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REVIEW 3 major objections 5 minor 139 references

The ViCTORIA project: description of a multi-frequency radio survey of the Virgo galaxy cluster

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

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Pith's one-line read ViCTORIA's radio surveys map Virgo about 60 times deeper than NVSS, and M87's lobes turn out to be full of filaments, including a rare synchrotron thread joining them.

desk verdict A well-crafted survey description that is honest about what is simulated versus what is in hand; the LBA depth is the one real risk, but the project deserves a serious referee. read the letter →

arxiv 2411.18204 v2 pith:6YXGK3FW submitted 2024-11-27 astro-ph.CO

F. de Gasperin , H.W. Edler , A. Boselli , P. Serra , M. Fossati , V. Heesen , A. Merloni , M. Murgia
show 3 more authors
T.H. Reiprich A. Spasic N. Zabel
This is my paper · ORCID
classification astro-ph.CO
keywords VirgoclusterradiosurveysM87LOFARMeerKATneutralhydrogensynchrotronfilamentsgalaxyevolution
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

The paper describes ViCTORIA, a coordinated set of three blind radio surveys of the Virgo cluster with LOFAR and MeerKAT covering 42–1712 MHz. Its central assertion is that a calibration strategy centred on peeling the overpowering emission of M87 makes it possible to image the entire cluster out to r200 about sixty times deeper than existing NVSS data, in full polarisation, while the companion H I survey should detect roughly seven times more galaxies than earlier experiments. Since Virgo is the nearest rich cluster, reaching this depth would let astronomers study galaxy evolution and ram-pressure stripping down to dwarf galaxies and low-column-density gas. The project's first images, presented as preliminary results, show M87's radio lobes filled with coherent filamentary structures, including the second known collimated synchrotron thread connecting the two lobes.

What carries the argument

The load-bearing technical mechanism is the 'peeling' step in the calibration chain. Before direction-dependent calibration, the interferometric visibilities are phase-shifted toward M87, solved against a high-quality model of the bright source, and M87 is subtracted from the full-resolution data; the field is then phase-shifted back and processed. This removes the dynamic-range killer that has limited earlier wide-area surveys of Virgo. The survey design also uses overlapping pointings, parallel multi-beam observations, and a simulated quasi-thermal noise calculation that sets the sensitivity expectations (about 1.7 mJy/beam for the 42–66 MHz survey in the overlap region).

What would settle it

Recompute the final LBA mosaic's median off-source rms in the overlap region and re-image the M87 field with different deconvolution settings: a noise well above the simulated ~1.7 mJy/beam would falsify the 60x depth claim, and disappearance of the thread between the ears would falsify the CST claim.

Watch

Extended reading notes

Core claim

The paper claims that a dedicated, M87-peeling calibration strategy makes it possible to obtain blind, high-fidelity radio images of the entire Virgo cluster, and that the first such images reveal that the radio lobes of M87 are not smooth cavities but volumes filled with complex synchrotron filaments. In particular, the 144 MHz image (with 4''×3'' resolution) shows a collimated synchrotron thread connecting the eastern and western 'ears' of the source below the central cocoon, only the second such structure ever observed. The same dataset yields the highest-resolution images of Virgo A at 54 and 1284 MHz, enabling resolved spectral studies. The authors present this as strong evidence that the lobes are threaded by coherent magnetic-field structures and that Rayleigh–Taylor instabilities shape both ears symmetrically.

Load-bearing premise

The sixty-fold depth improvement rests on the assumption that the M87 peeling and direction-dependent calibration will reach the simulated noise of about 1.7 mJy/beam across the entire 42–66 MHz LBA survey, a level demonstrated only for the HBA survey and a five-pointing MeerKAT pilot so far.

Editorial extensions

If this is right

  • Final continuum mosaics at 42–66, 120–168, and 856–1712 MHz should reach roughly 1700, 150, and 7 $\mu$Jy beam$^{-1}$, about 60 times the depth and six times the resolution of NVSS at 1.4 GHz.
  • The blind H I survey should resolve ~370 galaxies down to $M_{\rm HI} \simeq 2\times10^6\,M_\odot$ and map ram-pressure-stripped tails at column densities in the range $10^{18}$–$10^{20}$ cm$^{-2}$.
  • The polarization data should yield roughly 2000–3700 rotation measure sources, enough to map the cluster magnetic field and test whether compressed fields boost radio emission near the cluster centre.
  • The M87 images imply the lobes are filled with filamentary synchrotron structures and that Rayleigh–Taylor instabilities shape both ears, so the jet–ICM interaction is more structured than smooth-lobe models assume.
  • Combining the three frequencies gives resolved spectral index and curvature maps of every source with $S_{144\,\mathrm{MHz}} > 450\,\mu$Jy beam$^{-1}$, tracing particle ageing along stripped tails.

