373:. This situation is analogous to a balloon, where the motions of the air particles (stars in a bulge's case) are dominated by random motions. However, the kinematics of lenticular galaxies are dominated by the rotationally supported disk. Rotation support implies the average circular motion of stars in the disk is responsible for the stability of the galaxy. Thus, kinematics are often used to distinguish lenticular galaxies from elliptical galaxies. Determining the distinction between elliptical galaxies and lenticular galaxies often relies on the measurements of velocity dispersion (σ), rotational velocity (v), and ellipticity (ε). In order to differentiate between lenticulars and ellipticals, one typically looks at the v/σ ratio for a fixed ε. For example, a rough criterion for distinguishing between lenticular and elliptical galaxies is that elliptical galaxies have v/σ < 0.5 for ε = 0.3. The motivation behind this criterion is that lenticular galaxies do have prominent bulge and disk components whereas elliptical galaxies have no disk structure. Thus, lenticulars have much larger v/σ ratios than ellipticals due to their non-negligible rotational velocities (due to the disk component) in addition to not having as prominent of a bulge component compared to elliptical galaxies. However, this approach using a single ratio for each galaxy is problematic due to the dependence of the v/σ ratio on the radius out to which it is measured in some early-type galaxies. For example, the ES galaxies that bridge the E and S0 galaxies, with their intermediate-scale disks, have a high v/σ ratio at intermediate radii that then drops to a low ratio at large radii.
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consistent with the general structure of spiral galaxies. However, the bulge component of lenticulars is more closely related to elliptical galaxies in terms of morphological classification. This spheroidal region, which dominates the inner structure of lenticular galaxies, has a steeper surface brightness profile (Sérsic index typically ranging from n = 1 to 4) than the disk component. Lenticular galaxy samples are distinguishable from the diskless (excluding small nuclear disks) elliptical galaxy population through analysis of their surface brightness profiles.
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spiral. If S0s were formed by mergers of other spirals these observations would be fitting and it would also account for the increased frequency of globular clusters. It should be mentioned, however, that advanced models of the central bulge which include both a general Sersic profile and bar indicate a smaller bulge, and thus a lessened inconsistency. Mergers are also unable to account for the offset from the Tully–Fisher relation without assuming that the merged galaxies were quite different from those we see today.
403:
offset in the luminosity / absolute magnitude axis. This would result from brighter, redder stars dominating the stellar populations of lenticulars. An example of this effect can be seen in the adjacent plot. One can clearly see that the best-fit lines for the spiral galaxy data and the lenticular galaxy have the same slope (and thus follow the same Tully–Fisher relation), but are offset by ΔI ≈ 1.5. This implies that lenticular galaxies were once spiral galaxies but are now dominated by old, red stars.
78:. They may, however, retain significant dust in their disks. As a result, they consist mainly of aging stars (like elliptical galaxies). Despite the morphological differences, lenticular and elliptical galaxies share common properties like spectral features and scaling relations. Both can be considered early-type galaxies that are passively evolving, at least in the local part of the Universe. Connecting the E galaxies with the S0 galaxies are the ES galaxies with intermediate-scale discs.
423:, which increase the total stellar mass and might give the newly merged galaxy a disk-like, arm-less appearance. Alternatively, it has been proposed that they grew their disks via (gas and minor merger) accretion events. It had previously been suggested that the evolution of luminous lenticular galaxies may be closely linked to that of elliptical galaxies, whereas fainter lenticulars might be more closely associated with ram-pressure stripped spiral galaxies, although this latter
273:
152:. This results from lenticulars having both prominent disk and bulge components. The disk component is usually featureless, which precludes a classification system similar to spiral galaxies. As the bulge component is usually spherical, elliptical galaxy classifications are also unsuitable. Lenticular galaxies are thus divided into subclasses based upon either the amount of dust present or the prominence of a central bar. The classes of lenticular galaxies with no bar are S0
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considerable amount of difficulty in deriving accurate rotational velocities for lenticular galaxies. This is a combined effect from lenticulars having difficult inclination measurements, projection effects in the bulge-disk interface region, and the random motions of stars affecting the true rotational velocities. These effects make kinematic measurements of lenticular galaxies considerably more difficult compared to normal disk galaxies.
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dominance can be seen in the axis ratio (i.e. the ratio between the observed minor and major axial of a disk galaxy) distribution of a lenticular galaxy sample. The distribution for lenticular galaxies rises steadily in the range 0.25 to 0.85 whereas the distribution for spirals is essentially flat in that same range. Larger axial ratios can be explained by observing face-on disk galaxies
444:. If the spiral pattern then dissipated the resulting galaxy would be similar to many lenticulars. Moore et al. also document that tidal harassment – the gravitational effects from other, near-by galaxies – could aid this process in dense regions. The clearest support for this theory, however, is their adherence to slightly shifted version of Tully–Fisher relation, discussed above.
27:
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seen in nearby massive lenticular galaxies. In a "downsizing" scenario, bigger lenticular galaxies may have been built first – in a younger universe when more gas was available – and the lower-mass galaxies may have been slower to attract their disk-building material, as in the case of the isolated early-type galaxy
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emission lines, which are typically not present in lenticular galaxies due to their general lack of cool gas. Thus kinematic information and rough mass estimates for lenticular galaxies often comes from stellar absorption lines, which are less reliable than emission line measurements. There is also a
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are found more frequently in lenticular galaxies than in spiral galaxies of similar mass and luminosity. They also have little to no molecular gas (hence the lack of star formation) and no significant hydrogen α or 21-cm emission. Finally, unlike ellipticals, they may still possess significant dust.
