Login
Login

List of most massive black holes

{{Short description|None}}

{{pp-protected|reason=Persistent disruptive editing|small=yes}}

File:Black hole - Messier 87 crop max res.jpg at the core of Messier 87, here shown by an image by the Event Horizon Telescope, is among the black holes in this list.]]

This is an ordered list of the most massive black holes so far discovered (and probable candidates), measured in units of solar masses ({{Solar mass|link=yes}}), approximately {{val|2|u=kilograms|ul=|e=30}}.

Introduction

File:SizesCompared-GalaxyOJ287CentralBlackHoles&SolarSystem.jpg]]

A supermassive black hole (SMBH) is an extremely large black hole, on the order of hundreds of thousands to tens of billions of solar masses ({{Solar mass|link=y}}), and is theorized to exist in the center of almost all massive galaxies. In some galaxies, there are even binary systems of supermassive black holes (see the OJ 287 system.) Unambiguous dynamical evidence for SMBHs exists only in a handful of galaxies;{{cite book |last=Merritt|first=David|author-link=David Merritt|title=Dynamics and Evolution of Galactic Nuclei |url=http://press.princeton.edu/titles/10040.html |date=2013 |publisher=Princeton University Press |location=Princeton, NJ |isbn=978-0-691-15860-0 |page=23}} these include the Milky Way, the Local Group galaxies M31 and M32, and a few galaxies beyond the Local Group, e.g. NGC 4395. In these galaxies, the mean square (or root mean square) velocities of the stars or gas rises as ~1/r near the center, indicating a central point mass. In all other galaxies observed to date, the rms velocities are flat, or even falling, toward the center, making it impossible to state with certainty that a supermassive black hole is present. Nevertheless, it is commonly accepted that the center of nearly every galaxy contains a supermassive black hole.{{cite journal |last=King|first=Andrew|date=2003-09-15|title=Black Holes, Galaxy Formation, and the MBH-σ Relation|journal=The Astrophysical Journal Letters |volume=596 |issue=1|pages=L27–L29|arxiv = astro-ph/0308342 |bibcode = 2003ApJ...596L..27K |doi = 10.1086/379143 |s2cid=9507887}} The reason for this assumption is the M–sigma relation, a tight (low scatter) relation between the mass of the hole in the ~10 galaxies with secure detections, and the velocity dispersion of the stars in the bulges of those galaxies.{{cite journal |bibcode=2000ApJ...539L...9F |last1=Ferrarese| first1=Laura|last2=Merritt| first2=David|author-link2=David Merritt|date=2000-08-10|title=A Fundamental Relation between Supermassive Black Holes and Their Host Galaxies|journal=The Astrophysical Journal|publisher=The American Astronomical Society |pages=L9–12|doi=10.1086/312838|issue=1|volume=539|arxiv = astro-ph/0006053 |s2cid=6508110}} This correlation, although based on just a handful of galaxies, suggests to many astronomers a strong connection between the formation of the black hole and the galaxy itself.

Although SMBHs are currently theorized to exist in almost all massive galaxies, more massive black holes are rare; with only fewer than several dozen having been discovered to date. There is extreme difficulty in determining the mass of a particular SMBH, and so they still remain in the field of open research. SMBHs with accurate masses are limited only to galaxies within the Laniakea Supercluster and to active galactic nuclei.

Another problem for this list is the method used in determining the mass. Such methods, such as broad emission-line reverberation mapping (BLRM), Doppler measurements, velocity dispersion, and the aforementioned M–sigma relation have not yet been well established. Most of the time, the masses derived from the given methods contradict each other's values.

This list contains supermassive black holes with known masses, determined at least to the order of magnitude. Some objects in this list have two citations, like 3C 273; one from Bradley M. Peterson et al. using the BLRM method,{{cite journal

| doi = 10.1007/s11214-013-9987-4

| title = Measuring the Masses of Supermassive Black Holes

| journal = Space Science Reviews

| volume = 183

| issue = 1–4

| page = 253

| url = http://www.astronomy.ohio-state.edu/~peterson/Docs/petersonISSI.pdf

| year = 2013

| last1 = Peterson

| first1 = Bradley M.

| bibcode = 2014SSRv..183..253P

| s2cid = 16464532

| access-date = 2015-03-12

| archive-date = 2019-07-26

| archive-url = https://web.archive.org/web/20190726032645/http://www.astronomy.ohio-state.edu/~peterson/Docs/petersonISSI.pdf

| url-status = dead

}} and the other from Charles Nelson using [OIII]λ5007 value and velocity dispersion.{{cite journal|doi=10.1086/317314|title=Black Hole Mass, Velocity Dispersion, and the Radio Source in Active Galactic Nuclei|journal=The Astrophysical Journal|volume=544|issue=2|pages=L91–L94|year=2000|last1=Nelson|first1=Charles H.|bibcode=2000ApJ...544L..91N|arxiv = astro-ph/0009188 |s2cid=117449813}} Note that this list is very far from complete, as the Sloan Digital Sky Survey (SDSS) alone detected {{val|200,000}} quasars, which likely may be the homes of billion-solar-mass black holes. In addition, there are several hundred citations for black hole measurements not yet included on this list. Despite this, the majority of well-known black holes above 1 billion {{Solar mass|link=y}} are shown. Messier galaxies with precisely known black holes are all included.

New discoveries suggest that many black holes, dubbed 'stupendously large', may exceed {{solar mass|100 billion or even 1 trillion}}.{{Cite web|last=September 2020|first=Paul Sutter 29|title=Black holes so big we don't know how they form could be hiding in the universe|url=https://www.space.com/ginormous-black-holes-could-lurk-in-universe.html|access-date=2021-02-06|website=Space.com|date=29 September 2020|language=en}}

List

{{expand list|date=June 2017}}

Due to the very large numbers involved, the listed black holes have their mass values in scientific notation (numbers multiplied to powers of 10). Values with uncertainties are written in parentheses when possible. Note that different entries in this list have different methods and systematics in obtaining their mass values, and hence different levels of confidence in their masses. These methods are specified in their notes.

{{sticky header}}

class="wikitable sortable sticky-header"

|+ List of most massive black holes

! Host or black hole name

! Mass ({{Solar mass|link=y}})

!class=unsortable|Notes

style="background:#e6e6e6" class="sortbottom"

|(Maximal Theoretical Limit)

{{val|2.7|e=11}}This is the maximum mass of a black hole that models predict, at least for luminous accreting SMBHs. At around 1010 {{Solar mass}}, effects of both intense radiation and star formation in the accretion disc slow down black hole growth. Given the age of the universe and the composition of available matter, there is simply not enough time to grow black holes larger than this mass.

The limit is only {{solar mass|{{val|5|e=10}}}} for black holes with typical properties, but can reach {{solar mass|{{val|2.7|e=11}}}} at maximal prograde spin (a = 1).{{efn|name="Limit"|{{cite journal | title=How big can a black hole grow? | last1=King | first1=Andrew | journal=Monthly Notices of the Royal Astronomical Society: Letters | volume=456 | issue=1 | pages=L109–L112 | date=February 2016 | doi=10.1093/mnrasl/slv186 | doi-access=free | bibcode=2016MNRAS.456L.109K | arxiv=1511.08502 | s2cid=40147275 }}{{cite web | url=https://futurism.com/is-there-a-size-limit-to-how-large-a-black-hole-can-become | title=Is There a Limit to How Large Black Holes Can Become? | first1=Jaime | last1=Trosper | date=May 5, 2014 | website=futurism.com | access-date=November 27, 2018}}{{cite web | url=https://www.science.org/content/article/limit-how-big-black-holes-can-grow-astonishing | title=Limit to how big black holes can grow is astonishing | first1=Daniel | last1=Clery | date=December 21, 2015 | website=sciencemag.org | access-date=November 27, 2018}}{{cite web | url=https://www2.le.ac.uk/offices/press/press-releases/2015/december/black-holes-could-grow-as-large-as-50-billion-suns-before-their-food-crumbles-into-stars-research-shows | title=Black holes could grow as large as 50 billion suns before their food crumbles into stars, research shows | publisher=University of Leicester | access-date=November 27, 2018 | archive-date=October 25, 2021 | archive-url=https://web.archive.org/web/20211025005826/https://www2.le.ac.uk/offices/press/press-releases/2015/december/black-holes-could-grow-as-large-as-50-billion-suns-before-their-food-crumbles-into-stars-research-shows | url-status=dead }}}}

SDSS J123132.37+013814.1{{val|1.12|0.28|0.23|e=11}}{{cite journal | url=https://ui.adsabs.harvard.edu/abs/2020ApJS..249...17R/abstract | bibcode=2020ApJS..249...17R | title=Spectral Properties of Quasars from Sloan Digital Sky Survey Data Release 14: The Catalog | last1=Rakshit | first1=Suvendu | last2=Stalin | first2=C. S. | last3=Kotilainen | first3=Jari | journal=The Astrophysical Journal Supplement Series | date=2020 | volume=249 | issue=1 | page=17 | doi=10.3847/1538-4365/ab99c5 | doi-access=free | arxiv=1910.10395 }}{{cite web | url=https://vizier.cds.unistra.fr/viz-bin/VizieR-5?-ref=VIZ672025b136fc47&-out.add=.&-source=J/ApJS/249/17/dr14qpsp&recno=374296 | title=VizieR }}Estimated using C IV emission line spectra.
Phoenix A{{val|1|e=11}},{{cite journal |title=Unveiling Gargantua: A new search strategy for the most massive central cluster black holes |journal=Astronomy & Astrophysics |last1=Brockamp |first1=M. |last2=Baumgardt |first2=H. |last3=Britzen |first3=S. |last4=Zensus |first4=A. |volume=585 |at=A153 |date=January 2016 |doi=10.1051/0004-6361/201526873 |bibcode=2016A&A...585A.153B |arxiv=1509.04782|s2cid=54641547 }}
~{{val|1.26e10}}		Estimated using a calorimetric model on the adiabatic behavior of core regrowth and an assumed core-Sérsic model of n=4. It is consistent with evolutionary modelling of gas accretion and the dynamics and density profiles of the galaxy. Mass has not been measured directly.

Another recent estimate gives ~{{solar mass|{{val|1.26|e=10}}}},{{Cite journal|last1=Rusinek|first1=Katarzyna|last2=Sikora|first2=Marek|last3=Kozieł-Wierzbowska|first3=Dorota|last4=Gupta|first4=Maitrayee|date=8 September 2020|title=On the Diversity of Jet Production Efficiency in Swift/BAT AGNs|journal=The Astrophysical Journal|volume=900|issue=2|pages=13|bibcode=2020ApJ...900..125R|doi=10.3847/1538-4357/aba75f|arxiv=2006.11049|s2cid=219955960|issn=1538-4357 |doi-access=free }} though this is still uncertain due to low resolution of X-ray/MIR data.

