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Characterizing the roles of transitory obscured phases and inner torus in shaping the fractions of obscured AGN at cosmic noon

T0 review · 3 major / 4 minor · reviewed 2026-08-05 · deepseek-v4-flash

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Pith's one-line read Long-lived torus explains hidden AGN at cosmic noon

desk verdict The negative result is solid — long post-peak visible phases underproduce obscured AGN at z~2–3 — but the positive matches rely on trial-and-error tuning and a Wada torus prescription imported from the local universe, so the quantitative conclusions are shakier than the qualitative ones. read the letter →

arxiv 2509.04553 v1 pith:RNBVQ3XO submitted 2025-09-04 astro-ph.GA hep-th

Alba V. Alonso-Tetilla , Francesco Shankar , Fabio Fontanot , Andrea Lapi , Milena Valentini , Annagrazia Puglisi , Nicola Menci , Hao Fu
show 6 more authors
Lumen Boco Johannes Buchner Michaela Hirschmann Cristina Ramos Almeida Carolin Villforth Lizhi Xie
This is my paper
classification astro-ph.GAhep-th
keywords AGNobscurationCompton-thicklightcurvesinnertoruscosmicnoonsemi-analyticgalaxyformationX-raysurveysblackholeaccretion
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 settle whether the many obscured supermassive black holes seen at z~2-3 are caught in a brief dust-shrouded growth phase or are hidden by a persistent ring of material around the black hole. It shows that the simplest evolutionary story—a short hidden pre-peak phase followed by a long unobscured post-peak phase—cannot reproduce the high fraction of obscured AGN measured in X-ray surveys. Matching the data requires either fine-tuned light curves in which brighter AGN stay visible much longer, or a long-lived torus whose thickness shrinks as AGN power grows. The authors conclude that small-scale orientation effects may remain essential even in evolutionary scenarios, and that starbursts or major mergers alone cannot account for the heavily obscured faint AGN.

What carries the argument

The central object is the AGN light curve: an exponential pre-peak accretion phase followed by a power-law post-peak decline, with the total duration fixed near 2e8 years. Obscuration is assigned by which phase of the light curve an AGN is caught in, with a 'visibility window' defining how long it shines unobscured in the optical/UV. The decisive addition is a long-lived torus—a parsec-scale dusty ring assumed to survive the whole light curve—whose thickness decreases with AGN luminosity, so bright AGN obscure a smaller solid angle. This torus converts flat, too-low obscured fractions into the luminosity-dependent fractions seen in the data.

What would settle it

Measure the torus covering factor for a luminosity-stratified sample of z~2-3 AGN using ALMA molecular-line or mid-IR imaging: if the covering factor is roughly constant across luminosity, or if only a minority of AGN show compact tori, the long-lived torus explanation fails. Alternatively, showing that bright quasars remain unobscured for longer than 1e8 years with no torus present would undercut the fine-tuned light-curve interpretation.

Watch

Extended reading notes

Core claim

Working within a cosmological semi-analytic model that tracks individual black hole accretion events, the paper assigns each AGN a column density and luminosity from a four-phase light curve: Compton-thick pre-peak, Compton-thin pre-peak, visible peak, and optional visible or Compton-thin post-peak. It finds that models with short pre-peak obscured phases followed by extended optical/UV visible post-peak phases produce only roughly 40% obscured fractions, far below the 60-80% reported by several X-ray surveys at z~2-3. Models that cut the light curve sharply after the peak, or that allow a late Compton-thin phase, do better. The cleanest match comes from adding a long-lived inner torus whose

Load-bearing premise

The conclusion that a long-lived torus naturally produces the observed luminosity dependence rests on the assumption that every AGN always has enough circumnuclear material to form a torus and that the torus's thickness shrinks as AGN luminosity grows; if tori are transient or their covering factor is constant, the claimed boost and luminosity trend weaken.

Editorial extensions

If this is right

  • Evolution models with extended visible post-peak phases underpredict obscured AGN fractions at z~2-3; the post-peak phase must be short or partially obscured.
  • Luminosity-dependent visibility windows, with bright AGN visible for up to ~1e8 years, reproduce the steep decline in obscured fraction with X-ray luminosity and are consistent with clustering-based duty-cycle estimates.
  • A long-lived torus with luminosity-dependent thickness boosts both Compton-thin and Compton-thick fractions and produces a similar luminosity trend, so orientation effects remain viable inside evolutionary models.
  • Starburst or major-merger selection criteria, taken alone, cannot generate the large population of heavily obscured faint AGN; an additional obscuring component is needed.
  • Models that match the Compton-thin fractions via a torus versus via fine-tuned light curves predict different absolute number densities of Compton-thick AGN, which deep X-ray surveys can distinguish.

Reading between the lines

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

  • If the torus is replenished by accretion-disc winds, the obscured fraction should correlate with Eddington ratio and black hole mass; existing Eddington-ratio distributions could be re-examined to test this.
  • The degeneracy between luminosity-dependent light curves and a long-lived torus could be broken by clustering: a long-lived torus leaves the intrinsic quasar lifetime long, whereas a fine-tuned light curve shortens it, producing different large-scale bias at fixed luminosity.
  • The finding that major mergers fail to explain faint Compton-thick AGN predicts that deep, high-resolution imaging at z~2-3 will find heavily obscured AGN in galaxies with no recent merger or strong starburst.
  • If the torus is long-lived, the obscured fraction should be nearly independent of time-since-trigger within a single AGN episode, contrary to pure evolutionary expectations.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 4 minor

Summary. This paper combines the GAEA semi-analytic model with semi-empirical prescriptions to explore the origin of AGN obscuration at 1<z<3. It defines four pure Evolution models that differ in the fraction of the AGN light curve spent in Compton-thin, Compton-thick, and optical/UV-visible phases, and then adds luminosity-dependent visibility windows, short- and long-lived tori, hybrid orientation/evolution models, and starburst/merger-based obscuration criteria. The predicted CTN and CTK fractions are compared to the U14, B15, and A19 X-ray data at z~2.4. The central conclusions are that traditional pure Evolution models with extended post-peak visible phases produce too few obscured AGN, that sharp post-peak declines or persistent obscuration do better, that a luminosity-dependent visibility window or a long-lived, luminosity-thinned torus can reproduce the steep luminosity trend seen by U14/A19, and that major mergers and starbursts alone cannot account for the faint CTK population.

Significance. If the main negative result holds, it is a useful quantitative statement: within the GAEA framework, simple Evolution models with extended optical/UV-visible post-peak phases are disfavoured, and some form of prolonged or geometry-based obscuration is needed. The paper is commendably transparent about the ad hoc nature of its most successful variants, and it explicitly discusses degeneracies between fine-tuned light curves and torus models. The absolute CTK luminosity functions in Fig. 11 are a potentially testable discriminator. However, the positive alternatives are not independent predictions: the luminosity-dependent visibility windows are fitted to the same data they reproduce, the Model 3 phase split is chosen to match CTK fractions, and the long-lived torus conclusion imports the Wada (2015) luminosity-dependent covering factor without testing its validity at cosmic noon.

