Daftar lubang hitam paling masif
Tampilan
Berikut ini adalah sebuah daftar dari lubang hitam paling masif yang sejauh ini ditemukan (dan kandidat-kandidatnya), yang diukur dalam satuan massa matahari (M☉), sekitar 2×1030 kg.
Daftar
Daftar ini belum tentu lengkap. Anda dapat membantu Wikipedia dengan mengembangkannya. (Juni 2017) |
Nama | Massa matahari (Matahari = 1) |
Catatan |
---|---|---|
TON 618 | 6,6×1010[1] | Estimated from quasar Hβ emission line correlation. |
Holmberg 15A | (4,0±0,8)×1010[2] | 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.[3] |
IC 1101 | (4–10)×1010[4] | Estimated from properties of the host galaxy; mass has not been measured directly. |
S5 0014+81 | 4×1010[5][6][7] | 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.[5] |
SMSS J215728.21-360215.1 | (3,4±0,6)×1010[8] | |
SDSS J102325.31+514251.0 | (3,31±0,61)×1010[9] | Estimated from quasar MgII emission line correlation. |
H1821+643 | 3×1010[10] | Nearest galaxy cluster harboring a quasar in its core.[10] |
NGC 6166 | 3×1010[11] | |
APM 08279+5255 | 2,3×1010[12] 1,0+0,17 −0,13×1010[13] |
Based on velocity width of CO line from orbiting molecular gas,[12] and reverberation mapping using SiIV and CIV emission lines.[13] |
NGC 4889 | (2,1±1,6)×1010[14][15] | Best fit: the estimate ranges from 6 billion to 37 billion M☉.[14][15] |
Central black hole of Phoenix Cluster | 2×1010[16] | This black hole is continuously growing at the rate of ~60 M☉ per year. |
SDSS J074521.78+734336.1 | (1,95±0,05)×1010[9] | Estimated from quasar MgII emission line correlation. |
OJ 287 primary | 1,8×1010[17] | A smaller 100 million M☉ black hole orbits this one in a 12-year period (see OJ 287 secondary below). But this measurement is in question due to the limited number and precision of observed companion orbits. |
NGC 1600 | (1,7±0,15)×1010[18][19] | Unprecedentedly massive in relation of its location: an elliptical galaxy host in a sparse environment. |
SDSS J08019.69+373047.3 | (1,51±0,31)×1010[9] | Estimated from quasar MgII emission line correlation. |
SDSS J115954.33+201921.1 | (1,41±0,10)×1010[9] | Estimated from quasar MgII emission line correlation. |
SDSS J075303.34+423130.8 | (1,38±0,03)×1010[9] | Estimated from quasar Hβ emission line correlation. |
SDSS J080430.56+542041.1 | (1,35±0,22)×1010[9] | Estimated from quasar MgII emission line correlation. |
Abell 1201 BCG | (1,3±0,6)×1010[20] | Estimated from the strong gravitational lensing of a background galaxy behind the BCG.[20] Beware of ambiguity between the BH mass determination and the galaxy cluster's dark matter profile.[21] |
SDSS J0100+2802 | (1,24±0,19)×1010[22][23] | Estimated from quasar MgII emission line correlation. This object grew early in cosmic history (redshift 6.30). |
SDSS J081855.77+095848.0 | (1,20±0,06)×1010[9] | Estimated from quasar MgII emission line correlation. |
NGC 1270 | 1,2×1010[24] | Elliptical galaxy located in the Perseus Cluster. Also is a low-luminosity AGN (LLAGN).[25] |
SDSS J082535.19+512706.3 | (1,12±0,20)×1010[9] | Estimated from quasar Hβ emission line |
SDSS J013127.34-032100.1 | (1,1±0,2)×1010[26] | Estimated from accretion disk spectrum modelling.[26] |
PSO J334.2028+01.4075 | 1×1010[27] | 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.[27] |
Black hole of central elliptical galaxy of RX J1532.9+3021 | 1×1010[28] | |
QSO B2126-158 | 1×1010[5] | |
NGC 1281 | 1×1010[29] | Compact elliptical galaxy in the Perseus Cluster. Mass estimates range from 10 billion M☉ down to <5 billion M☉.[30] |
SDSS J015741.57-010629.6 | (9,8±1,4)×109[9] | |
NGC 3842 | 9,7+3,0 −2,5×109[14][15] |
Brightest galaxy in the Leo Cluster |
