Pith. sign in

REVIEW 3 major objections 4 minor 152 references

Ionized gas in NGC 4258: Exploring the AGN -- Star formation connection

T0 review · 3 major / 4 minor · reviewed 2026-08-06 · deepseek-v4-flash

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

Pith's one-line read The anomalous spiral arms of NGC 4258 are jet-driven features that shock the interstellar medium out to 5–6 kpc, both quenching and triggering star formation.

desk verdict Beautiful new full-galaxy IFS maps of NGC 4258, but the jet-driven anomalous-arm interpretation outruns the kinematics, which the authors themselves admit co-rotate. read the letter →

arxiv 2507.16153 v1 pith:WGWEAKYW submitted 2025-07-22 astro-ph.GA

D. Fernández-Arenas , L. Rousseau-Nepton , C. Robert , L. Drissen , R. P. Martin , P. Amram , B. Epinat , Duarte Puertas
show 4 more authors
R. Garner III G. Savard S. Vicens-Mouret É. Massé
This is my paper
classification astro-ph.GA
keywords NGC4258low-luminosityAGNfeedbackjet-ISMinteractionintegralfieldspectroscopySITELLEBPTdiagramanomalousspiralarmsstarformation
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 new integral-field spectroscopy from SITELLE, this paper maps the ionized gas of NGC 4258 across nearly its entire disk and argues that the galaxy's 'anomalous spiral arms' are not ordinary density-wave arms but are carved by a low-power jet from the active nucleus. The jet shocks the interstellar medium out to 5–6 kpc, producing broad, double-peaked emission lines and velocity dispersions up to 200–250 km/s, while simultaneously suppressing star formation in some regions and compressing gas to trigger it in others. If correct, this demonstrates that even a low-luminosity AGN can mechanically shape its host galaxy on kiloparsec scales, providing a nearby benchmark for understanding AGN feedback and its influence on star formation.

What carries the argument

The central machinery is the SITELLE integral-field spectrograph's wide-field data combined with spatially resolved BPT diagrams and velocity dispersion maps. BPT diagrams (NII and SII) separate AGN ionization, star-forming regions, and composite objects; the 'mixing-sequence' decomposition assigns each spaxel a star-forming fraction (f_SF) to correct H-alpha for AGN contamination. Kinematic line-profile fitting, using single and double Gaussian models selected by the Bayesian information criterion, traces broad and asymmetric components that reveal jet-ISM interactions.

What would settle it

High-spatial-resolution IFU observations (e.g., JWST/NIRSpec at ~0.1″) of the anomalous spiral arms: if the jet-driven picture is correct, the broad double-peaked lines should resolve into a narrow star-forming component plus a broad shock component whose centroid velocity deviates from the disk rotation curve by a systematic radial component; conversely, if the broad lines split into many narrow H II-region lines or follow pure rotation, the jet-driven interpretation would be falsified.

Watch

Extended reading notes

Core claim

The central claim is that in NGC 4258 the anomalous spiral arms are jet-driven features: shocked gas and sparse star formation, distinct from the normal spiral density-wave arms. Spatially resolved Baldwin-Phillips-Terlevich diagrams, velocity dispersion maps, covering fractions, and line-profile fits show that the jet's path is traced by high-velocity-dispersion gas (up to 200–250 km/s) with AGN-like ionization, whereas the classical spiral arms host star-forming regions with low dispersions (30–50 km/s). The jet influences the ISM out to 5–6 kpc, as seen in the anomalous arc where shocks quench star formation, and in other areas where jet-induced compression may stimulate it. The authors also derive a galaxy-wide star formation rate of about 3 M_sun/yr, decreasing to 0.3 M_sun/yr within the central 3.4 $kpc^{2}$, and confirm that the polarized radio emission along the jet arises from non-thermal, AGN-related processes, not from star-forming regions.

Load-bearing premise

The kinematic interpretation of the anomalous spiral arms as jet-driven rests on attributing the broad, double-peaked H-alpha profiles and high velocity dispersions to jet-ISM interaction instead of to projection of the galaxy's rotation or to unresolved star-forming regions along the line of sight; the paper itself notes that the jet-like arm rotates consistently with the other arm and appeals to a radial component that is not directly observed.

Editorial extensions

If this is right

  • Low-luminosity AGN jets can mechanically affect the host galaxy's ISM out to 5–6 kpc, not just the nuclear region.
  • The anomalous spiral arms are a record of jet activity, implying that jets can create spiral-like structures distinct from density waves.
  • Shock quenching and shock-triggered star formation can coexist in different parts of the same galaxy, so AGN feedback is simultaneously negative and positive.
  • The derived galaxy-wide SFR of about 3 M_sun/yr and central SFR of 0.3 M_sun/yr provide a quantitative benchmark for LLAGN feedback in a nearby spiral galaxy.
  • The spatial match between BPT-classified AGN ionization and polarized radio emission supports a jet origin for the non-thermal radio lobes.

Reading between the lines

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

  • The kinematic degeneracy noted in §4.2.7 (the jet-like arm rotates consistently with the other arm) suggests the jet-driven interpretation would be strengthened if the unseen radial component could be independently measured, for example with high-resolution CO or H I kinematics or proper motions; otherwise the anomalous arms might be partly shaped by bar-driven shocks.
  • The small (<100 pc) Seyfert-ionized clumps in the anomalous arm may be sites where the jet is compressing dense clouds; JWST observations of Pa-alpha or Br-alpha could confirm whether these are genuinely young star-forming regions induced by the jet.
  • The f_SF mixing-sequence method applied here could be extended to a sample of other low-luminosity AGNs with weak jets to search for similar kiloparsec-scale mechanical feedback, turning this single-galaxy case into a statistical probe.
  • The asymmetry in ionization-cone opening angles (about 50° north-west versus 90° south-east) could indicate a precessing jet or a projection effect; a time-dependent jet-precession model might explain the trailing curvature of the anomalous arm.
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. The paper presents new SITELLE integral-field spectroscopy of the nearby LLAGN NGC 4258, covering the galaxy out to large radii. The authors map emission-line fluxes, Balmer decrements, BPT diagnostics, velocity fields, and velocity dispersions. They interpret the "anomalous spiral arms" as jet-driven features consisting of shocked gas and sparse star formation, argue that the jet mechanically affects the ISM out to 5-6 kpc, and report evidence for both shock quenching and jet-triggered star formation. They also derive a galaxy-wide star formation rate of about 3 M_sun/yr and a central 3.4 kpc^2 SFR of 0.3 M_sun/yr using a mixing-sequence analysis. The data products and maps are presented in detail, and the reduction includes stellar continuum subtraction and a cross-check of the Balmer decrement against SDSS.

Significance. If the jet-driven interpretation of the anomalous spiral arms is correct, the paper would provide a striking example of low-luminosity AGN mechanical feedback operating on kiloparsec scales, with direct consequences for star formation. The observational dataset is valuable: SITELLE's large field of view and public data cubes give the community a comprehensive view of a nearby Seyfert galaxy, and several of the maps (e.g., BPT classifications, velocity dispersion, line-ratio maps) will be useful for comparison with other galaxies and with the forthcoming JWST data. The authors also explicitly connect their results to the SIGNALS survey methodology. The main weakness is that the central kinematic claim rests on an unobserved radial component, and the paper itself acknowledges that the anomalous arm's rotation is consistent with disk rotation; this needs to be addressed before the jet-driven interpretation can be considered established.

