Energy input from quasars regulates the growth and activity of black holes and their host galaxies

CMU); Lars Hernquist (Harvard); Tiziana Di Matteo (MPA; Volker Springel (MPA)

REVIEW

Energy input from quasars regulates the growth and activity of black holes and their host galaxies

Tiziana Di Matteo (MPA, CMU), Volker Springel (MPA), Lars Hernquist (Harvard)

Astrophysics · Submitted 9 Feb 2005 · 31 references

Pith's verdict: The landmark AGN-feedback merger simulation: the qualitative quenching result and the M_BH–σ slope hold up, but the ~100 Myr quasar lifetime is a model output the abstract dresses up as a determination.

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CitationCMU), Lars Hernquist (Harvard), Tiziana Di Matteo (MPA, Volker Springel (MPA). "Energy input from quasars regulates the growth and activity of black holes and their host galaxies." arXiv:astro-ph/0502199 (2005). https://pith.science/paper/7EHA7PNL

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Editor's note

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This is the paper that put AGN feedback into hydrodynamical galaxy formation as a working mechanism rather than a hand-wave, and it earns that place. The controlled comparison is the whole trick: same merger, same star formation and supernova physics, black hole growth and feedback switched on in one run and off in the other. The remnant with black holes ends up gas-poor, with accretion and star formation both quenched; the one without keeps a cold gas reservoir and keeps forming stars. That is a clean, interpretable result, and the six-mass, three-gas-fraction sweep landing near the observed M_BH–σ relation is more than a poster figure. Measuring σ as a line-of-sight dispersion within the effective radius, the way observers do, is the right instinct and makes the comparison meaningful rather than decorative. On the stress-test note: it is right, and it corrects the reader. The M_BH–σ normalization is not a circular fit to M_BH–σ. The black hole grows until f η M_BH c² can unbind the bulge gas, so M_BH,final ∝ 1/f, and f = 0.05 is fixed against an independent observable — the quasar number density Wyithe and Loeb needed. That is an anchor, not a fit. I would only trim the enthusiasm: 'consistent with' is a loose anchor, and the 1/f scaling makes the amplitude a one-parameter prediction, not a zero-parameter one. The slope and the existence of the correlation are genuinely not fitted, and that is the real content. Where I would push back on the paper: the abstract's 'This determines the lifetime of the quasar phase' is its weakest sentence. The lifetime falls straight out of the Bondi-Hoyle accretion history applied to resolved, clumpy, angular-momentum-bearing gas. Nothing external calibrates the timing, so approaching 100 Myr is a model output, not a determination. The body is more careful than the abstract — it notes the lifetime grows toward smaller black holes and that this matches the low-luminosity quasar counts — but the abstract should have said 'predicts.' Second real gap: the accretion and feedback implementation lives in ref. 21, listed as submitted. For a paper whose central claim rests on a sub-grid prescription, that is a reproducibility problem, not a fatal one. Who should read it: anyone working on AGN feedback, quenching, or black hole–bulge coevolution. It is the reference point the field still argues from. Recommendation: send it out. The central claim is supported within the model's scope, and the soft spots are what referees should press on, not reasons to desk-reject.

Referee report

Significance

If it holds, this is an important result: it is the first hydrodynamical treatment in which black hole growth, its energetic feedback, and the star formation history of the host are evolved together self-consistently through a merger, rather than being connected by post-hoc energy-balance arguments. The paper earns credit for several things a referee should name explicitly. It makes falsifiable predictions that can be checked against existing data: that the M_BH-sigma correlation should continue to hold toward low black hole masses and low velocity dispersions (tentatively supported by ref. 30), that low-luminosity quasars should outnumber bright ones because the active phase lasts longer in smaller systems, and that quenched merger remnants should be red, gas-poor spheroids. It also anchors its feedback efficiency to an independent observable, the quasar number density used in semi-analytic models (ref. 8), rather than tuning f to the M_BH-sigma relation itself, which is a genuine methodological strength. The simulation setup is described in enough detail in the Fig. 1 caption to be reproduced.

Major objections (3)

[Main text, third paragraph; abstract:s7] The abstract states that the simulations 'determine' the quasar lifetime of approaching 100 million years, but this number is a direct, uncalibrated output of the Bondi-Hoyle sub-grid prescription described in the third paragraph of the main text (Mdot proportional to M_BH^2 rho / c_s^3), applied to gas whose angular momentum, clumping, and disk structure are not resolved. Nothing external fixes the timing: the final mass is anchored by energy balance, but the epoch at which the black hole reaches Eddington-limited growth and the duration of the luminous phase are set entirely by the accretion-rate history. The manuscript should therefore (i) define operationally how the 'lifetime' is measured (time above what fraction of Eddington, or above what luminosity threshold), (ii) quote the lifetime separately for the 80, 160, and 320 km/s models rather than only asserting that it increases toward lower mass, and (iii) state how the lifetime responds to a factor-of-two change in the Bondi coefficient or in the estimated sound speed at the sink. As written, the lifetime is the softest quantitative claim in the paper and the abstract's 'This determines the lifetime' overstates its robustness relative to the better-supported M_BH-sigma result.
[Main text, paragraph beginning 'We note that the final black hole masses'; Fig. 3] The manuscript states that the final black hole masses scale roughly as 1/f, and that f = 0.05 was chosen to be consistent with the value semi-analytic models require to match the quasar number density (ref. 8). This is a defensible and, I think, commendable choice, but it means the normalization of the reproduced M_BH-sigma relation in Fig. 3 is calibrated rather than predicted, and the paper should say so plainly in the main text rather than leaving the reader to infer it. Concretely, the authors should quote the range of f that keeps the simulated points within the observed scatter of Fig. 3; a factor-of-two change in f shifts every point by about 0.3 dex in M_BH, which is comparable to the scatter of the observed relation, so the allowed range is informative. It would also help to separate explicitly what is predicted (the slope, the residual dependence on gas fraction, and the low-mass extrapolation) from what is anchored (the overall normalization).
[Fig. 3 and its caption] The central claim that the simulations 'reproduce the observed M_BH-sigma correlation very well' is supported only by visual inspection of Fig. 3. No fitted slope, normalization, or intrinsic scatter is quoted for the 18 simulated points, even though the observed sample is fit by the power law given in the caption (M_BH = 1.5e8 (sigma/200)^4.02). A fit to the simulated points, with the scatter about it, would convert a qualitative impression into a testable statement and would let the reader judge the claim in the text that different gas fractions partly compensate to keep the relation tight. In addition, the caption does not state at what time sigma is measured, nor is it demonstrated that the remnants at t = 2.5 Gyr are dynamically relaxed enough for a bulge velocity dispersion to be meaningful; the authors should state the measurement epoch and show, for at least one model, that sigma is stable over the last several hundred Myr.

