Pith. sign in

REVIEW 1 major objections 5 minor 1 cited by

Revisiting the Group-Dominant Elliptical NGC 5044 in the Radio Band: Continuum Emission and Detection of HI Absorption

T0 review · 1 major / 5 minor · reviewed 2026-08-10 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read This paper reports the first direct detection of neutral atomic hydrogen in NGC 5044, a 3.8σ double-peaked 21-cm absorption line toward the active nucleus, plus a ~25 kpc steep-spectrum diffuse radio halo around the core.

desk verdict A solid continuum reimaging and a plausible but statistically marginal HI absorption claim; send to review with a request for a trials-corrected significance. read the letter →

arxiv 2501.02076 v2 pith:6FVDFL3Y submitted 2025-01-03 astro-ph.GA

Kamlesh Rajpurohit , Tirna Deb , Konstantinos Kolokythas , Kshitij Thorat , Ewan O'Sullivan , Gerrit Schellenberger , Laurence P. David , Jan M. Vrtilek
show 4 more authors
Simona Giacintucci William Forman Christine Jones Mpati Ramatsoku
This is my paper · ORCID
classification astro-ph.GA
keywords NGC5044HIabsorptiongalaxygroupscool-coreradiocontinuumAGNfeedbackatomicgaschaoticcoldaccretion
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

Using MeerKAT L-band and upgraded GMRT observations, this paper tries to settle the radio morphology of NGC 5044, the dominant elliptical of the X-ray brightest group in the sky, and to find the neutral atomic gas that cooling models say should be present in its core. It reports a previously unseen diffuse radio halo roughly 25 kpc across, with a spectrum that steepens from $\alpha=-0.70$ below 1 GHz to $\alpha=-1.53$ at higher frequencies, and shows that the emission overlaps the X-ray cavities but is not confined to them. It also reports the first detection of neutral hydrogen in this galaxy, a 3.8$\sigma$ double-peaked 21-cm absorption line against the active nucleus whose velocities match the known CO(2-1) absorption. If correct, the HI detection closes a gap in the cooling-flow picture: atomic gas is present, it is cold ($T_{\rm spin}\le950$ K), and the molecular-to-atomic mass ratio of at least 1.7:1 matches predictions of chaotic cold accretion.

What carries the argument

The load-bearing measurement is the 21-cm HI absorption line seen against the unresolved radio nucleus: the integrated optical depth $\int\tau\,dv=0.526\pm0.103$ km/s converts through $N_{\rm HI}=1.82\times10^{18}\,T_{\rm spin}\int\tau\,dv$ cm$^{-2}$ into a column density, while the ratio of the HI emission upper limit to the absorption column sets $T_{\rm spin}\le950$ K. On the continuum side, the machinery is the multi-band spectral index map between 380 MHz and 1.28 GHz plus a Jaffe-Perola spectral aging fit, which yields the equipartition field $B\approx1.4\,\mu$G and a radiative age of $77\pm10$ Myr.

What would settle it

Re-observe the NGC 5044 nucleus in the 21-cm line with a longer MeerKAT integration or an independent array and check whether the two absorption dips at roughly 280 and 297 km/s reappear at >5$\sigma$; if they do not, or if the feature is traced to bandpass or continuum-subtraction residuals, the HI detection and its derived column density, spin temperature, and mass ratio are false. The continuum and spectral-index results would survive such a test.

Watch

Extended reading notes

Core claim

The central discovery is that NGC 5044's radio core is surrounded by diffuse, steep-spectrum emission extending about 25 kpc, and that neutral atomic gas exists in its nuclear region. The diffuse emission has a curved spectrum typical of aged relativistic plasma, with a fitted spectral age around 77-80 Myr, and it fills but extends well beyond the intermediate X-ray cavities; the authors argue it is old jet or lobe plasma redistributed by intra-group medium weather. The HI absorption, the first direct evidence of atomic gas in the galaxy, is concentrated within the central 800 pc and splits into two components at 280 and 297 km/s, slightly broader than the CO lines, implying that HI and CO trace different density zones of the same infalling clouds. The non-detection of HI emission gives $M_{\rm HI}<5.4\times10^{7}\,M_\odot$ in the central 2.2 kpc, so molecular gas outweighs atomic gas by at least 1.7 to 1, which the authors take as evidence that both phases condense out of the hot intra-group medium rather than being accreted from another galaxy.

Load-bearing premise

The load-bearing premise is that the 3.8$\sigma$ HI absorption feature is a genuine astrophysical line rather than a residual calibration or continuum-subtraction artifact; if it is a noise fluctuation, the HI detection, column density, spin temperature, and molecular-to-atomic mass ratio all collapse.

Editorial extensions

If this is right

  • The previously reported kiloparsec-scale jets, lobes, and east-west structures in older GMRT and VLA images are not reproduced in the new deep data or in reprocessed archival data, so those features are likely artifacts; the true large-scale radio structure is a ~25 kpc diffuse halo.
  • Because the diffuse radio emission fills but is not bounded by the X-ray cavities and shows no spectral index gradient, the radio plasma has mixed into the surrounding intra-group medium rather than remaining trapped in expanding lobes.
  • The velocity match between HI and CO(2-1) absorption, with HI broader, indicates a single population of cold clouds in front of the nucleus in which atomic and molecular gas coexist at different densities.
  • A molecular-to-atomic mass ratio above 1.7:1 places NGC 5044 at the high end for early-type galaxies and agrees with chaotic cold accretion simulations, supporting in-situ condensation over merger acquisition.
  • The cold neutral medium implied by $T_{\rm spin}\le950$ K and the predicted HI mass imply that an improvement in sensitivity by a factor of about 2.3 could detect the neutral phase in emission.

