Pith. sign in

REVIEW 3 major objections 5 minor 83 references

Investigating the HI distribution and kinematics of ESO444-G084 and [KKS2000]23: New insights from the MHONGOOSE survey

T0 review · 3 major / 5 minor · reviewed 2026-08-07 · deepseek-v4-flash

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

Pith's one-line read The paper claims that two isolated dwarf galaxies with similar rotation speeds conceal opposite dark matter structures: one compact and dense, the other diffuse and cored.

desk verdict A useful two-galaxy MeerKAT study whose headline halo-density contrast rests on an under-tested inner rotation-curve fit, not the M/L assumption. read the letter →

arxiv 2506.04101 v1 pith:MP3FFLOZ submitted 2025-06-04 astro-ph.GA

Brenda Namumba , Roger Ianjamasimanana , Bärbel Koribalski , Albert Bosma , Evangelia Athanassoula , Claude Carignan , Gyula I. G. Józsa , Peter Kamphuis
show 20 more authors
Roger P. Deane Sinenhlanhla P. Sikhosana Lourdes Verdes-Montenegro Amidou Sorgho Xola Ndaliso Philippe Amram Elias Brinks Laurent Chemin Francoise Combes Erwin de Blok Nathan Deg Jayanne English Julia Healy Sushma Kurapati Antonino Marasco Stacy McGaugh Kyle Oman Kristine Spekkens Simone Veronese O. Ivy Wong
This is my paper
classification astro-ph.GA
keywords dwarfirregulargalaxiesneutralhydrogen21-cmHIobservationsrotationcurvesdarkmatterhalomassmodelingToomreQstabilitystarformation
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

This paper uses the deepest available 21-centimeter hydrogen maps of two isolated dwarf galaxies, ESO444-G084 and [KKS2000]23, to ask how gas, dark matter, and star formation interact in low-mass systems. It claims that the two galaxies, despite reaching similar maximum rotation speeds, have very different inner mass distributions: ESO444-G084 rises fast and requires a compact dark-matter halo with central density $\rho_0 = (16.05 \pm 1.45)\times10^{-3} M_\odot\,\mathrm{pc}^{-3}$, while [KKS2000]23 rises gradually and is best fit by a more diffuse halo with $\rho_0 = (4.29 \pm 0.43)\times10^{-3} M_\odot\,\mathrm{pc}^{-3}$. The same data show a decoupling of gravitational stability from star formation: ESO444-G084 is globally stable yet forming stars in localized clumps, whereas [KKS2000]23 is unstable but shows little recent star formation. If right, the results imply that dwarf galaxy halos are diverse in concentration even at fixed rotation speed, and that internal gas processes, not inflows or outflows, set the pace of star formation.

What carries the argument

The argument is carried by 3D tilted-ring kinematic fitting (the TiRiFiC and PyFAT codes) applied directly to the HI data cubes, which corrects for beam smearing and allows separate approaching- and receding-side rotation curves. The rotation curves are corrected for asymmetric drift using the pressure-gradient formula of Meurer et al. (1996), and then decomposed with the pseudo-isothermal (ISO) halo profile $\rho(r) = \rho_0/[1+(r/r_c)^2]$ inside a rotation-curve fitting routine that fixes the stellar disk via WISE 3.4-micron surface brightness and a mass-to-light ratio, and the gas disk via HI surface density scaled by 1.4 for helium. The two fitted halo parameters, central density $\rho_0$ and core radius $r_c$, are what the paper compares between the two galaxies. Disk stability is assessed through pixel-by-pixel Toomre $Q_{\rm gas}$ and $\Sigma_{\rm gas}/\Sigma_{\rm crit}$ maps, with uncertainties propagated from the rotation curve, velocity dispersion, and gas surface density.

What would settle it

A direct test would measure the stellar mass-to-light ratios independently, for example by fitting the full optical-to-infrared spectral energy distribution or using resolved stellar populations, and then re-fitting the isothermal halo parameters. If the true $M/L$ for ESO444-G084 is close to 0.5, its fitted core radius expands from 3.48 to 5.84 kpc and becomes unconstrained, erasing the factor-of-four central-density contrast; alternatively, a high-resolution inner rotation curve using CO or H-alpha integral-field data inside 1 kpc would show whether the fast rise is real or smoothed by the beam.

Watch

Extended reading notes

Core claim

On its own terms, the paper's central claim is that high-sensitivity, high-resolution HI observations resolve two contrasting dwarf galaxy states. ESO444-G084 shows smooth, centrally concentrated neutral hydrogen with a kinematic warp beyond roughly 1.8 kpc and a fast-rising rotation curve, which the authors interpret as a centrally concentrated dark matter halo; [KKS2000]23 shows clumpy, asymmetric HI and a gently rising rotation curve that continues to climb past 6 kpc, indicating a more extended, cored dark matter halo. Using a pseudo-isothermal halo and WISE-based stellar mass-to-light ratios of 0.20 and 0.18 respectively, the fitted core radii are $3.48\pm0.57$ kpc and $5.49\pm0.60$ kpc, and the central dark matter densities differ by nearly a factor of four. The rotation curves, after asymmetric-drift correction, imply disk-like kinematics in both galaxies, with no significant radial inflows or outflows detected. The paper further claims that spatially resolved Toomre $Q$ maps and $\Sigma_{\rm gas}/\Sigma_{\rm crit}$ maps show ESO444-G084 remains globally stable while its H$\alpha$ and FUV emission indicate localized star formation, whereas [KKS2000]23 has unstable regions yet weak H$\alpha$, suggesting that turbulence, gas depletion, or past feedback suppresses star formation.