major comments (3)
  1. [§4.2.7 and §6] The paper's central claim that the anomalous spiral arms are jet-driven is not yet supported by the kinematic data. In §4.2.7, the authors state that the rotation of the jet-like arm is fairly consistent with that of the other arm and that a radial component "may not be observed due to the orientation along the major axis." This means the observed line-of-sight velocity field does not distinguish the anomalous arm from disk rotation. The broad and double-peaked line profiles, and the high velocity dispersions, could also be produced by projection of the rotating disk, superposed star-forming regions, or multiple kinematic components within the beam. To make the jet-driven claim load-bearing, the authors need to present a rotation-subtracted velocity field or an explicit kinematic model that includes radial/vertical flows, and to show that the residuals are localized to the anomalous arms. Without that, the conclusion in §6 that "the anomalous spiral arms appear to be jet-driven features" is an inference from morphology and BPT classification alone, which alternative mechanisms (e.g., bar shocks; Cox & Downes 1996) can also satisfy.
  2. [§4.2.4] There is an internal inconsistency in the SFR estimate. The authors report a galaxy-wide SFR of 3 M_sun/yr and a central (3.4 kpc^2) SFR of 0.3 M_sun/yr. However, when they adopt a uniform A_V=0.7, they obtain central values of 0.1 and 0.07 M_sun/yr, which are the values that "closely align" with Ogle et al. (2014) (0.084 and 0.069 M_sun/yr). The headline central value of 0.3 is thus a factor ~3-4 higher than the SED-based estimate, and the claim in §6 that "These values are consistent with previous SED-fitting studies" is misleading unless the average-extinction scenario is adopted. The authors should state which extinction treatment is preferred and quantify the systematic uncertainty in the SFR.
  3. [§4.2.4 and §6] The inference of shock quenching in the lower "anomalous arc" is not quantitatively supported. The authors argue that shocks quench star formation because they do not observe significant extinction in this region. However, a deficit of star formation could also result from low gas density, from incompleteness in Hβ detection at the S/N>3 threshold, or from an intrinsically lower SFR unrelated to the jet. To support the quenching claim, the paper should compare the anomalous arc to a control region with similar extinction and gas conditions, or place a quantitative upper limit on the extinction and on the star formation deficit.
minor comments (4)
  1. [Figures 5-16] Most maps are shown without explicit uncertainty maps. Since the BPT classifications and velocity-dispersion values are used for quantitative inferences, the authors should provide at least representative error maps or a discussion of spatially varying uncertainties beyond the S/N masks.
  2. [Throughout] There are several typos, e.g., "Halfha" in §4.2.4 (likely H-alpha), "ANG" in §4.2.5 (likely AGN), and "SRF" in §4.2.4 (likely SFR). A careful proofread is needed.
  3. [§5] The discussion of cosmic-ray pressure and bar-induced shear as additional feedback mechanisms is speculative and not tied to the SITELLE data. These paragraphs should be clearly labeled as qualitative discussion or condensed, as they presently resemble additional conclusions not supported by the observations.
  4. [§4.2.5, Figure 14] The azimuthal covering-fraction analysis states the jet position with a green dotted line, but the exact azimuthal bin width and the uncertainties on the peak positions are not given; please add these details to the figure caption or text.

Circularity Check

0 steps flagged · score 2.0 of 10

No circular derivation: jet-ISM interpretation rests on independent kinematic and ionization maps; only a minor unpublished self-citation and the acknowledged co-rotation caveat are flagged.

full rationale

The derivation chain is observational and not circular. The central claim that the anomalous spiral arms are jet-driven rests on (i) spatial coincidence of high [Sii]/Halpha and broad or double-peaked Halpha profiles with the radio/X-ray jet morphology, (ii) BPT classification showing AGN-like ionization along the arms, and (iii) velocity dispersions up to 200-250 km/s in those regions. None of these is fitted to the conclusion. The mixing-sequence SFR (Eq. 1) fits the fraction f_SF to the observed [NII]/Halpha and [OIII]/Hbeta ratios and then applies the Kennicutt (1998) Halpha calibration; f_SF is not fitted to any SFR target, and the SFR does not feed back into the jet-ISM interpretation. The comparison showing that 85% of the galaxy-wide SFR originates from BPT-selected star-forming spaxels is a consistency statement implied by the decomposition, not a prediction, and it is not load-bearing for the paper's main claim. The kinematic support is weakened by the paper's own admission in Section 4.2.7 that the rotation of the jet-like arm is fairly consistent with that of the other arm, which is surprising if the arm is a jet, and the authors invoke an unobserved radial component; this is a testability and robustness limitation, not a circular step, and they defer deeper modelling to a future paper. The only self-citations are methodological: Rousseau-Nepton et al. (2018) for the reference-spectrum subtraction, Masse et al. (in preparation) for the pPXF stellar-continuum implementation, and SIGNALS survey papers for the observing program. These are not load-bearing for the jet-driven-arm conclusion, but the unpublished Masse et al. reference is a missing-support flag: the BPT maps depend on Hbeta, and the exact continuum-correction code is not independently available. That is a reproducibility concern, not a circularity. No equation is shown to be equivalent to its inputs by construction, and no fitted parameter is renamed as a prediction.

Assumptions & free parameters 3 free parameters · 6 assumptions · 0 invented entities

The central scientific claims rest on standard spectroscopic assumptions plus the mixing-sequence decomposition. The new contributions are observational; no new physical entities are introduced. The most consequential fitted inputs are the per-spaxel star-forming fraction and the chosen basis vectors, which directly set the SFR values.

free parameters (3)
  • Star-forming fraction f_SF per spaxel = not a single number; MCMC posterior per spaxel over [0,1]
    Central to the SFR estimate: the extinction-corrected H-alpha luminosity is multiplied by f_SF (Eqs. 1-2), and the fraction is fit to each spaxel's BPT line ratios rather than measured independently.
  • Mixing sequence basis vectors (pure SF and pure AGN endpoints) = selected from extremes of the observed BPT distribution; no numerical values given
    Equation 1 requires endpoints representing pure star formation and pure AGN; these are chosen from the data, and the paper notes that different methodologies can introduce errors of up to 15 percent.
  • Upper-limit extinction A_V = 1.52 mag = 1.52 mag
    Assumed by hand to derive an upper limit on the SFR of about 7 solar masses per year, taking all H-alpha with S/N > 3 and excluding the jet region, as reported in Section 4.2.4.
assumptions (6)
  • domain assumption All fitted emission lines share the same line-of-sight velocity and velocity dispersion in each spaxel.
    Used throughout line fitting with ORCS in Section 4; if this is untrue for one or more lines, the kinematic and line ratio maps could be biased.
  • domain assumption Case B recombination with T_e = 10000 K and n_e = 100 cm^-3 gives H-alpha/H_beta = 2.86, used to convert the observed Balmer decrement into extinction.
    Adopted in Section 4.1; observed ratios below the theoretical value are set to zero extinction, which can bias A_V low in noisy spaxels.
  • domain assumption The observed emission line ratios are a linear combination of a pure star-forming component and a pure AGN component, with f_SF + f_AGN = 1.
    Equation 1 in Section 4.2.4; the whole mixing-sequence SFR correction depends on this decomposition being valid for every spaxel.
  • domain assumption The Kennicutt (1998) conversion from extinction-corrected H-alpha luminosity to SFR applies to NGC 4258.
    Equation 2; assumes a standard IMF, no significant leakage of ionizing photons, and that the residual AGN contribution is fully removed by f_SF.
  • domain assumption The Cardelli et al. (1989) extinction curve with R_V = 3.1 describes the dust in NGC 4258.
    Used for A_V from the Balmer decrement in Section 4.1; if the dust properties differ, the extinction corrections and the resulting SFR shift.
  • domain assumption The SITELLE instrumental line profile is a sinc function, and the ORCS fitting model is correct.
    Adopted in line fitting; a mismatch in the profile shape would affect the measured velocity dispersions and line fluxes.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Ionized gas in NGC 4258: Exploring the AGN -- Star formation connection." pith.science (2026). https://pith.science/paper/WGWEAKYW

@misc{pith2026250716153,
  author       = {Pith},
  title        = {Pith review of: Ionized gas in NGC 4258: Exploring the AGN -- Star formation connection},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/WGWEAKYW}},
  note         = {Machine review of arXiv:2507.16153}
}
abstract

NGC 4258 is a prime target for studying feedback in Low-Luminosity Active Galactic Nuclei (LLAGNs) due to its proximity and comprehensive multi-wavelength coverage. Using new Integral Field Spectroscopy (IFS) data from SITELLE at the Canada-France-Hawaii Telescope, we analysed the galaxy's nebular emission lines. Our study focused on spatially resolved line ratios and Baldwin-Phillips-Terlevich diagrams, revealing that the ''anomalous spiral arms'' exhibit intense interactions between the jet and interstellar medium (ISM) extending up to 6 kpc with velocity dispersions peak at 200-250 km/s in these regions, contrasting with star-forming areas showing lower values around of 30-50 km/s. Analysis of covering fractions indicates heightened AGN ionization cones aligned with the radio jet, alongside evidence of shock quenching observed in the lower "anomalous arc". Conversely, jet-induced compression may stimulate star formation in other areas. We derived a galaxy-wide star formation rate of $\sim3 M_{\odot}\mathrm{yr}^{-1}$ decreasing to $0.3 M_{\odot}\mathrm{yr}^{-1}$ within the central $3.4 \mathrm{kpc}^2$. SITELLE's broad field coverage elucidates the galaxy's structural details, confirming that low-power jets significantly influence the host galaxy across parsec and kpc scales. The velocity dispersion map reveals asymmetric or double-peaked emission lines, tracing jet-disk interactions likely responsible for the formation of anomalous arm features. Small-scale ionizing clusters were detected in regions with disrupted gas flows, possibly formed through tidal interactions or shock compression. NGC~4258 thus presents a compelling case for studying LLAGN-driven feedback, illustrating how optical IFS combined with multi-wavelength data clarifies the impact of outflows and shocks on nearby spiral galaxies, providing insights into how these processes shape star formation and ISM conditions.