Reading between the lines

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

  • Our inference: if the HI absorption is confirmed at higher significance, the double-peaked structure matching CO gives a rare joint atomic-molecular probe of the accretion flow within a few tens of parsecs of a supermassive black hole, and could be used to measure cloud kinematics and infall rates.
  • Our inference: the disappearance of several previously published radio features with deeper data suggests that some AGN duty-cycle and jet-cavity alignment statistics built on shallow low-frequency images may need revision.
  • Our inference: the paper's interpretation that the diffuse emission is old lobe plasma redistributed by sloshing predicts that higher-frequency, higher-resolution observations should reveal filamentary or tail-like substructures aligned with the H$\alpha$ nebula and sloshing fronts; such a test is directly observable with existing arrays.
  • Our inference: the narrow gap between the current HI mass upper limit and the chaotic cold accretion prediction makes NGC 5044 a prime target for a next-generation 21-cm emission search; a detection would directly weigh the atomic reservoir and distinguish cooling from tidal-stripping origins.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

1 major / 5 minor

Summary. The paper presents new MeerKAT L-band and uGMRT Band 3/4 continuum and HI observations of the group-dominant elliptical NGC 5044. The continuum data reveal diffuse, steep-spectrum radio emission extending roughly 25 kpc from the unresolved core, with consistent morphology across 150 MHz, 235 MHz, 380/675 MHz, 986 MHz, and 1.28/1.56 GHz after archival reprocessing. The paper reports a 3.8 sigma two-component HI absorption feature against the core, claims the first detection of neutral atomic gas in this galaxy, and uses it to derive an HI column density, a spin temperature upper limit (Tspin ≤ 950 K), an HI mass upper limit, and a molecular-to-atomic mass ratio (MH2/MHI ≥ 1.7). The final sections interpret the diffuse radio emission as aged AGN lobe plasma mixed into the IGrM and the HI as condensed cold gas probably falling toward the SMBH.

Significance. If the HI absorption detection is real, this is the first detection of neutral atomic gas in NGC 5044 and one of few HI absorption detections in X-ray luminous group-dominant galaxies. The velocity match with previously detected CO(2-1) absorption supports the idea that the HI and CO trace different density zones of the same infalling clouds, and the inferred Tspin ≤ 950 K places the gas in the cold neutral phase. The continuum results are a substantial step forward: they resolve a long-standing morphological controversy by showing consistent diffuse emission at multiple frequencies, and they place the diffuse radio source in the context of other group-dominant systems. The manuscript makes good use of modern reduction pipelines (CARACal, SPAM, WSClean), includes independent reprocessing of archival data, and provides a clear statement of the caveats in the spectral-age modeling. The chief weakness is that the headline HI detection rests on a single 3.8 sigma feature for which the global false-alarm probability is not quantified.

major comments (1)
  1. [§3.2, Figure 7] The abstract and §3.1 quote different uncertainties for the same spectral index: the abstract gives α = -1.53 ± 0.6 while §3.1 gives α = -1.53 ± 0.06 (and the same value appears in §4.1 and §5). This is a factor-of-ten discrepancy. If the larger uncertainty is correct, the claimed high-frequency steepening is not statistically significant and the JP model fit is poorly constrained; if the smaller uncertainty is correct, the abstract must be corrected. Please resolve this inconsistency and ensure all quoted error bars are consistent throughout the manuscript.
minor comments (5)
  1. [§2.1.2] The statement 'The frequency range covering Galactic emission was flagged' is vague; please specify the exact frequency range that was removed.
  2. [§3.2, Figure 6/Figure 7] In the paragraph after Figure 6, the text says the boxcar-smoothed spectrum is shown in 'Figure 6 right panel', but Figure 6 is a moment-zero map and the spectrum appears in Figure 7. Please correct the cross-reference.
  3. [Appendix A.2] The caption for Figure A.2 says images were created using Briggs weighting with 'roboust = −2'; this should read 'robust = −2'.
  4. [§3.2.1] Equation (6) uses the symbol Sint for the integrated emission flux density, but the same symbol is used in §3.2.2 for the integrated line flux density of the HI absorption; please clarify the distinction or use different notation.
  5. [§4.1] The comparison with NGC 1407 and NGC 3411 is useful, but the text does not include a reference for the NGC 3411 spectral index value (the cited Giacintucci et al. papers should be checked for the specific value).

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: all central claims are direct measurements or externally anchored model fits.

full rationale

The paper's headline results are direct observational measurements: the continuum morphology and flux densities come from new uGMRT/MeerKAT images, and the HI optical depth is measured from the spectral line cube via Eq. 4. The spectral age (77-80 Myr) is a model fit using an assumed JP injection model, equipartition field, and fixed ν1, ν2, and γmin; it is presented as an estimate, not as an independent prediction, so no fitted-input-called-prediction pattern applies. The HI column density, spin-temperature upper limit, and mass upper limit follow from standard radiative-transfer relations (Eqs. 3, 5-7) and the non-detection of HI emission, with no quantity defined in terms of the conclusion. The CO(2-1) comparison and molecular mass use prior published observations (Schellenberger et al. 2020); although this is a self-citation, the CO data are independent, externally falsifiable measurements, not fitted to this paper's results, so they provide real evidence rather than circular support. The 3.8σ significance of the HI absorption is below the conventional 5σ standalone threshold and no global trials correction is given, but that is a statistical robustness concern, not circularity. No equation reduces to its own input, no uniqueness theorem is imported, and no ansatz is smuggled in via citation; the central derivation chain is self-contained.