Reading between the lines

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

  • If the lobe-connecting thread is confirmed, it implies the two ears of M87 are magnetically connected; the survey's Faraday rotation data could test whether the thread carries a coherent field by looking for a systematic RM gradient along it.
  • A natural extension is to search for similar collimated synchrotron threads in other nearby radio galaxies; the detection rate would constrain how long such connections survive relative to the lobe expansion timescale.
  • The advertised depth also implies that the survey should detect radio emission from stripped and accreting gas far beyond galaxy stellar disks, providing an unbiased census that existing pointed samples like VIVA cannot offer.
  • If the simulated LBA noise is reached, the 42–66 MHz survey becomes the deepest low-frequency view of any rich cluster, which would anchor studies of faint fossil radio plasma and cluster halos at low frequency.
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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

3 major / 5 minor

Summary. This paper describes the ViCTORIA project, a multi-frequency radio survey of the Virgo galaxy cluster using LOFAR LBA, LOFAR HBA, and MeerKAT L-band observations. It presents the survey footprints, observing strategies, calibration plans, and expected noise levels, and compares the planned depth with existing surveys such as NVSS, TGSS, RACS, and GLEAM. The paper also reports preliminary data products: H I maps that recover and extend VIVA and ALFALFA detections for galaxies and cloud complexes, and high-resolution images of M87 that show filamentary structure within the lobes, including a candidate collimated synchrotron thread. The stated aims are to deliver continuum images about 60 times deeper than current surveys, a blind H I survey sensitive to dwarf galaxies, and polarization data for thousands of sources.

Significance. If the projected sensitivities are achieved, ViCTORIA will be a benchmark dataset for the Virgo cluster, enabling studies of environmental quenching, ram-pressure stripping, AGN feedback, and cluster magnetic fields at physical scales of ~500 pc over the full r200 region. The published HBA survey and the five-pointing MeerKAT pilot give strong empirical support for the HBA and L-band pillars, and the public release of HBA data and the use of the open-source LiLF pipeline are commendable. The M87 images illustrate the potential of the combined dataset. The main caveat is that the LBA depth is still based on a simulation and the polarization source counts are partially based on private communication, so the numerical projections should be read as expectations rather than fully demonstrated survey performance.

major comments (3)
  1. [Section 2.1.1, Table 1] The quoted LBA sensitivity (1.7–2.2 mJy/beam) is derived from a quasi-thermal noise simulation, and the text states that a peeling strategy for M87 'will be employed' but does not demonstrate that it has been applied to the LBA data. Because the abstract and Section 2.2 claim that the project will deliver images 'about 60 times deeper' from 42 MHz to 1.7 GHz, this depth claim for the LBA band currently rests on an unverified calibration assumption. If the peeling or direction-dependent calibration fails, off-source artifacts around M87 could raise the effective noise over a large fraction of the 166 deg^2 footprint. Please either provide a representative validation (e.g., a single calibrated LBA field processed with the described peeling and direction-dependent calibration) or explicitly qualify the LBA noise and the 60x statement as a projected goal that has not yet been demonstrated.
  2. [Section 2.2 vs Section 4.5] The expected yield of the polarization survey is stated as 'an estimated 2000 objects through RM synthesis' in the deliverable list (Section 2.2, citing a private communication) but as 3677 polarized sources in Section 4.5, following Rudnick & Owen (2014). The footnote in Section 4.5 notes that MIGHTEE early science suggests a factor-2 underestimation, which makes the two numbers even harder to reconcile. Since the polarisation survey is one of the three core deliverables, please reconcile these estimates, specify the detection threshold and survey area used for each, and replace the private communication with a citable public reference or a transparent extrapolation.
  3. [Section 4.2, Figures 8 and 9] The claimed detection of filamentary structures filling the M87 lobes and 'the second known case of CST' is a striking scientific result, but the paper provides only visual evidence and defers quantitative spectral analysis to de Gasperin et al. (in prep.). If this result is to remain in the survey-description paper, it needs quantitative support (e.g., surface-brightness detection significance, intensity profiles, or comparison with the X-ray filaments). Otherwise, it should be presented more clearly as an early, qualitative preview with the detailed analysis to follow.
minor comments (5)
  1. [Section 2.1.2, Table 1] The resolution listed in Table 1 (7 arcsec) differs from the quoted '9''x5'' (high)' and '20'' (low)' mosaics; please clarify whether 7 arcsec is the best common resolution or a representative value.
  2. [Section 2.2] The statement 'No other large survey of the Virgo cluster has been attempted at these frequencies' is too strong given that LoTSS, TGSS, and VLSSr cover the region; rephrase to emphasize the improved depth, fidelity, and dedicated calibration.
  3. [Section 4.1] There is a typo in 'magneto-hdyrdodynamic waves'; it should be 'magnetohydrodynamic waves'.
  4. [Section 4.5] The number 3677 for polarized sources is given with two significant figures and a footnote indicating a factor-2 uncertainty; please round appropriately and state the uncertainty in the main text.
  5. [References] The reference list contains duplicates (e.g., Boselli et al. 2014; Gunn & Gott 1972; Boselli et al. 2018) and LaTeX artifacts in author names such as 'V ollmer'; please clean the bibliography.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the survey's quantitative claims are benchmarked against external surveys and scaling relations, not fitted to the new data.

full rationale

I find no significant circularity. The paper is a survey description; its central quantitative claims are sensitivity specifications (Table 1), comparisons against external surveys (NVSS, RACS, TGSS, VLSSr, VIVA, ALFALFA), and extrapolated source counts using external scaling relations (Boselli et al. 2015; Rudnick & Owen 2014; O'Sullivan et al. 2023). The '60 times deeper' statement is an arithmetic comparison of Table 1 sensitivities with published NVSS noise, not a value fitted to the new data. The LBA noise levels in Section 2.1.1 are explicitly derived from a simulation using van Haarlem et al. (2013) source-equivalent flux densities; this is a stated planning assumption rather than a fitted parameter, and the text properly indicates that the M87 peeling strategy 'will be employed' rather than claiming the calibration is already demonstrated. Self-citations (the LiLF pipeline, the Edler et al. 2023 HBA survey, and de Gasperin et al. in prep.) describe software, a previous data release, and forthcoming analysis; none carries the load of deriving a ViCTORIA result, and the HBA survey's 112 detections are presented as a published external data product. The M87 filamentary structures and the collimated synchrotron thread are presented as preliminary images with deferred detailed analysis, and the text explicitly attributes the earlier known filamentary morphology of the inner cocoon to Owen et al. (2000), so no known result is being renamed as a new prediction. No step reduces by construction to its own input, and no load-bearing uniqueness theorem or ansatz is imported from the authors' prior work.