IC 11019.77 {{±|17.14|6.22}} × {{val|e=10}}Estimated from the break radius of the central core; previous estimations using properties of the host galaxy (Faber–Jackson relation) yield about (4-10){{e|10}} {{solar mass}}{{cite journal|last1=Dullo|first1=Bililign T.|last2=Graham|first2=Alister W.|last3=Knapen|first3=Johan H.|title=A remarkably large depleted core in the Abell 2029 BCG IC 1101|journal=Monthly Notices of the Royal Astronomical Society|date=October 2017|volume=471|issue=2|pages=2321–2333|doi=10.1093/mnras/stx1635|doi-access=free |arxiv=1707.02277|bibcode=2017MNRAS.471.2321D|s2cid=119000593}}
SDSS J150848.79+605551.9{{val|6.8|0.42|0.46|e=10}}https://vizier.cds.unistra.fr/viz-bin/VizieR-5?-ref=VIZ6754269ef2e75&-out.add=.&-source=J/ApJS/249/17/dr14qpsp&recno=409784Estimated using MgII emission line correlation.
4C +74.13{{val|5.13|9.66|3.35|e=10}}Produced a colossal AGN outburst after accreting 600 million {{Solar mass}} worth of material.

Estimated using the break radius of 0.5 kpc core of the central galaxy. Previous indirect assumptions about the efficiencies of gas accretion and jet power yield a lower limit of 1 billion {{Solar mass}}.[https://www.sciencedaily.com/releases/2005/01/050106091317.htm Most Powerful Eruption In The Universe Discovered] NASA/Marshall Space Flight Center (ScienceDaily) January 6, 2005{{cite journal

| last1 = McNamara | first1 = B. R.

| last2 = Nulsen | first2 = P. E. J.

| last3 = Wise | first3 = M. W.

| last4 = Rafferty | first4 = D. A.

| last5 = Carilli | first5 = C.

| last6 = Sarazin | first6 = C. L.

| last7 = Blanton | first7 = E. L. | author7-link = Elizabeth Blanton

| title = The heating of gas in a galaxy cluster by X-ray cavities and large-scale shock fronts

| year = 2005

| journal = Nature

| volume = 433

| issue = 7021

| pages = 45–47

| doi = 10.1038/nature03202

| pmid = 15635404

| bibcode = 2005Natur.433...45M

| s2cid = 4340763

}}{{cite journal

| last1 = Rafferty | first1 = D. A.

| last2 = McNamara | first2 = B. R.

| last3 = Nulsen | first3 = P. E. J.

| last4 = Wise | first4 = M. W.

| title = The Feedback-regulated Growth of Black Holes and Bulges through Gas Accretion and Starbursts in Cluster Central Dominant Galaxies

| year = 2006

| journal = The Astrophysical Journal

| volume = 652

| issue = 1

| pages = 216–231

| doi = 10.1086/507672

| arxiv = astro-ph/0605323

| bibcode = 2006ApJ...652..216R

| s2cid = 9481371

}}

style="background:#e6e6e6" class="sortbottom"

|(Typical Theoretical Limit)

{{val|5e10}}This is the maximum mass of a black hole with typical properties that models predict, at least for luminous accreting SMBHs. At around 1010 {{Solar mass}}, effects of both intense radiation and star formation in the accretion disc slow down black hole growth. Given the age of the universe and the composition of available matter, there is simply not enough time to grow black holes larger than this mass.

The limit is only {{solar mass|{{val|5|e=10}}}} for black holes with typical properties, but can reach {{solar mass|{{val|2.7|e=11}}}} at maximal prograde spin (a = 1).{{efn|name="Limit"}}

TON 618{{val|4.07|e=10}}{{cite journal|last1=Ge|first1=Xue|last2=Bi-Xuan|first2=Zhao|last3=Wei-Hao|first3= Bian|last4=Green Richard|first4=Frederick|title=The Blueshift of the C IV Broad Emission Line in QSOs|journal=The Astronomical Journal|date=21 March 2019|volume=157|issue=4|page=14|arxiv=1903.08830|bibcode=2019AJ....157..148G|doi=10.3847/1538-3881/ab0956|s2cid=84842636 |doi-access=free }}Estimated from quasar C IV line correlation. An older estimate gives a mass of {{val|6.6|e=10}}{{Solar mass}} based on the quasar Hβ emission line correlation.{{cite journal|last1=Shemmer|first1=O.|last2=Netzer|first2=H.|last3=Maiolino|first3=R.|last4=Oliva|first4=E.|last5=Croom|first5=S.|last6=Corbett|first6=E.|last7=di Fabrizio|first7=L.|title=Near-infrared spectroscopy of high-redshift active galactic nuclei. I. A metallicity-accretion rate relationship|journal=The Astrophysical Journal|date=2004|volume=614|issue=2|pages=547–557|arxiv=astro-ph/0406559|bibcode=2004ApJ...614..547S|doi=10.1086/423607|s2cid=119010341}}
Holmberg 15A{{val|4.0|0.8}} × {{val|e=10}}{{cite journal

| title = A 40-billion solar mass black hole in the extreme core of Holm 15A, the central galaxy of Abell 85

| year = 2019

| last1 = Mehrgan | first1 = K.

| last2 = Thomas | first2 = J.

| last3 = Saglia | first3 = R.

| last4 = Massalay | first4 = X.

| last5 = Erwin | first5 = P.

| last6 = Bender | first6 = R.

| last7 = Kluge | first7 = M.

| last8 = Fabricius | first8 = M.

| journal = The Astrophysical Journal

| volume = 887

| issue = 2

| page = 195

| arxiv = 1907.10608 | doi = 10.3847/1538-4357/ab5856

| bibcode = 2019ApJ...887..195M

| s2cid = 198899965

| doi-access = free

}}

Mass specified obtained through orbit-based, axisymmetric Schwarzschild models. Earlier estimates range from ~310 billion {{Solar mass}} down to 3 billion {{Solar mass}}, all relying on empirical scaling relations and are thus obtained from extrapolation and not from kinematical measurements.{{cite journal| doi = 10.1088/2041-8205/795/2/L31

| title = The Brightest Cluster Galaxy in Abell 85: The Largest Core Known So Far

| journal = The Astrophysical Journal

| volume = 795

| issue = 2

| pages = L31

| year = 2014

| last1 = López-Cruz | first1 = O.

| last2 = Añorve | first2 = C.

| last3 = Birkinshaw | first3 = M.

| last4 = Worrall | first4 = D. M.

| last5 = Ibarra-Medel | first5 = H. J.

| last6 = Barkhouse | first6 = W. A.

| last7 = Torres-Papaqui | first7 = J. P.

| last8 = Motta | first8 = V.

| arxiv = 1405.7758

| bibcode = 2014ApJ...795L..31L

| s2cid = 1140857

}}

S5 0014+81{{val|4e10}}{{cite journal| title = Chasing the heaviest black holes in active galactic nuclei, the largest black hole

| journal = Monthly Notices of the Royal Astronomical Society

| volume = 405

| issue = 1

| page = 387

| arxiv = 0912.0001

|bibcode = 2010MNRAS.405..387G |doi = 10.1111/j.1365-2966.2010.16449.x | year = 2010

| last1 = Ghisellini

| first1 = G.

| last2 = Ceca

| first2 = R. Della

| last3 = Volonteri

| first3 = M.

| last4 = Ghirlanda

| first4 = G.

| last5 = Tavecchio

| first5 = F.

| last6 = Foschini

| first6 = L.

| last7 = Tagliaferri

| first7 = G.

| last8 = Haardt

| first8 = F.

| last9 = Pareschi

| first9 = G.

| last10 = Grindlay

| first10 = J.

| doi-access = free

| s2cid = 40214759

}}{{Cite journal|last1=Ghisellini|first1=G. |last2=Foschini|first2=L. |arxiv=0906.0575 |title=The blazar S5 0014+813: a real or apparent monster? |journal=Monthly Notices of the Royal Astronomical Society: Letters |volume=399 |issue=1 |pages=L24–L28 |date=14 July 2009 |version=v2 |last3=Volonteri |first3= M. |last4= Ghirlanda |first4=G. |last5= Haardt |first5=F. |last6= Burlon |first6=D. |last7= Tavecchio |first7=F. |doi=10.1111/j.1745-3933.2009.00716.x |doi-access=free |bibcode = 2009MNRAS.399L..24G |s2cid=14438667 |display-authors=etal}}{{cite book |title=Extreme Cosmos: A Guided Tour of the Fastest, Brightest, Hottest, Heaviest, Oldest, and Most Amazing Aspects of Our Universe |url=https://books.google.com/books?id=RNvQsCMq920C&pg=PT103|isbn=978-1-101-58701-0 |last1=Gaensler |first1=Bryan |date=2012-07-03 | publisher=Penguin }}

A 2010 paper suggested that a funnel collimates the radiation around the jet axis, creating an optical illusion of very high brightness, and thus a possible overestimation of the black hole mass.
SDSS J114833.14+193003.2

|{{val|3.631|0.550|0.625|e=10}}{{Cite arxiv|display-authors=etal|author=Melo-Carneiro, Carlos R.|date=19 February 2025|title=Unveiling a 36 Billion Solar Mass Black Hole at the Centre of the Cosmic Horseshoe Gravitational Lens|arxiv=2502.13788v2}}

|

NGC 3842{{val|3.46|6.30|2.24|e=10}}Brightest galaxy in the Leo Cluster; estimation using break radius. Previous estimates yield at least 9.7 billion {{solar mass}}.
SMSS J215728.21-360215.1{{val|3.4|0.6}} × {{val|e=10}}{{citation|title= thirty-four billion solar mass black hole in SMSS J2157–3602, the most luminous known quasar |journal=Monthly Notices of the Royal Astronomical Society |author=Christopher A Onken |author2=Fuyan Bian |author3=Xiaohui Fan |author4=Feige Wang |author5=Christian Wolf |author6=Jinyi Yang |date=August 2020|volume=496|issue=2|page=2309|doi=10.1093/mnras/staa1635|arxiv=2005.06868|bibcode=2020MNRAS.496.2309O|doi-access=free}}Estimated using near-infrared spectroscopic measurements of the MgII emission line doublet.
SDSS J102325.31+514251.0{{val|3.31|0.67|0.56|e=10}}Estimated from quasar MgII emission line correlation.
Abell 1201 BCG{{val|3.27|0.71}} × {{val|e=10}}{{citation |title= Abell 1201: detection of an ultramassive black hole in a strong gravitational lens |author=J W Nightingale |author2=Russell J Smith |author3=Qiuhan He |author4=Conor M O'Riordan |author5=Jacob A Kegerreis |author6=Aristeidis Amvrosiadis |author7=Alastair C Edge |author8=Amy Etherington |author9=Richard G Hayes |author10=Ash Kelly |author11=John R Lucey |author12=Richard J Massey |journal=Monthly Notices of the Royal Astronomical Society|volume =521|issue= 3|pages=3298–3322|doi=10.1093/mnras/stad587|date= May 2023|doi-access=free|arxiv=2303.15514 }} (published online 29 March 2023 )Estimated using strong gravitational lensing from a distant galaxy 1.3 arcseconds separated from the nucleus of the BCG. Earlier estimates suggest a mass of 1.3{{e|10}} {{Solar mass}}.{{cite journal

| last1 = Smith | first1 = R. J.