major comments (3)
  1. [Sec. 3.2.1, Eqs. (4)-(5)] The luminosity-dependent visibility windows are explicitly 'empirically calibrated via trial and error to produce an improved match to the fractions of obscured AGN measured by U14 and A19'. The agreement of the long-dashed red curves in Figs. 3-4 with U14/A19 is therefore a fit, not a prediction. This circularity should be stated prominently wherever these models are used as evidence that 'fine-tuned' LCs can explain the data. The paper's wording mostly acknowledges this, but the conclusions still count the match as support. I recommend reframing: the models demonstrate that a particular ad hoc luminosity dependence can reproduce the data, not that such a dependence is required. A quantitative comparison (e.g., residuals or a goodness-of-fit statistic) for all models would also help the reader distinguish by-eye agreement from statistical support.
  2. [Sec. 3.2, Model 3] Model 3 sets the CTK and CTN phase durations to 1/3 and 2/3 of the pre-peak LC 'to ensure that at least 30% of CTK AGN are generated, in line with the measurements by U14 and A19'. The strong CTK fractions predicted by Model 3 in Fig. 4 are thus partly built in by construction. The same issue applies to Model 4, where the full pre-peak phase is assumed CTK. To make the relative success of Models 3/4 meaningful, the paper should quantify the sensitivity of the CTK/CTN fractions to these phase-duration choices and, ideally, connect them to external constraints on the Eddington-ratio distribution or on the duration of heavily obscured phases rather than to the target fractions themselves.
  3. [Sec. 3.2.2 and Sec. 5.1] The claim that a long-lived torus 'naturally' reproduces the observed luminosity-dependent obscured fractions rests entirely on the Wada (2015) prescription, which assumes that a torus always exists and that its covering factor decreases with AGN luminosity. If at z~2-3 the circumnuclear material is transient, or if the covering factor is not a strong function of luminosity, the long-lived-torus curves in Figs. 5-6 and 8 would lose their advantage. This is a load-bearing assumption for one of the paper's two main alternatives. The paper should at least test the sensitivity to the torus prescription, e.g., by varying the luminosity dependence of the covering factor or using a constant covering factor. In addition, the absolute CTK number densities in Fig. 11 are not compared to empirical CTK luminosity functions or CTK number-density constraints; such a comparison is needed before the tor
minor comments (4)
  1. [Fig. 3 caption / Sec. 4.1] The caption says 'long-dashed red lines refer to the model variants with luminosity-dependent visibility window', while the text says 'the blue solid lines show the predictions of the same models with a fine-tuned luminosity dependency'. This is inconsistent and confusing; please clarify which curves correspond to the constant and luminosity-dependent cases.
  2. [Sec. 3.2.1, Eq. (4)] Equation (4) contains (L_lim/L_peak)^alpha, which becomes larger than unity for L_peak < L_lim, making the bracket negative. The subsequent floor of 10^7 yr presumably prevents unphysical values, but the domain of applicability of the formula should be stated explicitly.
  3. [Sec. 5.1] The text refers to 'predicted CTN/CTK LCs'; this should be 'luminosity functions' or 'LF contributions', as the figure shows number densities versus luminosity.
  4. [Sec. 6, last bullet] Typo: 'some data dets' should be 'some data sets'.

Circularity Check

2 steps flagged · score 6.0 of 10

Partial circularity: the luminosity-dependent visibility window and Model 3 CTK/CTN duty-cycle are calibrated to U14/A19 and then reported as successful matches; the torus luminosity dependence is inherited from Wada (2015) rather than independently derived.

  1. fitted input called prediction [Sec. 3.2.1, Eqs. (4)-(5); results in Sec. 4.1, Fig. 3]
    "The form and choice of parameters for the luminosity-dependent expressions of ΔτQSO given above have been empirically calibrated via trial and error to produce an improved match to the fractions of obscured AGN measured by U14 and A19, which sharply drop with increasing AGN luminosity."

    The parameter ΔτQSO(L_peak) directly sets the duty cycle of optically/UV-visible AGN. Calibrating Eqs. (4)-(5) to the U14/A19 obscured fractions and then presenting Models 1-4 with these windows as 'a good match to the U14;A19 data' (Sec. 4.1) is a fit, not an independent prediction. The decreasing obscured fraction with luminosity is introduced by hand; the match is thus guaranteed by construction for the data used in the calibration.

  2. fitted input called prediction [Sec. 3.2, Model 3 definition; Sec. 4.1, Fig. 4]
    "We assume that the CTK and CTN phases last, respectively, 1/3 and 2/3 of the whole pre-peak duration of the LC, to ensure that at least 30% of CTK AGN are generated, in line with the measurements by U14 and A19, as further detailed below."

    In Model 3 the fraction of the LC spent in CTK vs CTN phases is chosen to produce at least 30% CTK AGN, i.e., to match U14/A19. Since the phase durations translate directly into the predicted CTK/CTN fractions, the agreement displayed in Fig. 4 is a consequence of this input choice. The text confirms: 'Our choice of reserving 1/3 and 2/3 of the LC in Model 3 to, respectively, the CTK and CTN phases, is simply to broadly align the model predictions with the observed fractions of CTK/CTN AGN.'

full rationale

The paper contains two clear cases where a parameter is fitted to the same U14/A19 obscured fractions it is later said to reproduce: the luminosity-dependent visibility window of Eqs. (4)-(5), explicitly 'empirically calibrated via trial and error' to U14/A19, and the Model 3 CTK/CTN 1/3-2/3 duty cycle, explicitly chosen to generate at least 30% CTK AGN 'in line with the measurements by U14 and A19.' These are not independent predictions; they are calibrated inputs presented as successful matches. The core negative result — that pure Evolution models with extended post-peak phases underproduce obscured AGN — is not circular, since it uses fixed LC shapes and a constant ΔτQSO and does not require the obscured-fraction data as input. The long-lived torus scenario is not circular in the same strict sense: its luminosity-dependent covering factor is imported from Wada (2015), an external model, rather than fitted to U14/A19. However, the 'natural boost' of luminosity-dependent obscured fractions is inherited from that input assumption, so it weakens the claim that orientation effects are required, though it does not constitute a fitted-input circularity. Because the paper's central successful variants partly reduce to calibration to the target data, the overall circularity score is 6.

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

The central conclusions rest on several modeling choices inherited from GAEA and prior LC/torus prescriptions, plus explicit fine-tuning of the visibility window and CTK/CTN phase fractions. The luminosity-dependent visibility window is a fit to the target data, while the torus model is an external prescription. No new physical entities are introduced.

free parameters (5)
  • Luminosity-dependent visibility window parameters (alpha, L_lim, Delta_tau_QSO_min) = alpha=0.1, L_lim=10^45 erg/s, Delta_tau_QSO from 10^7 to 8x10^7 yr
    Eqs. 4 and 5 are explicitly calibrated via trial and error to match U14/A19 obscured fractions; these are fit parameters, not predictions.
  • Model 3 CTK/CTN phase split = 1/3 of pre-peak phase CTK, 2/3 CTN
    Chosen to ensure at least 30% CTK AGN, in line with U14 and A19 measurements, as stated in Section 3.2.
  • Gas disc compactness ratio N = 0.3
    R_d,gas = N R_d,star, preferred in Paper I to match CTN fractions and adopted here, although some observed support exists.
  • Starburst SFR thresholds = SFR>100 M_sun/yr, SFR>4x MS, SFR>MS
    Ad hoc thresholds used in Section 4.5 to define CTK sources; the choice strongly affects the resulting CTK fractions.
  • Merger mass ratio thresholds = major merger ratio >1/3, minor 0.1-1/3
    Ad hoc thresholds used in Section 4.6 to assign CTK/CTN status to merger-triggered AGN.
assumptions (5)
  • domain assumption GAEA HQ11 model provides a reliable population of galaxies and SMBHs at z=1-3, calibrated to AGN bolometric LF and galaxy properties.
    Section 2.1: the entire comparison assumes the SAM is representative of the real AGN host population.
  • domain assumption The AGN light curve is an exponential rise followed by a Hopkins et al. (2006) power-law decline, with Eddington time 4.5e7 yr and radiative efficiency 0.15.
    Section 3.1, Eqs. 1-2: the LC shape is taken as input from prior hydrodynamical simulations.
  • domain assumption Obscuration phase and N_H are assigned solely by random time sampling within the LC, with N_H drawn uniformly in log(N_H) within each phase.
    Section 3.2: this bypasses geometry and gas content, a strong simplification for pure Evolution models.
  • domain assumption The Wada (2015) torus model: there is always enough circumnuclear material to form a torus, and torus thickness/opening angle decreases with AGN luminosity.
    Section 3.2.2: this drives the luminosity dependence in the torus variants and is essential to the claim that a torus naturally matches the data.
  • standard math Duras et al. (2020) bolometric correction converts bolometric luminosity to 2-10 keV intrinsic X-ray luminosity.
    Section 2.1: used to compare model predictions with X-ray samples, with alternative corrections noted.

