223:
270:
31:
2448:
83:
307:
296:
2460:
285:
278:
2500:
2524:
2512:
2488:
362:
Bars. Galaxies are divided on the basis of the presence or absence of a nuclear bar. De
Vaucouleurs introduced the notation SA to denote spiral galaxies without bars, complementing Hubbleâs use of SB for barred spirals. He also allowed for an intermediate class, denoted SAB, containing weakly barred
237:
The Hubble sequence is often represented in the form of a two-pronged fork, with the ellipticals on the left (with the degree of ellipticity increasing from left to right) and the barred and unbarred spirals forming the two parallel prongs of the fork on the right. Lenticular galaxies are placed
462:
Elliptical galaxies are divided into three 'stages': compact ellipticals (cE), normal ellipticals (E) and late types (E). Lenticulars are similarly subdivided into early (S), intermediate (S) and late (S) types. Irregular galaxies can be of type magellanic irregulars
406:
The different elements of the classification scheme are combined â in the order in which they are listed â to give the complete classification of a galaxy. For example, a weakly barred spiral galaxy with loosely wound arms and a ring is denoted SAB(r)c.
369:
Spiral arms. As in Hubbleâs original scheme, spiral galaxies are assigned to a class based primarily on the tightness of their spiral arms. The de
Vaucouleurs scheme extends the arms of Hubbleâs tuning fork to include several additional spiral classes:
363:
spirals. Lenticular galaxies are also classified as unbarred (SA0) or barred (SB0), with the notation S0 reserved for those galaxies for which it is impossible to tell if a bar is present or not (usually because they are edge-on to the line-of-sight).
656:, Morgan also developed the MK system for the classification of stars through their spectra. The Yerkes scheme uses the spectra of stars in the galaxy; the shape, real and apparent; and the degree of the central concentration to classify galaxies.
102:
in 1926. It is often known colloquially as the âHubble tuning-forkâ because of the shape in which it is traditionally represented. Hubble's scheme divides galaxies into three broad classes based on their visual appearance (originally on
384:
Most galaxies in these three classes were classified as Irr I in Hubbleâs original scheme. In addition, the Sd class contains some galaxies from Hubbleâs Sc class. Galaxies in the classes Sm and Im are termed the
438:
run from â6 to +10, with negative numbers corresponding to early-type galaxies (ellipticals and lenticulars) and positive numbers to late types (spirals and irregulars). Thus, as a rough rule, lower values of
200:, which is similar in appearance to an elliptical galaxy. They are given the symbol "S". Roughly half of all spirals are also observed to have a bar-like structure, extending from the central bulge. These
177:
366:
Rings. Galaxies are divided into those possessing ring-like structures (denoted â(r)â) and those without rings (denoted â(s)â). So-called âtransitionâ galaxies are given the symbol (rs).
330:âbased on the tightness of the spiral arms and the presence or absence of a barâdid not adequately describe the full range of observed galaxy morphologies. In particular, he argued that
443:
correspond to a larger fraction of the stellar mass contained in a spheroid/bulge relative to the disk. The approximate mapping between the spheroid-to-total stellar mass ratio (M
52:
into groups based on their visual appearance. There are several schemes in use by which galaxies can be classified according to their morphologies, the most famous being the
357:. To complement Hubble's scheme, de Vaucouleurs introduced a more elaborate classification system for spiral galaxies, based on three morphological characteristics:
1503:
Obreschkow, D.; Croton, D.; De Lucia, G.; Khochfar, S.; Rawlings, S. (2009). "Simulation of the Cosmic
Evolution of Atomic and Molecular Hydrogen in Galaxies".
2270:
1443:
1448:
Proceedings of "Quantifying Galaxy
Morphology at High Redshift", A Workshop Held at the Space Telescope Science Institute, Baltimore MD, April 27-29 1994
1224:
1220:"Galaxy Zoo: unwinding the winding problem â observations of spiral bulge prominence and arm pitch angles suggest local spiral galaxies are winding"
118:
representing their degree of ellipticity on the sky. The specific ellipticity rating depends on ratio of the major (a) to minor axes (b), thus:
241:
To this day, the Hubble sequence is the most commonly used system for classifying galaxies, both in professional astronomical research and in
2317:
2549:
114:
have smooth, featureless light distributions and appear as ellipses in images. They are denoted by the letter "E", followed by an integer
1967:
218:, the disks of lenticular galaxies have no visible spiral structure and are not actively forming stars in any significant quantity.
