Khác biệt giữa bản sửa đổi của “Danh sách lỗ đen lớn nhất”

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}}
}}
</ref>
</ref>
||Best fit: the estimate ranges from 6 billion to 37 billion {{Solar mass}}.<ref name="McConnell" /><ref name="mcconnell2012" />
||Best fit: the estimate ranges from 6 billion to 37 billion <i>M</i><sub>&#x2609;</sub>.<ref name="McConnell" /><ref name="mcconnell2012" />
|-
|-
|Black hole of central elliptical galaxy of [[Phoenix Cluster]] || '''{{val|20000000000}}'''<ref name=NATURE>{{cite journal|bibcode=2012Natur.488..349M|title=A massive, cooling-flow-induced starburst in the core of a luminous cluster of galaxies|journal=Nature|volume=488|issue=7411|pages=349–52|last1=McDonald|first1=M.|last2=Bayliss|first2=M.|last3=Benson|first3=B. A.|last4=Foley|first4=R. J.|last5=Ruel|first5=J.|last6=Sullivan|first6=P.|last7=Veilleux|first7=S.|last8=Aird|first8=K. A.|last9=Ashby|first9=M. L. N.|last10=Bautz|first10=M.|last11=Bazin|first11=G.|last12=Bleem|first12=L. E.|last13=Brodwin|first13=M.|last14=Carlstrom|first14=J. E.|last15=Chang|first15=C. L.|last16=Cho|first16=H. M.|last17=Clocchiatti|first17=A.|last18=Crawford|first18=T. M.|last19=Crites|first19=A. T.|last20=De Haan|first20=T.|last21=Desai|first21=S.|last22=Dobbs|first22=M. A.|last23=Dudley|first23=J. P.|last24=Egami|first24=E.|last25=Forman|first25=W. R.|last26=Garmire|first26=G. P.|last27=George|first27=E. M.|last28=Gladders|first28=M. D.|last29=Gonzalez|first29=A. H.|last30=Halverson|first30=N. W.|display-authors=29|year=2012|doi=10.1038/nature11379|pmid=22895340|arxiv = 1208.2962 }}</ref>|| This black hole is continuously growing at the rate of ~60 {{Solar mass}} per year.
|Black hole of central elliptical galaxy of [[Phoenix Cluster]] || '''{{val|20000000000}}'''<ref name=NATURE>{{cite journal|bibcode=2012Natur.488..349M|title=A massive, cooling-flow-induced starburst in the core of a luminous cluster of galaxies|journal=Nature|volume=488|issue=7411|pages=349–52|last1=McDonald|first1=M.|last2=Bayliss|first2=M.|last3=Benson|first3=B. A.|last4=Foley|first4=R. J.|last5=Ruel|first5=J.|last6=Sullivan|first6=P.|last7=Veilleux|first7=S.|last8=Aird|first8=K. A.|last9=Ashby|first9=M. L. N.|last10=Bautz|first10=M.|last11=Bazin|first11=G.|last12=Bleem|first12=L. E.|last13=Brodwin|first13=M.|last14=Carlstrom|first14=J. E.|last15=Chang|first15=C. L.|last16=Cho|first16=H. M.|last17=Clocchiatti|first17=A.|last18=Crawford|first18=T. M.|last19=Crites|first19=A. T.|last20=De Haan|first20=T.|last21=Desai|first21=S.|last22=Dobbs|first22=M. A.|last23=Dudley|first23=J. P.|last24=Egami|first24=E.|last25=Forman|first25=W. R.|last26=Garmire|first26=G. P.|last27=George|first27=E. M.|last28=Gladders|first28=M. D.|last29=Gonzalez|first29=A. H.|last30=Halverson|first30=N. W.|display-authors=29|year=2012|doi=10.1038/nature11379|pmid=22895340|arxiv = 1208.2962 }}</ref>|| This black hole is continuously growing at the rate of ~60 <i>M</i><sub>&#x2609;</sub> per year.
