Pith. sign in

REVIEW 3 major objections 4 minor 1 cited by

The AGN fuelling/feedback cycle in nearby radio galaxies II. Kinematics of the molecular gas

T0 review · 3 major / 4 minor · reviewed 2026-08-14 · deepseek-v4-flash

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

Pith's one-line read This paper claims that molecular gas discs in low-excitation radio galaxies rotate but are not settled, and in at least one object the gas is inflowing and can feed the black hole.

desk verdict A careful, honest kinematics paper that adds six LERGs to a small sample; the SMBH mass and inflow claims are plausible but rest on residuals from a simple model in marginally resolved discs. read the letter →

arxiv 1908.09229 v1 pith:GQX6JT3H submitted 2019-08-24 astro-ph.GA

Ilaria Ruffa (INAF-IRA/University of Bologna) , Timothy A. Davis (Cardiff University) , Isabella Prandoni (INAF-IRA) , Robert A. Laing (SKAO) , Rosita Paladino (INAF-IRA) , Paola Parma (INAF-IRA) , Hans de Ruiter (INAF-IRA) , Viviana Casasola (INAF-IRA)
show 2 more authors
Martin Bureau (Oxford University/Yonsei University) Joshua Warren (Oxford University)
This is my paper · ORCID
classification astro-ph.GA
keywords moleculargaskinematicslow-excitationradiogalaxiesAGNfuellingCO(2-1)ALMAobservationssupermassiveblackholemassgalacticwarpsnon-circularmotionsToomrestability
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 tries to establish what the cold molecular gas around nearby low-excitation radio galaxies is doing: is it feeding the central black hole, being pushed around by jets, or sitting in stable orbits? Using ALMA observations of six galaxies detected in carbon monoxide, the authors model each CO disc in three dimensions. They find that the bulk of the gas rotates in an ordered way, but every disc shows low-level kinematic distortions. They argue these distortions mean the gas is not fully settled into the host galaxy's gravitational potential, and in at least one case, NGC 3100, the radial motions are likely inflows that contribute to AGN fuelling.

What carries the argument

The central tool is the KinMS forward-modelling code coupled to an MCMC fitter: it generates mock ALMA data cubes from a parametric gas distribution and velocity law, so observed cubes can be compared with models that include beam smearing, disc thickness, and velocity dispersion. The default velocity law is an arctangent rotation curve $v(R)=(2v_{\rm flat}/\pi)\arctan(R/r_{\rm turn})$. Deviations between data and model are then interpreted through added ingredients: position-angle and inclination warps, a central surface-brightness hole or ring, and, for NGC 3100, a two-armed logarithmic spiral brightness pattern. A harmonic decomposition of the velocity field (kinemetry) quantifies non-circular motions, and for NGC 3557 a multi-Gaussian expansion of the stellar light supplies the stellar mass model against which the black hole mass is fitted.

What would settle it

Observe the same six galaxies at sub-100 pc resolution, or with a higher-density tracer such as CO(3-2), and ask whether the residuals between the data and the best simple rotating-disc model persist; if they vanish or shrink to the noise level, the conclusion that the gas is unsettled loses its support, and for NGC 3557 a map resolving the sphere of influence on both sides of the nucleus would show whether the velocity upturn is a Keplerian rise or a one-sided non-circular flow.

Watch

Extended reading notes

Core claim

The paper's central claim is that sub-kiloparsec molecular gas discs in low-excitation radio galaxies are common, mostly rotation-dominated, but not relaxed: deviations from a simple axisymmetric rotating disc appear in all six objects studied. For most the deviations are small and the discs are only marginally resolved, so the authors are cautious. The special cases carry the argument: NGC 3557 shows a central velocity upturn fitted as a Keplerian rise, giving a black hole mass of $(7.10\pm0.02)\times10^{8}\,M_\odot$; NGC 3100 requires a warped, two-armed spiral disc whose residual velocity field has non-negligible radial motions, most plausibly inflows toward the nucleus. On this basis the paper concludes that cold gas can contribute to fuelling the AGN in these objects, and that such disturbed discs distinguish radio-loud from radio-quiet early-type galaxies.

Load-bearing premise

The cold-gas discs in most of the sample are only marginally resolved, and the central claim that the residual velocity features are genuine warps, non-circular motions, or inflows assumes those features are not artifacts of fitting a simple thin axisymmetric rotating-disc model to barely resolved data, including effects like beam smearing.

Editorial extensions

If this is right

  • If the paper is right, low-level kinematic disturbances in CO discs should be regarded as the normal state of low-excitation radio galaxies, not as rare anomalies.
  • The NGC 3557 black hole mass joins the set of directly measured supermassive black hole masses in early-type galaxies and can be used to test the $M_{\rm SMBH}$--$\sigma_*$ relation at the high-mass end.
  • The inferred inflow in NGC 3100 supports externally accreted or chaotically cooling gas as a viable fuelling path for kinetic-mode AGN, not only hot halo accretion.
  • Disturbed, unrelaxed discs should be more common among radio-loud than radio-quiet early-type galaxies, a difference that can be tested with larger samples.
  • Most of the modelled discs are gravitationally stable (Toomre $Q>1$), so fuelling likely proceeds through slow, non-collapse channels rather than rapid fragmentation.

Reading between the lines

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

  • A testable extension the paper leaves implicit: compare CO residual maps with jet orientation and stellar kinematics in a larger LERG sample to see whether the asymmetries systematically align with jet axes, which would favour jet-gas interactions over unrelated warps.
  • If the central velocity rise in NGC 3557 were instead produced by a bar or a nuclear non-circular flow, the derived black hole mass would be an upper limit; a resolved map of the sphere of influence on both sides of the nucleus would settle this.
  • The relaxation timescales estimated for NGC 612 and NGC 3100 imply that externally acquired gas can survive several $10^8$ yr before settling, so young unsettled discs should be most common in galaxies with recent interaction signatures.
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 / 4 minor

Summary. This paper presents the 3D kinematic modelling of the six molecular gas discs detected in CO(2-1) with ALMA in a volume- and flux-limited sample of eleven nearby low-excitation radio galaxies (Paper I). Using the KinMS forward-modelling code and an MCMC sampler, the authors fit a thin axisymmetric disc model with a Gaussian surface brightness distribution and an arctangent rotation curve (Eq. 1), allowing for warps and an inner hole where needed. They find that the bulk of the gas is in ordered rotation in all six systems, but with low-level residuals that they attribute to warps or non-circular motions. Two sources receive special treatment: NGC 3557, where a central velocity rise is modelled as a Keplerian upturn yielding M_SMBH = (7.10 +/- 0.02) x 10^8 M_sun, and NGC 3100, where a two-armed spiral plus PA and inclination warps are fitted and kinemetric harmonic analysis indicates non-circular motions, interpreted as possible inflows feeding the AGN. The paper also discusses the external origin of the cold gas and estimates Toomre Q parameters.

