# List of most massive black holes

This is an ordered list of the most massive black holes so far discovered (and probable candidates), measured in units of solar masses (M$_☉$), approximately 2×10$^{30}$ kilograms.

## Introduction

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 (M$_☉$), 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; 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. 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. 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, and the other from Charles Nelson using [O$_{III}$]λ5007 value and velocity dispersion. Note that this list is very far from complete, as the Sloan Digital Sky Survey (SDSS) alone detected 200000 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 M$_☉$ are shown. Messier galaxies with precisely known black holes are all included.
New discoveries suggest that many black holes, dubbed 'stupendously large', may exceed 100 billion or even 1 trillion M$_☉$.

## List

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.
List of most massive black holes :
| Host or black hole name | Mass (M$_☉$) | Notes |
| (Maximal Theoretical Limit) | 2.7×10$^{11}$ | This is the maximum mass of a black hole that models predict, at least for luminous accreting SMBHs. At around 10$^{10}$ M$_☉$, 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 5×10$^{10}$ M$_☉$ for black holes with typical properties, but can reach 2.7×10$^{11}$ M$_☉$ at maximal prograde spin (a = 1). |
| SDSS J123132.37+013814.1 | 1.12+0.28 −0.23×10$^{11}$ | Estimated using C IV emission line spectra. |
| Phoenix A | 1×10$^{11}$, ~1.26×10$^{10}$ | 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 ~1.26×10$^{10}$ M$_☉$, though this is still uncertain due to low resolution of X-ray/MIR data. |
| IC 1101 | 9.77 $^{+17.14}$ $_{−6.22}$ × 10$^{10}$ | Estimated from the break radius of the central core; previous estimations using properties of the host galaxy (Faber–Jackson relation) yield about (4-10)×10$^{10}$ M$_☉$ |
| SDSS J150848.79+605551.9 | 6.8+0.42 −0.46×10$^{10}$ | Estimated using MgII emission line correlation. |
| 4C +74.13 | 5.13+9.66 −3.35×10$^{10}$ | Produced a colossal AGN outburst after accreting 600 million M$_☉$ 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 M$_☉$. |
| (Typical Theoretical Limit) | 5×10$^{10}$ | This is the maximum mass of a black hole with typical properties that models predict, at least for luminous accreting SMBHs. At around 10$^{10}$ M$_☉$, 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 5×10$^{10}$ M$_☉$ for black holes with typical properties, but can reach 2.7×10$^{11}$ M$_☉$ at maximal prograde spin (a = 1). |
| TON 618 | 4.07×10$^{10}$ | Estimated from quasar C IV line correlation. An older estimate gives a mass of 6.6×10$^{10}$M$_☉$ based on the quasar Hβ emission line correlation. |
| Holmberg 15A | 4.0±0.8 × 10$^{10}$ | Mass specified obtained through orbit-based, axisymmetric Schwarzschild models. Earlier estimates range from ~310 billion M$_☉$ down to 3 billion M$_☉$, all relying on empirical scaling relations and are thus obtained from extrapolation and not from kinematical measurements. |
