The Grand Universe

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List of the largest cosmic structures

Structure name (year discovered)	Maximum dimension (in light-years)	Notes
Hercules–Corona Borealis Great Wall (2014)[1]	9,700,000,000–10,000,000,000[2][3][4]	Discovered through gamma-ray burst mapping. Existence as a structure is disputed.[5][6][7]
Giant GRB Ring (2015)[8]	5,600,000,000[8]	Discovered through gamma-ray burst mapping. Largest-known regular formation in the observable universe.[8]
Huge-LQG (2012-2013)	4,000,000,000[9][10][11]	Decoupling of 73 quasars. Largest-known large quasar group and the first structure found to exceed 3 billion light-years.
“The Giant Arc” (2021)	3,300,000,000[12]	Located 9.2 billion light years away.
U1.11 LQG (2011)	2,500,000,000	Involves 38 quasars. Adjacent to the Clowes-Campusano LQG.
Clowes–Campusano LQG (1991)	2,000,000,000	Grouping of 34 quasars. Discovered by Roger Clowes and Luis Campusano.
Sloan Great Wall (2003)	1,380,000,000	Discovered through the 2dF Galaxy Redshift Survey and the Sloan Digital Sky Survey.
South Pole Wall (2020)	1,370,000,000[13][14][15][16][17][18]	The largest contiguous feature in the local volume and comparable to the Sloan Great Wall (see above) at half the distance. It is located at the celestial South Pole.
(Theoretical limit)	1,200,000,000	Structures larger than this size are incompatible with the cosmological principle according to all estimates. However, whether the existence of these structures itself constitutes a refutation of the cosmological principle is still unclear.[19]
BOSS Great Wall (BGW) (2016)	1,000,000,000	Structure consisting of 4 superclusters of galaxies. The mass and volume exceeds the amount of the Sloan Great Wall.[20]
Perseus–Pegasus Filament (1985)	1,000,000,000	This galaxy filament contains the Perseus–Pisces Supercluster.
Pisces–Cetus Supercluster Complex (1987)	1,000,000,000	Contains the Milky Way, and is the first galaxy filament to be discovered. (The first LQG was found earlier in 1982.) A new report in 2014 confirms the Milky Way as a member of the Laniakea Supercluster.
Caelum Supercluster	910,000,000[citation needed]	The Caelum Supercluster is a collection of over 550,000 galaxies. It is the largest of all galaxy superclusters.[citation needed]
CfA2 Great Wall (1989)	750,000,000	Also known as the Coma Wall.
Saraswati Supercluster	652,000,000[21]	The Saraswati Supercluster consists of 43 massive galaxy clusters, which include Abell 2361 and ZWCl 2341.1+0000.
Boötes Supercluster	620,000,000
Horologium-Reticulum Supercluster (2005)	550,000,000	Also known as the Horologium Supercluster.
Laniakea Supercluster (2014)	520,000,000	Galaxy supercluster in which Earth is located.
Komberg–Kravtsov–Lukash LQG 11	500,000,000	Discovered by Boris V. Komberg, Andrey V. Kravstov and Vladimir N. Lukash.[22][23]
Hyperion proto-supercluster (2018)	489,000,000	The largest and earliest known proto– supercluster.
Komberg–Kravtsov–Lukash LQG 12	480,000,000	Discovered by Boris V. Komberg, Andrey V. Kravstov and Vladimir N. Lukash.[22][23]
Newman LQG (U1.54)	450,000,000
Komberg–Kravtsov–Lukash LQG 5	430,000,000	Discovered by Boris V. Komberg, Andrey V. Kravstov and Vladimir N. Lukash.[22][23]
Tesch–Engels LQG	420,000,000
Draco Supercluster	410,000,000[citation needed]
Great Attractor	400,000,000
Shapley Supercluster	400,000,000	First identified by Harlow Shapley as a cloud of galaxies in 1930, it was not identified as a structure until 1989.
Komberg–Kravstov–Lukash LQG 3	390,000,000	Discovered by Boris V. Komberg, Andrey V. Kravstov and Vladimir N. Lukash.[22][23]
U1.90	380,000,000
Lynx–Ursa Major Filament (LUM Filament)	370,000,000
Sculptor Wall	370,000,000	Also known as the Southern Great Wall.
Pisces-Cetus Supercluster	350,000,000
Komberg–Kravtsov–Lukash LQG 2	350,000,000	Discovered by Boris V. Komberg, Andrey V. Kravstov and Vladimir N. Lukash.[22][23]
z=2.38 filament around protocluster ClG J2143-4423	330,000,000
Webster LQG	320,000,000	First LQG (Large Quasar Group) discovered.[23][24]
Komberg–Kravtsov–Lukash LQG 8	310,000,000	Discovered by Boris V. Komberg, Andrey V. Kravstov and Vladimir N. Lukash.[22][23]
Komberg–Kravtsov–Lukash LQG 1	280,000,000	Discovered by Boris V. Komberg, Andrey V. Kravstov and Vladimir N. Lukash.[22][23]
Komberg–Kravtsov–Lukash LQG 6	260,000,000	Discovered by Boris V. Komberg, Andrey V. Kravstov and Vladimir N. Lukash.[22][23]
Komberg–Kravtsov–Lukash LQG 7	250,000,000	Discovered by Boris V. Komberg, Andrey V. Kravstov and Vladimir N. Lukash.[22][23]
SCL @ 1338+27	228,314,341	One of most distant known superclusters.
Komberg–Kravtsov–Lukash LQG 9	200,000,000	Discovered by Boris V. Komberg, Andrey V. Kravstov and Vladimir N. Lukash.[22][23]
SSA22 Protocluster	200,000,000	Giant collection of Lyman-alpha blobs.
Ursa Major Supercluster	200,000,000
Komberg-Kravtsov-Lukash LQG 10	180,000,000	Discovered by Boris V. Komberg, Andrey V. Kravstov and Vladimir N. Lukash.[22][23]
Ophiuchus Supercluster	170,000,000[citation needed]
Virgo Supercluster	110,000,000	A part of the Laniakea Supercluster (see above). It also contains the Milky Way Galaxy, which contains the Solar System where Earth orbits the Sun. Reported for Reference.

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List of most massive black holes

Name	Solar mass (Sun = 1 × 100)	Notes
Phoenix A	1×1011[7]	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.[7] Mass has not been measured directly.
TON 618	6.6×1010[8]	Estimated from quasar Hβ emission line correlation.
4C +74.13	5.13+9.66 −3.35×1010[9][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.[9][10] Previous indirect assumptions about the efficiencies of gas accretion and jet power yield a lower limit of 1 billion M☉.[11][12][13]
The above masses are larger than what is predicted by current models of black hole growth, and are thus potentially unreliable
(Theoretical limit)	5×1010	This is the maximum mass of a black hole that models predict, at least for luminous accreting SMBH’s. At around 1010 M☉, both effects of intense radiation and star formation in the accretion disc slows 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.[14][15][16][17] Reported for reference.
Holmberg 15A	(4.0±0.8)×1010[18]	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.[19]
IC 1101	(4–10)×1010[20]	Estimated from properties of the host galaxy (Faber–Jackson relation); mass has not been measured directly.
S5 0014+81	4×1010[21][22][23]	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.[21]
SMSS J215728.21-360215.1	(3.4±0.6)×1010[24]	Estimated using near-infrared spectroscopic measurements of the MgII emission line doublet.
SDSS J102325.31+514251.0	3.31+0.67 −0.56×1010[25]	Estimated from quasar MgII emission line correlation.
H1821+643	3×1010[26]	Value obtained as an indirect estimate using a model of minimum Eddington luminosity required to account for the Compton cooling of the surrounding cluster.[26]
NGC 6166	2.84+0.27 −0.18×1010[27]	Central galaxy of Abell 2199; notable for its hundred thousand light year long relativistic jet.
2MASS J13260399+7023462	(2.7±0.4)×1010[28]	Estimated using the full-width half maxima of the CIV emission line and monochromatic luminosity at 1350 Å wavelength.
APM 08279+5255	2.3×1010[29] 1.0+0.17 −0.13×1010[30]	Based on velocity width of CO line from orbiting molecular gas,[29] and reverberation mapping using SiIV and CIV emission lines.[30]
NGC 4889	(2.1±1.6)×1010[31][32]	Best fit: the estimate ranges from 6 billion to 37 billion M☉.[31][32]
SDSS J074521.78+734336.1	(1.95±0.05)×1010[25]	Estimated from quasar MgII emission line correlation.
OJ 287 primary	1.8×1010[33]	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[by whom?] due to the limited number and precision of observed companion orbits.
NGC 1600	(1.7±0.15)×1010[34][35]	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[25]	Estimated from quasar MgII emission line correlation.
SDSS J115954.33+201921.1	(1.41±0.10)×1010[25]	Estimated from quasar MgII emission line correlation.
SDSS J075303.34+423130.8	(1.38±0.03)×1010[25]	Estimated from quasar Hβ emission line correlation.
SDSS J080430.56+542041.1	(1.35±0.22)×1010[25]	Estimated from quasar MgII emission line correlation.
Abell 1201 BCG	(1.3±0.6)×1010[36]	Estimated from the strong gravitational lensing of a background galaxy behind the BCG.[36] Beware of ambiguity between the BH mass determination and the galaxy cluster’s dark matter profile.[37]
SDSS J0100+2802	(1.24±0.19)×1010[38][39]	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[25]	Estimated from quasar MgII emission line correlation.
NGC 1270	1.2×1010[40]	Elliptical galaxy located in the Perseus Cluster. Also is a low-luminosity AGN (LLAGN).[41]
SDSS J082535.19+512706.3	(1.12±0.20)×1010[25]	Estimated from quasar Hβ emission line
SDSS J013127.34-032100.1	(1.1±0.2)×1010[42]	Estimated from accretion disk spectrum modelling.[42]
PSO J334.2028+01.4075	1×1010[43]	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.[43]
Black hole of central elliptical galaxy of RX J1532.9+3021	1×1010[44]
QSO B2126-158	1×1010[21]
NGC 1281	1×1010[45]	Compact elliptical galaxy in the Perseus Cluster. Mass estimates range from 10 billion M☉ down to <5 billion M☉.[46]
SDSS J015741.57-010629.6	(9.8±1.4)×109[25]
NGC 3842	9.7+3.0 −2.5×109[31][32]	Brightest galaxy in the Leo Cluster
SDSS J230301.45-093930.7	(9.12±0.88)×109[25]	Estimated from quasar MgII emission line correlation.
SDSS J140821.67+025733.2	8×109[47]	Estimated from quasar MgII emission line correlation.
SDSS J075819.70+202300.9	(7.8±3.9)×109[25]	Estimated from quasar Hβ emission line correlation.
CID-947	6.9+0.8 −1.2×109[48]	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[25]	Estimated from quasar Hβ emission line correlation.
SDSS J014214.75+002324.2	(6.31±1.16)×109[25]	Estimated from quasar MgII emission line correlation.
Messier 87	7.22+0.34 −0.40×109[49] 6.3×109[50]	Central galaxy of the Virgo Cluster; the first black hole directly imaged.
NGC 5419	7.2+2.7 −1.9×109[51]	Estimated from the stellar velocity distribution. A secondary satellite SMBH may orbit around 70 parsecs.[51]
SDSS J025905.63+001121.9	(5.25±0.73)×109[25]	Estimated from quasar Hβ emission line correlation.
SDSS J094202.04+042244.5	(5.13±0.71)×109[25]	Estimated from quasar Hβ emission line correlation.
QSO B0746+254	5×109[21]
QSO B2149-306	5×109[21]
SDSS J090033.50+421547.0	(4.7±0.2)×109[25]	Estimated from quasar MgII emission line correlation.
Messier 60	(4.5±1.0)×109[52]
SDSS J011521.20+152453.3	(4.1±2.4)×109[25]	Estimated from quasar Hβ emission line correlation.
QSO B0222+185	4×109[21]
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[53]
SDSS J213023.61+122252.0	(3.5±0.2)×109[25]	Estimated from quasar Hβ emission line correlation.
SDSS J173352.23+540030.4	(3.4±0.4)×109[25]	Estimated from quasar MgII emission line correlation.
SDSS J025021.76-075749.9	(3.1±0.6)×109[25]	Estimated from quasar MgII emission line correlation.
NGC 1271	3.0+1.0 −1.1×109[54]	Compact elliptical or lenticular galaxy in the Perseus Cluster.[55]
SDSS J030341.04-002321.9	(3.0±0.4)×109[25]	Estimated from quasar MgII emission line correlation.
QSO B0836+710	3×109[21]
SDSS J224956.08+000218.0	(2.63±1.21)×109[25]	Estimated from quasar Hβ emission line correlation.
SDSS J030449.85-000813.4	(2.4±0.50)×109[25]	Estimated from quasar Hβ emission line correlation.
SDSS J234625.66-001600.4	(2.24±0.15)×109[25]	Estimated from quasar Hβ emission line correlation.
PKS 2128-123	2.02×109[56]
ULAS J1120+0641	2×109[57][58]
QSO 0537-286	2×109[21]
NGC 3115	2×109[59]
Q0906+6930	2×109[60]	Most distant blazar, at z = 5.47
QSO B0805+614	1.5×109[21]
Messier 84	1.5×109[61]
J100758.264+211529.207 (“Pōniuāʻena”)	(1.5±0.2)×109[62]	Second most-distant quasar known
PKS 2059+034	1.36×109[56]
Abell 3565-BCG	1.34+0.21 −0.19×109[53]
NGC 7768	1.3+0.5 −0.4×109[32]
NGC 1277	1.2×109[63]	Once thought to harbor a black hole so large that it contradicted modern galaxy formation and evolutionary theories,[64] re-analysis of the data revised it downward to roughly a third of the original estimate.[65] and then one tenth.[63]
QSO B225155+2217	1×109[21]
QSO B1210+330	1×109[21]
Cygnus A	1×109[66]	Brightest extrasolar radio source in the sky as seen at frequencies above 1 GHz
Sombrero Galaxy	1×109[67]	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[68]	Brightest object in the sky in very high energy gamma rays.
PG 1426+015	(1.298±0.385)×109[4] 467740000[5]
3C 273	(8.86±1.87)×108[4] 550000000[5]	Brightest quasar in the sky
ULAS J1342+0928	8×108[69]	Most distant quasar[69] − currently on record as the most distant quasar at z=7.54[69]
Messier 49	5.6×108[70]
ESO 444-46	5.01×108–7.76×1010[9][10]	Brightest cluster galaxy of Abell 3558 in the center of the Shapley Supercluster; estimated using spheroidal luminosity profile of the host galaxy.
NGC 1399	5×108[71]	Central galaxy of the Fornax Cluster
PG 0804+761	(6.93±0.83)×108[4] 190550000[5]
PG 1617+175	(5.94±1.38)×108[4] 275420000[5]
PG 1700+518	7.81+1.82 −1.65×108[4] 60260000[5]
NGC 4261	4×108[72]	Notable for its 88000 light-year long relativistic jet.[73]
PG 1307+085	(4.4±1.23)×108[4] 281 840 000[5]
SAGE0536AGN	(3.5±0.8)×108[74][75]	Constitutes 1.4% of the mass of its host galaxy
NGC 1275	3.4×108[76][77]	Central galaxy of the Perseus Cluster
3C 390.3	(2.87±0.64)×108[4] 338840000[5]
II Zwicky 136	(4.57±0.55)×108[4] 144540000[5]
PG 0052+251	(3.69±0.76)×108[4] 218780000[5]
Messier 59	2.7×108[78]	This black hole has a retrograde rotation.[79]
PG 1411+442	(4.43±1.46)×108[4] 79430000[5]
Markarian 876	(2.79±1.29)×108[4] 240000000[5]
Andromeda Galaxy	2.3×108	Nearest large galaxy to the Milky Way
PG 0953+414	(2.76±0.59)×108[4] 182000000[5]
PG 0026+129	(3.93±0.96)×108[4] 53700000[5]
Fairall 9	(2.55±0.56)×108[4] 79430000[5]
NGC 7727	1.54+0.18 −0.15×108[80]	with 6.3×106 companion and the closest confirmed BBH to Earth at about 89 million light years away
Markarian 1095	(1.5±0.19)×108[4] 182000000[5]
Messier 105	1.4×108–2×108[81]
Markarian 509	(1.43±0.12)×108[4] 57550000[5]
OJ 287 secondary	1×108[33]	The smaller black hole orbiting OJ 287 primary (see above).
RX J124236.9-111935	1×108[82]	Observed by the Chandra X-ray Observatory to be tidally disrupting a star.[82][83]
Messier 85	1×108[84]
NGC 5548	(6.71±0.26)×107[4] 123000000[5]
PG 1211+143	(1.46±0.44)×108[4] 40740000[5]
Messier 88	8×107[85]
Messier 81 (Bode’s Galaxy)	7×107[86]
Markarian 771	(7.32±3.52)×107[4] 7.586×107[5]
Messier 58	7×107[87]
PG 0844+349	(9.24±3.81)×107[4] 2.138×107[5]
Centaurus A	5.5×107[88]	Also notable for its million light-year long relativistic jet.[89]
Markarian 79	(5.24±1.44)×107[4] 5.25×107[5]
Messier 96	48000000[90]	Estimates can be as low as 1.5 million solar masses
Markarian 817	(4.94±0.77)×107[4] 4.365×107[5]
NGC 3227	(4.22±2.14)×107[4] 3.89×107[5]
NGC 4151 primary	4×107[91][92]
3C 120	5.55+3.14 −2.25×107[4] 2.29×107[5]
Markarian 279	(3.49±0.92)×107[4] 4.17×107[5]
NGC 3516	(4.27±1.46)×107[4] 2.3×107[5]
NGC 863	(4.75±0.74)×107[4] 1.77×107[5]
Messier 82 (Cigar Galaxy)	3×107[93]	Prototype starburst galaxy.[94]
Messier 108	2.4×107[95]
M60-UCD1	2×107[96]	Constitutes 15% of the mass of its host galaxy.
NGC 3783	(2.98±0.54)×107[4] 9300000[5]
Markarian 110	(2.51±0.61)×107[4] 5620000[5]
Markarian 335	(1.42±0.37)×107[4] 6310000[5]
NGC 4151 secondary	10000000[92]
NGC 7469	(12.2±1.4)×106[4] 6460000[5]
IC 4329 A	9.90+17.88 −11.88×106[4] 5010000[5]
NGC 4593	5.36+9.37 −6.95×106[4] 8130000[5]
Messier 61	5×106[97]
Messier 32	1.5×106–5×106[98]	A dwarf satellite galaxy of the Andromeda Galaxy.
Sagittarius A*	4.3×106[99]	The black hole at the center of the Milky Way.