Significance. If the conclusions hold, the paper provides one of the few resolved molecular-gas kinematic studies of LERGs, supporting a picture in which cold gas is common in their centres and often not fully relaxed, with potential consequences for AGN fuelling. The NGC 3557 SMBH measurement adds a CO-based datum to the M_sigma relation, and the NGC 3100 analysis is a genuinely interesting case study. The authors are careful in several places, especially in acknowledging that the discriminating power of the data is limited; the use of public modelling tools and the explicit description of priors and fitting procedures is also a strength. However, the central "unsettled gas" claim and the two headline results rely on interpretations of residuals and of a one-sided kinematic feature that are not fully protected against model degeneracy and unquantified systematics.

major comments (3)
  1. [§5.1; Figures 1–4, Table 1] The conclusion that the molecular gas discs are "not fully settled" in the stellar potential rests on residual moment-one maps obtained with a deliberately simple axisymmetric arctangent model (Eq. 1). For the marginally resolved targets (IC 1531, IC 4296, NGC 7075, and NGC 3557; beams 0.4–0.9 arcsec in Table 1), residual amplitudes of ~30–60 km/s are comparable to what beam smearing, a mild radial PA or inclination gradient, or a non-arctangent rotation curve would plausibly generate. Section 5.1 itself states that "differentiating between the two through disc modelling alone is not always straightforward." The paper should either demonstrate with a synthetic-data or model-comparison test that these residuals cannot be absorbed by a slightly more flexible simple model, or restrict the unsettled-disc claim to the well-resolved cases (NGC 612, NGC 3100) and present the other cases as detections of ordered rotation with unclassified asymmetries.
  2. [§4.5; Table 4; Section 6] The quoted SMBH mass of NGC 3557, log(M_SMBH) = 8.85 +/- 0.02, is not a supported measure of the total uncertainty. The text notes that the Keplerian rise is seen only on the positive-velocity side, that central residuals of ~40 km/s remain, and that "we cannot definitively claim that a massive dark object is the cause." The error quoted in Table 4 is the statistical MCMC uncertainty only; the dependence on the dust-masked MGE model, the stellar M/L, the inclination, and the choice of the stellar potential is not quantified. Because the abstract and Section 6 present this value as a headline result and compare it with the M_sigma relation, the paper should supply a systematic error budget or explicitly downgrade the measurement to an indicative estimate with a conservatively enlarged uncertainty.
  3. [§4.6.1; §5.2] The claim that radial motions in NGC 3100 are likely inflows is one interpretive step beyond what the current modelling measures. The Kinemetry analysis establishes a non-zero k5/k1 ratio, i.e., the presence of non-circular motions, but the sign and radial nature of the velocity component are inferred from the residual pattern and from the dust-absorption near-side determination rather than from a fit that includes an explicit radial velocity term. A model with a free radial velocity component, or a clear statement that the inflow direction is not directly constrained, is needed before the fuelling conclusion can be given the prominence it receives in the abstract and in Section 5.2.
minor comments (4)
  1. [Table 1; Section 2.1] The note in Table 1 says the NGC 3557 observations are "combined Cycle 3 and Cycle 6 data," while Section 2.1 states the archival data were taken during Cycle 4; please correct the inconsistency.
  2. [§5.4; Table 6] The text says that "in two cases (IC 1531 and NGC 612) Q is below unity," but Table 6 lists IC 1531 only as a lower limit (>0.2); a lower limit does not establish Q < 1. Likewise, IC 4296 is listed as an upper limit (<29), so the statement that "Q is well above unity" should be qualified.
  3. [Figures 5 and 7] The captions describe panels as "mock" mean velocity maps; this should read "model" for consistency with Figures 1–4.
  4. [Throughout] There are several typographical errors (e.g., "thiss hypothesis" in Section 5.1 and missing periods after "e.g" in Sections 5.1 and 5.2); a careful proofread would improve the presentation.

Circularity Check

0 steps flagged · score 0.0 of 10

No circular derivation: all kinematic parameters and the SMBH mass are fitted to the CO data, with external benchmarks for the M-sigma comparison, so no claim reduces to its own input.

full rationale

The paper's central claims are produced by forward modelling the ALMA CO data cubes rather than by assuming the conclusions. The simple axisymmetric arctangent model (Eq. 1) is a deliberately minimal null hypothesis; the fitted parameters (PA, inclination, vflat, rturn, sigma_gas) are determined by an MCMC fit to the data, and the residual maps are then interpreted as distortions or non-circular motions. This is a data-fitting procedure, not a self-definitional one. The NGC 3557 SMBH mass is likewise an MCMC fit to the central velocity upturn of the CO velocity curve, with the stellar contribution removed using an MGE model of the HST light distribution; the quoted agreement with the M_SMBH-sigma* relation uses the independent stellar velocity dispersion from Brough et al. (2007) and the Tremaine et al. (2002) relation, so the comparison is not constructed from the fitted mass. The only self-citation to Paper I supplies detections, priors, and some measured quantities, but none of these inputs is equivalent to the kinematic conclusions or to the black-hole mass; those conclusions would stand or fall on the analysed CO data and external comparisons. The paper's repeated caveats that most discs are only marginally resolved and that warps versus non-circular motions are hard to distinguish are honest limitations on interpretation, not circularity. No equation, fitted parameter, or citation chain reduces a claimed prediction to an input, so no circular step can be identified.

Assumptions & free parameters 8 free parameters · 7 assumptions · 0 invented entities

The central analysis is a forward model that fits many parameters to the data; the list above separates kinematic and geometric quantities fitted in the MCMC runs from structural assumptions used to interpret them. No new physical entities are introduced.

free parameters (8)
  • v_flat (asymptotic circular velocity, per source) = 272-453 km/s depending on source (Tables 2 and 5)
    Fitted as free parameters in the arctangent rotation curve for each CO disc; the rotation amplitude underpins the ordered-rotation and Toomre Q claims.
  • r_turn (rotation curve turnover radius, per source) = 0.01-2.68 arcsec
    Fitted free parameter; controls the shape of the modelled rotation curve.
  • Kinematic position angle and inclination (per source) = PA 183-356 deg; inclination 20-81 deg; NGC 3100 has PA 190-250 deg and inclination 20-80 deg
    Fitted for each disc; for NGC 3100 and IC 4296, warps are fitted as radial ranges.
  • Gas velocity dispersion sigma_gas = 3.4-64 km/s
    Fitted as spatially constant; used in Toomre Q estimates and controls whether residuals are significant.
  • Kinematic centre velocity offset = -95 to +91.5 km/s
    Fitted to allow zero-point differences; affects all velocity-field interpretations.
  • Surface brightness profile parameters (Gaussian width/flux; R_disc, R_hole, spiral a,b,theta for NGC 3100) = E.g. NGC 612 central hole 0.3 arcsec; NGC 3100 R_disc=3.36 arcsec, R_hole=0.9 arcsec
    Fitted gas distribution parameters; define the model against which kinematic residuals are measured.
  • Stellar mass-to-light ratio (NGC 3557) = 5.4 +/- 0.1
    Fitted to CO kinematics as part of the SMBH mass model; its systematic uncertainty is not quantified.
  • SMBH mass M_SMBH (NGC 3557) = 7.10e8 M_sun (log = 8.85 +/- 0.02)
    Fitted point mass at the galaxy centre; the main quantitative result of Section 4.5.
assumptions (7)
  • domain assumption The CO discs are thin and axisymmetric.
    Section 3.1 states 'The CO disc is assumed to be thin and the model axisymmetric.' If a disc is significantly thicker or lopsided, the inferred kinematics are biased.
  • domain assumption The rotation curve follows an arctangent form.
    Equation (1) in Section 3.1. If the true rotation curve deviates from this shape, v_flat and r_turn are biased.
  • domain assumption Constant stellar mass-to-light ratio in the MGE mass model of NGC 3557.
    Section 4.5 uses a single M/L from the MGE fit. Radial M/L variations, dust extinction, or dark matter within the sphere of influence would change the inferred SMBH mass.
  • domain assumption Residuals larger than the channel width trace real non-circular motions rather than artifacts.
    Sections 4.1-4.6 interpret residuals as warps, inflows, or outflows. In marginally resolved discs this is not guaranteed.
  • domain assumption Dust absorption on the eastern side of the NGC 3100 ring marks the near side.
    Section 5.2 uses the B-I colour map to set the near side; this converts observed radial motions into inflows. If the near side is wrong, the flows could be outflows.
  • domain assumption The Kinemetry k5/k1 ratio measures non-circular motions.
    Section 4.6.1 interprets nonzero k5/k1 as radial streaming, relying on the thin-disc interpretation of the flattening parameter q.
  • domain assumption Standard flat Lambda-CDM cosmology with H0 = 70 km/s/Mpc, Omega_L = 0.7, Omega_M = 0.3.
    Adopted at the end of Section 1 for distance and scale conversions.