Minor objections (7)

[Fig. 3 caption] The caption refers to 'six merger simulations' but then lists five virial velocities (50, 80, 160, 320, and 500 km/s). Please reconcile the count with the list, and note that Fig. 2 uses a different subset (80, 160, 320 km/s).
[Fig. 2 and its caption] The no-black-hole control is shown only for the Vvir = 160 km/s model (dashed line). The statement in the caption that AGN feedback lowers the peak starburst amplitude 'by a significant factor' is therefore demonstrated at one mass only; either add the control runs at the other masses or restrict the claim to the 160 km/s case.
[Main text, paragraph on the mass dependence of quenching] The claim that the damping of star formation and black hole activity is more abrupt in more massive systems, and that the active phase lasts longer at lower black hole mass, would be much easier to assess if the inferred lifetimes were tabulated for each of the three masses shown in Fig. 2.
[Main text, third paragraph; ref. 21] The numerical implementation of star formation, supernova feedback, and sink accretion is deferred to ref. 21, which is listed as submitted. The Supplementary Information should at least summarize the star formation efficiency and density threshold, the gravitational softening, and the sink accretion radius, since the accretion rate depends directly on the gas properties at the resolution scale.
[Fig. 3 caption, final sentences] The caption states that the results were checked to be insensitive to the collision orbits, but gives neither the number of orbits tried nor the size of the variation. Please quantify this.
[Fig. 1 and its caption] The temperature colour scale is described only as 'blue to red' with no units or range. Since a central part of the argument is that the gas in the black hole run is hotter and less dense, a colour bar and, ideally, a radial temperature or density profile at t = 1.6 Gyr would make the comparison quantitative rather than impressionistic.
[Title and author lines] The title and author lines in the version supplied contain broken spacing ('galaxie s', 'V olker Springel', 'f¨ ur'), and similar artifacts recur in the body text; these should be cleaned up in the final version.

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The paper

The paper claims

The energy released by gas falling onto a supermassive black hole during a galaxy collision is enough to blow the remaining gas out of the nucleus, shutting down both star formation and the black hole's own growth.

The reading

The paper asks where the observed link between a galaxy's central black hole mass and the random motions of its bulge stars comes from, and why quasars blaze and then switch off. Its answer is that these are one story: a galaxy collision drives gas into the centre, that gas feeds the black hole, and the energy released by the feeding pushes the leftover gas back out. The authors run hydrodynamical simulations of colliding disk galaxies that follow gravity, gas cooling, star formation, supernova heating and black hole accretion at the same time, and compare runs with and without the black hole. With the black hole switched on, the merger remnant ends up gas-poor and quiet; without it, the remnant keeps a cold gas reservoir and keeps making stars. Because a black hole must grow larger to clear out a deeper gravitational well, the mass it reaches when growth stops tracks the depth of the bulge potential, which is exactly what the observed black hole mass versus stellar velocity dispersion relation records.

What carries the argument

The load-bearing device is a sub-grid prescription that couples a black hole 'sink' particle to the resolved gas around it: the accretion rate is estimated with a spherical Bondi-Hoyle formula from the local gas density and sound speed, and the feedback is a heating term $f L = f eta dot{M} c^2$ with $f=0.05$ and $eta=0.1$, so about $0.5$ per cent of the accreted rest mass energy is returned to the surrounding gas. That two-way loop is what does the work: accretion heats and pressurises the gas, the heated gas is expelled, the fuel supply is cut, and accretion stops. The mass at which the loop shuts off is therefore set by how much energy is needed to escape the bulge's gravitational well, which is how a relation between black hole mass and velocity dispersion emerges without being put in by hand.

Extended reading notes

Core claim

The claim is that black hole growth is self-regulating, and that self-regulation quantitatively reproduces the local black hole mass–velocity dispersion relation while also fixing how long a quasar shines. In the simulations, a major merger first produces the familiar starburst, and the same tidal inflows raise the central gas density so that the two black holes, which merge into one, accrete close to the Eddington rate. A fraction $f=0.05$ of the radiated luminosity, with radiative efficiency $f=0.05$ of the rest mass energy converted and $0.5$ per cent of the accreted rest mass returned to the gas as heat, raises the temperature of the circumnuclear gas and drives a wind that expels it. Star formation and accretion are then both quenched, the black hole mass saturates, and the remnant quickly reddens into a dead elliptical; the same merger run without a black hole keeps a dense cold gas supply and forms stars at a steady rate for far longer. Across six galaxy masses and three disk gas fractions, the final black hole masses and bulge velocity dispersions land close to the observed relation, including its normalisation and slope, and the luminous phase lasts approaching $10^8$ years. Because more massive systems have deeper wells and larger gas supplies, their black holes must grow further before the released energy suffices to expel the gas, while lower-mass black holes stay active longer, which the authors read as an explanation for why low-luminosity quasars are more numerous than bright ones.

Load-bearing premise

The load-bearing premise is that a spherical Bondi-Hoyle estimate applied to the resolved, large-scale gas around the black hole gives the true accretion rate on the much smaller scales the simulation cannot resolve; if that estimate is systematically wrong, the growth history that drives the feedback, and hence the final masses, shift with it.

Editorial extensions

If this is right

A gas-rich major merger should produce a bright quasar phase lasting up to roughly a hundred million years, after which the nucleus goes quiet on its own.
Merger remnants hosting a grown black hole should be gas-poor, have little residual star formation, and redden quickly, while otherwise identical remnants without one keep forming stars.
The black hole mass at shut-off should scale with the depth of the bulge potential, so the black hole mass–velocity dispersion relation is a consequence of energy balance rather than an imposed rule.
Lower-mass black holes should stay active longer than massive ones, making low-luminosity quasars more common than bright ones, as surveys indicate.
The final black hole mass should scale roughly inversely with the assumed feedback efficiency, and a coupling of about five per cent matches the value semi-analytic models need to reproduce the evolution of quasar number density.

Reading between the lines

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

Because the final mass scales as roughly $1/f$, an independent measurement of how efficiently quasar outflows couple to gas, combined with the normalisation of the observed relation, would convert a tuned parameter into a measured number.
The predicted anti-correlation between quasar lifetime and luminosity implies a particular shape and turnover for the AGN luminosity function; comparing these lifetimes with lifetimes inferred from quasar clustering would test the picture without new hydrodynamics.
The same prescription could be carried into cosmological volumes, where it makes a sharper prediction than the idealised mergers shown here: the strongest suppression of star formation should occur in the highest gas-fraction, highest-redshift mergers, leaving post-starburst ellipticals whose colours track their black hole masses.
Since the inflow's angular momentum is discarded by construction, the model is silent on whether the accreted gas settles into a disk or launches jets; a radiatively inefficient, jet-dominated phase would change the energy budget and could shift the predicted normalisation of the relation.

Original abstract

In the early Universe, while galaxies were still forming, black holes as massive as a billion solar masses powered quasars. Supermassive black holes are found at the centers of most galaxies today, where their masses are related to the velocity dispersions of stars in their host galaxies and hence to the mass of the central bulge of the galaxy. This suggests a link between the growth of the black holes and the host galaxies, which has indeed been assumed for a number of years. But the origin of the observed relation between black hole mass and stellar velocity dispersion, and its connection with the evolution of galaxies have remained unclear. Here we report simulations that simultaneously follow star formation and the growth of black holes during galaxy-galaxy collisions. We find that in addition to generating a burst of star formation, a merger leads to strong inflows that feed gas to the supermassive black hole and thereby power the quasar. The energy released by the quasar expels enough gas to quench both star formation and further black hole growth. This determines the lifetime of the quasar phase (approaching 100 million years) and explains the relationship between the black hole mass and the stellar velocity dispersion.

The compiled record

The paper's own sentences, arranged, kept beside the review and separate from it. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 6,260 input tokens.