Assumptions & free parameters 6 free parameters · 5 assumptions · 0 invented entities

The central HI detection and continuum morphology require no free parameters, but the secondary spectral-age estimate adopts several assumed or fitted quantities, and the HI column density, spin temperature, and mass upper limit rely on standard domain assumptions about optical depth, covering factor, and the velocity search window. No new entities are introduced.

free parameters (6)
  • Injection spectral index (alpha_inj) = -0.55
    Obtained by fitting the integrated spectrum with a JP model in synchrofit; used in the equipartition magnetic field and spectral age estimate.
  • Proton-to-electron energy ratio (k) = 1
    Assumed in the minimum-energy magnetic field calculation, Section 3.1.
  • Filling factor (eta) = 1
    Assumed in the equipartition field estimate, Section 3.1.
  • Minimum Lorentz factor (gamma_min) = 20
    Adopted following Brunetti et al. (1997) for spectral age estimate.
  • Path length (l) = 9.9 kpc
    Adopted as the transverse dimension measured from the uGMRT Band 3 map.
  • Low and high cutoff frequencies (nu_1, nu_2) = 0.010 GHz, 100 GHz
    Assumed for the JP model spectral age fit.
assumptions (5)
  • domain assumption The HI gas is optically thin and the background radiation at 21 cm is negligible, so the emission/absorption ratio gives the spin temperature via the standard relations.
    Section 3.2.1, Equations (3)-(6); if the gas is optically thick or partially covers the continuum, the derived column density and Tspin upper limit are not valid as stated.
  • domain assumption The absorbing HI uniformly covers the radio continuum source, so the optical depth is the ratio of absorption flux to observed continuum flux.
    Equation (4) in Section 3.2.1; partial covering would make the true column density higher than estimated.
  • domain assumption The noise in the HI spectral cube is Gaussian and independent between channels, so a 3.8-sigma peak can be assigned a 99.9 percent confidence.
    Section 3.2, 'The detection has a significance of 3.8 sigma (99.9% confidence)'; the entire HI detection claim rests on this statistical assumption.
  • domain assumption The velocity range of CO(2-1) emission (-520 to 330 km/s) brackets the velocity range over which HI emission could be present, so the number of channels used for the mass upper limit is appropriate.
    Section 3.2.2, following Schellenberger et al. (2020); HI emission outside this range would weaken the upper limit.
  • standard math A flat Lambda-CDM cosmology with H0=70, Omega_m=0.3, Omega_Lambda=0.7 and a distance of 31.2 Mpc to NGC 5044 are adopted.
    Section 1; all physical sizes and masses scale with the assumed distance and cosmology.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Revisiting the Group-Dominant Elliptical NGC 5044 in the Radio Band: Continuum Emission and Detection of HI Absorption." pith.science (2026). https://pith.science/paper/6FVDFL3Y

@misc{pith2026250102076,
  author       = {Pith},
  title        = {Pith review of: Revisiting the Group-Dominant Elliptical NGC 5044 in the Radio Band: Continuum Emission and Detection of HI Absorption},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/6FVDFL3Y}},
  note         = {Machine review of arXiv:2501.02076}
}
abstract

We present new MeerKAT L-band (continuum and HI) and upgraded Giant Metrewave Radio Telescope (300-850 MHz) observations of the archetypal cool-core group-dominant early-type galaxy NGC 5044. Our new continuum images reveal diffuse, steep spectrum ($\alpha_{0.99\,\rm GHz}^{1.56\,\rm GHz}=-1.53\pm0.6$) radio emission extending about 25 kpc around the unresolved radio core. The observed radio emission overlaps with the known X-ray cavities, but is not confined to them. We also find the first direct evidence of neutral atomic gas in NGC 5044, in the form of a 3.8$\sigma$ significant two-component HI absorption line seen against the emission of the active nucleus. The peak velocities are well correlated with the previously reported CO(2-1) absorption, but the HI lines are moderately broader, spanning velocities from $265\,\rm \, km\,s^{-1}$ to $305\,\rm \, km\,s^{-1}$. We do not detect HI emission, but place an upper limit of $M_{HI}< 5.4 \times 10^{7} \, M_{\odot}$ in the central 15 arcsec (2.2 kpc) of the galaxy. This is significantly less than the estimated molecular gas content, and implies a molecular-to-atomic mass ratio of $\geq $1.7:1, consistent with these gas phases forming through cooling from the hot intra-group medium. We also constrain the spin temperature to $T_{\rm spin}\leq 950\,\rm K$, indicating that the detected HI is in the cold neutral phase.

Figures

Figures reproduced from arXiv: 2501.02076 by the authors.