230:
These broad classes can be extended to enable finer distinctions of appearance and to encompass other types of galaxies, such as
17:
127:
1644:
1565:
1358:
1306:
1160:
1046:
434:
De
Vaucouleurs also assigned numerical values to each class of galaxy in his scheme. Values of the numerical Hubble stage
68:. However, galaxy classification and morphology are now largely done using computational methods and physical morphology.
2544:
879:
2383:
2302:
885:
1451:
2554:
1683:
2388:
1135:
2115:
374:
Sd (SBd) â diffuse, broken arms made up of individual stellar clusters and nebulae; very faint central bulge
222:
2285:
1606:
2478:
2403:
2358:
2225:
2166:
2062:
1755:
1750:
1723:
1350:
1187:
2004:
2084:
1782:
1219:
2307:
1328:
1191:
269:
2368:
2280:
2275:
2181:
2077:
2035:
1745:
1718:
1439:
1278:
323:
61:
2363:
2348:
2327:
2295:
1954:
1942:
1937:
1851:
1816:
1787:
1777:
1086:
1866:
1765:
1658:
to try your hand at classifying galaxies as part of an Oxford
University open community project
398:
394:
311:
238:
between the ellipticals and the spirals, at the point where the two prongs meet the âhandleâ.
2559:
2428:
2393:
2290:
1992:
1581:
988:
897:
649:
637:
1479:
2423:
2373:
2208:
2120:
1856:
1740:
1676:
1522:
1410:
1286:
1243:
1062:
960:
653:
201:
888: â Chart depicting the relationship between brightness and mass of large star systems
8:
2528:
2186:
2094:
2025:
1932:
1917:
1792:
1526:
1414:
1290:
1247:
964:
291:: a spiral galaxy (type SB(r)0/a) with three rings of different radii, as well as a bar.
2516:
2504:
2418:
2413:
2398:
2353:
2322:
2193:
2030:
1982:
1972:
1538:
1534:
1512:
1401:
de
Vaucouleurs, GĂ©rard (April 1963). "Revised Classification of 1500 Bright Galaxies".
1316:
1233:
982:
104:
1638:
2459:
2451:
2433:
2408:
2378:
2257:
2099:
2089:
2072:
1833:
1799:
1760:
1713:
1632:
1561:
1542:
1354:
1302:
1042:
992:
411:
390:
386:
346:
342:
318:
The de
Vaucouleurs system for classifying galaxies is a widely used extension to the
246:
242:
211:
207:
197:
111:
953:
Contributions from the Mount Wilson
Observatory / Carnegie Institution of Washington
2463:
2265:
2240:
2220:
2215:
2203:
2057:
1878:
1811:
1530:
1418:
1294:
1251:
1013:
923:
867:
354:
231:
2312:
2235:
1927:
1900:
1871:
1823:
1669:
1285:. Handbuch der Physik / Encyclopedia of Physics. Vol. 53. pp. 275â310.
335:
319:
258:
254:
77:
53:
35:
1298:
2176:
2009:
1912:
1907:
1861:
1804:
1110:
326:
in 1959. De
Vaucouleurs argued that Hubble's two-dimensional classification of
2538:
2332:
2198:
2161:
1895:
1883:
1735:
1730:
350:
327:
234:, which have no obvious regular structure (either disk-like or ellipsoidal).
215:
185:
65:
30:
1374:
1256:
2492:
2230:
2171:
2156:
1987:
1772:
1342:
978:
948:
903:
341:
The de Vaucouleurs system retains Hubble's basic division of galaxies into
99:
57:
2245:
2135:
2125:
1922:
1888:
1828:
1708:
1196:
2130:
2067:
1456:
891:
250:
82:
45:
1645:
The Spitzer Infrared Nearby Galaxies Survey (SINGS) Hubble Tuning-Fork
749:
Rotational symmetry without pronounced spiral or elliptical structure
306:
295:
2140:
284:
87:
277:
1422:
1238:
299:
288:
95:
1517:
94:
The Hubble sequence is a morphological classification scheme for
1502:
996:
1977:
1962:
1692:
1283:
Astrophysik IV: Sternsysteme / Astrophysics IV: Stellar Systems
193:
49:
1281:(1959). "Classification and Morphology of External Galaxies".