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Cite this review

Pith. "Pith review of Characterizing the roles of transitory obscured phases and inner torus in shaping the fractions of obscured AGN at cosmic noon." pith.science (2026). https://pith.science/paper/RNBVQ3XO

@misc{pith2026250904553,
  author       = {Pith},
  title        = {Pith review of: Characterizing the roles of transitory obscured phases and inner torus in shaping the fractions of obscured AGN at cosmic noon},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/RNBVQ3XO}},
  note         = {Machine review of arXiv:2509.04553}
}
read the original abstract

The origin of obscuration in Active Galactic Nuclei (AGN) is still a matter of contention. It is unclear whether obscured AGN are primarily due to line-of-sight effects, a transitory, dust-enshrouded phase in galaxy evolution, or a combination of both. The role of an inner torus around the central SMBH also remains unclear in pure Evolution models. We use cosmological semi-analytic models and semi-empirical prescriptions to explore obscuration effects in AGN at 1<z<3. We consider a realistic object-by-object modelling of AGN evolution including different light curves (LCs) composed of phases of varying levels of obscuration, mimicking the possible clearing effects of strong AGN feedback. Evolution models characterized by AGN LCs with relatively short pre-peak obscured phases followed by more extended optical/UV visible post-peak phases, struggle to reproduce the high fraction of obscured AGN at z~2-3 inferred from X-ray surveys. Evolution models characterised by LCs with sharp post-peak declines or persistent or multiple obscuration phases are more successful, although they still face challenges in reproducing the steady drop in the fractions of obscured AGN with increasing luminosity measured by some groups. Invoking a fine-tuning in the input LCs, with more luminous AGN defined by longer optical/UV visible windows, can improve the match to the decreasing fractions of obscured AGN with luminosity. Alternatively, a long-lived central torus-like component, with thickness decreasing with increasing AGN power, naturally boosts the luminosity-dependent fractions of obscured AGN, suggesting that small-scale orientation effects may still represent a key component even in Evolution models. We also find that in our models major mergers and starbursts, when considered in isolation, fall short in accounting for the large fractions of highly obscured faint AGN detected at cosmic noon.

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Cited by 1 Pith paper

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Reference graph

Works this paper leans on

171 extracted references · 34 canonical work pages · cited by 1 Pith paper

  1. [1]

    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.state := if if FUNCTION not #0 #1 if FUNCTION and 'skip pop #0 if FUNCTION or pop #1...

  2. [2]

    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.state := if if FUNCTION not #0 #1 if FUNCTION and 'skip pop #0 if FUNCTION or pop #1...

  3. [3]

    Afonso J., Hopkins A., Mobasher B., Almeida C., 2003, @doi [ ] 10.1086/378256 , https://ui.adsabs.harvard.edu/abs/2003ApJ...597..269A 597, 269

    work page doi:10.1086/378256 2003

  4. [4]

    L., Georgakakis A., Nandra K., Barro G., P \'e rez-Gonz \'a lez P

    Aird J., Coil A. L., Georgakakis A., Nandra K., Barro G., P \'e rez-Gonz \'a lez P. G., 2015, @doi [ ] 10.1093/mnras/stv1062 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.451.1892A 451, 1892

    doi:10.1093/mnras/stv1062 2015

  5. [5]

    B., et al., 2023, @doi [ ] 10.3847/1538-4357/acef21 , https://ui.adsabs.harvard.edu/abs/2023ApJ...956...61A 956, 61

    Akins H. B., et al., 2023, @doi [ ] 10.3847/1538-4357/acef21 , https://ui.adsabs.harvard.edu/abs/2023ApJ...956...61A 956, 61

    doi:10.3847/1538-4357/acef21 2023

  6. [6]

    B., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2406.10341 , https://ui.adsabs.harvard.edu/abs/2024arXiv240610341A p

    Akins H. B., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2406.10341 , https://ui.adsabs.harvard.edu/abs/2024arXiv240610341A p. arXiv:2406.10341

    arXiv doi:10.48550/arxiv.2406.10341 2024

  7. [7]

    M., Hickox R

    Alexander D. M., Hickox R. C., 2012, @doi [ ] 10.1016/j.newar.2011.11.003 , https://ui.adsabs.harvard.edu/abs/2012NewAR..56...93A 56, 93

    doi:10.1016/j.newar.2011.11.003 2012

  8. [8]

    M., Bauer F

    Alexander D. M., Bauer F. E., Chapman S. C., Smail I., Blain A. W., Brandt W. N., Ivison R. J., 2005, @doi [ ] 10.1086/444342 , https://ui.adsabs.harvard.edu/abs/2005ApJ...632..736A 632, 736

    doi:10.1086/444342 2005

Show all 171 references
  1. [9]

    M., et al., 2016, @doi [ ] 10.1093/mnras/stw1509 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.461.2944A 461, 2944

    Alexander D. M., et al., 2016, @doi [ ] 10.1093/mnras/stw1509 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.461.2944A 461, 2944

    2016 doi

  2. [10]

    V., et al., 2024, @doi [ ] 10.1093/mnras/stad3265 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.52710878A 527, 10878

    Alonso-Tetilla A. V., et al., 2024, @doi [ ] 10.1093/mnras/stad3265 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.52710878A 527, 10878

    2024 doi

  3. [11]

    T., et al., 2019, @doi [ ] 10.3847/1538-4357/aafb77 , https://ui.adsabs.harvard.edu/abs/2019ApJ...871..240A 871, 240

    Ananna T. T., et al., 2019, @doi [ ] 10.3847/1538-4357/aafb77 , https://ui.adsabs.harvard.edu/abs/2019ApJ...871..240A 871, 240

    2019 doi

  4. [12]

    Andonie C., et al., 2024, @doi [ ] 10.1093/mnrasl/slad144 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.527L.144A 527, L144

    2024 doi

  5. [13]

    Antonucci R., 1993, @doi [ ] 10.1146/annurev.aa.31.090193.002353 , https://ui.adsabs.harvard.edu/abs/1993ARA&A..31..473A 31, 473

    1993

  6. [14]

    Armus L., Heckman T., Miley G., 1987, @doi [ ] 10.1086/114517 , https://ui.adsabs.harvard.edu/abs/1987AJ.....94..831A 94, 831

    1987 doi

  7. [15]

    Aversa R., Lapi A., de Zotti G., Shankar F., Danese L., 2015, @doi [ ] 10.1088/0004-637X/810/1/74 , https://ui.adsabs.harvard.edu/abs/2015ApJ...810...74A 810, 74

    2015 doi

  8. [16]

    Baggen J. F. W., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2408.07745 , https://ui.adsabs.harvard.edu/abs/2024arXiv240807745B p. arXiv:2408.07745

    2024 doi arXiv

  9. [17]

    Banerji M., et al., 2015, @doi [ ] 10.1093/mnras/stv1881 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.454..419B 454, 419

    2015 doi

  10. [18]

    Barro G., et al., 2017, @doi [ ] 10.3847/1538-4357/aa6b05 , https://ui.adsabs.harvard.edu/abs/2017ApJ...840...47B 840, 47

    2017 doi

  11. [19]

    J., Filippenko A

    Barth A. J., Filippenko A. V., Moran E. C., 1999, @doi [ ] 10.1086/307941 , https://ui.adsabs.harvard.edu/abs/1999ApJ...525..673B 525, 673

    1999 doi

  12. [20]

    R., 2022, @doi [ ] 10.1093/mnras/stac1391 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.514.2145B 514, 2145

    Bate M. R., 2022, @doi [ ] 10.1093/mnras/stac1391 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.514.2145B 514, 2145

    2022 doi

  13. [21]

    B., et al., 2020, @doi [Nature Astronomy] 10.1038/s41550-019-0888-7 , https://ui.adsabs.harvard.edu/abs/2020NatAs...4..159B 4, 159

    Bayliss M. B., et al., 2020, @doi [Nature Astronomy] 10.1038/s41550-019-0888-7 , https://ui.adsabs.harvard.edu/abs/2020NatAs...4..159B 4, 159

    2020 doi

  14. [22]

    W., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2401.17277 , https://ui.adsabs.harvard.edu/abs/2024arXiv240117277B p

    Bickley R. W., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2401.17277 , https://ui.adsabs.harvard.edu/abs/2024arXiv240117277B p. arXiv:2401.17277

    2024 doi arXiv

  15. [23]

    arXiv:2503.15323

    Bisigello L., et al., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2503.15323 , https://ui.adsabs.harvard.edu/abs/2025arXiv250315323E p. arXiv:2503.15323

    2025 doi

  16. [24]

    Bl \'a nquez-Ses \'e D., et al., 2023, @doi [ ] 10.1051/0004-6361/202345977 , https://ui.adsabs.harvard.edu/abs/2023A&A...674A.166B 674, A166

    2023 doi

  17. [25]

    Bluck A. F. L., Piotrowska J. M., Maiolino R., 2023, @doi [ ] 10.3847/1538-4357/acac7c , https://ui.adsabs.harvard.edu/abs/2023ApJ...944..108B 944, 108