Figure 1
Figure 1. Radio and X-ray overlay of NGC 5044. The intensity in red shows the radio emission observed with uGMRT at a central frequency of 380 MHz (10′′ resolution). The intensity in blue shows Chandra X-ray emission in the 0.5 − 2.0 keV band. efficient than in clusters, leading to the finding that there are essentially no non-cool-core groups by the standards applied to clusters (O’Sullivan et al. 2017). It has also been sho… view at source ↗
Figure 2
Figure 2. MeerKAT L-band (left) and uGMRT Band 3 (right) full band continuum radio images of the NGC 5044 field at a common resolution of 15′′. The radio beam size is indicated in the bottom left corner of each image. The image properties are given in [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Zoomed-in uGMRT Band 3 (left), Band 4 (middle), and MeerKAT L-band (right) continuum images of NGC 5044, displayed on a square root scale. All images share a common resolution of 15′′. The beam size is indicated in the bottom left corner of each image. The images reveal diffuse radio emission surrounding NGC 5044 and extending almost 10 kpc from the galaxy in multiple directions. Radio contours are drawn at [1, 2, 4… view at source ↗
Figures from the paper (5 more)
Figure 4
Figure 4. Figure 4: Top Left: Chandra 0.5 − 2 keV image of the galaxy group NGC 5044 overlaid with the uGMRT Band 3 10′′ resolution contours. Top Right: Chandra 0.5 − 2 keV residual map, smoothed with a 2 pixel (∼1 ′′) Gaussian and overlaid with the same uGMRT contours. The newly detected…
Figure 5
Figure 5. Figure 5: Left: Integrated spectrum of the newly detected diffuse radio emission excluding NGC 5044 core (i.e., within a 6.5 kpc diameter) between 380 MHz and 1.56 GHz. The dashed and dot-dashed lines represent the fitted JP model and a single power law, respectively. The JP mod…
Figure 6
Figure 6. Figure 6: H I moment zero MeerKAT map (8.3 ′′ × 7.6 ′′) show￾ing absorption from the core of NGC 5044 overlaid with contin￾uum emission contours at 1.28 GHz (8.3 ′′ × 7.6 ′′). The H I cube was binned to a velocity resolution of 27.9 km s−1 (5 channel bin￾ning). The image reveals…
Figure 7
Figure 7. Figure 7: H I absorption spectra toward the compact core of NGC 5044 obtained from SoFiA. Both spectra are extracted from an H I cube with beam size of 8.3 ′′×7.6 ′′ using a circular region of radius 4.2′′, i.e, similar to the beam size. Left: Spectrum obtained by applying 5-cha…
Figure 8
Figure 8. Figure 8: CO (top) and H I (middle/bottom) absorption spectra from the nuclear region of NGC 5044. The raw H I spectrum is shown in the lower panel, and the middle panel shows the spectrum, boxcar smoothed to a velocity resolution of 16.7 km s−1 . The CO spectrum, adopted from S…

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Decoding AGN Feedback with X-arithmetic: From Morphology to Physical Mechanisms

    astro-ph.GA 2025-06 conditional novelty 5.0 of 10

    Applying X-arithmetic to 15 deeply observed Chandra halos, the authors classify AGN feedback structures and report multiple shocks in groups versus mainly isobaric structures around cavities in massive clusters.

Reference graph

Works this paper leans on

92 extracted references · 9 canonical work pages · cited by 1 Pith paper

  1. [1]

    Allison, J. R. 2021, Monthly Notices of the Royal Astronomical Society, 503, 985, doi: 10.1093/mnras/stab518 Astropy Collaboration, Robitaille, T. P., Tollerud, E. J., et al. 2013, A&A, 558, A33, doi: 10.1051/0004-6361/201322068 Astropy Collaboration, Price-Whelan, A. M., Sip˝ocz, B. M., et al. 2018, AJ, 156, 123, doi: 10.3847/1538-3881/aabc4f Bîrzan, L.,...

    doi:10.1093/mnras/stab518 2021

  2. [2]

    Wise, M. W. 2008, ApJ, 686, 859, doi: 10.1086/591416 Bîrzan, L., Rafferty, D. A., Brüggen, M., et al. 2020, MNRAS, 496, 2613, doi: 10.1093/mnras/staa1594

    doi:10.1086/591416 2008

  3. [3]

    D., Walsh, J

    Boizelle, B. D., Walsh, J. L., Barth, A. J., et al. 2021, ApJ, 908, 19, doi: 10.3847/1538-4357/abd24d

    doi:10.3847/1538-4357/abd24d 2021

  4. [4]

    A., & Sijacki, D

    Bourne, M. A., & Sijacki, D. 2017, MNRAS, 472, 4707, doi: 10.1093/mnras/stx2269 —. 2021, MNRAS, 506, 488, doi: 10.1093/mnras/stab1662

    doi:10.1093/mnras/stx2269 2017

  5. [5]

    2022, A&A, 661, A92, doi: 10.1051/0004-6361/202142579

    Brienza, M., Lovisari, L., Rajpurohit, K., et al. 2022, A&A, 661, A92, doi: 10.1051/0004-6361/202142579

    doi:10.1051/0004-6361/202142579 2022

  6. [6]

    Briggs, D. S. 1995, PhD thesis, New Mexico Institute of Mining and Technology

    1995

  7. [7]

    Brunetti, G., & Jones, T. W. 2014, International Journal of Modern Physics D, 23, 1430007, doi: 10.1142/S0218271814300079

    doi:10.1142/s0218271814300079 2014

  8. [8]