2050:
2045:
2040:
1997:
331:
196:
structure, and a central concentration of stars known as the
410:
Visually, the de Vaucouleurs system can be represented as a
1661:
1655:
1192:"Citizen scientists re-tune Hubble's galaxy classification"
214:
surrounded by an extended, disk-like structure but, unlike
189:
2487:
1648:
1480:"Qualitative and Quantitative Classifications of Galaxies"
1186:
414:
of Hubble's tuning fork, with stage (spiralness) on the
338:
are important structural components of spiral galaxies.
172:{\displaystyle E=10\times \left(1-{\frac {b}{a}}\right)}
377:
Sm (SBm) â irregular in appearance; no bulge component
2476:
1014:"The Hubble tuning fork â classification of galaxies"
648:
The Yerkes scheme was created by American astronomer
226:
The Hubble sequence throughout the universe's history
130:
1555:
1434:
1432:
1341:
27:
System for categorizing galaxies based on appearance
171:
1429:
1335:
1225:Monthly Notices of the Royal Astronomical Society
1217:
273:Hubble â de Vaucouleurs Galaxy Morphology Diagram
210:(designated S0) also consist of a bright central
2536:
1218:Masters, Karen L.; et al. (30 April 2019).
1111:"Hubble explores the origins of modern galaxies"
1008:
1006:
261:, may not be supported, and may need updating.
1651:Spitzer Space Telescope Legacy Science Project
1438:
1400:
1277:
1211:
2318:List of the most distant astronomical objects
1677:
1003:
882: â Russian catalogue of 30,642 galaxies
643:
636:The use of numerical stages allows for more
1180:
1684:
1670:
1635:â an introduction to galaxy classification
1067:COSMOS â The SAO Encyclopedia of Astronomy
1560:. Princeton: Princeton University Press.
1516:
1255:
1237:
1041:. Princeton: Princeton University Press.
429:
1444:"Global Physical Parameters of Galaxies"
1396:
1394:
941:
629:
623:
605:
602:
389:and irregulars, respectively, after the
305:
294:
283:
276:
268:
264:
221:
81:
29:
422:-axis, and variety (ringedness) on the
14:
2537:
1036:
977:
947:
894: â Crowdsourced astronomy project
1665:
1639:Near-Infrared Galaxy Morphology Atlas
1391:
459:=(10âT)/256 based on local galaxies.
906: â Swiss astronomer (1898â1974)
2550:Astronomical classification systems
1604:
1556:Binney, J.; Merrifield, M. (1998).
1158:
880:Morphological Catalogue of Galaxies
42:Galaxy morphological classification
24:
951:(1926). "Extra-galactic nebulae".
418:-axis, family (barredness) on the
188:consist of a flattened disk, with
71:
25:
2571:
1626:
302:: a spiral galaxy of type SA(s)d.
90:is classified as an S0/Sa galaxy.
34:Tuning-fork-style diagram of the
2522:
2510:
2498:
2486:
2458:
2447:
2446:
1403:Astrophysical Journal Supplement
765:Elliptical with dust absorption
1598:
1574:
1549:
1496:
1472:
1367:
1271:
1152:
2389:Galaxy formation and evolution
2384:Galaxy colorâmagnitude diagram
1128:
1103:
1079:
1055:
1030:
971:
924:"A remarkable galactic hybrid"
916:
886:Galaxy colorâmagnitude diagram
640:studies of galaxy morphology.