Load-bearing premise

The load-bearing premise is that the adopted stellar mass-to-light ratios ($0.20$ for ESO444-G084 and $0.18$ for [KKS2000]23, from the WISE color relation) correctly fix the stellar disk's contribution; if the true values are higher, the fitted halo densities and core radii change substantially, and the paper's own $M/L = 0.5$ test shows the concentrated-halo reading of ESO444-G084 would lose its constraint.

Editorial extensions

If this is right

  • Dwarf galaxy dark matter halos are not uniform: two isolated galaxies of similar rotation speed can differ by a factor of about four in central dark-matter density, so mass models of individual dwarfs matter more than averaged scaling relations.
  • A fast-rising HI rotation curve does not require a cuspy NFW halo; the pseudo-isothermal cored profile fits ESO444-G084, so conclusions about cusps versus cores must come from full fits rather than curve steepness alone.
  • Gravitational instability is neither necessary nor sufficient for star formation in dwarfs: ESO444-G084 forms stars while globally stable, and [KKS2000]23 is unstable yet has little recent H-alpha emission.
  • The FUV-to-H-alpha ratio difference implies that recent star formation has declined in [KKS2000]23 relative to the past 100 million years, pointing to episodic, internally regulated star-formation cycles.
  • With no detectable inflows or outflows at the survey's sensitivity, internal gas dynamics and feedback, not gas accretion, set the current star-formation behavior in these dwarfs.

Reading between the lines

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

  • Beyond the paper, if the adopted stellar mass-to-light ratios are even moderately underestimated, the claimed halo contrast weakens: the paper itself finds that raising both $M/L$ values to 0.5 moves ESO444-G084's core radius from 3.48 to 5.84 kpc and leaves it unconstrained, so an independent stellar-mass estimate from full spectral energy distribution fitting would directly test the concentrated
  • Beyond the paper, the beam-size interpretation of the HI diameter growth at low column density could be checked by observing a few dwarfs with the same integration time at even lower angular resolution or with longer baselines; if genuinely faint extended gas exists below the current surface-brightness limit, it would alter total HI masses and outer rotation curves.
  • Beyond the paper, comparing the spatially resolved $Q$ maps with molecular gas tracers would sharpen the stability-versus-star-formation puzzle: if [KKS2000]23 has no molecular clouds despite its instability, that would support the turbulence-suppression picture, whereas finding dense gas would shift the explanation toward feedback or depletion history.
  • Beyond the paper, the two galaxies may bracket an evolutionary sequence, with the compact-halo dwarf in a stable, star-forming state and the cored-halo dwarf in a post-burst, quiescent state; resolved stellar-population ages or color maps would test whether halo structure and star-formation phase are causally linked or merely correlated.
Share X Bluesky LinkedIn Reddit HN

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 presents MeerKAT/MHONGOOSE 21-cm HI observations of two nearby isolated dwarf irregular galaxies, ESO444-G084 and [KKS2000]23. The authors measure total HI fluxes and masses, derive rotation curves with the 3D tilted-ring codes PyFAT and TiRiFiC, apply an asymmetric-drift correction, fit pseudo-isothermal dark matter halo models to the circular velocities, and construct spatially resolved Toomre Q and Sigma_gas/Sigma_crit maps to connect disk stability with H-alpha and FUV star-formation tracers. The central physical claim is that the two dwarfs have contrasting dark matter distributions: ESO444-G084 has a high central halo density (rho0 = 16.05 +/- 1.45 x 10^-3 Msun pc^-3 at adopted M/L=0.2) and a relatively fast-rising rotation curve, whereas [KKS2000]23 has a lower central density (4.29 +/- 0.43 x 10^-3) and a more gradual rise, implying a more extended, cored halo. The paper also reports a kinematic warp in ESO444-G084, the absence of detectable inflows/outflows, and contrasting star-formation states: localized star formation in ESO444-G084 despite global stability, and gravitational instability in [KKS2000]23 despite weak H-alpha emission.

