IGM density is derived from the observed truncation radii, so the 'all but one' claim is a genuine consistency check rather than a tautology. The paper explicitly flags the halo-mass mismatch (13 < log M/Msun < 14 versus log Mhalo/Msun = 12.7) as a caveat; that is an assumption or uncertainty, not circularity. The paper does rely on companion papers (Castignani et al. 2022a,b; Conger et al. 2025; Ramatsoku et al. in prep) for group membership, SED stellar masses and SFRs, H2 deficiencies, and H I maps, but these are independent data products rather than restatements of the paper's conclusions. No equation reduces to its own input, no fitted parameter is renamed as a prediction, and no uniqueness theorem is imported from the authors' prior work. Therefore no circular step is identified.

Assumptions & free parameters 2 free parameters · 6 assumptions · 0 invented entities

The central claim rests on standard galaxy-evolution diagnostics plus two hand-chosen quantitative inputs: the gas-to-stellar scale length ratio and the borrowed intragroup medium density range. The Gunn and Gott criterion and the exponential disk assumption are standard but still modeling choices. No new physical entities are introduced.

free parameters (2)
  • Gas-to-stellar disk scale length ratio = 1.7
    Adopted from Cayatte et al. (1994) and Jaffe et al. (2015) in Equation 6. The computed restoring forces in Figure 11 depend on this ratio, which is not measured directly for these galaxies.
  • Intragroup medium density range = 2.5 to 4.4 x 10^-28 g cm^-3
    Taken from Sun et al. (2009) for groups with 13 < log(M/M_sun) < 14 as compiled in Boselli et al. (2022), used as the cyan comparison band in Figure 11. The NGC 5364 group has log(M_halo/M_sun) = 12.7 and is not directly detected in X-rays.
assumptions (6)
  • domain assumption Gunn and Gott (1972) ram pressure criterion: gas is stripped where ram pressure equals the disk restoring force per area.
    Used in Equations 2 through 4 to convert observed truncation radii to required intragroup pressures. This simple instantaneous balance ignores orbital geometry, disk inclination, and ISM inhomogeneity.
  • domain assumption Exponential stellar and gas disk profiles, with the gas scale length 1.7 times the stellar scale length.
    Equations 5 and 6 assume exponential distributions; the derived surface densities at the truncation radius follow from this assumed profile shape and the adopted scale length ratio.
  • domain assumption Group membership, velocity dispersion, and dynamical mass from Kourkchi and Tully (2017).
    Section 2 adopts the catalog membership and mass. All environmental attributions assume the 17 galaxies form a bound group rather than a line-of-sight coincidence.
  • domain assumption Intragroup medium properties of NGC 5364 are comparable to those of more massive groups.
    Section 5.3 and Figure 11 use an ICM density range from 13 < log(M/M_sun) < 14 groups because no X-ray measurement of this group's hot gas exists.
  • domain assumption H-alpha luminosity traces recent star formation through the Kennicutt and Evans (2012) calibration.
    Section 3.2 converts continuum-subtracted H-alpha to SFR maps. The calibration can break down at low SFRs and on small spatial scales, as the paper itself notes.
  • domain assumption The Virgo Cluster does not contribute significantly to stripping of these galaxies.
    Section 5.1 argues this from a projected distance of roughly 6 Mpc and an extrapolated eROSITA density profile; the extrapolation extends beyond the profile's fitted range.

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Cite this review

Pith. "Pith review of Virgo Filaments V: Disrupting the Baryon Cycle in the NGC 5364 Galaxy Group." pith.science (2026). https://pith.science/paper/T5HWKZQA

@misc{pith2026250509782,
  author       = {Pith},
  title        = {Pith review of: Virgo Filaments V: Disrupting the Baryon Cycle in the NGC 5364 Galaxy Group},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/T5HWKZQA}},
  note         = {Machine review of arXiv:2505.09782}
}
abstract