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

No new physical entities are introduced. The filamentary structures and collimated synchrotron thread are observed features, not postulates. All quantitative expectations come from prior literature and scaling relations.

assumptions (5)
  • domain assumption Flat Lambda-CDM cosmology with Omega_m=0.3 and H0=70 km/s/Mpc
    Stated in Section 1 and used for all distance and mass conversions.
  • domain assumption Virgo distance of 16.5 Mpc (Mei et al. 2007)
    Adopted in Section 1; uncertainty of +/-1.1 Mpc is acknowledged.
  • domain assumption r200 = 1.55 Mpc determined from the galaxy distribution
    Footnote 1; this value is larger than X-ray-derived values of about 1 Mpc, affecting the survey footprint and cluster boundary definition.
  • domain assumption The H-alpha-radio correlation (Boselli et al. 2015) is used to predict ~330 continuum detections
    Section 2.2; the prediction inherits the scatter and calibration of that relation.
  • domain assumption The expected number of polarized sources follows Rudnick & Owen (2014) with a 6-sigma threshold
    Section 4.5; also notes MIGHTEE suggests this may be underestimated by a factor of 2.

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Cite this review

Pith. "Pith review of The ViCTORIA project: description of a multi-frequency radio survey of the Virgo galaxy cluster." pith.science (2026). https://pith.science/paper/6YXGK3FW

@misc{pith2026241118204,
  author       = {Pith},
  title        = {Pith review of: The ViCTORIA project: description of a multi-frequency radio survey of the Virgo galaxy cluster},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/6YXGK3FW}},
  note         = {Machine review of arXiv:2411.18204}
}
read the original abstract

The Virgo cluster is the closest richest nearby galaxy cluster. It is in the formation process, with a number of sub-clusters undergoing merging and interactions. Although a great laboratory to study galaxy evolution and cluster formation, its large apparent size and the severe dynamic range limitations due to the presence of the bright radio source Virgo A (M 87) reduced the ability of past wide-area radio surveys to image the region with high sensitivity and fidelity. In this paper we describe the "Virgo Cluster multi-Telescope Observations in Radio of Interacting galaxies and AGN" (ViCTORIA) project. The survey and its data reduction strategy are designed to mitigate the challenges of this field and deliver: images from 42 MHz to 1.7 GHz frequencies of the Virgo cluster, about 60 times deeper than existing data, in full polarisation, and including a blind HI survey that aims at mapping seven times more galaxies than previous experiments and without selection biases. Data have been collected with the Low-Frequency Array (LOFAR) and with MeerKAT in L-band, including polarisation and enough frequency resolution to conduct local HI studies. At the distance of Virgo, current radio instruments have the resolution to probe scales of ~500 pc and the sensitivity to study dwarf galaxies, the most fragile systems given their shallow gravitational potential wells, making Virgo a unique laboratory to study galaxy evolution and AGN feedback in a rich environment. In this work, we present some preliminary results, including high resolution images of the radio emission surrounding M 87, that show that the lobes are filled with filamentary structures. The combination of the presented radio surveys with state-of-the-art optical, UV, X-ray surveys will massively increase the scientific output from the studies of the Virgo cluster, making the ViCTORIA Project's legacy value outstanding.

Figures

Figures reproduced from arXiv: 2411.18204 by the authors.