192:forming a (usually two-armed)
13:
1:
910:
245:. Nonetheless, in June 2019,
1691:
1535:10.1088/0004-637X/698/2/1467
1375:"Galaxy â Types of galaxies"
380:Im â highly irregular galaxy
7:
2271:Galaxies named after people
1582:"The Yerkes Classification"
1299:10.1007/978-3-642-45932-0_7
900: â American astronomer
873:
451:) and the Hubble stage is M
255:usual Hubble classification
10:
2576:
2545:Galaxy morphological types
2404:Gravitational microlensing
2359:Galactic coordinate system
1351:Princeton University Press
1188:Royal Astronomical Society
397:is of type SBm, while the
257:, particularly concerning
204:are given the symbol "SB".
75:
2442:
2341:
2256:
2149:
2108:
2018:
1953:
1844:
1699:
1633:Galaxies and the Universe
1505:The Astrophysical Journal
1345:; Merrifield, M. (1998).
644:Yerkes (or Morgan) scheme
600:approximate Hubble class
412:three-dimensional version
2369:Galactic magnetic fields
2182:Brightest cluster galaxy
2078:Luminous infrared galaxy
1115:ESA/Hubble Press Release
984:The Realm of the Nebulae
2555:Extragalactic astronomy
2364:Galactic habitable zone
2349:Extragalactic astronomy
1938:Supermassive black hole
1852:Active galactic nucleus
1607:"galaxy classification"
1379:Encyclopedia Britannica
866:Thus, for example, the
781:Low surface brightness
475:Numerical Hubble stage
2116:Low surface brightness
1867:Central massive object
1037:Binney, James (1998).
1018:www.spacetelescope.org
928:www.spacetelescope.org
870:is classified as kS5.
430:Numerical Hubble stage
399:Small Magellanic Cloud
395:Large Magellanic Cloud
315:
312:Large Magellanic Cloud
303:
292:
281:
274:
227:
173:
91:
60:and later expanded by
38:
18:Morphology (astronomy)
2394:Galaxy rotation curve
1611:www.daviddarling.info
1257:10.1093/mnras/stz1153
1161:"THE HUBBLE SEQUENCE"
1087:"Lenticular Galaxies"
989:Yale University Press
898:William Wilson Morgan
789:Small bright nucleus
650:William Wilson Morgan
542:de Vaucouleurs class
401:is an irregular (Im).
324:GĂ©rard de Vaucouleurs
322:, first described by
309:
298:
287:
280:
272:
265:De Vaucouleurs system
225:
174:
85:
62:GĂ©rard de Vaucouleurs
33:
2429:Population III stars
2424:Intergalactic travel
2374:Galactic orientation
2241:Voids and supervoids
1586:ned.ipac.caltech.edu
1511:(2). Equation (18).
1484:ned.ipac.caltech.edu
860:Galaxy is "edge-on"
817:Galaxy is "face-on"
713:Prominent GâK stars
697:Prominent FâG stars
681:Prominent AâF stars
467:= 10) or 'compact' (
387:âMagellanicâ spirals
314:: a type SBm galaxy.
128:
44:is a system used by
2419:Intergalactic stars
2308:Large quasar groups
2303:Groups and clusters
2167:Groups and clusters
2026:Lyman-alpha emitter
1918:Interstellar medium
1527:2009ApJ...698.1467O
1415:1963ApJS....8...31D
1291:1959HDP....53..275D
1248:2019MNRAS.487.1808M
1063:"Elliptical Galaxy"
965:1926CMWCI.324....1H
476:
208:Lenticular galaxies
112:Elliptical galaxies
105:photographic plates
2414:Intergalactic dust
2399:Gravitational lens
2354:Galactic astronomy
2323:Starburst galaxies
2063:blue compact dwarf
2019:Energetic galaxies
1983:BL Lacertae object
1558:Galactic Astronomy
1440:De Vaucouleurs, G.
1347:Galactic Astronomy
1279:De Vaucouleurs, G.