What the abstract itself states, as probabilities: claims first 0.05 · states limitation 0.08 · human participants 0.01 · controlled comparison 0.04 · randomized assignment 0.01 · states quantitative result 0.95 · compares with prior results 0.10 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v1. Results and the main claim are underlined; show every role.

In the early Universe, while galaxies were still forming, black holes as massive as a billion solar masses powered quasars. Supermassive black holes are found at the centers of most galaxies today, where their masses are related to the velocity dispersions of stars in their host galaxies and hence to the mass of the central bulge of the galaxy. This suggests a link between the growth of the black holes and the host galaxies, which has indeed been assumed for a number of years. But the origin of the observed relation between black hole mass and stellar velocity dispersion, and its connection with the evolution of galaxies have remained unclear. Here we report simulations that simultaneously follow star formation and the growth of black holes during galaxy-galaxy collisions. We find that in addition to generating a burst of star formation, a merger leads to strong inflows that feed gas to the supermassive black hole and thereby power the quasar. The energy released by the quasar expels enough gas to quench both star formation and further black hole growth. This determines the lifetime of the quasar phase (approaching 100 million years) and explains the relationship between the black hole mass and the stellar velocity dispersion.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	In the early Universe, while galaxies were still forming, black holes as massive as a billion solar masses powered quasars.	background 1.00	0.05	0.02	asserted 1.00
s1	Supermassive black holes are found at the centers of most galaxies today, where their masses are related to the velocity dispersions of stars in their host galaxies and hence to the mass of the central bulge of the galaxy.	background 1.00	0.06	0.03	asserted 1.00
s2	This suggests a link between the growth of the black holes and the host galaxies, which has indeed been assumed for a number of years.	background 0.99	0.04	0.03	hedged possibility 0.65
s3	But the origin of the observed relation between black hole mass and stellar velocity dispersion, and its connection with the evolution of galaxies have remained unclear.	gap 1.00	0.03	0.02	asserted 0.83
s4	Here we report simulations that simultaneously follow star formation and the growth of black holes during galaxy-galaxy collisions.	method 0.60	0.95	0.04	asserted 0.94
s5	We find that in addition to generating a burst of star formation, a merger leads to strong inflows that feed gas to the supermassive black hole and thereby power the quasar.	result 1.00	0.96	0.14	asserted 1.00
s6	The energy released by the quasar expels enough gas to quench both star formation and further black hole growth.	result 0.98	0.89	0.57	asserted 1.00
s7	This determines the lifetime of the quasar phase (approaching 100 million years) and explains the relationship between the black hole mass and the stellar velocity dispersion.	interpretation 0.81	0.85	0.76	asserted 1.00

What kind of paper the classifier reports this is: simulation study 1.00 · evidence from simulation or computation 1.00.

What was examined, and what was not

sources read

arXiv listing abstract v1

not examined

full text
figures and tables
references and citing sentences
relations to other papers

levels run

P abstract

not run

S sections
T body sentences
C citations
R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

Figures

**Figure 1.** — Snapshots of the simulated time evolution in merger

**Figure 2.** — Black hole activity, star formation and black hole g

**Figure 3.** — The relation between the final black hole mass,

Figures reproduced from arXiv:astro-ph/0502199 by the authors.

References

Works cited (31)

[1]

KR95 Kormendy J., Richstone D., Inward Bound--The Search For Supermassive Black Holes In Galactic Nuclei, Annu. Rev. Astron. Astrophys. , 33 , 581-624 (1995)

View on Pith 1995
[2]

M98 Magorrian, J., et al., The Demography of Massive Dark Objects in Galaxy Centers The Astron. J. , 115 , 2285-2305 (1998)

View on Pith 1998
[3]

FH04 Ferrarese, L., Ford, H.C., Supermassive Black Holes in Galactic Nuclei: Past, Present and Future Research Space Science Reviews , in press (2004)

View on Pith 2004
[4]

FM00 Ferrarese, L., Merritt, D., A Fundamental Relation between Supermassive Black Holes and Their Host Galaxies, The Astrophys. J. , 539 , L1--L4 (2000)

View on Pith 2000
[5]

G00 Gebhardt, K., et al., A Relationship between Nuclear Black Hole Mass and Galaxy Velocity Dispersion, The Astrophys. J. , 539 , L13--L16 (2000)

View on Pith 2000
[6]

KH00 Kauffmann, G., Haehnelt, M., A unified model for the evolution of galaxies and quasar, Mon. Not. R. Astron. Soc. , 311 , 576--588 (2000)

View on Pith 2000
[7]

VHM03 Volonteri, M., Haardt F., Madau, P., The Assembly and Merging History of Supermassive Black Holes in Hierarchical Models of Galaxy Formation, The Astrophys. J. , 582 , 559-573, (2003)

View on Pith 2003
[8]

Wy03 Wyithe, J. S. B., Loeb, A., Self-regulated Growth of Supermassive Black Holes in Galaxies as the Origin of the Optical and X-Ray Luminosity Functions of Quasars, The Astrophys. J. , 595 , 614--623 (2003)

View on Pith 2003
[9]

Gra04 Granato, G.L., De Zotti, G., Silva, L., Bressan, A., Danese, L., A Physical Model for the Coevolution of QSOs and Their Spheroidal Hosts, The Astrophys. J. , 600 , 580-594 (2004)

View on Pith 2004
[10]

MH96 Mihos, J.C., Hernquist, L., Gasdynamics and starbursts in major mergers, The Astrophys. J. , 464 , 641--663 (1996)

View on Pith 1996
[11]

S82 Soltan, A., Masses of quasars, Mon. Not. R. Astron. Soc. , 200 , 115--122 (1982)

View on Pith 1982
[12]

YT02 Yu, Q., Tremaine, S., Observational constraints on growth of massive black holes, Mon. Not. R. Astron. Soc. , 335 , 965-976, (2002)

View on Pith 2002
[13]

H89 Hernquist, L., Tidal triggering of starbursts and nuclear activity in galaxies, Nature , 340 , 687--691, (1989)

View on Pith 1989
[14]

BH91 Barnes, J., Hernquist, L.,

View on Pith
[15]

BH92 Barnes, J., Hernquist, L., Dynamics of interacting galaxies, Annu. Rev. Astron. Astrophys. , 30 , 705--742, (1992)

View on Pith 1992
[16]

SR98 Silk, J., Rees, M., Quasars and galaxy formation, Astr. & Astrophy. , 334 , L1--L4 (1998)

View on Pith 1998
[17]

F99 Fabian, A.C., The obscured growth of massive black holes, Mon. Not. R. Astron. Soc. , 308 , L39--L43 (1999)

View on Pith 1999
[18]

K03 King, A., Black Holes, Galaxy Formation, and the M_ BH - Relation, Mon. Not. R. Astron. Soc. , 596 , L27-L29 (2003)

View on Pith 2003
[19]

CBG03 Chartas, G., Brandt, W. N., Gallagher, S. C., XMM-Newton Reveals the Quasar Outflow in PG 1115+080, The Astrophys. J. , 595 , 85-93, (2003)

View on Pith 2003
[20]

CKG03 Crenshaw, D. M., Kraemer, S. B., George, I. M., Mass Loss from the Nuclei of Active Galaxies, Annu. Rev. Astron. Astrophys. , 41 , 117-167 (2003)

View on Pith 2003
[21]