    2023 doi

  18. [27]

    G., et al., 2025, @doi [ ] 10.3847/1538-4357/ad8236 , https://ui.adsabs.harvard.edu/abs/2025ApJ...978..118B 978, 118

    Boorman P. G., et al., 2025, @doi [ ] 10.3847/1538-4357/ad8236 , https://ui.adsabs.harvard.edu/abs/2025ApJ...978..118B 978, 118

    2025 doi

  19. [28]

    arXiv:2503.22543

    Bosi M., et al., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2503.22543 , https://ui.adsabs.harvard.edu/abs/2025arXiv250322543B p. arXiv:2503.22543

    2025 doi arXiv

  20. [29]

    N., Hasinger G., 2005, @doi [ ] 10.1146/annurev.astro.43.051804.102213 , https://ui.adsabs.harvard.edu/abs/2005ARA&A..43..827B 43, 827

    Brandt W. N., Hasinger G., 2005, @doi [ ] 10.1146/annurev.astro.43.051804.102213 , https://ui.adsabs.harvard.edu/abs/2005ARA&A..43..827B 43, 827

    2005 arXiv

  21. [30]

    Buchner J., et al., 2015, @doi [ ] 10.1088/0004-637X/802/2/89 , https://ui.adsabs.harvard.edu/abs/2015ApJ...802...89B 802, 89

    2015 doi

  22. [31]

    E., 2017, @doi [ ] 10.1093/mnras/stw2423 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.464.4545B 464, 4545

    Buchner J., Schulze S., Bauer F. E., 2017, @doi [ ] 10.1093/mnras/stw2423 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.464.4545B 464, 4545

    2017 doi

  23. [32]

    Burtscher L., et al., 2013, @doi [ ] 10.1051/0004-6361/201321890 , https://ui.adsabs.harvard.edu/abs/2013A&A...558A.149B 558, A149

    2013 doi

  24. [33]

    Carraro R., et al., 2020, @doi [ ] 10.1051/0004-6361/201936649 , https://ui.adsabs.harvard.edu/abs/2020A&A...642A..65C 642, A65

    2020 doi

  25. [34]

    H., Pastoriza M

    Cezar P. H., Pastoriza M. G., Riffel R., Ramos Almeida C., Krabbe A. C., Rembold S. B., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2405.19960 , https://ui.adsabs.harvard.edu/abs/2024arXiv240519960C p. arXiv:2405.19960

    2024 doi arXiv

  26. [35]

    J., et al., 2015, @doi [ ] 10.1088/0004-637X/802/1/50 , https://ui.adsabs.harvard.edu/abs/2015ApJ...802...50C 802, 50

    Chen C.-T. J., et al., 2015, @doi [ ] 10.1088/0004-637X/802/1/50 , https://ui.adsabs.harvard.edu/abs/2015ApJ...802...50C 802, 50

    2015 doi

  27. [36]

    Combes F., et al., 2019, @doi [ ] 10.1051/0004-6361/201834560 , https://ui.adsabs.harvard.edu/abs/2019A&A...623A..79C 623, A79

    2019 doi

  28. [37]

    J., Mundy C

    Conselice C. J., Mundy C. J., Ferreira L., Duncan K., 2022, @doi [ ] 10.3847/1538-4357/ac9b1a , https://ui.adsabs.harvard.edu/abs/2022ApJ...940..168C 940, 168

    2022 doi

  29. [40]

    S., Helmi A., Navarro J

    De Lucia G., Tornatore L., Frenk C. S., Helmi A., Navarro J. F., White S. D. M., 2014, @doi [ ] 10.1093/mnras/stu1752 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.445..970D 445, 970

    2014 doi

  30. [41]

    Di Matteo T., Springel V., Hernquist L., 2005, @doi [ ] 10.1038/nature03335 , https://ui.adsabs.harvard.edu/abs/2005Natur.433..604D 433, 604

    2005 doi

  31. [42]

    L., Semelin B., 2008, @doi [ ] 10.1051/0004-6361:200809480 , https://ui.adsabs.harvard.edu/abs/2008A&A...492...31D 492, 31

    Di Matteo P., Bournaud F., Martig M., Combes F., Melchior A. L., Semelin B., 2008, @doi [ ] 10.1051/0004-6361:200809480 , https://ui.adsabs.harvard.edu/abs/2008A&A...492...31D 492, 31

    2008 doi

  32. [43]

    Duras F., et al., 2020, @doi [ ] 10.1051/0004-6361/201936817 , https://ui.adsabs.harvard.edu/abs/2020A&A...636A..73D 636, A73

    2020 doi

  33. [44]

    C., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2406.10329 , https://ui.adsabs.harvard.edu/abs/2024arXiv240610329D p

    Durodola E., Pacucci F., Hickox R. C., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2406.10329 , https://ui.adsabs.harvard.edu/abs/2024arXiv240610329D p. arXiv:2406.10329

    2024 doi arXiv

  34. [45]

    arXiv:2403.07986

    Eilers A.-C., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2403.07986 , https://ui.adsabs.harvard.edu/abs/2024arXiv240307986E p. arXiv:2403.07986

    2024 doi arXiv

  35. [46]

    L., Mendel J

    Ellison S. L., Mendel J. T., Patton D. R., Scudder J. M., 2013, @doi [ ] 10.1093/mnras/stt1562 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.435.3627E 435, 3627

    2013 doi

  36. [47]

    arXiv:2503.15317

    Euclid Collaboration et al., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2503.15317 , https://ui.adsabs.harvard.edu/abs/2025arXiv250315317E p. arXiv:2503.15317

    2025 doi arXiv

  37. [49]

    Fontanot F., et al., 2020, @doi [ ] 10.1093/mnras/staa1716 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.496.3943F 496, 3943

    2020 doi

  38. [50]

    F., et al., 2016, @doi [ ] 10.3847/2041-8205/829/1/L7 , https://ui.adsabs.harvard.edu/abs/2016ApJ...829L...7G 829, L7

    Gallimore J. F., et al., 2016, @doi [ ] 10.3847/2041-8205/829/1/L7 , https://ui.adsabs.harvard.edu/abs/2016ApJ...829L...7G 829, L7

    2016 doi

  39. [51]

    G \'a mez Rosas V., et al., 2022, @doi [ ] 10.1038/s41586-021-04311-7 , https://ui.adsabs.harvard.edu/abs/2022Natur.602..403G 602, 403

    2022 doi

  40. [52]

    Gao F., et al., 2020, @doi [ ] 10.1051/0004-6361/201937178 , https://ui.adsabs.harvard.edu/abs/2020A&A...637A..94G 637, A94

    2020 doi

  41. [53]

    Garc \' a-Burillo S., et al., 2016, @doi [ ] 10.3847/2041-8205/823/1/L12 , https://ui.adsabs.harvard.edu/abs/2016ApJ...823L..12G 823, L12

    2016 doi

  42. [54]

    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

  43. [55]

    Garc \' a-Burillo S., et al., 2021, @doi [ ] 10.1051/0004-6361/202141075 , https://ui.adsabs.harvard.edu/abs/2021A&A...652A..98G 652, A98

    2021 doi

  44. [56]

    Garc \' a-Burillo S., et al., 2024, @doi [ ] 10.1051/0004-6361/202450268 , https://ui.adsabs.harvard.edu/abs/2024A&A...689A.347G 689, A347

    2024 doi

  45. [57]

    Georgantopoulos I., Pouliasis E., Mountrichas G., Van der Wel A., Marchesi S., Lanzuisi G., 2023, @doi [ ] 10.1051/0004-6361/202244875 , https://ui.adsabs.harvard.edu/abs/2023A&A...673A..67G 673, A67

    2023 doi

  46. [58]

    Giacconi R., 2009, @doi [Experimental Astronomy] 10.1007/s10686-009-9139-8 , https://ui.adsabs.harvard.edu/abs/2009ExA....25..143G 25, 143

    2009 doi

  47. [59]

    Gilli R., Comastri A., Hasinger G., 2007, @doi [ ] 10.1051/0004-6361:20066334 , https://ui.adsabs.harvard.edu/abs/2007A&A...463...79G 463, 79

    2007 doi

  48. [60]

    Gilli R., et al., 2014, @doi [ ] 10.1051/0004-6361/201322892 , https://ui.adsabs.harvard.edu/abs/2014A&A...562A..67G 562, A67