how reviews work

0 comments
Cite this review

Pith. "Pith review of The AGN fuelling/feedback cycle in nearby radio galaxies II. Kinematics of the molecular gas." pith.science (2026). https://pith.science/paper/GQX6JT3H

@misc{pith2026190809229,
  author       = {Pith},
  title        = {Pith review of: The AGN fuelling/feedback cycle in nearby radio galaxies II. Kinematics of the molecular gas},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/GQX6JT3H}},
  note         = {Machine review of arXiv:1908.09229}
}
abstract

This is the second paper of a series exploring the multi-component (stars, warm and cold gas and radio jets) properties of a sample of eleven nearby low excitation radio galaxies (LERGs), with the aim of better understanding the AGN fuelling/feedback cycle in these objects. Here we present a study of the molecular gas kinematics of six sample galaxies detected in $^{12}$CO(2-1) with ALMA. In all cases, our modelling suggests that the bulk of the gas in the observed (sub-)kpc CO discs is in ordered rotation. Nevertheless, low-level distortions are ubiquitous, indicating that the molecular gas is not fully relaxed into the host galaxy potential. The majority of the discs, however, are only marginally resolved, preventing us from drawing strong conclusions. NGC 3557 and NGC 3100 are special cases. The features observed in the CO velocity curve of NGC 3557 allow us to estimate a super-massive black hole (SMBH) mass of $(7.10\pm0.02)\times10^{8}$ M$_{\odot}$, in agreement with expectations from the M$_{\rm SMBH}- \sigma_{*}$ relation. The rotation pattern of NGC 3100 shows distortions that appear to be consistent with the presence of both a position angle and inclination warp. Non-negligible radial motions are also found in the plane of the CO disc, likely consistent with streaming motions associated with the spiral pattern found in the inner regions of the disc. The dominant radial motions are likely to be inflows, supporting a scenario in which the cold gas is contributing to the fuelling of the AGN.

Figures

Figures reproduced from arXiv: 1908.09229 by the authors.

Figure 1
Figure 1. IC 1531 observed, model and residual (data-model) mean velocity maps (panels a, b and c, respectively). The black dashed line in panel a indicates the direction of the radio jet axis. The synthesised beam is shown in the bottom-left corner of each panel. The wedges to the right show the colour scale. East is to the left and North to the top. Velocities are measured in the source frame and the zero-point corresponds … view at source ↗
Figure 2
Figure 2. NGC 612 observed, model, residual mean velocity maps and PVD as in [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. IC 4296 observed, model, residual mean velocity maps and PVD as in [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figures from the paper (5 more)
Figure 4
Figure 4. Figure 4: NGC 7075 observed, model, residual mean velocity maps and PVD as in [PITH_FULL_IMAGE:figures/full_fig_p008_4.png]
Figure 5
Figure 5. Figure 5: NGC 3557 observed, mock, residual mean velocity maps and PVD as in [PITH_FULL_IMAGE:figures/full_fig_p010_5.png]
Figure 6
Figure 6. Figure 6: MGE model of NGC 3557 (red contours), overlaid on a HST optical (F555W) image (black contours). Panel a shows the whole galaxy, while panel b shows a zoom in on the central region. The region masked due to dust is visible to the east of the galaxy nucleus in both panel…
Figure 7
Figure 7. Figure 7: NGC 3100 observed and simulated integrated intensity maps (moment 0, panels a and b), observed, mock, and residual mean velocity maps (panels c, d, and e) and PVD (panel f ) as in [PITH_FULL_IMAGE:figures/full_fig_p012_7.png]
Figure 8
Figure 8. Figure 8: Coefficients derived from the harmonic decomposition of the line-of-sight velocity field of NGC 3100 (see Section 4.6.1 for details). From the top to the bottom: kinematic PA; axial ratio of the best-fitting ellipses (directly related to the inclination in the approxim…

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. Jet--ISM Interactions in Gaseous Disks: Simulating Kinetic Feedback in the Radio Galaxy 3C 326 N

    astro-ph.GA 2026-07 conditional novelty 6.0 of 10

    Jet–ISM coupling in multi-scale cloudy disks produces asymmetric lobes and kinematics that match the JWST-observed bubble in 3C 326 N for a 10^45 erg s^{-1} jet.

Reference graph

Works this paper leans on

122 extracted references · 14 canonical work pages · cited by 1 Pith paper

  1. [1]

    Alatalo K., et al., 2011, @doi [ ] 10.1088/0004-637X/735/2/88 , http://adsabs.harvard.edu/abs/2011ApJ...735...88A 735, 88

    doi:10.1088/0004-637x/735/2/88 2011

  2. [2]

    Alatalo K., et al., 2013, @doi [ ] 10.1093/mnras/sts299 , http://adsabs.harvard.edu/abs/2013MNRAS.432.1796A 432, 1796

    doi:10.1093/mnras/sts299 2013

  3. [3]

    W., Dunn R

    Allen S. W., Dunn R. J. H., Fabian A. C., Taylor G. B., Reynolds C. S., 2006, @doi [ ] 10.1111/j.1365-2966.2006.10778.x , http://adsabs.harvard.edu/abs/2006MNRAS.372...21A 372, 21

    arXiv 2006

  4. [4]

    W., Vega O., Panuzzo P., 2010, @doi [ ] 10.1051/0004-6361/200913774 , http://adsabs.harvard.edu/abs/2010A

    Annibali F., Bressan A., Rampazzo R., Zeilinger W. W., Vega O., Panuzzo P., 2010, @doi [ ] 10.1051/0004-6361/200913774 , http://adsabs.harvard.edu/abs/2010A

    doi:10.1051/0004-6361/200913774 2010

  5. [5]