| S5 0014+81 | 4×10$^{10}$ | 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. |
| NGC 3842 | 3.46+6.30 −2.24×10$^{10}$ | Brightest galaxy in the Leo Cluster; estimation using break radius. Previous estimates yield at least 9.7 billion M$_☉$. |
| SMSS J215728.21-360215.1 | 3.4±0.6 × 10$^{10}$ | Estimated using near-infrared spectroscopic measurements of the MgII emission line doublet. |
| SDSS J102325.31+514251.0 | 3.31+0.67 −0.56×10$^{10}$ | Estimated from quasar MgII emission line correlation. |
| Abell 1201 BCG | 3.27±0.71 × 10$^{10}$ | 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 1.3×10$^{10}$ M$_☉$. Beware of ambiguity between the BH mass determination and the galaxy cluster's dark matter profile. |
| H1821+643 | 3×10$^{10}$ | Value obtained as an indirect estimate using a model of minimum Eddington luminosity required to account for the Compton cooling of the surrounding cluster. |
| NGC 6166 | 2.84+0.27 −0.18×10$^{10}$ | Central galaxy of Abell 2199; notable for its hundred thousand light year long relativistic jet. |
| 4C +37.11 | 2.8+0.8 −0.8×10$^{10}$ | Total mass of black hole binary system. |
| ESO 383-76 | 2.75+4.66 −1.73×10$^{10}$ | Estimated using break radius of the galaxy central core. |
| 2MASS J13260399+7023462 | 2.7±0.4 × 10$^{10}$ | Estimated using the full-width half maxima of the C$_{IV}$ emission line and monochromatic luminosity at 1350 Å wavelength. |
| ESO 444-46 | 2.69×10$^{10}$(5.01×10$^8$–7.76×10$^{10}$) | Brightest cluster galaxy of Abell 3558 in the center of the Shapley Supercluster; estimated using break radius of the host galaxy. |
| APM 08279+5255 | 2.3×10$^{10}$, 1.0+0.17 −0.13×10$^{10}$ | Based on velocity width of CO line from orbiting molecular gas, and reverberation mapping using SiIV and CIV emission lines. |
| NGC 4889 | 2.1±1.6 × 10$^{10}$ | Best fit: the estimate ranges from 6 billion to 37 billion M$_☉$. |
| SDSS J074521.78+734336.1 | 1.95±0.05 × 10$^{10}$ | Estimated from quasar MgII emission line correlation. |
| OJ 287 primary | 1.835×10$^{10}$ | A smaller 100 million M$_☉$ black hole orbits this one in a 12-year period (see below). |
| NGC 1600 | 1.7±0.15 × 10$^{10}$ | Unprecedentedly massive in relation of its location: an elliptical galaxy host in a sparse environment. |
| SDSS J010013.02+280225.8 | 5.0×10$^9$ – 1.58×10$^{10}$ | |
| SDSS J08019.69+373047.3 | (1.51±0.31)×10$^{10}$ | Estimated from quasar MgII emission line correlation. |
| SDSS J115954.33+201921.1 | (1.41±0.10)×10$^{10}$ | Estimated from quasar MgII emission line correlation. |
| SDSS J075303.34+423130.8 | (1.38±0.03)×10$^{10}$ | Estimated from quasar Hβ emission line correlation. |
| SDSS J080430.56+542041.1 | (1.35±0.22)×10$^{10}$ | Estimated from quasar MgII emission line correlation. |
| SDSS J081855.77+095848.0 | (1.20±0.06)×10$^{10}$ | Estimated from quasar MgII emission line correlation. |
