384:. 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.
589:
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628:
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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.
284:
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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.
662:
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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.
118:
89:. 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.
332:
479:
434:, 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
163:. 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.
369:
38:
133:
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240:
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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
455:. 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.
103:
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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
395:
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
354:
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.
230:
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
155:
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.
489:
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
498:
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
413:
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
150:
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
203:
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
450:
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
156:
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.
1127:
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".
379:
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
212:
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.
408:
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
430:, 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
136:
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
145:
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
109:
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:
217:
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
780:
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".
627:
323:
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.
1329:
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".
588:
1182:
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
346:. 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
607:
646:
49:. 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
159:
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
676:
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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.
1464:
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".
1570:
Kormendy, John; Ralf Bender (2012). "A Revised
Parallel-sequence Morphological Classification of Galaxies: Structure and Formation of S0 and Spheroidal Galaxies".
175:
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
2627:
1215:
734:
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".
661:
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336:
2324:
652:
17:
1453:
Implications for the origin of early-type dwarf galaxies - the discovery of rotation in isolated, low-mass early-type galaxies
1699:
Dressler, A; Gilmore, Diane M. (1980). "On the interpretation of the morphology-density relation for galaxies in clusters".
2848:
2057:
74:
62:
2740:
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scenario has since been queried due to the existence of extremely isolated, low-luminosity lenticular galaxies such as
866:
2040:
507:
removes gas and prevents the accretion of new gas that might be capable of furthering the development of the disk.
573:
2745:
2472:
77:
schemes. It contains a large-scale disc but does not have large-scale spiral arms. Lenticular galaxies are
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779:
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435:
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2112:
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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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2139:
1399:
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Inclination- and dust-corrected galaxy parameters: bulge-to-disc ratios and size-luminosity relations
347:
2664:
946:
Blanton, Michael; John
Moustakas (2009). "Physical Properties and Environments of Nearby Galaxies".
2725:
2637:
2632:
2538:
2434:
2392:
2102:
2075:
520:
1517:
Moore, Ben; George Lake; Neal Katz (1998). "Morphological
Transformation from Galaxy Harassment".
458:
A 2012 paper that suggests a new classification system, first proposed by the
Canadian astronomer
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714:
111:
1738:(2004). "Can Early-Type Galaxies Evolve from the Fading of the Disks of Late-Type Galaxies?".
2853:
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2349:
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Sandage, A (2005). "THE CLASSIFICATION OF GALAXIES: Early History and Ongoing Developments".
46:
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The morphology and kinematics of lenticular galaxies each, to a degree, suggest a mode of
8:
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82:
50:
31:
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Bedregal, A.G.; A. Aragon-Salamanca; M.R. Merrifield; B. Milvang-Jensen (October 2006).
1151:
977:
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is a lenticular galaxy, lying about 50 million light-years away in the constellation of
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1383:
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
1167:
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1996:
1975:
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1933:
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283:
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86:
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2240:
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1735:
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835:
The Distribution of Intensity in Elliptical Galaxies of the Virgo Cluster. II
717: – Class of galaxy that is cigar shaped and rotates around its long axis
556:
452:
431:
392:
331:
70:
1024:
Supermassive Black Holes and Their Host Spheroids. I. Disassembling Galaxies
519:, lenticular galaxy about 500 million light-years away in the constellation
478:
426:. Their disk-like, possibly dusty, appearance suggests they come from faded
2587:
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is located just under 100 million light-years away in the constellation of
598:
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2065:
1809:
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1478:
1288:
1229:
1142:
754:
78:
1381:
Graham, Alister W.; Dullo, Bililign T.; Savorgnan, Giulia A. D. (2015),
1270:
Bedregal, A. G.; A. Aragon-Salamanca; M. R. Merrifield (December 2006).
342:
In many respects the composition of lenticular galaxies is like that of
2487:
2424:
1625:"TheK-Band Luminosities of Galaxies: Do S0s Come from Spiral Galaxies?"
667:
655:
is a lenticular galaxy classified as type S0 on the Hubble Tuning Fork.
618:
544:, a barred lenticular galaxy about 56 million light years away in Virgo
482:
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is a lenticular galaxy discovered in 1826 by the Scottish astronomer
594:
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682:
633:
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547:
541:
536:
531:
525:
372:
320:
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296:
274:
252:
227:
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profiles of lenticular galaxies are well described by the sum of a
121:
106:
42:
1584:
1413:
1343:
960:
795:
37:
1790:
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The Shape of the Luminosity Profiles of Bulges of Spiral Galaxies
388:
27:
Class of galaxy between an elliptical galaxy and a spiral galaxy
2334:
2319:
2049:
881:
559:
1622:
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is a lenticular galaxy located in the constellation of Virgo.