Significance. If the central density contrast is robust, the paper provides a useful addition to the small set of low-mass galaxies with well-resolved HI rotation curves and dark matter decompositions, and it sharpens the observational picture of dwarf-galaxy halo diversity. The strengths of the manuscript are the high-quality 50-hour MeerKAT data, the use of established 3D kinematic modeling pipelines, the detailed channel-map and position-velocity comparisons, and the explicit uncertainty maps for the stability diagnostics. The mass-modeling and stability analysis are presented transparently, with both WISE-based and alternative mass-to-light ratios explored. The principal significance rests on a single comparison of two galaxies, so the result is suggestive rather than statistical, but it is a legitimate case study.

major comments (3)
  1. [Section 5.2.1, Eq. (8), Table 8] The central claim of a factor ~3.7 difference in central isothermal halo density rho0 is set primarily by the inner slope of the rotation curve, because V_iso^2 ~ (4*pi*G*rho0/3) r^2 for r << r_c (Eq. 8). For ESO444-G084 that slope is measured in a region where the paper reports radial velocities of up to ~20 km/s (Section 5.2.1, Fig. 6) while V_rot is only ~10-35 km/s over the same radii (Table 5), and the TiRiFiC model explicitly includes a fitted radial-velocity term with a manually guided iterative fit. The paper does not report a control fit with V_rad fixed to zero, nor does it give confidence contours in the (rho0, r_c) plane that include the V_rot-V_rad covariance. Without such a test, the reader cannot assess whether the fast-rise/concentrated-halo interpretation is robust or is partly an artifact of the non-circular-motion degeneracy. Please add a control fit or otherwise quantify how much rho0 and r_c shift when V_rad is forced to zero or varied over its plausible range.
  2. [Section 6.4, Table 8] The adopted stellar mass-to-light ratio is a load-bearing input for the absolute halo parameters. The paper's own Table 8 shows that for ESO444-G084, changing (M/L)_3.4 from 0.2 to 0.5 changes rho0 from 16.05 to 11.47 x 10^-3 Msun pc^-3 and makes the core radius poorly constrained (5.84 +/- 2.64 kpc, similar to or larger than the outermost data point). The qualitative ESO-versus-KKS contrast survives this change, but the magnitude of the central concentration and the 'centrally concentrated halo' wording depend on the adopted M/L. Please either present the halo parameter constraints as a function of M/L over a plausible range (e.g., 0.1-0.6) or marginalize over M/L with a prior, rather than quoting a single WISE-based value as the headline result.
  3. [Section 5.2.1 versus Abstract and Conclusions] There is a direct internal tension in the description of ESO444-G084's rotation curve. Section 5.2.1 states that the curve exhibits a gradual rise in the inner region (R < 2 kpc) 'rather than the steep, abrupt increase expected for an NFW-like halo,' while the abstract and conclusions call it 'fast-rising' and use it to support a centrally concentrated dark matter distribution. Please reconcile these statements by defining a quantitative measure of 'fast' versus 'gradual' (e.g., V(2 kpc)/V_max, logarithmic slope, or rise time) and apply the same measure to both galaxies.
minor comments (5)
  1. [Table 6] The table caption reads '[KKS2000]2' but should read '[KKS2000]23'.
  2. [Eq. (2)] The quantity b in the asymmetric-drift equation is used but never defined; please state explicitly that it is the one-dimensional velocity dispersion and clarify the relation between b and sigma_D.
  3. [Section 4.2] The sentence 'The velocity and dispersion maps included in Fig. 2 will be analyzed in detail in Section 5' appears to refer to the [KKS2000]23 maps, which are shown in Fig. 3 rather than Fig. 2; please correct the cross-reference.
  4. [Section 8.3] The reference to 'Girelli et al. 2020' is preceded by a stray '?' in the text; please fix the citation formatting.
  5. [Section 7, Eq. (14)-(16)] The uncertainty propagation for Q_gas and Sigma_gas/Sigma_crit uses only absolute values of first-order partial derivatives and ignores covariance terms between kappa, Sigma, and sigma_HI; since kappa itself comes from a fitted rotation curve, please state this simplification or include the leading covariance terms.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the rotation curves are observed inputs, halo parameters are fit to them, and no claim reduces to its own input by construction.

full rationale

The paper's derivation chain is self-contained against external data. Rotation curves are measured from the MeerKAT cubes via 3D tilted-ring modeling (Section 5), and the dark matter halo parameters in Table 8 are obtained by fitting the pseudo-isothermal circular-velocity profile (Eq. 8) to those curves, with baryonic contributions fixed by an externally calibrated WISE-based M/L. The central-density comparison (rho0 = 16.05 vs 4.29 x 10^-3 M_sun pc^-3) is therefore a fitted result, not a prediction that reduces to its input. The Toomre-Q / stability analysis uses the same rotation information through Eq. (13) as a smooth parameterization of the observed kinematics, and the stability criterion is not fed back into the mass-model fit, so this is a diagnostic applied after fitting rather than a circular derivation. Citations to de Blok et al. (2024), TiRiFiC, and PyFAT are data and software provenance, not load-bearing self-citations; the ISO halo is adopted as an explicit empirical model with stated alternatives, not smuggled in via a self-citation. The paper's own caveats, such as the M/L = 0.5 case leaving the core radius only weakly constrained and radial motions up to ~20 km/s in the inner region of ESO444-G084, are robustness and systematic-uncertainty issues, not circularity. The broken citation '?Girellietal.2020' in Section 8.3 is a completeness/formatting artefact and does not affect the circularity verdict. No equation or conclusion is equivalent to its own input by construction.