P03 Pounds, K. A., Reeves, J. N., King, A. R., Page, K. L., O'Brien, P. T., Turner, M. J. L., A high-velocity ionized outflow and XUV photosphere in the narrow emission line quasar PG1211+143, Mon. Not. R. Astron. Soc. , 345 , 705--713, (2003)

View on Pith 2003
[22]

SDH04s Springel, V., Di Matteo, T., Hernquist, L., Modeling feedback from stars and black holes in galaxy mergers, Mon. Not. R. Astron. Soc. , submitted, preprint astro-ph/0411108 at http://xxx.lanl.gov/ (2004)

View on Pith Pith review arXiv 2004
[23]

B52 Bondi, H., On spherically symmetrical accretion, Mon. Not. R. Astron. Soc. , 112 , 195--204, (1952)

View on Pith 1952
[24]

SS73 Shakura, N.I., Sunyaev, R.A., Black holes in binary systems. Observational appearance, Astron. & Astrophys. , 24 , 337--355, (1973)

View on Pith 1973
[25]

SH03 Springel, V., Hernquist, L., Cosmological smoothed particle hydrodynamics simulations: a hybrid multiphase model for star formation, Mon. Not. R. Astron. Soc. , 339 , 289--311, (2003)

View on Pith 2003
[26]

SDH04 Springel, V., Di Matteo, T., Hernquist, L., Black holes in galaxy mergers: The formation of red elliptical galaxies, The Astrophys. J. , in press, (2005)

View on Pith 2005
[27]

SH04 Springel, V., Hernquist, L., Formation of a spiral galaxy in a major merger, The Astrophys. J. , submitted, (2005)

View on Pith 2005
[28]

HMS04 Hasinger G., Miyaji T., Schmidt M., Luminosity Dependent Evolution of Soft X-ray Selected AGN, Astron. & Astroph. , submitted, (2004)

View on Pith 2004
[29]

Bar04 Barger A.J., Cowie L.L., Mushotzky R.F., Yang Y., Wang W.-H, Steffen A.T., Capak P., The Cosmic Evolution of Hard X-ray Selected Active Galactic Nuclei, The Astrophys. J. , in press (2004)

View on Pith 2004
[30]

T02 Tremaine, S., et al., The slope of the black hole mass versus velocity dispersion correlation, The Astrophys. J. , 574 , 740--753 (2002)

View on Pith 2002
[31]

GH04 Greene, J.E., Ho, L.C., Active galactic nuclei with candidate intermediate-mass black holes, The Astrophys. J. , in press, (2004)

View on Pith 2004

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

A uniform spectral decomposition of 1,717,774 DESI DR1 quasars yields line properties, black hole masses, luminosities, improved systemic redshifts, and coronal-line measurements.
The black hole-galaxy correlations of the 12 micron local AGN sample: a NuSTAR perspective
astro-ph.GA 2026-10 accept novelty 6.0 of 10

The local active-galaxy M-sigma relation has large scatter and lies below the inactive-galaxy relation, so it is not a reliable individual black hole mass estimator.
Dual and lensed AGN at sub-arcsecond separations uncovered by ERIS
astro-ph.GA 2026-10 accept novelty 6.0 of 10

ERIS-SPIFFIER spectroscopy confirms six new dual AGN and seven new lensed quasars (four double, three quadruple) at sub-arcsecond separations, substantially enlarging the census of compact multiple AGN at z>0.5.
A Comprehensive AGN Inventory for the Dwarf-Dominated RESOLVE and ECO Surveys: Mass-Dependent AGN Types and Occupation Fractions
astro-ph.GA 2026-10 accept novelty 6.0 of 10

In complete nearby surveys, AGN occupy 2-5% of dwarf galaxies but 16-27% of transitional galaxies, a roughly 5x jump at baryonic mass ~10^9.7 solar masses, with the dominant AGN flavor shifting from star-forming AGN t...
A relativistic inflow candidate in a quasar at cosmic noon
astro-ph.HE 2026-10 conditional novelty 6.0 of 10

Two weak X-ray absorption features in quasar WISEA J094835.95+432302.6 at z=1.893 are best explained as iron K-shell lines from gas falling into the supermassive black hole at roughly one third of the speed of light.
The star-forming past and quenching of brightest cluster galaxies in TNG-Cluster
astro-ph.GA 2026-10 conditional novelty 6.0 of 10

In TNG-Cluster, brightest cluster galaxies quench for the first time when cumulative SMBH kinetic feedback energy overtakes the galaxy's gas binding energy (beta near 1), typically 2.3 billion years after feedback sta...
Diverse Metallicities in Protoclusters at $z \sim 3.4$ detected by Deep Learning
astro-ph.GA 2026-09 conditional novelty 6.0 of 10

Spectroscopic follow-up confirms four protoclusters at z~3.4 selected by the deep learning model PCFNet, with marginal diversity in gas-phase metallicity among them.
The lifetimes and properties of Little Red Dots in the AMBRA simulation
astro-ph.GA 2026-09 conditional novelty 6.0 of 10

In the AMBRA simulation, little red dots are existing black hole-galaxy systems caught in a bright, temporary phase that lasts roughly 3 to 300 million years and scales with host and black hole mass.
The WISSH quasars project XIII. A multi-epoch study of ultra-fast broad absorption line outflows at cosmic noon
astro-ph.GA 2026-09 accept novelty 6.0 of 10

Multi-epoch observations of three luminous quasars reveal that ultra-fast broad absorption line outflows (0.1-0.2c) have kinetic powers up to 25% of the bolometric luminosity and can provide effective AGN feedback.
C3PO: A Ly{\alpha} Emitting Galaxy at $z \sim 9$
astro-ph.GA 2026-09 unverdicted novelty 6.0 of 10

C3PO-84478 is a low-mass, vigorously star-forming galaxy at z=9 that alone sustains the small ionized bubble required for its Lyα line to escape.
Local Heavily Obscured Active Galaxies Observed With Chandra (I): Spectral Properties of the Nuclear and Extended X-ray Emission
astro-ph.GA 2026-08 accept novelty 6.0 of 10

A uniform spatially resolved Chandra spectral analysis of 20 heavily obscured nearby AGN reveals multiphase extended X-ray emission, common hard X-ray excess, and extended Fe K-alpha fluorescence on kiloparsec scales.
Probing ultralight bosons with LISA observations of spinning black hole mergers and follow-up searches of merger remnants
gr-qc 2026-08 conditional novelty 6.0 of 10

LISA spin measurements could exclude scalar and vector ultralight bosons over roughly four orders of magnitude in mass, while post-merger follow-up searches offer a narrower, model-dependent window for detecting vecto...
The Quasar Feedback Survey: Ionised Outflows in type 2 QSOs with MUSE data
astro-ph.GA 2026-08 conditional novelty 6.0 of 10

Electron densities from [Ar IV] lines in 16 type 2 QSOs imply outflow mass rates and kinetic powers roughly 1 dex lower than assuming n_e=1000 cm^-3, plus a positive density-velocity correlation above 630 km/s.
Scattering from Dusty Outflows in Hot Dust-Obscured Galaxies with Blue Excess Emission
astro-ph.GA 2026-08 conditional novelty 6.0 of 10