    1997, A&A, 325, 898, doi: 10.48550/arXiv.astro-ph/9704162

    Brunetti, G., Setti, G., & Comastri, A. 1997, A&A, 325, 898, doi: 10.48550/arXiv.astro-ph/9704162

    arXiv doi:10.48550/arxiv.astro-ph/9704162 1997

Show all 92 references
  1. [9]

    A., Lewis, A

    Buote, D. A., Lewis, A. D., Brighenti, F., & Mathews, W. G. 2003, ApJ, 594, 741, doi: 10.1086/377094

    2003 doi

  2. [10]

    2001, ApJ, 554, 261, doi: 10.1086/321357

    Forman, W. 2001, ApJ, 554, 261, doi: 10.1086/321357

    2001 doi

  3. [11]

    2000, A&A, 356, 788, doi: 10.48550/arXiv.astro-ph/0002375

    Churazov, E., Forman, W., Jones, C., & Böhringer, H. 2000, A&A, 356, 788, doi: 10.48550/arXiv.astro-ph/0002375

    2000 doi arXiv

  4. [12]

    2002, MNRAS, 332, 729, doi: 10.1046/j.1365-8711.2002.05332.x

    Churazov, E., Sunyaev, R., Forman, W., & Böhringer, H. 2002, MNRAS, 332, 729, doi: 10.1046/j.1365-8711.2002.05332.x

    2002

  5. [13]

    2021, CARTA: The Cube Analysis and Rendering Tool for Astronomy, 2.0.0, Zenodo, doi: 10.5281/zenodo.4905459

    Comrie, A., Wang, K.-S., Hsu, S.-C., et al. 2021, CARTA: The Cube Analysis and Rendering Tool for Astronomy, 2.0.0, Zenodo, doi: 10.5281/zenodo.4905459

    2021 doi

  6. [14]

    P., Jones, C., Forman, W., & Daines, S

    David, L. P., Jones, C., Forman, W., & Daines, S. 1994, ApJ, 428, 544, doi: 10.1086/174264

    1994 doi

  7. [15]

    P., Jones, C., Forman, W., et al

    David, L. P., Jones, C., Forman, W., et al. 2009, ApJ, 705, 624, doi: 10.1088/0004-637X/705/1/624

    2009 doi

  8. [16]

    P., Vrtilek, J., O’Sullivan, E., et al

    David, L. P., Vrtilek, J., O’Sullivan, E., et al. 2017, ApJ, 842, 84, doi: 10.3847/1538-4357/aa756c

    2017 doi

  9. [17]

    P., O’Sullivan, E., Jones, C., et al

    David, L. P., O’Sullivan, E., Jones, C., et al. 2011, ApJ, 728, 162, doi: 10.1088/0004-637X/728/2/162

    2011 doi

  10. [18]

    P., Lim, J., Forman, W., et al

    David, L. P., Lim, J., Forman, W., et al. 2014, ApJ, 792, 94, doi: 10.1088/0004-637X/792/2/94

    2014 doi

  11. [19]

    A., Greene, J

    Davis, T. A., Greene, J. E., Ma, C.-P., et al. 2019, MNRAS, 486, 1404, doi: 10.1093/mnras/stz871

    2019 doi

  12. [20]

    Deb, T., Verheijen, M. A. W., Poggianti, B. M., et al. 2022, Monthly Notices of the Royal Astronomical Society, 516, 2683–2696, doi: 10.1093/mnras/stac2441

    2022 doi

  13. [21]

    D., Gallagher, S

    Desjardins, T. D., Gallagher, S. C., Hornschemeier, A. E., et al. 2014, ApJ, 790, 132

    2014

  14. [22]

    Diniz, S. I. F., Pastoriza, M. G., Hernandez-Jimenez, J. A., et al. 2017, MNRAS, 470, 1703, doi: 10.1093/mnras/stx1322

    2017 doi

  15. [23]

    Donahue, M., & V oit, G. M. 2022, PhR, 973, 1, doi: 10.1016/j.physrep.2022.04.005

    2022 doi

  16. [24]

    Dong, R., Rasmussen, J., & Mulchaey, J. S. 2010, ApJ, 712, 883, doi: 10.1088/0004-637X/712/2/883

    2010 doi

  17. [25]

    L., Bania, T

    Dressel, L. L., Bania, T. M., & Davis, M. M. 1983, ApJL, 266, L97, doi: 10.1086/183986

    1983 doi

  18. [26]

    Eckert, D., Gaspari, M., Gastaldello, F., Le Brun, A. M. C., & O’Sullivan, E. 2021, Universe, 7, 142, doi: 10.3390/universe7050142

    2021 doi

  19. [27]

    2016, A&A, 592, A12

    Eckert, D., Ettori, S., Coupon, J., et al. 2016, A&A, 592, A12

    2016

  20. [28]

    Edge, A. C. 2001, MNRAS, 328, 762, doi: 10.1046/j.1365-8711.2001.04802.x

    2001

  21. [29]

    Fabian, A. C. 2012, ARA&A, 50, 455, doi: 10.1146/annurev-astro-081811-125521

    2012 doi

  22. [30]

    2017, MNRAS, 466, 677, doi: 10.1093/mnras/stw3108

    Gaspari, M., Temi, P., & Brighenti, F. 2017, MNRAS, 466, 677, doi: 10.1093/mnras/stw3108