350:(see below). In addition to these general stellar attributes,
132:
2407:
2402:
2397:
2354:
141:
1851:
Elliptical and Disk Galaxy Structure and Modern Scaling Laws
1791:
Laurikainen, Eija; Heikki Salo; Ronald Buta (October 2005).
368:
261:
2018:
1793:"Multicomponent decompositions for a sample of S0 galaxies"
1397:(2012). "Luminosities of Barred and Unbarred S0 Galaxies".
404:
239:
102:
1122:
1120:
1118:
387:
The kinematics of disk galaxies are usually determined by
363:
1516:
1037:"The nature of 'box' and 'peanut' shaped galactic bulges"
998:
Andredakis, Y. C.; Peletier, R. F.; Balcells, M. (2016),
924:
Multicomponent decompositions for a sample of S0 galaxies
124:
has a large nuclear ring. This galaxy is a member of the
1115:
856:
231:
formation or evolution history of lenticular galaxies.
1733:
1322:
922:
Laurikainen, Eija; Salo, Heikki; Buta, Ronald (2005),
755:
R. J. Buta; H. G. Corwin, Jr.; S. C. Odewahn (2007s).
945:
670:
is a lenticular galaxy also known for its supernovae.
1393:
1569:
1186:
Kinematic Scaling, and the Spin-Ellipticity Diagram
1276:Monthly Notices of the Royal Astronomical Society
1216:Monthly Notices of the Royal Astronomical Society
1041:Monthly Notices of the Royal Astronomical Society
2835:
1623:Burstein, D; Ho LC; Huchra JP; Macri LM (2005).
882:Lambas, D.G.; S.J.Maddox and J. Loveday (1992).
1698:
773:
399:
2675:List of the most distant astronomical objects
2034:
1010:Alister W. Graham and Clare C. Worley(2016),
1263:
1211:"S0 Galaxies in Fornax: data and kinematics"
1022:G. A. D. Savorgnan and G. W. Graham (2016),
493:
305:Barred lenticular galaxies by classification
1666:Annual Review of Astronomy and Astrophysics
1272:"The Tully-Fisher relation for S0 galaxies"
948:Annual Review of Astronomy and Astrophysics
748:
555:is a prototypical lenticular galaxy in the
92:
2041:
2027:
1692:
1563:
941:
939:
937:
935:
933:
931:
728:
30:"S0s" redirects here. For other uses, see
1826:
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1305:
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1202:
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852:
850:
848:
846:
844:
842:
477:
403:
367:
330:
140:
131:
116:
101:
81:that have used up or lost most of their
36:
1663:
928:
364:Measurement difficulties and techniques
190:
85:and therefore have very little ongoing
45:(NGC 5866), a lenticular galaxy in the
14:
2836:
1727:
1686:10.1146/annurev.astro.43.112904.104839
466:(S0a-S0b-S0c-dSph) that parallels the
2022:
1784:
1510:
875:
839:
417:
1934:"Elegance conceals an eventful past"
1616:
1572:The Astrophysical Journal Supplement
1034:
757:The de Vaucouleurs Atlas of Galaxies
311:
978:10.1146/annurev-astro-082708-101734
759:. Cambridge: Cambridge University.
75:galaxy morphological classification
24:
1955:"At the centre of the tuning fork"
25:
2865:
1180:Alister W. Graham et al. (2017),
97:
2815:
2804:
2803:
1828:10.1111/j.1365-2966.2005.09404.x
1307:10.1111/j.1365-2966.2006.11031.x
1248:10.1111/j.1365-2966.2006.10829.x
1196:Sabine Bellstedt et al. (2017),
884:"On the true shapes of galaxies"
857:Binney & Merrifield (1998).
694:
675:
660:
645:
626:
606:
587:
572:
445:
282:
260:
238:
1989:
1968:
1947:
1926:
1905:
1880:
1855:
1843:
1445:
1387:
1375:
1190:
1174:
1090:
1069:
1028:
1016:
1004:
582:contains three compact regions.
2746:Galaxy formation and evolution
2741:Galaxy color–magnitude diagram
1102:ESA/Hubble Picture of the Week
992:
916:
861:. Princeton University Press.