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Galaxies with diameters 500 kly or greater

Galaxy name/designation	Major axis diameter (in light-years)	Minor axis diameter (in light years)	Comoving distance (in millions of light-years)	Apparent visible magnitude	Morphology	Estimation method	Link for object
ESO 383-76 (ESO 383-G 076)[a]	1,764,000	882,100	654.9	13.01	cD5; E5; BrClG	90% total B-light	NED
ESO 409-25 (ESO 409-G 025)[a]	1,454,000	901,700	885.5	13.9	cD4; E4; BrClG	90% total B-light	NED
ESO 151-41 (ESO 151-G 041)	1,132,000	453,000	1,131	15.61	Sc	90% total B-light	NED
MCG-04-02-013[a]	1,115,000	1,115,000	770.4	16	E	27.0 B-mag arcsec−2	NED
ESO 306-17 (ESO 306-G 017)	1,070,000	706,100	517.3	13.33	cD3; E3	90% total B-light	NED
ESO 350-15 (ESO 350-G 015)	1,043,000	521,600	712.3	14.2	cD3; E3	90% total B-light	NED
Abell 1146 BCG	1,009,000	767,100	2,045	15.7	E	2MASS K-band total mag	NED
Abell 747 BCG	995,300	437,900	3,712	18.2	BrClG	2MASS K-band total mag	NED
ESO 473-5 (ESO 473-G 005)	944,600	632,900	921.7	14.57	Sc; BrClG	90% total B-light	NED
LEDA 1654342	916,400	623,100	3,921	18.3	BrClG	2MASS K-band total mag	NED
Abell 384 BCG	913,900	274,200	3,354	19.31	~[b]	2MASS K-band total mag	NED
Abell 697 BCG[a]	885,200	637,400	4,076	18.7	BrClG	2MASS K-band total mag	NED
Abell 963 BCG	841,200	605,700	2,976	17.5	BrClG	2MASS K-band total mag	NED
ESO 541-13 (ESO 541-G 013)	840,700	655,700	811.2	13.8	cD; E3 pec	90% total B-light	NED
Abell 1602 BCG	822,000	575,400	2,859	17.4	BrClG	2MASS K-band total mag	NED
NGC 623	803,900	611,000	426.3	13.88	cD; E	27.0 B-mag arcsec−2	NED
ESO 197-1 NED03 (ESO 197-G 001 NED03)	803,800	401,900	802.7	15.71	E	27.0 B-mag arcsec−2	NED
Abell 1413 BCG[a]	801,400	256,400	2,081	17.82	cD; E; BrClG	25.0 r-mag arcsec−2	NED
ESO 291-9 (ESO 291-G 009)	795,100	461,200	812.5	14.64	cD4; SA0−;BrClG	90% total B-light	NED
LEDA 1816387	782,500	336,500	4,304	18.7	~[b]	2MASS K-band total mag	NED
Abell 812 BCG[a]	772,900	541,000	2,763	17.6	BrClG	2MASS K-band total mag	NED
7C 1043+5953	771,000	400,900	3,299	18.1	BrClG	2MASS K-band total mag	NED
LEDA 2463193	769,500	769,500	5,023	19.6	BrClG	2MASS K-band total mag	NED
Abell 781 b	766,500	337,300	4,327	19.0	BrClG	25.0 r-mag arcsec−2	NED
Abell 655 BCG	760,000	577,600	1,864	16.0	BrClG	2MASS K-band total mag	NED
Abell 908 BCG	750,200	555,100	3,541	18.0	BrClG	2MASS K-band total mag	NED
ESO 198-1 (ESO 198-G 001)	741,600	563,600	921.4	14.36	cD4; E4	27.0 B-mag arcsec−2	NED
3C 295	738,000	738,000	5,926	19.8	E/S0;LEG;BrClG NLRG	2MASS K-band total mag	NED
Abell 267 BCG	736,700	302,000	3,297	17.8	BrClG	25.0 r-mag arcsec−2	NED
Abell 360 BCG	727,700	363,900	3,160	17.65	cD	2MASS K-band total mag	NED
ESO 251-21 (ESO 251-G 021)	727,700	458,400	480.1	13.9	SAB0- pec; E/S0	90% total B-light	NED
NGC 6872	717,000	143,400	246.6	12.69	SAB(rs)c	25.5 r-mag arcsec−2	NED
B3 1715+425	715,200	472,000	2,653	16.4	BrClG; AGN[c]	2MASS K-band total mag	NED
ESO 552-20 (ESO 552-G 020)[a]	710,000	411,800	447.5	13.32	cD; E	90% total B-light	NED
ESO 11-4 (ESO 011-G 004)	707,400	488,100	839.5	15.38	cD4; E4 pec	90% total B-light	NED
IC 1633[a]	705,700	543,400	349.3	12.48	cD; E1	27.0 B-mag arcsec−2	NED
LEDA 2262657	704,000	521,000	3,832	17.8	BrClG	2MASS K-band total mag	NED
NGC 1759	702,800	632,500	778.5	14.08	cD; E	27.0 B-mag arcsec−2	NED
Abell 242 BCG	699,900	287,000	3,259	17.94	cD; db	2MASS K-band total mag	NED
2MASS J14342214-0232472	676,600	399,200	4,216	18.9	BrClG	2MASS K-band total mag	NED
ESO 444-46 (ESO 444-G 046)[a]	670,700	382,300	654.9	15.23	cD4; E4; BrClG	27.0 B-mag arcsec−2	NED
Abell 227 BCG	667,400	493,900	2,526	17.11	cD	2MASS K-band total mag	NED
ESO 351-21 (ESO 351-G 021)	664,600	584,900	816.7	15.21	SA0-	90% total B-light	NED
NGC 1668	660,100	435,700	483.0	13.73	SA0−; D/cD	90% total B-light	NED
Abell 980 BCG	658,500	342,400	2,294	17.5	BrClG	2MASS K-band total mag	NED
2MASX J06583806-5557256	658,300	408,200	4,008	20.32	~[b]	2MASS K-band total mag	NED
ESO 253-27 (ESO 253-G 027)[a]	658,200	447,600	745.9	14.88	cD3; E3	90% total B-light	NED
Abell 38 BCG	658,200	368,600	2,017	16.87	BrClG	2MASS K-band total mag	NED
LEDA 1127620	657,400	552,200	3,626	18.2	~[b]	2MASS K-band total mag	NED
MACS J0257.6-2209 BCG	656,200	446,200	4,089	19.49	BrClG	2MASS K-band total mag	NED
LEDA 1694905	656,100	472,400	3,426	18.0	BrClG	2MASS K-band total mag	NED
LEDA 1769306	655,800	524,700	4,201	18.8	BrClG	2MASS K-band total mag	NED
ESO 488-27 (ESO 488-G 027)[a]	654,300	536,500	569.1	13.99	cD; E1	27.0 B-mag arcsec−2	NED
Abell 635 BCG	652,900	470,100	1,344	11.1(K)	cD	2MASS K-band total mag	NED
Abell 209 BCG	652,500	365,400	3,011	18.29	BrClG	2MASS K-band total mag	NED
Abell 690 BCG[a]	647,800	492,300	1,145	15.3	cD; BrClG; WLRG	2MASS K-band total mag	NED
IC 5353[a]	647,600	524,600	394.3	14.05	cD; S0−	26.0 B-mag arcsec−2	NED
LEDA 2637071	643,000	347,200	2,690	17.1	~[b]	2MASS K-band total mag	NED
ESO 488-15 (ESO 488-G 015)[a]	642,900	501,500	606.3	14.72	E	90% total B-light	NED
ESO 349-10 (ESO 349-G 010)	642,200	398,200	703.2	13.0	cD4; E4; BrClG	90% total B-light	NED
Abell 1835 BCG[d][a]	637,100	471,500	3,660	17.6	cD; BrClG	2MASS K-band total mag	NED
Abell 1277 BCG	636,800	471,200	3,559	18.6	BrClG	2MASS K-band total mag	NED
LEDA 1933247	634,600	342,700	3,023	17.5	BrClG	2MASS K-band total mag	NED
Abell 122 BCG	633,800	557,800	1,614	15.42	cD; E	2MASS K-band total mag	NED
UGC 2438[a]	633,100	367,200	1,013	16.5	cD	2MASS K-band total mag	NED
LEDA 2628046	632,800	379,700	3,967	18.2	BrClG	2MASS K-band total mag	NED
OGC 79	623,700	324,300	2,840	17.6	BrClG	2MASS K-band total mag	NED
LEDA 2197890	619,900	520,700	3,347	16.5	BrClG	2MASS K-band total mag	NED
Abell 907 BCG	618,700	457,800	2,350	16.9	BrClG	2MASS K-band total mag	NED
Abell 523-178	618,100	445,000	1,477	11.1	~[b]	2MASS K-band total mag	NED
LEDA 1183804	616,500	468,600	3,522	18.1	~[b]	2MASS K-band total mag	NED
ESO 539-11 (ESO 539-G 011)	613,300	361,800	753.4	14.9	S0	90% total B-light	NED
Abell 123 BCG	610,400	415,100	1,358	15.40	D/cD	2MASS K-band total mag	NED
ESO 33-3 (ESO 033-G 003)	607,800	370,800	378.7	13.7	E4	90% total B-light	NED
Abell 1068 BCG	607,400	243,000	2,008	16.4	cD; Sy2	25.0 r-mag arcsec−2	NED
ESO 307-13 (ESO 307-G 013)	607,400	406,900	672.9	13.5	cD3; E3; BrClG	90% total B-light	NED
Abell 586 BCG[a]	606,700	351,900	2,075	15.4	E; BrClG	2MASS K-band total mag	NED
ESO 482-21 (ESO 482-G 021)	604,400	344,500	786.7	15.24	S0	90% total B-light	NED
Abell 1047 G1[a]	602,600	518,300	2,256	17.1	BrClG	2MASS K-band total mag	NED
ESO 86-62 (ESO 086-G 062)	602,300	373,400	536.2	13.55	cD4; E4	90% total B-light	NED
WISEA J005939.38-181807.5	602,100	457,600	1,300	16.01	SB(s)a pec	2MASS K-band total mag	NED
WISEA J085404.52+290312.7[a]	601,600	433,200	1,224	15.8	S0; BrClG	2MASS K-band total mag	NED
Abell 315-5200[a]	600,800	324,400	2,499	18.1	BrClG	2MASS K-band total mag	NED
Abell 140 BCG	600,400	408,200	2,289	17.94	cD	2MASS K-band total mag	NED
Abell 3880 BCG	597,800	143,500	837.2	14.0	cD3; E3; BrClG	25.0 B-mag arcsec−2	NED
Abell 370 BCG[a]	595,700	595,700	5,437	18.85	E; BrClG	2MASS K-band total mag	NED
2MASX J03032123+0155344	595,600	345,500	2,190	19.3	cD	2MASS K-band total mag	NED
Abell 971 BCG	595,400	404,900	1,331	15.7	cD; BrClG	2MASS K-band total mag	NED
ESO 488-13 (ESO 488-G 013)[a]	595,300	375,000	652.0	15.1	SA(r)0+	27.0 B-mag arcsec−2	NED
LEDA 1369756	592,500	391,100	3,348	18.0	BrClG	2MASS K-band total mag	NED
Abell 1132 BCG[a]	592,500	509,500	1,959	16.8	BrClG	2MASS K-band total mag	NED
IC 5358[a]	592,000	272,300	413.6	13.58	cD4; E4 pec	27.0 B-mag arcsec−2	NED
Abell 1045 BCG[a]	590,900	307,200	1,995	16.7	BrClG	2MASS K-band total mag	NED
Abell 705 BCG	590,200	507,600	1,520	16.4	BrClG	2MASS K-band total mag	NED
Abell 1027B BCG	590,000	413,000	1,985	18.1	BrClG	2MASS K-band total mag	NED
Abell 2187 BCG[a]	589,400	405,000	2,555	17.2	BrClG	25.0 r-mag arcsec-2	NED
Abell S78 BCG	589,000	524,200	715.6	14.96	S0	90% total B-light	NED
Abell 359 BCG	575,900	299,500	3,453	17.36	cD	2MASS K-band total mag	NED
ESO 146-28 (ESO 146-G 028)	574,800	396,600	601.1	13.9	cD3; E3	27.0 B-mag arcsec−2	NED
ESO 161-8 (ESO 161-G 008)	574,000	287,000	705.2	13.8	cD5; E5; BrClG	90% total B-light	NED
OGC 58	565,700	294,200	3,825	18.0	BrClG	25.0 r-mag arcsec-2	NED
LEDA 139714	561,500	185,300	2,396	17.6	BrClG	25.0 r-mag arcsec-2	NED
ESO 306-4 (ESO 306-G 004)	560,300	280,100	454.7	14.71	cD4; E4 pec	90% total B-light	NED
Abell 521 BCG	560,100	291,300	3,566	16.1	Early-type[e]	2MASS K-band total mag	NED
Tadpole Galaxy	558,400	111,700	468.4	14.6	SB(s)c pec	25.0 B-mag arcsec-2	NED
Abell 1246 G1	557,900	234,300	2,727	18.3	BrClG	2MASS K-band total mag	NED
Abell 223B BCG	556,500	556,500	3,021	18.33	BrClG	2MASS K-band total mag	NED
ESO 424-1 (ESO 424-G 001)	551,500	402,600	852.9	15.20	cD4; E4 pec	90% total B-light	NED
2MASX J09420304+0857189	550,500	192,700	2,973	20.4	~[f]	2MASS K-band total mag	NED
Abell 394 BCG	548,100	350,800	2,952	17.29	cD	2MASS K-band total mag	NED
Abell 279A BCG[a]	547,600	427,200	1,123	15.6	BrClG	2MASS K-band total mag	NED
WISEA J222418.56-551451.7	546,500	393,500	1,142	15.83	cD3; E3	2MASS K-band total mag	NED
Abell S968A BCG	545,300	196,300	781.5	15.48	cD5; E5 pec	25.0 B-mag arcsec−2	NED
LEDA 1483121[a]	545,200	327,100	2,377	17	BrClG	2MASS K-band total mag	NED
ESO 349-1 (ESO 349-G 001)	544,900	403,200	823.5	14.52	cD1; E1	27.0 B-mag arcsec−2	NED
Abell 2261 BCG[a]	544,600	533,800	3,237	19.2	cD; E	2MASS K-band total mag	NED
ESO 118-6 (ESO 118-IG 006)[a]	544,400	310,300	700.6	15.23	cD4; E4	26.0 B-mag arcsec−2	NED
NGC 77	543,400	527,100	900.8	15.67	SA0-	90% total B-light	NED
Abell 329 BCG	542,400	314,600	1,998	16.56	cD	2MASS K-band total mag	NED
Abell 750 G1	541,300	281,500	2,371	17.3	BrClG	2MASS K-band total mag	NED
NGC 7012	541,100	330,100	434.1	13.65	cD4; E4 pec	90% total B-light	NED
Abell 415 BCG	540,600	508,200	1,121	16.64	S0	2MASS K-band total mag	NED
Abell 773 D2[a]	540,300	398,600	3,249	18.4	cD; BrClG	2MASS K-band total mag	NED
B2 1003+26[a]	539,800	431,900	1,697	16.5	E; BrClG	2MASS K-band total mag	NED
LEDA 2155337	539,700	367,000	3,626	18.1	BrClG	2MASS K-band total mag	NED
Abell 983-4822[a]	539,600	453,300	2,876	17.6	BrClG	2MASS K-band total mag	NED
LEDA 1860126	536,300	504,100	3,081	16.0	E; BrClG	25.0 r-mag arcsec-2	NED
LEDA 2623325	531,200	302,800	2,502	16.9	~[b]	2MASS K-band total mag	NED
Abell 1232 BCG[a]	527,500	411,400	2,439	17.2	BrClG	2MASS K-band total mag	NED
Abell 1382 BCG[a]	525,000	346,500	1,523	13.01(K)[g]	BrClG	2MASS K-band total mag	NED
Abell 1165 BCG	524,000	324,900	2,730	17.5	cD	2MASS K-band total mag	NED
LEDA 1166681	520,900	328,200	3,907	18.4	BrClG	2MASS K-band total mag	NED
OGC 81	520,000	265,200	3,942	18.9	BrClG	25.0 r-mag arcsec-2	NED
Abell 208A BCG[a]	519,600	426,100	1,128	15.7	E; BrClG, AGN	2MASS K-band total mag	NED
Abell 715 BCG	515,400	484,400	2,068	16.9	BrClG	2MASS K-band total mag	NED
LEDA 1013135	509,300	325,900	3,108	17.8	BrClG	2MASS K-band total mag	NED
UGC 9589	505,800	126,500	1,402	16.5	SB	Intermed. surface brightness	NED
LEDA 1374261	505,200	262,700	3,392	18.0	BrClG	25.0 r-mag arcsec-2	NED
Abell 1351 BCG	502,400	445,000	4,656	18.8	BrClG	2MASS K-band total mag	NED
Abell 667 BCG	502,400	341,600	2,094	17.1	BrClG	2MASS K-band total mag	NED