Figures

Figures reproduced from arXiv: 2507.16153 by the authors.

Figure 1
Figure 1. Mask selection for the sky emission subtraction and correction for the stellar continuum absorption for our observations of NGC 4258 with SITELLE. Black squares labelled from SKY-1 to -12 correspond to areas where the sky background extraction was performed to correct the spectra. Each square averages 10000 spaxels covering each more than 1000 arcsec2 . The continuum areas were selected based on contours derived fro… view at source ↗
Figure 2
Figure 2. Spectra corresponding to the sky emission from the different regions marked by the black squares in [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Example of the spectrum extracted for region R2 (see [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figures from the paper (15 more)
Figure 4
Figure 4. Figure 4: Left panels: The RGB image of NGC4258 is generated using three deep images obtained from the SN3 filter [6470Å-6850Å] (red), SN2 filter [4820Å-5130Å] (green), and SN1 filter [3630Å-3860Å] (blue). We highlight in yellow the H𝛼 emission map and in purple the X-ray emissi…
Figure 5
Figure 5. Figure 5: Top to bottom: Surface brightness H𝛼 map, line-of-sight velocity, and velocity dispersion for NGC 4258 derived from the fitting of the H𝛼 emission line. Spaxels with S/N<3 have been masked. The background image and the contours have been plotted as a reference and come…
Figure 7
Figure 7. Figure 7: Balmer decrement for H𝛽 and H𝛼 emission lines and visual extinction (𝐴𝑉 ) assuming the theoretical ratios for case B recombination 𝐹(H𝛼)/𝐹(H𝛽) = 2.86 and the extinction curve of Cardelli et al. (1989) with Rv=3.1. Horizontal lines show the mean and standard deviation o…
Figure 6
Figure 6. Figure 6: Balmer decrement for H𝛼 and H𝛽 emission lines (Top) and visual extinction (𝐴𝑉 ) (Bottom) assuming the theoretical ratios for case B recom￾bination 𝐹(H𝛼)/𝐹(H𝛽) = 2.86 and the extinction curve of Cardelli et al. (1989) with Rv=3.1. clear region and toward the north spira…
Figure 8
Figure 8. Figure 8: Maps of the diagnostic line ratios in logarithmic scale. The la￾bel inset indicates the line ratios [O iii]𝜆5007/H𝛽, [N ii]𝜆6584/H𝛼 and [S ii]𝜆𝜆6717,31/H𝛼. The contours have been plotted as a reference and come from the SN3 deep image. MNRAS 000, 1–25 (0000) [PITH_FUL…
Figure 9
Figure 9. Figure 9: Left panels: NII- and SII-BPT diagrams for NGC 4258. The Kewley et al. (2006) classifications are shown as the solid lines. The black solid lines separate the star-forming determined by the upper limit of the theoretical pure stellar photoionization models from those e…
Figure 10
Figure 10. Figure 10: Maps showing the centre of the galaxy and the spaxels classified according to their ionization source based on NII- and SII-BPT diagrams. In black, the contours correspond to observations using the VLA at 8.44 GHz, as reported by Krause & Löhr (2004).  [N ii]/H𝛼 [O i…
Figure 11
Figure 11. Figure 11: Top Panel: BPT diagram of NGC 4258 illustrating a mixing sequence between ionization by H ii regions and AGN. Middle Panels left and right, respectively: Distribution of 𝑓𝑆𝐹 across the galaxy, with blue points representing ionization by star-forming regions and red po…
Figure 12
Figure 12. Figure 12: illustrates the variation of the line ratios used in the BPT diagrams relative to the deprojected galactocentric radius and the velocity dispersion. The line ratios [N ii]/H𝛼 and [S ii]/H𝛼 exhibit a smooth decrease in the first 5 kpc, while [O iii]/H𝛽 drops sharply in…
Figure 13
Figure 13. Figure 13: displays the radial variation of [S ii]𝜆6717/[S ii]𝜆6731 ratio and the corresponding 𝑛𝑒 scale in the right axis the colour bar corresponds to the velocity dispersion. For individual spaxels, we found a larger variation with densities ranging between the limits of Sand…
Figure 14
Figure 14. Figure 14: Covering fraction of the pixels classified as AGN+composite (red) and star-forming (blue) according to BPT diagrams (BPT-NII with continuous lines, BPT-SII with dashed lines) as a function of the projected azimuthal angle. The green dotted line represents the peak of …
Figure 15
Figure 15. Figure 15: The top panels display the NII- and SII-BPT diagrams, while the bottom panels present maps showcasing spaxel locations in the centre of the galaxy, classified according to their ionizing source and colour-coded based on the H𝛼 velocity dispersion in km s −1 , the colo…
Figure 16
Figure 16. Figure 16: Zoom-in on the main features previously reported in the literature, as described in the main text and observed with SITELLE from top to bottom: H𝛼-filaments, H𝛼-loop, north and south arc shocks. The colour represents the NII-BPT ionizing source, red (AGN), blue (star-…
Figure 17
Figure 17. Figure 17: shows the L.O.S velocities along the P.A. and the model in green. Outside 10 kpc the galaxy seems to behave like a normal spiral galaxy, while closer to the nucleus is disturbed. In addition to integrated regions, we explore the kinematics and profiles along the jet i…
Figure 18
Figure 18. Figure 18: Both single and double profiles have been observed in H𝛼 emission within the central region of NGC 4258. Individual spectra are extracted from boxes measuring 20 × 20 pixels2 , corresponding to 220 × 220 pc2 . The plotted wavelength range shows the H𝛼 [N ii]𝜆𝜆6548,83 …

Discussion (0). Sign in to comment.

Reference graph

Works this paper leans on

152 extracted references · 37 canonical work pages

  1. [1]

    J., et al., 2021, @doi [ ] 10.3847/1538-4357/ac1e8d , https://ui.adsabs.harvard.edu/abs/2021ApJ...922..156A 922, 156

    Agostino C. J., et al., 2021, @doi [ ] 10.3847/1538-4357/ac1e8d , https://ui.adsabs.harvard.edu/abs/2021ApJ...922..156A 922, 156

    doi:10.3847/1538-4357/ac1e8d 2021

  2. [2]

    E., Sonbas E., Balman S., 2013, @doi [ ] 10.1088/0004-6256/145/3/67 , https://ui.adsabs.harvard.edu/abs/2013AJ....145...67A 145, 67

    Akyuz A., Kayaci S., Avdan H., Ozel M. E., Sonbas E., Balman S., 2013, @doi [ ] 10.1088/0004-6256/145/3/67 , https://ui.adsabs.harvard.edu/abs/2013AJ....145...67A 145, 67

    doi:10.1088/0004-6256/145/3/67 2013

  3. [4]

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

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

  4. [5]

    G., Groves B

    Allen M. G., Groves B. A., Dopita M. A., Sutherland R. S., Kewley L. J., 2008, @doi [ ] 10.1086/589652 , https://ui.adsabs.harvard.edu/abs/2008ApJS..178...20A 178, 20

    doi:10.1086/589652 2008

  5. [6]

    A., 2023, @doi [ ] 10.1093/mnras/stad2673 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.526..217A 526, 217

    Almeida I., Nemmen R., Riffel R. A., 2023, @doi [ ] 10.1093/mnras/stad2673 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.526..217A 526, 217

    doi:10.1093/mnras/stad2673 2023

  6. [7]

    Alonso-Herrero A., et al., 2019, @doi [ ] 10.1051/0004-6361/201935431 , https://ui.adsabs.harvard.edu/abs/2019A&A...628A..65A 628, A65

    doi:10.1051/0004-6361/201935431 2019

  7. [8]

    N., et al., 2018, @doi [ ] 10.3847/1538-4357/aaed2a , https://ui.adsabs.harvard.edu/abs/2018ApJ...869...61A 869, 61