    2014 doi

  49. [61]

    arXiv:2206.03508

    Gilli R., et al., 2022, arXiv e-prints, https://ui.adsabs.harvard.edu/abs/2022arXiv220603508G p. arXiv:2206.03508

    2022 arXiv

  50. [62]

    L., De Zotti G., Silva L., Bressan A., Danese L., 2004, @doi [ ] 10.1086/379875 , https://ui.adsabs.harvard.edu/abs/2004ApJ...600..580G 600, 580

    Granato G. L., De Zotti G., Silva L., Bressan A., Danese L., 2004, @doi [ ] 10.1086/379875 , https://ui.adsabs.harvard.edu/abs/2004ApJ...600..580G 600, 580

    2004 doi

  51. [63]

    L., Silva L., Lapi A., Shankar F., De Zotti G., Danese L., 2006, @doi [ ] 10.1111/j.1745-3933.2006.00160.x , https://ui.adsabs.harvard.edu/abs/2006MNRAS.368L..72G 368, L72

    Granato G. L., Silva L., Lapi A., Shankar F., De Zotti G., Danese L., 2006, @doi [ ] 10.1111/j.1745-3933.2006.00160.x , https://ui.adsabs.harvard.edu/abs/2006MNRAS.368L..72G 368, L72

    2006

  52. [64]

    Greenwell C., Gandhi P., Stern D., Lansbury G., Mainieri V., Boorman P., Toba Y., 2024, @doi [ ] 10.1093/mnras/stad3964 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.52712065G 527, 12065

    2024 doi

  53. [65]

    Haiman Z., Hui L., 2001, @doi [ ] 10.1086/318330 , https://ui.adsabs.harvard.edu/abs/2001ApJ...547...27H 547, 27

    2001 doi

  54. [66]

    R., et al., 2020, @doi [Nature] 10.1038/s41586-020-2649-2 , 585, 357

    Harris C. R., et al., 2020, @doi [Nature] 10.1038/s41586-020-2649-2 , 585, 357

    2020 doi

  55. [67]

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

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

    2017 doi

  56. [68]

    F., et al., 2010, @doi [ ] 10.1088/0004-637X/719/2/1672 , https://ui.adsabs.harvard.edu/abs/2010ApJ...719.1672H 719, 1672

    Hennawi J. F., et al., 2010, @doi [ ] 10.1088/0004-637X/719/2/1672 , https://ui.adsabs.harvard.edu/abs/2010ApJ...719.1672H 719, 1672

    2010 doi

  57. [69]

    Hernquist L., Katz N., 1989, @doi [ ] 10.1086/191344 , https://ui.adsabs.harvard.edu/abs/1989ApJS...70..419H 70, 419

    1989 doi

  58. [70]

    C., Alexander D

    Hickox R. C., Alexander D. M., 2018, @doi [ ] 10.1146/annurev-astro-081817-051803 , https://ui.adsabs.harvard.edu/abs/2018ARA&A..56..625H 56, 625

    2018 doi

  59. [71]

    Hickox R., Carroll C., Yan W., Whalen K., 2020, in American Astronomical Society Meeting Abstracts \#235. p. 125.03

    2020

  60. [72]

    Hirschmann M., De Lucia G., Fontanot F., 2016, @doi [ ] 10.1093/mnras/stw1318 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.461.1760H 461, 1760

    2016 doi

  61. [73]

    A., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2407.15846 , https://ui.adsabs.harvard.edu/abs/2024arXiv240715846H p

    Hodge J. A., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2407.15846 , https://ui.adsabs.harvard.edu/abs/2024arXiv240715846H p. arXiv:2407.15846

    2024 doi arXiv

  62. [74]

    F., 2019, @doi [ ] 10.3847/1538-4357/ab4591 , https://ui.adsabs.harvard.edu/abs/2019ApJ...884..171H 884, 171

    H \"o nig S. F., 2019, @doi [ ] 10.3847/1538-4357/ab4591 , https://ui.adsabs.harvard.edu/abs/2019ApJ...884..171H 884, 171

    2019 doi

  63. [75]

    F., Kishimoto M., 2017, @doi [ ] 10.3847/2041-8213/aa6838 , https://ui.adsabs.harvard.edu/abs/2017ApJ...838L..20H 838, L20

    H \"o nig S. F., Kishimoto M., 2017, @doi [ ] 10.3847/2041-8213/aa6838 , https://ui.adsabs.harvard.edu/abs/2017ApJ...838L..20H 838, L20

    2017 doi

  64. [76]

    F., Hernquist L., 2010, @doi [ ] 10.1111/j.1365-2966.2009.15933.x , https://ui.adsabs.harvard.edu/abs/2010MNRAS.402..985H 402, 985

    Hopkins P. F., Hernquist L., 2010, @doi [ ] 10.1111/j.1365-2966.2009.15933.x , https://ui.adsabs.harvard.edu/abs/2010MNRAS.402..985H 402, 985

    2010

  65. [78]

    F., Hernquist L., Cox T

    Hopkins P. F., Hernquist L., Cox T. J., Di Matteo T., Robertson B., Springel V., 2006, @doi [ ] 10.1086/499298 , https://ui.adsabs.harvard.edu/abs/2006ApJS..163....1H 163, 1

    2006 doi

  66. [79]

    F., Richards G

    Hopkins P. F., Richards G. T., Hernquist L., 2007a, @doi [ ] 10.1086/509629 , https://ui.adsabs.harvard.edu/abs/2007ApJ...654..731H 654, 731

    doi

  67. [80]

    F., Lidz A., Hernquist L., Coil A

    Hopkins P. F., Lidz A., Hernquist L., Coil A. L., Myers A. D., Cox T. J., Spergel D. N., 2007b, @doi [ ] 10.1086/517512 , https://ui.adsabs.harvard.edu/abs/2007ApJ...662..110H 662, 110

    doi

  68. [81]

    F., Hernquist L., Cox T

    Hopkins P. F., Hernquist L., Cox T. J., Kere s D., 2008, @doi [ ] 10.1086/524362 , https://ui.adsabs.harvard.edu/abs/2008ApJS..175..356H 175, 356

    2008 doi

  69. [82]

    arXiv:2406.18207

    Iani E., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2406.18207 , https://ui.adsabs.harvard.edu/abs/2024arXiv240618207I p. arXiv:2406.18207

    2024 doi arXiv

  70. [83]

    Imanishi M., Nakanishi K., Izumi T., 2016, @doi [ ] 10.3847/2041-8205/822/1/L10 , https://ui.adsabs.harvard.edu/abs/2016ApJ...822L..10I 822, L10

    2016 doi

  71. [84]

    W., et al., 2022, @doi [ ] 10.1051/0004-6361/202243271 , https://ui.adsabs.harvard.edu/abs/2022A&A...663A..35I 663, A35

    Isbell J. W., et al., 2022, @doi [ ] 10.1051/0004-6361/202243271 , https://ui.adsabs.harvard.edu/abs/2022A&A...663A..35I 663, A35

    2022 doi

  72. [85]

    W., et al., 2023, @doi [ ] 10.1051/0004-6361/202347307 , https://ui.adsabs.harvard.edu/abs/2023A&A...678A.136I 678, A136

    Isbell J. W., et al., 2023, @doi [ ] 10.1051/0004-6361/202347307 , https://ui.adsabs.harvard.edu/abs/2023A&A...678A.136I 678, A136

    2023 doi

  73. [86]

    C., 2016, @doi [ ] 10.1093/mnras/stw2063 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.463.1291I 463, 1291

    Ishibashi W., Fabian A. C., 2016, @doi [ ] 10.1093/mnras/stw2063 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.463.1291I 463, 1291

    2016 doi

  74. [87]

    J., Keel W

    Kennicutt Robert C. J., Keel W. C., van der Hulst J. M., Hummel E., Roettiger K. A., 1987, @doi [ ] 10.1086/114384 , https://ui.adsabs.harvard.edu/abs/1987AJ.....93.1011K 93, 1011

    1987 doi

  75. [88]

    Y., Weedman D

    Khachikian E. Y., Weedman D. W., 1974, @doi [ ] 10.1086/153093 , https://ui.adsabs.harvard.edu/abs/1974ApJ...192..581K 192, 581

    1974 doi

  76. [89]