Figure 1
Figure 1. Frequency – sensitivity plot comparing large radio sur￾veys covering the Virgo cluster. The size of the markers scales linearly with resolution from 7′′ of ViCTORIA LOFAR HBA to 150 ′′ of GLEAM. The sensitivity is derived from the Virgo re￾gion. References: GLEAM (GaLactic and Extragalactic All-sky Murchison Widefield Array survey; Hurley-Walker et al. 2017), TGSS ADR1 (TIFR GMRT Sky Survey - Alternative Data Releas… view at source ↗
Figure 2
Figure 2. Coverage of ViCTORIA project surveys. In green are the pointings at mid-frequency FWHM of the MeerKAT Virgo Survey designed to fill the orange region covered by NGVS in optical and VESTIGE in H α. In light and dark blue are the cov￾erages of LOFAR LBA and HBA, respectively (mid-frequency FWHM). The red dashed line is the estimated r200. The con￾tours trace the X-ray emission from ROSAT (Bohringer et al. ¨ 1994), gre… view at source ↗
Figure 3
Figure 3. MeerKAT L-band data mosaic of five pointings cover￾ing M87 and moving towards the north-east. These fields were used as a pilot experiment to derive a good calibration strategy. The dynamic range limitation due to the presence of the bright radio emission from M87 is evident in the increased rms noise in the pointings where the source is within the primary beam. The expected noise and resolution, confirmed by the pi… view at source ↗
Figures from the paper (6 more)
Figure 4
Figure 4. Figure 4: H i gas distribution of perturbed galaxy NGC 4424 seen by ViCTORIA. For each resolution, we show the lowest re￾liable contour (3σ over a line width of 25 km s−1 ). The contours are overlaid on an r-band image downloaded from the Legacy Survey database. The contour leve…
Figure 5
Figure 5. Figure 5: H i clouds detected during ALFALFA survey by Kent et al. (2009) as seen by ViCTORIA. For each resolution, we show the lowest reliable contour (3σ over a line width of 25 km s −1 ). The contours are overlaid on an r-band image downloaded from the Legacy Survey database.…
Figure 6
Figure 6. Figure 6: Comparison of various surveys in L band: ViCTORIA MeerKAT (from the pilot fields shown in [PITH_FULL_IMAGE:figures/full_fig_p008_6.png]
Figure 7
Figure 7. Figure 7: H i gas distribution of NGC 4523. For each resolution, we show the lowest reliable contour (3σ over a line width of 25 km s−1 ). The contours are overlaid on an r-band image down￾loaded from the Legacy Survey database. The contour levels and resolutions are listed in t…
Figure 8
Figure 8. Figure 8: Virgo A (the radio emission associated with M87) as seen by the three ViCTORIA surveys (de Gasperin et al. in prep.). From left to right: LOFAR LBA (54 MHz, beam: 16′′×12′′), LOFAR HBA (144 MHz, beam: 4′′×3 ′′ including LOFAR international stations), and MeerKAT L band…
Figure 9
Figure 9. Figure 9: Extract from central panel of [PITH_FULL_IMAGE:figures/full_fig_p010_9.png]

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Works this paper leans on

139 extracted references · 57 canonical work pages

  1. [1]

    Adams, E. A. K., Giovanelli, R., & Haynes, M. P. 2013, ApJ, 768, 77

    2013

  2. [2]

    Aguerri, J. A. L., Gerhard, O. E., Arnaboldi, M., et al. 2005, Astron. J., 129, 2585

    2005

  3. [3]

    2005, in AIP Conf

    Arnaboldi, M. 2005, in AIP Conf. Proc., V ol. 804, 301–308

    2005

  4. [4]

    W., et al

    Auld, R., Bianchi, S., Smith, M. W., et al. 2013, MNRAS, 428, 1880

    2013

  5. [5]

    2015, ApJ, 800, L15

    Bellazzini, M., Magrini, L., Mucciarelli, A., et al. 2015, ApJ, 800, L15

    2015

  6. [6]

    J., Galliano, F., & Madden, S

    Bendo, G. J., Galliano, F., & Madden, S. C. 2012, MNRAS, 423, 197

    2012

  7. [7]

    Bianchi, S., Giovanardi, C., Smith, M. W. L., et al. 2017, A&A, 597, A130

    2017

  8. [8]

    1985, Astron

    Binggeli, B. 1985, Astron. J., 90, 1681

    1985

Show all 139 references
  1. [9]

    A., & Sandage, A

    Binggeli, B., Tammann, G. A., & Sandage, A. 1987, Astron. J., 94, 251 B¨ohringer, H., Briel, U. G., Schwarz, R. A., et al. 1994, Nature, 368, 828

    1987

  2. [10]

    2015, A&A, 579, A29

    Boissier, S., Boselli, A., V oyer, E., et al. 2015, A&A, 579, A29

    2015

  3. [11]

    2010, A&A, 513, A30

    Bonafede, A., Feretti, L., Murgia, M., et al. 2010, A&A, 513, A30

    2010

  4. [12]

    2009, ApJ, 706, 1527

    Boselli, A., Boissier, S., Cortese, L., et al. 2009, ApJ, 706, 1527

    2009

  5. [13]

    2011, A&A, 528, A107

    Boselli, A., Boissier, S., Heinis, S., et al. 2011, A&A, 528, A107

    2011

  6. [14]

    C., Fossati, M., et al

    Boselli, A., Cuillandre, J. C., Fossati, M., et al. 2016, A&A, 587, A68

    2016

  7. [15]

    2018, A&A, 614, A56

    Boselli, A., Fossati, M., Ferrarese, L., et al. 2018, A&A, 614, A56

    2018

  8. [16]

    2015, A&A, 579, A102

    Boselli, A., Fossati, M., Gavazzi, G., et al. 2015, A&A, 579, A102

    2015

  9. [17]

    2022, Astron

    Boselli, A., Fossati, M., & Sun, M. 2022, Astron. Astrophys. Rev., 30, 3

    2022

  10. [18]

    & Gavazzi, G

    Boselli, A. & Gavazzi, G. 2006, PASP, 118, 517

    2006

  11. [19]

    2021, A&A, 646, A139

    Boselli, A., Lupi, A., Epinat, B., et al. 2021, A&A, 646, A139

    2021

  12. [20]

    2003, A&A, 406, 867

    Boselli, A., Sauvage, M., Lequeux, J., Donati, A., & Gavazzi, G. 2003, A&A, 406, 867

    2003

  13. [21]

    J., Gavazzi, G., Hippelein, H., & Pierini, D

    Boselli, A., Tuffs, R. J., Gavazzi, G., Hippelein, H., & Pierini, D. 1997, A&AS, 121, 507

    1997

  14. [23]