Assumptions & free parameters 7 free parameters · 6 assumptions · 0 invented entities

The free parameters are the adopted stellar mass-to-light ratios and the fitted halo parameters that determine the dark matter conclusions. The assumptions are standard in dwarf galaxy mass modeling and are stated in the text; none introduces a new entity.

free parameters (7)
  • (M/L)*3.4um for ESO444-G084 = 0.20
    Stellar mass-to-light ratio in WISE 3.4 micron band, derived from Cluver et al. (2014) relation using W3.4-W4.6 = 0.32; fixes stellar disk contribution in mass modeling (Section 6.1).
  • (M/L)*3.4um for [KKS2000]23 = 0.18
    Same relation using W3.4-W4.6 = 0.36; fixes stellar disk contribution (Section 6.1).
  • ISO halo core radius r_c for ESO444-G084 = 3.48 +/- 0.57 kpc
    Fitted free parameter of pseudo-isothermal halo model adjusted to match observed rotation curve (Section 6.4.1).
  • ISO halo central density rho0 for ESO444-G084 = (16.05 +/- 1.45) x 10^-3 M_sun pc^-3
    Fitted free parameter of halo model; result drives conclusion of concentrated dark matter.
  • ISO halo core radius r_c for [KKS2000]23 = 5.49 +/- 0.60 kpc
    Fitted free parameter, Section 6.4.2.
  • ISO halo central density rho0 for [KKS2000]23 = (4.29 +/- 0.43) x 10^-3 M_sun pc^-3
    Fitted free parameter, Section 6.4.2.
  • V_flat and l_flat in Eq. 13 for both galaxies = not reported in text
    Free parameters of the parameterized rotation curve used to compute epicyclic frequency and stability maps (Section 7); fitted to the mass model rotation curve but values are not listed.
assumptions (6)
  • domain assumption Galaxies are axisymmetric and in dynamical equilibrium so that circular velocity traces total gravitational potential (Eq. 3)
    Standard assumption in mass modeling, stated in Section 6.
  • domain assumption Molecular gas contribution is negligible
    Dwarf galaxies typically have low CO; Section 6.2 states only HI and helium are included.
  • domain assumption Helium correction factor of 1.4
    Widely adopted to account for helium; Section 6.2.
  • domain assumption Stellar disk is infinitely thin in ROTMOD
    Section 6.1 states ROTMOD assumes infinitely thin axisymmetric disk.
  • domain assumption Scale height gradient is negligible in pressure gradient correction (d ln h_z/dR = 0)
    Section 5.1 explicitly assumes negligible scale height gradient.
  • domain assumption Pseudo-isothermal (ISO) halo model describes the dark matter density profile
    Section 6.3 adopts ISO model as benchmark; alternative models are not fitted.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Investigating the HI distribution and kinematics of ESO444-G084 and [KKS2000]23: New insights from the MHONGOOSE survey." pith.science (2026). https://pith.science/paper/MP3FFLOZ

@misc{pith2026250604101,
  author       = {Pith},
  title        = {Pith review of: Investigating the HI distribution and kinematics of ESO444-G084 and [KKS2000]23: New insights from the MHONGOOSE survey},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/MP3FFLOZ}},
  note         = {Machine review of arXiv:2506.04101}
}
read the original abstract

We present the HI distribution, kinematics, mass modeling, and disk stability of the dwarf irregular galaxies ESO444-G084 and [KKS2000]23 using high-resolution, high-sensitivity MHONGOOSE survey data from MeerKAT. ESO444-G084 shows centrally concentrated HI emission, while [KKS2000]23 exhibits irregular high-density clumps. Total HI fluxes measured down to 10^19 and 10^18 cm^-2 are nearly identical, indicating that the increased HI diameter at lower column densities results mainly from the larger beam, with no significant extra emission detected. We derive total HI masses of (1.1 +/- 0.1) x 10^8 and (6.1 +/- 0.3) x 10^8 solar masses for ESO444-G084 and [KKS2000]23, respectively. Using PyFAT and TiRiFiC, we extract 3D rotation curves that reveal disk-like kinematics in both galaxies. ESO444-G084 shows a warp beyond ~1.8 kpc and a fast-rising curve consistent with a centrally concentrated dark matter distribution, while [KKS2000]23's more gradual rise suggests a more extended halo. Mass modeling with an isothermal halo and stellar mass-to-light ratios of 0.20 for ESO444-G084 and 0.18 for [KKS2000]23 yields consistent results. We analyze disk stability using spatially resolved Toomre Q and gas-to-critical surface density ratios, linking these with H-alpha and FUV-based star formation. ESO444-G084 supports localized star formation despite global stability, while [KKS2000]23 appears gravitationally unstable yet lacks H-alpha, suggesting that turbulence, gas depletion, or past feedback suppresses star formation. No inflows or outflows are detected, indicating internal processes regulate star formation. This study highlights the interplay between HI morphology, kinematics, dark matter distribution, and disk stability, showing how internal processes shape dwarf galaxy evolution.

Figures

Figures reproduced from arXiv: 2506.04101 by the authors.