Listed below are some notable galaxies under 500,000 light-years in diameter, for the purpose of comparison. All links to NED are available, except for the Milky Way, which is linked to the relevant paper detailing its size.

Notable galaxies with diameters 500kly or less

Galaxy name/designation	Major axis diameter (in light-years)	Minor axis diameter (in light years)	Comoving distance (in millions of light-years)	Apparent visible magnitude	Morphology	Estimation method	Link for object
Hercules A	459,800	285,100	2,258	17.7	E; WLRG; NLRG	2MASS K-band total mag	NED
UGC 2885 (Rubin’s Galaxy)[a]	438,100	201,500	274.0	13.5	SA(rs)c	25.0 B-mag arcsec−2	NED
NGC 1399[a]	412,300	379,300	64.91	10.6	cD; E1 pec	90% total B-light	NED
NeVe 1	332,100	239,100	438.7	8.94(K)[h]	cD; E	2MASS K-band total mag	NED
Alcyoneus (galaxy)	242,900[i]	155,400	3,561	19.6	E	25.0 r-mag arcsec−2	NED
IC 1101[a]	164,200	133,500	342.8	14.73	cD; S0-	2MASS K-band total mag	NED
Andromeda Galaxy	152,300	152,300	2.446	0.17	SA(s)b	25.0 mag/arcsec2	NED
Messier 87[a]	118,800[j]	93,870	48.92	9.59	cD; E0-E1 pec; NLRG; Sy	25.0 B-mag arcsec−2	NED
Malin 1	118,700[k]	118,700	1,218	17.6(g)	S; LSB	2MASS K-band total mag	NED
NGC 262[a]	101,100	78,860	213.3	13.2(r)	SA(s)0/a; Sy2	2MASS K-band total mag	NED
Milky Way	87,400 ± 3,590	87,400 ± 3,590	~[l]	-5.0	Sb; Sbc; SB(rs)bc	25.0 B-mag arcsec-2	[22][23]

*****************

List of the largest nebulae

Nebula	Maximum dimension (in light-years/parsecs)	Type	Notes
LAB Giant Concentration[verification needed] (coinciding with SSA22 Protocluster)	200,000,000 ly (61,000,000 pc)[1]	Complex of LαBs	Also on record as one of the largest structures in the universe.
NGC 262 Halo Cloud	1,300,000 ly (400,000 pc)[2]	H I region	Spiral nebula surrounding NGC 262, which is one of the largest known galaxies.
Leo Ring	650,000 ly (200,000 pc)[3]	HVC
Magellanic Stream	600,000 ly (180,000 pc)[4]	complex of HVCs	Connects the Large and Small Magellanic clouds; extends across 180° of the sky.
Lyman-alpha blob 1	300,000 ly (92,000 pc)[5]	LαB	Largest blob in the LAB Giant Concentration[citation needed]
Himiko Gas Cloud	55,000 ly (17,000 pc)[6]	Intergalactic cloud (possible LαB)	One of the most massive lyman-alpha blobs known
HVC 127-41-330	20,000 ly (6,100 pc)[7]	HVC
Smith’s Cloud	9,800 ly (3,000 pc)[8]	HVC	Extends about 20° of the sky
Tarantula Nebula	1,895 ly (581 pc)[9][a]	H II region	Most active starburst region in the Local Group
NGC 604	1,520 ly (470 pc)[10][11][b]	H II region	Located in the Triangulum Galaxy
N44	1,000 ly (310 pc)[12]	Emission nebula
N11	1,000 ly (310 pc)[13]	H II region
NGC 2404	940 ly (290 pc)	H II region	Largest H II region located in spiral galaxy NGC 2403
NGC 595	880 ly (270 pc)[14]	H II region
NGC 6822	838 ly (257 pc)	H II region
Gum Nebula	809–950 ly (248–291 pc)[15][16]	Emission nebula
Bubble Nebula (NGC 6822)	758 ly (232 pc)[17][18][19]	H II region
NGC 6188	600 ly (180 pc)	Emission nebula
NGC 592	590 ly (180 pc)[20][21]	H II region
N119	570 ly (170 pc)[22]	H II region	Peculiar S-shape
Sh2-310	531–681 ly (163–209 pc)[23][c]	H II region	Nebula surrounding VY Canis Majoris, which is one of largest known stars.
Carina Nebula	460 ly (140 pc)[24]	H II region	Nearest giant H II region to Earth
Dragonfish Nebula	450 ly (140 pc)[25]	Emission nebula
RCW 49	350 ly (110 pc)[26]	H II region
Heart Nebula	330 ly (100 pc)	H II region
Westerhout 5 (Soul Nebula)	330 ly (100 pc)	H II region
Henize 70 (N70 or DEM L301)[27]	300 ly (92 pc)[28]	H II region	The N 70 Nebula, in the Large Magellanic Cloud has a shell structure and is really a bubble in space. It is a “Super Bubble”.
Barnard’s Loop	300 ly (92 pc)[29][30]	H II region
Sh2-54	252 ly (77 pc)[31][32]	H II region
Prawn Nebula	250 ly (77 pc)[33]	H II region
NGC 7822	150 ly (46 pc)[34]	Emission nebula
IC 2944	142 ly (44 pc)[35][36]	Emission nebula
Eagle Nebula	140 ly (43 pc)[37]	H II region	Part of another diffuse nebula IC 4703.
Rosette Nebula	130 ly (40 pc)	H II region
Lagoon Nebula	110 ly (34 pc)	H II region
NGC 3576	100 ly (31 pc)	Emission nebula
Veil Nebula	100 ly (31 pc)	Supernova remnant

By angular diameter

Celestial object	Angular diameter or size	Relative size
Magellanic Stream	over 100°
Gum Nebula	36°	1,000 ly
Milky Way	30° (by 360°)	105,700 ly
Serpens-Aquila Rift	20° by 10°	575 ly or more
Canis Major Overdensity	12° by 12°
Smith’s Cloud	11°
Large Magellanic Cloud	10.75° by 9.17°	Brightest galaxy in the night sky, 0.9 apparent magnitude (V)
Barnard’s loop	10°
Zeta Ophiuchi Sh2-27 nebula	10°
Sagittarius Dwarf Spheroidal Galaxy	7.5° by 3.6°
Coalsack nebula	7° by 5°
Rho Ophiuchi cloud complex	4.5° by 6.5°
Hyades	5°30′	Brightest star cluster in the night sky, 0.5 apparent magnitude (V)
Small Magellanic Cloud	5°20′ by 3°5′
Andromeda Galaxy	3°10′ by 1°	About six times the size of the Sun or the Moon. Only the much smaller core is visible without long-exposure photography.
Veil Nebula	3°
Heart Nebula	2.5° by 2.5°
Westerhout 5	2.3° by 1.25°
Sh2-54	2.3°
Carina Nebula	2° by 2°	Brightest nebula in the night sky, 1.0 apparent magnitude (V)
North America Nebula	2° by 100′
Orion Nebula	1°5′ by 1°
Sun	31′27″ – 32′32″	30–31 times the maximum value for Venus (orange bar below) / 1887–1952″
Moon	29′20″ – 34′6″	28–32.5 times the maximum value for Venus (orange bar below) / 1760–2046″
Helix Nebula	About 16′ by 28′
Spire in Eagle Nebula	4′40″	Length is 280″

********************

List of the largest cosmic structures

Structure name (year discovered)	Maximum dimension (in light-years)	Notes
Hercules–Corona Borealis Great Wall (2014)[1]	9,700,000,000–10,000,000,000[2][3][4]	Discovered through gamma-ray burst mapping. Existence as a structure is disputed.[5][6][7]
Giant GRB Ring (2015)[8]	5,600,000,000[8]	Discovered through gamma-ray burst mapping. Largest-known regular formation in the observable universe.[8]
Huge-LQG (2012-2013)	4,000,000,000[9][10][11]	Decoupling of 73 quasars. Largest-known large quasar group and the first structure found to exceed 3 billion light-years.
“The Giant Arc” (2021)	3,300,000,000[12]	Located 9.2 billion light years away.
U1.11 LQG (2011)	2,500,000,000	Involves 38 quasars. Adjacent to the Clowes-Campusano LQG.
Clowes–Campusano LQG (1991)	2,000,000,000	Grouping of 34 quasars. Discovered by Roger Clowes and Luis Campusano.
Sloan Great Wall (2003)	1,380,000,000	Discovered through the 2dF Galaxy Redshift Survey and the Sloan Digital Sky Survey.
South Pole Wall (2020)	1,370,000,000[13][14][15][16][17][18]	The largest contiguous feature in the local volume and comparable to the Sloan Great Wall (see above) at half the distance. It is located at the celestial South Pole.
(Theoretical limit)	1,200,000,000	Structures larger than this size are incompatible with the cosmological principle according to all estimates. However, whether the existence of these structures itself constitutes a refutation of the cosmological principle is still unclear.[19]
BOSS Great Wall (BGW) (2016)	1,000,000,000	Structure consisting of 4 superclusters of galaxies. The mass and volume exceeds the amount of the Sloan Great Wall.[20]
Perseus–Pegasus Filament (1985)	1,000,000,000	This galaxy filament contains the Perseus–Pisces Supercluster.
Pisces–Cetus Supercluster Complex (1987)	1,000,000,000	Contains the Milky Way, and is the first galaxy filament to be discovered. (The first LQG was found earlier in 1982.) A new report in 2014 confirms the Milky Way as a member of the Laniakea Supercluster.
Caelum Supercluster	910,000,000[citation needed]	The Caelum Supercluster is a collection of over 550,000 galaxies. It is the largest of all galaxy superclusters.[citation needed]
CfA2 Great Wall (1989)	750,000,000	Also known as the Coma Wall.
Saraswati Supercluster	652,000,000[21]	The Saraswati Supercluster consists of 43 massive galaxy clusters, which include Abell 2361 and ZWCl 2341.1+0000.
Boötes Supercluster	620,000,000
Horologium-Reticulum Supercluster (2005)	550,000,000	Also known as the Horologium Supercluster.
Laniakea Supercluster (2014)	520,000,000	Galaxy supercluster in which Earth is located.
Komberg–Kravtsov–Lukash LQG 11	500,000,000	Discovered by Boris V. Komberg, Andrey V. Kravstov and Vladimir N. Lukash.[22][23]
Hyperion proto-supercluster (2018)	489,000,000	The largest and earliest known proto– supercluster.
Komberg–Kravtsov–Lukash LQG 12	480,000,000	Discovered by Boris V. Komberg, Andrey V. Kravstov and Vladimir N. Lukash.[22][23]
Newman LQG (U1.54)	450,000,000
Komberg–Kravtsov–Lukash LQG 5	430,000,000	Discovered by Boris V. Komberg, Andrey V. Kravstov and Vladimir N. Lukash.[22][23]
Tesch–Engels LQG	420,000,000
Draco Supercluster	410,000,000[citation needed]
Great Attractor	400,000,000
Shapley Supercluster	400,000,000	First identified by Harlow Shapley as a cloud of galaxies in 1930, it was not identified as a structure until 1989.
Komberg–Kravstov–Lukash LQG 3	390,000,000	Discovered by Boris V. Komberg, Andrey V. Kravstov and Vladimir N. Lukash.[22][23]
U1.90	380,000,000
Lynx–Ursa Major Filament (LUM Filament)	370,000,000
Sculptor Wall	370,000,000	Also known as the Southern Great Wall.
Pisces-Cetus Supercluster	350,000,000
Komberg–Kravtsov–Lukash LQG 2	350,000,000	Discovered by Boris V. Komberg, Andrey V. Kravstov and Vladimir N. Lukash.[22][23]
z=2.38 filament around protocluster ClG J2143-4423	330,000,000
Webster LQG	320,000,000	First LQG (Large Quasar Group) discovered.[23][24]
Komberg–Kravtsov–Lukash LQG 8	310,000,000	Discovered by Boris V. Komberg, Andrey V. Kravstov and Vladimir N. Lukash.[22][23]
Komberg–Kravtsov–Lukash LQG 1	280,000,000	Discovered by Boris V. Komberg, Andrey V. Kravstov and Vladimir N. Lukash.[22][23]
Komberg–Kravtsov–Lukash LQG 6	260,000,000	Discovered by Boris V. Komberg, Andrey V. Kravstov and Vladimir N. Lukash.[22][23]
Komberg–Kravtsov–Lukash LQG 7	250,000,000	Discovered by Boris V. Komberg, Andrey V. Kravstov and Vladimir N. Lukash.[22][23]
SCL @ 1338+27	228,314,341	One of most distant known superclusters.
Komberg–Kravtsov–Lukash LQG 9	200,000,000	Discovered by Boris V. Komberg, Andrey V. Kravstov and Vladimir N. Lukash.[22][23]
SSA22 Protocluster	200,000,000	Giant collection of Lyman-alpha blobs.
Ursa Major Supercluster	200,000,000
Komberg-Kravtsov-Lukash LQG 10	180,000,000	Discovered by Boris V. Komberg, Andrey V. Kravstov and Vladimir N. Lukash.[22][23]
Ophiuchus Supercluster	170,000,000[citation needed]
Virgo Supercluster	110,000,000	A part of the Laniakea Supercluster (see above). It also contains the Milky Way Galaxy, which contains the Solar System where Earth orbits the Sun. Reported for Reference.