    2014, A&A, 570, A69

    Boselli, A., V oyer, E., Boissier, S., et al. 2014, A&A, 570, A69

    2014

  15. [24]

    D., Zabel, N., et al

    Brown, T., Wilson, C. D., Zabel, N., et al. 2021, Astrophys. J. Suppl. Ser., 257, 21

    2021

  16. [25]

    P., Ferrarese, L., et al

    Cantiello, M., Blakeslee, J. P., Ferrarese, L., et al. 2024, ApJ, 966, 145

    2024

  17. [26]

    P., Ferrarese, L., et al

    Cantiello, M., Blakeslee, J. P., Ferrarese, L., et al. 2018, ApJ, 856, 126

    2018

  18. [27]

    J., Merritt, D., & Baldi, R

    Capetti, A., Kharb, P., Axon, D. J., Merritt, D., & Baldi, R. D. 2009, Astron. J., 138, 1990

    2009

  19. [28]

    2018, MNRAS, 476, 875

    Catinella, B., Saintonge, A., Janowiecki, S., et al. 2018, MNRAS, 476, 875

    2018

  20. [29]

    2023, A&A, 671, A118

    Cattorini, F., Gavazzi, G., Boselli, A., & Fossati, M. 2023, A&A, 671, A118

    2023

  21. [30]

    2020, MNRAS, 496, 4654

    Chen, H., Sun, M., Yagi, M., et al. 2020, MNRAS, 496, 4654

    2020

  22. [31]

    H., Kenney, J

    Chung, A., Van Gorkom, J. H., Kenney, J. D., Crowl, H., & V ollmer, B. 2009, Astron. J., 138, 1741

    2009

  23. [32]

    H., Kenney, J

    Chung, A., van Gorkom, J. H., Kenney, J. D. P., & V ollmer, B. 2007, ApJ, 659, L115

    2007

  24. [33]

    & Kaiser, C

    Churazov, E. & Kaiser, C. 2001, ApJ, 10, 261

    2001

  25. [34]

    Ciesla, L., Boselli, A., Smith, M. W. L., et al. 2012, A&A, 543, A161

    2012

  26. [35]

    J., Cotton, W

    Condon, J. J., Cotton, W. D., Greisen, E. W., et al. 1998, Astron. J., 8065, 1693

    1998

  27. [36]

    2011, MNRAS, 415, 1797

    Cortese, L., Catinella, B., Boissier, S., Boselli, A., & Heinis, S. 2011, MNRAS, 415, 1797

    2011

  28. [37]

    2014, MNRAS, 440, 942

    Cortese, L., Fritz, J., Bianchi, S., et al. 2014, MNRAS, 440, 942

    2014

  29. [38]

    P., Ferrarese, L., et al

    Cote, P., Blakeslee, J. P., Ferrarese, L., et al. 2004, Astrophys. J. Suppl. Ser., 153, 223

    2004

  30. [39]

    I., Baes, M., Bendo, G

    Davies, J. I., Baes, M., Bendo, G. J., et al. 2010, A&A, 518, L48 De Gasperin, F., Brunetti, G., Bruggen, M., et al. 2020a, A&A, 642, A85 De Gasperin, F., Dijkema, T. J., Drabent, A., et al. 2019, A&A, 622, A5 De Gasperin, F., Mevius, M., Ra fferty, D. A., Intema, H. T., & Fal...

    2010

  31. [40]

    1980, ApJ, 236, 351

    Dressler, A. 1980, ApJ, 236, 351

    1980

  32. [41]

    W., Thomson, A

    Duchesne, S. W., Thomson, A. J., Pritchard, J., et al. 2023, Publ. Astron. Soc. Aust., 40, e034

    2023

  33. [42]

    W., De Gasperin, F., Shimwell, T

    Edler, H. W., De Gasperin, F., Shimwell, T. W., et al. 2023, A&A, 676, A24

    2023

  34. [43]

    W., Roberts, I

    Edler, H. W., Roberts, I. D., Boselli, A., et al. 2024, A&A, 683, A149 Event Horizon Telescope Collaboration, Akiyama, K., Alberdi, A., et al. 2019, Astrophys. J. Lett., 875, L1

    2024

  35. [44]

    1992, Astrophys

    Fabbiano, G., Kim, D.-W., & Trinchieri, G. 1992, Astrophys. J. Suppl. Ser., 80, 531

    1992

  36. [45]

    Fabian, A. C. 2012, Annu. Rev. Astron. Astrophys., 50, 455

    2012

  37. [46]

    C., et al

    Ferrarese, L., C ˆot´e, P., Cuillandre, J. C., et al. 2012, Astrophys. Journal, Suppl. Ser., 200, 4

    2012

  38. [47]

    A., et al

    Ferrarese, L., Cˆot´e, P., MacArthur, L. A., et al. 2020, ApJ, 890, 128

    2020

  39. [48]

    2007, ApJ, 665, 1057

    Forman, W., Jones, C., Churazov, E., et al. 2007, ApJ, 665, 1057

    2007

  40. [49]

    2016, MNRAS, 455, 2028

    Fossati, M., Fumagalli, M., Boselli, A., et al. 2016, MNRAS, 455, 2028

    2016

  41. [50]

    2008, ApJ, 680, 154

    Gallo, E., Treu, T., Jacob, J., et al. 2008, ApJ, 680, 154

    2008

  42. [51]