|-
|-
| [[SDSS J074521.78+734336.1]] || '''{{val|1.95|0.05|e=10}}'''<ref name=XA /> ||Estimated from quasar MgII emission line correlation.
| [[SDSS J074521.78+734336.1]] || '''{{val|1.95|0.05|e=10}}'''<ref name=XA /> ||Estimated from quasar MgII emission line correlation.
|-
|-
|[[OJ 287]] primary || '''{{val|18000000000}}'''<ref name="frostbite">{{Cite journal|arxiv =1208.0906 |last1 = Valtonen |first1 = M. J. |title = On the masses of OJ287 black holes |journal = Monthly Notices of the Royal Astronomical Society |volume = 427 |pages = 77 |last2 = Ciprini |first2 = S. |last3 = Lehto |first3 = H. J. |year = 2012 |doi = 10.1111/j.1365-2966.2012.21861.x |bibcode = 2012MNRAS.427...77V }}</ref> || A smaller 100 million {{Solar mass}} 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.
|[[OJ 287]] primary || '''{{val|18000000000}}'''<ref name="frostbite">{{Cite journal|arxiv =1208.0906 |last1 = Valtonen |first1 = M. J. |title = On the masses of OJ287 black holes |journal = Monthly Notices of the Royal Astronomical Society |volume = 427 |pages = 77 |last2 = Ciprini |first2 = S. |last3 = Lehto |first3 = H. J. |year = 2012 |doi = 10.1111/j.1365-2966.2012.21861.x |bibcode = 2012MNRAS.427...77V }}</ref> || A smaller 100 million <i>M</i><sub>&#x2609;</sub> 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]] || '''{{val|1.7|0.15|e=10}}'''<ref name="thomas2016">
| [[NGC 1600]] || '''{{val|1.7|0.15|e=10}}'''<ref name="thomas2016">
Dòng 200: Dòng 200:
| arxiv = 1405.7758
| arxiv = 1405.7758
| bibcode = 2014ApJ...795L..31L
| bibcode = 2014ApJ...795L..31L
}}</ref>|| Mass estimates range from ~310 billion {{Solar mass}} down to 3 billion {{Solar mass}}. They all rely on empirical scaling relations and are thus obtained from extrapolation and not from kinematical measurements.
}}</ref>|| Mass estimates range from ~310 billion <i>M</i><sub>&#x2609;</sub> down to 3 billion <i>M</i><sub>&#x2609;</sub>. They all rely on empirical scaling relations and are thus obtained from extrapolation and not from kinematical measurements.
|-
|-
| [[SDSS J015741.57-010629.6]] || '''{{val|9.8|1.4|e=9}}'''<ref name=XA /> ||Estimated from quasar MgII emission line correlation.
| [[SDSS J015741.57-010629.6]] || '''{{val|9.8|1.4|e=9}}'''<ref name=XA /> ||Estimated from quasar MgII emission line correlation.
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||
||
|-
|-
|Black hole of central elliptical galaxy of [[MS 0735.6+7421]] || '''{{val|1|e=9}}'''<ref name=DS/><ref name="mcnamara2005"/><ref name="rafferty2006"/> || Produced a colossal AGN outburst after accreting 600 million {{Solar mass}} worth of material. BH mass not explicitly stated; just a lower limit. Requires assumptions about the efficiencies of gas accretion and jet power.<ref name=DS>[http://www.sciencedaily.com/releases/2005/01/050106091317.htm Most Powerful Eruption In The Universe Discovered] NASA/Marshall Space Flight Center (ScienceDaily) January 6, 2005</ref><ref name="mcnamara2005">
|Black hole of central elliptical galaxy of [[MS 0735.6+7421]] || '''{{val|1|e=9}}'''<ref name=DS/><ref name="mcnamara2005"/><ref name="rafferty2006"/> || Produced a colossal AGN outburst after accreting 600 million <i>M</i><sub>&#x2609;</sub> worth of material. BH mass not explicitly stated; just a lower limit. Requires assumptions about the efficiencies of gas accretion and jet power.<ref name=DS>[http://www.sciencedaily.com/releases/2005/01/050106091317.htm Most Powerful Eruption In The Universe Discovered] NASA/Marshall Space Flight Center (ScienceDaily) January 6, 2005</ref><ref name="mcnamara2005">
{{cite journal
{{cite journal
| last1 = McNamara | first1 = B. R.
| last1 = McNamara | first1 = B. R.