*****************

Stars with 60 M_☉ or greater

Star name	Mass (M☉, Sun = 1)	Approx. distance from earth (ly)	Apparent visible magnitude	Effective temperature (K)	Estimation method	Link	Reference
Westerhout 49-2 (in Westerhout 49)	250	36,200	18.246 (J band)	35,500	Spectroscopy	SIMBAD	[5][6]
BAT99-98 (in Tarantula Nebula of LMC)	226	165,000	13.37	45,000	Spectroscopy	SIMBAD	[7][8]
R136a1 (in Tarantula Nebula of LMC)	196	163,000	12.23	46,000	Evolution	SIMBAD	[9][10]
Melnick 42 (in Tarantula Nebula of LMC)	189	163,000	12.78	47,300	Spectroscopy	SIMBAD	[11][8]
VFTS 1022 (in Tarantula Nebula of LMC)	178	164,000	13.47	42,200	Spectroscopy	SIMBAD	[11][8]
Westerhout 51-57 (in Westerhout 51)	160	20,000	16.66 (J band)	42,700	Evolution		[12]
R136a3 (in Tarantula Nebula of LMC)	155	163,000	12.97	50,000	Evolution	SIMBAD	[9][10]
VFTS 682 (in Tarantula Nebula of LMC)	153	164,000	16.08	52,200	Spectroscopy	SIMBAD	[13][8]
HD 15558 A (in IC 1805 of Heart Nebula)	152	24,400	7.87 (combined)	39,500	Binary	SIMBAD	[14][15]
R136a2 (in Tarantula Nebula of LMC)	151	163,000	12.34	50,000	Evolution	SIMBAD	[9][10]
Westerhout 51-3 (in Westerhout 51)	148	20,000	17.79 (J band)	39,800	Evolution	SIMBAD	[12]
Melnick 34 A (in Tarantula Nebula of LMC)	147	163,000	13.09 (combined)	53,000	Binary	SIMBAD	[16][8]
VFTS 482 (in Tarantula Nebula of LMC)	145	164,000	12.95	42,200	Spectroscopy	SIMBAD	[11][8]
R136c (in Tarantula Nebula of LMC)	142	163,000	13.43	51,000	Evolution	SIMBAD	[17][8]
VFTS 1021 (in Tarantula Nebula of LMC)	141	164,000	13.35	39,800	Spectroscopy	SIMBAD	[11][8]
LH 10-3209 A (in NGC 1763 of LMC)	140	160,000	11.859 (combined)	42,500	Spectroscopy	SIMBAD	[18][19][e]
VFTS 506 (in Tarantula Nebula of LMC)	138	164,000	13.31	47,300	Spectroscopy	SIMBAD	[13][8]
Melnick 34 B (in Tarantula Nebula of LMC)	136	163,000	13.09 (combined)	53,000	Binary	SIMBAD	[16][8]
Westerhout 51d (in Westerhout 51)	135	20,000	15.11 (J band)	42,700	Evolution		[12]
VFTS 545 (in Tarantula Nebula of LMC)	133	164,000	13.32	47,300	Spectroscopy	SIMBAD	[11][8]
HD 97950 B (WR 43b in HD 97950 of NGC 3603)	132	24,800	11.33	42,000	Spectroscopy	SIMBAD	[20][21]
HD 269810 (in NGC 2029 of LMC)	130	163,000	12.22	52,500	Spectroscopy	SIMBAD	[22][23]
Westerhout 49-1 (in Westerhout 49)	130	36,200	15.531 (J band)	44,700	Evolution	SIMBAD	[5][6]
R136a7 (in Tarantula Nebula of LMC)	127	163,000	13.97	54,000	Evolution	SIMBAD	[24][8]
WR 42e (in HD 97950 of NGC 3603)	123	25,000	14.53	43,000	Ejection	SIMBAD	[25][f]
HD 97950 A1a (WR 43a A in HD 97950 of NGC 3603)	120	24,800	11.18 (combined)	42,000	Binary	SIMBAD	[20][21]
LSS 4067 (in HM 1)	120	11,000	11.44	40,000	Evolution	SIMBAD	[26][27]
WR 93 (in Pismis 24 of NGC 6357)	120	5,900	10.68	71,000	Evolution	SIMBAD	[26][15]
Sk -69° 212 (in NGC 2044 of LMC)	119	160,000	12.416	45,400	Evolution	SIMBAD	[28][19]
Sk -69° 249 A (in NGC 2074 of LMC)	119	160,000	12.02 (combined)	38,900	Evolution	SIMBAD	[28][29]
ST5-31 (in NGC 2074 of LMC)	119	160,000	12.273	50,700	Evolution	SIMBAD	[28][30]
R136a5 (in Tarantula Nebula of LMC)	116	157,000	13.71	48,000	Evolution	SIMBAD	[24][8]
MSP 183 (in Westerlund 2)	115	20,000	13.878	46,300	Spectroscopy	SIMBAD	[31][32]
WR 24 (in Collinder 228 of Carina Nebula)	114	14,000	6.48	50,100	Evolution	SIMBAD	[33][34]
HD 97950 C1 (WR 43c A in HD 97950 of NGC 3603)	113	24,800	11.89 (combined)	44,000	Spectroscopy	SIMBAD	[20][21][e]
Arches-F9 (WR 102ae in Arches Cluster)	111.3	25,000	16.1 (J band)	36,600	Spectroscopy	SIMBAD	[35][36]
Cygnus OB2 #12 A (in Cygnus OB2)	110	5,200	11.702 (combined)	13,700	Spectroscopy	SIMBAD	[37][38][e]
HD 93129 Aa (in Trumpler 14 of Carina Nebula)	110	7,500	6.9 (combined)	42,500	Trinary	SIMBAD	[39][15]
HSH95-36 (in Tarantula Nebula of LMC)	110	163,000	14.41	49,500	Evolution	SIMBAD	[24][8]
R146 (in Tarantula Nebula of LMC)	109	164,000	13.11	63,000	Spectroscopy	SIMBAD	[7][8]
R136a4 (in Tarantula Nebula of LMC)	108	157,000	13.41	50,000	Evolution	SIMBAD	[24][8]
VFTS 621 (in Tarantula Nebula of LMC)	107	164,000	15.39	54,000	Spectroscopy	SIMBAD	[11][8]
R136a6 (in Tarantula Nebula of LMC)	105	157,000	13.35	52,000	Evolution	SIMBAD	[24][8]
Westerhout 49-3 (in Westerhout 49)	105	36,200	16.689 (J band)	40,700	Evolution	SIMBAD	[5][6]
WR 21a A (Runaway star from Westerlund 2)	103.6	26,100	12.661 (combined)	45,000	Binary	SIMBAD	[40][23]
R99 (in N44 of LMC)	103	164,000	11.52	28,000	Spectroscopy	SIMBAD	[7][15]
Arches-F6 (WR 102ah in Arches Cluster)	101	25,000	15.75 (J band)	33,900	Spectroscopy	SIMBAD	[35][36]
Sk -65° 47 (in NGC 1923 of LMC)	101	160,000	12.466	47,800	Evolution	SIMBAD	[28][19]
Arches-F1 (WR 102ad in Arches Cluster)	100.9	25,000	16.3 (J band)	33,200	Spectroscopy	SIMBAD	[35][36]
Peony Star (WR 102ka in Peony Nebula near Galactic Center)	100	26,000	12.978 (J band)	25,100	Spectroscopy	SIMBAD	[41][6]
VFTS 457 (in Tarantula Nebula of LMC)	100	164,000	13.74	39,800	Spectroscopy	SIMBAD	[11][8]
η Carinae A (in Trumpler 16 of Carina Nebula)	100	7,500	4.3 (combined)	9,400-35,200	Spectroscopy	SIMBAD	[42][43]
Mercer 30-1 A (WR 46-3 A in Mercer 30 of Dragonfish Nebula)	99	40,000	10.33 (J band)	32,200	Evolution	SIMBAD	[44][g][e]
Sk -68° 137 (in Tarantula Nebula of LMC)	99	160,000	13.346	50,000	Spectroscopy	SIMBAD	[18][19]
WR 25 A (in Trumpler 16 of Carina Nebula)	98	6,500	8.8 (combined)	50,100	Evolution	SIMBAD	[33][15][e]
BI 253 (Runaway star from Tarantula Nebula of LMC)	97.6	164,000	13.76	54,000	Spectroscopy	SIMBAD	[17][45]
R136a8 (in Tarantula Nebula of LMC)	96	157,000	14.42	49,500	Evolution	SIMBAD	[24][46]
Westerhout 49-15 (in Westerhout 49)	96	36,200	18.307 (J band)	43,700	Evolution	SIMBAD	[5][6]
HD 38282 B (in Tarantula Nebula of LMC)	95	163,000	11.11 (combined)	47,000	Binary	SIMBAD	[47][23]
HM 1-6 (in HM 1)	95	11,000	11.64	44,700	Evolution	SIMBAD	[26][48]
NGC 3603-42 (in HD 97950 of NGC 3603)	95	25,000	12.86	50,000	Spectroscopy	SIMBAD	[18][21]
R139 A (in Tarantula Nebula of LMC)	95	163,000	11.94 (combined)	35,000	Binary	SIMBAD	[7][8]
BAT99-6 (in NGC 1747 of LMC)	94	165,000	11.95	56,000	Spectroscopy	SIMBAD	[7][19]
Sk -66° 172 (in N64 of LMC)	94	160,000	13.1	46,300	Spectroscopy	SIMBAD	[18][19][h]
ST2-22 (in NGC 2044 of LMC)	94	160,000	14.3	51,300	Evolution	SIMBAD	[28][49]
VFTS 259 (in Tarantula Nebula of LMC)	94	164,000	13.65	37,600	Spectroscopy	SIMBAD	[11][8]
VFTS 562 (in Tarantula Nebula of LMC)	94	164,000	13.66	42,200	Spectroscopy	SIMBAD	[11][8]
VFTS 512 (in Tarantula Nebula of LMC)	93	164,000	14.28	47,300	Spectroscopy	SIMBAD	[11][8]
HD 97950 A1b (WR 43a B in HD 97950 of NGC 3603)	92	24,800	11.18 (combined)	40,000	Binary	SIMBAD	[20][21]
R136b (in Tarantula Nebula of LMC)	92	163,000	13.24	35,500	Evolution	SIMBAD	[24][8]
VFTS 16 (in Tarantula Nebula of LMC)	91.6	164,000	13.55	50,600	Spectroscopy	SIMBAD	[17][8]
HD 97950 A3 (in HD 97950 of NGC 3603)	91	24,800	12.95	50,000	Spectroscopy	SIMBAD	[18][21]
NGC 346-W1 (in NGC 346 of SMC)	91	200,000	12.57	43,400	Evolution	SIMBAD	[28][50]
R127 (in NGC 2055 of LMC)	90	160,000	10.15	10,000-27,000	Evolution	SIMBAD	[51][23]
VFTS 333 (in Tarantula Nebula of LMC)	90	164,000	12.49	37,600	Spectroscopy	SIMBAD	[11][8]
VFTS 267 (in Tarantula Nebula of LMC)	89	164,000	13.49	44,700	Spectroscopy	SIMBAD	[11][8]
VFTS 64 (in Tarantula Nebula of LMC)	88	164,000	14.621	39,800	Spectroscopy	SIMBAD	[11][19]
BAT99-80 A (in NGC 2044 of LMC)	87	165,000	13 (combined)	45,000	Spectroscopy	SIMBAD	[28][49]
R140b (in Tarantula Nebula of LMC)	87	165,000	12.66	47,000	Spectroscopy	SIMBAD	[7][8]
VFTS 542 (in Tarantula Nebula of LMC)	87	164,000	13.47	44,700	Spectroscopy	SIMBAD	[11][8]
VFTS 599 (in Tarantula Nebula of LMC)	87	164,000	13.8	44,700	Spectroscopy	SIMBAD	[11][8]
WR 89 (in HM 1)	87	11,000	11.02	39,800	Evolution	SIMBAD	[33][23]
Arches-F7 (WR 102aj in Arches Cluster)	86.3	25,000	15.74 (J band)	32,900	Spectroscopy	SIMBAD	[35][36]
Sk -69° 104 (in NGC 1910 of LMC)	86	160,000	12.1	39,900	Evolution	SIMBAD	[28][19]
VFTS 1017 (in Tarantula Nebula of LMC)	86	164,000	14.5	50,100	Spectroscopy	SIMBAD	[11][8]
LH 10-3061 (in NGC 1763 of LMC)	85	160,000	13.491	52,000	Spectroscopy	SIMBAD	[18][19]
Sk 80 (in NGC 346 of SMC)	85	200,000	12.31	38,900	Evolution	SIMBAD	[28][52]
VFTS 603 (in Tarantula Nebula of LMC)	85	164,000	13.99	42,200	Spectroscopy	SIMBAD	[11][8]
Sk -70° 91 (in BSDL 1830 of LMC)	84.09	165,000	12.78	48,900	Evolution	SIMBAD	[53][19][i]
R147 (in Tarantula Nebula of LMC)	84	164,000	12.993	47,300	Spectroscopy	SIMBAD	[11][54]
HD 93250 A (in Trumpler 16 of Carina Nebula)	83.3	7,500	7.5 (combined)	46,000	Evolution	SIMBAD	[55][15][e]
Melnick 33Na A (in Tarantula Nebula of LMC)	83	163,000	13.79 (combined)	50,000	Evolution	SIMBAD	[56][57]
WR 20a A (in Westerlund 2)	82.7	20,000	13.28 (combined)	43,000	Binary	SIMBAD	[58]
TIC 276934932 A (in NGC 2048 of LMC)	82	160,000	14.05 (combined)	45,000	Spectroscopy	SIMBAD	[18][19]
WR 20a B (in Westerlund 2)	81.9	20,000	13.28 (combined)	43,000	Binary	SIMBAD	[58]
Trumpler 27-27 (in Trumpler 27)	81	3,900	13.31	37,000	Evolution	SIMBAD	[26][23]
BAT99-96 (in Tarantula Nebula of LMC)	80	165,000	13.76	42,000	Spectroscopy	SIMBAD	[7][8]
HD 15570 (in IC 1805 of Heart Nebula)	80	7,500	8.11	46,000	Spectroscopy	SIMBAD	[14][15]
HD 38282 A (in Tarantula Nebula of LMC)	80	163,000	11.11 (combined)	47,000	Binary	SIMBAD	[47][23]
HSH95-46 (in Tarantula Nebula of LMC)	80	163,000	14.56	47,500	Evolution	SIMBAD	[24][8]
Arches-F15 (in Arches Cluster)	79.7	25,000	16.12 (J band)	35,600	Spectroscopy	SIMBAD	[35][36]
BI 237 (in BSDL 2527 of LMC)	79.66	165,000	13.83	51,300	Spectroscopy	SIMBAD	[53][19][j]