| last2 = Lucey | first2 = J. R.

| last3 = Edge | first3 = A. C.

| title = A counterimage to the gravitational arc in Abell 1201: Evidence for IMF variations or a 1010 Msun black hole?

| year = 2017

| journal = Monthly Notices of the Royal Astronomical Society

| volume = 467

| issue = 1

| pages = 836–848

| doi = 10.1093/mnras/stx059

| doi-access = free

| arxiv = 1701.02745

| bibcode = 2017MNRAS.467..836S

| s2cid = 59965783

}} Beware of ambiguity between the BH mass determination and the galaxy cluster's dark matter profile.{{cite journal

| last1 = Smith | first1 = R. J.

| last2 = Lucey | first2 = J. R.

| last3 = Edge | first3 = A. C.

| title = Stellar dynamics in the strong-lensing central galaxy of Abell 1201: A low stellar mass-to-light ratio a large central compact mass and a standard dark matter halo

| year = 2017

| journal = Monthly Notices of the Royal Astronomical Society

| volume = 1706

| issue = 1

| pages = 383–393

| arxiv = 1706.07055

| url = http://esoads.eso.org/abs/2017arXiv170607055S

| bibcode = 2017MNRAS.471..383S

| doi=10.1093/mnras/stx1573

| doi-access = free

| s2cid = 54757451

}}

H1821+643{{val|3e10}}Value obtained as an indirect estimate using a model of minimum Eddington luminosity required to account for the Compton cooling of the surrounding cluster.{{cite journal |doi=10.1093/mnras/stu1067| arxiv=1405.7522 |last1 = Walker |first1 = S. A. |title = The effect of the quasar H1821+643 on the surrounding intracluster medium: Revealing the underlying cooling flow | journal=Monthly Notices of the Royal Astronomical Society | volume=442 | issue=3 | page=2809 |last2 = Fabian |first2 = A. C. |last3 = Russell |first3 = H. R. |last4 = Sanders |first4 = J. S. |year = 2014 | doi-access=free | bibcode=2014MNRAS.442.2809W | s2cid=118724526 }}
NGC 6166{{val|2.84|0.27|0.18|e=10}}{{cite journal|last1=Magorrian|first1=J.|last2=Tremaine|first2=S.|last3=Richstone|first3=D.|last4=Bender|first4=R.|last5=Bower|first5=G.|last6=Dressler|first6=A.|last7=Faber|first7=S.~M.|last8=Gebhardt|first8=K.|last9=Green|first9=R.|last10=Grillmair|first10=C.|last11=Kormendy|first11=J.|last12=Lauer|first12=T.|title=The Demography of Massive Dark Objects in Galaxy Centers|journal=The Astronomical Journal|date=June 1998|volume=115|issue=6|pages=2285–2305|doi=10.1086/300353 |arxiv = astro-ph/9708072 |bibcode = 1998AJ....115.2285M |s2cid=17256372}}Central galaxy of Abell 2199; notable for its hundred thousand light year long relativistic jet.
4C +37.11

|{{val|2.8|0.8|0.8|e=10}}{{Cite journal|last1=Surti|first1=Tirth|last2=Romani|first2=Roger W.|last3=Scharwächter|first3=Julia|last4=Peck|first4=Alison|last5=Taylor|first5=Greg B.|date=5 January 2024|journal=The Astrophysical Journal|title=The Central Kinematics and Black Hole Mass of 4C+37.11|volume=960|issue=2|pages=6|bibcode=2024ApJ...960..110S|doi=10.3847/1538-4357/ad14fa|doi-access=free |arxiv=2312.07766|s2cid=266191216|issn=1538-4357}}

|Total mass of black hole binary system.

ESO 383-76{{val|2.75|4.66|1.73|e=10}}Estimated using break radius of the galaxy central core.
2MASS J13260399+7023462{{val|2.7|0.4}} × {{val|e=10}}{{cite journal|doi=10.3847/1538-4357/ab9c95|title=An Extremely Bright QSO at z = 2.89|year=2020|last1=Jeram|first1=Sarik|last2=Gonzalez|first2=Anthony|last3=Eikenberry|first3=Stephen|last4=Stern|first4=Daniel|last5=Mendes De Oliveira|first5=Claudia Lucia|last6=Izuti Nakazono|first6=Lilianne Mariko|last7=Ackley|first7=Kendall|journal=The Astrophysical Journal|volume=899|issue=1|page=76|arxiv=2006.11915|bibcode=2020ApJ...899...76J|s2cid=219966890 |doi-access=free }}Estimated using the full-width half maxima of the CIV emission line and monochromatic luminosity at 1350 Å wavelength.
ESO 444-46{{val|2.69|e=10}}({{val|5.01|e=8}}–{{val|7.76|e=10}}){{cite journal|last=Dullo|first=B.T.|title=The Most Massive Galaxies with Large Depleted Cores: Structural Parameter Relations and Black Hole Masses|journal=The Astrophysical Journal|date=22 November 2019|volume=886|issue=2|page=80|arxiv=1910.10240|bibcode=2019ApJ...886...80D|doi=10.3847/1538-4357/ab4d4f|s2cid=204838306 |doi-access=free }}{{cite journal|last1=Dullo|first1=B.T.|last2=de Paz|first2=A.G.|last3=Knapen|first3=J.H.|title=Ultramassive black holes in the most massive galaxies: MBH−σ versus MBH−Rb|journal=The Astrophysical Journal|date=18 February 2021|volume=908|issue=2|page=134|arxiv=2012.04471|bibcode=2021ApJ...908..134D|doi=10.3847/1538-4357/abceae|s2cid=227745078 |doi-access=free }}Brightest cluster galaxy of Abell 3558 in the center of the Shapley Supercluster; estimated using break radius of the host galaxy.
APM 08279+5255{{val|2.3|e=10}},{{cite journal

| last1 = Riechers | first1 = D. A.

| last2 = Walter | first2 = F.

| last3 = Carilli | first3 = C. L.

| last4 = Lewis | first4 = G. F.

| title = Imaging The Molecular Gas in a z = 3.9 Quasar Host Galaxy at 0farcs3 Resolution: A Central Sub-Kiloparsec Scale Star Formation Reservoir in APM 08279+5255

| year = 2009

| journal = The Astrophysical Journal

| volume = 690

| issue = 1

| pages = 463–485

| doi = 10.1088/0004-637X/690/1/463

| arxiv = 0809.0754

| bibcode = 2009ApJ...690..463R

| s2cid = 13959993

}}
{{val|1.0|0.17|0.13|e=10}}{{cite journal

| last1 = Saturni | first1 = F. G.

| last2 = Trevese | first2 = D.

| last3 = Vagnetti | first3 = F.

| last4 = Perna | first4 = M.

| last5 = Dadina | first5 = M.

| title = A multi-epoch spectroscopic study of the BAL quasar APM 08279+5255. II. Emission- and absorption-line variability time lags

| year = 2016

| journal = Astronomy and Astrophysics

| volume = 587

| pages = A43

| doi = 10.1051/0004-6361/201527152

| arxiv = 1512.03195

| bibcode = 2016A&A...587A..43S

| s2cid = 118548618

}}

Based on velocity width of CO line from orbiting molecular gas, and reverberation mapping using SiIV and CIV emission lines.
NGC 4889{{val|2.1|1.6}} × {{val|e=10}}{{Cite journal|arxiv=1112.1078|last1= McConnell|first1= Nicholas J.|title= Two ten-billion-solar-mass black holes at the centres of giant elliptical galaxies|journal= Nature|volume= 480|issue= 7376|pages= 215–8|last2= Ma|first2= Chung-Pei|author-link2=Chung-Pei Ma|last3= Gebhardt|first3= Karl|last4= Wright|first4= Shelley A.|last5= Murphy|first5= Jeremy D.|last6= Lauer|first6= Tod R.|last7= Graham|first7= James R.|last8= Richstone|first8= Douglas O.|year= 2011|doi= 10.1038/nature10636|pmid= 22158244|bibcode= 2011Natur.480..215M|s2cid= 4408896}}{{cite journal

| last1 = McConnell | first1 = N. J.

| last2 = Ma | first2 = C.-P.

| last3 = Murphy | first3 = J. D.

| last4 = Gebhardt | first4 = K.

| last5 = Lauer | first5 = T. R.

| last6 = Graham | first6 = J. R.

| last7 = Wright | first7 = S. A.

| last8 = Richstone | first8 = D. O.

| title = Dynamical Measurements of Black Hole Masses in Four Brightest Cluster Galaxies at 100 Mpc

| year = 2012

| journal = The Astrophysical Journal

| volume = 756

| issue = 2

| page = 179

| doi = 10.1088/0004-637X/756/2/179

| arxiv = 1203.1620

| bibcode = 2012ApJ...756..179M

| s2cid = 119114155

}}

Best fit: the estimate ranges from 6 billion to 37 billion {{Solar mass}}.
SDSS J074521.78+734336.1{{val|1.95|0.05}} × {{val|e=10}}Estimated from quasar MgII emission line correlation.
OJ 287 primary{{val|1.835e10}}{{Cite journal |last1=Valtonen |first1=Mauri J. |last2=Zola |first2=Staszek |last3=Gopakumar |first3=Achamveedu |last4=Lähteenmäki |first4=Anne |last5=Tornikoski |first5=Merja |last6=Dey |first6=Lankeswar |last7=Gupta |first7=Alok C. |last8=Pursimo |first8=Tapio |last9=Knudstrup |first9=Emil |last10=Gomez |first10=Jose L. |last11=Hudec |first11=Rene |last12=Jelínek |first12=Martin |last13=Štrobl |first13=Jan |last14=Berdyugin |first14=Andrei V. |last15=Ciprini |first15=Stefano |date=2023-08-09 |title=On the need of an ultramassive black hole in OJ 287 |journal=Monthly Notices of the Royal Astronomical Society |volume=525 |issue=1 |pages=1153–1157 |doi=10.1093/mnras/stad2249 |doi-access=free |arxiv=2308.03017 |issn=0035-8711}}A smaller 100 million {{Solar mass}} black hole orbits this one in a 12-year period (see below).
NGC 1600{{val|1.7|0.15}} × {{val|e=10}}{{cite journal

| last1 = Thomas | first1 = J.