827:
597:image obtained as part of the
13:
1:
1888:"Standing out from the crowd"
741:
358:
2048:
528:, a barred lenticular galaxy
400:Offset Tully–Fisher relation
7:
2628:Galaxies named after people
1997:"The third way of galaxies"
1849:Graham, Alister W. (2013),
708:
510:
503:. Within galaxy clusters,
10:
2870:
2849:Galaxy morphological types
2761:Gravitational microlensing
2716:Galactic coordinate system
1431:10.1088/0004-637X/754/1/68
1035:Shaw, M. A. (1987-12-01).
565:
473:
326:
29:
2799:
2698:
2613:
2506:
2465:
2375:
2310:
2201:
2056:
1740:The Astrophysical Journal
1701:The Astrophysical Journal
1629:The Astrophysical Journal
1602:10.1088/0067-0049/198/1/2
1519:The Astrophysical Journal
1400:The Astrophysical Journal
1331:The Astrophysical Journal
1130:The Astrophysical Journal
1098:"A stranger in the crowd"
783:The Astrophysical Journal
494:Disk growth via accretion
464:dwarf spheroidal galaxies
453:"anemic", spiral galaxies
2726:Galactic magnetic fields
2539:Brightest cluster galaxy
2435:Luminous infrared galaxy
1466:The Astronomical Journal
721:
93:Morphology and structure
65:intermediate between an
18:Barred lenticular galaxy
2721:Galactic habitable zone
2706:Extragalactic astronomy
2295:Supermassive black hole
2209:Active galactic nucleus
1678:2005ARA&A..43..581S
1054:10.1093/mnras/229.4.691
970:2009ARA&A..47..159B
909:10.1093/mnras/258.2.404
207:
2473:Low surface brightness
2224:Central massive object
2001:www.spacetelescope.org
1892:www.spacetelescope.org
1867:www.spacetelescope.org
505:ram-pressure stripping
486:
410:
376:
339:
147:
138:
129:
114:
54:
2751:Galaxy rotation curve
833:Liller, M.H. (1966),
481:
462:, for lenticular and
407:
371:
348:Tully–Fisher relation
334:
144:
135:
120:
105:
40:
2786:Population III stars
2781:Intergalactic travel
2731:Galactic orientation
2598:Voids and supervoids
1976:"A fascinating core"
1451:Janz et al. (2017),
1395:Sidney van den Bergh
460:Sidney van den Bergh
191:Sérsic decomposition
2844:Lenticular galaxies
2776:Intergalactic stars
2665:Large quasar groups
2660:Groups and clusters
2524:Groups and clusters
2383:Lyman-alpha emitter
2275:Interstellar medium
1819:2005MNRAS.362.1319L
1762:2004ApJ...616..192C
1713:1991ApJ...367...64W
1641:2005ApJ...621..246B
1594:2012ApJS..198....2K
1541:1998ApJ...495..139M
1488:2002AJ....124..777E
1423:2012ApJ...754...68V
1353:2007ApJ...671..203C
1298:2006MNRAS.373.1125B
1239:2006MNRAS.371.1912B
1152:2007ApJ...665.1067M
1077:"A galaxy in bloom"
900:1992MNRAS.258..404L
805:2007ApJ...671.1624D
485:is a merged galaxy.
382:velocity dispersion
222:galaxies, like the
83:interstellar matter
51:interstellar matter
47:constellation Draco
2771:Intergalactic dust
2756:Gravitational lens
2711:Galactic astronomy
2680:Starburst galaxies
2420:blue compact dwarf
2376:Energetic galaxies
2340:BL Lacertae object
859:Galactic Astronomy
613:Lenticular galaxy
487:
418:Formation theories
411:
377:
340:
197:surface brightness
148:
139:
130:
115:
69:(denoted E) and a
61:(denoted S0) is a
55:
2831:
2830:
2791:Galaxy X (galaxy)
2766:Illustris project
2736:Galactic quadrant
2457:Wolf-Rayet galaxy
2447:Green bean galaxy
2442:Hot dust-obscured
2393:Luminous infrared
2157:Elliptical galaxy
436:galaxy harassment
352:globular clusters
312:Box-shaped bulges
59:lenticular galaxy
16:(Redirected from
2861:
2819:
2807:
2806:
2452:Hanny's Voorwerp
2362:Relativistic jet
2236:Dark matter halo
2043:
2036:
2029:
2020:
2019:
2013:
2012:
2010:
2008:
1993:
1987:
1986:
1984:
1982:
1972:
1966:
1965:
1963:
1961:
1951:
1945:
1944:
1942:
1940:
1930:
1924:
1923:
1921:
1919:
1909:
1903:
1902:
1900:
1898:
1884:
1878:
1877:
1875:
1873:
1863:"A greedy giant"
1859:
1853:
1847:
1841:
1840:
1830:
1812:
1810:astro-ph/0508097
1803:(4): 1319–1347.