    J., et al

    Gallo, E., Treu, T., Marshall, P. J., et al. 2010, ApJ, 714, 25

    2010

  43. [52]

    2002, ApJ, 576, 135

    Gavazzi, G., Bonfanti, C., Sanvito, G., Boselli, A., & Scodeggio, M. 2002, ApJ, 576, 135

    2002

  44. [53]

    1991, AJ, 101, 1207

    Gavazzi, G., Boselli, A., & Kennicutt, R. 1991, AJ, 101, 1207

    1991

  45. [54]

    2005, A&A, 429, 439

    Gavazzi, G., Boselli, A., Van Driel, W., & O’Neil, K. 2005, A&A, 429, 439

    2005

  46. [55]

    1995, A&A, 304, 325

    Gavazzi, G., Contursi, A., Carrasco, L., et al. 1995, A&A, 304, 325

    1995

  47. [56]

    2013, H α 3: An H α imaging survey of HI selected galaxies from ALFALFA : Star formation properties of galaxies in the Virgo cluster and surroundings

    Gavazzi, G., Fumagalli, M., Fossati, M., et al. 2013, H α 3: An H α imaging survey of HI selected galaxies from ALFALFA : Star formation properties of galaxies in the Virgo cluster and surroundings

    2013

  48. [57]

    Geller, M. J. & Huchra, J. P. 1989, Mapping the universe

    1989

  49. [58]

    P., Kent, B

    Giovanelli, R., Haynes, M. P., Kent, B. R., et al. 2005, Astron. J., 130, 2598

    2005

  50. [59]

    Gunn, J. E. & Gott, J. Richard, I. 1972, ApJ, 176, 1

    1972

  51. [60]

    E., Gott, J

    Gunn, J. E., Gott, J. R., & Gott, J. Richard, I. 1972, ApJ, 176, 1

    1972

  52. [61]

    P., Giovanelli, R., & Kent, B

    Haynes, M. P., Giovanelli, R., & Kent, B. R. 2007, ApJ, 665, L19

    2007

  53. [62]

    P., Giovanelli, R., Kent, B

    Haynes, M. P., Giovanelli, R., Kent, B. R., et al. 2018, ApJ, 861, 49 11 F. de Gasperin et al.:

    2018

  54. [63]

    L., Lewis, B

    Hoffman, G. L., Lewis, B. M., & Salpeter, E. E. 1995, ApJ, 441, 28

    1995

  55. [64]

    2024, Astrophys

    Hou, M., Hu, Z., & Li, Z. 2024, Astrophys. J. Lett., 965, L24

    2024

  56. [65]

    R., Hancock, P

    Hurley-Walker, N., Callingham, J. R., Hancock, P. J., et al. 2017, MNRAS, 464, 1146

    2017

  57. [66]

    2023, A&A, 675, A118

    Ignesti, A., Vulcani, B., Botteon, A., et al. 2023, A&A, 675, A118

    2023

  58. [67]

    M., et al

    Ignesti, A., Vulcani, B., Poggianti, B. M., et al. 2022, ApJ, 924, 64

    2022

  59. [68]

    T., Jagannathan, P., Mooley, K

    Intema, H. T., Jagannathan, P., Mooley, K. P., & Frail, D. A. 2017, A&A, 598, A78

    2017

  60. [69]

    2014, ApJ, 786, 105

    Janz, J., Laurikainen, E., Lisker, T., et al. 2014, ApJ, 786, 105

    2014

  61. [70]

    Jonas, J. L. 2016, in Proc. Sci. (Sissa Medialab Srl), 1

    2016

  62. [71]

    G., Janowiecki, S., Dey, S., et al

    Jones, M. G., Janowiecki, S., Dey, S., et al. 2024, ApJ, 966, L15

    2024

  63. [72]

    2022, A&A, 667, A76

    Junais, Boissier, S., Boselli, A., et al. 2022, A&A, 667, A76

    2022

  64. [73]

    1998, ARA&A, 36, 189

    Kennicutt, Robert C., J. 1998, ARA&A, 36, 189

    1998

  65. [74]

    R., Giovanelli, R., Haynes, M

    Kent, B. R., Giovanelli, R., Haynes, M. P., et al. 2007, ApJ, 665, L15

    2007

  66. [75]

    R., Spekkens, K., Giovanelli, R., et al

    Kent, B. R., Spekkens, K., Giovanelli, R., et al. 2009, ApJ, 691, 1595

    2009

  67. [76]

    C., Jerjen, H., et al

    Kim, S., Rey, S. C., Jerjen, H., et al. 2015, Astrophys. Journal, Suppl. Ser., 215, 22

    2015

  68. [77]

    V ., & Gottlober, S

    Klypin, A., Hoffman, Y ., Kravtsov, A. V ., & Gottlober, S. 2003, ApJ, 596, 19

    2003

  69. [78]

    A., Giovanelli, R., Haynes, M

    Koopmann, R. A., Giovanelli, R., Haynes, M. P., et al. 2008, ApJ, 682, L85

    2008

  70. [79]

    A., Kenney, J

    Koopmann, R. A., Kenney, J. D. P., & Young, J. 2001, Astrophys. J. Suppl. Ser., 135, 125

    2001

  71. [80]

    S., Staveley-Smith, L., Westmeier, T., et al

    Koribalski, B. S., Staveley-Smith, L., Westmeier, T., et al. 2020, Astrophys. Space Sci., 365, 118

    2020

  72. [81]