| last2 = Ma | first2 = C.-P.

| last3 = McConnell | first3 = N. J.

| last4 = Greene | first4 = J. E.

| last5 = Blakeslee | first5 = J. P.

| last6 = Janish | first6 = R.

| title = A 17-billion-solar-mass black hole in a group galaxy with a diffuse core

| year = 2016

| journal = Nature

| volume = 532

| issue = 7599

| pages = 340–342

| doi = 10.1038/nature17197

| pmid = 27049949

| arxiv = 1604.01400

| bibcode = 2016Natur.532..340T

| s2cid = 4454301

}}{{cite web|url=http://www.nasa.gov/feature/goddard/2016/behemoth-black-hole-found-in-an-unlikely-place|title=Behemoth Black Hole Found in an Unlikely Place|first=Ashley|last=Morrow|date=5 April 2016}}

Unprecedentedly massive in relation of its location: an elliptical galaxy host in a sparse environment.
SDSS J010013.02+280225.8{{val|5.0|e=9}} – {{val|1.58|e=10}}{{Cite journal| arxiv=2211.16261 | last1=Eilers | first1=Anna-Christina | last2=Simcoe | first2=Robert A. | last3=Yue | first3=Minghao | last4=Mackenzie | first4=Ruari | last5=Matthee | first5=Jorryt | last6=Durovcikova | first6=Dominika | last7=Kashino | first7=Daichi | last8=Bordoloi | first8=Rongmon | last9=Lilly | first9=Simon J. | title=EIGER. III. JWST/NIRCam Observations of the Ultraluminous High-redshift Quasar J0100+2802 | journal=The Astrophysical Journal | year=2023 | volume=950 | issue=1 | page=68 | doi=10.3847/1538-4357/acd776 | bibcode=2023ApJ...950...68E | doi-access=free }}
SDSS J08019.69+373047.3{{val|1.51|0.31|e=10}}Estimated from quasar MgII emission line correlation.
SDSS J115954.33+201921.1{{val|1.41|0.10|e=10}}Estimated from quasar MgII emission line correlation.
SDSS J075303.34+423130.8{{val|1.38|0.03|e=10}}{{Cite journal|arxiv =1412.2438 |last1 =Zuo |first1 =Wenwen |title =Black Hole Mass Estimates and Rapid Growth of Supermassive Black Holes in Luminous $z \sim$ 3.5 Quasars |journal =The Astrophysical Journal |volume =799 |issue =2 |page =189 |last2 =Wu |first2 =Xue-Bing |last3 =Fan |first3 =Xiaohui |last4 =Green |first4 =Richard |last5 =Wang |first5 =Ran |last6 =Bian |first6 =Fuyan |year =2014 |doi =10.1088/0004-637X/799/2/189 |bibcode =2015ApJ...799..189Z |s2cid =73642040 }}Estimated from quasar Hβ emission line correlation.
SDSS J080430.56+542041.1{{val|1.35|0.22|e=10}}Estimated from quasar MgII emission line correlation.
SDSS J081855.77+095848.0{{val|1.20|0.06|e=10}}Estimated from quasar MgII emission line correlation.
NGC 1270{{val|1.2|e=10}}{{Cite journal|last1=Ferré-Mateu|first1=Anna|last2=Mezcua|first2=Mar|author2-link=Mar Mezcua|last3=Trujillo|first3=Ignacio|last4=Balcells|first4=Marc|last5=Bosch|first5=Remco C. E. van den|date=2015-07-21|journal=The Astrophysical Journal|language=en|volume=808|issue=1|page=79|doi=10.1088/0004-637X/808/1/79|issn=1538-4357|bibcode=2015ApJ...808...79F|arxiv=1506.02663|title=Massive Relic Galaxies Challenge the Co-Evolution of Super-Massive Black Holes and Their Host Galaxies|s2cid=118777377}}Elliptical galaxy located in the Perseus Cluster. Also is a low-luminosity AGN (LLAGN).{{Cite journal|last1=Park|first1=Songyoun|last2=Yang|first2=Jun|last3=Oonk|first3=J. B. Raymond|last4=Paragi|first4=Zsolt|date=2016-11-22|title=Discovery of five low-luminosity active galactic nuclei at the centre of the Perseus cluster|url=http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1611.05986|journal=Monthly Notices of the Royal Astronomical Society|language=en|volume=465|issue=4|pages=3943–3948|doi=10.1093/mnras/stw3012|doi-access=free |issn=0035-8711|arxiv=1611.05986|bibcode=2017MNRAS.465.3943P|s2cid=53538944}}
SDSS J082535.19+512706.3{{val|1.12|0.20|e=10}}Estimated from quasar Hβ emission line
SDSS J013127.34-032100.1{{val|1.1|0.2|e=10}}{{Cite journal|arxiv = 1501.07269|last1 = Ghisellini|first1 = G.|title = SDSS J013127.34-032100.1: A candidate blazar with a 11 billion solar mass black hole at $z$=5.18|journal = Monthly Notices of the Royal Astronomical Society: Letters|volume = 450|pages = L34–L38|last2 = Tagliaferri|first2 = G.|last3 = Sbarrato|first3 = T.|last4 = Gehrels|first4 = N.|year = 2015|doi = 10.1093/mnrasl/slv042| doi-access=free |bibcode = 2015MNRAS.450L..34G|s2cid = 118449836}}Estimated from accretion disk spectrum modelling.
ICRF J131043.3-555211{{val|1.05|0.02|0.05|e=10}}{{Cite journal|author=Mejía-Restrepo Julian E.|display-authors=etal|date=11 April 2022|title=BASS. XXV. DR2 Broad-line-based Black Hole Mass Estimates and Biases from Obscuration|journal=The Astrophysical Journal Supplement Series|volume=261|issue=1|page=29|bibcode=2022ApJS..261....5M|doi=10.3847/1538-4365/ac6602|doi-access=free|arxiv=2204.05321|s2cid=248118783|issn=1538-4365}}Estimated from MgII emission line correlation.
PSO J334.2028+01.4075{{val|1e10}}There are actually two black holes, orbiting at each other in a close pair with a 542-day period. The largest one is quoted, while the smaller one's mass is not defined.{{Cite journal|arxiv =1503.02083 |last1 =Liu |first1 =Tingting |title =A Periodically Varying Luminous Quasar at z=2 from the Pan-STARRS1 Medium Deep Survey: A Candidate Supermassive Black Hole Binary in the Gravitational Wave-Driven Regime |journal =The Astrophysical Journal |volume =803 |issue =2 |pages =L16 |last2 =Gezari |first2 =Suvi |last3 =Heinis |first3 =Sebastien |last4 = Magnier |first4 =Eugene A. |last5 = Burgett |first5 =William S. |last6 =Chambers |first6 =Kenneth |last7 =Flewelling |first7 =Heather |last8 =Huber |first8 =Mark |last9 = Hodapp |first9 =Klaus W. |last10 =Kaiser |first10 =Nicholas |last11 =Kudritzki |first11 =Rolf-Peter |last12 = Tonry |first12 =John L. |last13 = Wainscoat |first13 =Richard J. |last14 =Waters |first14 =Christopher |year =2015 |doi =10.1088/2041-8205/803/2/L16 |bibcode =2015ApJ...803L..16L |s2cid =118580031 }}
RX J1532.9+3021{{val|1e10}}{{cite journal |arxiv=1306.0907 |title=Probing the extreme realm of AGN feedback in the massive galaxy cluster, RX J1532.9+3021|journal=The Astrophysical Journal |volume=777 |issue=2 |page=163 |doi=10.1088/0004-637X/777/2/163 |year=2013 |last1=Hlavacek-Larrondo |first1=J. |last2=Allen |first2=S. W. |last3=Taylor |first3=G. B. |last4=Fabian |first4=A. C. |last5=Canning |first5=R. E. Ato. |last6=Werner |first6=N. |last7=Sanders |first7=J. S. |last8=Grimes |first8=C. K. |last9=Ehlert |first9=S. |last10=von Der Linden |first10=A. |bibcode=2013ApJ...777..163H |s2cid=118597740 }}

  • {{cite web |title=RX J1532.9+3021: Extreme Power of Black Hole Revealed |website=Chandra X-ray Observatory |url=http://chandra.harvard.edu/photo/2014/rxj1532/}}
QSO B2126-158{{val|1e10}}–{{val|4.9|1.13|1.01|e=10}}Higher value estimated with quasar Hβ emission line correlation.
NGC 1281{{val|1e10}}{{Cite journal|last1=Yıldırım|first1=Akın|last2=Bosch|first2=Van Den|last3=E|first3=Remco C.|last4=van de Ven|first4=Glenn|last5=Dutton|first5=Aaron|last6=Läsker|first6=Ronald|last7=Husemann|first7=Bernd|last8=Walsh|first8=Jonelle L.|last9=Gebhardt|first9=Karl|date=2016-02-11|title=The massive dark halo of the compact early-type galaxy NGC 1281|journal=Monthly Notices of the Royal Astronomical Society|language=en|volume=456|issue=1|pages=538–553|doi=10.1093/mnras/stv2665|doi-access=free |issn=0035-8711|bibcode=2016MNRAS.456..538Y|arxiv=1511.03131|s2cid=118483580}}Compact elliptical galaxy in the Perseus Cluster. Mass estimates range from 10 billion {{Solar mass}} down to <5 billion {{Solar mass}}.
SDSS J015741.57-010629.6{{val|9.8|1.4|e=9}}
SDSS J230301.45-093930.7{{val|9.12|0.88|e=9}}Estimated from quasar MgII emission line correlation.
SDSS J140821.67+025733.2{{val|8e9}}{{Cite journal|doi =10.3847/2515-5172/abd7f9 |last1 =Guo |first1 =Hengxiao |title =The Quasar SDSS J140821.67+025733.2 Does Not Contain a 196 Billion Solar Mass Black Hole |journal =American Astronomical Society |volume =5 |issue =1 |last2 =J. Barth |first2 =Aaron |year =2021 |page =2 |bibcode = 2021RNAAS...5....2G |doi-access =free }}Initially reported the mass of {{val|1.96|e=11|ul=Solar mass}}, making this black hole the most massive one discovered, due to incorrect measurement of its C iv width in the DR12Q catalog, amplified by a correction method that exacerbated the overestimate of mass, based on measurements from the SDSS DR12 Quasar Catalog, the new study report that the mass is estimated {{val|8|e=9|ul=Solar mass}} using quasar MgII emission line correlation.
SDSS J075819.70+202300.9{{val|7.8|3.9|e=9}}Estimated from quasar Hβ emission line correlation.
CID-947{{val|6.9|0.8|1.2|e=9}}{{Cite journal|arxiv =1507.02290 |last1 =Trakhtenbrot |first1 =Benny |title =An Over-Massive Black Hole in a Typical Star-Forming Galaxy, 2 Billion Years After the Big Bang |journal =Science |volume =349 |issue =168 |last2 = Megan Urry |first2 =C. |last3 =Civano |first3 =Francesca |last4 = Rosario |first4 =David J. |last5 =Elvis |first5 =Martin |last6 =Schawinski |first6 =Kevin |last7 =Suh |first7 =Hyewon |last8 =Bongiorno |first8 =Angela |last9 = Simmons |first9 =Brooke D. |year =2015 |bibcode = 2015Sci...349..168T |doi = 10.1126/science.aaa4506 |pmid =26160942 |pages=168–171|s2cid =22406584 }}Constitutes 10% of the total mass of its host galaxy. Estimated from quasar Hβ emission line correlation.
SDSS J080956.02+502000.9{{val|6.46|0.45|e=9}}Estimated from quasar Hβ emission line correlation.
SDSS J014214.75+002324.2{{val|6.31|1.16|e=9}}Estimated from quasar MgII emission line correlation.
Messier 87{{val|7.22|0.34|0.40|e=9}}{{cite journal

| last1 = Oldham | first1 = L. J.