    D., Capetti A., 2008, @doi [ ] 10.1051/0004-6361:200809810 , http://adsabs.harvard.edu/abs/2008A

    Balmaverde B., Baldi R. D., Capetti A., 2008, @doi [ ] 10.1051/0004-6361:200809810 , http://adsabs.harvard.edu/abs/2008A

    doi:10.1051/0004-6361:200809810 2008

  6. [7]

    N., Kaiser C

    Best P. N., Kaiser C. R., Heckman T. M., Kauffmann G., 2006, @doi [ ] 10.1111/j.1745-3933.2006.00159.x , http://adsabs.harvard.edu/abs/2006MNRAS.368L..67B 368, L67

    arXiv 2006

  7. [8]

    D., Barth A

    Boizelle B. D., Barth A. J., Darling J., Baker A. J., Buote D. A., Ho L. C., Walsh J. L., 2017, @doi [ ] 10.3847/1538-4357/aa8266 , http://adsabs.harvard.edu/abs/2017ApJ...845..170B 845, 170

    work page doi:10.3847/1538-4357/aa8266 2017

  8. [9]

    Bondi H., 1952, @doi [ ] 10.1093/mnras/112.2.195 , http://adsabs.harvard.edu/abs/1952MNRAS.112..195B 112, 195

    doi:10.1093/mnras/112.2.195 1952

Show all 122 references
  1. [10]

    Bosma A., 1981a, @doi [ ] 10.1086/113062 , http://adsabs.harvard.edu/abs/1981AJ.....86.1791B 86, 1791

    doi

  2. [11]

    Bosma A., 1981b, @doi [ ] 10.1086/113063 , http://adsabs.harvard.edu/abs/1981AJ.....86.1825B 86, 1825

    doi

  3. [13]

    K., van der Marel R

    Cappellari M., Verolme E. K., van der Marel R. P., Verdoes Kleijn G. A., Illingworth G. D., Franx M., Carollo C. M., de Zeeuw P. T., 2002, @doi [ ] 10.1086/342653 , http://adsabs.harvard.edu/abs/2002ApJ...578..787C 578, 787

    2002 doi

  4. [14]

    K., L \'e on S., Baker A

    Casasola V., Combes F., Garc \' a-Burillo S., Hunt L. K., L \'e on S., Baker A. J., 2008, @doi [ ] 10.1051/0004-6361:200809545 , http://adsabs.harvard.edu/abs/2008A

    2008 doi

  5. [15]

    K., Combes F., Garc \' a-Burillo S., Neri R., 2011, @doi [ ] 10.1051/0004-6361/201015680 , https://ui.adsabs.harvard.edu/abs/2011A

    Casasola V., Hunt L. K., Combes F., Garc \' a-Burillo S., Neri R., 2011, @doi [ ] 10.1051/0004-6361/201015680 , https://ui.adsabs.harvard.edu/abs/2011A

    2011 doi

  6. [16]

    Ching J. H. Y., et al., 2017, @doi [ ] 10.1093/mnras/stx1173 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.469.4584C 469, 4584

    2017 doi

  7. [17]

    G., Corsini E

    Combes F., 2001, in Funes J. G., Corsini E. M., eds, Astronomical Society of the Pacific Conference Series Vol. 230, Galaxy Disks and Disk Galaxies. pp 213--220 ( @eprint astro-ph/0008341 )

    2001 arXiv

  8. [18]

    Combes F., 2006, arXiv Astrophysics e-prints, http://adsabs.harvard.edu/abs/2006astro.ph..8616C

    2006

  9. [19]

    Combes F., 2017, @doi [Frontiers in Astronomy and Space Sciences] 10.3389/fspas.2017.00010 , http://adsabs.harvard.edu/abs/2017FrASS...4...10C 4, 10

    2017

  10. [20]

    Combes F., et al., 2013, @doi [ ] 10.1051/0004-6361/201322288 , http://adsabs.harvard.edu/abs/2013A

    2013 doi

  11. [21]

    M., 2011, preprint, http://adsabs.harvard.edu/abs/2011arXiv1101.1499D ( @eprint arXiv 1101.1499 )

    Dame T. M., 2011, preprint, http://adsabs.harvard.edu/abs/2011arXiv1101.1499D ( @eprint arXiv 1101.1499 )

    2011 arXiv

  12. [22]

    P., et al., 2014, @doi [ ] 10.1088/0004-637X/792/2/94 , http://adsabs.harvard.edu/abs/2014ApJ...792...94D 792, 94

    David L. P., et al., 2014, @doi [ ] 10.1088/0004-637X/792/2/94 , http://adsabs.harvard.edu/abs/2014ApJ...792...94D 792, 94

    2014 doi

  13. [23]

    A., Bureau M., 2016, @doi [ ] 10.1093/mnras/stv2998 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.457..272D 457, 272

    Davis T. A., Bureau M., 2016, @doi [ ] 10.1093/mnras/stv2998 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.457..272D 457, 272

    2016 doi

  14. [25]

    A., et al., 2013, @doi [ ] 10.1093/mnras/sts353 , http://adsabs.harvard.edu/abs/2013MNRAS.429..534D 429, 534

    Davis T. A., et al., 2013, @doi [ ] 10.1093/mnras/sts353 , http://adsabs.harvard.edu/abs/2013MNRAS.429..534D 429, 534

    2013 doi

  15. [26]

    A., et al., 2015, @doi [ ] 10.1093/mnras/stv1973 , http://adsabs.harvard.edu/abs/2015MNRAS.454..657D 454, 657

    Davis T. A., et al., 2015, @doi [ ] 10.1093/mnras/stv1973 , http://adsabs.harvard.edu/abs/2015MNRAS.454..657D 454, 657

    2015 doi

  16. [27]

    A., Bureau M., Onishi K., Cappellari M., Iguchi S., Sarzi M., 2017, @doi [ ] 10.1093/mnras/stw3217 , http://adsabs.harvard.edu/abs/2017MNRAS.468.4675D 468, 4675

    Davis T. A., Bureau M., Onishi K., Cappellari M., Iguchi S., Sarzi M., 2017, @doi [ ] 10.1093/mnras/stw3217 , http://adsabs.harvard.edu/abs/2017MNRAS.468.4675D 468, 4675

    2017 doi

  17. [28]

    A., et al., 2018, @doi [ ] 10.1093/mnras/stx2600 , http://adsabs.harvard.edu/abs/2018MNRAS.473.3818D 473, 3818

    Davis T. A., et al., 2018, @doi [ ] 10.1093/mnras/stx2600 , http://adsabs.harvard.edu/abs/2018MNRAS.473.3818D 473, 3818

    2018 doi

  18. [29]

    A., Greene J

    Davis T. A., Greene J. E., Ma C.-P., Blakeslee J. P., Dawson J. M., Pandya V., Veale M., Zabel N., 2019, @doi [ ] 10.1093/mnras/stz871 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.486.1404D 486, 1404

    2019 doi

  19. [30]

    H., Winkler H., 2016, @doi [ ] 10.1051/0004-6361/201528047 , http://adsabs.harvard.edu/abs/2016A