    Appleton P. N., et al., 2018, @doi [ ] 10.3847/1538-4357/aaed2a , https://ui.adsabs.harvard.edu/abs/2018ApJ...869...61A 869, 61

    doi:10.3847/1538-4357/aaed2a 2018

  8. [9]

    L., Greenhill L

    Argon A. L., Greenhill L. J., Reid M. J., Moran J. M., Humphreys E. M. L., 2007, @doi [ ] 10.1086/512718 , https://ui.adsabs.harvard.edu/abs/2007ApJ...659.1040A 659, 1040

    doi:10.1086/512718 2007

Show all 152 references
  1. [10]

    Avdan H., Avdan S., Akyuz A., Balman S., Aksaker N., Akkaya Oralhan I., 2016, @doi [ ] 10.3847/0004-637X/828/2/105 , https://ui.adsabs.harvard.edu/abs/2016ApJ...828..105A 828, 105

    2016 doi

  2. [11]

    Avdan2016 A., Avdan S., Allak S., Aksaker N., Akkaya Oralhan I., Balman S., 2020, @doi [ ] 10.1093/mnras/staa2823 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.499.2138A 499, 2138

    2020 doi

  3. [12]

    Bagchi J., et al., 2025, @doi [ ] 10.1093/mnras/staf229 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.538.1628B 538, 1628

    2025 doi

  4. [13]

    A., Phillips M

    Baldwin J. A., Phillips M. M., Terlevich R., 1981, @doi [ ] 10.1086/130766 , http://adsabs.harvard.edu/abs/1981PASP...93....5B 93, 5

    1981 doi

  5. [14]

    Belfiore F., et al., 2022, @doi [ ] 10.1051/0004-6361/202141859 , https://ui.adsabs.harvard.edu/abs/2022A&A...659A..26B 659, A26

    2022 doi

  6. [15]

    A., et al., 2013, @doi [ ] 10.1088/0004-6256/145/5/138 , https://ui.adsabs.harvard.edu/abs/2013AJ....145..138B 145, 138

    Blanc G. A., et al., 2013, @doi [ ] 10.1088/0004-6256/145/5/138 , https://ui.adsabs.harvard.edu/abs/2013AJ....145..138B 145, 138

    2013 doi

  7. [16]

    Bresolin F., 2011, @doi [ ] 10.1088/0004-637X/729/1/56 , https://ui.adsabs.harvard.edu/abs/2011ApJ...729...56B 729, 56

    2011 doi

  8. [17]

    J., Garnett D

    Bresolin F., Kennicutt Robert C. J., Garnett D. R., 1999, @doi [ ] 10.1086/306576 , https://ui.adsabs.harvard.edu/abs/1999ApJ...510..104B 510, 104

    1999 doi

  9. [19]

    S., Quinn T

    Butsky I. S., Quinn T. R., 2018, @doi [ ] 10.3847/1538-4357/aaeac2 , https://ui.adsabs.harvard.edu/abs/2018ApJ...868..108B 868, 108

    2018 doi

  10. [20]

    Cappellari M., 2017, @doi [ ] 10.1093/mnras/stw3020 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.466..798C 466, 798

    2017 doi

  11. [21]

    A., Clayton G

    Cardelli J. A., Clayton G. C., Mathis J. S., 1989, @doi [ ] 10.1086/167900 , https://ui.adsabs.harvard.edu/abs/1989ApJ...345..245C 345, 245

    1989 doi

  12. [22]

    Cecchi-Pestellini C., Casu S., Barsella B., 2001, @doi [Astronomy & Astrophysics] 10.1051/0004-6361:20010457 , 372, 83

    2001 doi

  13. [23]

    S., Tully R

    Cecil G., Wilson A. S., Tully R. B., 1992, @doi [ ] 10.1086/171288 , https://ui.adsabs.harvard.edu/abs/1992ApJ...390..365C 390, 365

    1992 doi

  14. [24]

    A., Veilleux S., 1995, @doi [ ] 10.1086/176334 , https://ui.adsabs.harvard.edu/abs/1995ApJ...452..613C 452, 613

    Cecil G., Morse J. A., Veilleux S., 1995, @doi [ ] 10.1086/176334 , https://ui.adsabs.harvard.edu/abs/1995ApJ...452..613C 452, 613

    1995 doi

  15. [25]

    Cecil G., et al., 2000, @doi [ ] 10.1086/308959 , https://ui.adsabs.harvard.edu/abs/2000ApJ...536..675C 536, 675

    2000 doi

  16. [26]

    E., 1997, @doi [ ] 10.1086/310813 , https://ui.adsabs.harvard.edu/abs/1997ApJ...485L..75C 485, L75

    Chary R., Becklin E. E., 1997, @doi [ ] 10.1086/310813 , https://ui.adsabs.harvard.edu/abs/1997ApJ...485L..75C 485, L75

    1997 doi

  17. [27]

    S., Mateus A., Vale Asari N., Schoenell W., Sodr \'e L., 2010, @doi [ ] 10.1111/j.1365-2966.2009.16185.x , https://ui.adsabs.harvard.edu/abs/2010MNRAS.403.1036C 403, 1036

    Cid Fernandes R., Stasi \'n ska G., Schlickmann M. S., Mateus A., Vale Asari N., Schoenell W., Sodr \'e L., 2010, @doi [ ] 10.1111/j.1365-2966.2009.16185.x , https://ui.adsabs.harvard.edu/abs/2010MNRAS.403.1036C 403, 1036

    2010

  18. [29]

    Cohen Y., et al., 2018, @doi [ ] 10.3847/1538-4357/aae7c8 , https://ui.adsabs.harvard.edu/abs/2018ApJ...868...96C 868, 96

    2018 doi

  19. [30]

    J., Watson W

    Collison A. J., Watson W. D., 1995, @doi [ ] 10.1086/309729 , https://ui.adsabs.harvard.edu/abs/1995ApJ...452L.103C 452, L103

    1995 doi

  20. [31]

    T., Martin P., Blecha A., Huguenin D., Golay M., 1993, , https://ui.adsabs.harvard.edu/abs/1993A&A...268..419C 268, 419

    Courtes G., Petit H., Hua C. T., Martin P., Blecha A., Huguenin D., Golay M., 1993, , https://ui.adsabs.harvard.edu/abs/1993A&A...268..419C 268, 419

    1993

  21. [32]

    Cox P., Downes D., 1996, @doi [ ] 10.1086/178137 , https://ui.adsabs.harvard.edu/abs/1996ApJ...473..219C 473, 219

    1996 doi

  22. [33]

    Cresci G., et al., 2023, @doi [ ] 10.1051/0004-6361/202346001 , https://ui.adsabs.harvard.edu/abs/2023A&A...672A.128C 672, A128

    2023 doi

  23. [35]

    J., Poetrodjojo H., Ho I

    D'Agostino J. J., Poetrodjojo H., Ho I. T., Groves B., Kewley L., Madore B. F., Rich J., Seibert M., 2018, @doi [ ] 10.1093/mnras/sty1676 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.479.4907D 479, 4907

    2018 doi

  24. [36]

    L., Kewley L

    Davies R. L., Kewley L. J., Ho I. T., Dopita M. A., 2014, @doi [ ] 10.1093/mnras/stu1740 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.444.3961D 444, 3961

    2014 doi

  25. [37]

    L., et al., 2016, @doi [ ] 10.1093/mnras/stw1754 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.462.1616D 462, 1616

    Davies R. L., et al., 2016, @doi [ ] 10.1093/mnras/stw1754 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.462.1616D 462, 1616

    2016 doi

  26. [38]

    L., et al., 2017, @doi [ ] 10.1093/mnras/stx1559 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.470.4974D 470, 4974

    Davies R. L., et al., 2017, @doi [ ] 10.1093/mnras/stx1559 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.470.4974D 470, 4974

    2017 doi

  27. [39]

    J., Koribalski B., 1990, , https://ui.adsabs.harvard.edu/abs/1990A&A...240L..15D 240, L15

    Dettmar R. J., Koribalski B., 1990, , https://ui.adsabs.harvard.edu/abs/1990A&A...240L..15D 240, L15

    1990

  28. [41]

    Ding X., et al., 2020, @doi [ ] 10.3847/1538-4357/ab5b90 , https://ui.adsabs.harvard.edu/abs/2020ApJ...888...37D 888, 37

    2020 doi

  29. [42]