SDSS J230301.45-093930.7 | (9,12±0,88)×109[9] | Estimated from quasar MgII emission line correlation. |
SDSS J075819.70+202300.9 | (7,8±3,9)×109[9] | Estimated from quasar Hβ emission line correlation. |
CID-947 | 6,9+0,8 −1,2×109[31] |
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)×109[9] | Estimated from quasar Hβ emission line correlation. |
SDSS J014214.75+002324.2 | (6,31±1,16)×109[9] | Estimated from quasar MgII emission line correlation. |
Messier 87 "Powehi"[32] | 7,22+0,34 −0,40×109[33] 6,3×109[34] |
Central galaxy of the Virgo Cluster; the first black hole directly imaged. |
NGC 5419 | 7,2+2,7 −1,9×109[35] |
Estimated from the stellar velocity distribution. A secondary satellite SMBH may orbit around 70 parsecs.[35] |
SDSS J025905.63+001121.9 | (5,25±0,73)×109[9] | Estimated from quasar Hβ emission line correlation. |
SDSS J094202.04+042244.5 | (5,13±0,71)×109[9] | Estimated from quasar Hβ emission line correlation. |
QSO B0746+254 | 5×109[5] | |
QSO B2149-306 | 5×109[5] | |
SDSS J090033.50+421547.0 | (4,7±0,2)×109[9] | Estimated from quasar MgII emission line correlation. |
Messier 60 | (4,5±1,0)×109[36] | |
SDSS J011521.20+152453.3 | (4,1±2,4)×109[9] | Estimated from quasar Hβ emission line correlation. |
QSO B0222+185 | 4×109[5] | |
Hercules A (3C 348) | 4×109 | Notable for its million light-year long relativistic jet. |
Abell 1836-BCG | 3,61+0,41 −0,50×109[37] |
|
SDSS J213023.61+122252.0 | (3,5±0,2)×109[9] | Estimated from quasar Hβ emission line correlation. |
SDSS J173352.23+540030.4 | (3,4±0,4)×109[9] | Estimated from quasar MgII emission line correlation. |
SDSS J025021.76-075749.9 | (3,1±0,6)×109[9] | Estimated from quasar MgII emission line correlation. |
NGC 1271 | 3,0+1,0 −1,1×109[38] |
Compact elliptical or lenticular galaxy in the Perseus Cluster.[39] |
SDSS J030341.04-002321.9 | (3,0±0,4)×109[9] | Estimated from quasar MgII emission line correlation. |
QSO B0836+710 | 3×109[5] | |
SDSS J224956.08+000218.0 | (2,63±1,21)×109[9] | Estimated from quasar Hβ emission line correlation. |
SDSS J030449.85-000813.4 | (2,4±0,50)×109[9] | Estimated from quasar Hβ emission line correlation. |
SDSS J234625.66-001600.4 | (2,24±0,15)×109[9] | Estimated from quasar Hβ emission line correlation. |
PKS 2128-123 | 2,02×109[40] | |
ULAS J1120+0641 | 2×109[41][42] | |
QSO 0537-286 | 2×109[5] | |
NGC 3115 | 2×109[43] | |
Q0906+6930 | 2×109[44] | Most distant blazar, at z = 5.47 |
QSO B0805+614 | 1,5×109[5] | |
Messier 84 | 1,5×109[45] | |
J100758.264+211529.207 ("Pōniuāʻena") | (1,5±0,2)×109[46] | Second most-distant quasar known |
PKS 2059+034 | 1,36×109[47] | |
Abell 3565-BCG | 1,34+0,21 −0,19×109[37] |
|
NGC 7768 | 1,3+0,5 −0,4×109[15] |
|
NGC 1277 | 1,2×109[48] | Once thought to harbor a black hole so large that it contradicted modern galaxy formation and evolutionary theories,[49] re-analysis of the data revised it downward to roughly a third of the original estimate.[50] and then one tenth.[48] |
Black hole of central elliptical galaxy of MS 0735.6+7421 | 1×109[51][52][53] | Produced a colossal AGN outburst after accreting 600 million M☉ worth of material. BH mass not explicitly stated; just a lower limit. Requires assumptions about the efficiencies of gas accretion and jet power.[51][52][53] |
QSO B225155+2217 | 1×109[5] | |
QSO B1210+330 | 1×109[5] | |
NGC 6166 | 1×109[54] | Central galaxy of Abell 2199; notable for its hundred thousand light year long relativistic jet. |
Cygnus A | 1×109[55] | Brightest extrasolar radio source in the sky as seen at frequencies above 1 GHz |
Sombrero Galaxy | 1×109[56] | Bolometrically most luminous galaxy in the local universe and also the nearest billion-solar-mass black hole to Earth. |