VFTS 94 (in Tarantula Nebula of LMC)	79	164,000	14.161	42,200	Spectroscopy	SIMBAD	[11][19]
VFTS 151 (in Tarantula Nebula of LMC)	79	164,000	14.13	42,200	Spectroscopy	SIMBAD	[11][8]
LH 41-32 (in NGC 1910 of LMC)	78	160,000	13.086	48,200	Evolution	SIMBAD	[28][19]
Pismis 24-17 (in Pismis 24 of NGC 6357)	78	5,900	11.84	42,700	Spectroscopy	SIMBAD	[59][48]
VFTS 404 (in Tarantula Nebula of LMC)	78	164,000	14.14	44,700	Spectroscopy	SIMBAD	[11][8]
Westerhout 51-2 (in Westerhout 51)	77	20,000	13.68 (J band)	42,700	Evolution	SIMBAD	[12]
BAT99-68 (in BSDL 2505 of LMC)	76	165,000	14.13	45,000	Spectroscopy	SIMBAD	[7][19][k]
HD 93632 (in Collinder 228 of Carina Nebula)	76	10,000	8.23	45,400	Evolution	SIMBAD	[26][15]
NGC 346-W3 (in NGC 346 of SMC)	76	200,000	12.8	52,500	Evolution	SIMBAD	[28][50]
VFTS 169 (in Tarantula Nebula of LMC)	76	164,000	14.437	47,300	Spectroscopy	SIMBAD	[11][19]
VFTS 440 (in Tarantula Nebula of LMC)	76	164,000	12.046	39,800	Spectroscopy	SIMBAD	[11][19]
AB1 (in DEM S10 of SMC)	75	197,000	15.238	79,000	Spectroscopy	SIMBAD	[60][50][l]
WR 22 A (in Bochum 10 of Carina Nebula)	75	8,300	6.42 (combined)	44,700	Evolution	SIMBAD	[33][15][m]
Pismis 24-1NE (in Pismis 24 of NGC 6357)	74	6,500	11	42,500	Binary	SIMBAD	[59][61]
VFTS 608 (in Tarantula Nebula of LMC)	74	164,000	14.22	42,200	Spectroscopy	SIMBAD	[11][8]
HSH95-31 (in Tarantula Nebula of LMC)	73	163,000	14.12	47,500	Evolution	SIMBAD	[24][8]
Mercer 30-3 (in Mercer 30 of Dragonfish Nebula)	73	40,000	12.62 (J band)	39,300	Evolution	SIMBAD	[44][g]
Mercer 30-11 (in Mercer 30 of Dragonfish Nebula)	73	40,000	12.33 (J band)	36,800	Evolution	SIMBAD	[44][g]
VFTS 566 (in Tarantula Nebula of LMC)	73	164,000	14.05	44,700	Spectroscopy	SIMBAD	[11][8]
LH 64-16 (in NGC 2001 of LMC)	72	160,000	13.666	50,900	Evolution	SIMBAD	[28][30]
NGC 2044-W35 (in NGC 2044 of LMC)	72	160,000	14.1	48,200	Evolution	SIMBAD	[28][19]
VFTS 216 (in Tarantula Nebula of LMC)	72	164,000	14.389	44,700	Spectroscopy	SIMBAD	[11][19]
ST2-1 (in NGC 2044 of LMC)	71	160,000	14.3	44,100	Evolution	SIMBAD	[28][49]
VFTS 3 (in Tarantula Nebula of LMC)	71	164,000	11.56	21,000	Spectroscopy	SIMBAD	[62][8]
Arches-F12 (WR 102af in Arches Cluster)	70	25,000	16.4 (J band)	36,900	Spectroscopy	SIMBAD	[35][36]
HD 15629 (in IC 1805 of Heart Nebula)	70	7,500	8.42	45,900	Spectroscopy	SIMBAD	[14][15]
HD 37974 (in N135 of LMC)	70	163,000	10.99	22,500	Spectroscopy	SIMBAD	[63][23][n]
HD 93129 Ab (in Trumpler 14 of Carina Nebula)	70	7,500	7.31 (combined)	44,000	Trinary	SIMBAD	[39][64]
M33 X-7 B (in Triangulum Galaxy)	70	2,700,000	18.7	35,000	Binary	SIMBAD	[65][66]
Sk -69° 194 A (in NGC 2033 of LMC)	70	160,000	12.131 (combined)	45,000	Evolution	SIMBAD	[28][54][e]
VFTS 125 (in Tarantula Nebula of LMC)	69.6	164,000	16.6	55,200	Spectroscopy	SIMBAD	[17][49]
HD 46150 (in NGC 2244 of Rosette Nebula)	69	5,200	6.73	44,000	Spectroscopy	SIMBAD	[18][15]
HD 229059 (in Berkeley 87)	69	3,000	8.7	26,300	Evolution	SIMBAD	[26][15]
ST2-3 (in NGC 2044 of LMC)	69	160,000	14.264	44,900	Evolution	SIMBAD	[28][19]
ST2-32 (in NGC 2044 of LMC)	69	160,000	13.903	45,400	Evolution	SIMBAD	[28][19]
W28-23 (in NGC 2033 of LMC)	69	160,000	13.702	51,300	Evolution	SIMBAD	[28][30]
HD 93403 A (in Trumpler 16 of Carina Nebula)	68.5	10,400	8.27 (combined)	39,300	Binary	SIMBAD	[67][23]
HD 93130 (in Collinder 228 of Carina Nebula)	68	10,000	8.04	39,900	Evolution	SIMBAD	[26][15]
HM 1-8 (in HM 1)	68	11,000	12.52	46,100	Evolution	SIMBAD	[26][48]
HSH95-47 (in Tarantula Nebula of LMC)	68	163,000	14.72	43,500	Evolution	SIMBAD	[24][8]
HSH95-48 (in Tarantula Nebula of LMC)	68	163,000	14.75	46,500	Evolution	SIMBAD	[24][46]
Westerhout 51-61 (in Westerhout 51)	68	20,000	18.16 (J band)	38,000	Evolution	SIMBAD	[12][6]
BAT99-93 (in Tarantula Nebula of LMC)	67	165,000	13.446	45,000	Spectroscopy	SIMBAD	[7][19]
Sk -69° 200 (in NGC 2033 of LMC)	67	160,000	11.18	26,300	Evolution	SIMBAD	[28][19]
Arches-F18 (in Arches Cluster)	66.9	25,000	16.7 (J band)	36,900	Spectroscopy	SIMBAD	[35][36]
Arches-F4 (WR 102al in Arches Cluster)	66.4	25,000	15.63 (J band)	36,800	Spectroscopy	SIMBAD	[35][36]
BAT99-59 A (in NGC 2020 of LMC)	66	165,000	13.186 (combined)	71,000	Spectroscopy	SIMBAD	[7][19][e]
BAT99-104 (in Tarantula Nebula of LMC)	66	165,000	12.5	63,000	Spectroscopy	SIMBAD	[7][19]
HD 5980 B (in NGC 346 of SMC)	66	200,000	11.31 (combined)	45,000	Trinary	SIMBAD	[68][64]
HD 190429 A (near Barnard 146)	66	7,800	6.63 (combined)	46,000	Binary	SIMBAD	[69][15]
LH 31-1003 (in NGC 1858 of LMC)	66	160,000	13.186	41,900	Evolution	SIMBAD	[28][19]
LH 114-7 (in N70 of LMC)	66	160,000	13.66	50,000	Spectroscopy	SIMBAD	[18][19][o]
Pismis 24-1SW (in Pismis 24 of NGC 6357)	66	6,500	11.1	40,000	Binary	SIMBAD	[59][61]
BAT99-126 (in NGC 2081 of LMC)	65	165,000	13.166	71,000	Spectroscopy	SIMBAD	[7][19]
HSH95-40 (in Tarantula Nebula of LMC)	65	163,000	14.56	47,500	Evolution	SIMBAD	[24][8]
HSH95-58 (in Tarantula Nebula of LMC)	65	163,000	14.8	47,500	Evolution	SIMBAD	[24][8]
HSH95-89 (in Tarantula Nebula of LMC)	65	163,000	14.76	44,000	Spectroscopy	SIMBAD	[46]
VFTS 63 (in Tarantula Nebula of LMC)	65	164,000	14.4	42,200	Spectroscopy	SIMBAD	[11][49]
VFTS 145 (in Tarantula Nebula of LMC)	65	164,000	14.3	39,800	Spectroscopy	SIMBAD	[11][8]
VFTS 518 (in Tarantula Nebula of LMC)	65	164,000	15.11	44,700	Spectroscopy	SIMBAD	[11][8]
Westerhout 49-8 (in Westerhout 49)	65	36,200	15.617 (J band)	40,700	Evolution	SIMBAD	[5][6]
BD+43° 3654 (Runaway star from Cygnus OB2)	64.6	5,400	10.06	40,400	Evolution	SIMBAD	[70][64]
BAT99-129 A (in DEM L294 of LMC)	64	165,000	14.701 (combined)	79,000	Spectroscopy	SIMBAD	[7][19][p][e]
HSH95-50 (in Tarantula Nebula of LMC)	64	163,000	14.65	47,000	Evolution	SIMBAD	[24][8]
Sk -69° 25 (in NGC 1748 of LMC)	64	160,000	11.886	43,600	Evolution	SIMBAD	[28][19]
Trumpler 27-23 (in Trumpler 27)	64	3,900	10.09	27,500	Evolution	SIMBAD	[26][23]
Westerhout 49-5 (in Westerhout 49)	64	36,200	15.623 (J band)	42,700	Evolution	SIMBAD	[5][6]
HD 46223 (in NGC 2244 of Rosette Nebula)	63	5,200	7.28	46,000	Spectroscopy	SIMBAD	[18][15]
HD 64568 (in NGC 2467 of Puppis OB2)	63	16,000	9.39	54,000	Spectroscopy	SIMBAD	[18][23]
HD 303308 (in Trumpler 16 of Carina Nebula)	63	9,200	8.17	51,300	Evolution	SIMBAD	[26][23]
HR 6187 A (in NGC 6193 of Ara OB1)	63	4,300	5.54 (combined)	46,500	Septenary	SIMBAD	[71][15]
LH 10-3058 (in NGC 1763 of LMC)	63	160,000	14.089	54,000	Spectroscopy	SIMBAD	[18][19]
ST5-71 (in NGC 2074 of LMC)	63	160,000	13.266	45,400	Evolution	SIMBAD	[28][19]
AB9 (in DEM S80 of SMC)	62	197,000	15.431	100,000	Spectroscopy	SIMBAD	[60][50][q]
Brey 32 B (in NGC 1966 of LMC)	62	165,000	12.32 (combined)	43,600	Evolution	SIMBAD	[28][23]
HD 93160 (in Trumpler 14 of Carina Nebula)	62	8,000	7.6	42,700	Evolution	SIMBAD	[26][15]
HSH95-35 (in Tarantula Nebula of LMC)	62	163,000	14.43	47,500	Evolution	SIMBAD	[24][8]
LH 41-1017 (in NGC 1910 of LMC)	62	160,000	12.266	42,700	Evolution	SIMBAD	[28][19]
Mercer 30-6a A (WR 46-4 A in Mercer 30 of Dragonfish Nebula)	62	40,000	10.39 (J band)	29,900	Evolution	SIMBAD	[44][g][e]
ST4-18 (in NGC 2081 of LMC)	62	160,000	13.639	44,800	Evolution	SIMBAD	[28][19]
VFTS 664 (in Tarantula Nebula of LMC)	62	164,000	13.937	39,900	Spectroscopy	SIMBAD	[11][19]
HD 229196 (in Cygnus OB9)	61.6	5,000	8.59	40,900	Evolution	SIMBAD	[70][48]
AB8 B (in NGC 602 of SMC)	61	197,000	12.83 (combined)	45,000	Binary	SIMBAD	[68][72]
BAT99-79 A (in NGC 2044 of LMC)	61	165,000	13.486 (combined)	42,000	Spectroscopy	SIMBAD	[7][19][e]
HD 5980 A (in NGC 346 of SMC)	61	200,000	11.31 (combined)	21,000-53,000	Trinary	SIMBAD	[68][64]
LH 41-18 (in NGC 1910 of LMC)	61	160,000	12.586	38,500	Evolution	SIMBAD	[28][19]
Mercer 30-9 A (in Mercer 30 of Dragonfish Nebula)	61	40,000	12.25 (J band)	34,500	Evolution	SIMBAD	[44][g][e]
ST5-25 (in NGC 2074 of LMC)	61	160,000	13.551	48,600	Evolution	SIMBAD	[28][30]
VFTS 422 (in Tarantula Nebula of LMC)	61	164,000	15.14	39,800	Spectroscopy	SIMBAD	[11][8]
WR 102hb (in Quintuplet cluster)	61	26,000	13.9 (J band)	25,100	Evolution	SIMBAD	[73][74]
Sk -67° 166 (in GKK-A144 of LMC)	60.68	160,000	12.22	41,800	Spectroscopy	SIMBAD	[53][19][r]
Sk -67° 167 (in GKK-A144 of LMC)	60.68	160,000	12.586	41,800	Spectroscopy	SIMBAD	[53][19][r]
Sk -71° 46 (in BSDL 2242 of LMC)	60.68	160,000	13.241	41,800	Spectroscopy	SIMBAD	[53][19][s]
Brey 10 (in NGC 1770 of LMC)	60	165,000	12.69	117,000	Evolution	SIMBAD	[28][23]
Brey 94 A (in NGC 2081 of LMC)	60	165,000	12.996 (combined)	83,000	Evolution	SIMBAD	[28][19][e]
Brey 95a A (in NGC 2081 of LMC)	60	165,000	12.2 (combined)	83,000	Evolution	SIMBAD	[28][75][e]
HSH95-55 (in Tarantula Nebula of LMC)	60	163,000	14.74	47,500	Evolution	SIMBAD	[24][8]
Mercer 30-7 A (WR 46-5 A in Mercer 30 of Dragonfish Nebula)	60	40,000	11.516 (J band)	41,400	Evolution	SIMBAD	[44][g][e]
R134 (in Tarantula Nebula of LMC)	60	164,000	12.75	39,800	Spectroscopy	SIMBAD	[11][8]
R142 (in Tarantula Nebula of LMC)	60	164,000	11.82	18,000	Spectroscopy	SIMBAD	[62][8]
R143 (in Tarantula Nebula of LMC)	60	160,000	12.014	18,000-36,000	Evolution	SIMBAD	[51][19]
Sk -69° 142a (in NGC 1983 of LMC)	60	160,000	11.093	34,000	Evolution	SIMBAD	[51][54]
Sk -69° 259 (in NGC 2081 of LMC)	60	160,000	11.93	23,000	Evolution	SIMBAD	[28][23]
Var 83 (in Triangulum Galaxy)	60	3,000,000	16.027	18,000-37,000	Evolution	SIMBAD	[76][77]
VFTS 430 (in Tarantula Nebula of LMC)	60	164,000	15.11	24,500	Spectroscopy	SIMBAD	[62][8]

A few notable stars of mass less than 60 M_☉ are included for the purpose of comparison.