    H., Cisternas M., Querejeta M., 2015, @doi [ ] 10.1093/mnras/stv2135 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.454.1742K 454, 1742

    Knapen J. H., Cisternas M., Querejeta M., 2015, @doi [ ] 10.1093/mnras/stv2135 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.454.1742K 454, 1742

    2015 doi

  77. [90]

    D., et al., 2015, @doi [ ] 10.1088/0004-637X/814/2/104 , https://ui.adsabs.harvard.edu/abs/2015ApJ...814..104K 814, 104

    Kocevski D. D., et al., 2015, @doi [ ] 10.1088/0004-637X/814/2/104 , https://ui.adsabs.harvard.edu/abs/2015ApJ...814..104K 814, 104

    2015 doi

  78. [91]

    Kokorev V., et al., 2024, @doi [ ] 10.3847/1538-4357/ad4265 , https://ui.adsabs.harvard.edu/abs/2024ApJ...968...38K 968, 38

    2024 doi

  79. [92]

    arXiv:2504.08123

    Kovacevic N., et al., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2504.08123 , https://ui.adsabs.harvard.edu/abs/2025arXiv250408123K p. arXiv:2504.08123

    2025 doi

  80. [93]

    Kuhn L., et al., 2024, @doi [ ] 10.1051/0004-6361/202348138 , https://ui.adsabs.harvard.edu/abs/2024A&A...684A..52K 684, A52

    2024 doi

  81. [94]

    Kuraszkiewicz J., et al., 2021, @doi [ ] 10.3847/1538-4357/abf3c0 , https://ui.adsabs.harvard.edu/abs/2021ApJ...913..134K 913, 134

    2021 doi

  82. [95]

    Laloux B., et al., 2023, @doi [ ] 10.1093/mnras/stac3255 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.518.2546L 518, 2546

    2023 doi

  83. [96]

    Lanzuisi G., et al., 2015, @doi [ ] 10.1051/0004-6361/201424924 , https://ui.adsabs.harvard.edu/abs/2015A&A...573A.137L 573, A137

    2015 doi

  84. [97]

    Lapi A., Cavaliere A., Menci N., 2005, @doi [ ] 10.1086/42637610.48550/arXiv.astro-ph/0410028 , https://ui.adsabs.harvard.edu/abs/2005ApJ...619...60L 619, 60

    2005

  85. [98]

    L., Silva L., De Zotti G., Danese L., 2006, @doi [ ] 10.1086/507122 , https://ui.adsabs.harvard.edu/abs/2006ApJ...650...42L 650, 42

    Lapi A., Shankar F., Mao J., Granato G. L., Silva L., De Zotti G., Danese L., 2006, @doi [ ] 10.1086/507122 , https://ui.adsabs.harvard.edu/abs/2006ApJ...650...42L 650, 42

    2006 doi

  86. [99]

    Y., Negrello M., Celotti A., De Zotti G., Danese L., 2014, @doi [ ] 10.1088/0004-637X/782/2/69 , https://ui.adsabs.harvard.edu/abs/2014ApJ...782...69L 782, 69

    Lapi A., Raimundo S., Aversa R., Cai Z. Y., Negrello M., Celotti A., De Zotti G., Danese L., 2014, @doi [ ] 10.1088/0004-637X/782/2/69 , https://ui.adsabs.harvard.edu/abs/2014ApJ...782...69L 782, 69

    2014 doi

  87. [100]

    Lapiner S., et al., 2023, @doi [ ] 10.1093/mnras/stad1263 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.522.4515L 522, 4515

    2023 doi

  88. [101]

    Lim C.-F., et al., 2020, @doi [ ] 10.3847/1538-4357/ab607f , https://ui.adsabs.harvard.edu/abs/2020ApJ...889...80L 889, 80

    2020 doi

  89. [102]

    T., Mihos J

    Linden S. T., Mihos J. C., 2022, @doi [ ] 10.3847/2041-8213/ac7c06 , https://ui.adsabs.harvard.edu/abs/2022ApJ...933L..33L 933, L33

    2022 doi

  90. [103]

    Liu Z., et al., 2024, @doi [ ] 10.3847/1538-4357/ad4096 , https://ui.adsabs.harvard.edu/abs/2024ApJ...968...15L 968, 15

    2024 doi

  91. [104]

    L \'o pez-Gonzaga N., Burtscher L., Tristram K. R. W., Meisenheimer K., Schartmann M., 2016, @doi [ ] 10.1051/0004-6361/201527590 , https://ui.adsabs.harvard.edu/abs/2016A&A...591A..47L 591, A47

    2016 doi

  92. [105]

    arXiv:2406.11571

    Lyu Y., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2406.11571 , https://ui.adsabs.harvard.edu/abs/2024arXiv240611571L p. arXiv:2406.11571

    2024 doi arXiv

  93. [106]

    arXiv:2504.08032

    Ma Y., et al., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2504.08032 , https://ui.adsabs.harvard.edu/abs/2025arXiv250408032M p. arXiv:2504.08032

    2025 doi arXiv

  94. [107]

    Madau P., Dickinson M., 2014, @doi [ ] 10.1146/annurev-astro-081811-125615 , https://ui.adsabs.harvard.edu/abs/2014ARA&A..52..415M 52, 415

    2014 doi

  95. [108]

    Magnelli B., et al., 2023, @doi [ ] 10.1051/0004-6361/202347052 , https://ui.adsabs.harvard.edu/abs/2023A&A...678A..83M 678, A83

    2023 doi

  96. [109]

    arXiv:2405.00504

    Maiolino R., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2405.00504 , https://ui.adsabs.harvard.edu/abs/2024arXiv240500504M p. arXiv:2405.00504

    2024 doi arXiv

  97. [110]

    Marchesi S., Ajello M., Marcotulli L., Comastri A., Lanzuisi G., Vignali C., 2018, The Astrophysical Journal, 854, 49

    2018

  98. [112]

    G., Krumpe M., Nikutta R., 2014, @doi [ ] 10.1093/mnras/stt2492 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.439.1403M 439, 1403

    Markowitz A. G., Krumpe M., Nikutta R., 2014, @doi [ ] 10.1093/mnras/stt2492 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.439.1403M 439, 1403

    2014 doi

  99. [113]

    C., ed., Coevolution of Black Holes and Galaxies

    Martini P., 2004, in Ho L. C., ed., Coevolution of Black Holes and Galaxies. p. 169 ( @eprint arXiv astro-ph/0304009 ), @doi 10.48550/arXiv.astro-ph/0304009

    2004 doi arXiv

  100. [114]

    H., 2001, @doi [ ] 10.1086/318331 , https://ui.adsabs.harvard.edu/abs/2001ApJ...547...12M 547, 12

    Martini P., Weinberg D. H., 2001, @doi [ ] 10.1086/318331 , https://ui.adsabs.harvard.edu/abs/2001ApJ...547...12M 547, 12

    2001 doi

  101. [115]

    Marulli F., Bonoli S., Branchini E., Moscardini L., Springel V., 2008, @doi [ ] 10.1111/j.1365-2966.2008.12988.x , https://ui.adsabs.harvard.edu/abs/2008MNRAS.385.1846M 385, 1846

    2008

  102. [116]

    Matthee J., et al., 2024, @doi [ ] 10.3847/1538-4357/ad2345 , https://ui.adsabs.harvard.edu/abs/2024ApJ...963..129M 963, 129

    2024 doi

  103. [117]

    Menci N., Fiore F., Feruglio C., Lamastra A., Shankar F., Piconcelli E., Giallongo E., Grazian A., 2019, @doi [ ] 10.3847/1538-4357/ab1a3a , https://ui.adsabs.harvard.edu/abs/2019ApJ...877...74M 877, 74

    2019 doi

  104. [118]

    Merloni A., et al., 2014, @doi [ ] 10.1093/mnras/stt2149 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.437.3550M 437, 3550

    2014 doi

  105. [119]

    C., Hernquist L., 1996, @doi [ ] 10.1086/177353 , https://ui.adsabs.harvard.edu/abs/1996ApJ...464..641M 464, 641

    Mihos J. C., Hernquist L., 1996, @doi [ ] 10.1086/177353 , https://ui.adsabs.harvard.edu/abs/1996ApJ...464..641M 464, 641

    1996 doi

  106. [121]