    A., Kewley L

    Dopita M. A., Kewley L. J., Heisler C. A., Sutherland R. S., 2000, @doi [ ] 10.1086/309538 , https://ui.adsabs.harvard.edu/abs/2000ApJ...542..224D 542, 224

    2000 doi

  30. [43]

    A., Storchi-Bergmann T., Ferrari F., Cappellari M., Riffel R

    Drehmer D. A., Storchi-Bergmann T., Ferrari F., Cappellari M., Riffel R. A., 2015, @doi [ ] 10.1093/mnras/stv536 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.450..128D 450, 128

    2015 doi

  31. [44]

    Drevet Mulard M., et al., 2023, @doi [ ] 10.1051/0004-6361/202245173 , https://ui.adsabs.harvard.edu/abs/2023A&A...676A..35D 676, A35

    2023 doi

  32. [45]

    Drissen L., et al., 2019, @doi [ ] 10.1093/mnras/stz627 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.485.3930D 485, 3930

    2019 doi

  33. [46]

    Dutil Y., Beauchamp D., Roy J.-R., 1995, @doi [ ] 10.1086/187866 , https://ui.adsabs.harvard.edu/abs/1995ApJ...444L..85D 444, L85

    1995 doi

  34. [47]

    Emsellem E., et al., 2004, @doi [ ] 10.1111/j.1365-2966.2004.07948.x , https://ui.adsabs.harvard.edu/abs/2004MNRAS.352..721E 352, 721

    2004

  35. [48]

    Emsellem E., et al., 2022, @doi [ ] 10.1051/0004-6361/202141727 , https://ui.adsabs.harvard.edu/abs/2022A&A...659A.191E 659, A191

    2022 doi

  36. [49]

    Erroz-Ferrer S., et al., 2015, @doi [ ] 10.1093/mnras/stv924 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.451.1004E 451, 1004

    2015 doi

  37. [50]

    Erroz-Ferrer S., et al., 2019, @doi [ ] 10.1093/mnras/stz194 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.484.5009E 484, 5009

    2019 doi

  38. [51]

    S., Simpson C., Bower G

    Falcke H., Wilson A. S., Simpson C., Bower G. A., 1996, @doi [ ] 10.1086/310299 , https://ui.adsabs.harvard.edu/abs/1996ApJ...470L..31F 470, L31

    1996 doi

  39. [52]

    A., et al., 2020, @doi [ ] 10.1051/0004-6361/201936552 , https://ui.adsabs.harvard.edu/abs/2020A&A...633A.127F 633, A127

    Fern \'a ndez-Ontiveros J. A., et al., 2020, @doi [ ] 10.1051/0004-6361/201936552 , https://ui.adsabs.harvard.edu/abs/2020A&A...633A.127F 633, A127

    2020 doi

  40. [53]

    C., Dahari O., Jacoby G

    Ford H. C., Dahari O., Jacoby G. H., Crane P. C., Ciardullo R., 1986, @doi [ ] 10.1086/184788 , https://ui.adsabs.harvard.edu/abs/1986ApJ...311L...7F 311, L7

    1986 doi

  41. [54]

    Fragkoudi F., Grand R. J. J., Pakmor R., G \'o mez F., Marinacci F., Springel V., 2025, @doi [ ] 10.1093/mnras/staf389 , https://ui.adsabs.harvard.edu/abs/2025MNRAS.538.1587F 538, 1587

    2025 doi

  42. [55]

    J., Filippenko A

    Fruscione A., Greenhill L. J., Filippenko A. V., Moran J. M., Herrnstein J. R., Galle E., 2005, @doi [ ] 10.1086/428658 , https://ui.adsabs.harvard.edu/abs/2005ApJ...624..103F 624, 103

    2005 doi

  43. [56]

    L., et al., 2002, @doi [ ] 10.1086/342355 , https://ui.adsabs.harvard.edu/abs/2002PASP..114.1043G 114, 1043

    Gach J. L., et al., 2002, @doi [ ] 10.1086/342355 , https://ui.adsabs.harvard.edu/abs/2002PASP..114.1043G 114, 1043

    2002 doi

  44. [57]

    Garc \' a-Bernete I., et al., 2021, @doi [ ] 10.1051/0004-6361/202038256 , https://ui.adsabs.harvard.edu/abs/2021A&A...645A..21G 645, A21

    2021 doi

  45. [58]

    Garc \' a-Burillo S., et al., 2019, @doi [ ] 10.1051/0004-6361/201936606 , https://ui.adsabs.harvard.edu/abs/2019A&A...632A..61G 632, A61

    2019 doi

  46. [59]

    A., et al., 2019, @doi [ ] 10.3847/1538-4357/ab113a , https://ui.adsabs.harvard.edu/abs/2019ApJ...876...39G 876, 39

    Gonz \'a lez-L \'o pezlira R. A., et al., 2019, @doi [ ] 10.3847/1538-4357/ab113a , https://ui.adsabs.harvard.edu/abs/2019ApJ...876...39G 876, 39

    2019 doi

  47. [60]

    S., Ramsay S

    Grandmont F., Drissen L., Mandar J., Thibault S., Baril M., 2012, in McLean I. S., Ramsay S. K., Takami H., eds, Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series Vol. 8446, Ground-based and Airborne Instrumentation for Astronomy IV. p. 84460U, @doi 1...

    2012 doi

  48. [61]

    E., Ho L

    Greene J. E., Ho L. C., 2005, @doi [ ] 10.1086/431897 , https://ui.adsabs.harvard.edu/abs/2005ApJ...630..122G 630, 122

    2005 doi

  49. [62]

    Grosb l P., Dottori H., 2012, @doi [ ] 10.1051/0004-6361/201118099 , https://ui.adsabs.harvard.edu/abs/2012A&A...542A..39G 542, A39

    2012 doi

  50. [63]

    J., 2012, @doi [ ] 10.1111/j.1365-2966.2011.19796.x , https://ui.adsabs.harvard.edu/abs/2012MNRAS.419.1402G 419, 1402

    Groves B., Brinchmann J., Walcher C. J., 2012, @doi [ ] 10.1111/j.1365-2966.2011.19796.x , https://ui.adsabs.harvard.edu/abs/2012MNRAS.419.1402G 419, 1402

    2012

  51. [64]

    M., Alexander D

    Harrison C. M., Alexander D. M., Mullaney J. R., Swinbank A. M., 2014, @doi [ ] 10.1093/mnras/stu515 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.441.3306H 441, 3306

    2014 doi

  52. [65]

    Heald G., et al., 2011, @doi [ ] 10.1051/0004-6361/201015938 , https://ui.adsabs.harvard.edu/abs/2011A&A...526A.118H 526, A118

    2011 doi

  53. [66]

    R., Moran J

    Herrnstein J. R., Moran J. M., Greenhill L. J., Trotter A. S., 2005, @doi [ ] 10.1086/431421 , https://ui.adsabs.harvard.edu/abs/2005ApJ...629..719H 629, 719

    2005 doi

  54. [67]

    C., Filippenko A

    Ho L. C., Filippenko A. V., Sargent W. L. W., 1997, @doi [ ] 10.1086/313041 , https://ui.adsabs.harvard.edu/abs/1997ApJS..112..315H 112, 315

    1997 doi

  55. [68]

    F., Chan T

    Hopkins P. F., Chan T. K., Squire J., Quataert E., Ji S., Kere s D., Faucher-Gigu \`e re C.-A., 2021, @doi [ ] 10.1093/mnras/staa3692 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.501.3663H 501, 3663

    2021 doi

  56. [70]

    Humphreys E. M. L., Reid M. J., Moran J. M., Greenhill L. J., Argon A. L., 2013a, @doi [ ] 10.1088/0004-637X/775/1/13 , http://adsabs.harvard.edu/abs/2013ApJ...775...13H 775, 13

    doi

  57. [71]

    M., 2018, @doi [Nature Astronomy] 10.1038/s41550-018-0407-2 , https://ui.adsabs.harvard.edu/abs/2018NatAs...2..196H 2, 196

    Husemann B., Harrison C. M., 2018, @doi [Nature Astronomy] 10.1038/s41550-018-0407-2 , https://ui.adsabs.harvard.edu/abs/2018NatAs...2..196H 2, 196

    2018 doi

  58. [72]

    N., Mainieri V., Woo J

    Husemann B., Scharw \"a chter J., Bennert V. N., Mainieri V., Woo J. H., Kakkad D., 2016, @doi [ ] 10.1051/0004-6361/201527992 , https://ui.adsabs.harvard.edu/abs/2016A&A...594A..44H 594, A44