    Duah Asabere B., Horellou C., Jarrett T. H., Winkler H., 2016, @doi [ ] 10.1051/0004-6361/201528047 , http://adsabs.harvard.edu/abs/2016A

    2016 doi

  20. [31]

    Duc P.-A., et al., 2015, @doi [ ] 10.1093/mnras/stu2019 , http://adsabs.harvard.edu/abs/2015MNRAS.446..120D 446, 120

    2015 doi

  21. [32]

    Emonts B. H. C., Morganti R., Oosterloo T. A., Holt J., Tadhunter C. N., van der Hulst J. M., Ojha R., Sadler E. M., 2008, @doi [ ] 10.1111/j.1365-2966.2008.13142.x , http://adsabs.harvard.edu/abs/2008MNRAS.387..197E 387, 197

    2008

  22. [33]

    Emsellem E., Monnet G., Bacon R., 1994, , http://adsabs.harvard.edu/abs/1994A

    1994

  23. [34]

    Emsellem E., Greusard D., Combes F., Friedli D., Leon S., P \'e contal E., Wozniak H., 2001, @doi [ ] 10.1051/0004-6361:20000523 , http://adsabs.harvard.edu/abs/2001A

    2001 doi

  24. [35]

    M., et al., 2007, @doi [ ] 10.1086/519294 , http://adsabs.harvard.edu/abs/2007ApJ...665..265F 665, 265

    Faber S. M., et al., 2007, @doi [ ] 10.1086/519294 , http://adsabs.harvard.edu/abs/2007ApJ...665..265F 665, 265

    2007 doi

  25. [36]

    C., 2012, @doi [ ] 10.1146/annurev-astro-081811-125521 , http://adsabs.harvard.edu/abs/2012ARA

    Fabian A. C., 2012, @doi [ ] 10.1146/annurev-astro-081811-125521 , http://adsabs.harvard.edu/abs/2012ARA

    2012 doi

  26. [37]

    A., Winge C., Axon D

    Fathi K., Storchi-Bergmann T., Riffel R. A., Winge C., Axon D. J., Robinson A., Capetti A., Marconi A., 2006, @doi [ ] 10.1086/503832 , http://adsabs.harvard.edu/abs/2006ApJ...641L..25F 641, L25

    2006 doi

  27. [38]

    E., Zurita A., Rela \ n o M., Knapen J

    Fathi K., Beckman J. E., Zurita A., Rela \ n o M., Knapen J. H., Daigle O., Hernandez O., Carignan C., 2007, @doi [ ] 10.1051/0004-6361:20066990 , http://adsabs.harvard.edu/abs/2007A

    2007 doi

  28. [39]

    Fathi K., Axon D. J., Storchi-Bergmann T., Kharb P., Robinson A., Marconi A., Maciejewski W., Capetti A., 2011, @doi [ ] 10.1088/0004-637X/736/2/77 , http://adsabs.harvard.edu/abs/2011ApJ...736...77F 736, 77

    2011 doi

  29. [40]

    Fathi K., et al., 2013, @doi [ ] 10.1088/2041-8205/770/2/L27 , http://adsabs.harvard.edu/abs/2013ApJ...770L..27F 770, L27

    2013 doi

  30. [41]

    Garc \' a-Burillo S., et al., 2014, @doi [ ] 10.1051/0004-6361/201423843 , http://adsabs.harvard.edu/abs/2014A

    2014 doi

  31. [42]

    P., 2013, @doi [ ] 10.1093/mnras/stt692 , http://adsabs.harvard.edu/abs/2013MNRAS.432.3401G 432, 3401

    Gaspari M., Ruszkowski M., Oh S. P., 2013, @doi [ ] 10.1093/mnras/stt692 , http://adsabs.harvard.edu/abs/2013MNRAS.432.3401G 432, 3401

    2013 doi

  32. [43]

    Gaspari M., Brighenti F., Temi P., 2015, @doi [ ] 10.1051/0004-6361/201526151 , http://adsabs.harvard.edu/abs/2015A

    2015 doi

  33. [44]

    Gaspari M., Temi P., Brighenti F., 2017, @doi [ ] 10.1093/mnras/stw3108 , http://adsabs.harvard.edu/abs/2017MNRAS.466..677G 466, 677

    2017 doi

  34. [45]

    A., et al., 2019, arXiv e-prints, https://ui.adsabs.harvard.edu/abs/2019arXiv190500018G p

    Gordon Y. A., et al., 2019, arXiv e-prints, https://ui.adsabs.harvard.edu/abs/2019arXiv190500018G p. arXiv:1905.00018

    2019 arXiv

  35. [46]

    E., Janish R., Ma C.-P., McConnell N

    Greene J. E., Janish R., Ma C.-P., McConnell N. J., Blakeslee J. P., Thomas J., Murphy J. D., 2015, @doi [ ] 10.1088/0004-637X/807/1/11 , http://adsabs.harvard.edu/abs/2015ApJ...807...11G 807, 11

    2015 doi

  36. [47]

    Grossova R., et al., 2019, arXiv e-prints, https://ui.adsabs.harvard.edu/abs/2019arXiv190303198G

    2019

  37. [48]

    Hardcastle M., 2018, @doi [Nature Astronomy] 10.1038/s41550-018-0424-1 , http://adsabs.harvard.edu/abs/2018NatAs...2..273H 2, 273

    2018 doi

  38. [50]

    M., 2017, @doi [Nature Astronomy] 10.1038/s41550-017-0165 , http://adsabs.harvard.edu/abs/2017NatAs...1E.165H 1, 0165

    Harrison C. M., 2017, @doi [Nature Astronomy] 10.1038/s41550-017-0165 , http://adsabs.harvard.edu/abs/2017NatAs...1E.165H 1, 0165

    2017 doi

  39. [51]

    M., Best P

    Heckman T. M., Best P. N., 2014, @doi [ ] 10.1146/annurev-astro-081913-035722 , http://adsabs.harvard.edu/abs/2014ARA

    2014 doi

  40. [52]

    Heller C., Shlosman I., Englmaier P., 2001, @doi [ ] 10.1086/320983 , http://adsabs.harvard.edu/abs/2001ApJ...553..661H 553, 661

    2001 doi

  41. [53]

    C., Filippenko A

    Ho L. C., Filippenko A. V., Sargent W. L. W., 1997, @doi [ ] 10.1086/304642 , https://ui.adsabs.harvard.edu/abs/1997ApJ...487..579H 487, 579

    1997 doi

  42. [54]

    F., Quataert E., 2010, @doi [ ] 10.1111/j.1365-2966.2010.17064.x , http://adsabs.harvard.edu/abs/2010MNRAS.407.1529H 407, 1529

    Hopkins P. F., Quataert E., 2010, @doi [ ] 10.1111/j.1365-2966.2010.17064.x , http://adsabs.harvard.edu/abs/2010MNRAS.407.1529H 407, 1529

    2010

  43. [55]

    F., Quataert E., 2011, @doi [ ] 10.1111/j.1365-2966.2011.18542.x , http://adsabs.harvard.edu/abs/2011MNRAS.415.1027H 415, 1027