Figure 1
Figure 1. MeerKAT H i column density contours from different H i resolution cubes of ESO444–G084 (left) and [KKS2000]23 (right) are overlaid on DECaLS grayscale images in the gri bands. Each contour level represents the H i column density at S/N = 3 for each spatial resolution. The color bar values indicate the average beam size corresponding to each spatial resolution. The ellipses in the lower-left corner of each map denote… view at source ↗
Figure 2
Figure 2. High-resolution maps of ESO444–G084. Top left: H i column density maps from the highest resolution cubes. Top right: The GALEX FUV images. Bottom left: Velocity field models (pink contours) and observed (white contours) overlaid on velocity field maps (observed). Bottom right: Dispersion map models (pink contours) overlaid on the data. The velocity field and dispersion map models were derived from the kinematic anal… view at source ↗
Figure 3
Figure 3. High-resolution maps of [KKS2000]23. Top left: H i column density maps from the highest resolution cubes. Top right: The GALEX FUV images. Bottom left: Velocity field models (pink contours) and observed (white contours) overlaid on velocity field maps (observed). Bottom right: Dispersion map models (pink contours) overlaid on the data. The velocity field and dispersion map models were derived from the kinematic anal… view at source ↗
Figures from the paper (14 more)
Figure 4
Figure 4. Figure 4: Integrated H i spectra of ESO444–G084 (left) and [KKS2000]23 (right) from MeerKAT (black solid line) and HIPASS (black dashed line, Koribalski et al. 2004). The black arrow on each figure shows the kinematic systemic velocity of each galaxy derived in Section 5. The ho…
Figure 5
Figure 5. Figure 5: Observed rotation curves (grey) and asymmetric drift-corrected rotation curves (black) for ESO444–G084 (left) and [PITH_FULL_IMAGE:figures/full_fig_p008_5.png]
Figure 6
Figure 6. Figure 6: Best-fit kinematic parameters of ESO444–G084 derived from the H [PITH_FULL_IMAGE:figures/full_fig_p009_6.png]
Figure 7
Figure 7. Figure 7: Best-fit kinematic parameters of [KKS2000]23 derived from the H [PITH_FULL_IMAGE:figures/full_fig_p010_7.png]
Figure 8
Figure 8. Figure 8: Individual channel maps of ESO444-G084 from the MeerKAT high-resolution cube. Blue contours represent the channel [PITH_FULL_IMAGE:figures/full_fig_p011_8.png]
Figure 9
Figure 9. Figure 9: Individual channel maps of [KKS2000]23 from the MeerKAT high-resolution cube. Blue contours represent the channel [PITH_FULL_IMAGE:figures/full_fig_p012_9.png]
Figure 10
Figure 10. Figure 10: Top: The moment-0 map of ESO444-G084 from the MeerKAT high-resolution cube, displaying grey arrows that indicate [PITH_FULL_IMAGE:figures/full_fig_p013_10.png]
Figure 11
Figure 11. Figure 11: Top: The moment-0 map of [KKS2000]23 from the MeerKAT high-resolution cube, displaying grey arrows that indicate the [PITH_FULL_IMAGE:figures/full_fig_p014_11.png]
Figure 12
Figure 12. Figure 12: Isothermal (ISO) mass modeling results for ESO444–G084. The decomposition for both galaxies was performed under two [PITH_FULL_IMAGE:figures/full_fig_p015_12.png]
Figure 13
Figure 13. Figure 13: Isothermal (ISO) mass modeling results for [KKS2000]23. The decomposition for both galaxies was performed under two [PITH_FULL_IMAGE:figures/full_fig_p015_13.png]
Figure 14
Figure 14. Figure 14: The black points represent the best-fit rotation velocities from the ISO mass model, while the red points correspond to the [PITH_FULL_IMAGE:figures/full_fig_p017_14.png]
Figure 15
Figure 15. Figure 15: MeerKAT high resolution maps of the Qgas parameter and Σgas/Σcrit for ESO444-G084 (top) and [KKS2000]23 (bottom). The black contours present values of 𝑄 < 1 while the blue contours show Σgas/Σcrit >1. Note: The color scale for Q is limited to a maximum of Q = 2 for vi…
Figure 16
Figure 16. Figure 16: Spatial distribution of uncertainties associated with the Toomre [PITH_FULL_IMAGE:figures/full_fig_p018_16.png]
Figure 17
Figure 17. Figure 17: High-resolution MeerKAT H i column density maps (black contours), GALEX FUV (cyan contours), and H𝛼 (crimson contours) of ESO444–G084 (left) and [KKS2000]23 (right) overlaid on DECaLS optical maps. The H i column density contours are set at (2.0, 2.5, 4.0) ×1021 cm−2 …

Discussion (0). Sign in to comment.