| NGC 1270 | 1.2×10$^{10}$ | Elliptical galaxy located in the Perseus Cluster. Also is a low-luminosity AGN (LLAGN). |
| SDSS J082535.19+512706.3 | (1.12±0.20)×10$^{10}$ | Estimated from quasar Hβ emission line |
| SDSS J013127.34-032100.1 | (1.1±0.2)×10$^{10}$ | Estimated from accretion disk spectrum modelling. |
| ICRF J131043.3-555211 | 1.05+0.02 −0.05×10$^{10}$ | Estimated from MgII emission line correlation. |
| PSO J334.2028+01.4075 | 1×10$^{10}$ | 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. |
| RX J1532.9+3021 | 1×10$^{10}$ | |
| QSO B2126-158 | 1×10$^{10}$–4.9+1.13 −1.01×10$^{10}$ | Higher value estimated with quasar Hβ emission line correlation. |
| NGC 1281 | 1×10$^{10}$ | Compact elliptical galaxy in the Perseus Cluster. Mass estimates range from 10 billion M$_☉$ down to <5 billion M$_☉$. |
| SDSS J015741.57-010629.6 | (9.8±1.4)×10$^9$ | |
| SDSS J230301.45-093930.7 | (9.12±0.88)×10$^9$ | Estimated from quasar MgII emission line correlation. |
| SDSS J140821.67+025733.2 | 8×10$^9$ | Initially reported the mass of 1.96×10$^{11}$ M$_☉$, 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 8×10$^9$ M$_☉$ using quasar MgII emission line correlation. |
| SDSS J075819.70+202300.9 | (7.8±3.9)×10$^9$ | Estimated from quasar Hβ emission line correlation. |
| CID-947 | 6.9+0.8 −1.2×10$^9$ | Constitutes 10% of the total mass of its host galaxy. Estimated from quasar Hβ emission line correlation. |
| SDSS J080956.02+502000.9 | (6.46±0.45)×10$^9$ | Estimated from quasar Hβ emission line correlation. |
| SDSS J014214.75+002324.2 | (6.31±1.16)×10$^9$ | Estimated from quasar MgII emission line correlation. |
| Messier 87 | 7.22+0.34 −0.40×10$^9$ 6.3×10$^9$ | Central galaxy of the Virgo Cluster; the first black hole directly imaged. |
| NGC 5419 | 7.2+2.7 −1.9×10$^9$ | Estimated from the stellar velocity distribution. A secondary satellite SMBH may orbit around 70 parsecs. |
| SDSS J025905.63+001121.9 | (5.25±0.73)×10$^9$ | Estimated from quasar Hβ emission line correlation. |
| SDSS J094202.04+042244.5 | (5.13±0.71)×10$^9$ | Estimated from quasar Hβ emission line correlation. |
| QSO B0746+254 | 5×10$^9$ | |
| QSO B2149-306 | 5×10$^9$ | |
| SDSS J090033.50+421547.0 | (4.7±0.2)×10$^9$ | Estimated from quasar MgII emission line correlation. |
| Messier 60 | (4.5±1.0)×10$^9$ | |
| SDSS J011521.20+152453.3 | (4.1±2.4)×10$^9$ | Estimated from quasar Hβ emission line correlation. |
| QSO B0222+185 | 4×10$^9$ | |
| Hercules A (3C 348) | 4×10$^9$ | Notable for its million light-year long relativistic jet. |
| SDSS J075403.60+481428.0 | 3.89×10$^9$ | |
| SDSS J150752.66+133844.5 | 3.681×10$^9$ | |
| Abell 1836-BCG | 3.61+0.41 −0.50×10$^9$ | |
| SDSS J213023.61+122252.0 | (3.5±0.2)×10$^9$ | Estimated from quasar Hβ emission line correlation. |
| SDSS J173352.23+540030.4 | (3.4±0.4)×10$^9$ | Estimated from quasar MgII emission line correlation. |
| WISE J104222.11+164115.3 | 3.24×10$^9$ | Estimated from quasar Hα line correlation. Another paper suggests much higher masses of (8.318±0.6)×10$^{10}$ M$_☉$ and 8.511+2.2 −1.8×10$^{10}$ M$_☉$ based on Hα and Hβ line correlations, however, this is likely inaccurate due to the model not taking into account the reddening of the AGN. |