    Hopkins P. F., Quataert E., 2011, @doi [ ] 10.1111/j.1365-2966.2011.18542.x , http://adsabs.harvard.edu/abs/2011MNRAS.415.1027H 415, 1027

    2011

  44. [56]

    H., Hardcastle M

    Ineson J., Croston J. H., Hardcastle M. J., Kraft R. P., Evans D. A., Jarvis M., 2015, @doi [ ] 10.1093/mnras/stv1807 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.453.2682I 453, 2682

    2015 doi

  45. [57]

    Jungwiert B., Combes F., Palou s J., 2001, @doi [ ] 10.1051/0004-6361:20010966 , https://ui.adsabs.harvard.edu/abs/2001A

    2001 doi

  46. [59]

    King A., Nixon C., 2015, @doi [ ] 10.1093/mnrasl/slv098 , http://adsabs.harvard.edu/abs/2015MNRAS.453L..46K 453, L46

    2015 doi

  47. [60]

    R., Pringle J

    King A. R., Pringle J. E., 2007, @doi [ ] 10.1111/j.1745-3933.2007.00296.x , http://adsabs.harvard.edu/abs/2007MNRAS.377L..25K 377, L25

    2007

  48. [62]

    Lagos C. d. P., Davis T. A., Lacey C. G., Zwaan M. A., Baugh C. M., Gonzalez-Perez V., Padilla N. D., 2014, @doi [ ] 10.1093/mnras/stu1209 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.443.1002L 443, 1002

    2014 doi

  49. [63]

    Lagos C. d. P., Padilla N. D., Davis T. A., Lacey C. G., Baugh C. M., Gonzalez-Perez V., Zwaan M. A., Contreras S., 2015, @doi [ ] 10.1093/mnras/stu2763 , http://adsabs.harvard.edu/abs/2015MNRAS.448.1271L 448, 1271

    2015 doi

  50. [64]

    A., Bridle A

    Laing R. A., Bridle A. H., 2002, @doi [ ] 10.1046/j.1365-8711.2002.05873.x , http://adsabs.harvard.edu/abs/2002MNRAS.336.1161L 336, 1161

    2002

  51. [65]

    Lake G., Norman C., 1983, @doi [ ] 10.1086/161097 , https://ui.adsabs.harvard.edu/abs/1983ApJ...270...51L 270, 51

    1983 doi

  52. [66]

    R., et al., 2005, @doi [ ] 10.1086/429565 , http://adsabs.harvard.edu/abs/2005AJ....129.2138L 129, 2138

    Lauer T. R., et al., 2005, @doi [ ] 10.1086/429565 , http://adsabs.harvard.edu/abs/2005AJ....129.2138L 129, 2138

    2005 doi

  53. [67]

    S., 2005, @doi [ ] 10.1086/430205 , https://ui.adsabs.harvard.edu/abs/2005ApJ...626..823L 626, 823

    Li Y., Mac Low M.-M., Klessen R. S., 2005, @doi [ ] 10.1086/430205 , https://ui.adsabs.harvard.edu/abs/2005ApJ...626..823L 626, 823

    2005 doi

  54. [68]

    Lim J., Ao Y., Dinh-V-Trung 2008, @doi [ ] 10.1086/523664 , https://ui.adsabs.harvard.edu/abs/2008ApJ...672..252L 672, 252

    2008 doi

  55. [69]

    M., Morganti R., Oosterloo T

    Maccagni F. M., Morganti R., Oosterloo T. A., Oonk J. B. R., Emonts B. H. C., 2018, @doi [ ] 10.1051/0004-6361/201732269 , http://adsabs.harvard.edu/abs/2018A

    2018 doi

  56. [71]

    Maciejewski W., 2004b, @doi [ ] 10.1111/j.1365-2966.2004.08254.x , http://adsabs.harvard.edu/abs/2004MNRAS.354..892M 354, 892

    2004

  57. [72]

    S., 2000, @doi [ ] 10.1046/j.1365-8711.2000.03270.x , http://adsabs.harvard.edu/abs/2000MNRAS.313..745M 313, 745

    Maciejewski W., Sparke L. S., 2000, @doi [ ] 10.1046/j.1365-8711.2000.03270.x , http://adsabs.harvard.edu/abs/2000MNRAS.313..745M 313, 745

    2000

  58. [73]

    A., Gorjian V., Tam R., 1998, @doi [ ] 10.1086/313110 , https://ui.adsabs.harvard.edu/abs/1998ApJS..117...25M 117, 25

    Malkan M. A., Gorjian V., Tam R., 1998, @doi [ ] 10.1086/313110 , https://ui.adsabs.harvard.edu/abs/1998ApJS..117...25M 117, 25

    1998 doi

  59. [74]

    W., 1999, @doi [ ] 10.1086/301140 , http://adsabs.harvard.edu/abs/1999AJ....118.2646M 118, 2646

    Martini P., Pogge R. W., 1999, @doi [ ] 10.1086/301140 , http://adsabs.harvard.edu/abs/1999AJ....118.2646M 118, 2646

    1999 doi

  60. [75]

    W., Mulchaey J

    Martini P., Regan M. W., Mulchaey J. S., Pogge R. W., 2003, @doi [ ] 10.1086/374685 , https://ui.adsabs.harvard.edu/abs/2003ApJ...589..774M 589, 774

    2003 doi

  61. [76]

    G., Brighenti F., 2003, @doi [ ] 10.1146/annurev.astro.41.090401.094542 , https://ui.adsabs.harvard.edu/abs/2003ARA

    Mathews W. G., Brighenti F., 2003, @doi [ ] 10.1146/annurev.astro.41.090401.094542 , https://ui.adsabs.harvard.edu/abs/2003ARA

    2003

  62. [77]

    J., Ma C.-P., 2013, @doi [ ] 10.1088/0004-637X/764/2/184 , http://adsabs.harvard.edu/abs/2013ApJ...764..184M 764, 184

    McConnell N. J., Ma C.-P., 2013, @doi [ ] 10.1088/0004-637X/764/2/184 , http://adsabs.harvard.edu/abs/2013ApJ...764..184M 764, 184

    2013 doi

  63. [78]

    P., Waters B., Schiebel D., Young W., Golap K., 2007, in Shaw R

    McMullin J. P., Waters B., Schiebel D., Young W., Golap K., 2007, in Shaw R. A., Hill F., Bell D. J., eds, Astronomical Society of the Pacific Conference Series Vol. 376, Astronomical Data Analysis Software and Systems XVI. p. 127

    2007

  64. [79]

    M \'e ndez-Abreu J., Aguerri J. A. L., Corsini E. M., Simonneau E., 2008, @doi [ ] 10.1051/0004-6361:20078089e , https://ui.adsabs.harvard.edu/abs/2008A

    2008 doi

  65. [80]

    Merloni A., Heinz S., 2007, @doi [ ] 10.1111/j.1365-2966.2007.12253.x , http://adsabs.harvard.edu/abs/2007MNRAS.381..589M 381, 589

    2007

  66. [81]

    arXiv:1905.06017

    Nagai H., et al., 2019, arXiv e-prints, https://ui.adsabs.harvard.edu/abs/2019arXiv190506017N p. arXiv:1905.06017

    2019 arXiv

  67. [82]