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| [[Markarian 501]] || '''{{val|900000000}}–{{val|3400000000}}'''<ref name="Rieger">{{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/0210326v1|journal=Astronomy and Astrophysics|volume=397|page=121|year=2003|last1=Rieger|first1=F. M.|last2=Mannheim|first2=K.}}</ref> || Brightest object in the sky in very high energy gamma rays.
| [[Markarian 501]] || '''{{val|900000000}}–{{val|3400000000}}'''<ref name="Rieger">{{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/0210326v1|journal=Astronomy and Astrophysics|volume=397|page=121|year=2003|last1=Rieger|first1=F. M.|last2=Mannheim|first2=K.}}</ref> || Brightest object in the sky in very high energy gamma rays.
|-
|-
| [[PG 1426+015]] || '''{{val|1.298|0.385|e=9}}'''<ref name= 1A /><br />'''{{val|467740000}}'''<ref name=2A /> ||
| [[PG 1426+015]] || '''{{val|1.298|0.385|e=9}}'''<ref name=1A>{{cite journal
|doi=10.1007/s11214-013-9987-4
| title = Measuring the Masses of Supermassive Black Holes
| journal = Space Science Reviews
| volume = 183
| page = 253
| url = http://www.astronomy.ohio-state.edu/~peterson/Docs/petersonISSI.pdf
| year = 2013
| last1 = Peterson
| first1 = Bradley M.
| bibcode = 2014SSRv..183..253P
}}</ref><br />'''{{val|467740000}}'''<ref name=2A>{{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|year=2000|last1=Nelson|first1=Charles H.|bibcode=2000ApJ...544L..91N|arxiv = astro-ph/0009188 }}
</ref> ||
|-
|-
| [[3C 273]] || '''{{val|8.86|1.87|e=8}}'''<ref name= 1A /><br />'''{{val|550000000}}'''<ref name=2A /> || Brightest quasar in the sky
| [[3C 273]] || '''{{val|8.86|1.87|e=8}}'''<ref name= 1A /><br />'''{{val|550000000}}'''<ref name=2A /> || Brightest quasar in the sky
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| [[PG 0844+349]] || '''{{val|9.24|3.81|e=7}}'''<ref name= 1A /><br />'''{{val|21380000}}'''<ref name=2A /> ||
| [[PG 0844+349]] || '''{{val|9.24|3.81|e=7}}'''<ref name= 1A /><br />'''{{val|21380000}}'''<ref name=2A /> ||
|-
|-
| [[Centaurus A]] || '''{{val|55000000}}'''<ref>{{cite web|title=Radio Telescopes Capture Best-Ever Snapshot of Black Hole Jets|url=http://www.nasa.gov/topics/universe/features/radio-particle-jets.html|publisher=NASA|accessdate=2012-10-02}}</ref> || Also notable for its million light-year long [[Polar jet#Relativistic jet|relativistic jet]].<ref>{{Cite APOD|title=Centaurus Radio Jets Rising|access-date=2011-04-16|date=2011-04-13}}</ref>
| [[Centaurus A]] || '''{{val|55000000}}'''<ref>{{cite web|title=Radio Telescopes Capture Best-Ever Snapshot of Black Hole Jets|url=http://www.nasa.gov/topics/universe/features/radio-particle-jets.html|publisher=NASA|accessdate=2012-10-02}}</ref> || Also notable for its million light-year long [[Polar jet#Relativistic jet|relativistic jet]].<ref>{{Cite web|title=Centaurus Radio Jets Rising|access-date=2011-04-16|date=2011-04-13}}</ref>
|-
|-
| [[Markarian 79]] || '''{{val|5.24|1.44|e=7}}'''<ref name= 1A /><br />'''{{val|52500000}}'''<ref name=2A /> ||
| [[Markarian 79]] || '''{{val|5.24|1.44|e=7}}'''<ref name= 1A /><br />'''{{val|52500000}}'''<ref name=2A /> ||
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== Liên kết ngoài ==