Polarization of five hot, dust-obscured quasars confirms their blue excess is scattered AGN light, and the wavelength trend in one object requires graphite-dominated dust in a polar outflow.
On the Origin of the Ly$\alpha$ Damping Wing in Galaxies at $8\le z \le 10$: Explorations using the NINJA Simulations
astro-ph.GA 2026-08 conditional novelty 6.0 of 10

At z=8-10, the strongest JWST damped Lyα absorbers require neutral gas inside and around galaxies, and the NINJA models still underproduce them unless additional unresolved birth-cloud gas is invoked.
Cosmic Pairs: A DESI Census of Dual and Offset AGN as Precursors to Massive Black Hole Binaries
astro-ph.GA 2026-07 conditional novelty 6.0 of 10

DESI DR1 spectroscopy yields >7,000 candidate dual-AGN pairs, expanding the known kpc-scale census by ~4x and linking host-galaxy demographics to LISA-detectable massive black hole mergers.
Outflows in a super-Eddington quasar drive clumpy circumgalactic medium and extended H$\alpha$ nebulae at $z \gtrsim 6$
astro-ph.GA 2026-07 conditional novelty 6.0 of 10

In z≈6 quasar simulations, super-Eddington black-hole growth clears escape channels, ejects cold clumps that raise neutral-hydrogen covering, and powers extended Hα nebulae that shrink when the quasar is obscured.
What's Missing in AGN Feedback? Lessons learnt from Magneticum, IllustrisTNG and Simba
astro-ph.GA 2026-07 conditional novelty 6.0 of 10

No current simulation simultaneously reproduces observed halo hot-gas fractions and local galaxy star-formation/quenching demographics; strong AGN feedback overquenches, weak feedback retains too much gas.
AGN Feedback Models and AGN Demographics II: Comparing Predictions of Radiative and Total Feedback to Observations
astro-ph.GA 2026-07 conditional novelty 6.0 of 10

EAGLE, SIMBA, and TNG100 all fail to reproduce observed trends in which galaxies host radiatively efficient AGN, and EAGLE matches only after a factor-of-ten normalization adjustment.
Mass--size evolution and the emerging passive--density relation revealed by JWST/NIRCam in the Spiderweb protocluster
astro-ph.GA 2026-07 conditional novelty 6.0 of 10

In the Spiderweb protocluster, passive fraction rises with local density to ~60% while passive mass–size intercepts sit between field and cluster values, indicating advanced quenching but ongoing size growth.
The youth of the intracluster medium. I. A non-parametric characterisation of the gas and electron number density profiles of $z \simeq 2$ protoclusters
astro-ph.CO 2026-07 conditional novelty 6.0 of 10

At z≈2, Magneticum protoclusters show moderate self-similarity deviations, double-β density profiles, and hot ionised gas dominant only beyond ~0.1–0.5 R500c, with clear mass, merger and AGN trends.
Identifying Observational Signatures of Flux Eruption Events in Supermassive Black Hole Accretion Flows with Machine Learning
astro-ph.HE 2026-06 unverdicted novelty 6.0 of 10

Machine learning on simulated images identifies that flux eruption events cause more diffuse, polarized, lower-flux millimeter emission with decreased Q-U loop rotation rate, achieving ~80% accuracy with random forest...
Understanding the Broad-line Region of Active Galactic Nuclei with Photoionization. II. Slim disks, Self-shadowing, and BLR sizes
astro-ph.GA 2026-05 conditional novelty 6.0 of 10

Slim-disk self-shadowing plus accretion-rate-dependent BLR density enhancement explains the observed offsets of high-Eddington AGNs below the canonical R-L relation.
$\textit{BMAD}$-Circumbinary Magnetically Arrested Disks around Stellar or Black Hole Binaries: Hot Accretion Flows, Disk Properties, and Angular Momentum Transfer
astro-ph.HE 2025-08 conditional novelty 6.0 of 10

Circumbinary accretion disks can enter a magnetically arrested state, and in weakly cooled or adiabatic regimes the resulting magnetic flux eruptions may drive the binary orbit to shrink.
Efficient formation of a massive quiescent galaxy at redshift 4.9
astro-ph.GA 2024-04 conditional novelty 6.0 of 10

JWST/NIRSpec spectroscopy confirms RUBIES-EGS-QG-1 as a quiescent galaxy at z=4.90 with a stellar mass near 10^11 solar masses, assembled in a short burst and quenched before z about 5.5.
The PAU Survey: Active galactic nucleus galaxies in galaxy pairs
astro-ph.GA 2026-10 conditional novelty 5.0 of 10

PAUS data reveals that AGNs in galaxy pairs become redder at z>0.6 and are preferentially found in morphologically disturbed, close pairs, indicating a redshift-dependent link between interactions and AGN activity.
A ${}^{13}$CO Detection in a Massive Molecular Gas Flow in Abell 1795's Central Galaxy
astro-ph.GA 2026-10 conditional novelty 5.0 of 10

Detection of 13CO in Abell 1795's northern molecular filament yields a CO-to-H2 conversion factor 0.1-1.1 times the Milky Way value, implying filament masses that enable AGN entrainment.
Common Excitation Patterns of Star Formation, Active Galactic Nuclei, and Shocks in Seyfert Galaxies
astro-ph.GA 2026-09 accept novelty 5.0 of 10

Nine Seyfert galaxies show a common spatial pattern of star-forming rings, AGN-ionized bicones, and shock-dominated regions perpendicular to the bicones.
Unveiling a cosmic tango: Integral field spectroscopy and numerical simulations of Arp 143's interaction
astro-ph.GA 2026-06 unverdicted novelty 5.0 of 10

New spectroscopy and simulations of Arp 143 suggest it formed via head-on collision between S0 and Sc galaxies following a flyby.
Dust destruction signals shock-accelerated outflows in the nearby active galaxy NGC 1068
astro-ph.GA 2026-06 unverdicted novelty 5.0 of 10

Line ratio diagnostics in NGC 1068 indicate that AGN outflows are accelerated by shocks that destroy dust and compress gas.
Satellite compaction pathways: environmental drivers shaping dwarf galaxy corpulence in the TNG50 simulation
astro-ph.GA 2026-06 unverdicted novelty 5.0 of 10

In TNG50, compact dwarf satellites (log M_star 8.4-9.2) form via DM-rich gas inflows in low-merger environments, tidal stripping for DM-poor cases, and ram-pressure starbursts for some metal-rich ones.
One Merge to Rule Them All: From Galaxy Interactions to Black Hole Mergers Using Horizon-AGN
astro-ph.GA 2026-05 unverdicted novelty 5.0 of 10

Horizon-AGN shows galaxy and black hole merger rates both rise with stellar mass and fall with redshift, peaking near z=2-3, establishing a direct evolutionary link from galaxy interactions to black hole coalescences.
Direct VLBI evidence for a buried AGN in the triple-merger LIRG UGC 2369S
astro-ph.GA 2026-07 unverdicted novelty 4.0 of 10

VLBI imaging detects a compact radio source with Tb > 10^7 K and flat spectrum in the northern core of UGC 2369S, confirming a buried low-luminosity AGN.
Mapping the star formation peak with LIGO A# and Next-Generation detectors
gr-qc 2026-06 unverdicted novelty 4.0 of 10

Simulations show LIGO-A# constrains the peak redshift of binary black hole merger rate (tracing star formation) to ±0.1 in one year, improving to ±0.02 with next-generation detectors.
Science with the TianQin observatory: Preliminary results on massive black hole binaries
astro-ph.HE 2019-02 conditional novelty 4.0 of 10