    Narayan R., Yi I., 1995, @doi [ ] 10.1086/176343 , http://adsabs.harvard.edu/abs/1995ApJ...452..710N 452, 710

    1995 doi

  68. [83]

    R., 2012, @doi [ ] 10.1088/0004-637X/753/1/15 , http://adsabs.harvard.edu/abs/2012ApJ...753...15N 753, 15

    Nayakshin S., Power C., King A. R., 2012, @doi [ ] 10.1088/0004-637X/753/1/15 , http://adsabs.harvard.edu/abs/2012ApJ...753...15N 753, 15

    2012 doi

  69. [84]

    Negri A., Posacki S., Pellegrini S., Ciotti L., 2014, @doi [ ] 10.1093/mnras/stu1834 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.445.1351N 445, 1351

    2014 doi

  70. [85]

    Nyland K., et al., 2016, @doi [ ] 10.1093/mnras/stw391 , http://adsabs.harvard.edu/abs/2016MNRAS.458.2221N 458, 2221

    2016 doi

  71. [86]

    Oca \ n a Flaquer B., Leon S., Combes F., Lim J., 2010, @doi [ ] 10.1051/0004-6361/200913392 , http://adsabs.harvard.edu/abs/2010A

    2010 doi

  72. [87]

    Okuda T., Kohno K., Iguchi S., Nakanishi K., 2005, @doi [ ] 10.1086/427140 , http://adsabs.harvard.edu/abs/2005ApJ...620..673O 620, 673

    2005 doi

  73. [88]

    A., Bureau M., Cappellari M., Sarzi M., Blitz L., 2017, @doi [ ] 10.1093/mnras/stx631 , http://adsabs.harvard.edu/abs/2017MNRAS.468.4663O 468, 4663

    Onishi K., Iguchi S., Davis T. A., Bureau M., Cappellari M., Sarzi M., Blitz L., 2017, @doi [ ] 10.1093/mnras/stx631 , http://adsabs.harvard.edu/abs/2017MNRAS.468.4663O 468, 4663

    2017 doi

  74. [89]

    B., Morganti R., Combes F., Dasyra K., Salom \'e P., Vlahakis N., Tadhunter C., 2017, @doi [ ] 10.1051/0004-6361/201731781 , http://adsabs.harvard.edu/abs/2017A

    Oosterloo T., Raymond Oonk J. B., Morganti R., Combes F., Dasyra K., Salom \'e P., Vlahakis N., Tadhunter C., 2017, @doi [ ] 10.1051/0004-6361/201731781 , http://adsabs.harvard.edu/abs/2017A

    2017 doi

  75. [90]

    A., Parma P., de Ruiter H

    Prandoni I., Laing R. A., Parma P., de Ruiter H. R., Montenegro-Montes F. M., Wilson T. L., 2007, in Baker A. J., Glenn J., Harris A. I., Mangum J. G., Yun M. S., eds, Astronomical Society of the Pacific Conference Series Vol. 375, From Z-Machines to ALMA: (Sub)Millimeter Spec...

    2007 arXiv

  76. [91]

    A., de Ruiter H

    Prandoni I., Laing R. A., de Ruiter H. R., Parma P., 2010, @doi [ ] 10.1051/0004-6361/201015456 , http://adsabs.harvard.edu/abs/2010A

    2010 doi

  77. [92]

    H., Combes F., Carignan C., Deg N., 2015, @doi [ ] 10.1093/mnras/stv2147 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.454.3743R 454, 3743

    Randriamampandry T. H., Combes F., Carignan C., Deg N., 2015, @doi [ ] 10.1093/mnras/stv2147 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.454.3743R 454, 3743

    2015 doi

  78. [93]

    B., Mogotsi K

    Romeo A. B., Mogotsi K. M., 2017, @doi [ ] 10.1093/mnras/stx844 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.469..286R 469, 286

    2017 doi

  79. [94]

    Ruffa I., et al., 2019, @doi [ ] 10.1093/mnras/stz255 , http://adsabs.harvard.edu/abs/2019MNRAS.484.4239R 484, 4239

    2019 doi

  80. [95]

    P., 1999, in Taylor G

    Rupen M. P., 1999, in Taylor G. B., Carilli C. L., Perley R. A., eds, Astronomical Society of the Pacific Conference Series Vol. 180, Synthesis Imaging in Radio Astronomy II. p. 229

    1999

  81. [96]

    R., McNamara B

    Russell H. R., McNamara B. R., Edge A. C., Hogan M. T., Main R. A., Vantyghem A. N., 2013, @doi [ ] 10.1093/mnras/stt490 , http://adsabs.harvard.edu/abs/2013MNRAS.432..530R 432, 530

    2013 doi

  82. [97]

    R., et al., 2016, @doi [ ] 10.1093/mnras/stw409 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.458.3134R 458, 3134

    Russell H. R., et al., 2016, @doi [ ] 10.1093/mnras/stw409 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.458.3134R 458, 3134

    2016 doi

  83. [98]

    N., Argudo-Fern \'a ndez M., 2013, @doi [ ] 10.1093/mnras/sts675 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.430..638S 430, 638

    Sabater J., Best P. N., Argudo-Fern \'a ndez M., 2013, @doi [ ] 10.1093/mnras/sts675 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.430..638S 430, 638

    2013 doi

  84. [99]

    Salim S., et al., 2007, @doi [ ] 10.1086/519218 , http://adsabs.harvard.edu/abs/2007ApJS..173..267S 173, 267

    2007 doi

  85. [100]

    Sarzi M., et al., 2006, @doi [ ] 10.1111/j.1365-2966.2005.09839.x , https://ui.adsabs.harvard.edu/abs/2006MNRAS.366.1151S 366, 1151

    2006

  86. [101]

    I., Sunyaev R

    Shakura N. I., Sunyaev R. A., 1973, , http://adsabs.harvard.edu/abs/1973A

    1973

  87. [102]

    H., Beckman J

    Shlosman I., 2001, in Knapen J. H., Beckman J. E., Shlosman I., Mahoney T. J., eds, Astronomical Society of the Pacific Conference Series Vol. 249, The Central Kiloparsec of Starbursts and AGN: The La Palma Connection. p. 55

    2001

  88. [103]

    783, The Evolution of Starbursts

    Shlosman I., 2005, in H \"u ttmeister S., Manthey E., Bomans D., Weis K., eds, American Institute of Physics Conference Series Vol. 783, The Evolution of Starbursts. pp 223--240 ( @eprint astro-ph/0412163 ), @doi 10.1063/1.2034990

    2005 arXiv

  89. [104]

    D., Storchi-Bergmann T., de F \'a tima Saraiva M., Martini P., 2007, @doi [ ] 10.1086/510064 , http://adsabs.harvard.edu/abs/2007ApJ...655..718S 655, 718

    Sim \ o es Lopes R. D., Storchi-Bergmann T., de F \'a tima Saraiva M., Martini P., 2007, @doi [ ] 10.1086/510064 , http://adsabs.harvard.edu/abs/2007ApJ...655..718S 655, 718

    2007 doi

  90. [105]

    Smith M. W. L., et al., 2012, @doi [ ] 10.1088/0004-637X/748/2/123 , https://ui.adsabs.harvard.edu/abs/2012ApJ...748..123S 748, 123