    2017 doi

  23. [31]

    2020, Nature Astronomy, 4, 10, doi: 10.1038/s41550-019-0970-1

    Gaspari, M., Tombesi, F., & Cappi, M. 2020, Nature Astronomy, 4, 10, doi: 10.1038/s41550-019-0970-1

    2020 doi

  24. [32]

    A., Humphrey, P

    Gastaldello, F., Buote, D. A., Humphrey, P. J., et al. 2007, ApJ, 669, 158, doi: 10.1086/521519

    2007 doi

  25. [33]

    A., Temi, P., et al

    Gastaldello, F., Buote, D. A., Temi, P., et al. 2009, ApJ, 693, 43, doi: 10.1088/0004-637X/693/1/43

    2009 doi

  26. [34]

    2013, ApJ, 770, 56, doi: 10.1088/0004-637X/770/1/56

    Gastaldello, F., Di Gesu, L., Ghizzardi, S., et al. 2013, ApJ, 770, 56, doi: 10.1088/0004-637X/770/1/56

    2013 doi

  27. [35]

    2019, ApJ, 880, 70, doi: 10.3847/1538-4357/ab29f1

    Giacintucci, S., Markevitch, M., Cassano, R., et al. 2019, ApJ, 880, 70, doi: 10.3847/1538-4357/ab29f1

    2019 doi

  28. [36]

    M., O’Sullivan, E., et al

    Giacintucci, S., Vrtilek, J. M., O’Sullivan, E., et al. 2009, in American Institute of Physics Conference Series, V ol. 1201, The Monster’s Fiery Breath: Feedback in Galaxies, Groups, and Clusters, ed. S. Heinz & E. Wilcots (AIP), 229–232, doi: 10.1063/1.3293043

    2009 doi

  29. [37]

    2011, ApJ, 732, 95, doi: 10.1088/0004-637X/732/2/95

    Giacintucci, S., O’Sullivan, E., Vrtilek, J., et al. 2011, ApJ, 732, 95, doi: 10.1088/0004-637X/732/2/95

    2011 doi

  30. [38]

    E., et al

    Giacintucci, S., O’Sullivan, E., Clarke, T. E., et al. 2012, ApJ, 755, 172, doi: 10.1088/0004-637X/755/2/172

    2012 doi

  31. [39]

    Gitti, M., Brighenti, F., & McNamara, B. R. 2012, Advances in Astronomy, 2012, 950641, doi: 10.1155/2012/950641 Grossová, R., Werner, N., Massaro, F., et al. 2022, ApJS, 258, 30, doi: 10.3847/1538-4365/ac366c

    2012 doi

  32. [40]

    Healy, J., Deb, T., Verheijen, M. A. W., et al. 2021, A&A, 654, A173, doi: 10.1051/0004-6361/202141377

    2021 doi

  33. [41]

    Hogan, M. T. 2014, PhD thesis, Durham University, UK

    2014

  34. [42]

    Hunter, J. D. 2007, Computing in Science & Engineering, 9, 90, doi: 10.1109/MCSE.2007.55 CONTINUUM EMISSION AND H I ABSORPTION IN THE EARLY TYPE GALAXY NGC 5044 17

    2007 doi

  35. [43]

    2020, A&A, 640, A37, doi: 10.1051/0004-6361/201937207

    Ignesti, A., Brunetti, G., Gitti, M., & Giacintucci, S. 2020, A&A, 640, A37, doi: 10.1051/0004-6361/201937207

    2020 doi

  36. [44]

    T., van der Tol, S., Cotton, W

    Intema, H. T., van der Tol, S., Cotton, W. D., et al. 2009, A&A, 501, 1185, doi: 10.1051/0004-6361/200811094

    2009 doi

  37. [45]

    Jaffe, W., & McNamara, B. R. 1994, ApJ, 434, 110, doi: 10.1086/174708

    1994 doi

  38. [46]

    J., & Perola, G

    Jaffe, W. J., & Perola, G. C. 1973, A&A, 26, 423

    1973

  39. [47]

    A., & Mandel, E

    Joye, W. A., & Mandel, E. 2003, in Astronomical Society of the Pacific Conference Series, V ol. 295, Astronomical Data Analysis Software and Systems XII, ed. H. E. Payne, R. I. Jedrzejewski, & R. N. Hook, 489 Józsa, G. I. G., White, S. V ., Thorat, K., et al. 2020, CARACal: Co...

    2003

  40. [48]

    2008, ApJ, 684, 270, doi: 10.1086/590243

    Kaneda, H., Onaka, T., Sakon, I., et al. 2008, ApJ, 684, 270, doi: 10.1086/590243

    2008 doi

  41. [49]

    S., Smirnov, O

    Kenyon, J. S., Smirnov, O. M., Grobler, T. L., & Perkins, S. J. 2018, MNRAS, 478, 2399, doi: 10.1093/mnras/sty1221

    2018 doi

  42. [50]

    A., Forbes, D

    Kilborn, V . A., Forbes, D. A., Barnes, D. G., et al. 2009, MNRAS, 400, 1962

    2009

  43. [51]

    C., McNamara, B

    Kirkpatrick, C. C., McNamara, B. R., & Cavagnolo, K. W. 2011, ApJ, 731, L23, doi: 10.1088/2041-8205/731/2/L23