TianQin could detect between roughly 0.1 and 60 massive black hole binary mergers per year depending on the population model, and localize nearby events well enough for electromagnetic follow-up.
SUNRISE-3D: Sharp UNveiling of AGN feedback Regulation and its Impact on Star-formation at the cosmic noon Epoch
astro-ph.GA 2026-06 unverdicted novelty 3.0 of 10

Proposal for statistical study of AGN outflows at cosmic noon using adaptive-optics 3D spectroscopy to map outflow rates and SFR without geometry assumptions.
Dual AGN and Multiple SMBH Systems in the Era of SKAO
astro-ph.HE 2026-06 unverdicted novelty 2.0 of 10

A review outlining radio methods for dual AGN and SMBHB detection and the role of SKAO in enabling comprehensive studies across cosmic time.
A Review of Galaxy Quenching -- Part I: Defining the Problem and Observational Results
astro-ph.GA 2026-08 unverdicted novelty 1.0 of 10

A comprehensive observational review of galaxy quenching, synthesizing two decades of survey results and laying out the empirical case that star formation cessation is a mass-dependent, globally regulated process.
Cosmological Simulations of Galaxy Formation
astro-ph.GA 2019-09 accept novelty 1.0 of 10

A structured survey of the numerical methods, baryonic sub-resolution models, and validation status of cosmological galaxy formation simulations, plus their use in testing alternative dark matter, dark energy, and gravity.
A brief overview of the baryon cycle in galaxies
astro-ph.GA 2026-11 unverdicted

A concise review of the baryon cycle in galaxies, summarizing gas accretion, star formation, stellar feedback, AGN feeding and feedback, and outstanding open questions.
A Review of Galaxy Quenching -- Part II: Theoretical Solutions and Direct Observational Tests
astro-ph.GA 2026-08 unverdicted

This review of galaxy quenching theory concludes that massive galaxies quench through internal mechanisms, most likely AGN feedback, while satellite galaxies quench through environmental gas removal.

How later papers used it

753 later papers cite it

Evidence: substantial. 671 of the citing papers share no author with it, and 57 of those carry a confident label from Pith's citation classifier.

Pith read 40 of the 990 citing sentences, choosing only those whose citation markers point at this paper alone, and wrote the paraphrases from them. The summary, the counts, the evidence level, the links and the quotes come from code; the summary counts the papers listed below. A later paper is listed under a label when Pith's citation classifier gives one of its sentences that label at probability 0.8 or more (0.95 for support), Pith's reading finds that the citing paper itself did it, and a second check confirms the paraphrase against the sentence. This section lists uses only. It does not list criticism or disagreement, so their absence here says nothing about how the paper has been received. Papers that share an author with this one are listed apart, under "By the same authors". A quote is the citing authors' own sentence, shown when their paper's licence is CC BY, CC BY-SA or CC0. JSON

6 later papers by other authors are listed below: 6 used its method or tool. 19 more papers by the same authors are listed: 19 used its method or tool.

Uses its method or tool 25 of 65 papers with this label · 19 by the same authors

Modelled the unresolved physics of accretion in a subgrid fashion following another work and this paper.

How AGN feedback drives the size growth of the first quasars (2019) · 1.00 · paraphrased: the licence does not allow quoting
Our simulations also include a prescription for black hole (BH) growth and feedback from active galactic nuclei (AGN) based on the model presented by [ref] and [ref] , including the same modifications as [ref] and some minor changes.

On the Decline of Star Formation during the Evolution of Galaxies (2023) · Implementation of Physical Processes · 0.99
Estimated the accretion of gas onto the black hole using a Bondi-Hoyle-Lyttleton-like prescription from this paper.

The black hole occupation fraction as a fossil record of seeding, dynamics, and galaxy assembly (2026) · 0.99 · paraphrased: the licence does not allow quoting
Based the growth and dynamics of black holes and associated active galactic nucleus feedback on the model of another work and this paper, with modifications described in the other work.

Tracing the environmental history of observed galaxies via extended fast action minimization method (2022) · 0.94 · paraphrased: the licence does not allow quoting
Re-scaled its modified Bondi-Hoyle-Lyttleton accretion rate by a factor of 50 to account for higher central densities around accreting black holes, citing this paper.

The infrared-luminous progenitors of high-z quasars (2018) · 0.86 · paraphrased: the licence does not allow quoting
Estimated the accretion of gas onto the black hole using a Bondi-Hoyle-Lyttleton-like prescription from this paper.

Tracing black hole and galaxy growth across environments since cosmic noon (2026) · 0.98 · paraphrased: the licence does not allow quoting

By the same authors

Implemented a sub-grid recipe for black holes and related physical processes based on another work and this paper, calculating black hole accretion with a spherical Bondi model.

The Formation of the First Quasars. I. The Black Hole Seeds, Accretion and Feedback Models (2020) (same authors) · 1.00 · paraphrased: the licence does not allow quoting
Estimated the gas accretion rate onto the black hole via a Bondi-Hoyle-Lyttleton-like prescription from this paper.

Orbital and Radiative Properties of Wandering Intermediate-Mass Black Holes in the ASTRID Simulation (2022) (same authors) · 1.00 · paraphrased: the licence does not allow quoting
Incorporated black hole growth and feedback from active galactic nuclei based on the super-massive black hole model developed in this paper.

A tiny host galaxy for the first giant black hole: $z= 7.5$ quasar in BlueTides (2018) (same authors) · 1.00 · paraphrased: the licence does not allow quoting
A Bondi-Hoyle-Lyttleton-like prescription [ref] is used to estimate the gas accretion rate onto the BH: [equation] where $c_s$ and $ρ$ are the local sound speed and density of gas, $v_rel$ is the relative velocity of the BH with respect to the nearby gas and $α= 100$ is a dimensionless fudge parameter to account for the underestimation of the accretion rate due to the unresolved cold and hot phase of the subgrid interstellar medium in the surrounding.

Triple and Quadruple Black Holes in the ASTRID Simulation at $z \sim 2$ (2023) (same authors) · Simulation · 1.00
Gas accretion onto BHs is modeled with a Bondi-Hoyle-Lyttleton-like prescription [ref] : [equation] where $c_s$ and $ρ$ are the local sound speed and density of the gas, $v_rel$ is the relative velocity of the BH with respect to the nearby gas, and $α= 100$ is a dimensionless fudge parameter to account for the underestimation of the accretion rate due to the unresolved cold and hot phase of the subgrid interstellar medium in the surrounding.

MAGICS I. The First Few Orbits Encode the Fate of Seed Massive Black Hole Pairs (2023) (same authors) · The subgrid physics model for galaxy formation · 1.00
Modeled active galactic nucleus feedback as in the MassiveBlack I and II simulations, giving self-regulated super-massive black hole accretion following this paper.

Gas outflows from the z= 7.54 quasar : predictions from the BlueTides Simulation (2018) (same authors) · 1.00 · paraphrased: the licence does not allow quoting
Modeled black hole growth and active galactic nucleus feedback as in the MassiveBlack I and II simulations, based on the black hole sub-grid model developed in another work and this paper.