Reference graph

Works this paper leans on

83 extracted references · 49 canonical work pages

  1. [1]

    & Bureau, M

    Athanassoula, E. & Bureau, M. 1999, ApJ, 522, 699

    1999

  2. [2]

    G., Staveley-Smith, L., de Blok, W

    Barnes, D. G., Staveley-Smith, L., de Blok, W. J. G., et al. 2001, MNRAS, 322, 486

    2001

  3. [3]

    Begeman, K. G. 1989, A&A, 223, 47

    1989

  4. [4]

    G., Broeils, A

    Begeman, K. G., Broeils, A. H., & Sanders, R. H. 1991, MNRAS, 249, 523 Begum,A.,Chengalur,J.N.,Karachentsev,I.D.,Sharina,M.E.,&Kaisin,S.S. 2008, MNRAS, 386, 1667

    work page 1991

  5. [5]

    2008, AJ, 136, 2846

    Bigiel, F., Leroy, A., Walter, F., et al. 2008, AJ, 136, 2846

    2008

  6. [6]

    2004, A&A, 420, 147

    Blais-Ouellette, S., Amram, P., Carignan, C., & Swaters, R. 2004, A&A, 420, 147

    work page 2004

  7. [7]

    1978, PhD thesis, University of Groningen, Netherlands

    Bosma, A. 1978, PhD thesis, University of Groningen, Netherlands

    1978

  8. [8]

    Bullock, J. S. & Boylan-Kolchin, M. 2017, ARA&A, 55, 343

    2017

Show all 83 references
  1. [9]

    2018, ApJ, 856, 180

    Camilo, F., Scholz, P., Serylak, M., et al. 2018, ApJ, 856, 180

    2018

  2. [10]

    & Freeman, K

    Carignan, C. & Freeman, K. C. 1985, ApJ, 294, 494

    1985

  3. [11]

    & Freeman, K

    Carignan, C. & Freeman, K. C. 1988, ApJ, 332, L33

    1988

  4. [12]

    & Purton, C

    Carignan, C. & Purton, C. 1998, ApJ, 506, 125

    1998

  5. [13]

    D., Machacek, M

    Carlson, E. D., Machacek, M. E., & Hall, L. J. 1992, ApJ, 398, 43

    1992

  6. [14]

    M., Saintonge, A., et al

    Chamba, N., Marcum, P. M., Saintonge, A., et al. 2024, ApJ, 974, 247

    2024

  7. [15]

    E., Jarrett, T

    Cluver, M. E., Jarrett, T. H., Hopkins, A. M., et al. 2014, ApJ, 782, 90 Côté, S., Carignan, C., & Freeman, K. C. 2000, AJ, 120, 3027

    2014

  8. [16]

    A., Cohen, S

    Dale, D. A., Cohen, S. A., Johnson, L. C., et al. 2009, ApJ, 703, 517 de Blok, W. J. G. 2010, Advances in Astronomy, 2010, 789293 de Blok, W. J. G., Athanassoula, E., Bosma, A., et al. 2020, A&A, 643, A147 de Blok, W. J. G., Healy, J., Maccagni, F. M., et al. 2024, A&A, 688, A...

    2009

  9. [17]

    J., Lang, D., et al

    Dey, A., Schlegel, D. J., Lang, D., et al. 2019, AJ, 157, 168 Di Cintio, A., Brook, C. B., Dutton, A. A., et al. 2014, MNRAS, 441, 2986 Di Teodoro, E. M. & Fraternali, F. 2015, MNRAS, 451, 3021

    2019

  10. [18]

    Downing, E. R. & Oman, K. A. 2023, MNRAS, 522, 3318

    2023

  11. [19]

    A., Obreja, A., & Macciò, A

    Dutton, A. A., Obreja, A., & Macciò, A. V. 2019, MNRAS, 482, 5606

    2019

  12. [20]

    Elmegreen, B. G. 2002, ApJ, 577, 206

    2002

  13. [21]

    Elmegreen, B. G. & Hunter, D. A. 2015, ApJ, 805, 145

    2015

  14. [22]

    C., de Blok, W

    Elson, E. C., de Blok, W. J. G., & Kraan-Korteweg, R. C. 2012, AJ, 143, 1

    2012

  15. [23]

    Flores, R. A. & Primack, J. R. 1994, ApJ, 427, L1 Article number, page 21 of 22 A&A proofs: manuscript no. b

    1994

  16. [24]

    2017, A&A, 606, A47

    Fragkoudi, F., Di Matteo, P., Haywood, M., et al. 2017, A&A, 606, A47

    2017

  17. [25]

    & Jog, C

    Ghosh, S. & Jog, C. J. 2018, New A, 63, 38

    2018

  18. [26]

    2020, A&A, 634, A135

    Girelli, G., Pozzetti, L., Bolzonella, M., et al. 2020, A&A, 634, A135

    2020

  19. [27]

    Gnedin, O. Y. & Zhao, H. 2002, MNRAS, 333, 299

    2002

  20. [28]

    2012, MNRAS, 422, 1231

    Governato, F., Zolotov, A., Pontzen, A., et al. 2012, MNRAS, 422, 1231

    2012

  21. [29]

    Healy, J., de Blok, W. J. G., Maccagni, F. M., et al. 2024, A&A, 687, A254

    2024

  22. [30]

    F., Quataert, E., & Murray, N

    Hopkins, P. F., Quataert, E., & Murray, N. 2012, MNRAS, 421, 3488

    2012

  23. [31]