219:
is actually the galaxy with one of the largest bars seen among lenticular galaxies. Unfortunately, the properties of bars in lenticular galaxies have not been researched in great detail. Understanding these properties, as well as understanding the formation mechanism for bars, would help clarify the
144:
by having a sample of spheroidal (bulge-dominated) galaxies. Imagine looking at two disk galaxies edge-on, one with a bulge and one without a bulge. The galaxy with a prominent bulge will have a larger edge-on axial ratio compared to the galaxy without a bulge based on the definition of axial ratio.
478:
The analyses of
Burstein and Sandage showed that lenticular galaxies typically have surface brightness much greater than other spiral classes. It is also thought that lenticular galaxies exhibit a larger bulge-to-disk ratio than spiral galaxies and this may be inconsistent with simple fading from a
487:
The creation of disks in, at least some, lenticular galaxies via the accretion of gas, and small galaxies, around a pre-existing spheroidal structure was first suggested as an explanation to match the high-redshift compact massive spheroidal-shaped galaxies with the equally compact massive bulges
402:
The kinematic connection between spiral and lenticular galaxies is most clear when analyzing the Tully–Fisher relation for spiral and lenticular samples. If lenticular galaxies are an evolved stage of spiral galaxies then they should have a similar Tully–Fisher relation with spirals, but with an
139:
Lenticular galaxies are unique in that they have a visible disk component as well as a prominent bulge component. They have much higher bulge-to-disk ratios than typical spirals and do not have the canonical spiral arm structure of late-type galaxies, yet may exhibit a central bar. This bulge
192:
for the spheroidal component plus an exponentially declining model (Sérsic index of n ≈ 1) for the disk, and often a third component for the bar. Sometimes there is an observed truncation in the surface brightness profiles of lenticular galaxies at ~ 4 disk scalelengths. These features are
439:
The absence of gas, presence of dust, lack of recent star formation, and rotational support are all attributes one might expect of a spiral galaxy which had used up all of its gas in the formation of stars. This possibility is further enhanced by the existence of gas poor, or
145:
Thus a sample of disk galaxies with prominent spheroidal components will have more galaxies at larger axial ratios. The fact that the lenticular galaxy distribution rises with increasing observed axial ratio implies that lenticulars are dominated by a central bulge component.
1116:
Moran, Sean M.; Boon Liang Loh; Richard S. Ellis; Tommaso Treu; Kevin Bundy; Lauren MacArthur (20 August 2007). "The
Dynamical Distinction Between Elliptical and Lenticular Galaxies in Distant Clusters: Further Evidence for the Recent Origin of S0 Galaxies".
368:
Lenticular galaxies share kinematic properties with both spiral and elliptical galaxies. This is due to the significant bulge and disk nature of lenticulars. The bulge component is similar to elliptical galaxies in that it is pressure supported by a central
201:
Like spiral galaxies, lenticular galaxies can possess a central bar structure. While the classification system for normal lenticulars depends on dust content, barred lenticular galaxies are classified by the prominence of the central bar.
397:
This plot illustrates the Tully–Fisher relation for a spiral galaxy sample (black) as well as a lenticular galaxy sample (blue). One can see how the best-fit line for spiral galaxies differs from the best-fit line for lenticular
419:, whose arm features disappeared. However, some lenticular galaxies are more luminous than spiral galaxies, which suggests that they are not merely the faded remnants of spiral galaxies. Lenticular galaxies might result from a
125:
Grid showing the location of early-type galaxies (including the lenticular S0 galaxies) relative to the late-type spiral galaxies. The horizontal axis shows the morphological type, primarily dictated by the nature of the spiral
134:
The percentage of galaxies with a particular axis ratio (minor/major) for a sample of lenticular and spiral galaxies. The inset is a visual representation of the profile of either at the specified minor (b) to major (a) axis
616:
98:
is an example of a lenticular galaxy with visible dust absorption. While this galaxy has been classified as an S0 galaxy, one can see the difficulty in differentiating among spirals, ellipticals, and lenticulars. Credit:
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galaxies have the least defined bar structure and are only classified as having slightly enhanced surface brightness along opposite sides of the central bulge. The prominence of the bar increases with index number, thus
769:
DeGraaff, Regina Barber; Blakeslee, John P.; Meurer, Gerhardt R.; Putman, Mary E. (December 2007). "A Galaxy in
Transition: Structure, Globular Clusters, and Distance of the Star-Forming S0 Galaxy NGC 1533 in Dorado".
635:
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are examples of lenticular galaxies that have so-called box-shaped bulges. They are classified as SB0 pec. Box-shaped bulges are seen in edge-on galaxies, mostly spiral, but rarely lenticular.
1318:
Courteau, Stephane; Aaron A. Dutton; Frank C. van den Bosch; Lauren A. MacArthur; Avishai Dekel; Daniel H. McIntosh; Daniel A. Dale (10 December 2007). "Scaling
Relations of Spiral Galaxies".
596:
665:
1171:
Implications for the Origin of Early-type Dwarf
Galaxies: A Detailed Look at the Isolated Rotating Early-type Dwarf Galaxy LEDA 2108986 (CG 611), Ramifications for the Fundamental Plane's S
335:. For example, they both consist of predominately older, hence redder, stars. All of their stars are thought to be older than about a billion years, in agreement with their offset from the
38:. This image shows that lenticular galaxies may retain a considerable amount of dust in their disk. However, there is little to no gas, and thus they are considered deficient in
148:
Lenticular galaxies are often considered to be a poorly understood transition state between spiral and elliptical galaxies, which results in their intermediate placement on the
459:
for spirals and irregulars (Sa-Sb-Sc-Im) reinforces this idea showing how the spiral–irregular sequence is very similar to this new one for lenticulars and dwarf ellipticals.