MAGICS II. Seed black holes stripped of their surrounding stars do not sink (2024) (same authors) · 1.00 · paraphrased: the licence does not allow quoting
Black hole growth and AGN feedback are modeled in the same way as in the MassiveBlack I & II simulations, based on the black hole sub-grid model developed in [ref] and [ref] .

Modeling Quasar Proximity Zones in a Realistic Cosmological Environment with a Self-consistent Light Curve (2023) (same authors) · Physics: hydrodynamics and sub-grid modelling · 1.00
Used a Bondi-Hoyle-Lyttleton-like prescription from this paper to estimate the accretion rate of gas onto the black holes.

Over-massive Central Black Holes in the Cosmological Simulations ASTRID and Illustris TNG50 (2023) (same authors) · 1.00 · paraphrased: the licence does not allow quoting
Used the prescription described in this paper and another work to model the growth of supermassive black holes.

Multiplicity functions of quasars: Predictions from the MassiveBlackII simulation (2019) (same authors) · 1.00 · paraphrased: the licence does not allow quoting
Adopted its prescription for black hole growth from this paper and another work.

On the small scale clustering of quasars: constraints from the MassiveBlack II simulation (2018) (same authors) · 1.00 · paraphrased: the licence does not allow quoting
Modeled active galactic nucleus feedback as in the MassiveBlack I and II simulations, using the super-massive black hole model developed in this paper.

The BlueTides Simulation: First Galaxies and Reionization (2015) (same authors) · 1.00 · paraphrased: the licence does not allow quoting
Estimated the accretion rate onto the black hole using a Bondi-Hoyle-Lyttleton-like prescription from this paper.

The Astrid Simulation: Evolution of black holes and galaxies to z=0.5 and different evolution pathways for galaxy quenching (2024) (same authors) · 0.99 · paraphrased: the licence does not allow quoting
Estimated the gas accretion rate onto the black hole via a Bondi-Hoyle-Lyttleton-like prescription from this paper.

A vast population of wandering and merging IMBHs at cosmic noon (2022) (same authors) · 0.99 · paraphrased: the licence does not allow quoting
Estimated the gas accretion rate onto the black hole via a Bondi-Hoyle-Lyttleton-like prescription from this paper.

MAGICS III. Seeds sink swiftly: nuclear star clusters dramatically accelerate seed black hole mergers (2024) (same authors) · 0.99 · paraphrased: the licence does not allow quoting
Modeled black hole growth and active galactic nucleus feedback as in the MassiveBlack I and II simulations, using the supermassive black hole model developed in this paper with modifications consistent with Illustris.

BlueTides simulation: establishing black hole-galaxy relations at high-redshift (2018) (same authors) · 0.94 · paraphrased: the licence does not allow quoting
Modeled black hole accretion and feedback according to this paper, based on quasar-mode feedback.

Intrinsic alignments of disk and elliptical galaxies in the MassiveBlack-II and Illustris simulations (2015) (same authors) · 0.97 · paraphrased: the licence does not allow quoting
Implemented active galactic nucleus feedback using the same model used in MassiveBlack I and II, this paper.

Forecasts for the WFIRST High Latitude Survey using the BlueTides Simulation (2016) (same authors) · 0.97 · paraphrased: the licence does not allow quoting
Used the same black hole sub-grid model for black hole growth and active galactic nucleus feedback as the MassiveBlack I and II simulations, originally developed in another work and this paper, with modifications consistent with Illustris.

The host galaxies of z=7 quasars: predictions from the BlueTides simulation (2019) (same authors) · 0.98 · paraphrased: the licence does not allow quoting

How the literature uses it

107 arXiv papers cite this in 135 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 82 sentences without a confident label

Uses its method or tool 12 papers

To gain some information regarding the SMBH activity of the galaxies in our samples, we turn to a proxy which is the time-averaged supermassive black hole growth factor, $⟨Ṁ_SMBH ⟩$, [ref] .

The influence of galaxy mergers, black-hole growth, and gas processes on the evolution of the stellar mass-gas metallicity relation of galaxies in different cosmic environments · Supermassive Black Hole Growth Factor · 0.88
The BH accretion rate $Ṁ_BH$ is estimated using the Bondi-Hoyle formalism [ref] , which is based on the local properties of nearby gas particles: [equation] where $c_s$ is the local sound speed, $ρ_BH$ is the gas density around the BH, and $v_vel$ is the velocity of the black hole relative to the surrounding gas.

First results of AMBRA: Abundant Seeds and Early Mergers as a Pathway to the First Massive Black Holes · galaxy formation model · 1.00
Following [ref] , we implement a module of “continuous” BH accretion in GIZMO: instead of “discretely” swallowing an entire neighboring gas cell in a single timestep [ref] (which is not appropriate here since $M_BH ≲m_gas$), each BH (labeled $i$) receives a mass inflow of $Ṁ_BondiΔt$ in a time bin $Δt$.

The In Situ Growth of Stellar-mass "Light" Seed Black Holes in Nuclear Star Clusters · Remnant BH accretion and feedback · 0.98

Uses its data or values 1 paper

In the seminal work of Di Matteo et al. [ref] , the feedback efficiency ($ϵ_f$; the fraction of AGN luminosity that couples to the gas in the vicinity of the black hole) was calibrated to 5%, so the local M$_BH$-$σ$ relation was reproduced by the simulation.

Observational Tests of Active Galactic Nuclei Feedback: An Overview of Approaches and Interpretation · Outflow energetics and potential for impact · 0.80

Compares with it 1 paper

For $M_∙∼10^6 M_⊙$, this is $30%$ of the Eddington luminosity, significantly larger than the $Ė_K/L_bol∼0.5$–$5%$ measured for ultrafast outflows in high-$L_Edd$ AGN, the regime generally regarded as sufficient for efficient coupling to the host [ref] .

Relativistic outflows power a quasi-periodic eruption: constraints on energetics, mass loss, and emission mechanisms · Implications for reverberation and feedback · 0.98

Cites it as support 4 papers

Overall, our results align with a scenario in which the SMBH regulates its immediate surroundings and the host galaxy, with AGN radiation regulating the amount of circumnuclear material and driving powerful outflows into the ISM [ref] .

AGN radiative feedback as the main regulator of [O III] outflow activity and obscuration in X-ray AGN · Outflow incidence in the $N_H - λ_Edd$ plane · 0.99
Such a causal connection has been amply documented in numerical studies (e.g. [ref] ) and further indirectly bolstered by an extensive observational literature showing a clear increase in the AGN fraction in close pairs of galaxies (e.g. [ref] ).

Black hole-galaxy co-evolution and the role of feedback · Interacting galaxies · 1.00
More so, the wind energy deposit can be efficient (e.g., [ref] ).

Impacts of Jets and Winds From Primordial Black Holes · Winds · 0.98

Cites it as background 34 papers

A variety of quenching mechanisms have been proposed, including radiative and mechanical feedback from accreting matter, and merger-driven star formation and associated gas depletion [ref] .

Halo-driven Origin and Evolution of Overmassive Black Holes and Little Red Dots · Transition to Halo-thermodynamics driven suppression · 0.89
It suppresses star formation by expelling cold gas through powerful outflows (ejective feedback; [ref] ) and by heating the surrounding medium and preventing further accretion (preventive feedback; [ref] ).

Unveiling the population of massive quenched galaxies at $z\ge2$ in the COLIBRE simulations - II. The role of AGN feedback and environment on their emergence · Introduction · 0.82
Feedback from active galactic nuclei (AGN) may further contribute by heating or expelling gas, though its role relative to gravitational and stellar processes is still under investigation [ref] .