    2011 doi

  44. [52]

    H., et al

    Kokotanekov, G., Wise, M., Heald, G. H., et al. 2017, A&A, 605, A48, doi: 10.1051/0004-6361/201730940

    2017 doi

  45. [53]

    2019, MNRAS, 489, 2488, doi: 10.1093/mnras/stz2082

    Kolokythas, K., O’Sullivan, E., Intema, H., et al. 2019, MNRAS, 489, 2488, doi: 10.1093/mnras/stz2082

    2019 doi

  46. [54]

    2018, MNRAS, 481, 1550, doi: 10.1093/mnras/sty2030

    Kolokythas, K., O’Sullivan, E., Raychaudhury, S., et al. 2018, MNRAS, 481, 1550, doi: 10.1093/mnras/sty2030

    2018 doi

  47. [55]

    2018, MNRAS, 481, 4472, doi: 10.1093/mnras/sty2565

    Lakhchaura, K., Werner, N., Sun, M., et al. 2018, MNRAS, 481, 4472, doi: 10.1093/mnras/sty2565

    2018 doi

  48. [56]

    H., & Schellenberger, G

    Lovisari, L., Reiprich, T. H., & Schellenberger, G. 2015, A&A, 573, A118, doi: 10.1051/0004-6361/201423954

    2015 doi

  49. [57]

    M., Ruffa, I., Loni, A., et al

    Maccagni, F. M., Ruffa, I., Loni, A., et al. 2023, A&A, 675, A59, doi: 10.1051/0004-6361/202346521

    2023 doi

  50. [58]

    R., & Nulsen, P

    McNamara, B. R., & Nulsen, P. E. J. 2012, New Journal of Physics, 14, 055023, doi: 10.1088/1367-2630/14/5/055023

    2012 doi

  51. [59]

    2017, PASA, 34, 52, doi: 10.1017/pasa.2017.31

    Meyer, M., Robotham, A., Obreschkow, D., et al. 2017, PASA, 34, 52, doi: 10.1017/pasa.2017.31

    2017 doi

  52. [60]

    2018, A&A Rv, 26, 4, doi: 10.1007/s00159-018-0109-x

    Morganti, R., & Oosterloo, T. 2018, A&A Rv, 26, 4, doi: 10.1007/s00159-018-0109-x

    2018 doi

  53. [61]

    B., Oosterloo, T

    Morganti, R., Peck, A. B., Oosterloo, T. A., et al. 2009, A&A, 505, 559, doi: 10.1051/0004-6361/200912605

    2009 doi

  54. [62]

    T., Oosterloo, T

    Morganti, R., de Zeeuw, P. T., Oosterloo, T. A., et al. 2006, MNRAS, 371, 157, doi: 10.1111/j.1365-2966.2006.10681.x

    2006

  55. [64]

    2009, A&A, 499, 679, doi: 10.1051/0004-6361/200911659

    Murgia, M., Govoni, F., Markevitch, M., et al. 2009, A&A, 499, 679, doi: 10.1051/0004-6361/200911659

    2009 doi

  56. [66]

    C., Koopmann, R

    Odekon, M. C., Koopmann, R. A., Haynes, M. P., et al. 2016, ApJ, 824, 110

    2016

  57. [67]

    R., de Bruyn, A

    Offringa, A. R., de Bruyn, A. G., Biehl, M., et al. 2010, MNRAS, 405, 155, doi: 10.1111/j.1365-2966.2010.16471.x

    2010

  58. [68]

    R., McKinley, B., Hurley-Walker, N., et al

    Offringa, A. R., McKinley, B., Hurley-Walker, N., et al. 2014, MNRAS, 444, 606, doi: 10.1093/mnras/stu1368

    2014 doi

  59. [69]

    2019, A&A, 631, A22, doi: 10.1051/0004-6361/201935350

    Olivares, V ., Salome, P., Combes, F., et al. 2019, A&A, 631, A22, doi: 10.1051/0004-6361/201935350

    2019 doi

  60. [71]

    2021, MNRAS, 505, 2628, doi: 10.1093/mnras/stab1451

    Pasini, T., Finoguenov, A., Brüggen, M., et al. 2021, MNRAS, 505, 2628, doi: 10.1093/mnras/stab1451

    2021 doi

  61. [72]

    N., et al

    Pasini, T., Brüggen, M., Hoang, D. N., et al. 2022, A&A, 661, A13, doi: 10.1051/0004-6361/202141211 Plšek, T., Werner, N., Topinka, M., & Simionescu, A. 2024, MNRAS, 527, 3315, doi: 10.1093/mnras/stad3371

    2022 doi

  62. [73]

    A., McNamara, B

    Pulido, F. A., McNamara, B. R., Edge, A. C., et al. 2018, ApJ, 853, 177, doi: 10.3847/1538-4357/aaa54b

    2018 doi

  63. [74]

    W., Nulsen, P

    Randall, S. W., Nulsen, P. E. J., Jones, C., et al. 2015, ApJ, 805, 112, doi: 10.1088/0004-637X/805/2/112

    2015 doi

  64. [75]

    2012, APLpy: Astronomical Plotting Library in Python

    Robitaille, T., & Bressert, E. 2012, APLpy: Astronomical Plotting Library in Python. http://ascl.net/1208.017