    2016 doi

  59. [73]

    A., Jahnke K., Dannerbauer H., Urrutia T., Hodge J., 2017, @doi [ ] 10.1093/mnras/stx1123 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.470.1570H 470, 1570

    Husemann B., Davis T. A., Jahnke K., Dannerbauer H., Urrutia T., Hodge J., 2017, @doi [ ] 10.1093/mnras/stx1123 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.470.1570H 470, 1570

    2017 doi

  60. [74]

    Husemann B., et al., 2022, @doi [ ] 10.1051/0004-6361/202141312 , https://ui.adsabs.harvard.edu/abs/2022A&A...659A.124H 659, A124

    2022 doi

  61. [75]

    D., Calle D., Weiler K

    Hyman S. D., Calle D., Weiler K. W., Lacey C. K., Van Dyk S. D., Sramek R., 2001, @doi [ ] 10.1086/320231 , https://ui.adsabs.harvard.edu/abs/2001ApJ...551..702H 551, 702

    2001 doi

  62. [77]

    Juneau S., et al., 2022, @doi [ ] 10.3847/1538-4357/ac425f , https://ui.adsabs.harvard.edu/abs/2022ApJ...925..203J 925, 203

    2022 doi

  63. [78]

    Kakkad D., et al., 2023, @doi [ ] 10.1093/mnras/stad439 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.520.5783K 520, 5783

    2023 doi

  64. [79]

    Kang D., Woo J.-H., 2018, @doi [ ] 10.3847/1538-4357/aad561 , https://ui.adsabs.harvard.edu/abs/2018ApJ...864..124K 864, 124

    2018 doi

  65. [80]

    Karouzos M., Woo J.-H., Bae H.-J., 2016, @doi [ ] 10.3847/0004-637X/819/2/148 , https://ui.adsabs.harvard.edu/abs/2016ApJ...819..148K 819, 148

    2016 doi

  66. [81]

    Kauffmann G., et al., 2003, @doi [ ] 10.1111/j.1365-2966.2003.07154.x , http://adsabs.harvard.edu/abs/2003MNRAS.346.1055K 346, 1055

    2003

  67. [82]

    J., 1998, @doi [ ] 10.1146/annurev.astro.36.1.189 , https://ui.adsabs.harvard.edu/abs/1998ARA&A..36..189K 36, 189

    Kennicutt Robert C. J., 1998, @doi [ ] 10.1146/annurev.astro.36.1.189 , https://ui.adsabs.harvard.edu/abs/1998ARA&A..36..189K 36, 189

    1998 doi

  68. [83]

    Kennicutt Jr. R. C., et al., 1998, @doi [ ] 10.1086/305538 , http://adsabs.harvard.edu/abs/1998ApJ...498..181K 498, 181

    1998 doi

  69. [85]

    J., Maier C., Yabe K., Ohta K., Akiyama M., Dopita M

    Kewley L. J., Maier C., Yabe K., Ohta K., Akiyama M., Dopita M. A., Yuan T., 2013a, @doi [ ] 10.1088/2041-8205/774/1/L10 , https://ui.adsabs.harvard.edu/abs/2013ApJ...774L..10K 774, L10

    doi

  70. [86]

    J., Dopita M

    Kewley L. J., Dopita M. A., Leitherer C., Dav \'e R., Yuan T., Allen M., Groves B., Sutherland R., 2013b, @doi [ ] 10.1088/0004-637X/774/2/100 , https://ui.adsabs.harvard.edu/abs/2013ApJ...774..100K 774, 100

    doi

  71. [87]

    C., 2013, @doi [ ] 10.1146/annurev-astro-082708-101811 , https://ui.adsabs.harvard.edu/abs/2013ARA&A..51..511K 51, 511

    Kormendy J., Ho L. C., 2013, @doi [ ] 10.1146/annurev-astro-082708-101811 , https://ui.adsabs.harvard.edu/abs/2013ARA&A..51..511K 51, 511

    2013 doi

  72. [88]

    Krause M., L \"o hr A., 2004, @doi [ ] 10.1051/0004-6361:20034165 , https://ui.adsabs.harvard.edu/abs/2004A&A...420..115K 420, 115

    2004 doi

  73. [89]

    A., Downes D., 1990, , https://ui.adsabs.harvard.edu/abs/1990A&A...233L...1K 233, L1

    Krause M., Cox P., Garcia-Barreto J. A., Downes D., 1990, , https://ui.adsabs.harvard.edu/abs/1990A&A...233L...1K 233, L1

    1990

  74. [90]

    Krause M., Fendt C., Neininger N., 2007, @doi [ ] 10.1051/0004-6361:20066445 , https://ui.adsabs.harvard.edu/abs/2007A&A...467.1037K 467, 1037

    2007 doi

  75. [91]

    S., Siopis C., 2010, @doi [ ] 10.1088/0004-6256/140/4/1084 , https://ui.adsabs.harvard.edu/abs/2010AJ....140.1084L 140, 1084

    Laine S., Krause M., Tabatabaei F. S., Siopis C., 2010, @doi [ ] 10.1088/0004-6256/140/4/1084 , https://ui.adsabs.harvard.edu/abs/2010AJ....140.1084L 140, 1084

    2010 doi

  76. [92]

    F., Bland-Hawthorn J., Moiseev A

    L \'o pez-Cob \'a C., S \'a nchez S. F., Bland-Hawthorn J., Moiseev A. V., Cruz-Gonz \'a lez I., Garc \' a-Benito R., Barrera-Ballesteros J. K., Galbany L., 2019, @doi [ ] 10.1093/mnras/sty2960 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.482.4032L 482, 4032

    2019 doi

  77. [93]

    Makishima K., et al., 1994, , https://ui.adsabs.harvard.edu/abs/1994PASJ...46L..77M 46, L77

    1994

  78. [94]

    Y., 1989, @doi [ ] 10.1086/167943 , https://ui.adsabs.harvard.edu/abs/1989ApJ...345..707M 345, 707

    Martin P., Roy J.-R., Noreau L., Lo K. Y., 1989, @doi [ ] 10.1086/167943 , https://ui.adsabs.harvard.edu/abs/1989ApJ...345..707M 345, 707

    1989 doi

  79. [95]

    R., Rosolowsky E., eds, Astronomical Society of the Pacific Conference Series Vol

    Martin T., Drissen L., Joncas G., 2015, in Taylor A. R., Rosolowsky E., eds, Astronomical Society of the Pacific Conference Series Vol. 495, Astronomical Data Analysis Software an Systems XXIV (ADASS XXIV). p. 327

    2015

  80. [96]

    B., Prunet S., Drissen L., 2016, @doi [ ] 10.1093/mnras/stw2315 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.463.4223M 463, 4223

    Martin T. B., Prunet S., Drissen L., 2016, @doi [ ] 10.1093/mnras/stw2315 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.463.4223M 463, 4223

    2016 doi

  81. [97]

    B., Drissen L., Melchior A.-L., 2018, @doi [ ] 10.1093/mnras/stx2513 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.473.4130M 473, 4130

    Martin T. B., Drissen L., Melchior A.-L., 2018, @doi [ ] 10.1093/mnras/stx2513 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.473.4130M 473, 4130

    2018 doi

  82. [98]

    M., Pracy M., Sharp R., Ho I

    McElroy R., Croom S. M., Pracy M., Sharp R., Ho I. T., Medling A. M., 2015, @doi [ ] 10.1093/mnras/stu2224 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.446.2186M 446, 2186

    2015 doi

  83. [99]

    B., da Silva P., Steiner J

    Menezes R. B., da Silva P., Steiner J. E., 2018, @doi [ ] 10.1093/mnras/stx2448 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.473.2198M 473, 2198

    2018 doi

  84. [100]

    Mingozzi M., Venturi G., Mannucci F., Marconi A., Cresci G., 2019, @doi [Communications of the Byurakan Astrophysical Observatory] 10.52526/25792776-2019.66.2-159 , https://ui.adsabs.harvard.edu/abs/2019CoBAO..66..159M 66, 159

    2019 doi

  85. [101]

    C., Wang R., Shangguan J., Bauer F

    Molina J., Ho L. C., Wang R., Shangguan J., Bauer F. E., Treister E., 2023, @doi [ ] 10.3847/1538-4357/acaa9b , https://ui.adsabs.harvard.edu/abs/2023ApJ...944...30M 944, 30