The Virgo Filament Survey (VFS) is a comprehensive study of galaxies that reside in the extended filamentary structures surrounding the Virgo Cluster, out to 12 virial radii. The primary goal is to characterize all of the dominant baryonic components within galaxies and to understand whether and how they are affected by the filament environment. A key constituent of VFS is a narrowband H$\alpha$ imaging survey of over 600 galaxies, VFS-H$\alpha$. The H$\alpha$ images reveal detailed, resolved maps of the ionized gas and massive star-formation. This imaging is particularly powerful as a probe of environmentally-induced quenching because different physical processes affect the spatial distribution of star formation in different ways. In this paper, we present the first results from the VFS-H$\alpha$ for the NGC~5364 group, a low-mass ($\log_{10}(M_{dyn}/M_\odot) < 13)$ system located at the western edge of the Virgo~III filament. We combine H$\alpha$ imaging with resolved H~I observations from MeerKAT for eight group members. These galaxies exhibit peculiar morphologies, including strong distortions in the stars and the gas, truncated H~I and H$\alpha$ disks, H~I tails, extraplanar H$\alpha$ emission, and off-center H$\alpha$ emission. These signatures are suggestive of environmental processing such as tidal interactions, ram pressure stripping, and starvation. We quantify the role of ram pressure stripping expected in this group, and find that it can explain the cases of H~I tails and truncated H-alpha for all but one of the disk-dominated galaxies. Our observations indicate that multiple physical mechanisms are disrupting the baryon cycle in these group galaxies.

Figures

Figures reproduced from arXiv: 2505.09782 by the authors.

Figure 1
Figure 1. Location of the NGC 5364 Group on the plane of the sky relative to the Virgo Cluster and surrounding large-scale structure covered by the Virgo Filament Survey. The magenta line shows the Virgo III filament spine, and the gray lines show the spines of the other filaments identified by Castignani et al. (2022b). The NGC 5364 group galaxies are shown with the cyan circles. The group is located at the western end of th… view at source ↗
Figure 2
Figure 2. Decl. vs. R.A. for the 17 NGC 5364 group members. Circles are color coded by stellar mass, and the size of the circles scales with the isophotal size of the galaxies. The black rectangles show the approximate location of the four detectors of the Wide Field Camera. The eight group members within the Hα field of view are the focus of this paper. The cyan X shows the mass-weighted center of the group. We did not obtai… view at source ↗
Figure 3
Figure 3. Legacy DR9 grz image showing the location of group members. The dashed cyan line shows the location of the Virgo III filament spine, projected in R.A. and decl. Group members are labeled with their VFID (Castignani et al. 2022b). galaxies within the Hα FOV. We present the galaxies in order of decreasing stellar mass. We discuss these results in the context of previous work in Section 5.2. 4.1.1. The Two Most Massive… view at source ↗
Figures from the paper (8 more)
Figure 4
Figure 4. Figure 4: Results for the two most massive (log10(M⋆/M⊙) > 10) galaxies in the group. (Top) VFID5851, the most massive galaxy and central elliptical. The left panel shows the Legacy grz color image, with log(M⋆/M⊙) written in the lower left and a scale bar in the top left. The s…
Figure 5
Figure 5. Figure 5: Results for the three 9 < log10(M⋆/M⊙) ≤ 10 group galaxies: VFID5842 (top), VFID5855 (middle), and VFID5892 (bottom). The left panel shows the Legacy grz color image, with log(M⋆/M⊙) noted in the lower left and a scale bar in the top left. The second panel shows the st…
Figure 6
Figure 6. Figure 6: Multiwavelength SFR indicators NUV, Hα, and Wide-field Infrared Survey Explorer (WISE) 12µm for (top) VFID5842 and (bottom) VFID5892. Both galaxies show truncated Hα emission, and the NUV and IR show a similar extent to Hα. This indicates that dust is not causing the t…
Figure 7
Figure 7. Figure 7: Results for 7.5 < log10(M⋆/M⊙) < 8.5 group galaxies, with galaxies ordered from top to bottom by decreasing stellar mass. The left panel shows the Legacy grz color image, with log(M⋆/M⊙) written in the lower left and a scale bar in the top left. The second panel shows …
Figure 8
Figure 8. Figure 8: Legacy grz color image of VFID5859 with MeerKAT H I contours shown in gray. This figure provides a zoomed-out image that includes the full H I tail that is not captured in [PITH_FULL_IMAGE:figures/full_fig_p012_8.png]
Figure 9
Figure 9. Figure 9: (Left) SFR vs. stellar mass for the full Virgo Filament Survey sample (gray) and the group members (squares). For group members on the Hα image, the squares are color coded by the ratio of R90(SFR)/R90(M⋆). The remaining group members are shown with the gray squares. T…
Figure 10
Figure 10. Figure 10: (Left) decl. vs. R.A. of NGC 5364 group members compared to Virgo Cluster members. (Right) Recession velocity vs. projected angular separation from the center of Virgo. Black lines show the model for the escape velocity from Castignani et al. (2022b). of both gravitat…
Figure 11
Figure 11. Figure 11: To illustrate the potential influence of ram pres￾sure stripping, we plot the relative velocity of galaxy with respect to group center vs. the density of the ICM. The solid diagonal lines show lines of constant pressure, and each line reflects the pressure required to…

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