    2012

  65. [76]

    C., Combes, F., et al

    Rose, T., Edge, A. C., Combes, F., et al. 2019, MNRAS, 489, 349, doi: 10.1093/mnras/stz2138

    2019 doi

  66. [77]

    R., Combes, F., et al

    Rose, T., McNamara, B. R., Combes, F., et al. 2023, MNRAS, 518, 878, doi: 10.1093/mnras/stac3194 —. 2024, MNRAS, 533, 771, doi: 10.1093/mnras/stae1831

    2023 doi

  67. [78]

    A., et al

    Ruffa, I., Prandoni, I., Laing, R. A., et al. 2019a, MNRAS, 484, 4239, doi: 10.1093/mnras/stz255

    doi

  68. [79]

    A., Prandoni, I., et al

    Ruffa, I., Davis, T. A., Prandoni, I., et al. 2019b, MNRAS, 489, 3739, doi: 10.1093/mnras/stz2368

    doi

  69. [80]

    R., McNamara, B

    Russell, H. R., McNamara, B. R., Fabian, A. C., et al. 2019, MNRAS, 490, 3025, doi: 10.1093/mnras/stz2719 Salomé, P., & Combes, F. 2003, A&A, 412, 657, doi: 10.1051/0004-6361:20031438 18 R AJPUROHIT ET AL

    2019 doi

  70. [81]

    S., Fabian, A

    Sanders, J. S., Fabian, A. C., & Taylor, G. B. 2009, MNRAS, 396, 1449, doi: 10.1111/j.1365-2966.2009.14892.x

    2009

  71. [82]

    I., Cortese, L., & Koribalski, B

    Saraf, M., Wong, O. I., Cortese, L., & Koribalski, B. S. 2023, MNRAS, 519, 4128, doi: 10.1093/mnras/stac3695

    2023 doi

  72. [83]

    Scaife, A. M. M., & Heald, G. H. 2012, MNRAS, 423, L30, doi: 10.1111/j.1745-3933.2012.01251.x

    2012

  73. [84]

    P., Vrtilek, J., et al

    Schellenberger, G., David, L. P., Vrtilek, J., et al. 2021, ApJ, 906, 16, doi: 10.3847/1538-4357/abc488 —. 2020, ApJ, 894, 72, doi: 10.3847/1538-4357/ab879c

    2021 doi

  74. [85]

    P., et al

    Schellenberger, G., O’Sullivan, E., David, L. P., et al. 2024, ApJ, 976, 246, doi: 10.3847/1538-4357/ad89bc

    2024 doi

  75. [86]

    2012, MNRAS, 422, 1835, doi: 10.1111/j.1365-2966.2012.20219.x

    Serra, P., Oosterloo, T., Morganti, R., et al. 2012, MNRAS, 422, 1835, doi: 10.1111/j.1365-2966.2012.20219.x

    2012

  76. [87]

    2015, MNRAS, 448, 1922, doi: 10.1093/mnras/stv079

    Serra, P., Westmeier, T., Giese, N., et al. 2015, MNRAS, 448, 1922, doi: 10.1093/mnras/stv079

    2015 doi

  77. [88]

    2018, ApJ, 858, 17, doi: 10.3847/1538-4357/aab9b0

    Temi, P., Amblard, A., Gitti, M., et al. 2018, ApJ, 858, 17, doi: 10.3847/1538-4357/aab9b0

    2018 doi

  78. [89]

    L., Dressler, A., Blakeslee, J

    Tonry, J. L., Dressler, A., Blakeslee, J. P., et al. 2001, ApJ, 546, 681, doi: 10.1086/318301

    2001 doi

  79. [90]

    2023, ApJ, 944, 216, doi: 10.3847/1538-4357/acacf9 van Weeren, R

    Ubertosi, F., Gitti, M., Brighenti, F., et al. 2023, ApJ, 944, 216, doi: 10.3847/1538-4357/acacf9 van Weeren, R. J., Timmerman, R., Vaidya, V ., et al. 2024, arXiv e-prints, arXiv:2410.02863, doi: 10.48550/arXiv.2410.02863

    2023 doi arXiv

  80. [91]

    N., McNamara, B

    Vantyghem, A. N., McNamara, B. R., Edge, A. C., et al. 2017, ApJ, 848, 101, doi: 10.3847/1538-4357/aa8fd0

    2017 doi

  81. [92]

    A., Sage, L

    Welch, G. A., Sage, L. J., & Young, L. M. 2010, ApJ, 725, 100, doi: 10.1088/0004-637X/725/1/100

    2010 doi

  82. [93]

    Werner, N., Oonk, J. B. R., Sun, M., et al. 2014, MNRAS, 439, 2291, doi: 10.1093/mnras/stu006

    2014 doi

  83. [94]

    G., Hollenbach, D., McKee, C

    Wolfire, M. G., Hollenbach, D., McKee, C. F., Tielens, A. G. G. M., & Bakes, E. L. O. 1995, ApJ, 443, 152, doi: 10.1086/175510

    1995 doi

  84. [95]

    M., Bureau, M., Davis, T

    Young, L. M., Bureau, M., Davis, T. A., et al. 2011, MNRAS, 414, 940, doi: 10.1111/j.1365-2966.2011.18561.x

    2011

Pith tools

Reviewed August 10, 2026 · model on record in the stance chip above.