    Monaco P., Fontanot F., Taffoni G., 2007, @doi [ ] 10.1111/j.1365-2966.2006.11253.x , https://ui.adsabs.harvard.edu/abs/2007MNRAS.375.1189M 375, 1189

    2007

  107. [122]

    L., Patton D

    Moreno J., Torrey P., Ellison S. L., Patton D. R., Bluck A. F. L., Bansal G., Hernquist L., 2015, @doi [ ] 10.1093/mnras/stv094 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.448.1107M 448, 1107

    2015 doi

  108. [123]

    Mountrichas G., Shankar F., 2023, @doi [ ] 10.1093/mnras/stac3211 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.518.2088M 518, 2088

    2023 doi

  109. [124]

    Mountrichas G., Siudek M., Cucciati O., 2024, @doi [ ] 10.1051/0004-6361/202348763 , https://ui.adsabs.harvard.edu/abs/2024A&A...686A.229M 686, A229

    2024 doi

  110. [125]

    R., et al., 2015, @doi [ ] 10.1093/mnrasl/slv110 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.453L..83M 453, L83

    Mullaney J. R., et al., 2015, @doi [ ] 10.1093/mnrasl/slv110 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.453L..83M 453, L83

    2015 doi

  111. [126]

    S., Murayama T., Ohyama Y., Taniguchi Y., Sumiya R., Sasaki S

    Nagao T., Kawabata K. S., Murayama T., Ohyama Y., Taniguchi Y., Sumiya R., Sasaki S. S., 2004, @doi [ ] 10.1086/421740 , https://ui.adsabs.harvard.edu/abs/2004AJ....128..109N 128, 109

    2004 doi

  112. [127]

    Netzer H., 2015, @doi [ ] 10.1146/annurev-astro-082214-122302 , https://ui.adsabs.harvard.edu/abs/2015ARA&A..53..365N 53, 365

    2015 doi

  113. [128]

    T., Roche P

    Packham C., Radomski J. T., Roche P. F., Aitken D. K., Perlman E., Alonso-Herrero A., Colina L., Telesco C. M., 2005, @doi [ ] 10.1086/427691 , https://ui.adsabs.harvard.edu/abs/2005ApJ...618L..17P 618, L17

    2005 doi

  114. [129]

    Paolillo M., et al., 2023, @doi [ ] 10.1051/0004-6361/202245291 , https://ui.adsabs.harvard.edu/abs/2023A&A...673A..68P 673, A68

    2023 doi

  115. [130]

    Parlanti E., et al., 2024, @doi [ ] 10.1051/0004-6361/202347914 , https://ui.adsabs.harvard.edu/abs/2024A&A...684A..24P 684, A24

    2024 doi

  116. [131]

    G., et al., 2024, @doi [ ] 10.3847/1538-4357/ad38bb , https://ui.adsabs.harvard.edu/abs/2024ApJ...968....4P 968, 4

    P \'e rez-Gonz \'a lez P. G., et al., 2024, @doi [ ] 10.3847/1538-4357/ad38bb , https://ui.adsabs.harvard.edu/abs/2024ApJ...968....4P 968, 4

    2024 doi

  117. [132]

    M., 1997, An Introduction to Active Galactic Nuclei

    Peterson B. M., 1997, An Introduction to Active Galactic Nuclei

    1997

  118. [133]

    C., Hickox R

    Petter G. C., Hickox R. C., Alexander D. M., Myers A. D., Geach J. E., Whalen K. E., Andonie C. P., 2023, @doi [ ] 10.3847/1538-4357/acb7ef , https://ui.adsabs.harvard.edu/abs/2023ApJ...946...27P 946, 27

    2023 doi

  119. [134]

    Pierce J. C. S., et al., 2023, @doi [ ] 10.1093/mnras/stad455 , https://ui.adsabs.harvard.edu/abs/2023MNRAS.522.1736P 522, 1736

    2023 doi

  120. [135]

    arXiv:2403.12140

    Pizzati E., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2403.12140 , https://ui.adsabs.harvard.edu/abs/2024arXiv240312140P p. arXiv:2403.12140

    2024 doi arXiv

  121. [136]

    Polletta M., Courvoisier T. J. L., 1999, in Cox P., Kessler M., eds, ESA Special Publication Vol. 427, The Universe as Seen by ISO. p. 953

    1999

  122. [137]

    Polletta M., et al., 2008, @doi [ ] 10.1051/0004-6361:200810345 , https://ui.adsabs.harvard.edu/abs/2008A&A...492...81P 492, 81

    2008 doi

  123. [138]

    Polletta M., Nesvadba N. P. H., Neri R., Omont A., Berta S., Bergeron J., 2011, @doi [ ] 10.1051/0004-6361/201116446 , https://ui.adsabs.harvard.edu/abs/2011A&A...533A..20P 533, A20

    2011 doi

  124. [139]

    arXiv:2405.07986

    Polletta M., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2405.07986 , https://ui.adsabs.harvard.edu/abs/2024arXiv240507986P p. arXiv:2405.07986

    2024 doi arXiv

  125. [140]

    arXiv:2401.13515

    Pouliasis E., et al., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2401.13515 , https://ui.adsabs.harvard.edu/abs/2024arXiv240113515P p. arXiv:2401.13515

    2024 doi arXiv

  126. [141]

    Pozzi F., et al., 2024, @doi [ ] 10.1051/0004-6361/202348996 , https://ui.adsabs.harvard.edu/abs/2024A&A...686A.187P 686, A187

    2024 doi

  127. [142]

    H., et al., 2025, @doi [ ] 10.3847/1538-4357/ada0b1 , https://ui.adsabs.harvard.edu/abs/2025ApJ...980...11P 980, 11

    Price S. H., et al., 2025, @doi [ ] 10.3847/1538-4357/ada0b1 , https://ui.adsabs.harvard.edu/abs/2025ApJ...980...11P 980, 11

    2025 doi

  128. [143]

    Puglisi A., et al., 2019, @doi [ ] 10.3847/2041-8213/ab1f92 , https://ui.adsabs.harvard.edu/abs/2019ApJ...877L..23P 877, L23

    2019 doi

  129. [144]

    Puglisi A., et al., 2021, @doi [ ] 10.1093/mnras/stab2914 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.508.5217P 508, 5217

    2021 doi

  130. [145]

    T., et al., 2008, @doi [ ] 10.1086/587771 , https://ui.adsabs.harvard.edu/abs/2008ApJ...681..141R 681, 141

    Radomski J. T., et al., 2008, @doi [ ] 10.1086/587771 , https://ui.adsabs.harvard.edu/abs/2008ApJ...681..141R 681, 141

    2008 doi

  131. [146]

    Ramos Almeida C., Ricci C., 2017, @doi [Nature Astronomy] 10.1038/s41550-017-0232-z , https://ui.adsabs.harvard.edu/abs/2017NatAs...1..679R 1, 679

    2017 doi

  132. [147]

    M., Acosta-Pulido J

    Ramos Almeida C., P \'e rez Garc \' a A. M., Acosta-Pulido J. A., Gonz \'a lez-Mart \' n O., 2008, @doi [ ] 10.1086/589771 , https://ui.adsabs.harvard.edu/abs/2008ApJ...680L..17R 680, L17

    2008 doi

  133. [148]

    Ramos Almeida C., et al., 2009, @doi [ ] 10.1088/0004-637X/702/2/1127 , https://ui.adsabs.harvard.edu/abs/2009ApJ...702.1127R 702, 1127

    2009 doi

  134. [149]

    J., Hardcastle M

    Ramos Almeida C., Dicken D., Tadhunter C., Asensio Ramos A., Inskip K. J., Hardcastle M. J., Mingo B., 2011, @doi [ ] 10.1111/j.1365-2966.2011.18309.x10.48550/arXiv.1101.1868 , https://ui.adsabs.harvard.edu/abs/2011MNRAS.413.2358R 413, 2358

    2011

  135. [150]

    J., Asensio Ramos A., Acosta-Pulido J

    Ramos Almeida C., Mart \' nez Gonz \'a lez M. J., Asensio Ramos A., Acosta-Pulido J. A., H \"o nig S. F., Alonso-Herrero A., Tadhunter C. N., Gonz \'a lez-Mart \' n O., 2016, @doi [ ] 10.1093/mnras/stw1388 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.461.1387R 461, 1387

    2016 doi

  136. [151]

    Renaud F., Segovia Otero \'A ., Agertz O., 2022, @doi [ ] 10.1093/mnras/stac2557 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.516.4922R 516, 4922