Markarian 501 | 9×108–3,4×109[57] | Brightest object in the sky in very high energy gamma rays. |
PG 1426+015 | (1,298±0,385)×109[58] 467.740.000[59] |
|
3C 273 | (8,86±1,87)×108[58] 550.000.000[59] |
Brightest quasar in the sky |
ULAS J1342+0928 | 8×108[60] | Most distant quasar[60] − currently on record as the most distant quasar at z=7.54[60] |
Messier 49 | 5,6×108[61] | |
NGC 1399 | 5×108[62] | Central galaxy of the Fornax Cluster |
PG 0804+761 | (6,93±0,83)×108[58] 190.550.000[59] |
|
PG 1617+175 | (5,94±1,38)×108[58] 275.420.000[59] |
|
PG 1700+518 | 7,81+1,82 −1,65×108[58] 60.260.000[59] |
|
NGC 4261 | 4×108[63] | Notable for its 88.000 light-year long relativistic jet.[64] |
PG 1307+085 | (4,4±1,23)×108[58] 281 840 000[59] |
|
SAGE0536AGN | (3,5±0,8)×108[65][66] | Constitutes 1.4% of the mass of its host galaxy |
NGC 1275 | 3,4×108[67][68] | Central galaxy of the Perseus Cluster |
3C 390.3 | (2,87±0,64)×108[58] 338.840.000[59] |
|
II Zwicky 136 | (4,57±0,55)×108[58] 144.540.000[59] |
|
PG 0052+251 | (3,69±0,76)×108[58] 218.780.000[59] |
|
Messier 59 | 2,7×108[69] | This black hole has a retrograde rotation.[70] |
PG 1411+442 | (4,43±1,46)×108[58] 79.430.000[59] |
|
Markarian 876 | (2,79±1,29)×108[58] 240.000.000[59] |
|
Andromeda Galaxy | 2,3×108 | Nearest large galaxy to the Milky Way |
PG 0953+414 | (2,76±0,59)×108[58] 182.000.000[59] |
|
PG 0026+129 | (3,93±0,96)×108[58] 53.700.000[59] |
|
Fairall 9 | (2,55±0,56)×108[58] 79.430.000[59] |
|
Markarian 1095 | (1,5±0,19)×108[58] 182.000.000[59] |
|
Messier 105 | 1,4×108–2×108[71] | |
Markarian 509 | (1,43±0,12)×108[58] 57.550.000[59] |
|
OJ 287 secondary | 1×108[17] | The smaller black hole orbiting OJ 287 primary (see above). |
RX J124236.9-111935 | 1×108[72] | Observed by the Chandra X-ray Observatory to be tidally disrupting a star.[72][73] |
Messier 85 | 1×108[74] | |
NGC 5548 | (6,71±0,26)×107[58] 123.000.000[59] |
|
PG 1211+143 | (1,46±0,44)×108[58] 40.740.000[59] |
|
Messier 88 | 8×107[75] | |
Messier 81 (Bode's Galaxy) | 7×107[76] | |
Markarian 771 | (7,32±3,52)×107[58] 7,586×107[59] |
|
Messier 58 | 7×107[77] | |
PG 0844+349 | (9,24±3,81)×107[58] 2,138×107[59] |
|
Centaurus A | 5,5×107[78] | Also notable for its million light-year long relativistic jet.[79] |
Markarian 79 | (5,24±1,44)×107[58] 5,25×107[59] |
|
Messier 96 | 48.000.000[80] | Estimates can be as low as 1.5 million solar masses |
Markarian 817 | (4,94±0,77)×107[58] 4,365×107[59] |
|
NGC 3227 | (4,22±2,14)×107[58] 3,89×107[59] |
|
NGC 4151 primary | 4×107[81][82] | |
3C 120 | 5,55+3,14 −2,25×107[58] 2,29×107[59] |
|
Markarian 279 | (3,49±0,92)×107[58] 4,17×107[59] |
|
NGC 3516 | (4,27±1,46)×107[58] 2,3×107[59] |
|
NGC 863 | (4,75±0,74)×107[58] 1,77×107[59] |
|
Messier 82 (Cigar Galaxy) | 3×107[83] | Prototype starburst galaxy.[84] |
Messier 108 | 2,4×107[85] | |
M60-UCD1 | 2×107[86] | Constitutes 15% of the mass of its host galaxy. |
NGC 3783 | (2,98±0,54)×107[58] 9.300.000[59] |
|
Markarian 110 | (2,51±0,61)×107[58] 5.620.000[59] |
|
Markarian 335 | (1,42±0,37)×107[58] 6.310.000[59] |
|
NGC 4151 secondary | 10.000.000[82] | |
NGC 7469 | (12,2±1,4)×106[58] 6.460.000[59] |
|
IC 4329 A | 9,90+17,88 −11,88×106[58] 5.010.000[59] |
|
NGC 4593 | 5,36+9,37 −6,95×106[58] 8.130.000[59] |
|
Messier 61 | 5×106[87] | |
Messier 32 | 1,5×106–5×106[88] | Sebuah galaksi satelit katai di Galaksi Andromeda. |
Sagittarius A* | 4,3×106[89] | The black hole at the center of the Milky Way. |
Lihat pula
- Daftar struktur kosmik terbesar
- Daftar galaksi terbesar
- Daftar lubang hitam paling tidak masif
- Daftar eksoplanet paling masif
Referensi
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