    2012 doi

  91. [106]

    D., et al., 2019, @doi [ ] 10.1093/mnras/stz625 , http://adsabs.harvard.edu/abs/2019MNRAS.tmp..613S

    Smith M. D., et al., 2019, @doi [ ] 10.1093/mnras/stz625 , http://adsabs.harvard.edu/abs/2019MNRAS.tmp..613S

    2019 doi

  92. [107]

    M., Sobral D., Smail I., Geach J

    Swinbank A. M., Sobral D., Smail I., Geach J. E., Best P. N., McCarthy I. G., Crain R. A., Theuns T., 2012, @doi [ ] 10.1111/j.1365-2966.2012.21774.x , http://adsabs.harvard.edu/abs/2012MNRAS.426..935S 426, 935

    2012

  93. [108]

    G., David L., 2018, @doi [ ] 10.3847/1538-4357/aab9b0 , http://adsabs.harvard.edu/abs/2018ApJ...858...17T 858, 17

    Temi P., Amblard A., Gitti M., Brighenti F., Gaspari M., Mathews W. G., David L., 2018, @doi [ ] 10.3847/1538-4357/aab9b0 , http://adsabs.harvard.edu/abs/2018ApJ...858...17T 858, 17

    2018 doi

  94. [109]

    Thomas D., Maraston C., Bender R., Mendes de Oliveira C., 2005, @doi [ ] 10.1086/426932 , http://adsabs.harvard.edu/abs/2005ApJ...621..673T 621, 673

    2005 doi

  95. [110]

    E., Simonson G

    Tohline J. E., Simonson G. F., Caldwell N., 1982, @doi [ ] 10.1086/159537 , https://ui.adsabs.harvard.edu/abs/1982ApJ...252...92T 252, 92

    1982 doi

  96. [111]

    Toomre A., 1964, @doi [ ] 10.1086/147861 , https://ui.adsabs.harvard.edu/abs/1964ApJ...139.1217T 139, 1217

    1964 doi

  97. [112]

    Tremaine S., et al., 2002, @doi [ ] 10.1086/341002 , https://ui.adsabs.harvard.edu/abs/2002ApJ...574..740T 574, 740

    2002 doi

  98. [113]

    R., et al., 2016, @doi [ ] 10.1038/nature17969 , http://adsabs.harvard.edu/abs/2016Natur.534..218T 534, 218

    Tremblay G. R., et al., 2016, @doi [ ] 10.1038/nature17969 , http://adsabs.harvard.edu/abs/2016Natur.534..218T 534, 218

    2016 doi

  99. [114]

    R., et al., 2018, @doi [ ] 10.3847/1538-4357/aad6dd , https://ui.adsabs.harvard.edu/abs/2018ApJ...865...13T 865, 13

    Tremblay G. R., et al., 2018, @doi [ ] 10.3847/1538-4357/aad6dd , https://ui.adsabs.harvard.edu/abs/2018ApJ...865...13T 865, 13

    2018 doi

  100. [115]

    Valentini M., Brighenti F., 2015, @doi [ ] 10.1093/mnras/stv090 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.448.1979V 448, 1979

    2015 doi

  101. [116]

    Veilleux S., Cecil G., Bland-Hawthorn J., 2005, @doi [ ] 10.1146/annurev.astro.43.072103.150610 , http://adsabs.harvard.edu/abs/2005ARA

    2005 arXiv

  102. [117]

    Vila-Vilaro B., Espada D., Cortes P., Leon S., Pompei E., Cepa J., 2019, @doi [ ] 10.3847/1538-4357/aaef7f , http://adsabs.harvard.edu/abs/2019ApJ...870...39V 870, 39

    2019 doi

  103. [118]

    Wada K., Habe A., 1992, @doi [ ] 10.1093/mnras/258.1.82 , https://ui.adsabs.harvard.edu/abs/1992MNRAS.258...82W 258, 82

    1992 doi

  104. [119]

    A., 2002, @doi [ ] 10.1086/342151 , http://adsabs.harvard.edu/abs/2002ApJ...577..197W 577, 197

    Wada K., Meurer G., Norman C. A., 2002, @doi [ ] 10.1086/342151 , http://adsabs.harvard.edu/abs/2002ApJ...577..197W 577, 197

    2002 doi

  105. [120]

    P., Spaans M., 2009, @doi [ ] 10.1088/0004-637X/702/1/63 , http://adsabs.harvard.edu/abs/2009ApJ...702...63W 702, 63

    Wada K., Papadopoulos P. P., Spaans M., 2009, @doi [ ] 10.1088/0004-637X/702/1/63 , http://adsabs.harvard.edu/abs/2009ApJ...702...63W 702, 63

    2009 doi

  106. [121]

    Y., Bicknell G

    Wagner A. Y., Bicknell G. V., Umemura M., 2012, @doi [ ] 10.1088/0004-637X/757/2/136 , http://adsabs.harvard.edu/abs/2012ApJ...757..136W 757, 136

    2012 doi

  107. [122]

    Werner N., et al., 2014, @doi [ ] 10.1093/mnras/stu006 , http://adsabs.harvard.edu/abs/2014MNRAS.439.2291W 439, 2291

    2014 doi

  108. [123]

    M., et al., 2014, @doi [ ] 10.1093/mnras/stt2474 , http://adsabs.harvard.edu/abs/2014MNRAS.444.3408Y 444, 3408

    Young L. M., et al., 2014, @doi [ ] 10.1093/mnras/stt2474 , http://adsabs.harvard.edu/abs/2014MNRAS.444.3408Y 444, 3408

    2014 doi

  109. [124]

    Yuan C., Yen D. C. C., 2004, in Johnstone D., Adams F. C., Lin D. N. C., Neufeeld D. A., Ostriker E. C., eds, Astronomical Society of the Pacific Conference Series Vol. 323, Star Formation in the Interstellar Medium: In Honor of David Hollenbach. p. 67

    2004

  110. [125]

    van de Ven G., Fathi K., 2010, @doi [ ] 10.1088/0004-637X/723/1/767 , https://ui.adsabs.harvard.edu/abs/2010ApJ...723..767V 723, 767

    2010 doi

  111. [126]

    A., Kere s D., Quataert E., Faucher-Gigu \`e re C.-A., Hopkins P

    van de Voort F., Davis T. A., Kere s D., Quataert E., Faucher-Gigu \`e re C.-A., Hopkins P. F., 2015, @doi [ ] 10.1093/mnras/stv1217 , http://adsabs.harvard.edu/abs/2015MNRAS.451.3269V 451, 3269

    2015 doi

  112. [127]

    van de Voort F., et al., 2018, @doi [ ] 10.1093/mnras/sty228 , http://adsabs.harvard.edu/abs/2018MNRAS.476..122V 476, 122

    2018 doi

  113. [128]

    C., Shostak G

    van der Kruit P. C., Shostak G. S., 1982, , http://adsabs.harvard.edu/abs/1982A

    1982

  114. [129]

    write newline

    " write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.stat...

Pith tools

Reviewed August 14, 2026 · model on record in the stance chip above.