Star name	Mass (M☉, Sun = 1)	Approx. distance from earth (ly)	Apparent visible magnitude	Effective temperature (K)	Estimation method	Link	Reference
ζ Puppis (Naos in Vela R2 of Vela Molecular Ridge)	56.1	1,080	2.25	40,000	Spectroscopy	SIMBAD	[69][15][t]
λ Cephei (Runaway star from Cepheus OB3)	51.4	3,100	5.05	36,000	Spectroscopy	SIMBAD	[69][15]
τ Canis Majoris Aa (in NGC 2362)	50	5,120	4.89	32,000	Evolution	SIMBAD	[78][15]
θ Muscae Ab (in Centaurus OB1)	44	7,400	5.53 (combined)	33,000	Evolution	SIMBAD	[79][15]
ε Orionis (Alnilam in Orion OB1 of Orion complex)	40	2,000	1.69	27,500	Evolution	SIMBAD	[80][15]
θ2 Orionis A (in Orion OB1 of Orion complex)	39	1,500	5.02	34,900	Evolution	SIMBAD	[81][82]
α Camelopardalis (Runaway star from NGC 1502)	37.6	6,000	4.29	29,000	Evolution	SIMBAD	[83][15]
P Cygni (in IC 4996 of Cygnus OB1)	37	5,100	4.82	18,700	Spectroscopy	SIMBAD	[84][15][u]
ζ1 Scorpii (in NGC 6231 of Scorpius OB1)	36	8,210	4.705	17,200	Spectroscopy	SIMBAD	[37][85]
ζ Orionis Aa (Alnitak in Orion OB1 of Orion complex)	33	1,260	2.08	29,500	Evolution	SIMBAD	[86]
θ1 Orionis C1 (in Trapezium Cluster of Orion complex)	33	1,340	5.13 (combined)	39,000	Evolution	SIMBAD	[87][15]
κ Cassiopeiae (in Cassiopeia OB14)	33	4,000	4.16	23,500	Evolution	SIMBAD	[88][15]
μ Normae (in NGC 6169)	33	3,260	4.91	28,000	Spectroscopy	SIMBAD	[89][15]
η Carinae B (in Trumpler 16 of Carina Nebula)	30	7,500	4.3 (combined)	37,200	Binary	SIMBAD	[90][43]
γ2 Velorum B (in Vela OB2)	28.5	1,230	1.83 (combined)	35,000	Evolution	SIMBAD	[91][15]
λ Orionis A (Meissa in Collinder 69 of Orion complex)	27.9	1,100	3.54	37,700	Spectroscopy	SIMBAD	[89][92]
ξ Persei (Menkib in California Nebula of Perseus OB2)	26.1	1,200	4.04	35,000	Evolution	SIMBAD	[83][15]
WR 79a (in NGC 6231 of Scorpius OB1)	24.4	5,600	5.77	35,000	Spectroscopy	SIMBAD	[89][15]
δ Orionis Aa1 (Mintaka in Orion OB1 of Orion complex)	24	1,200	2.5 (combined)	29,500	Evolution	SIMBAD	[93][94]
ι Orionis Aa1 (Hatysa in NGC 1980 of Orion complex)	23.1	1,340	2.77 (combined)	32,500	Evolution	SIMBAD	[95][96]
κ Crucis (in Jewel Box Cluster of Centaurus OB1)	23	7,500	5.98	16,300	Evolution	SIMBAD	[97][64]
WR 78 (in NGC 6231 of Scorpius OB1)	22	4,100	6.48	50,100	Spectroscopy	SIMBAD	[33][34]
ο2 Canis Majoris (in Collinder 121)	21.4	2,800	3.043	15,500	Evolution	SIMBAD	[89][15]
β Orionis A (Rigel in Orion OB1 of Orion complex)	21	860	0.13	12,100	Evolution	SIMBAD	[98][15]
η Canis Majoris (Aludra in Collinder 121)	21	2,000	2.45	15,000	Evolution	SIMBAD	[88][15]
ζ Ophiuchi (in Upper Scorpius subgroup of Scorpius OB2)	20.2	370	2.569	34,000	Evolution	SIMBAD	[83][15]
υ Orionis (in Orion OB1 of Orion complex)	20	2,900	4.618	33,400	Evolution	SIMBAD	[99][100]
σ Orionis Aa (in Orion OB1 of Orion complex)	18	1,260	4.07 (combined)	35,000	Spectroscopy	SIMBAD	[101][102]
μ Columbae (Runaway star from Trapezium Cluster)	16	1,300	5.18	33,000	Spectroscopy	SIMBAD	[103][15]
κ Orionis (Saiph in Orion OB1 of Orion complex)	15.5	650	2.09	26,500	Evolution	SIMBAD	[104][15]
σ Cygni (in Cygnus OB4)	15	3,260	4.233	10,800	Evolution	SIMBAD	[105][106]
θ Carinae A (in IC 2602 of Scorpius OB2)	14.9	460	2.76 (combined)	31,000	Evolution	SIMBAD	[89][107]
θ2 Orionis B (in Orion OB1 of Orion complex)	14.8	1,500	6.38	29,300	Spectroscopy	SIMBAD	[108]
ζ Persei (in Perseus OB2)	14.5	750	2.86	20,800	Evolution	SIMBAD	[104][15]
σ Orionis B (in Orion OB1 of Orion complex)	14	1,260	4.07 (combined)	31,000	Spectroscopy	SIMBAD	[101][102]
β Canis Majoris (Mirzam in Local Bubble of Scorpius OB2)	13.5	490	1.985	23,200	Evolution	SIMBAD	[109][110]
ε Persei A (in α Persei Cluster)	13.5	640	2.88 (combined)	26,500	Evolution	SIMBAD	[111][112]
ι Orionis Aa2 (in NGC 1980 of Orion complex)	13.1	1,340	2.77 (combined)	27,000	Evolution	SIMBAD	[95][96]
δ Scorpii A (Dschubba in Upper Scorpius subgroup of Scorpius OB2)	13	440	2.307 (combined)	27,400	Evolution	SIMBAD	[113][114]
σ Orionis Ab (in Orion OB1 of Orion complex)	13	1,260	4.07 (combined)	29,000	Spectroscopy	SIMBAD	[101][102]
θ Muscae Aa (WR 48 in Centaurus OB1)	11.5	7,400	5.53 (combined)	83,000	Spectroscopy	SIMBAD	[115][15]
γ2 Velorum A (WR 11 in Vela OB2)	9	1,230	1.83 (combined)	57,000	Spectroscopy	SIMBAD	[91][15]
ρ Ophiuchi A (in ρ Ophiuchi cloud complex of Scorpius OB2)	8.7	360	4.63 (combined)	22,000	Evolution	SIMBAD	[89][15]
γ Orionis (Bellatrix in Bellatrix Cluster of Orion complex)	7.7	250	1.64	21,800	Evolution	SIMBAD	[116][15]
α Scorpii B (in Loop I Bubble of Scorpius OB2)	7.2	550	5.5	18,500	Evolution	SIMBAD	[117][92]
λ Tauri A (in Pisces-Eridanus stellar stream)	7.18	480	3.47 (combined)	18,700	Evolution	SIMBAD	[118][119]
δ Persei (in α Persei Cluster)	7	520	3.01	14,900	Evolution	SIMBAD	[89][107]
ψ Persei (in α Persei Cluster)	6.2	580	4.31	16,000	Evolution	SIMBAD	[89][15]
α Pavonis Aa (Peacock in Tucana-Horologium association)	5.91	180	1.94	17,700	Evolution	SIMBAD	[120][96]
η Tauri A (Alcyone in Pleiades)	5.9	440	2.87 (combined)	12,300	Evolution	SIMBAD	[121][15]
γ Canis Majoris (Muliphein in Collinder 121)	5.6	440	4.1	13,600	Evolution	SIMBAD	[89][122]
ο Velorum (in IC 2391 of Scorpius OB2)	5.5	490	3.6	16,200	Evolution	SIMBAD	[123][107]
ο Aquarii (in Pisces-Eridanus stellar stream)	4.2	440	4.71	13,500	Evolution	SIMBAD	[124][125]
ν Fornacis (in Pisces-Eridanus stellar stream)	3.65	370	4.69	13,400	Evolution	SIMBAD	[126][15]
φ Eridani (in Tucana-Horologium association)	3.55	150	3.55	13,700	Evolution	SIMBAD	[120][127]
η Chamaeleontis (in η Chamaeleontis moving group of Scorpius OB2)	3.2	310	5.453	12,500	Evolution	SIMBAD	[128][64]
ε Chamaeleontis (in ε Chamaeleontis moving group of Scorpius OB2)	2.87	360	4.91	10,900	Evolution	SIMBAD	[129][107]
τ1 Aquarii (in Pisces-Eridanus stellar stream)	2.68	320	5.66	10,600	Evolution	SIMBAD	[130][131]
ε Hydri (in Tucana-Horologium association)	2.64	150	4.12	11,000	Evolution	SIMBAD	[130][132]
β1 Tucanae (in Tucana-Horologium association)	2.5	140	4.37	10,600	Evolution	SIMBAD	[89][92]
Sun (in Solar System)	1	0.0000158	−26.744	5,772	Standard	IAU	[133][134][135]

*******************

List of the largest known stars in the Milky Way

Star name	Solar radii (Sun = 1)	Method[a]	Notes
Stephenson 2-18	2,150[4]	L/Teff	Located in close proximity to the extremely massive open cluster Stephenson 2 (RSGC2), where 25 other red supergiants are also located. Membership in the cluster currently uncertain, with large uncertainties in the measurements.
Orbit of Saturn	2,047–2,049.9[5][b]		Reported for reference
UY Scuti	1,708±192[6]	AD	The radius of UY Sct is more extreme than what current stellar evolution models predict. One paper mentions this extremity, and the reason for it is not yet clear.[7]
RSGC1-F01	1,530[8]	L/Teff
The above radii are larger than what stellar evolution theory predicts, and are thus potentially unreliable
Theoretical limit of star size (Milky Way)	~1,500[9]		This value comes from the rough average radii of the three largest stars studied in the paper. It is consistent with the largest possible stellar radii predicted from the current evolutionary theory, and it is believed that stars above this radius would be too unstable and simply do not form.[9] Reported for reference
RSGC1-F04	1,422[8]	L/Teff
VY Canis Majoris	1,420±120[10]	AD
KY Cygni	1,420±284–(2,850±570)[9]	L/Teff
CM Velorum	1,416.2385+0.3981 −0.9623[11]	L/Teff
AH Scorpii	1,411±124[6]	AD
RSGC1-F06	1,382[8]	L/Teff
CD-26 5055	1,279.8291+20.4064 −122.9196[11]	L/Teff
AS Cephei	1,262.5137+18.8257 −8.6085[11]	L/Teff
RSGC1-F10	1,246[8]	L/Teff
Westerlund 1 W237 (Westerlund 1 BKS B)	1,241±70[12]	L/Teff
IRC -10414	~1,200[13]	L/Teff
V517 Monocerotis	1,196.2521+79.7298 −158.8974[11]	L/Teff
PZ Cassiopeiae	1,190±238(–1,940±388)[9]	L/Teff
BC Cygni	1,186.6136+33.6601 −37.1276[11]	L/Teff	A more detailed but older study gives values of 1,081 R☉ (856–1,375) for the year 2000, and 1,303 R☉ (1,021–1,553) for the year 1900.[14]
RSGC1-F05	1,185[8]	L/Teff
NML Cygni	1,183[15]	L/Teff
GCIRS 7	1,170±60[16]–1,368[17]	AD
Westerlund 1 W26 (Westerlund 1 BKS AS)	1,165±58–1,221±120[12]	L/Teff
RSGC1-F08	1,150[8]	L/Teff
RSGC1-F02	1,128[8]	L/Teff
Orbit of Jupiter	1,114.5–1,115.8[5][b]		Reported for reference
V766 Centauri Aa	1,110±50[18]	?	V766 Centauri Aa is a rare variable yellow supergiant.
RT Carinae	1,090±218[9]	L/Teff
UU Persei	1,078.8212+8.5103 −8.2887[11]	L/Teff
V396 Centauri	1,070±214[9] – 1,145.31[19]	L/Teff & ?
HD 126577	1,065.5137+8.6624 −31.799[11]	L/Teff
W Persei	1,052.6853+76.7502 −85.3499[11]	L/Teff
V602 Carinae	1,050±165[20]	AD
RSGC1-F11	1,035[8]	L/Teff
RSGC1-F13	1,017[8]	L/Teff
CK Carinae	1,013.42 – 1,060±212[9]	L/Teff
KW Sagittarii	1,009±142[6]	AD
RSGC1-F07	1,006[8]	L/Teff
V349 Carinae	1,001.6769+12.0794 −73.6583[11]	L/Teff
RSGC1-F09	996[8]	L/Teff
RSGC1-F12	955[8]	L/Teff
RSGC1-F03	942[8]	L/Teff
AZ Cygni	911+57 −50[21]	AD
NSV 25875	891[15]	L/Teff
V437 Scuti	874[15]	L/Teff
LL Pegasi	869[15]	L/Teff
V669 Cassiopeiae	859[15]	L/Teff
Westerlund 1 W20 (Westerlund 1 BKS D)	858±48[12]	L/Teff
VX Sagittarii	853[15]–1,335±215[22]	L/Teff
BI Cygni	851.14[23]–1,240±248[9]	L/Teff
μ Cephei (Herschel’s Garnet Star)	830[15]–972±228[24]	AD
V1185 Scorpii	830[15]	L/Teff
CW Leonis	826[15]	L/Teff
LP Andromedae	815[15]	L/Teff
U Arietis	801±205[25]	AD
RT Ophiuchi	801±217[26]	AD
BO Carinae	790±158[9]	L/Teff
S Persei	780±156(–1,230±246)[9]	L/Teff
SU Persei	780±156[9] – 971.405[19]	L/Teff
RS Persei	770±30[27]	AD
V355 Cephei	770±154[9]	L/Teff
GU Cephei A	766.486[19]	?
Betelgeuse (α Orionis)	764+116 −62[28]	?	Tenth brightest star in the night sky.[29]
HD 303250	750±150[9]	L/Teff
UU Pegasi	742±193[26]	AD
Westerlund 1 W75 (Westerlund 1 BKS E)	722±36[12]	L/Teff
V Camelopardalis	716±185[26]	AD
V923 Centauri	715.539[19]	?
V528 Carinae	700±140[9]	L/Teff
The following well-known stars are listed for the purpose of comparison.
V354 Cephei	685[30]	L/Teff
Antares A (α Scorpii)	680[31]	AD	Fourteenth brightest star in the night sky.[29]
Mira A (ο Ceti)	541[15]	L/Teff
Unurgunite (σ Canis Majoris)	420±84[9]	L/Teff
Orbit of Mars	322–323.1[5][b]		Reported for reference
Pistol Star (V4647 Sagittarii)	306[32]	?
Rasalgethi A (α Herculis)	284±60 (264–303)[33]	L/Teff
Wezen (δ Canis Majoris)	215±66[34]	AD	Thirty-sixth brightest star in the night sky.[29]
Orbit of Earth (~1 AU)	214[5][b]		Reported for reference
Enif (ε Pegasi)	210.37 – 210.69[35]	?
Suhail (λ Velorum)	210[36]	?
Deneb (α Cygni)	203±17[37]	?	Eighteenth brightest star in the night sky.[29]
Orbit of Venus	158.6[5][b]		Reported for reference
Orbit of Mercury	82.9–84.6[5][b]		Reported for reference
Vega (α Lyrae)	2.726±0.006 × 2.418±0.012[38]		Fifth brightest star in the night sky.[29] Reported for reference
Sun	1		The largest object in the Solar System. Reported for reference