| last2 = Auger | first2 = M. W.

| title = Galaxy structure from multiple tracers – II. M87 from parsec to megaparsec scales

| year = 2016

| journal = Monthly Notices of the Royal Astronomical Society

| volume = 457

| issue = 1

| pages = 421–439

| doi = 10.1093/mnras/stv2982

| doi-access = free

| arxiv = 1601.01323

| bibcode = 2016MNRAS.457..421O

| s2cid = 119166670

}}
{{val|6.3e9}}{{cite journal | author=Walsh, Jonelle L. | author2= Barth, Aaron J. | author3= Ho, Luis C. | author4= Sarzi, Marc | title=The M87 Black Hole Mass from Gas-dynamical Models of Space Telescope Imaging Spectrograph Observations | journal=The Astrophysical Journal | volume=770 | issue=2 |page=86 |date=June 2013 | doi= 10.1088/0004-637X/770/2/86 | bibcode= 2013ApJ...770...86W |arxiv = 1304.7273 | s2cid= 119193955 }}

Central galaxy of the Virgo Cluster; the first black hole directly imaged.
NGC 5419{{val|7.2|2.7|1.9|e=9}}{{cite journal

| last1 = Mazzalay | first1 = X.

| last2 = Thomas | first2 = J.

| last3 = Saglia | first3 = R. P.

| last4 = Wegner | first4 = G. A.

| last5 = Bender | first5 = R.

| last6 = Erwin | first6 = P.

| last7 = Fabricius | first7 = M. H.

| last8 = Rusli | first8 = S. P.

| title = The supermassive black hole and double nucleus of the core elliptical NGC 5419

| year = 2016

| journal = Monthly Notices of the Royal Astronomical Society

| volume = 462

| issue = 3

| pages = 2847–2860

| doi = 10.1093/mnras/stw1802

| doi-access = free

| arxiv = 1607.06466

| bibcode = 2016MNRAS.462.2847M

| s2cid = 119236364

}}

Estimated from the stellar velocity distribution. A secondary satellite SMBH may orbit around 70 parsecs.
SDSS J025905.63+001121.9{{val|5.25|0.73|e=9}}Estimated from quasar Hβ emission line correlation.
SDSS J094202.04+042244.5{{val|5.13|0.71|e=9}}Estimated from quasar Hβ emission line correlation.
QSO B0746+254{{val|5e9}}
QSO B2149-306{{val|5e9}}
SDSS J090033.50+421547.0{{val|4.7|0.2|e=9}}Estimated from quasar MgII emission line correlation.
Messier 60{{val|4.5|1.0|e=9}}{{cite journal|author=Juntai Shen |author2=Karl Gebhardt |date=2010 |title=The Supermassive Black Hole and Dark Matter Halo of NGC 4649 (M60) |journal=The Astrophysical Journal |volume=711 |issue=1 |pages=484–494 |arxiv=0910.4168|doi=10.1088/0004-637X/711/1/484 |bibcode = 2010ApJ...711..484S |s2cid=119291328 }}
SDSS J011521.20+152453.3{{val|4.1|2.4|e=9}}Estimated from quasar Hβ emission line correlation.
QSO B0222+185{{val|4e9}}
Hercules A (3C 348){{val|4e9}}Notable for its million light-year long relativistic jet.
SDSS J075403.60+481428.0

|{{val|3.89|e=9}}

|

SDSS J150752.66+133844.5

|{{val|3.681|e=9}}

|

Abell 1836-BCG{{val|3.61|0.41|0.50|e=9}}{{cite journal

| last1 = Dalla Bontà| first1 = E.

| last2 = Ferrarese | first2 = L.

| last3 = Corsini | first3 = E. M.

| last4 = Miralda-Escudé | first4 = J.

| last5 = Coccato | first5 = L.

| last6 = Sarzi | first6 = M.

| last7 = Pizzella | first7 = A.

| last8 = Beifiori | first8 = A.

| title = The High-Mass End of the Black Hole Mass Function: Mass Estimates in Brightest Cluster Galaxies

| year = 2009

| journal = The Astrophysical Journal

| volume = 690

| issue = 1

| pages = 537–559

| doi = 10.1088/0004-637X/690/1/537

| arxiv = 0809.0766

| bibcode = 2009ApJ...690..537D

| s2cid = 17074507

}}

SDSS J213023.61+122252.0{{val|3.5|0.2|e=9}}Estimated from quasar Hβ emission line correlation.
SDSS J173352.23+540030.4{{val|3.4|0.4|e=9}}Estimated from quasar MgII emission line correlation.
WISE J104222.11+164115.3

|{{val|3.24|e=9}}{{Cite journal|display-authors=etal|author=Glikman, Eliat|date=20 January 2023|title=A Highly Magnified Gravitationally Lensed Red QSO at z = 2.5 with a Significant Flux Ratio Anomaly|journal=The Astrophysical Journal|volume=943|issue=1|pages=22|bibcode=2023ApJ...943...25G|doi=10.3847/1538-4357/aca093|doi-access=free |arxiv=2211.03866|s2cid=253397439|issn=1538-4357}}

|Estimated from quasar Hα line correlation. Another paper suggests much higher masses of {{solar mass|{{val|8.318|0.6|e=10}}}} and {{solar mass|{{val|8.511|2.2|1.8|e=10}}}} based on Hα and Hβ line correlations,{{Cite journal|last1=Matsuoka|first1=K.|last2=Toba|first2=Y.|last3=Shidatsu|first3=M.|last4=Terashima|first4=Y.|last5=Imanshi|first5=M.|last6=Nagao|first6=T.|last7=Marconi|first7=A.|last8=Wang|first8=W. -H.|date=30 November 2018|title=Ratio of black hole to galaxy mass of an extremely red dust-obscured galaxy at z = 2.52|journal=Astronomy & Astrophysics|volume=620|issue=6|pages=L3 |url=https://www.aanda.org/articles/aa/full_html/2018/12/aa33943-18/aa33943-18.html|bibcode=2018A&A...620L...3M|doi=10.1051/0004-6361/201833943|arxiv=1811.07902|s2cid=119211138|issn=0004-6361}} however, this is likely inaccurate due to the model not taking into account the reddening of the AGN.

SDSS J025021.76-075749.9{{val|3.1|0.6|e=9}}Estimated from quasar MgII emission line correlation.
NGC 1271{{Val|3.0|1.0|1.1|e=9}}{{Cite journal|last1=Walsh|first1=Jonelle L.|last2=Bosch|first2=Remco C. E. van den|last3=Gebhardt|first3=Karl|last4=Yildirim|first4=Akin|last5=Gültekin|first5=Kayhan|last6=Husemann|first6=Bernd|last7=Richstone|first7=Douglas O.|date=2015-08-03|url=http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1506.05129|journal=The Astrophysical Journal|language=en|volume=808|issue=2|page=183|doi=10.1088/0004-637X/808/2/183|issn=1538-4357|bibcode=2015ApJ...808..183W|arxiv=1506.05129|title=The Black Hole in the Compact, High-Dispersion Galaxy NGC 1271|s2cid=41570998}}Compact elliptical or lenticular galaxy in the Perseus Cluster.{{Cite journal|last1=Graham|first1=Alister W.|last2=Ciambur|first2=Bogdan C.|last3=Savorgnan|first3=Giulia A. D.|date=2016|title=Disky Elliptical Galaxies and the Allegedly Over-massive Black Hole in the Compact "ES" Galaxy NGC 1271|journal=The Astrophysical Journal|language=en|volume=831|issue=2|page=132|doi=10.3847/0004-637X/831/2/132|issn=0004-637X|bibcode=2016ApJ...831..132G|arxiv=1608.00711|hdl=1959.3/432781|s2cid=118435675 |doi-access=free }}
SDSS J030341.04-002321.9{{val|3.0|0.4|e=9}}Estimated from quasar MgII emission line correlation.
QSO B0836+710{{val|3e9}}
SDSS J162752.18+541912.5

|{{val|2.75|e=9}}

|

SDSS J224956.08+000218.0{{val|2.63|1.21|e=9}}Estimated from quasar Hβ emission line correlation.
SDSS J030449.85-000813.4{{val|2.4|0.50|e=9}}Estimated from quasar Hβ emission line correlation.
SDSS J234625.66-001600.4{{val|2.24|0.15|e=9}}Estimated from quasar Hβ emission line correlation.
ULAS J1120+0641{{val|2e9}}{{cite journal |title=A luminous quasar at a redshift of z = 7.085 |author=Daniel J. Mortlock |author2=Stephen J. Warren |author3=Bram P. Venemans |display-authors=etal |journal=Nature |volume=474 |issue=7353 |pages=616–619 |date=2011 |doi=10.1038/nature10159|pmid=21720366 |arxiv=1106.6088 |bibcode = 2011Natur.474..616M |last4=Patel |last5=Hewett |last6=McMahon |last7=Simpson |last8=Theuns |last9=Gonzáles-Solares |last10=Adamson |last11=Dye |last12=Hambly |last13=Hirst |last14=Irwin |last15=Kuiper |last16=Lawrence |last17=Röttgering |s2cid=2144362 }}{{cite magazine |title=Brilliant, but Distant: Most Far-Flung Known Quasar Offers Glimpse into Early Universe |author=John Matson |date=2011-06-29 |magazine=Scientific American |url=http://www.scientificamerican.com/article.cfm?id=farthest-quasar |access-date=2011-06-30 }}
QSO 0537-286{{val|2e9}}
NGC 3115{{val|2e9}}{{cite journal|bibcode=1992ApJ...393..559K|pages= 559–578|doi=10.1086/171528|title= Evidence for a supermassive black hole in NGC 3115|journal= The Astrophysical Journal|volume= 393|year= 1992|last1= Kormendy|first1= John|last2= Richstone|first2= Douglas}}
Q0906+6930{{val|2e9}}{{cite journal |last=Romani |first=Roger W. |title=The Spectral Energy Distribution of the High-z Blazar Q0906+6930 |journal=The Astronomical Journal |volume=132 |issue=5 |pages=1959–1963 |date=2006 |doi=10.1086/508216 |bibcode=2006AJ....132.1959R |arxiv = astro-ph/0607581 |s2cid=119331684 }}Most distant blazar, at z = 5.47
SDSS J025231.19+034112.7