== Liên kết ngoài ==


Phiên bản lúc 05:14, ngày 17 tháng 8 năm 2017

Minh họa đĩa bồi đắp quanh lỗ đen
Quan sát trực tiếp sóng hấp dẫn lần đầu tiên GW150914 về hai lỗ đen quay cạnh nhau

Danh sách các lỗ đen lớn nhất xếp theo thứ tự khối lượng dự đoán mà khoa học của loài người đã quan sát được, đơn vị tính là Khối lượng Mặt Trời (M☉=). Các lỗ đen siêu khối lượng có khối lượng từ hàng trăm ngàn tới hàng vài chục tỷ lần M☉ có thể tìm thấy ở hầu hết trung tâm các thiên hà lớn, ví dụ như Ngân Hà của chúng ta, hay các hàng xóm như Thiên hà Tiên Nữ, Messier 32 và xa hơn như NGC 4395.

Danh sách

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Danh sách lỗ đen lớn nhất
Tên Khối lượng Mặt trời
(Mặt Trời = 1) 		Ghi chú
S5 0014+81 40000000000[1][2][3] 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.[1]
SDSS J102325.31+514251.0 (331±061)×1010[4] Estimated from quasar MgII emission line correlation.
Black hole of central quasar of H1821+643 30000000000[5] Nearest galaxy cluster harboring a quasar in its core.[5]
APM 08279+5255 23×1010[6]
10+017
−013×1010[7]		 Based on velocity width of CO line from orbiting molecular gas,[6] and reverberation mapping using SiIV and CIV emission lines.[7]
NGC 4889 (21±16)×1010[8][9] Best fit: the estimate ranges from 6 billion to 37 billion M☉.[8][9]
Black hole of central elliptical galaxy of Phoenix Cluster 20000000000[10] This black hole is continuously growing at the rate of ~60 M☉ per year.
SDSS J074521.78+734336.1 (195±005)×1010[4] Estimated from quasar MgII emission line correlation.
OJ 287 primary 18000000000[11] 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 (17±015)×1010[12][13] Unprecedentedly massive in relation of its location: an elliptical galaxy host in a sparse environment.
SDSS J08019.69+373047.3 (151±031)×1010[4] Estimated from quasar MgII emission line correlation.
SDSS J115954.33+201921.1 (141±010)×1010[4] Estimated from quasar MgII emission line correlation.
SDSS J075303.34+423130.8 (138±003)×1010[4] Estimated from quasar Hβ emission line correlation.
SDSS J080430.56+542041.1 (135±022)×1010[4] Estimated from quasar MgII emission line correlation.
Abell 1201 BCG (13±06)×1010[14] Estimated from the strong gravitational lensing of a background galaxy behind the BCG.[14] Beware of ambiguity between the BH mass determination and the galaxy cluster's dark matter profile.[15]
SDSS J081855.77+095848.0 (120±006)×1010[4] Estimated from quasar MgII emission line correlation.
SDSS J0100+2802 (124±019)×1010[16][17] Estimated from quasar MgII emission line correlation. This object grew early in cosmic history (redshift 6.30).
SDSS J082535.19+512706.3 (112±020)×1010[4] Estimated from quasar Hβ emission line
SDSS J013127.34-032100.1 (11±02)×1010[18] Estimated from accretion disk spectrum modelling.[18]
PSO J334.2028+01.4075 10000000000[19] 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.[19]
Black hole of central elliptical galaxy of RX J1532.9+3021 10000000000[20]
QSO B2126-158 10000000000[1]
Holmberg 15A 10000000000[21] Mass estimates range from ~310 billion M☉ down to 3 billion M☉. They all rely on empirical scaling relations and are thus obtained from extrapolation and not from kinematical measurements.