    2000, Phys

    Hu, W., Barkana, R., & Gruzinov, A. 2000, Phys. Rev. Lett., 85, 1158

    2000

  24. [32]

    A., Elmegreen, B

    Hunter, D. A., Elmegreen, B. G., Goldberger, E., et al. 2021, AJ, 161, 71

    2021

  25. [33]

    A., Elmegreen, B

    Hunter, D. A., Elmegreen, B. G., Oh, S.-H., et al. 2011, AJ, 142, 121

    2011

  26. [34]

    A., Ficut-Vicas, D., Ashley, T., et al

    Hunter, D. A., Ficut-Vicas, D., Ashley, T., et al. 2012, AJ, 144, 134

    2012

  27. [35]

    & MeerKAT Team

    Jonas, J. & MeerKAT Team. 2016, in MeerKAT Science: On the Pathway to the SKA, 1 Józsa, G. I. G., Kenn, F., Klein, U., & Oosterloo, T. A. 2007, A&A, 468, 731 Józsa, G. I. G., Kenn, F., Oosterloo, T. A., & Klein, U. 2012, TiRiFiC: Tilted Ring Fitting Code, Astrophysics Source C...

    2016

  28. [36]

    Kaldare, R., Colless, M., Raychaudhury, S., & Peterson, B. A. 2003, MNRAS, 339, 652

    2003

  29. [37]

    2024, pyFAT: Python Fully Automated TiRiFiC, Astrophysics Source Code Library, record ascl:2407.002

    Kamphuis, P. 2024, pyFAT: Python Fully Automated TiRiFiC, Astrophysics Source Code Library, record ascl:2407.002

    2024

  30. [38]

    Kamphuis, P., Józsa, G. I. G., Oh, S. . H., et al. 2015, MNRAS, 452, 3139 Karachentsev,I.D.,Karachentseva,V.E.,Suchkov,A.A.,&Grebel,E.K.2000, A&AS, 145, 415

    2015

  31. [39]

    D., Sharina, M

    Karachentsev, I. D., Sharina, M. E., Dolphin, A. E., et al. 2002, A&A, 385, 21

    2002

  32. [40]

    1989, ApJ, 344, 685

    Kennicutt, Robert C., J. 1989, ApJ, 344, 685

    1989

  33. [41]

    Kennicutt, R. C. & Evans, N. J. 2012, ARA&A, 50, 531 Kereš, D., Katz, N., Weinberg, D. H., & Davé, R. 2005, Monthly Notices of the Royal Astronomical Society, 363, 2, provided by SAO/NASA Astrophysics Data System

    2012

  34. [42]

    2021, A&A, 654, A7

    Khademi, M., Yang, Y., Hammer, F., & Nasiri, S. 2021, A&A, 654, A7

    2021

  35. [43]

    S., Staveley-Smith, L., Kilborn, V

    Koribalski, B. S., Staveley-Smith, L., Kilborn, V. A., et al. 2004, AJ, 128, 16

    2004

  36. [44]

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

    Koribalski, B. S., Staveley-Smith, L., Westmeier, T., et al. 2020, Ap&SS, 365, 118

    2020

  37. [45]

    S., Wang, J., Kamphuis, P., et al

    Koribalski, B. S., Wang, J., Kamphuis, P., et al. 2018, MNRAS, 478, 1611

    2018

  38. [46]

    S., Boylan-Kolchin, M., et al

    Lazar, A., Bullock, J. S., Boylan-Kolchin, M., et al. 2020, MNRAS, 497, 2393

    2020

  39. [47]

    S., & Schombert, J

    Lelli, F., McGaugh, S. S., & Schombert, J. M. 2016, AJ, 152, 157

    2016

  40. [48]

    K., Walter, F., Brinks, E., et al

    Leroy, A. K., Walter, F., Brinks, E., et al. 2008, AJ, 136, 2782 López-Sánchez, Á. R., Koribalski, B. S., van Eymeren, J., et al. 2012, MNRAS, 419, 1051 Mac Low, M.-M. & Ferrara, A. 1999, ApJ, 513, 142

    2008

  41. [49]

    A., Navarro, J

    Marasco, A., Oman, K. A., Navarro, J. F., Frenk, C. S., & Oosterloo, T. 2018, MNRAS, 476, 2168

    2018

  42. [50]

    C., Fanson, J., Schiminovich, D., et al

    Martin, D. C., Fanson, J., Schiminovich, D., et al. 2005, ApJ, 619, L1

    2005

  43. [51]

    Martinsson, T. P. K., Verheijen, M. A. W., Westfall, K. B., et al. 2013, A&A, 557, A131

    2013

  44. [52]

    R., Carignan, C., Beaulieu, S

    Meurer, G. R., Carignan, C., Beaulieu, S. F., & Freeman, K. C. 1996, AJ, 111, 1551

    1996

  45. [53]

    R., Hanish, D

    Meurer, G. R., Hanish, D. J., Ferguson, H. C., et al. 2006, ApJS, 165, 307

    2006

  46. [54]

    F., Eke, V

    Navarro, J. F., Eke, V. R., & Frenk, C. S. 1996, MNRAS, 283, L72

    1996

  47. [55]