    M., Cotton, W

    Lane, W. M., Cotton, W. D., van Velzen, S., et al. 2014, MNRAS, 440, 327

    2014

  73. [82]

    B., Tinsley, B

    Larson, R. B., Tinsley, B. M., & Caldwell, C. N. 1980, ApJ, 237, 692

    1980

  74. [83]

    J., V¨olk, H

    Leech, K. J., V¨olk, H. J., Heinrichsen, I., et al. 1999, MNRAS, 310, 317

    1999

  75. [84]

    W., et al

    Lim, S., Cˆot´e, P., Peng, E. W., et al. 2020, ApJ, 899, 69

    2020

  76. [85]

    K., Binggeli, B., & Glatt, K

    Lisker, T., Grebel, E. K., Binggeli, B., & Glatt, K. 2007, ApJ, 660, 1186

    2007

  77. [86]

    W., et al

    Liu, C., Cˆot´e, P., Peng, E. W., et al. 2020, Astrophys. J. Suppl. Ser., 250, 17

    2020

  78. [87]

    P., et al

    Lu, R.-S., Asada, K., Krichbaum, T. P., et al. 2023, Nature, 616, 686

    2023

  79. [88]

    M., Papastergis, E., Giovanelli, R., et al

    Martin, A. M., Papastergis, E., Giovanelli, R., et al. 2010, ApJ, 723, 1359

    2010

  80. [89]

    H., Veronica, A., et al

    McCall, H., Reiprich, T. H., Veronica, A., et al. 2024, A&A, in press

    2024

  81. [90]

    L., Lenc, E., et al

    McConnell, D., Hale, C. L., Lenc, E., et al. 2020, Publ. Astron. Soc. Aust

    2020

  82. [91]

    B., & Roediger, J

    McDonald, M., Courteau, S., Tully, R. B., & Roediger, J. 2011, MNRAS, 414, 2055

    2011

  83. [92]

    McLaughlin, D. E. 1999, ApJ, 512, L9

    1999

  84. [93]

    P., Cote, P., et al

    Mei, S., Blakeslee, J. P., Cote, P., et al. 2007, ApJ, 655, 144

    2007

  85. [94]

    J., Zwaan, M

    Meyer, M. J., Zwaan, M. A., Webster, R. L., et al. 2004, The HIPASS catalogue - I. Data presentation

    2004

  86. [95]

    T., Werner, N., Simionescu, a., et al

    Million, E. T., Werner, N., Simionescu, a., et al. 2010, MNRAS, 407, 2046

    2010

  87. [96]

    2007, ApJ, 670, 1056

    Minchin, R., Davies, J., Disney, M., et al. 2007, ApJ, 670, 1056

    2007

  88. [97]

    F., Taylor, R., K¨oppen, J., et al

    Minchin, R. F., Taylor, R., K¨oppen, J., et al. 2019, AJ, 158, 121

    2019

  89. [98]

    1998, ApJ, 495, 139

    Moore, B., Lake, G., & Katz, N. 1998, ApJ, 495, 139

    1998

  90. [99]

    M., V ogeley, M

    Moorman, C. M., V ogeley, M. S., Hoyle, F., et al. 2014, MNRAS, 444, 3559 Mu˜noz, R. P., Puzia, T. H., Lanc ¸on, A., et al. 2014, Astrophys. Journal, Suppl. Ser., 210, 4

    2014

  91. [100]

    2004, A&A, 424, 429

    Murgia, M., Govoni, F., Feretti, L., et al. 2004, A&A, 424, 429

    2004

  92. [101]

    J., Kenney, J

    Murphy, E. J., Kenney, J. D. P., Helou, G., Chung, A., & Howell, J. H. 2009, ApJ, 694, 1435

    2009

  93. [102]

    1995, A&A, 293, 56

    Niklas, S., Klein, U., & Wielebinski, R. 1995, A&A, 293, 56

    1995

  94. [103]

    P., Marvil, J., Collier, J

    Norris, R. P., Marvil, J., Collier, J. D., et al. 2021, Publ. Astron. Soc. Aust., 38, e046

    2021

  95. [104]

    J., Andrade-Santos, F., et al

    Osinga, E., Van Weeren, R. J., Andrade-Santos, F., et al. 2022, A&A, 665, A71 O’Sullivan, S. P., Shimwell, T. W., Hardcastle, M. J., et al. 2023, MNRAS, 519, 5723

    2022

  96. [105]

    & Biretta, J

    Owen, F. & Biretta, J. 1999, VLA 7mm images of the M 87 jet, V ol. 530 (Roser Hermann-Josef and Meisenheimer Klaus), 186–187

    1999

  97. [106]

    2000, ApJ, 543, 611

    Owen, F., Eilek, J., & Kassim, N. 2000, ApJ, 543, 611

    2000

  98. [107]

    Peek, J. E. G., Heiles, C., Douglas, K. A., et al. 2011, ApJS, 194, 20

    2011

  99. [108]

    2014, ApJ, 797, 102

    Raichoor, A., Mei, S., Erben, T., et al. 2014, ApJ, 797, 102

    2014

  100. [109]

    2020, A&A, 636, L1

    Ramatsoku, M., Murgia, M., Vacca, V ., et al. 2020, A&A, 636, L1

    2020

  101. [110]

    J., Tufte, S

    Reynolds, R. J., Tufte, S. L., Haffner, L. M., Jaehnig, K., & Percival, J. W. 1998, PASA, 15, 14