    2022 doi

  137. [152]

    Ricci C., Trakhtenbrot B., 2023, @doi [Nature Astronomy] 10.1038/s41550-023-02108-4 , https://ui.adsabs.harvard.edu/abs/2023NatAs...7.1282R 7, 1282

    2023 doi

  138. [153]

    J., Trakhtenbrot B., Bauer F

    Ricci C., Ueda Y., Koss M. J., Trakhtenbrot B., Bauer F. E., Gandhi P., 2015, @doi [ ] 10.1088/2041-8205/815/1/L13 , https://ui.adsabs.harvard.edu/abs/2015ApJ...815L..13R 815, L13

    2015 doi

  139. [154]

    Ricci C., et al., 2017, @doi [ ] 10.1093/mnras/stx173 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.468.1273R 468, 1273

    2017 doi

  140. [155]

    Ricci F., et al., 2022a, @doi [ ] 10.3847/1538-4365/ac5b67 , https://ui.adsabs.harvard.edu/abs/2022ApJS..261....8R 261, 8

    doi

  141. [156]

    Ricci C., et al., 2022b, @doi [ ] 10.3847/1538-4357/ac8e67 , https://ui.adsabs.harvard.edu/abs/2022ApJ...938...67R 938, 67

    doi

  142. [157]

    Riccio G., et al., 2023, @doi [ ] 10.1051/0004-6361/202346857 , https://ui.adsabs.harvard.edu/abs/2023A&A...678A.164R 678, A164

    2023 doi

  143. [158]

    Richstone D., et al., 1998, @doi [ ] 10.48550/arXiv.astro-ph/9810378 , https://ui.adsabs.harvard.edu/abs/1998Natur.395A..14R 385, A14

    1998 doi arXiv

  144. [159]

    A., et al., 2013, @doi [ ] 10.1038/nature12050 , https://ui.adsabs.harvard.edu/abs/2013Natur.496..329R 496, 329

    Riechers D. A., et al., 2013, @doi [ ] 10.1038/nature12050 , https://ui.adsabs.harvard.edu/abs/2013Natur.496..329R 496, 329

    2013 doi

  145. [160]

    Risaliti G., Maiolino R., Salvati M., 1999, @doi [ ] 10.1086/307623 , https://ui.adsabs.harvard.edu/abs/1999ApJ...522..157R 522, 157

    1999 doi

  146. [161]

    Rodighiero G., et al., 2015, @doi [ ] 10.1088/2041-8205/800/1/L10 , https://ui.adsabs.harvard.edu/abs/2015ApJ...800L..10R 800, L10

    2015 doi

  147. [162]

    B., Mirabel I

    Sanders D. B., Mirabel I. F., 1996, @doi [ ] 10.1146/annurev.astro.34.1.749 , https://ui.adsabs.harvard.edu/abs/1996ARA&A..34..749S 34, 749

    1996 doi

  148. [163]

    B., Soifer B

    Sanders D. B., Soifer B. T., Elias J. H., Madore B. F., Matthews K., Neugebauer G., Scoville N. Z., 1988, @doi [ ] 10.1086/165983 , https://ui.adsabs.harvard.edu/abs/1988ApJ...325...74S 325, 74

    1988 doi

  149. [164]

    B., Phinney E

    Sanders D. B., Phinney E. S., Neugebauer G., Soifer B. T., Matthews K., 1989, @doi [ ] 10.1086/168094 , https://ui.adsabs.harvard.edu/abs/1989ApJ...347...29S 347, 29

    1989 doi

  150. [165]

    Santini P., et al., 2014, @doi [ ] 10.1051/0004-6361/201322835 , https://ui.adsabs.harvard.edu/abs/2014A&A...562A..30S 562, A30

    2014 doi

  151. [166]

    K., 1943, @doi [ ] 10.1086/144488 , https://ui.adsabs.harvard.edu/abs/1943ApJ....97...28S 97, 28

    Seyfert C. K., 1943, @doi [ ] 10.1086/144488 , https://ui.adsabs.harvard.edu/abs/1943ApJ....97...28S 97, 28

    1943 doi

  152. [167]

    Shankar F., 2009, @doi [Proceedings of the International Astronomical Union] 10.1017/S1743921310006356 , 5, 248–253

    2009 doi

  153. [168]

    L., De Zotti G., Danese L., 2004, @doi [ ] 10.1111/j.1365-2966.2004.08261.x , https://ui.adsabs.harvard.edu/abs/2004MNRAS.354.1020S 354, 1020

    Shankar F., Salucci P., Granato G. L., De Zotti G., Danese L., 2004, @doi [ ] 10.1111/j.1365-2966.2004.08261.x , https://ui.adsabs.harvard.edu/abs/2004MNRAS.354.1020S 354, 1020

    2004

  154. [169]

    R., 2008, @doi [ ] 10.1086/591488 , https://ui.adsabs.harvard.edu/abs/2008ApJ...687..859S 687, 859

    Shankar F., Dai X., Sivakoff G. R., 2008, @doi [ ] 10.1086/591488 , https://ui.adsabs.harvard.edu/abs/2008ApJ...687..859S 687, 859

    2008 doi

  155. [170]

    H., Miralda-Escud \'e J., 2009, @doi [ ] 10.1088/0004-637X/690/1/20 , https://ui.adsabs.harvard.edu/abs/2009ApJ...690...20S 690, 20

    Shankar F., Weinberg D. H., Miralda-Escud \'e J., 2009, @doi [ ] 10.1088/0004-637X/690/1/20 , https://ui.adsabs.harvard.edu/abs/2009ApJ...690...20S 690, 20

    2009 doi

  156. [171]

    H., Shen Y., 2010, @doi [ ] 10.1111/j.1365-2966.2010.16801.x , https://ui.adsabs.harvard.edu/abs/2010MNRAS.406.1959S 406, 1959

    Shankar F., Weinberg D. H., Shen Y., 2010, @doi [ ] 10.1111/j.1365-2966.2010.16801.x , https://ui.adsabs.harvard.edu/abs/2010MNRAS.406.1959S 406, 1959

    2010

  157. [172]

    Shankar F., Marulli F., Mathur S., Bernardi M., Bournaud F., 2012, @doi [ ] 10.1051/0004-6361/201118387 , https://ui.adsabs.harvard.edu/abs/2012A&A...540A..23S 540, A23

    2012 doi

  158. [173]

    H., Miralda-Escud \'e J., 2013, @doi [ ] 10.1093/mnras/sts026 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.428..421S 428, 421

    Shankar F., Weinberg D. H., Miralda-Escud \'e J., 2013, @doi [ ] 10.1093/mnras/sts026 , https://ui.adsabs.harvard.edu/abs/2013MNRAS.428..421S 428, 421

    2013 doi

  159. [174]

    Shen Y., 2009, @doi [ ] 10.1088/0004-637X/704/1/89 , https://ui.adsabs.harvard.edu/abs/2009ApJ...704...89S 704, 89

    2009 doi

  160. [175]

    Shen Y., et al., 2010, @doi [ ] 10.1088/0004-637X/719/2/1693 , https://ui.adsabs.harvard.edu/abs/2010ApJ...719.1693S 719, 1693

    2010 doi

  161. [176]

    F., Faucher-Gigu \`e re C.-A., Alexander D

    Shen X., Hopkins P. F., Faucher-Gigu \`e re C.-A., Alexander D. M., Richards G. T., Ross N. P., Hickox R. C., 2020, @doi [ ] 10.1093/mnras/staa1381 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.495.3252S 495, 3252

    2020 doi

  162. [177]

    Shen L., et al., 2023, @doi [ ] 10.3847/1538-4357/acc944 , https://ui.adsabs.harvard.edu/abs/2023ApJ...950....7S 950, 7

    2023 doi

  163. [178]

    D., Martis N., Iono D., Espada D., Skelton R., 2021, @doi [ ] 10.3847/1538-4357/abdbb1 , https://ui.adsabs.harvard.edu/abs/2021ApJ...909..124S 909, 124

    Silva A., Marchesini D., Silverman J. D., Martis N., Iono D., Espada D., Skelton R., 2021, @doi [ ] 10.3847/1538-4357/abdbb1 , https://ui.adsabs.harvard.edu/abs/2021ApJ...909..124S 909, 124

    2021 doi

Pith tools

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