1204:
1453:
Elmegreen, Debra; Bruce G. Elmegreen; Jay A. Frogel; Paul B. Eskridge; Richard W. Pogge; Andrew
Gallagher; Joel Iams (2002). "Arm Structure in Anemic Spiral Galaxies".
2616:
1559:
Kormendy, John; Ralf Bender (2012). "A Revised
Parallel-sequence Morphological Classification of Galaxies: Structure and Formation of S0 and Spheroidal Galaxies".
164:
where the subscripted numbers indicate the amount of dust absorption in the disk component; the corresponding classes for lenticulars with a central bar are SB0
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2313:
650:
723:
Galaxies to the left side of the Hubble classification scheme are sometimes referred to as "early-type", while those to the right are "late-type".
2837:
2046:
63:
51:
2729:
2648:
753:
855:
2029:
1442:
Implications for the origin of early-type dwarf galaxies - the discovery of rotation in isolated, low-mass early-type galaxies
2734:
562:
1688:
Dressler, A; Gilmore, Diane M. (1980). "On the interpretation of the morphology-density relation for galaxies in clusters".
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scenario has since been queried due to the existence of extremely isolated, low-luminosity lenticular galaxies such as
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2704:
2512:
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removes gas and prevents the accretion of new gas that might be capable of furthering the development of the disk.
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schemes. It contains a large-scale disc but does not have large-scale spiral arms. Lenticular galaxies are
2212:
2111:
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100:
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2338:
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35:
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have very well defined bars that can extend through the transition region between the bulge and disk.
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Inclination- and dust-corrected galaxy parameters: bulge-to-disc ratios and size-luminosity relations
954:
884:
789:
448:
935:
Blanton, Michael; John
Moustakas (2009). "Physical Properties and Environments of Nearby Galaxies".
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2138:
370:
332:
272:
71:
39:
20:
2805:
1506:
Moore, Ben; George Lake; Neal Katz (1998). "Morphological
Transformation from Galaxy Harassment".
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A 2012 paper that suggests a new classification system, first proposed by the
Canadian astronomer
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1727:(2004). "Can Early-Type Galaxies Evolve from the Fading of the Disks of Late-Type Galaxies?".
1047:
851:
749:
340:
55:
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Sandage, A (2005). "THE CLASSIFICATION OF GALAXIES: Early History and Ongoing Developments".
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2015:
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The morphology and kinematics of lenticular galaxies each, to a degree, suggest a mode of
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1411:
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1227:
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Bedregal, A.G.; A. Aragon-Salamanca; M.R. Merrifield; B. Milvang-Jensen (October 2006).
1140:
966:
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is a lenticular galaxy, lying about 50 million light-years away in the constellation of
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Hiding in Plain Sight: An Abundance of Compact Massive Spheroids in the Local Universe
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The SLUGGS Survey: trails of SLUGGS galaxies in a modified spin-ellipticity diagram
1156:
675:
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1985:
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824:
The Distribution of Intensity in Elliptical Galaxies of the Virgo Cluster. II
706: – Class of galaxy that is cigar shaped and rotates around its long axis
2486:
1013:
Supermassive Black Holes and Their Host Spheroids. I. Disassembling Galaxies
583:
508:, lenticular galaxy about 500 million light-years away in the constellation
415:. Their disk-like, possibly dusty, appearance suggests they come from faded
606:
is located just under 100 million light-years away in the constellation of
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1131:
671:
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568:
541:
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520:
514:
361:
309:
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285:
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110:
95:
31:
1370:
Graham, Alister W.; Dullo, Bililign T.; Savorgnan, Giulia A. D. (2015),
1259:
Bedregal, A. G.; A. Aragon-Salamanca; M. R. Merrifield (December 2006).
331:
In many respects the composition of lenticular galaxies is like that of
121:
1614:"TheK-Band Luminosities of Galaxies: Do S0s Come from Spiral Galaxies?"
644:
is a lenticular galaxy classified as type S0 on the Hubble Tuning Fork.
533:, a barred lenticular galaxy about 56 million light years away in Virgo
377:
130:
357:
250:
2323:
2308:
2038:
674:
is a lenticular galaxy discovered in 1826 by the Scottish astronomer
548:
393:
228:
91:
1758:
1709:
1638:
1613:
1537:
1484:
1349:
1148:
801:
188:
profiles of lenticular galaxies are well described by the sum of a
2396:
2391:
2386:
2343:
1573:
1402:
1332:
949:
784:
466:
356:
319:
105:
90:
25:
989:
The Shape of the Luminosity Profiles of Bulges of Spiral Galaxies
16:
Class of galaxy between an elliptical galaxy and a spiral galaxy
2011:
364:
is a lenticular galaxy located in the constellation of Virgo.
339:(see below). In addition to these general stellar attributes,
1840:
Elliptical and Disk Galaxy Structure and Modern Scaling Laws
1780:
Laurikainen, Eija; Heikki Salo; Ronald Buta (October 2005).
2007:
1782:"Multicomponent decompositions for a sample of S0 galaxies"
1386:(2012). "Luminosities of Barred and Unbarred S0 Galaxies".