|{{val|1.51|e=9}}

|

QSO B0805+614{{val|1.5e9}}
Messier 84{{val|1.5e9}}{{cite journal | author=Bower, G.A. | date=1998| title=Kinematics of the Nuclear Ionized Gas in the Radio Galaxy M84 (NGC 4374) | journal=Astrophysical Journal | volume=492 | issue=1 | pages=111–114 | bibcode=1998ApJ...492L.111B | doi=10.1086/311109|arxiv = astro-ph/9710264 | display-authors=1 | last2=Green | first2=R. F. | last3=Danks | first3=A. | last4=Gull | first4=T. | last5=Heap | first5=S. | last6=Hutchings | first6=J. | last7=Joseph | first7=C. | last8=Kaiser | first8=M. E. | last9=Kimble | first9=R. | last10=Kraemer| first10=S.| last11=Weistrop| first11=D.| last12=Woodgate| first12=B.| last13=Lindler| first13=D.| last14=Hill| first14=R. S.| last15=Malumuth| first15=E. M.| last16=Baum| first16=S.| last17=Sarajedini| first17=V.| last18=Heckman| first18=T. M.| last19=Wilson| first19=A. S.| last20=Richstone| first20=D. O.| s2cid=119456112}}
Pōniuāʻena
(J100758.264+211529.207)		{{val|1.5|0.2|e=9}}{{cite journal |title=Pōniuāʻena: A Luminous z=7.5 Quasar Hosting a 1.5 Billion Solar Mass Black Hole |journal=The Astrophysical Journal Letters

|author=Jinyi Yang |author2=Feige Wang |author3=Xiaohui Fan |author4=Joseph F. Hennawi |author5=Frederick B. Davies |author6=Minghao Yue |author7=Eduardo Banados |author8=Xue-Bing Wu |author9=Bram Venemans |author10=Aaron J. Barth |author11=Fuyan Bian |author12=Konstantina Boutsia |author13=Roberto Decarli |author14=Emanuele Paolo Farina |author15=Richard Green |author16=Linhua Jiang |author17=Jiang-Tao Li |author18=Chiara Mazzucchelli |author19=Fabian Walter

|year=2020

|volume=897

|issue=1

|pages=L14

|doi=10.3847/2041-8213/ab9c26

|arxiv=2006.13452

|bibcode=2020ApJ...897L..14Y

|s2cid=220042206

|doi-access=free

}}

Second most-distant quasar known
PKS 2059+034

| {{val|1.36e9}}{{Cite journal|doi = 10.1086/341729|title = Black Hole Mass Estimates of Radio-selected Quasars|year = 2002|last1 = Oshlack|first1 = A. Y. K. N.|last2 = Webster|first2 = R. L.|last3 = Whiting|first3 = M. T.|journal = The Astrophysical Journal|volume = 576|issue = 1|pages = 81–88|arxiv = astro-ph/0205171|bibcode = 2002ApJ...576...81O|s2cid = 15343258}}

|

Abell 3565-BCG{{val|1.34|0.21|0.19|e=9}}
NGC 7768{{val|1.3|0.5|0.4|e=9}}
NGC 1277{{val|1.2e9}}{{cite journal|last1=Graham|first1=Alister W.|last2=Durré|first2=Mark|last3=Savorgnan|first3=Giulia A. D.|last4=Medling|first4=Anne M.|last5=Batcheldor|first5=Dan|last6=Scott|first6=Nicholas|last7=Watson|first7=Beverly|last8=Marconi|first8=Alessandro|title=A Normal Supermassive Black Hole in NGC 1277|journal=The Astrophysical Journal|date=1 March 2016|volume=819|issue=1|page=43|doi=10.3847/0004-637X/819/1/43|issn=0004-637X|bibcode=2016ApJ...819...43G|arxiv = 1601.05151 |s2cid=36974319 |doi-access=free }}Once thought to harbor a black hole so large that it contradicted modern galaxy formation and evolutionary theories,{{cite journal |last1=van den Bosch |first1=Remco C. E. |last2=Gebhardt |first2=Karl |last3=Gültekin |first3=Kayhanl |last4=van de Ven |first4=Glenn |last5=van der Wel |first5=Arjen |last6=Walsh |first6=Jonelle L. |display-authors=1 |title=An over-massive black hole in the compact lenticular galaxy NGC 1277 |journal=Nature |volume=491 |issue=7426 |pages=729–731 |date=29 Nov 2012 |doi=10.1038/nature11592 |arxiv = 1211.6429 |bibcode = 2012Natur.491..729V |pmid=23192149|s2cid=205231230 }} re-analysis of the data revised it downward to roughly a third of the original estimate.{{cite journal |last=Emsellem |first=Eric |title=Is the black hole in NGC 1277 really overmassive? |journal=Monthly Notices of the Royal Astronomical Society |volume=433 |issue=3 |pages=1862–1870 |date=Aug 2013 |doi=10.1093/mnras/stt840 |doi-access=free |bibcode = 2013MNRAS.433.1862E |arxiv = 1305.3630 |s2cid=54011632 }} and then one tenth.
SDSS J233254.46+151305.5

|{{val|1.094|e=9}}

|

QSO B225155+2217{{val|1e9}}
QSO B1210+330{{val|1e9}}
Cygnus A{{val|1e9}}{{cite web|url=http://hubblesite.org/explore_astronomy/black_holes/encyc_mod1_q12.html |title=Black Holes: Gravity's Relentless Pull interactive: Encyclopedia |publisher=HubbleSite |access-date=2015-05-20}}Brightest extrasolar radio source in the sky as seen at frequencies above 1 GHz
Sombrero Galaxy{{val|1e9}}{{cite journal | author=J. Kormendy | author2=R. Bender | author3=E. A. Ajhar| author4=A. Dressler | author5=S. M. Faber| author6=K. Gebhardt | author7=C. Grillmair| author8=T. R. Lauer | author9=D. Richstone| author10=S. Tremaine | date=1996 | title=Hubble Space Telescope Spectroscopic Evidence for a 1 X 10 9 Msun Black Hole in NGC 4594 | journal=Astrophysical Journal Letters | volume=473 | issue=2 | pages=L91–L94 | bibcode=1996ApJ...473L..91K | doi=10.1086/310399| doi-access=free }}Bolometrically most luminous galaxy in the local universe and also the nearest billion-solar-mass black hole to Earth.
Markarian 501{{val|9e8}}–{{val|3.4e9}}{{cite journal|doi=10.1051/0004-6361:20021482|bibcode=2003A&A...397..121R|title=On the central black hole mass in Mkn 501|arxiv=astro-ph/0210326|journal=Astronomy and Astrophysics|volume=397|pages=121–126|year=2003|last1=Rieger|first1=F. M.|last2=Mannheim|first2=K.|s2cid=14579804}}Brightest object in the sky in very high energy gamma rays.
PG 1426+015{{val|1.298|0.385|e=9}}
{{val|467740000}}
3C 109{{val|9.3|e=8}}{{Cite journal |last1=Chalise |first1=Sulov |last2=Lohfink |first2=Anne M. |last3=Kara |first3=Erin |last4=Fabian |first4=Andy C. |date=2020-07-01 |title=Broad-band X-ray observation of broad-line radio galaxy 3C 109 |journal=The Astrophysical Journal |volume=897 |issue=1 |pages=47 |doi=10.3847/1538-4357/ab94a2 |doi-access=free |arxiv=2005.09077 |bibcode=2020ApJ...897...47C |issn=0004-637X}}
3C 273{{val|8.86|1.87|e=8}}
{{val|550000000}}		Brightest quasar in the sky
ULAS J1342+0928{{val|8|e=8}}{{cite journal |author=Bañados, Eduardo |display-authors=et al |title=An 800-million-solar-mass black hole in a significantly neutral Universe at a redshift of 7.5 |date=6 December 2017 |journal=Nature |volume=553 |issue=7689 |pages=473–476 |doi=10.1038/nature25180 |pmid=29211709 |arxiv=1712.01860 |bibcode=2018Natur.553..473B |s2cid=205263326 }}
SDSS J155053.16+052112.1

|{{val|7.94|e=8}}

|

Messier 49{{val|5.6e8}}{{cite journal | display-authors=1 | last1=Loewenstein | first1=Michael | last2=Mushotzky | first2=Richard F. | last3=Angelini | first3=Lorella | last4=Arnaud | first4=Keith A. | last5=Quataert | first5=Eliot | title=Chandra Limits on X-Ray Emission Associated with the Supermassive Black Holes in Three Giant Elliptical Galaxies | journal=The Astrophysical Journal | volume=555 | issue=1 | pages=L21–L24 |date=July 2001 | doi=10.1086/323157 | bibcode=2001ApJ...555L..21L |arxiv = astro-ph/0106326 | s2cid=14873290 | url=https://zenodo.org/record/1235686 }}
NGC 1399{{val|5e8}}{{Cite journal

| last1 = GEBHARDT

| first1 = K.

| last2 = LAUER

| first2 = T. R.

| last3 = PINKNEY

| first3 = J.

| last4 = BENDER

| first4 = R.

| last5 = RICHSTONE

| first5 = D.

| last6 = ALLER

| first6 = M.

| last7 = BOWER

| first7 = G.

| last8 = DRESSLER

| first8 = A.

| date = December 2007

| journal = The Astrophysical Journal

| volume = 671

| issue = 2

| pages = 1321–1328

| title = The Black Hole Mass and Extreme Orbital Structure in NGC 1399

|arxiv = 0709.0585 |bibcode = 2007ApJ...671.1321G |doi = 10.1086/522938 | s2cid = 12042010