| SDSS J025021.76-075749.9 | (3.1±0.6)×10$^9$ | Estimated from quasar MgII emission line correlation. |
| NGC 1271 | 3.0+1.0 −1.1×10$^9$ | Compact elliptical or lenticular galaxy in the Perseus Cluster. |
| SDSS J030341.04-002321.9 | (3.0±0.4)×10$^9$ | Estimated from quasar MgII emission line correlation. |
| QSO B0836+710 | 3×10$^9$ | |
| SDSS J162752.18+541912.5 | 2.75×10$^9$ | |
| SDSS J224956.08+000218.0 | (2.63±1.21)×10$^9$ | Estimated from quasar Hβ emission line correlation. |
| SDSS J030449.85-000813.4 | (2.4±0.50)×10$^9$ | Estimated from quasar Hβ emission line correlation. |
| SDSS J234625.66-001600.4 | (2.24±0.15)×10$^9$ | Estimated from quasar Hβ emission line correlation. |
| ULAS J1120+0641 | 2×10$^9$ | |
| QSO 0537-286 | 2×10$^9$ | |
| NGC 3115 | 2×10$^9$ | |
| Q0906+6930 | 2×10$^9$ | Most distant blazar, at z = 5.47 |
| SDSS J025231.19+034112.7 | 1.51×10$^9$ | |
| QSO B0805+614 | 1.5×10$^9$ | |
| Messier 84 | 1.5×10$^9$ | |
| Pōniuāʻena (J100758.264+211529.207) | (1.5±0.2)×10$^9$ | Second most-distant quasar known |
| PKS 2059+034 | 1.36×10$^9$ | |
| Abell 3565-BCG | 1.34+0.21 −0.19×10$^9$ | |
| NGC 7768 | 1.3+0.5 −0.4×10$^9$ | |
| NGC 1277 | 1.2×10$^9$ | Once thought to harbor a black hole so large that it contradicted modern galaxy formation and evolutionary theories, re-analysis of the data revised it downward to roughly a third of the original estimate. and then one tenth. |
| SDSS J233254.46+151305.5 | 1.094×10$^9$ | |
| QSO B225155+2217 | 1×10$^9$ | |
| QSO B1210+330 | 1×10$^9$ | |
| Cygnus A | 1×10$^9$ | Brightest extrasolar radio source in the sky as seen at frequencies above 1 GHz |
| Sombrero Galaxy | 1×10$^9$ | Bolometrically most luminous galaxy in the local universe and also the nearest billion-solar-mass black hole to Earth. |
| Markarian 501 | 9×10$^8$–3.4×10$^9$ | Brightest object in the sky in very high energy gamma rays. |
| PG 1426+015 | (1.298±0.385)×10$^9$ 467740000 | |
| 3C 109 | 9.3×10$^8$ | |
| 3C 273 | (8.86±1.87)×10$^8$ 550000000 | Brightest quasar in the sky |
| ULAS J1342+0928 | 8×10$^8$ | |
| SDSS J155053.16+052112.1 | 7.94×10$^8$ | |
| Messier 49 | 5.6×10$^8$ | |
| NGC 1399 | 5×10$^8$ | Central galaxy of the Fornax Cluster |
| PG 0804+761 | (6.93±0.83)×10$^8$ 190550000 | |
| PG 1617+175 | (5.94±1.38)×10$^8$ 275420000 | |
| PG 1700+518 | 7.81+1.82 −1.65×10$^8$ 60260000 | |
| UGC 12591 | (6.18±2.61)×10$^8$ | |
| SDSS J214611.58-070449.2 | 2.75×10$^9$ | |
| SDSS J020151.65+012902.5 | 5.37×10$^8$ | |
| SDSS J113029.48+634620.4 | 4.90×10$^8$ | |
| NGC 4261 | 4×10$^8$ | Notable for its 88000 light-year long relativistic jet. |
| PG 1307+085 | 4.4±1.23 × 10$^8$, 281 840 000 | |
| SDSS J134617.54+622045.5 | 3.98×10$^8$ | |
| SAGE0536AGN | 3.5±0.8 × 10$^8$ | Constitutes 1.4% of the mass of its host galaxy |
| NGC 1275 | 3.4×10$^8$ | Central galaxy of the Perseus Cluster |
| 3C 390.3 | 2.87±0.64 × 10$^8$ 338840000 | |