    1998

  102. [111]

    D., van Weeren, R

    Roberts, I. D., van Weeren, R. J., Lal, D. V ., et al. 2024, A&A, 683, A11

    2024

  103. [112]

    D., van Weeren, R

    Roberts, I. D., van Weeren, R. J., Timmerman, R., et al. 2022, A&A, 658, A44

    2022

  104. [113]

    Rosenberg, J. L. & Schneider, S. E. 2002, ApJ, 567, 247

    2002

  105. [114]

    & Owen, F

    Rudnick, L. & Owen, F. N. 2014, ApJ, 785, 45

    2014

  106. [115]

    Ruszkowski, M., Br¨uggen, M., Lee, D., & Shin, M. S. 2014, ApJ, 784, 75

    2014

  107. [116]

    C., & Staveley-Smith, L

    Said, K., Kraan-Korteweg, R. C., & Staveley-Smith, L. 2019, MNRAS, 486, 1796

    2019

  108. [117]

    & Catinella, B

    Saintonge, A. & Catinella, B. 2022, The Cold Interstellar Medium of Galaxies in the Local Universe

    2022

  109. [118]

    Sandage, A., Binggeli, B., & Tammann, G. A. 1985, Astron. J., 90, 395

    1985

  110. [119]

    R., Peek, J

    Saul, D. R., Peek, J. E. G., Grcevich, J., et al. 2012, ApJ, 758, 44

    2012

  111. [120]

    L., et al

    Schinnerer, E., Smolˇci´c, V ., Carilli, C. L., et al. 2007, ApJS, 172, 46

    2007

  112. [121]

    M., Kleiner, D., et al

    Serra, P., MacCagni, F. M., Kleiner, D., et al. 2023, A&A, 673, A146

    2023

  113. [122]

    Shapley, A., Fabbiano, G., & Eskridge, P. B. 2001, ApJS, 137, 139

    2001

  114. [123]

    W., Hardcastle, M

    Shimwell, T. W., Hardcastle, M. J., Tasse, C., et al. 2022, A&A, 659, A1

    2022

  115. [124]

    W., Tasse, C., Hardcastle, M

    Shimwell, T. W., Tasse, C., Hardcastle, M. J., et al. 2019, A&A, 622, A1

    2019

  116. [125]

    W., & Urban, O

    Simionescu, A., Werner, N., Mantz, A., Allen, S. W., & Urban, O. 2017, MNRAS, 469, 1476 Smolˇci´c, V ., Novak, M., Bondi, M., et al. 2017, A&A, 602, A1

    2017

  117. [126]

    Sorgho, A., Hess, K., Carignan, C., & Oosterloo, T. A. 2017, MNRAS, 464, 530

    2017

  118. [127]

    W., et al

    Soria, R., Kolehmainen, M., Graham, A. W., et al. 2022, MNRAS, 512, 3284

    2022

  119. [128]

    W., Su, Y ., et al

    Spasic, A., Edler, H. W., Su, Y ., et al. 2024, A&A, 690, A195

    2024

  120. [129]

    J., et al

    Tasse, C., Shimwell, T., Hardcastle, M. J., et al. 2021, A&A, 648, A1

    2021

  121. [130]

    R., Sekhar, S., Heino, L., et al

    Taylor, A. R., Sekhar, S., Heino, L., et al. 2024, MNRAS, 528, 2511

    2024

  122. [131]

    & Bryan, G

    Tonnesen, S. & Bryan, G. L. 2010, ApJ, 709, 1203

    2010

  123. [132]

    & Bryan, G

    Tonnesen, S. & Bryan, G. L. 2012, MNRAS, 422, 1609

    2012

  124. [133]

    L., & Chen, R

    Tonnesen, S., Bryan, G. L., & Chen, R. 2011, ApJ, 731, 98

    2011

  125. [134]

    & Stone, J

    Tonnesen, S. & Stone, J. 2014, ApJ, 795, 148

    2014

  126. [135]

    J., Popescu, C

    Tuffs, R. J., Popescu, C. C., Pierini, D., et al. 2002, Astrophys. J. Suppl. Ser., 139, 37

    2002

  127. [136]

    W., & B ¨ohringer, H

    Urban, O., Werner, N., Simionescu, A., Allen, S. W., & B ¨ohringer, H. 2011, MNRAS, 414, 2101 van Haarlem, M. P., Wise, M. W., Gunst, a. W., et al. 2013, A&A, 556, A2 V¨olk, H. J. & Xu, C. 1994, Infrared Physics and Technology, 35, 527 V ollmer, B., Cayatte, V ., Balkowski, C....

    2011

  128. [137]

    L., Eisenhardt, P

    Wright, E. L., Eisenhardt, P. R., Mainzer, A. K., et al. 2010, Astron. J., 140, 1868

    2010

  129. [138]

    Zhang, C., Churazov, E., & Schekochihin, A. A. 2018, MNRAS, 478, 4785

    2018

  130. [139]

    A., Briggs, F

    Zwaan, M. A., Briggs, F. H., Sprayberry, D., & Sorar, E. 1997, ApJ, 490, 173

    1997

  131. [140]

    A., Meyer, M

    Zwaan, M. A., Meyer, M. J., Staveley-Smith, L., & Webster, R. L. 2005, The HIPASS catalogue:ωHI and environmental e ffects on the HI mass function of galaxies 12

    2005

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