1111:
1109:
1107:
376:
The kinematics of disk galaxies are usually determined by
1026:"The nature of 'box' and 'peanut' shaped galactic bulges"
987:
Andredakis, Y. C.; Peletier, R. F.; Balcells, M. (2016),
913:
Multicomponent decompositions for a sample of S0 galaxies
113:
has a large nuclear ring. This galaxy is a member of the
220:
formation or evolution history of lenticular galaxies.
911:
Laurikainen, Eija; Salo, Heikki; Buta, Ronald (2005),
744:
R. J. Buta; H. G. Corwin, Jr.; S. C. Odewahn (2007s).
659:
is a lenticular galaxy also known for its supernovae.
2687:
2602:
2495:
2454:
2364:
2299:
2190:
2045:
1175:
Kinematic Scaling, and the Spin-Ellipticity Diagram
1265:Monthly Notices of the Royal Astronomical Society
1205:Monthly Notices of the Royal Astronomical Society
1030:Monthly Notices of the Royal Astronomical Society
1612:Burstein, D; Ho LC; Huchra JP; Macri LM (2005).
871:Lambas, D.G.; S.J.Maddox and J. Loveday (1992).
2664:List of the most distant astronomical objects
2023:
999:Alister W. Graham and Clare C. Worley(2016),
8:
1200:"S0 Galaxies in Fornax: data and kinematics"
1011:G. A. D. Savorgnan and G. W. Graham (2016),
294:Barred lenticular galaxies by classification
1655:Annual Review of Astronomy and Astrophysics
1261:"The Tully-Fisher relation for S0 galaxies"
937:Annual Review of Astronomy and Astrophysics
544:is a prototypical lenticular galaxy in the
2030:
2016:
2008:
930:
928:
926:
924:
922:
920:
19:"S0s" redirects here. For other uses, see
1815:
1797:
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1637:
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1401:
1331:
1294:
1276:
1235:
1217:
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1041:
948:
896:
783:
841:
839:
837:
835:
833:
831:
392:
129:
120:
70:that have used up or lost most of their
736:
716:
558:
353:Measurement difficulties and techniques
74:and therefore have very little ongoing
34:(NGC 5866), a lenticular galaxy in the
1675:10.1146/annurev.astro.43.112904.104839
455:(S0a-S0b-S0c-dSph) that parallels the
7:
1923:"Elegance conceals an eventful past"
1561:The Astrophysical Journal Supplement
746:The de Vaucouleurs Atlas of Galaxies
967:10.1146/annurev-astro-082708-101734
748:. Cambridge: Cambridge University.
64:galaxy morphological classification
1944:"At the centre of the tuning fork"
14:
1169:Alister W. Graham et al. (2017),
2804:
2793:
2792:
1817:10.1111/j.1365-2966.2005.09404.x
1296:10.1111/j.1365-2966.2006.11031.x
1237:10.1111/j.1365-2966.2006.10829.x
1185:Sabine Bellstedt et al. (2017),
873:"On the true shapes of galaxies"
846:Binney & Merrifield (1998).
683:
664:
649:
634:
615:
595:
576:
561:
271:
249:
227:
571:contains three compact regions.
2735:Galaxy formation and evolution
2730:Galaxy color–magnitude diagram
1091:ESA/Hubble Picture of the Week
850:. Princeton University Press.
586:image obtained as part of the
1:
1877:"Standing out from the crowd"
517:, a barred lenticular galaxy
389:Offset Tully–Fisher relation
2617:Galaxies named after people
1986:"The third way of galaxies"
1838:Graham, Alister W. (2013),
492:. Within galaxy clusters,
2861:
2838:Galaxy morphological types
2750:Gravitational microlensing
2705:Galactic coordinate system
1420:10.1088/0004-637X/754/1/68
1024:Shaw, M. A. (1987-12-01).
18:
2788:
1729:The Astrophysical Journal
1690:The Astrophysical Journal
1618:The Astrophysical Journal
1591:10.1088/0067-0049/198/1/2
1508:The Astrophysical Journal
1389:The Astrophysical Journal
1320:The Astrophysical Journal
1119:The Astrophysical Journal
1087:"A stranger in the crowd"
772:The Astrophysical Journal
483:Disk growth via accretion
453:dwarf spheroidal galaxies
442:"anemic", spiral galaxies
2715:Galactic magnetic fields
2528:Brightest cluster galaxy
2424:Luminous infrared galaxy
1455:The Astronomical Journal
82:Morphology and structure
54:intermediate between an
2710:Galactic habitable zone
2695:Extragalactic astronomy
2284:Supermassive black hole
2198:Active galactic nucleus
1667:2005ARA&A..43..581S
1043:10.1093/mnras/229.4.691
959:2009ARA&A..47..159B
898:10.1093/mnras/258.2.404
2462:Low surface brightness
2213:Central massive object
1990:www.spacetelescope.org
1881:www.spacetelescope.org
1856:www.spacetelescope.org
494:ram-pressure stripping
475:
399:
365:
328:
136:
127:
118:
103:
43:
2740:Galaxy rotation curve
822:Liller, M.H. (1966),
470:
451:, for lenticular and
396:
360:
337:Tully–Fisher relation
323:
133:
124:
109:
94:
29:
2775:Population III stars
2770:Intergalactic travel
2720:Galactic orientation
2587:Voids and supervoids
1965:"A fascinating core"
1440:Janz et al. (2017),
1384:Sidney van den Bergh
449:Sidney van den Bergh
180:Sérsic decomposition
2833:Lenticular galaxies
2765:Intergalactic stars
2654:Large quasar groups
2649:Groups and clusters
2513:Groups and clusters
2372:Lyman-alpha emitter
2264:Interstellar medium
1808:2005MNRAS.362.1319L
1751:2004ApJ...616..192C
1702:1991ApJ...367...64W
1630:2005ApJ...621..246B
1583:2012ApJS..198....2K
1530:1998ApJ...495..139M
1477:2002AJ....124..777E
1412:2012ApJ...754...68V
1342:2007ApJ...671..203C
1287:2006MNRAS.373.1125B
1228:2006MNRAS.371.1912B
1141:2007ApJ...665.1067M
1066:"A galaxy in bloom"
889:1992MNRAS.258..404L
794:2007ApJ...671.1624D
474:is a merged galaxy.