***********************

Large Quasar Groups

LQG	Date	Mean Distance	Dimension	# of quasars	Notes
Webster LQG (LQG 1)	1982	z=0.37	100 Mpc	5	First LQG discovered. At the time of its discovery, it was the largest structure known.[1][4][5]
Crampton–Cowley–Hartwick LQG (LQG 2, CCH LQG, Komberg-Kravtsov-Lukash LQG 10)	1987	z=1.11	60 Mpc	28	Second LQG discovered [1][4][6]
Clowes–Campusano LQG (U1.28, CCLQG, LQG 3)	1991	z=1.28	longest dimension: 630 Mpc	34	Third LQG discovered [4][7]
U1.90	1995	z=1.9	120 Mpc/h	10	Discovered by Graham, Clowes, Campusano.[1][6][8]
7Sf Group (U0.19)	1995	z=0.19	60 Mpc/h	7	Discovered by Graham, Clowes, Campusano; this is a grouping of 7 Seyfert galaxies.[1][6][8]
Komberg–Kravtsov–Lukash LQG 1	1996	z=0.6	R=96 Mpc/h	12	Discovered by Komberg, Kravtsov, Lukash.[1][6]
Komberg–Kravtsov–Lukash LQG 2	1996	z=0.6	R=111 Mpc/h	12	Discovered by Komberg, Kravtsov, Lukash.[1][6]
Komberg–Kravtsov–Lukash LQG 3	1996	z=1.3	R=123 Mpc/h	14	Discovered by Komberg, Kravtsov, Lukash.[1][6]
Komberg–Kravtsov–Lukash LQG 4	1996	z=1.9	R=104 Mpc/h	14	Discovered by Komberg, Kravtsov, Lukash.[1][6]
Komberg–Kravtsov–Lukash LQG 5	1996	z=1.7	R=146 Mpc/h	13	Discovered by Komberg, Kravtsov, Lukash.[1][6]
Komberg–Kravtsov–Lukash LQG 6	1996	z=1.5	R=94 Mpc/h	10	Discovered by Komberg, Kravtsov, Lukash.[1][6]
Komberg–Kravtsov–Lukash LQG 7	1996	z=1.9	R=92 Mpc/h	10	Discovered by Komberg, Kravtsov, Lukash.[1][6]
Komberg–Kravtsov–Lukash LQG 8	1996	z=2.1	R=104 Mpc/h	12	Discovered by Komberg, Kravtsov, Lukash.[1][6]
Komberg–Kravtsov–Lukash LQG 9	1996	z=1.9	R=66 Mpc/h	18	Discovered by Komberg, Kravtsov, Lukash.[1][6]
Komberg–Kravtsov–Lukash LQG 11	1996	z=0.7	R=157 Mpc/h	11	Discovered by Komberg, Kravtsov, Lukash.[1][6]
Komberg–Kravtsov–Lukash LQG 12	1996	z=1.2	R=155 Mpc/h	14	Discovered by Komberg, Kravtsov, Lukash.[1][6]
Newman LQG (U1.54)	1998	z=1.54	150 Mpc/h	21	Discovered by P.R. Newman et al. This structure is parallel to the CCLQG, with its discovery, suggesting that the cellular structure of sheets and voids already existed in this era, as found in later void bubbles and walls of galaxies.,[1][7]
Tesch–Engels LQG	2000	z=0.27	140 Mpc/h	7	The first X-ray selected LQG.[1]
U1.11	2011	z=1.11	longest dimension: 780 Mpc	38	[4][7]
Huge-LQG (U1.27)	2013	z=1.27	characteristic size: 500 Mpc longest dimension: 1240 Mpc	73	The largest structure known in the observable universe[4][9] until it was eclipsed by the Hercules–Corona Borealis Great Wall found one year later.[10][11][12]

*******************

Pre-20th century

• 5th century BC — Democritus proposes that the bright band in the night sky known as the Milky Way might consist of stars.
• 4th century BC — Aristotle believes the Milky Way to be caused by “the ignition of the fiery exhalation of some stars which were large, numerous and close together” and that the “ignition takes place in the upper part of the atmosphere, in the region of the world which is continuous with the heavenly motions“,^[1]
• 964 — Abd al-Rahman al-Sufi (Azophi), a Persian astronomer, makes the first recorded observations of the Andromeda Galaxy^[2] and the Large Magellanic Cloud^[3][4] in his Book of Fixed Stars, and which are the first galaxies other than the Milky Way to be observed from Earth,
• 11th century — Al-Biruni, another Persian astronomer, describes the Milky Way galaxy as a collection of numerous nebulous stars,^[5]
• 11th century — Alhazen (Ibn al-Haytham), an Arabian astronomer, refutes Aristotle’s theory on the Milky Way by making the first attempt at observing and measuring the Milky Way’s parallax,^[6] and he thus “determined that because the Milky Way had no parallax, it was very remote from the Earth and did not belong to the atmosphere”,^[7]
• 12th century — Avempace (Ibn Bajjah) of Islamic Spain proposes the Milky Way to be made up of many stars but that it appears to be a continuous image due to the effect of refraction in the Earth’s atmosphere,^[1]
• 14th century — Ibn Qayyim al-Jawziyya of Syria proposes the Milky Way galaxy to be “a myriad of tiny stars packed together in the sphere of the fixed stars” and that these stars are larger than planets,^[8]
• 1521 — Ferdinand Magellan observes the Magellanic Clouds during his circumnavigating expedition,
• 1610 — Galileo Galilei uses a telescope to determine that the bright band on the sky, the “Milky Way“, is composed of many faint stars
• 1612 – Simon Marius using a moderate telescope observes Andromeda and describes as a “flame seen through horn”.
• 1750 — Thomas Wright discusses galaxies and the flattened shape of the Milky Way and speculates nebulae as separate
• 1755 — Immanuel Kant drawing on Wright’s work conjectures our galaxy is a rotating disk of stars held together by gravity, and that the nebulae are separate such galaxies; he calls them Island Universes
• 1774 — Charles Messier releases a preliminary list of 45 Messier objects, three of which turn out to be the galaxies including Andromeda and Triangulum. By 1781 the final published list grows to 103 objects, 34 of which turn out to be galaxies.
• 1785 — William Herschel carried the first attempt to describe the shape of the Milky Way and the position of the Sun in it by carefully counting the number of stars in different regions of the sky. He produced a diagram of the shape of the galaxy with the solar system close to the center.
• 1845 — Lord Rosse discovers a nebula with a distinct spiral shape

Early 20th century

• 1912 — Vesto Slipher spectrographic studies of spiral nebulae find high Doppler shifts indicating recessional velocity.
• 1917 — Heber Curtis find novae in Andromeda Nebula M31 were ten magnitudes fainter than normal giving a distance estimate of 150,000 parsecs supporting the “island universes” or independent galaxies hypothesis for spiral nebulae.
• 1918 — Harlow Shapley demonstrates that globular clusters are arranged in a spheroid or halo whose center is not the Earth, and hypothesizes, correctly, that its center is the Galactic Center of the galaxy,
• 26 April 1920 — Harlow Shapley and Heber Curtis debate whether Andromeda Nebula is within the Milky Way. Curtis notes dark lanes in Andromeda resembling the dust clouds in the Milky Way, as well as significant Doppler shift.
• 1922 — Ernst Öpik distance determination supports Andromeda as extra-galactic object.
• 1923 — Edwin Hubble resolves the Shapley–Curtis debate by finding Cepheids in the Andromeda Galaxy, definitively proving that there are other galaxies beyond the Milky Way.
• 1930 — Robert Trumpler uses open cluster observations to quantify the absorption of light by interstellar dust in the galactic plane; this absorption had plagued earlier models of the Milky Way,
• 1932 — Karl Guthe Jansky discovers radio noise from the center of the Milky Way,
• 1933 — Fritz Zwicky applies the virial theorem to the Coma Cluster and obtains evidence for unseen mass,
• 1936 — Edwin Hubble introduces the spiral, barred spiral, elliptical, and irregular galaxy classifications,
• 1939 — Grote Reber discovers the radio source Cygnus A,
• 1943 — Carl Keenan Seyfert identifies six spiral galaxies with unusually broad emission lines, named Seyfert galaxies,
• 1949 — J. G. Bolton, G. J. Stanley, and O. B. Slee identify NGC 4486 (M87) and NGC 5128 as extragalactic radio sources,

Mid-20th century

• 1953 — Gérard de Vaucouleurs discovers that the galaxies within approximately 200 million light-years of the Virgo Cluster are confined to a giant supercluster disk,
• 1954 — Walter Baade and Rudolph Minkowski identify the extragalactic optical counterpart of the radio source Cygnus A,
• 1959 — Hundreds of radio sources are detected by the Cambridge Interferometer which produces the 3C catalogue. Many of these are later found to be distant quasars and radio galaxies
• 1960 — Thomas Matthews determines the radio position of the 3C source 3C 48 to within 5″,
• 1960 — Allan Sandage optically studies 3C 48 and observes an unusual blue quasistellar object,
• 1962 — Cyril Hazard, M. B. Mackey, and A. J. Shimmins use lunar occultations to determine a precise position for the quasar 3C 273 and deduce that it is a double source,
• 1962 — Olin Eggen, Donald Lynden-Bell, and Allan Sandage theorize galaxy formation by a single (relatively) rapid monolithic collapse, with the halo forming first, followed by the disk.
• 1963 — Maarten Schmidt identifies the redshifted Balmer lines from the quasar 3C 273
• 1973 — Jeremiah Ostriker and James Peebles discover that the amount of visible matter in the disks of typical spiral galaxies is not enough for Newtonian gravitation to keep the disks from flying apart or drastically changing shape,
• 1973 — Donald Gudehus finds that the diameters of the brightest cluster galaxies have increased due to merging, the diameters of the faintest cluster galaxies have decreased due to tidal distention, and that the Virgo cluster has a substantial peculiar velocity,
• 1974 — B. L. Fanaroff and J. M. Riley distinguish between edge-darkened (FR I) and edge-brightened (FR II) radio sources,
• 1976 — Sandra Faber and Robert Jackson discover the Faber-Jackson relation between the luminosity of an elliptical galaxy and the velocity dispersion in its center. In 1991 the relation is revised by Donald Gudehus,
• 1977 — R. Brent Tully and Richard Fisher publish the Tully–Fisher relation between the luminosity of an isolated spiral galaxy and the velocity of the flat part of its rotation curve,
• 1978 — Steve Gregory and Laird Thompson describe the Coma supercluster,
• 1978 — Donald Gudehus finds evidence that clusters of galaxies are moving at several hundred kilometers per second relative to the cosmic microwave background radiation,
• 1978 — Vera Rubin, Kent Ford, N. Thonnard, and Albert Bosma measure the rotation curves of several spiral galaxies and find significant deviations from what is predicted by the Newtonian gravitation of visible stars,
• 1978 — Leonard Searle and Robert Zinn theorize that galaxy formation occurs through the merger of smaller groups.

• 1981 — Robert Kirshner, August Oemler, Paul Schechter, and Stephen Shectman find evidence for a giant void in Boötes with a diameter of approximately 100 million light years,
• 1985 — Robert Antonucci and J. Miller discover that the Seyfert II galaxy NGC 1068 has broad lines which can only be seen in polarized reflected light,
• 1986 — Amos Yahil, David Walker, and Michael Rowan-Robinson find that the direction of the IRAS galaxy density dipole agrees with the direction of the cosmic microwave background temperature dipole,
• 1987 — David Burstein, Roger Davies, Alan Dressler, Sandra Faber, Donald Lynden-Bell, R. J. Terlevich, and Gary Wegner claim that a large group of galaxies within about 200 million light years of the Milky Way are moving together towards the “Great Attractor” in the direction of Hydra and Centaurus,
• 1987 — R. Brent Tully discovers the Pisces–Cetus Supercluster Complex, a structure one billion light years long and 150 million light years wide,
• 1989 — Margaret Geller and John Huchra discover the “Great Wall“, a sheet of galaxies more than 500 million light years long and 200 million wide, but only 15 million light years thick,
• 1990 — Michael Rowan-Robinson and Tom Broadhurst discover that the IRAS galaxy IRAS F10214+4724 is the brightest known object in the Universe,
• 1991 — Donald Gudehus discovers a serious systematic bias in certain cluster galaxy data (surface brightness vs. radius parameter, and the D n {\displaystyle D_{n}} method) which affect galaxy distances and evolutionary history; he devises a new distance indicator, the reduced galaxian radius parameter, r g {\displaystyle r_{g}} , which is free of biases,
• 1992 — First detection of large-scale structure in the Cosmic microwave background indicating the seeds of the first clusters of galaxies in the early Universe
• 1995 — First detection of small-scale structure in the cosmic microwave background
• 1995 — Hubble Deep Field survey of galaxies in field 144 arc seconds across.
• 1998 — The 2dF Galaxy Redshift Survey maps the large-scale structure in a section of the Universe close to the Milky Way
• 1998 — Hubble Deep Field South
• 1998 — Discovery of accelerating universe
• 2000 — Data from several cosmic microwave background experiments give strong evidence that the Universe is “flat” (space is not curved, although space-time is), with important implications for the formation of large-scale structure

Early 21st century

• 2001 — First data release from the ongoing Sloan Digital Sky Survey
• 2004 — The European Southern Observatory discovers Abell 1835 IR1916, the most distant galaxy yet seen from Earth.
• 2004 — The Arcminute Microkelvin Imager begins to map the distribution of distant clusters of galaxies
• 2005 — Spitzer Space Telescope data confirm what had been considered likely since the early 1990s from radio telescope data, i.e., that the Milky Way Galaxy is a barred spiral galaxy.^[9][10][11]
• 2012 — Astronomers report the discovery of the most distant dwarf galaxy yet found, approximately 10 billion light-years away.^[12]
• 2012 — The Huge-LQG, a large quasar group, one of the largest known structures in the universe, is discovered.^[13]
• 2013 — The galaxy Z8 GND 5296 is confirmed by spectroscopy to be one of the most distant galaxies found up to this time. Formed just 700 million years after the Big Bang, expansion of the universe has carried it to its current location, about 13 billion light years away from Earth (30 billion light years comoving distance).^[14]
• 2013 — The Hercules–Corona Borealis Great Wall, a massive galaxy filament and the largest known structure in the universe, was discovered through gamma-ray burst mapping.^[15][16][17]
• 2014 — The Laniakea Supercluster, the galaxy supercluster that is home to the Milky Way is defined via a new way of defining superclusters according to the relative velocities of galaxies.^[18][19] The new definition of the local supercluster subsumes the prior defined local supercluster, the Virgo Supercluster, as an appendage.^{[20][21][22][23][24]}
• 2020 — Astronomers report the discovery of a large cavity in the Ophiuchus Supercluster, first detected in 2016 and originating from a supermassive black hole with the mass of 10 million solar masses. The cavity is a result of the largest known explosion in the Universe. The formerly active galactic nucleus created it by emitting radiation and particle jets, possibly as a result of a spike in supply of gas to the black hole that could have occurred if a galaxy fell into the centre of the cavity.^[25][26][27]
• 2020 — Astronomers report to have discovered the disk galaxy Wolfe Disk, dating back to when the universe was only 1.5 billion years old, possibly indicating the need to revise theories of galaxy formation and evolution.^{[28][29][30][31]}
• 2020 — The South Pole Wall is a massive cosmic structure formed by a giant wall of galaxies (a galaxy filament) that extends across at least 1.37 billion light-years of space, and is located approximately a half billion light-years away.^{[32][33][34][35][36][37]}
• 2020 — After a 20-year-long survey, astrophysicists of the Sloan Digital Sky Survey publish the largest, most detailed 3D map of the universe so far, fill a gap of 11 billion years in its expansion history, and provide data which supports the theory of a flat geometry of the universe and confirms that different regions seem to be expanding at different speeds.^[38][39]
• 2022 — James Webb Space telescope releases the Webb’s First Deep Field

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The Extinction Cycle a.k.a. the Biblical Great Tribulation Period

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The following information is generally being placed on the bottom of some of the pages in which are being renamed and reworked. The goal is to help any visitor to better understand the overall theme of the End Times Biblical Teaching of the Great Tribulation Period, etc. It is not to overwhelm the page or the viewer, but to capture your attention, as some viewers only visit one page or many just a few and then move on, never to return again. Maybe with this material, you will understand how, then the why of the method. This bottom information material was created on June 4, 2022 and I may add a few more notes of time to time, which will appear on some pages, but not others. Most recent updates added to this page was on June 27, 2022.