    2023 doi

  86. [102]

    Y., Oosterloo T., Guillard P., Mukherjee D., Bicknell G., 2022, @doi [Nature Astronomy] 10.1038/s41550-021-01596-6 , https://ui.adsabs.harvard.edu/abs/2022NatAs...6..488M 6, 488

    Murthy S., Morganti R., Wagner A. Y., Oosterloo T., Guillard P., Mukherjee D., Bicknell G., 2022, @doi [Nature Astronomy] 10.1038/s41550-021-01596-6 , https://ui.adsabs.harvard.edu/abs/2022NatAs...6..488M 6, 488

    2022 doi

  87. [103]

    Nandi P., et al., 2023, @doi [ ] 10.3847/1538-4357/ad0c57 , https://ui.adsabs.harvard.edu/abs/2023ApJ...959..116N 959, 116

    2023 doi

  88. [104]

    Nelson D., et al., 2019, @doi [ ] 10.1093/mnras/stz2306 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.490.3234N 490, 3234

    2019 doi

  89. [105]

    Neumann J., et al., 2019, @doi [ ] 10.1051/0004-6361/201834441 , https://ui.adsabs.harvard.edu/abs/2019A&A...627A..26N 627, A26

    2019 doi

  90. [106]

    S., Kennicutt R

    Oey M. S., Kennicutt R. C. J., 1993, @doi [ ] 10.1086/172814 , https://ui.adsabs.harvard.edu/abs/1993ApJ...411..137O 411, 137

    1993 doi

  91. [107]

    M., Lanz L., Appleton P

    Ogle P. M., Lanz L., Appleton P. N., 2014, @doi [ ] 10.1088/2041-8205/788/2/L33 , https://ui.adsabs.harvard.edu/abs/2014ApJ...788L..33O 788, L33

    2014 doi

  92. [108]

    M., Jarrett T., Lanz L., Cluver M., Alatalo K., Appleton P

    Ogle P. M., Jarrett T., Lanz L., Cluver M., Alatalo K., Appleton P. N., Mazzarella J. M., 2019, @doi [ ] 10.3847/2041-8213/ab459e , https://ui.adsabs.harvard.edu/abs/2019ApJ...884L..11O 884, L11

    2019 doi

  93. [109]

    E., Ferland G

    Osterbrock D. E., Ferland G. J., 2006, Astrophysics of gaseous nebulae and active galactic nuclei . University Science Books

    2006

  94. [110]

    Perna M., Lanzuisi G., Brusa M., Cresci G., Mignoli M., 2017, @doi [ ] 10.1051/0004-6361/201730819 , https://ui.adsabs.harvard.edu/abs/2017A&A...606A..96P 606, A96

    2017 doi

  95. [111]

    Pillepich A., et al., 2018, @doi [ ] 10.1093/mnras/stx2656 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.473.4077P 473, 4077

    2018 doi

  96. [112]

    J., Groves B., Kewley L., Ho I

    Poetrodjojo H., D'Agostino J. J., Groves B., Kewley L., Ho I. T., Rich J., Madore B. F., Seibert M., 2019, @doi [ ] 10.1093/mnras/stz1241 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.487...79P 487, 79

    2019 doi

  97. [113]

    Ptak A., Serlemitsos P., Yaqoob T., Mushotzky R., 1999, @doi [ ] 10.1086/313179 , https://ui.adsabs.harvard.edu/abs/1999ApJS..120..179P 120, 179

    1999 doi

  98. [114]

    J., Pesce D

    Reid M. J., Pesce D. W., Riess A. G., 2019, @doi [ ] 10.3847/2041-8213/ab552d , https://ui.adsabs.harvard.edu/abs/2019ApJ...886L..27R 886, L27

    2019 doi

  99. [115]

    Revalski M., et al., 2021, @doi [ ] 10.3847/1538-4357/abdcad , https://ui.adsabs.harvard.edu/abs/2021ApJ...910..139R 910, 139

    2021 doi

  100. [116]

    S., Nowak M

    Reynolds C. S., Nowak M. A., Maloney P. R., 2000, @doi [ ] 10.1086/309327 , https://ui.adsabs.harvard.edu/abs/2000ApJ...540..143R 540, 143

    2000 doi

  101. [117]

    T., Allen J

    Richardson C. T., Allen J. T., Baldwin J. A., Hewett P. C., Ferland G. J., 2014, @doi [ ] 10.1093/mnras/stt2056 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.437.2376R 437, 2376

    2014 doi

  102. [118]

    C., et al., 2021, @doi [ ] 10.3847/2041-8213/abd32f , https://ui.adsabs.harvard.edu/abs/2021ApJ...906L...6R 906, L6

    Robleto-Or \'u s A. C., et al., 2021, @doi [ ] 10.3847/2041-8213/abd32f , https://ui.adsabs.harvard.edu/abs/2021ApJ...906L...6R 906, L6

    2021 doi

  103. [119]

    F., Kennicutt R

    Rosales-Ortega F. F., Kennicutt R. C., S \'a nchez S. F., D \' az A. I., Pasquali A., Johnson B. D., Hao C. N., 2010, @doi [ ] 10.1111/j.1365-2966.2010.16498.x , https://ui.adsabs.harvard.edu/abs/2010MNRAS.405..735R 405, 735

    2010

  104. [120]

    P., Drissen L., Martin T., 2018, @doi [ ] 10.1093/mnras/sty477 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.477.4152R 477, 4152

    Rousseau-Nepton L., Robert C., Martin R. P., Drissen L., Martin T., 2018, @doi [ ] 10.1093/mnras/sty477 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.477.4152R 477, 4152

    2018 doi

  105. [121]

    Rousseau-Nepton L., et al., 2019, @doi [ ] 10.1093/mnras/stz2455 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.489.5530R 489, 5530

    2019 doi

  106. [122]

    R., Arsenault R., Noreau L., 1985, @doi [ ] 10.1086/131489 , https://ui.adsabs.harvard.edu/abs/1985PASP...97...32R 97, 32

    Roy J. R., Arsenault R., Noreau L., 1985, @doi [ ] 10.1086/131489 , https://ui.adsabs.harvard.edu/abs/1985PASP...97...32R 97, 32

    1985 doi

  107. [123]

    C., Graham J

    Rubin V. C., Graham J. A., 1990, @doi [ ] 10.1086/185834 , https://ui.adsabs.harvard.edu/abs/1990ApJ...362L...5R 362, L5

    1990 doi

  108. [124]

    Ruschel-Dutra D., et al., 2021, @doi [ ] 10.1093/mnras/stab2058 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.507...74R 507, 74

    2021 doi

  109. [125]

    F., et al., 2012, @doi [ ] 10.1051/0004-6361/201219578 , https://ui.adsabs.harvard.edu/abs/2012A&A...546A...2S 546, A2

    S \'a nchez S. F., et al., 2012, @doi [ ] 10.1051/0004-6361/201219578 , https://ui.adsabs.harvard.edu/abs/2012A&A...546A...2S 546, A2

    2012 doi

  110. [126]

    L., et al., 2016, @doi [ ] 10.3847/0004-637X/816/1/23 , https://ui.adsabs.harvard.edu/abs/2016ApJ...816...23S 816, 23

    Sanders R. L., et al., 2016, @doi [ ] 10.3847/0004-637X/816/1/23 , https://ui.adsabs.harvard.edu/abs/2016ApJ...816...23S 816, 23

    2016 doi

  111. [127]

    A., et al., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2505.14781 , https://ui.adsabs.harvard.edu/abs/2025arXiv250514781S p

    Silva-Lima L. A., et al., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2505.14781 , https://ui.adsabs.harvard.edu/abs/2025arXiv250514781S p. arXiv:2505.14781

    2025 doi arXiv

  112. [128]

    Smirnova-Pinchukova I., et al., 2022, @doi [ ] 10.1051/0004-6361/202142011 , https://ui.adsabs.harvard.edu/abs/2022A&A...659A.125S 659, A125

    2022 doi

  113. [129]

    Sofue Y., Doi M., Krause M., Nakai N., Handa T., 1989, , https://ui.adsabs.harvard.edu/abs/1989PASJ...41..113S 41, 113

    1989

  114. [130]

    V., 2006, @doi [ ] 10.1111/j.1365-2966.2006.10732.x , https://ui.adsabs.harvard.edu/abs/2006MNRAS.371..972S 371, 972