1039:Galactic Astronomy
721:Prominent K stars
705:Prominent G stars
689:Prominent F stars
673:Prominent A stars
474:
316:
304:
293:
282:
275:
253:reported that the
247:citizen scientists
232:irregular galaxies
228:
169:
92:
39:
2474:
2473:
2434:Galaxy X (galaxy)
2409:Illustris project
2379:Galactic quadrant
2100:Wolf-Rayet galaxy
2090:Green bean galaxy
2085:Hot dust-obscured
2036:Luminous infrared
1800:Elliptical galaxy
1567:978-0-691-02565-0
1360:978-0-691-02565-0
1308:978-3-642-45934-4
1168:uni-heidelberg.de
1048:978-0-691-02565-0
864:
863:
801:
800:
725:
724:
652:. Together with
634:
633:
391:Magellanic Clouds
243:amateur astronomy
162:
16:(Redirected from
2567:
2527:
2526:
2525:
2515:
2514:
2513:
2503:
2502:
2501:
2491:
2490:
2482:
2462:
2450:
2449:
2095:Hanny's Voorwerp
2005:Relativistic jet
1879:Dark matter halo
1686:
1679:
1672:
1663:
1662:
1621:
1620:
1618:
1617:
1605:Darling, David.
1602:
1596:
1595:
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1592:
1578:
1572:
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1520:
1500:
1494:
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1470:
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1467:
1466:
1460:
1450:. Archived from
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1388:
1386:
1385:
1371:
1365:
1364:
1339:
1333:
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1322:
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1312:
1275:
1269:
1268:
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1264:
1259:
1241:
1232:(2): 1808â1820.
1215:
1209:
1208:
1206:
1204:
1190:(11 June 2019).
1184:
1178:
1177:
1175:
1174:
1165:
1156:
1150:
1149:
1147:
1146:
1140:www.jb.man.ac.uk
1132:
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975:
969:
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945:
939:
938:
936:
934:
920:
868:Andromeda Galaxy
803:
802:
727:
726:
659:
658:
477:
473:
178:
176:
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155:
21:
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2509:
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2497:
2485:
2477:
2475:
2470:
2438:
2337:
2252:
2145:
2104:
2014:
1949:
1928:Galaxy filament
1872:Galactic Center
1840:
1695:
1690:
1629:
1624:
1615:
1613:
1603:
1599:
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930:
922:
921:
917:
913:
876:
730:Galactic Shape
646:
458:
454:
450:
446:
432:
404:
383:
328:spiral galaxies
320:Hubble sequence
267:
259:spiral galaxies
216:spiral galaxies
186:Spiral galaxies
154:
147:
143:
129:
126:
125:
80:
78:Hubble sequence
74:
72:Hubble sequence
54:Hubble sequence
36:Hubble sequence
28:
23:
22:
15:
12:
11:
5:
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2249:
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2228:
2226:Stellar stream
2223:
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2206:
2201:
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2110:
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2016:
2015:
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1995:
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1965:
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1951:
1950:
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1945:
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1915:
1913:Galactic ridge
1910:
1908:Galactic plane
1905:
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1903:
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1641:, T.H. Jarrett
1636:
1628:
1627:External links
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86:Spiral galaxy
76:Main article:
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2328:Superclusters
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2231:Superclusters
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2162:Galactic tide
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2121:Ultra diffuse
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1461:on 2018-08-17
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986:
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979:Hubble, E. P.
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949:Hubble, E. P.
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480:Hubble stage
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66:Allan Sandage
63:
59:
56:, devised by
55:
51:
47:
43:
37:
32:
19:
2560:Edwin Hubble
2529:Solar System
2464:
2452:
2187:fossil group
2109:Low activity
1943:Ultramassive
1773:Dwarf galaxy
1756:intermediate
1751:grand design
1700:
1614:. Retrieved
1610:
1600:
1589:. Retrieved
1585:
1576:
1557:
1551:
1508:
1504:
1498:
1487:. Retrieved
1483:
1474:
1463:. Retrieved
1452:the original
1447:
1406:
1402:
1382:. Retrieved
1378:
1369:
1346:
1337:
1282:
1273:
1261:. Retrieved
1229:
1223:
1213:
1201:. Retrieved
1195:
1182:
1171:. Retrieved
1167:
1159:Iafrate, G.