}}

Central galaxy of the Fornax Cluster
PG 0804+761{{val|6.93|0.83|e=8}}
{{val|190550000}}
PG 1617+175{{val|5.94|1.38|e=8}}
{{val|275420000}}
PG 1700+518{{val|7.81|+1.82
1.65|e=8}}
{{val|60260000}}
UGC 12591{{val|6.18|2.61|e=8}}{{cite journal | doi=10.1093/mnras/stac2683 | title=Hubble Space Telescope Captures UGC 12591: Bulge/Disc properties, star formation and 'missing baryons' census in a very massive and fast-spinning hybrid galaxy | year=2022 | last1=Ray | first1=Shankar | last2=Bagchi | first2=Joydeep | last3=Dhiwar | first3=Suraj | last4=Pandge | first4=M. B. | last5=Mirakhor | first5=Mohammad | last6=Walker | first6=Stephen A. | last7=Mukherjee | first7=Dipanjan | journal=Monthly Notices of the Royal Astronomical Society | volume=517 | issue=1 | pages=99–117 | doi-access=free | bibcode=2022MNRAS.517...99R | arxiv=2203.02885 }}
SDSS J214611.58-070449.2

|{{val|2.75|e=9}}

|

SDSS J020151.65+012902.5

|{{val|5.37|e=8}}{{Cite journal|last1=Prokhorenko|first1=S. A.|last2=Sazonov|first2=S. Yu.|last3=Gilfanov|first3=M. R.|last4=Balashev|first4=S. A.|last5=Medvedev|first5=P. S.|last6=Starobinsky|first6=A. A.|last7=Sunyaev|first7=R. A.|date=2 March 2024|title=X-ray variability of SDSS quasars based on the SRG/eROSITA all-sky survey|journal=Monthly Notices of the Royal Astronomical Society|volume=528|issue=4|pages=5972–5989|url=https://academic.oup.com/mnras/article/528/4/5972/7588863|bibcode=2024MNRAS.528.5972P|doi=10.1093/mnras/stae261|doi-access=free |arxiv=2401.12860|s2cid=267095212|issn=0035-8711}}

|

SDSS J113029.48+634620.4

|{{val|4.90|e=8}}

|

NGC 4261{{val|4e8}}{{cite web |date=1997-01-13 |title=Massive Black Holes Dwell in Most Galaxies, According to Hubble Census |publisher=Hubblesite STScI-1997-01 |url=http://hubblesite.org/newscenter/archive/releases/1997/01/text/ |access-date=2010-05-02}}Notable for its {{val|88000}} light-year long relativistic jet.{{cite web |title=The Giant Elliptical Galaxy NGC 4261 |publisher=Astronomy 162 (Dept. Physics & Astronomy University of Tennessee) |url=http://csep10.phys.utk.edu/astr162/lect/active/ngc4261.html |access-date=2010-05-02}}
PG 1307+085{{val|4.4|1.23}} × {{val|e=8}},
281 840 000
SDSS J134617.54+622045.5

|{{val|3.98|e=8}}

|

SAGE0536AGN{{val|3.5|0.8}} × {{val|e=8}}{{cite journal

| last1 = van | first1 = Loon J. T.

| last2 = Sansom | first2 = A. E.

| title = An evolutionary missing link? A modest-mass early-type galaxy hosting an oversized nuclear black hole

| year = 2015

| journal = Monthly Notices of the Royal Astronomical Society

| volume = 453

| issue = 3

| pages = 2341–2348

| doi = 10.1093/mnras/stv1787

| doi-access = free

| arxiv = 1508.00698

| bibcode = 2015MNRAS.453.2341V

| s2cid = 56459588

}}{{Cite web|url=https://phys.org/news/2015-09-black-hole-size.html|title=Black hole is 30 times expected size|website=phys.org}}

Constitutes 1.4% of the mass of its host galaxy
NGC 1275{{val|3.4e8}}{{cite journal

| volume = 359

| issue = 2

| pages = 755–764

| last1 = Wilman

| first1 = R. J.

| last2 = Edge

| first2 = A. C.

| last3 = Johnstone

| first3 = R. M.

| title = The nature of the molecular gas system in the core of NGC 1275

| journal = Monthly Notices of the Royal Astronomical Society

| date = 2005

|bibcode = 2005MNRAS.359..755W

| doi = 10.1111/j.1365-2966.2005.08956.x

| doi-access = free

|arxiv = astro-ph/0502537 | s2cid = 18190288

}}

Central galaxy of the Perseus Cluster
3C 390.3{{val|2.87|0.64}} × {{val|e=8}}
{{val|338840000}}
II Zwicky 136{{val|4.57|0.55|e=8}}
{{val|144540000}}
PG 0052+251{{val|3.69|0.76|e=8}}
{{val|218780000}}
Messier 59{{val|2.7e8}}{{cite journal| author=Wrobel, J. M.| author2=Terashima, Y.| author3=Ho, L. C. | date=2008 | title=Outflow-dominated Emission from the Quiescent Massive Black Holes in NGC 4621 and NGC 4697 | journal=The Astrophysical Journal | volume=675 | issue= 2 | pages=1041–1047 | bibcode=2008ApJ...675.1041W | doi=10.1086/527542|arxiv = 0712.1308 | s2cid=119208491}}This black hole has a retrograde rotation.{{cite journal | author=Wernli, F. | author2=Emsellem, E. | author3=Copin, Y. | year=2002 | title=A 60 pc counter-rotating core in NGC 4621 | journal=Astronomy & Astrophysics | volume=396 | pages=73–81 | bibcode=2002A&A...396...73W | doi=10.1051/0004-6361:20021333|arxiv = astro-ph/0209361 | s2cid=18545003 }}
PG 1411+442{{val|4.43|1.46|e=8}}
{{val|79430000}}
Markarian 876{{val|2.79|1.29|e=8}}
{{val|240000000}}
PG 0953+414{{val|2.76|0.59|e=8}}
{{val|182000000}}
PG 0026+129{{val|3.93|0.96|e=8}}
{{val|53700000}}
Fairall 9{{val|2.55|0.56|e=8}}
{{val|79430000}}
NGC 7727

|{{val|1.54|0.18|0.15|e=8}}{{Cite journal|last1=Voggel|first1=K. T.|last2=Seth|first2=A. C.|last3=Baumgardt|first3=H.|last4=Husemann|first4=B.|last5=Neumayer|first5=N.|last6=Hilker|first6=M.|last7=Pechetti|first7=R.|last8=Mieske|first8=S.|last9=Dumont|first9=A.|last10=Georgiev|first10=I.|date=2021-11-30|title=First direct dynamical detection of a dual super-massive black hole system at sub-kpc separation|journal=Astronomy & Astrophysics|volume=658 |pages=A152 |doi=10.1051/0004-6361/202140827|s2cid=244729851 |issn=0004-6361|doi-access=free|arxiv=2111.14854}}

|with {{val|6.3|e=6}} companion and the closest confirmed BBH to Earth at about 89 million light years away

Markarian 1095{{val|1.5|0.19|e=8}}
{{val|182000000}}
Andromeda Galaxy
(Messier 31)		{{val|1.41|0.63|4.4|e=8}},
{{val|6.22|3.19|2.11|e=7}},
{{val|9.4|8.1|4.35|e=7}},
{{val|6.98|7.88|3.29|e=7}},
{{val|3.74|11.43|1.39|e=7}},
{{val|1.19|2.41|0.8|e=8}},
{{val|4.36|3.57|1.96|e=7}},
{{val|2.96|3.08|1.51|e=7}}{{Cite journal|last1=Al-Baidhany|first1=Ismaeel A.|last2=Chiad|first2=Sami S.|last3=Jabbar|first3=Wasmaa A.|last4=Al-Kadumi|first4=Ahmed K.|last5=Habubi|first5=Nadir F.|last6=Mansour|first6=Hazim L.|date=4 December 2020|title=Determine the mass of supermassive black hole in the centre of M31 in different methods|journal=AIP Conference Proceedings|series=International Conference of Numerical Analysis and Applied Mathematics Icnaam 2019 |volume=2290|issue=1|page=050050 |url=https://pubs.aip.org/aip/acp/article/2290/1/050050/1003183/Determine-the-mass-of-supermassive-black-hole-in|bibcode=2020AIPC.2290e0050A|doi=10.1063/5.0027838|doi-access=free}}		Nearest large galaxy to the Milky Way. Masses measured with different methods.
OJ 287 secondary{{val|1.5e8}}The smaller black hole orbiting OJ 287 primary (see above).
PG 1211+143{{val|1.46|0.44}} × {{val|e=8}},
{{val|40740000}}
Messier 105{{val|1.4e8}}–{{val|2e8}}{{cite journal | author=Thilker, David A. | author2=Donovan, Jennifer | author3=Schiminovich, David | author4=Bianchi, Luciana | author5=Boissier, Samuel | author6=Gil de Paz | author7= Armando | author8=Madore, Barry F. | author9=Martin, D. Christopher | author10=Seibert, Mark | date=2009 | title=Massive star formation within the Leo 'primordial' ring | journal=Nature | volume=457 | issue=7232 | pages=990–993 | bibcode=2009Natur.457..990T | doi=10.1038/nature07780 | pmid=19225520| s2cid=4424307 }}
Markarian 509{{val|1.43|0.12}} × {{val|e=8}},
{{val|57550000}}
RX J124236.9-111935{{val|1e8}}Observed by the Chandra X-ray Observatory to be tidally disrupting a star.{{cite journal | last1 = Komossa | first1 = S. | last2 = Halpern | first2 = J. | last3 = Schartel | first3 = N. | last4 = Hasinger | first4 = G. |last5 = Santos-Lleo | first5 = M. | last6 = Predehl | first6 = P. | title = A Huge Drop in the X-Ray Luminosity of the Nonactive Galaxy RX J1242.6-1119A, and the First Postflare Spectrum: Testing the Tidal Disruption Scenario | journal = The Astrophysical Journal Letters | volume = 603 | issue = 1 | pages = L17–L20 | date = May 2004 |arxiv = astro-ph/0402468 |bibcode = 2004ApJ...603L..17K |doi = 10.1086/382046 | s2cid = 53724998 }}NASA: [http://www.nasa.gov/home/hqnews/2004/feb/HQ_04061_black_hole.html "Giant Black Hole Rips Apart Unlucky Star"]
Messier 85{{val|1e8}}{{cite journal

| author=Kormendy, John

| author2=Bender, Ralf

| date=2009

| title=Correlations between Supermassive Black Holes, Velocity Dispersions, and Mass Deficits in Elliptical Galaxies with Cores