    Stasi \'n ska G., Cid Fernandes R., Mateus A., Sodr \'e L., Asari N. V., 2006, @doi [ ] 10.1111/j.1365-2966.2006.10732.x , https://ui.adsabs.harvard.edu/abs/2006MNRAS.371..972S 371, 972

    2006

  115. [131]

    J., Zeippen C

    Storey P. J., Zeippen C. J., 2000, @doi [ ] 10.1046/j.1365-8711.2000.03184.x , https://ui.adsabs.harvard.edu/abs/2000MNRAS.312..813S 312, 813

    2000

  116. [132]

    Teimoorinia H., Keown J., 2018, @doi [ ] 10.1093/mnras/sty1331 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.478.3177T 478, 3177

    2018 doi

  117. [133]

    I., Terlevich R., 1990, @doi [ ] 10.1093/mnras/242.3.271 , https://ui.adsabs.harvard.edu/abs/1990MNRAS.242..271T 242, 271

    Terlevich E., Diaz A. I., Terlevich R., 1990, @doi [ ] 10.1093/mnras/242.3.271 , https://ui.adsabs.harvard.edu/abs/1990MNRAS.242..271T 242, 271

    1990 doi

  118. [134]

    D., Kewley L

    Thomas A. D., Kewley L. J., Dopita M. A., Groves B. A., Hopkins A. M., Sutherland R. S., 2018, @doi [ ] 10.3847/2041-8213/aacce7 , https://ui.adsabs.harvard.edu/abs/2018ApJ...861L...2T 861, L2

    2018 doi

  119. [135]

    A., Armus L., Murray N., Walth G., 2021, @doi [ ] 10.3847/1538-4357/ac2b9e , https://ui.adsabs.harvard.edu/abs/2021ApJ...923...59V 923, 59

    Vayner A., Zakamska N., Wright S. A., Armus L., Murray N., Walth G., 2021, @doi [ ] 10.3847/1538-4357/ac2b9e , https://ui.adsabs.harvard.edu/abs/2021ApJ...923...59V 923, 59

    2021 doi

  120. [136]

    Vayner A., et al., 2023, @doi [ ] 10.3847/1538-4357/ace784 , https://ui.adsabs.harvard.edu/abs/2023ApJ...955...92V 955, 92

    2023 doi

  121. [137]

    Vazdekis A., Koleva M., Ricciardelli E., R \"o ck B., Falc \'o n-Barroso J., 2016, @doi [ ] 10.1093/mnras/stw2231 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.463.3409V 463, 3409

    2016 doi

  122. [138]

    E., 1987, in Lonsdale Persson C

    Veilleux S., Osterbrock D. E., 1987, in Lonsdale Persson C. J., ed., NASA Conference Publication Vol. 2466, NASA Conference Publication. pp 737--740

    1987

  123. [139]

    Veilleux S., et al., 2023, @doi [ ] 10.3847/1538-4357/ace10f , https://ui.adsabs.harvard.edu/abs/2023ApJ...953...56V 953, 56

    2023 doi

  124. [140]

    Venturi G., et al., 2018, @doi [ ] 10.1051/0004-6361/201833668 , https://ui.adsabs.harvard.edu/abs/2018A&A...619A..74V 619, A74

    2018 doi

  125. [141]

    Venturi G., et al., 2021, @doi [ ] 10.1051/0004-6361/202039869 , https://ui.adsabs.harvard.edu/abs/2021A&A...648A..17V 648, A17

    2021 doi

  126. [142]

    Villar-Mart \' n M., Cabrera-Lavers A., Humphrey A., Silva M., Ramos Almeida C., Piqueras-L \'o pez J., Emonts B., 2018, @doi [ ] 10.1093/mnras/stx2911 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.474.2302V 474, 2302

    2018 doi

  127. [143]

    Vogler A., Pietsch W., 1999, , https://ui.adsabs.harvard.edu/abs/1999A&A...352...64V 352, 64

    1999

  128. [144]

    B., et al., 2024, @doi [ ] 10.1093/mnras/stae898 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.530.1968W 530, 1968

    Watts A. B., et al., 2024, @doi [ ] 10.1093/mnras/stae898 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.530.1968W 530, 1968

    2024 doi

  129. [145]

    Weinberger R., et al., 2017, @doi [ ] 10.1093/mnras/stw2944 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.465.3291W 465, 3291

    2017 doi

  130. [146]

    S., Clements D

    Westmoquette M. S., Clements D. L., Bendo G. J., Khan S. A., 2012, @doi [ ] 10.1111/j.1365-2966.2012.21214.x , https://ui.adsabs.harvard.edu/abs/2012MNRAS.424..416W 424, 416

    2012

  131. [147]

    J., Schmidt G

    Wilkes B. J., Schmidt G. D., Smith P. S., Mathur S., McLeod K. K., 1995, @doi [ ] 10.1086/309817 , https://ui.adsabs.harvard.edu/abs/1995ApJ...455L..13W 455, L13

    1995 doi

  132. [148]

    S., Tsvetanov Z

    Wilson A. S., Tsvetanov Z. I., 1994, @doi [ ] 10.1086/116935 , https://ui.adsabs.harvard.edu/abs/1994AJ....107.1227W 107, 1227

    1994 doi

  133. [149]

    S., Yang Y., 2001, @doi [Astrophysical Journal] 10.1086/338882 , 568, 133

    Wilson A. S., Yang Y., 2001, @doi [Astrophysical Journal] 10.1086/338882 , 568, 133

    2001 doi

  134. [150]

    S., Yang Y., Cecil G., 2001, @doi [ ] 10.1086/322766 , https://ui.adsabs.harvard.edu/abs/2001ApJ...560..689W 560, 689

    Wilson A. S., Yang Y., Cecil G., 2001, @doi [ ] 10.1086/322766 , https://ui.adsabs.harvard.edu/abs/2001ApJ...560..689W 560, 689

    2001 doi

  135. [151]

    Woo J.-H., Bae H.-J., Son D., Karouzos M., 2016, @doi [ ] 10.3847/0004-637X/817/2/108 , https://ui.adsabs.harvard.edu/abs/2016ApJ...817..108W 817, 108

    2016 doi

  136. [152]

    L., Greene J

    Wylezalek D., Zakamska N. L., Greene J. E., Riffel R. A., Drory N., Andrews B. H., Merloni A., Thomas D., 2018, @doi [ ] 10.1093/mnras/stx2784 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.474.1499W 474, 1499

    2018 doi

  137. [153]

    M., Zakamska N

    Wylezalek D., Flores A. M., Zakamska N. L., Greene J. E., Riffel R. A., 2020, @doi [ ] 10.1093/mnras/staa062 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.492.4680W 492, 4680

    2020 doi

  138. [154]

    Wylezalek D., et al., 2022, @doi [ ] 10.3847/2041-8213/ac98c3 , https://ui.adsabs.harvard.edu/abs/2022ApJ...940L...7W 940, L7

    2022 doi

  139. [155]

    L., 2002, @doi [ ] 10.1051/0004-6361:20020817 , https://ui.adsabs.harvard.edu/abs/2002A&A...391..139Y 391, 139

    Yuan F., Markoff S., Falcke H., Biermann P. L., 2002, @doi [ ] 10.1051/0004-6361:20020817 , https://ui.adsabs.harvard.edu/abs/2002A&A...391..139Y 391, 139

    2002 doi

  140. [156]

    J., Gaulle A., 2020, @doi [ ] 10.1093/mnras/staa2488 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.498.4345Z 498, 4345

    Zewdie D., Povi \'c M., Aravena M., Assef R. J., Gaulle A., 2020, @doi [ ] 10.1093/mnras/staa2488 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.498.4345Z 498, 4345

    2020 doi

  141. [157]

    J., Buta R

    de Vaucouleurs G., de Vaucouleurs A., Corwin Herold G. J., Buta R. J., Paturel G., Fouque P., 1991, Third Reference Catalogue of Bright Galaxies . Springer-Verlag

    1991

  142. [158]

    D., 1980, , https://ui.adsabs.harvard.edu/abs/1980A&AS...39..283V 39, 283

    van Albada G. D., 1980, , https://ui.adsabs.harvard.edu/abs/1980A&AS...39..283V 39, 283

    1980

  143. [159]

    C., Oort J

    van der Kruit P. C., Oort J. H., Mathewson D. S., 1972, , https://ui.adsabs.harvard.edu/abs/1972A&A....21..169V 21, 169

    1972

  144. [160]

    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 6, 2026 · model on record in the stance chip above.