SDSS J015741.57-010629.6 (98±14)×109[4] Estimated from quasar MgII emission line correlation.
NGC 3842 97+30
−25×109[8][9] 		Brightest galaxy in the Leo Cluster
SDSS J230301.45-093930.7 (912±088)×109[4] Estimated from quasar MgII emission line correlation.
SDSS J075819.70+202300.9 (78±39)×109[4] Estimated from quasar Hβ emission line correlation.
CID-947 69+08
−12×109[22] 		Constitutes 10% of the total mass of its host galaxy. Estimated from quasar Hβ emission line correlation.
SDSS J080956.02+502000.9 (646±045)×109[4] Estimated from quasar Hβ emission line correlation.
SDSS J014214.75+002324.2 (631±116)×109[4] Estimated from quasar MgII emission line correlation.
Messier 87 722+034
−040×109[23]
6300000000[24] 		Central galaxy of the Virgo Cluster; notable for its 4,300 light-year long relativistic jet.
NGC 5419 72+27
−19×109[25]		 Estimated from the stellar velocity distribution. A secondary satellite SMBH may orbit around 70 parsecs.[25]
SDSS J025905.63+001121.9 (525±073)×109[4] Estimated from quasar Hβ emission line correlation.
SDSS J094202.04+042244.5 (513±071)×109[4] Estimated from quasar Hβ emission line correlation.
QSO B0746+254 5000000000[1]
QSO B2149-306 5000000000[1]
NGC 1277 5000000000[26] Once thought to harbor a black hole so large that it contradicted modern galaxy formation and evolutionary theories,[27] re-analysis of the data revised it downward to roughly a third of the original estimate.[26]
SDSS J090033.50+421547.0 (47±02)×109[4] Estimated from quasar MgII emission line correlation.
Messier 60 (45±10)×109[28]
SDSS J011521.20+152453.3 (41±24)×109[4] Estimated from quasar Hβ emission line correlation.
QSO B0222+185 4000000000[1]
Hercules A (3C 348) 4000000000 Notable for its million light-year long relativistic jet.
Abell 1836-BCG 361+041
−050×109[29]
SDSS J213023.61+122252.0 (35±02)×109[4] Estimated from quasar Hβ emission line correlation.
SDSS J173352.23+540030.4 (34±04)×109[4] Estimated from quasar MgII emission line correlation.
SDSS J025021.76-075749.9 (31±06)×109[4] Estimated from quasar MgII emission line correlation.
SDSS J030341.04-002321.9 (30±04)×109[4] Estimated from quasar MgII emission line correlation.
QSO B0836+710 3000000000[1]
SDSS J224956.08+000218.0 (263±121)×109[4] Estimated from quasar Hβ emission line correlation.
SDSS J030449.85-000813.4 (24±050)×109[4] Estimated from quasar Hβ emission line correlation.
SDSS J234625.66-001600.4 (224±015)×109[4] Estimated from quasar Hβ emission line correlation.
ULAS J1120+0641 2000000000[30][31] Also, currently on record as the most distant quasar, at z=7.085[30]
QSO 0537-286 2000000000[1]
NGC 3115 2000000000[32]
Q0906+6930 2000000000[33] Most distant blazar, at z = 5.47
QSO B0805+614 1500000000[1]
Messier 84 1500000000[34]
Abell 3565-BCG 134+021
−019×109[29]
NGC 7768 13+05
−04×109[9]
Black hole of central elliptical galaxy of MS 0735.6+7421 1×109[35][36][37] 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.[35][36][37]
QSO B225155+2217 1000000000[1]
QSO B1210+330 1000000000[1]
NGC 6166 1000000000[38] Central galaxy of Abell 2199; notable for its hundred thousand light year long relativistic jet.
Cygnus A 1000000000[39] Brightest extrasolar radio source in the sky as seen at frequencies above 1 GHz
Thiên hà Sombrero 1000000000[40] Bolometrically most luminous galaxy in the local universe and also the nearest billion-solar-mass black hole to Earth.