371:velocity dispersion
211:galaxies, like the
72:interstellar matter
40:interstellar matter
36:constellation Draco
2760:Intergalactic dust
2745:Gravitational lens
2700:Galactic astronomy
2669:Starburst galaxies
2409:blue compact dwarf
2365:Energetic galaxies
2329:BL Lacertae object
848:Galactic Astronomy
602:Lenticular galaxy
476:
407:Formation theories
400:
366:
329:
186:surface brightness
137:
128:
119:
104:
58:(denoted E) and a
50:(denoted S0) is a
44:
2820:
2819:
2780:Galaxy X (galaxy)
2755:Illustris project
2725:Galactic quadrant
2446:Wolf-Rayet galaxy
2436:Green bean galaxy
2431:Hot dust-obscured
2382:Luminous infrared
2146:Elliptical galaxy
425:galaxy harassment
341:globular clusters
301:Box-shaped bulges
48:lenticular galaxy
2850:
2808:
2796:
2795:
2441:Hanny's Voorwerp
2351:Relativistic jet
2225:Dark matter halo
2032:
2025:
2018:
2009:
2002:
2001:
1999:
1997:
1982:
1976:
1975:
1973:
1971:
1961:
1955:
1954:
1952:
1950:
1940:
1934:
1933:
1931:
1929:
1919:
1913:
1912:
1910:
1908:
1898:
1892:
1891:
1889:
1887:
1873:
1867:
1866:
1864:
1862:
1852:"A greedy giant"
1848:
1842:
1836:
1830:
1829:
1819:
1801:
1799:astro-ph/0508097
1792:(4): 1319–1347.
1777:
1771:
1770:
1744:
1742:astro-ph/0408036
1720:
1714:
1713:
1685:
1679:
1678:
1650:
1644:
1643:
1641:
1609:
1603:
1602:
1576:
1556:
1550:
1549:
1523:
1521:astro-ph/9701211
1503:
1497:
1496:
1470:
1468:astro-ph/0205105
1450:
1444:
1438:
1432:
1431:
1405:
1380:
1374:
1368:
1362:
1361:
1335:
1315:
1309:
1308:
1298:
1280:
1278:astro-ph/0609076
1271:(3): 1125–1140.
1256:
1250:
1249:
1239:
1221:
1219:astro-ph/0607434
1212:(4): 1912–1924.
1195:
1189:
1183:
1177:
1167:
1161:
1160:
1134:
1132:astro-ph/0701114
1125:(2): 1067–1073.
1113:
1102:
1101:
1099:
1097:
1083:
1077:
1076:
1074:
1072:
1062:
1056:
1055:
1045:
1021:
1015:
1009:
1003:
997:
991:
985:
979:
978:
952:
932:
915:
909:
903:
902:
900:
868:
862:
861:
843:
826:
820:
814:
813:
787:
778:(2): 1624–1639.
766:
760:
759:
741:
724:
721:
691:Cartwheel Galaxy
687:
668:
653:
638:
619:
599:
580:
565:
506:Cartwheel Galaxy
413:galaxy formation
324:Hubble image of
275:
253:
231:
2860:
2859:
2853:
2852:
2851:
2849:
2848:
2847:
2823:
2822:
2821:
2816:
2784:
2683:
2598:
2491:
2450:
2360:
2295:
2274:Galaxy filament
2218:Galactic Center
2186:
2041:
2036:
2006:
2005:
1995:
1993:
1984:
1983:
1979:
1969:
1967:
1963:
1962:
1958:
1948:
1946:
1942:
1941:
1937:
1927:
1925:
1921:
1920:
1916:
1906:
1904:
1900:
1899:
1895:
1885:
1883:
1875:
1874:
1870:
1860:
1858:
1850:
1849:
1845:
1837:
1833:
1779:
1778:
1774:
1723:Christlein, D;
1722:
1721:
1717:
1687:
1686:
1682:
1652:
1651:
1647:
1611:
1610:
1606:
1558:
1557:
1553:
1505:
1504:
1500:
1452:
1451:
1447:
1439:
1435:
1382:
1381:
1377:
1369:
1365:
1317:
1316:
1312:
1258:
1257:
1253:
1197:
1196:
1192:
1184:
1180:
1174:
1168:
1164:
1115:
1114:
1105:
1095:
1093:
1085:
1084:
1080:
1070:
1068:
1064:
1063:
1059:
1023:
1022:
1018:
1010:
1006:
998:
994:
986:
982:
934:
933:
918:
910:
906:
870:
869:
865:
858:
845:
844:
829:
821:
817:
768:
767:
763:
756:
743:
742:
738:
733:
728:
727:
722:
718:
713:
700:
693:
688:
679:
669:
660:
654:
645:
639:
630:
620:
611:
600:
591:
581:
572:
566:
557:
502:
485:
465:
457:Hubble sequence
437:
417:spiral galaxies
409:
391:
355:
350:
318:
303:
298:
297:
296:
295:
291:
290:
289:
282:
276:
268:
267:
260:
254:
246:
245:
238:
232:
210:
205:
199:
182:
175:
171:
167:
163:
159:
155:
150:Hubble sequence
89:
84:
24:
17:
12:
11:
5:
2858:
2857:
2854:
2846:
2845:
2840:
2835:
2825:
2824:
2818:
2817:
2815:
2814:
2802:
2789:
2786:
2785:
2783:
2782:
2777:
2772:
2767:
2762:
2757:
2752:
2747:
2742:
2737:
2732:
2727:
2722:
2717:
2712:
2707:
2702:
2697:
2691:
2689:
2685:
2684:
2682:
2681:
2676:
2671:
2666:
2661:
2656:
2651:
2646:
2645:
2644:
2639:
2634:
2629:
2624:
2619:
2608:
2606:
2600:
2599:
2597:
2596:
2595:
2594:
2584:
2579:
2574:
2572:Stellar stream
2569:
2564:
2559:
2558:
2557:
2552:
2547:
2537:
2536:
2535:
2530:
2525:
2520:
2510:
2505:
2499:
2497:
2493:
2492:
2490:
2489:
2484:
2479:
2474:
2469:
2464:
2458:
2456:
2452:
2451:
2449:
2448:
2443:
2438:
2433:
2428:
2427:
2426:
2421:
2416:
2411:
2401:
2400:
2399:
2394:
2389:
2379:
2374:
2368:
2366:
2362:
2361:
2359:
2358:
2353:
2348:
2347:
2346:
2341:
2331:
2326:
2321:
2316:
2311:
2305:
2303:
2297:
2296:
2294:
2293:
2292:
2291:
2281:
2276:
2271:
2266:
2261:
2259:Galactic ridge
2256:
2254:Galactic plane
2251:
2250:
2249:
2239:
2238:
2237:
2227:
2222:
2221:
2220:
2210:
2205:
2200:
2194:
2192:
2188:
2187:
2185:
2184:
2183:
2182:
2172:
2167:
2166:
2165:
2155:
2154:
2153:
2143:
2142:
2141:
2136:
2131:
2126:
2116:
2115:
2114:
2109:
2104:
2099:
2094:
2089:
2084:
2074:
2073:
2072:
2067:
2057:
2051:
2049:
2043:
2042:
2037:
2035:
2034:
2027:
2020:
2012:
2004:
2003:
1977:
1956:
1935:
1914:
1893:
1868:
1843:
1831:
1772:
1759:10.1086/424909
1715:
1710:10.1086/169602
1680:
1661:(1): 581–624.
1645:
1639:10.1086/427408
1604:
1551:
1538:10.1086/305264
1514:(1): 139–151.
1498:
1485:10.1086/341613
1461:(2): 777–781.
1445:
1433:
1375:
1363:
1350:10.1086/522193
1326:(1): 203–225.
1310:
1251:
1190:
1178:
1172:
1162:
1149:10.1086/519550
1103:
1078:
1057:
1036:(4): 691–706.
1016:
1004:
992:
980:
943:(1): 159–210.
916:
904:
883:(2): 404–414.
863:
856:
827:
815:
802:10.1086/523640
761:
755:978-0521820486
754:
735:
734:
732:
729:
726:
725:
715:
714:
712:
709:
708:
707:
704:Spindle galaxy
699:
696:
695:
694:
689:
682:
680:
670:
663:
661:
655:
648:
646:
640:
633:
631:
627:Canes Venatici
621:
614:
612:
601:
594:
592:
582:
575:
573:
567:
560:
556:
553:
552:
551:
539:
534:
528:
523:
518:
512:
501:
498:
484:
481:
464:
461:
436:
433:
408:
405:
390:
387:
354:
351:
349:
346:
317:
314:
302:
299:
293:
292:
280:
277:
270:
269:
258:
255:
248:
247:
236:
233:
226:
225:
224:
223:
222:
208:
203:
198:
195:
181:
178:
173:
169:
165:
161:
157:
153:
115:Fornax Cluster
88:
87:Classification
85:
83:
80:
76:star formation
52:type of galaxy
32:Spindle Galaxy
15:
13:
10:
9:
6:
4:
3:
2:
2856:
2855:
2844:
2841:
2839:
2836:
2834:
2831:
2830:
2828:
2813:
2812:
2807:
2803:
2801:
2800:
2791:
2790:
2787:
2781:
2778:
2776:
2773:
2771:
2768:
2766:
2763:
2761:
2758:
2756:
2753:
2751:
2748:
2746:
2743:
2741:
2738:
2736:
2733:
2731:
2728:
2726:
2723:
2721:
2718:
2716:
2713:
2711:
2708:
2706:
2703:
2701:
2698:
2696:
2693:
2692:
2690:
2686:
2680:
2677:
2675:
2674:Superclusters
2672:
2670:
2667:
2665:
2662:
2660:
2657:
2655:
2652:
2650:
2647:
2643:
2640:
2638:
2635:
2633:
2630:
2628:
2625:
2623:
2620:
2618:
2615:
2614:
2613:
2610:
2609:
2607:
2605:
2601:
2593:
2590:
2589:
2588:
2585:
2583:
2580:
2578:
2577:Superclusters
2575:
2573:
2570:
2568:
2565:
2563:
2560:
2556:
2553:
2551:
2548:
2546:
2543:
2542:
2541:
2538:
2534:
2531:
2529:
2526:
2524:
2521:
2519:
2516:
2515:
2514:
2511:
2509:
2508:Galactic tide
2506:
2504:
2501:
2500:
2498:
2494:
2488:
2485:
2483:
2480:
2478:
2475:
2473:
2470:
2468:
2467:Ultra diffuse
2465:
2463:
2460:
2459:
2457:
2453:
2447:
2444:
2442:
2439:
2437:
2434:
2432:
2429:
2425:
2422:
2420:
2417:
2415:
2412:
2410:
2407:
2406:
2405:
2402:
2398:
2395:
2393:
2390:
2388:
2385:
2384:
2383:
2380:
2378:
2375:
2373:
2370:
2369:
2367:
2363:
2357:
2354:
2352:
2349:
2345:
2342:
2340:
2337:
2336:
2335:
2332:
2330:
2327:
2325:
2322:
2320:
2317:
2315:
2312:
2310:
2307:
2306:
2304:
2302:
2301:Active nuclei
2298:
2290:
2287:
2286:
2285:
2282:
2280:
2277:
2275:
2272:
2270:
2267:
2265:
2262:
2260:
2257:
2255:
2252:
2248:
2245:
2244:
2243:
2240:
2236:
2233:
2232:
2231:
2228:
2226:
2223:
2219:
2216:
2215:
2214:
2211:
2209:
2206:
2204:
2201:
2199:
2196:
2195:
2193:
2189:
2181:
2178:
2177:
2176:
2173:
2171:
2168:
2164:
2161:
2160:
2159:
2156:
2152:
2149:
2148:
2147:
2144:
2140:
2137:
2135:
2132:
2130:
2127:
2125:
2122:
2121:
2120:
2117:
2113:
2110:
2108:
2105:
2103:
2100:
2098:
2095:
2093:
2090:
2088:
2085:
2083:
2080:
2079:
2078:
2075:
2071:
2068:
2066:
2063:
2062:
2061:
2058:
2056:
2053:
2052:
2050:
2048:
2044:
2040:
2033:
2028:
2026:
2021:
2019:
2014:
2013:
2010:
1991:
1987:
1981:
1978:
1966:
1960:
1957:
1945:
1939:
1936:
1924:
1918:
1915:
1903:
1897:
1894:
1882:
1878:
1872:
1869:
1857:
1853:
1847:
1844:
1841:
1835:
1832:
1827:
1823:
1818:
1813:
1809:
1805:
1800:
1795:
1791:
1787:
1783:
1776:
1773:
1768:
1764:
1760:
1756:
1752:
1748:
1743:
1738:
1735:(1): 192–98.
1734:
1730:
1726:
1719:
1716:
1711:
1707:
1703:
1699:
1695:
1691:
1684:
1681:
1676:
1672:
1668:
1664:
1660:
1656:
1649:
1646:
1640:
1635:
1631:
1627:
1624:(1): 246–55.
1623:
1619:
1615:
1608:
1605:
1600:
1596:
1592:
1588:
1584:
1580:
1575:
1570:
1566:
1562:
1555:
1552:
1547:
1543:
1539:
1535:
1531:
1527:
1522:
1517:
1513:
1509:
1502:
1499:
1494:
1490:
1486:
1482:
1478:
1474:
1469:
1464:
1460:
1456:
1449:
1446:
1443:
1437:
1434:
1429:
1425:
1421:
1417:
1413:
1409:
1404:
1399:
1395:
1391:
1390:
1385:
1379:
1376:
1373:
1367:
1364:
1359:
1355:
1351:
1347:
1343:
1339:
1334:
1329:
1325:
1321:
1314:
1311:
1306:
1302:
1297:
1292:
1288:
1284:
1279:
1274:
1270:
1266:
1262:
1255:
1252:
1247:
1243:
1238:
1233:
1229:
1225:
1220:
1215:
1211:
1207:
1206:
1201:
1194:
1191:
1188:
1182:
1179:
1176:
1166:
1163:
1158:
1154:
1150:
1146:
1142:
1138:
1133:
1128:
1124:
1120:
1112:
1110:
1108:
1104:
1092:
1088:
1082:
1079:
1067:
1061:
1058:
1053:
1049:
1044:
1039:
1035:
1031:
1027:
1020:
1017:
1014:
1008:
1005:
1002:
996:
993:
990:
984:
981:
976:
972:
968:
964:
960:
956:
951:
946:
942:
938:
931:
929:
927:
925:
923:
921:
917:
914:
908:
905:
899:
894:
890:
886:
882:
878:
874:
867:
864:
859:
857:0-691-02565-7
853:
849:
842:
840:
838:
836:
834:
832:
828:
825:
819:
816:
811:
807:
803:
799:
795:
791:
786:
781:
777:
773:
765:
762:
757:
751:
747:
740:
737:
730:
720:
717:
710:
705:
702:
701:
697:
692:
686:
681:
677:
673:
667:
662:
658:
652:
647:
643:
637:
632:
628:
624:
618:
613:
609:
605:
598:
593:
589:
585:
579:
574:
570:
564:
559:
554:
550:
547:
546:constellation
543:
540:
538:
535:
532:
529:
527:
524:
522:
519:
516:
513:
511:
507:
504:
503:
499:
497:
495:
491:
482:
480:
473:
469:
462:
460:
458:
454:
450:
445:
443:
435:Faded spirals
434:
432:
430:
426:
422:
421:galaxy merger
418:
414:
406:
404:
395:
388:
386:
383:
379:
374:
372:
363:
359:
352:
347:
345:
342:
338:
334:
327:
322:
315:
313:
311:
307:
300:
287:
283:
274:
265:
261:
252:
243:
239:
230:
221:
218:
214:
196:
194:
191:
187:
179:
177:
151:
146:
143:
132:
123:
116:
112:
108:
102:
97:
93:
86:
81:
79:
77:
73:
69:
68:disc galaxies
65:
61:
60:spiral galaxy
57:
53:
49:
41:
37:
33:
28:
22:
2843:Edwin Hubble
2810:
2798:
2533:fossil group
2455:Low activity
2289:Ultramassive
2119:Dwarf galaxy
2102:intermediate
2097:grand design
2059:
1994:. Retrieved
1992:. ESA/Hubble