| II Zwicky 136 | (4.57±0.55)×10$^8$ 144540000 | |
| PG 0052+251 | (3.69±0.76)×10$^8$ 218780000 | |
| Messier 59 | 2.7×10$^8$ | This black hole has a retrograde rotation. |
| PG 1411+442 | (4.43±1.46)×10$^8$ 79430000 | |
| Markarian 876 | (2.79±1.29)×10$^8$ 240000000 | |
| PG 0953+414 | (2.76±0.59)×10$^8$ 182000000 | |
| PG 0026+129 | (3.93±0.96)×10$^8$ 53700000 | |
| Fairall 9 | (2.55±0.56)×10$^8$ 79430000 | |
| NGC 7727 | 1.54+0.18 −0.15×10$^8$ | with 6.3×10$^6$ companion and the closest confirmed BBH to Earth at about 89 million light years away |
| Markarian 1095 | (1.5±0.19)×10$^8$ 182000000 | |
| Andromeda Galaxy (Messier 31) | 1.41+0.63 −4.4×10$^8$, 6.22+3.19 −2.11×10$^7$, 9.4+8.1 −4.35×10$^7$, 6.98+7.88 −3.29×10$^7$, 3.74+11.43 −1.39×10$^7$, 1.19+2.41 −0.8×10$^8$, 4.36+3.57 −1.96×10$^7$, 2.96+3.08 −1.51×10$^7$ | Nearest large galaxy to the Milky Way. Masses measured with different methods. |
| OJ 287 secondary | 1.5×10$^8$ | The smaller black hole orbiting OJ 287 primary (see above). |
| PG 1211+143 | 1.46±0.44 × 10$^8$, 40740000 | |
| Messier 105 | 1.4×10$^8$–2×10$^8$ | |
| Markarian 509 | 1.43±0.12 × 10$^8$, 57550000 | |
| RX J124236.9-111935 | 1×10$^8$ | Observed by the Chandra X-ray Observatory to be tidally disrupting a star. |
| Messier 85 | 1×10$^8$ | |
| NGC 5548 | 6.71±0.26 × 10$^7$ 123000000 | |
| Messier 88 | 8×10$^7$ | |
| Messier 81 (Bode's Galaxy) | 7×10$^7$ | |
| Markarian 771 | 7.32±3.52 × 10$^7$ 7.586×10$^7$ | |
| Messier 58 | 7×10$^7$ | |
| PG 0844+349 | 9.24±3.81 × 10$^7$ 2.138×10$^7$ | |
| Centaurus A | 5.5×10$^7$ | Also notable for its million light-year long relativistic jet. |
| Markarian 79 | 5.24±1.44 × 10$^7$ 5.25×10$^7$ | |
| Messier 96 | 4.8×10$^7$ (48000000) | Estimates can be as low as 1.5 million solar masses |
| Markarian 817 | 4.94±0.77 × 10$^7$ 4.365×10$^7$ | |
| NGC 3227 | 4.22±2.14 × 10$^7$ 3.89×10$^7$ | |
| NGC 4151 primary | 4×10$^7$ | A small black hole of 10×10$^6$ M$_☉$ orbits this one (see below) |
| 3C 120 | 5.55+3.14 −2.25×10$^7$ 2.29×10$^7$ | |
| Markarian 279 | 3.49±0.92 × 10$^7$ 4.17×10$^7$ | |
| NGC 3516 | 4.27±1.46 × 10$^7$ 2.3×10$^7$ | |
| NGC 863 | 4.75±0.74 × 10$^7$ 1.77×10$^7$ | |
| Messier 82 (Cigar Galaxy) | 3×10$^7$ | Prototype starburst galaxy. |
| Messier 108 | 2.4×10$^7$ | |
| M60-UCD1 | 2×10$^7$ | Constitutes 15% of the mass of its host galaxy. |
| NGC 3783 | 2.98±0.54 × 10$^7$ 9300000 | |
| Markarian 110 | 2.51±0.61 × 10$^7$ 5620000 | |
| Markarian 335 | 1.42±0.37 × 10$^7$ 6310000 | |
| NGC 4151 secondary | 10×10$^6$ (10000000) | Orbiting larger companion (see above) |
| NGC 7469 | 12.2±1.4 × 10$^6$, 6460000 | |
| IC 4329 A | 9.90+17.88 −11.88×10$^6$, 5010000 | |
| NGC 4593 | 5.36+9.37 −6.95×10$^6$, 8130000 | |
| Messier 61 | 5×10$^6$ | |
| Sagittarius A* | 4.3×10$^6$ (8.54×10$^{36}$ kg) | The black hole at the center of the Milky Way; second black hole directly imaged (after Messier 87) |
| Messier 32 | 1.5×10$^6$–5×10$^6$ | A dwarf satellite galaxy of the Andromeda Galaxy. |
| NGC 4395 | 3.599×10$^5$ | May be the smallest supermassive black hole. |