| journal=Astrophysical Journal Letters

| volume=691 | issue=2 | pages=L142–L146

| bibcode=2009ApJ...691L.142K

| doi=10.1088/0004-637X/691/2/L142|arxiv = 0901.3778 | s2cid=18919128

}}

NGC 5548{{val|6.71|0.26}} × {{val|e=7}}
{{val|123000000}}
Messier 88{{val|8e7}}
Messier 81
(Bode's Galaxy)		{{val|7e7}}{{cite journal | author=N. Devereux | author2= H. Ford | author3=Z. Tsvetanov | author4=J. Jocoby | name-list-style=amp | date=2003 | title=STIS Spectroscopy of the Central 10 Parsecs of M81: Evidence for a Massive Black Hole | journal=Astronomical Journal | volume=125 | issue=3 | pages=1226–1235 | bibcode=2003AJ....125.1226D | doi=10.1086/367595| doi-access=free }}
Markarian 771{{val|7.32|3.52}} × {{val|e=7}}
{{val|7.586e7}}
Messier 58{{val|7e7}}{{cite journal | author=Merloni, Andrea | author2=Heinz, Sebastian | author3=di Matteo, Tiziana|author3-link=Tiziana Di Matteo (astrophysicist) | date=2003 | title=A Fundamental Plane of black hole activity | journal=Monthly Notices of the Royal Astronomical Society | volume=345 | issue=4 | pages=1057–1076 | bibcode=2003MNRAS.345.1057M | doi=10.1046/j.1365-2966.2003.07017.x|arxiv = astro-ph/0305261 | s2cid=14310323 }}
PG 0844+349{{val|9.24|3.81}} × {{val|e=7}}
{{val|2.138e7}}
Centaurus A{{val|5.5e7}}{{cite web|title=Radio Telescopes Capture Best-Ever Snapshot of Black Hole Jets|date=20 May 2011 |url=http://www.nasa.gov/topics/universe/features/radio-particle-jets.html|publisher=NASA|access-date=2012-10-02}}Also notable for its million light-year long relativistic jet.{{Cite APOD|title=Centaurus Radio Jets Rising|access-date=2011-04-16|date=2011-04-13}}
Markarian 79{{val|5.24|1.44}} × {{val|e=7}}
{{val|5.25e7}}
Messier 96{{val|4.8e7}}
({{val|48000000}}){{cite journal | display-authors=1 | last1=Nowak | first1=N. | last2=Thomas | first2=J. | last3=Erwin | first3=P. | last4=Saglia | first4=R. P. | last5=Bender | first5=R. | last6=Davies | first6=R. I. | title=Do black hole masses scale with classical bulge luminosities only? The case of the two composite pseudo-bulge galaxies NGC 3368 and NGC 3489. | journal=Monthly Notices of the Royal Astronomical Society | volume=403 | issue=2 | pages=646–672 |date=April 2010 | doi=10.1111/j.1365-2966.2009.16167.x | doi-access=free | bibcode=2010MNRAS.403..646N |arxiv = 0912.2511 | s2cid=59580555 }}		Estimates can be as low as 1.5 million solar masses
Markarian 817{{val|4.94|0.77}} × {{val|e=7}}
{{val|4.365e7}}
NGC 3227{{val|4.22|2.14}} × {{val|e=7}}
{{val|3.89e7}}
NGC 4151 primary{{val|4e7}}{{cite web|title=NGC 4151: An active black hole in the "Eye of Sauron"|url=http://www.astronomy.com/News-Observing/News/2011/03/NGC%204151%20active%20black%20hole%20in%20the%20Eye%20of%20Sauron.aspx|publisher=Astronomy magazine|access-date=2011-03-14|date=2011-03-11|archive-date=2019-03-29|archive-url=https://web.archive.org/web/20190329112815/http://www.astronomy.com/News-Observing/News/2011/03/NGC|url-status=dead}}{{cite journal| arxiv=1209.4524 | author1=Bon | author2=Jovanović | author3=Marziani | author4=Shapovalova | author5=Bon | author6=Borka Jovanović | author7=Borka | author8=Sulentic | author9=Popović | title=The First Spectroscopically Resolved Sub-parsec Orbit of a Supermassive Binary Black Hole | journal=The Astrophysical Journal | volume=759 | issue=2 | pages=118–125 | date=2012| doi=10.1088/0004-637X/759/2/118 |bibcode = 2012ApJ...759..118B | s2cid=119257514 }}A small black hole of {{val|10e6|ul=Solar mass}} orbits this one (see below)
3C 120{{val|5.55|3.14|2.25|e=7}}
{{val|2.29e7}}
Markarian 279{{val|3.49|0.92}} × {{val|e=7}}
{{val|4.17e7}}
NGC 3516{{val|4.27|1.46}} × {{val|e=7}}
{{val|2.3e7}}
NGC 863{{val|4.75|0.74}} × {{val|e=7}}
{{val|1.77e7}}
Messier 82
(Cigar Galaxy)		{{val|3e7}}{{cite journal | author=Gaffney, N. I. | author2=Lester, D. F. | author3=Telesco, C. M. | name-list-style=amp | date = 1993 | title = The stellar velocity dispersion in the nucleus of M82 | journal=Astrophysical Journal Letters | volume = 407 | pages = L57–L60 | doi = 10.1086/186805 | bibcode = 1993ApJ...407L..57G}}Prototype starburst galaxy.{{cite journal | last1 = Barker | first1 = S. | last2 = de Grijs | first2 = R. | last3 = Cerviño | first3 = M. | date = 2008 | title = Star cluster versus field star formation in the nucleus of the prototype starburst galaxy M 82 | journal=Astronomy and Astrophysics | volume = 484 | issue = 3 | pages = 711–720 | bibcode = 2008A&A...484..711B | doi = 10.1051/0004-6361:200809653|arxiv = 0804.1913 | s2cid = 18885080 }}
Messier 108{{val|2.4e7}}{{cite journal

| author=Satyapal, S.|author-link=Shobita Satyapal

|display-authors=etal

| date=2008

| title=Spitzer Uncovers Active Galactic Nuclei Missed by Optical Surveys in Seven Late-Type Galaxies

| journal=Astrophysical Journal

| volume=677 | issue=2 | pages=926–942

| doi=10.1086/529014

| bibcode=2008ApJ...677..926S

|arxiv = 0801.2759 |last2=Vega

|first2=D.

|last3=Dudik

|first3=R. P.

|last4=Abel

|first4=N. P.

|last5=Heckman

|first5=T.

|s2cid=16050838

}}

M60-UCD1{{val|2e7}}{{cite journal

| author=Strader, J.

| display-authors=etal

| date=2013

| title=The Densest Galaxy

| journal=The Astrophysical Journal

| volume=775

| issue=1

| pages=L6

| bibcode=2013ApJ...775L...6S

| arxiv=1307.7707

| doi=10.1088/2041-8205/775/1/L6| s2cid=52207639

}}

Constitutes 15% of the mass of its host galaxy.
NGC 3783{{val|2.98|0.54}} × {{val|e=7}}
{{val|9300000}}
Markarian 110{{val|2.51|0.61}} × {{val|e=7}}
{{val|5620000}}
Markarian 335{{val|1.42|0.37}} × {{val|e=7}}
{{val|6310000}}
NGC 4151 secondary{{val|10e6}}
({{val|10000000}})		Orbiting larger companion (see above)
NGC 7469{{val|12.2|1.4}} × {{val|e=6}},
{{val|6460000}}
IC 4329 A{{val|9.90|+17.88
11.88|e=6}},
{{val|5010000}}
NGC 4593{{val|5.36|+9.37
6.95|e=6}},
{{val|8130000}}
Messier 61{{val|5e6}}{{cite journal

| last1=Pastorini |first1=G. |last2=Marconi |first2=A. |last3=Capetti |first3=A. |last4=Axon |first4=D. J. |last5=Alonso-Herrero |first5=A.|author5-link=Almudena Alonso-Herrero |last6=Atkinson |first6=J. |author7-link=Daniel Batcheldor |last7=Batcheldor, D.|last8=Carollo |first8=C. M. | author-link8= C. Marcella Carollo| last9=Collett |first9=J. |last10=Dressel |first10=L. |last11=Hughes |first11=M. A. |last12=Macchetto |first12=D. |last13=Maciejewski |first13=W. |last14=Sparks |first14=W. |last15=van der Marel |first15=R.

| date=2007

| title=Supermassive black holes in the Sbc spiral galaxies NGC 3310, NGC 4303 and NGC 4258

| journal=Astronomy and Astrophysics

| volume=469 |issue=2 |pages=405–423

| doi=10.1051/0004-6361:20066784

| bibcode=2007A&A...469..405P

| arxiv=astro-ph/0703149

|s2cid=849621 }}

Sagittarius A*{{val|4.3e6}}{{cite journal | author = Ghez, A. M. |display-authors=etal | title = Measuring Distance and Properties of the Milky Way's Central Supermassive Black Hole with Stellar Orbits | journal = Astrophysical Journal | date = 2008 | volume = 689 | issue = 2 | pages = 1044–1062 | doi = 10.1086/592738 | bibcode = 2008ApJ...689.1044G | arxiv=0808.2870|last2=Salim |last3=Weinberg |last4=Lu |last5=Do |last6=Dunn |last7=Matthews |last8=Morris |last9=Yelda |last10=Becklin |last11=Kremenek |last12=Milosavljevic |last13=Naiman |s2cid=18335611 }}
({{val|8.54e36|u=kg}})		The black hole at the center of the Milky Way; second black hole directly imaged (after Messier 87)
Messier 32{{val|1.5e6}}–{{val|5e6}}{{Cite journal

| last1 = Valluri | first1 = M.

| last2 = Merritt | first2 = D. |author2-link=David Merritt

| last3 = Emsellem | first3 = E.

| title = Difficulties with Recovering the Masses of Supermassive Black Holes from Stellar Kinematical Data

| journal = Astrophysical Journal

| volume = 602 | issue = 1| pages = 66–92

| date = 2004

| bibcode = 2004ApJ...602...66V

| doi = 10.1086/380896

|arxiv = astro-ph/0210379 | s2cid = 16899097

}}

A dwarf satellite galaxy of the Andromeda Galaxy.
NGC 4395{{val|3.599e5}}{{Cite journal |last1=Peterson |first1=Bradley M. |last2=Bentz |first2=Misty C. |last3=Desroches |first3=Louis-Benoit |last4=Filippenko |first4=Alexei V. |last5=Ho |first5=Luis C. |last6=Kaspi |first6=Shai |last7=Laor |first7=Ari |last8=Maoz |first8=Dan |last9=Moran |first9=Edward C. |last10=Pogge |first10=Richard W. |last11=Quillen |first11=Alice C. |date=2005-10-20 |title=Multiwavelength Monitoring of the Dwarf Seyfert 1 Galaxy NGC 4395. I. A Reverberation-Based Measurement of the Black Hole Mass |journal=The Astrophysical Journal |volume=632 |issue=2 |pages=799–808 |doi=10.1086/444494 |arxiv=astro-ph/0506665 |bibcode=2005ApJ...632..799P |hdl=1811/48314 |s2cid=13886279 |issn=0004-637X}}May be the smallest supermassive black hole.

See also

Notes

{{notelist}}

References

{{Reflist|30em}}

{{Black holes}}

{{portal bar|Astronomy|Physics|Space|Star}}

*

Black holes

Black holes, Most massive

Black holes

Category:Heaviest or most massive things