1989:
1980:
1968:. Retrieved
1959:
1947:. Retrieved
1938:
1926:. Retrieved
1917:
1905:. Retrieved
1896:
1886:12 September
1884:. Retrieved
1880:
1871:
1859:. Retrieved
1855:
1846:
1834:
1789:
1785:
1775:
1732:
1728:
1725:Zabludoff AI
1718:
1693:
1689:
1683:
1658:
1654:
1648:
1621:
1617:
1607:
1564:
1560:
1554:
1511:
1507:
1501:
1458:
1454:
1448:
1436:
1393:
1387:
1378:
1366:
1323:
1319:
1313:
1268:
1264:
1254:
1209:
1203:
1193:
1181:
1165:
1122:
1118:
1094:. Retrieved
1090:
1081:
1069:. Retrieved
1060:
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588:Coma Cluster
490:LEDA 2108986
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190:Sérsic model
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2592:void galaxy
2555:cannibalism
2540:Interacting
2496:Interaction
2482:Blue Nugget
2472:Dark galaxy
2377:Lyman-break
2269:Protogalaxy
2235:Disc galaxy
1902:"Busy bees"
333:ellipticals
2827:Categories
2632:Polar-ring
2477:Red nugget
2419:faint blue
2279:Spiral arm
2134:spheroidal
2124:elliptical
2107:Magellanic
2092:flocculent
2060:Lenticular
2047:Morphology
1996:12 January
1949:2 November
1861:7 December
1696:: 351–65.
731:References
657:Messier 84
608:Ursa Major
472:Messier 85
348:Kinematics
326:ESO 381-12
56:elliptical
2567:Satellite
2562:Jellyfish
2550:collision
2487:Dead disk
2404:Starburst
2319:Markarian
2191:Structure
2158:Irregular
2129:irregular
1599:118326756
1574:1110.4384
1428:118629605
1403:1205.6183
1396:(1): 68.
1333:0708.0422
1052:0035-8711
950:0908.3017
785:0710.0893
584:PGC 83677
398:galaxies.
172:, and SB0
2799:Category
2688:See also
2612:Galaxies
2339:X-shaped
2170:Peculiar
2112:unbarred
2070:unbarred
2039:Galaxies
1928:18 April
1826:15159305
1767:13813083
1567:(1): 2.
1358:15229921
975:16543920
810:14312626
698:See also
672:NGC 6861
623:NGC 4111
604:NGC 5308
569:NGC 1222
542:NGC 1533
537:NGC 5866
531:NGC 4608
526:NGC 3632
521:NGC 3115
515:NGC 2787
510:Sculptor
500:Examples
362:NGC 4866
310:NGC 1175
306:NGC 1375
286:NGC 1460
264:NGC 1533
242:NGC 2787
217:NGC 1460
213:NGC 1460
160:, and S0
111:NGC 1387
96:NGC 2787
2659:Quasars
2627:Nearest
2622:Largest
2523:cluster
2356:Seyfert
1804:Bibcode
1747:Bibcode
1698:Bibcode
1663:Bibcode
1626:Bibcode
1579:Bibcode
1546:1429279
1526:Bibcode
1493:7757634
1473:Bibcode
1408:Bibcode
1338:Bibcode
1305:9274153
1283:Bibcode
1246:6872442
1224:Bibcode
1157:8602518
1137:Bibcode
1096:21 July
1071:13 July
955:Bibcode
885:Bibcode
790:Bibcode
642:Mrk 820
555:Gallery
463:Mergers
316:Content
135:ratios.
2811:Portal
2642:Spiral
2545:merger
2324:Quasar
2309:Blazar
2247:corona
2163:barred
2139:spiral
2087:barred
2082:anemic
2077:Spiral
2065:barred
1970:8 June
1907:16 May
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590:Survey
549:Dorado
2679:Voids
2604:Lists
2582:Walls
2518:group
2503:Field
2397:ELIRG
2392:HLIRG
2387:ULIRG
2344:DRAGN
2334:Radio
2314:LINER
2208:Bulge
2180:Polar
1822:S2CID
1794:arXiv
1786:MNRAS
1763:S2CID
1737:arXiv
1595:S2CID
1569:arXiv
1542:S2CID
1516:arXiv
1489:S2CID
1463:arXiv
1424:S2CID
1398:arXiv
1354:S2CID
1328:arXiv
1301:S2CID
1273:arXiv
1242:S2CID
1214:arXiv
1153:S2CID
1127:arXiv
971:S2CID
945:arXiv
877:MNRAS
806:S2CID
780:arXiv
711:Notes
382:21-cm
168:, SB0
126:arms.
2637:Ring
2242:Halo
2230:Disc
2175:Ring
2055:Disc
1998:2015
1972:2015
1951:2015
1930:2016
1909:2016
1888:2016
1863:2016
1098:2013
1073:2015
1048:ISSN
852:ISBN
750:ISBN
308:and
197:Bars
184:The
156:, S0
30:The
2414:pea
2203:Bar
1812:doi
1790:362
1755:doi
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