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When the coming Extinction Cycle a.k.a the Biblical Great Tribulation Period actually begins with the Great Earthquakes; Massive Volcanic Eruptions; Tsunamis on a Global scale; a Comet hits the earth; the Magnetic Field weakens and allows Comic Lightening to strike the earth; and all the World Governmental, Corporate Business and Mainstream Religious Leaders, including all of the so called powers-that-be fail to provide Truthful answers; how are the almost 8 billion masses of humanity going to feel, when their lives are about to vanish away?

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It is going to be so amazing when these events begin to unfold and the people who present themselves as Leaders of People, (great and powerful), become nothing but mere frighten helpless creatures of earthen clay.

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Here are some Excellent, actually; they are Most Outstanding Videos from:

https://www.youtube.com/c/GeologyHub

Be sure to take time to watch them.

They will help you to understand how God will use the Earth to bring about the Great Tribulation Period with the use of Earthquakes and Volcanoes, including Tsunamis, which are produced by Underwater Earthquakes and Volcanic Eruptions, throughout the Oceans and Seas of the world.

From:  https://www.youtube.com/c/GeologyHub

and:  https://www.youtube.com/c/GeologyHub/videos

and:  https://twitter.com/HubGeology

and:  https://www.facebook.com/GeologyHubYT

and:  https://www.youtube.com/c/GeologyHub/community

and:  http://prospectingarizona.com/

and:  https://www.patreon.com/geologyhub

and amazing photos:   https://www.pinterest.com/prospectingarizona/

and their shop:  https://www.etsy.com/shop/prospectingarizona/

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01.   20 Largest Earthquakes in the World

02.   Global Earthquakes

03.   Megathrust Earthquake List

04.   Megathrust Earthquake

05.   Megathrust Earthquake Images

06.   Historical Earthquakes

07.   Deadly Earthquakes since 1900

08.   8.0+ Earthqauake in Images

09.   8.0+ Earthqauake in Videos

10.  EarthquakeTrack.com 8.0+ Earthquake List

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June 2, 2022: a new galaxy discovered as to be the farthest from earth.

01.    New Galaxy Farthest from Earth

02.   New Galaxy Farthest from Earth in Images

03.   Farthest Galaxy From Earth; Jan 22, 2022

04.  HUBBLE ULTRA DEEP FIELD

05.   Deep Universe Observatory videos

06.   HD1 (galaxy)

07.   Galaxy Cluster

08.   Supercluster

09.   List of Largest Cosmic Structures

10.   List of the Most Distant Astronomical Objects

11.   Blue Variable Star

12.  Luminous Blue Variable

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13.   The Largest Black Holes in the Universe; Sep 26, 2012

14.   Stunning Portrait of the Milky Way Galaxy; Dec 31, 2008

15.   Hubble Dazzling First Light Images in HD; Sep 9, 2009

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There is virtually an unlimited amount of comprehension in the Universe. It is going to be so amazing, when True Christian Believers enter into infinity!!! Likewise, it is going to be very unfortunate for others, who are not True Christian Believers, but simply put on a show of religion or else those individuals who have never been Saved by Grace through Faith in the Lord Jesus Christ.

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June 14, 2022: Hey Viewers, if any??? Here is a brief review with links about some Bible Prophecy dealing with Islam, Judaism and Roman Catholics.

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01.  There are several pages of studies on this website about how the Roman Catholics will unite with Islam and eventually with the Biblical Antichrist of the 10 Islamic nations in the Middle East; which will form an Islamic Caliphate. Sometime during this 3 ½ year time frame, the followers of Islam will turn against the Catholics within the region and basically pillage and burn their buildings, then kill them by the millions.

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02.  Islam in a round-about-way is trying and will more so in the future, to deceive the Jews in Israel; that they want peace, at least in some regards, among some groups of people. This will catch them off guard; then the Islamic masses surrounding the nation Israel will conduct a surprise military attack and kill 2/3rds of the Jewish population, capture Jerusalem and all the land from Dan to Beersheba; then hold it for 3 ½ years. There are about 6,894,000 Jews in Israel. The Bible informs us that of this Jewish population, 2/3rds will be killed during the invasion from the Islamic forces, which will amount to about 4,619,000 Jews; more or less, depending on when this invasion occurs.

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03.  The followers of Islam during this end time prophecy, will be giving an allegiance to the Biblical Antichrist or Beast of Revelation. This person is the Islamic leader of the core 10 Islamic Nations that unite to form this Caliphate in the Middle East. At the end of this 3 ½ years at the Battle of Armageddon; when it is assembled in the Valley of Megiddo, (Megiddo valley is also called Plain of Esdraelon or Plain of Jezreel (Vale of Jezreel) the Jordan River Valley will spread apart enough to create a Basalt Lava Field and destroy the majority of the army of the Antichrist. The masses of Islamic followers, along with the Islamic Antichrist and the Islamic Religious leader will all be cast into the Lake of Fire.

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04. This study reminds me of the Story of Babel, when people built a tower and were of one language, then God came down and put an end to their project. The Great Tribulation Period will be a process of putting an end to this one world type religious merger. Of course, most people will not accept this fact; but this new world religious merger will only be allowed to exist for a few years; as the Great Tribulation Period, with the Wrath of God from the Book of Revelation will put an end to this process; with the destruction of most of the population of the world and finally the complete and total burning of the Vatican City in Rome, Italy by the Volcanic Fire from the Volcanic Complex above the Subduction Zone, then the entire land will subside into Hades; and then being covered by the Mediterranean Sea. This will be the End of the Vatican City, as the leadership of this religious system will not be allowed to enter into the Millennial Reign of the Lord Jesus Christ.

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Here is where the Vatican City and it’s leadership will be going in the near future; including all the followers of Islam; the Devil; the Islamic Antichrist, who is the Islamic Leader of the Caliphate and the Islamic False Prophet; the masses of False Religions; the Atheists and every human being who is considered accountable to be able to make a decision about receiving the Lord Jesus Christ as their Savior; but will not put their Faith in the Blood Sacrifice of Christ alone. There future is under the crust of the earth, which is Hades or even further down, within the core of the earth and eventually they all will be cast into the Lake of Fire, which will probably be some form of energy, beyond the elements of the present earth or even the stars in the universe. At least you will not be concerned about Climate Change or Global Warming!!! Wow, I made a little joke!!!

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Revelation 14: [9] And the third angel followed them, saying with a loud voice, If any man worship the beast and his image, and receive his mark in his forehead, or in his hand, [10] The same shall drink of the wine of the wrath of God, which is poured out without mixture into the cup of his indignation; and he shall be tormented with fire and brimstone in the presence of the holy angels, and in the presence of the Lamb: [11] And the smoke of their torment ascendeth up for ever and ever: and they have no rest day nor night, who worship the beast and his image, and whosoever receiveth the mark of his name.

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Revelation 19: [20] And the beast was taken, and with him the false prophet that wrought miracles before him, with which he deceived them that had received the mark of the beast, and them that worshipped his image. These both were cast alive into a lake of fire burning with brimstone.

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Revelation 20: [10] And the devil that deceived them was cast into the lake of fire and brimstone, where the beast and the false prophet are, and shall be tormented day and night for ever and ever. [11] And I saw a great white throne, and him that sat on it, from whose face the earth and the heaven fled away; and there was found no place for them. [12] And I saw the dead, small and great, stand before God; and the books were opened: and another book was opened, which is the book of life: and the dead were judged out of those things which were written in the books, according to their works. [13] And the sea gave up the dead which were in it; and death and hell delivered up the dead which were in them: and they were judged every man according to their works. [14] And death and hell were cast into the lake of fire. This is the second death. [15] And whosoever was not found written in the book of life was cast into the lake of fire.

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Here is a preview of your future!!!

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01.   Earth Core

02.   Earth Mantle

03.   Earth Interior

04.   Earth Magma Core

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05.   Sun Core Temperature

06.   Sun Core Temperature Images

07.    Star Core Temperature

08.   Star Core Temperature Images

09.   Hottest Star Temperature

10.    Hottest Star Temperature Images

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An upper layer of the sun’s atmosphere called the photosphere has a temperature of about 10,000 degrees Fahrenheit. If one compares this temperature to the Earth’s core temperature, which is approximately 10,800 degrees Fahrenheit, one finds that the Earth’s core is hotter than this layer of the sun’s surface. However, the sun’s core temperature can be as high as 27 million degrees Fahrenheit. If one compares this to Earth’s core temperature of 10,800 degrees Fahrenheit, then the sun’s core temperature is much hotter than that of the Earth’s core. If one goes more in-depth into the universe, a helium flash in the core of Red Giant Stars; the temperature reaches 200 million Kelvin = 359,999,540 degrees Fahrenheit.

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Perhaps the hottest place is in the star core temperature that rises to over 100 billion degrees Fahrenheit as the iron atoms are crushed together, just before a star goes supernova, then turns into a black hole.

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Of course, these temperatures are estimated; but such places will not be a pleasant environment to exist in for eternity!!!

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Genesis 11: [1] And the whole earth was of one language, and of one speech.[2] And it came to pass, as they journeyed from the east, that they found a plain in the land of Shinar; and they dwelt there. [3] And they said one to another, Go to, let us make brick, and burn them throughly. And they had brick for stone, and slime had they for morter. [4] And they said, Go to, let us build us a city and a tower, whose top may reach unto heaven; and let us make us a name, lest we be scattered abroad upon the face of the whole earth. [5] And the LORD came down to see the city and the tower, which the children of men builded. [6] And the LORD said, Behold, the people is one, and they have all one language; and this they begin to do: and now nothing will be restrained from them, which they have imagined to do. [7] Go to, let us go down, and there confound their language, that they may not understand one another’s speech. [8] So the LORD scattered them abroad from thence upon the face of all the earth: and they left off to build the city. [9] Therefore is the name of it called Babel; because the LORD did there confound the language of all the earth: and from thence did the LORD scatter them abroad upon the face of all the earth.

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05.  Here are some interesting links. I am not going to include all of the links here to the studies on this site, if you are interested enough, then take time to scroll down the page list and look them up or you can also use the Search Button at the top of the page for faster results.

A.    Abrahamic Family House from Wikipedia

B.    Abrahamic Family House on the Internet
C.    Abrahamic Family House in Images

D.   Chrislam

E.   Chrislam Movement and the Pope

F.    One World Religion Headquarters

G.    Pope Announces New World Religion

H.   One World Religion Headquarters to Open 2022

I.    Catholic Muslim Interfaith Council

J.   Chrislam One World Religion

K….

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A.   My study:  Roman Catholicism in the End Times

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May 26, 2022:

There will be a comet coming in the future; as it will be Trumpet 3 and Vial 3 of the Book of Revelation, as it will actually hit the earth’s atmosphere, melt and cause a massive meteor storm, with the chemical poisons being absorbed into the hydrological cycle possible over Eurasia. Here are some interesting links about the subject:

01.   Fire In The Sky! Comet SW3; May 24, 2022

02.   fragments-of-a-dying-comet

03.   shattered-comet-tau-herculids-meteor-shower

04.   dying-comet a good show

05.   tau-herculid-meteors-may-intense-shower

06.  crumbling-comet-could-create-new-meteor-shower

07…..

Some studies on my website:

01.   revelation-3rd-trumpet-and-3rd-vial

02.   science-in-revelation-part-12-comet

03.   seven-trumpets-of-revelation-3rd-trumpet

04.  seven-vials-of-revelation-3rd-vial

05.  wormwood-stinks-comets

06.   wormwood

07…….

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The general focus of this website is to provide Biblical, Astronomical, Geological and Meteorological; including Middle East Political events, related to the Islamic Caliphate that are forthcoming; with information about the Great Tribulation Period from the 7 Trumpets and 7 Vials of the Book of Revelation and the Parousia of the Lord Jesus Christ.

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There is sufficient study material on this website to serve as a guide towards understanding the Truthful Teaching of the Biblical Antichrist and his Islamic Caliphate in the Middle East Region; the Great Tribulation Period; the Seven Trumpets and Vials of the Book of Revelation; the 45+/- Days of the Wrath of God; the Rapture of the True Christian Believers, a.k.a. the Catching Out; the Parousia of the Lord Jesus Christ; and finally, some general information about the beginning of the Millennial Reign.

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Here are some interesting Videos about the Economy. This is important, as the economy worsens, this will cause the rise of the Biblical Antichrist in the Middle East Region and eventually the Mark, Name and Number of the Beast, 666; which will basically be a means of identification, mostly used in the Islamic Caliphate Empire for the food rations program.

01.    Mark, Name and Number of the Biblical Antichrist

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01.    Gravitas: US stocks lose $7 trillion in 2022; May 13, 2022

02.   Gravitas Plus: a Debt Storm is Coming; May 14, 2022

03……

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All of the Sermons are on both Websites:

01.     02 Sermons on BibleSermonsMP3.org

02.    03 Sermons on BibleSermonsMP3.com

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01.Video Link.   Mount Edgecumbe Volcano; Apr 14, 2022

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A Big Solar Storm may be coming in 2022:

01.Video Link.   Big Solar Storm Coming Soon? Mar 7, 2022

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Coronal Mass Ejections from the Sun. I believe eventually, these charged particles will hit the Earth in the Future; that will be so intense, they will penetrate through an opening in the Magnetic Shield, as it will be at a weaken state; then upon striking the Earth, will cause the three Earthquakes, with the 3rd being the Greatest Earthquake in Human History, as is mentioned in the Book of Revelation.

Page on Website:  01C Geomagnetic Storms

Page on Website:  01C Solar Activity

Page on Website:  Cosmic Lightning

01.Video Link.    Sun Erupts at Earth; Mar 10, 2022

02.Video Link.   Solar Eruption; Mar 11, 2022

03.Video Link.   Solar Flare; Mar 12, 2022

04.Video Link.   CME Impact; Mar 13, 2022

05.Video Link.   CME Impact; Mar 14, 2022

06.Video Link.  Many Solar Flares; Mar 28, 2022

07.Video Link.   7 Solar Flares; Mar 29, 2022

08.Video Link.   Solar Storm Approaching; Mar 30, 2022

09.Video Link.   X Class Solar Flare & CME; Mar 30, 2022

10.Video Link.    Strong Geomagnetic Storm in Progress; Apr 10, 2022

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There are a few verses in the Book of Revelation that have the word: lightning in the text.

It is possible, this Cosmic Lightning could occur and cause Earthquakes, which in turn cause Volcanic Eruptions, which have Volcanic Lightning!!!

Here are the Verses in Revelation. It starts with the Seven Trumpets and Ends with the Seven Vials of the Wrath of God.

1. Revelation 8:5: and there were voices, and thunderings, and lightnings, and an earthquake.

2. Revelation 11:19: and there were lightnings, and voices, and thunderings, and an earthquake, and great hail.

3. Revelation 16:18 & 21: And there were voices, and thunders, and lightnings; and there was a great earthquake, such as was not since men were upon the earth, so mighty an earthquake, and so great. [21] And there fell upon men a great hail out of heaven, every stone about the weight of a talent: and men blasphemed God because of the plague of the hail; for the plague thereof was exceeding great.

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Here is a brief statement of what I a referring to, with regards to Cosmic Lightning:  “For an hour on March 13^th, a big crack opened in Earth’s magnetic field – one of the biggest in years (For specialists: BsubZ less than -20 nT),” Dr. Tony Phillips of SpaceWeather.com noted.³  “Solar wind poured through the gap, adding its energy to that of the CME which struck earlier in the day. This increases the chances that high-latitude auroras may remain visible at least through the early hours of March 14^th.” What Dr. Phillips described took place from 21:33 to 22:36 UTC.  From:   Watchers.News/2022/03/13/CME Hits Earth

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Awesome Video; be sure to take time to Watch it…!!!

01.Video Link.  Asteroid Impacts; Mar 8, 2022

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