Markarian 501 900000000–3400000000[41] Brightest object in the sky in very high energy gamma rays.
PG 1426+015 (1298±0385)×109[42]
467740000[43]
3C 273 (886±187)×108[42]
550000000[43]		 Brightest quasar in the sky
Messier 49 560000000[44]
NGC 1399 500000000[45] Central galaxy of the Fornax Cluster
PG 0804+761 (693±083)×108[42]
190550000[43]
PG 1617+175 (594±138)×108[42]
275420000[43]
PG 1700+518 781+182
−165×108[42]
60260000[43]
NGC 4261 400000000[46] Notable for its 88000 light-year long relativistic jet.[47]
PG 1307+085 (44±123)×108[42]
281 840 000[43]
SAGE0536AGN (35±08)×108[48][49] Constitutes 1.4% of the mass of its host galaxy
NGC 1275 340000000[50][51] Central galaxy of the Perseus Cluster
3C 390.3 (287±064)×108[42]
338840000[43]
II Zwicky 136 (457±055)×108[42]
144540000[43]
PG 0052+251 (369±076)×108[42]
218780000[43]
Messier 59 270000000[52] This black hole has a retrograde rotation.[53]
PG 1411+442 (443±146)×108[42]
79430000[43]
Markarian 876 (279±129)×108[42]
240000000[43]
Thiên hà Tiên Nữ 230000000 Nearest large galaxy to the Milky Way
PG 0953+414 (276±059)×108[42]
182000000[43]
PG 0026+129 (393±096)×108[42]
53700000[43]
Fairall 9 (255±056)×108[42]
79430000[43]
Markarian 1095 (15±019)×108[42]
182000000[43]
Messier 105 140000000–200000000[54]
Markarian 509 (143±012)×108[42]
57550000[43]
OJ 287 secondary 100000000[11] The smaller black hole orbiting OJ 287 primary (see above).
RX J124236.9-111935 100000000[55] Observed by the Chandra X-ray Observatory to be tidally disrupting a star.[55][56]
Messier 85 100000000[57]
NGC 5548 (671±026)×107[42]
123000000[43]
PG 1221+143 (146±044)×108[42]
40740000[43]
Messier 88 80000000[58]
Messier 81 (Bode's Galaxy) 70000000[59]
Markarian 771 (732±352)×107[42]
75860000[43]
Messier 58 70000000[60]
PG 0844+349 (924±381)×107[42]
21380000[43]
Centaurus A 55000000[61] Also notable for its million light-year long relativistic jet.[62]
Markarian 79 (524±144)×107[42]
52500000[43]
Messier 96 48000000[63] Estimates can be as low as 1.5 million solar masses
Markarian 817 (494±077)×107[42]
43650000[43]
NGC 3227 (422±214)×107[42]
38900000[43]
NGC 4151 primary 40000000[64][65]
3C 120 555+314
−225×107[42]
22900000[43]
Markarian 279 (349±092)×107[42]
41700000[43]
NGC 3516 (427±146)×107[42]
23000000[43]
NGC 863 (475±074)×107[42]
17700000[43]
Messier 82 (Cigar Galaxy) 30000000[66] Prototype starburst galaxy.[67]
Messier 108 24000000[68]
M60-UCD1 20000000[69] Constitutes 15% of the mass of its host galaxy.
NGC 3783 (298±054)×107[42]
9300000[43]
Markarian 110 (251±061)×107[42]
5620000[43]
Markarian 335 (142±037)×107[42]
6310000[43]
NGC 4151 secondary 10000000[65]
NGC 7469 (122±14)×106[42]
6460000[43]
IC 4329 A 990+1788
−1188×106[42]
5010000[43]
NGC 4593 536+937
−695×106[42]
8130000[43]
Messier 61 5000000[70]
Messier 32 1500000–5000000[71] A dwarf satellite galaxy of the Andromeda Galaxy.
Sagittarius A* 4300000[72] The black hole at the center of the Milky Way.

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