Interplay of Compaction, Quenching, and Black Hole Growth in the Most Massive Galaxies since $z\sim5$: Insights from JWST and Chandra Data · Introduction · 0.95

Discussion

Disagree with the review, or know something it missed? Leave a comment, highlight any passage above to comment on it, or challenge this review formally.

[1] [1]

KR95 Kormendy J., Richstone D., Inward Bound--The Search For Supermassive Black Holes In Galactic Nuclei, Annu. Rev. Astron. Astrophys. , 33 , 581-624 (1995)

View on Pith 1995

[2] [2]

M98 Magorrian, J., et al., The Demography of Massive Dark Objects in Galaxy Centers The Astron. J. , 115 , 2285-2305 (1998)

View on Pith 1998

[3] [3]

FH04 Ferrarese, L., Ford, H.C., Supermassive Black Holes in Galactic Nuclei: Past, Present and Future Research Space Science Reviews , in press (2004)

View on Pith 2004

[4] [4]

FM00 Ferrarese, L., Merritt, D., A Fundamental Relation between Supermassive Black Holes and Their Host Galaxies, The Astrophys. J. , 539 , L1--L4 (2000)

View on Pith 2000

[5] [5]

G00 Gebhardt, K., et al., A Relationship between Nuclear Black Hole Mass and Galaxy Velocity Dispersion, The Astrophys. J. , 539 , L13--L16 (2000)

View on Pith 2000

[6] [6]

KH00 Kauffmann, G., Haehnelt, M., A unified model for the evolution of galaxies and quasar, Mon. Not. R. Astron. Soc. , 311 , 576--588 (2000)

View on Pith 2000

[7] [7]

VHM03 Volonteri, M., Haardt F., Madau, P., The Assembly and Merging History of Supermassive Black Holes in Hierarchical Models of Galaxy Formation, The Astrophys. J. , 582 , 559-573, (2003)

View on Pith 2003

[8] [8]

Wy03 Wyithe, J. S. B., Loeb, A., Self-regulated Growth of Supermassive Black Holes in Galaxies as the Origin of the Optical and X-Ray Luminosity Functions of Quasars, The Astrophys. J. , 595 , 614--623 (2003)

View on Pith 2003

[9] [9]

Gra04 Granato, G.L., De Zotti, G., Silva, L., Bressan, A., Danese, L., A Physical Model for the Coevolution of QSOs and Their Spheroidal Hosts, The Astrophys. J. , 600 , 580-594 (2004)

View on Pith 2004

[10] [10]

MH96 Mihos, J.C., Hernquist, L., Gasdynamics and starbursts in major mergers, The Astrophys. J. , 464 , 641--663 (1996)

View on Pith 1996

[11] [11]

S82 Soltan, A., Masses of quasars, Mon. Not. R. Astron. Soc. , 200 , 115--122 (1982)

View on Pith 1982

[12] [12]

YT02 Yu, Q., Tremaine, S., Observational constraints on growth of massive black holes, Mon. Not. R. Astron. Soc. , 335 , 965-976, (2002)

View on Pith 2002

[13] [13]

H89 Hernquist, L., Tidal triggering of starbursts and nuclear activity in galaxies, Nature , 340 , 687--691, (1989)

View on Pith 1989

[14] [14]

BH91 Barnes, J., Hernquist, L.,

View on Pith

[15] [15]

BH92 Barnes, J., Hernquist, L., Dynamics of interacting galaxies, Annu. Rev. Astron. Astrophys. , 30 , 705--742, (1992)

View on Pith 1992

[16] [16]

SR98 Silk, J., Rees, M., Quasars and galaxy formation, Astr. & Astrophy. , 334 , L1--L4 (1998)

View on Pith 1998

[17] [17]

F99 Fabian, A.C., The obscured growth of massive black holes, Mon. Not. R. Astron. Soc. , 308 , L39--L43 (1999)

View on Pith 1999

[18] [18]

K03 King, A., Black Holes, Galaxy Formation, and the M_ BH - Relation, Mon. Not. R. Astron. Soc. , 596 , L27-L29 (2003)

View on Pith 2003

[19] [19]

CBG03 Chartas, G., Brandt, W. N., Gallagher, S. C., XMM-Newton Reveals the Quasar Outflow in PG 1115+080, The Astrophys. J. , 595 , 85-93, (2003)

View on Pith 2003

[20] [20]

CKG03 Crenshaw, D. M., Kraemer, S. B., George, I. M., Mass Loss from the Nuclei of Active Galaxies, Annu. Rev. Astron. Astrophys. , 41 , 117-167 (2003)

View on Pith 2003

[21] [21]

P03 Pounds, K. A., Reeves, J. N., King, A. R., Page, K. L., O'Brien, P. T., Turner, M. J. L., A high-velocity ionized outflow and XUV photosphere in the narrow emission line quasar PG1211+143, Mon. Not. R. Astron. Soc. , 345 , 705--713, (2003)

View on Pith 2003

[22] [22]

SDH04s Springel, V., Di Matteo, T., Hernquist, L., Modeling feedback from stars and black holes in galaxy mergers, Mon. Not. R. Astron. Soc. , submitted, preprint astro-ph/0411108 at http://xxx.lanl.gov/ (2004)

View on Pith Pith review arXiv 2004

[23] [23]

B52 Bondi, H., On spherically symmetrical accretion, Mon. Not. R. Astron. Soc. , 112 , 195--204, (1952)

View on Pith 1952

[24] [24]

SS73 Shakura, N.I., Sunyaev, R.A., Black holes in binary systems. Observational appearance, Astron. & Astrophys. , 24 , 337--355, (1973)

View on Pith 1973

[25] [25]

SH03 Springel, V., Hernquist, L., Cosmological smoothed particle hydrodynamics simulations: a hybrid multiphase model for star formation, Mon. Not. R. Astron. Soc. , 339 , 289--311, (2003)

View on Pith 2003

[26] [26]

SDH04 Springel, V., Di Matteo, T., Hernquist, L., Black holes in galaxy mergers: The formation of red elliptical galaxies, The Astrophys. J. , in press, (2005)

View on Pith 2005

[27] [27]

SH04 Springel, V., Hernquist, L., Formation of a spiral galaxy in a major merger, The Astrophys. J. , submitted, (2005)

View on Pith 2005

[28] [28]

HMS04 Hasinger G., Miyaji T., Schmidt M., Luminosity Dependent Evolution of Soft X-ray Selected AGN, Astron. & Astroph. , submitted, (2004)

View on Pith 2004

[29] [29]

Bar04 Barger A.J., Cowie L.L., Mushotzky R.F., Yang Y., Wang W.-H, Steffen A.T., Capak P., The Cosmic Evolution of Hard X-ray Selected Active Galactic Nuclei, The Astrophys. J. , in press (2004)

View on Pith 2004

[30] [30]

T02 Tremaine, S., et al., The slope of the black hole mass versus velocity dispersion correlation, The Astrophys. J. , 574 , 740--753 (2002)

View on Pith 2002

[31] [31]

GH04 Greene, J.E., Ho, L.C., Active galactic nuclei with candidate intermediate-mass black holes, The Astrophys. J. , in press, (2004)

View on Pith 2004