    Niemeyer, J. C. 2020, Progress in Particle and Nuclear Physics, 113, 103787

    2020

  48. [56]

    Oh, S.-H., de Blok, W. J. G., Brinks, E., Walter, F., & Kennicutt, Jr., R. C. 2011, AJ, 141, 193

    2011

  49. [57]

    Oh, S.-H., de Blok, W. J. G., Walter, F., Brinks, E., & Kennicutt, Robert C., J. 2008, AJ, 136, 2761

    2008

  50. [58]

    A., Brinks, E., et al

    Oh, S.-H., Hunter, D. A., Brinks, E., et al. 2015, AJ, 149, 180

    2015

  51. [59]

    A., Navarro, J

    Oman, K. A., Navarro, J. F., Fattahi, A., et al. 2015, MNRAS, 452, 3650

    2015

  52. [60]

    Pence, W. D. & Blackman, C. P. 1984, MNRAS, 210, 547

    1984

  53. [61]

    & Governato, F

    Pontzen, A. & Governato, F. 2012, MNRAS, 421, 3464

    2012

  54. [62]

    Read, J. I. & Gilmore, G. 2005, MNRAS, 356, 107

    2005

  55. [63]

    I., Walker, M

    Read, J. I., Walker, M. G., & Steger, P. 2019, MNRAS, 484, 1401

    2019

  56. [64]

    Rocha, M., Peter, A. H. G., Bullock, J. S., et al. 2013, MNRAS, 430, 81

    2013

  57. [65]

    2023, A&A, 677, A44

    Romano, M., Nanni, A., Donevski, D., et al. 2023, A&A, 677, A44

    2023

  58. [66]

    Romeo, A. B. & Falstad, N. 2013, MNRAS, 433, 1389

    2013

  59. [67]

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

    Ryan-Weber, E., Koribalski, B. S., Staveley-Smith, L., et al. 2002, AJ, 124, 1954

    2002

  60. [68]

    V., Wetzel, A., & Fattahi, A

    Sales, L. V., Wetzel, A., & Fattahi, A. 2022, Nature Astronomy, 6, 897 Sánchez-Salcedo, F. J. 2006, MNRAS, 365, 555 Santos-Santos,I.M.E.,Navarro,J.F.,Robertson,A.,etal.2020,MNRAS,495, 58

    2022

  61. [69]

    J., Pingel, N

    Sardone, A., Pisano, D. J., Pingel, N. M., et al. 2021, ApJ, 910, 69

    2021

  62. [70]

    K., Walter, F., et al

    Schruba, A., Leroy, A. K., Walter, F., et al. 2012, AJ, 143, 138

    2012

  63. [71]

    J., et al

    Sorgho, A., Carignan, C., Pisano, D. J., et al. 2019, MNRAS, 482, 1248

    2019

  64. [72]

    Spergel, D. N. & Steinhardt, P. J. 2000, Phys. Rev. Lett., 84, 3760

    2000

  65. [73]

    A., Madore, B

    Swaters, R. A., Madore, B. F., van den Bosch, F. C., & Balcells, M. 2003, ApJ, 583, 732

    2003

  66. [74]

    A., Sancisi, R., van Albada, T

    Swaters, R. A., Sancisi, R., van Albada, T. S., & van der Hulst, J. M. 2009, Astronomy & Astrophysics, 493, 871

    2009

  67. [75]

    V., Dutton, A

    Tollet, E., Macciò, A. V., Dutton, A. A., et al. 2016, MNRAS, 456, 3542

    2016

  68. [76]

    1964, ApJ, 139, 1217

    Toomre, A. 1964, ApJ, 139, 1217

    1964

  69. [77]

    & Yu, H.-B

    Tulin, S. & Yu, H.-B. 2018, Phys. Rep., 730, 1

    2018

  70. [78]

    B., Courtois, H

    Tully, R. B., Courtois, H. M., & Sorce, J. G. 2016, AJ, 152, 50

    2016

  71. [79]

    Veronese, S., de Blok, W. J. G., Healy, J., et al. 2025, A&A, 693, A97

    2025

  72. [80]

    Walter, F., Brinks, E., de Blok, W. J. G., et al. 2008, AJ, 136, 2563

    2008

  73. [81]

    B., Hau, G

    Whiting, A. B., Hau, G. K. T., & Irwin, M. 2002, ApJS, 141, 123

    2002

  74. [82]

    B., Hau, G

    Whiting, A. B., Hau, G. K. T., Irwin, M., & Verdugo, M. 2007, AJ, 133, 715

    2007

  75. [83]

    L., Eisenhardt, P

    Wright, E. L., Eisenhardt, P. R. M., Mainzer, A. K., et al. 2010, AJ, 140, 1868 1 InstitutodeAstrofísicadeAndalucía(CSIC),GlorietadelaAstronomías/n,18008Granada, Spain 2 Wits Centre for Astrophysics, School of Physics, University of the Witwatersrand, 1 Jan Smuts Avenue, 2000,...

    2010

Pith tools

Reviewed August 7, 2026 · model on record in the stance chip above.