1154:
1143:. Retrieved
1139:
1130:
1118:. Retrieved
1114:
1105:
1094:. Retrieved
1091:cas.sdss.org
1090:
1081:
1070:. Retrieved
1066:
1057:
1038:
1032:
1021:. Retrieved
1017:
983:
973:
956:
952:
943:
931:. Retrieved
927:
918:
904:Fritz Zwicky
865:
809:Explanation
733:Explanation
665:Explanation
647:
638:quantitative
635:
481:
468:
464:
461:
440:
435:
433:
423:
419:
415:
409:
405:
340:
317:
240:
236:
229:
115:
100:Edwin Hubble
98:invented by
93:
58:Edwin Hubble
41:
40:
2517:Outer space
2505:Spaceflight
2246:void galaxy
2209:cannibalism
2194:Interacting
2150:Interaction
2136:Blue Nugget
2126:Dark galaxy
2031:Lyman-break
1923:Protogalaxy
1889:Disc galaxy
1197:EurekAlert!
933:27 February
806:Inclination
757:Elliptical
347:lenticulars
343:ellipticals
46:astronomers
2539:Categories
2286:Polar-ring
2131:Red nugget
2073:faint blue
1933:Spiral arm
1788:spheroidal
1778:elliptical
1761:Magellanic
1746:flocculent
1714:Lenticular
1701:Morphology
1616:2019-02-06
1591:2019-02-06
1489:2019-02-06
1465:2008-01-02
1457:PostScript
1384:2019-02-06
1343:Binney, J.
1239:1904.11436
1173:2019-02-06
1145:2019-02-06
1136:"Galaxies"
1096:2019-02-06
1072:2020-09-19
1023:2019-02-06
911:References
892:Galaxy Zoo
773:Irregular
355:irregulars
251:Galaxy Zoo
48:to divide
2221:Satellite
2216:Jellyfish
2204:collision
2141:Dead disk
2058:Starburst
1973:Markarian
1845:Structure
1812:Irregular
1783:irregular
1543:204925243
1518:0904.2221
1327:ignored (
1317:cite book
1120:20 August
152:−
141:×
88:UGC 12591
2453:Category
2342:See also
2266:Galaxies
1993:X-shaped
1824:Peculiar
1766:unbarred
1724:unbarred
1693:Galaxies
1442:(1994).
997:36018182
981:(1936).
959:: 1â49.
874:See also
300:NGC 7793
289:NGC 6782
249:through
96:galaxies
50:galaxies
2479:Portals
2313:Quasars
2281:Nearest
2276:Largest
2177:cluster
2010:Seyfert
1523:Bibcode
1411:Bibcode
1287:Bibcode
1263:12 June
1244:Bibcode
1203:11 June
961:Bibcode
797:Spiral
627:Sc-Irr
471:= 11).
426:-axis.
351:spirals
2465:Portal
2296:Spiral
2199:merger
1978:Quasar
1963:Blazar
1901:corona
1817:barred
1793:spiral
1741:barred
1736:anemic
1731:Spiral
1719:barred
1654:Go to
1564:
1541:
1409:: 31.
1357:
1305:
1045:
995:
630:Irr I
393:. The
336:lenses
194:spiral
2493:Stars
2333:Voids
2258:Lists
2236:Walls
2172:group
2157:Field
2051:ELIRG
2046:HLIRG
2041:ULIRG
1998:DRAGN
1988:Radio
1968:LINER
1862:Bulge
1834:Polar
1649:SINGS
1539:S2CID
1513:arXiv
1234:arXiv
1164:(PDF)
621:Sb-c
615:Sa-b
609:S0/a
563:S0/a
332:rings
212:bulge
198:bulge
190:stars
2291:Ring
1896:Halo
1884:Disc
1829:Ring
1709:Disc
1562:ISBN
1355:ISBN
1329:help
1303:ISBN
1265:2019
1205:2019
1122:2013
1043:ISBN
993:LCCN
935:2017
587:Sdm
581:Scd
575:Sbc
569:Sab
353:and
334:and
310:The
64:and
2068:pea
1857:Bar
1531:doi
1509:698
1419:doi
1295:doi
1252:doi
1230:487
957:324
624:Sc
618:Sb
612:Sa
606:S0
593:Im
590:Sm
584:Sd
578:Sc
572:Sb
566:Sa
560:S0
557:S0
554:S0
545:cE
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718:k
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686:f
670:a
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436:T
424:z
420:y
416:x
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160:a
157:b
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132:E
116:n
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