1788:
1782:
1781:
1755:
1753:astro-ph/0408036
1731:
1725:
1724:
1696:
1690:
1689:
1661:
1655:
1654:
1652:
1620:
1614:
1613:
1587:
1567:
1561:
1560:
1534:
1532:astro-ph/9701211
1514:
1508:
1507:
1481:
1479:astro-ph/0205105
1461:
1455:
1449:
1443:
1442:
1416:
1391:
1385:
1379:
1373:
1372:
1346:
1326:
1320:
1319:
1309:
1291:
1289:astro-ph/0609076
1282:(3): 1125–1140.
1267:
1261:
1260:
1250:
1232:
1230:astro-ph/0607434
1223:(4): 1912–1924.
1206:
1200:
1194:
1188:
1178:
1172:
1171:
1145:
1143:astro-ph/0701114
1136:(2): 1067–1073.
1124:
1113:
1112:
1110:
1108:
1094:
1088:
1087:
1085:
1083:
1073:
1067:
1066:
1056:
1032:
1026:
1020:
1014:
1008:
1002:
996:
990:
989:
963:
943:
926:
920:
914:
913:
911:
879:
873:
872:
854:
837:
831:
825:
824:
798:
789:(2): 1624–1639.
777:
771:
770:
752:
735:
732:
702:Cartwheel Galaxy
698:
679:
664:
649:
630:
610:
591:
576:
517:Cartwheel Galaxy
424:galaxy formation
335:Hubble image of
286:
264:
242:
21:
2869:
2868:
2864:
2863:
2862:
2860:
2859:
2858:
2834:
2833:
2832:
2827:
2795:
2694:
2609:
2502:
2461:
2371:
2306:
2285:Galaxy filament
2229:Galactic Center
2197:
2052:
2047:
2017:
2016:
2006:
2004:
1995:
1994:
1990:
1980:
1978:
1974:
1973:
1969:
1959:
1957:
1953:
1952:
1948:
1938:
1936:
1932:
1931:
1927:
1917:
1915:
1911:
1910:
1906:
1896:
1894:
1886:
1885:
1881:
1871:
1869:
1861:
1860:
1856:
1848:
1844:
1789:
1785:
1734:Christlein, D;
1732:
1728:
1697:
1693:
1662:
1658:
1621:
1617:
1568:
1564:
1515:
1511:
1462:
1458:
1450:
1446:
1392:
1388:
1380:
1376:
1327:
1323:
1268:
1264:
1207:
1203:
1195:
1191:
1185:
1179:
1175:
1125:
1116:
1106:
1104:
1096:
1095:
1091:
1081:
1079:
1075:
1074:
1070:
1033:
1029:
1021:
1017:
1009:
1005:
997:
993:
944:
929:
921:
917:
880:
876:
869:
855:
840:
832:
828:
778:
774:
767:
753:
749:
744:
739:
738:
733:
729:
724:
711:
704:
699:
690:
680:
671:
665:
656:
650:
641:
631:
622:
611:
602:
592:
583:
577:
568:
513:
496:
476:
468:Hubble sequence
448:
428:spiral galaxies
420:
402:
366:
361:
329:
314:
309:
308:
307:
306:
302:
301:
300:
293:
287:
279:
278:
271:
265:
257:
256:
249:
243:
221:
216:
210:
193:
186:
182:
178:
174:
170:
166:
161:Hubble sequence
100:
95:
35:
28:
23:
22:
15:
12:
11:
5:
2867:
2857:
2856:
2851:
2846:
2829:
2828:
2826:
2825:
2813:
2800:
2797:
2796:
2794:
2793:
2788:
2783:
2778:
2773:
2768:
2763:
2758:
2753:
2748:
2743:
2738:
2733:
2728:
2723:
2718:
2713:
2708:
2702:
2700:
2696:
2695:
2693:
2692:
2687:
2682:
2677:
2672:
2667:
2662:
2657:
2656:
2655:
2650:
2645:
2640:
2635:
2630:
2619:
2617:
2611:
2610:
2608:
2607:
2606:
2605:
2595:
2590:
2585:
2583:Stellar stream
2580:
2575:
2570:
2569:
2568:
2563:
2558:
2548:
2547:
2546:
2541:
2536:
2531:
2521:
2516:
2510:
2508:
2504:
2503:
2501:
2500:
2495:
2490:
2485:
2480:
2475:
2469:
2467:
2463:
2462:
2460:
2459:
2454:
2449:
2444:
2439:
2438:
2437:
2432:
2427:
2422:
2412:
2411:
2410:
2405:
2400:
2390:
2385:
2379:
2377:
2373:
2372:
2370:
2369:
2364:
2359:
2358:
2357:
2352:
2342:
2337:
2332:
2327:
2322:
2316:
2314:
2308:
2307:
2305:
2304:
2303:
2302:
2292:
2287:
2282:
2277:
2272:
2270:Galactic ridge
2267:
2265:Galactic plane
2262:
2261:
2260:
2250:
2249:
2248:
2238:
2233:
2232:
2231:
2221:
2216:
2211:
2205:
2203:
2199:
2198:
2196:
2195:
2194:
2193:
2183:
2178:
2177:
2176:
2166:
2165:
2164:
2154:
2153:
2152:
2147:
2142:
2137:
2127:
2126:
2125:
2120:
2115:
2110:
2105:
2100:
2095:
2085:
2084:
2083:
2078:
2068:
2062:
2060:
2054:
2053:
2046:
2045:
2038:
2031:
2023:
2015:
2014:
1988:
1967:
1946:
1925:
1904:
1879:
1854:
1842:
1783:
1770:10.1086/424909
1726:
1721:10.1086/169602
1691:
1672:(1): 581–624.
1656:
1650:10.1086/427408
1615:
1562:
1549:10.1086/305264
1525:(1): 139–151.
1509:
1496:10.1086/341613
1472:(2): 777–781.
1456:
1444:
1386:
1374:
1361:10.1086/522193
1337:(1): 203–225.
1321:
1262:
1201:
1189:
1183:
1173:
1160:10.1086/519550
1114:
1089:
1068:
1047:(4): 691–706.
1027:
1015:
1003:
991:
954:(1): 159–210.
927:
915:
894:(2): 404–414.
874:
867:
838:
826:
813:10.1086/523640
772:
766:978-0521820486
765:
746:
745:
743:
740:
737:
736:
726:
725:
723:
720:
719:
718:
715:Spindle galaxy
710:
707:
706:
705:
700:
693:
691:
681:
674:
672:
666:
659:
657:
651:
644:
642:
638:Canes Venatici
632:
625:
623:
612:
605:
603:
593:
586:
584:
578:
571:
567:
564:
563:
562:
550:
545:
539:
534:
529:
523:
512:
509:
495:
492:
475:
472:
447:
444:
419:
416:
401:
398:
365:
362:
360:
357:
328:
325:
313:
310:
304:
303:
291:
288:
281:
280:
269:
266:
259:
258:
247:
244:
237:
236:
235:
234:
233:
219:
214:
209:
206:
192:
189:
184:
180:
176:
172:
168:
164:
126:Fornax Cluster
99:
98:Classification
96:
94:
91:
87:star formation
63:type of galaxy
43:Spindle Galaxy
26:
9:
6:
4:
3:
2:
2866:
2855:
2852:
2850:
2847:
2845:
2842:
2841:
2839:
2824:
2823:
2818:
2814:
2812:
2811:
2802:
2801:
2798:
2792:
2789:
2787:
2784:
2782:
2779:
2777:
2774:
2772:
2769:
2767:
2764:
2762:
2759:
2757:
2754:
2752:
2749:
2747:
2744:
2742:
2739:
2737:
2734:
2732:
2729:
2727:
2724:
2722:
2719:
2717:
2714:
2712:
2709:
2707:
2704:
2703:
2701:
2697:
2691:
2688:
2686:
2685:Superclusters
2683:
2681:
2678:
2676:
2673:
2671:
2668:
2666:
2663:
2661:
2658:
2654:
2651:
2649:
2646:
2644:
2641:
2639:
2636:
2634:
2631:
2629:
2626:
2625:
2624:
2621:
2620:
2618:
2616:
2612:
2604:
2601:
2600:
2599:
2596:
2594:
2591:
2589:
2588:Superclusters
2586:
2584:
2581:
2579:
2576:
2574:
2571:
2567:
2564:
2562:
2559:
2557:
2554:
2553:
2552:
2549:
2545:
2542:
2540:
2537:
2535:
2532:
2530:
2527:
2526:
2525:
2522:
2520:
2519:Galactic tide
2517:
2515:
2512:
2511:
2509:
2505:
2499:
2496:
2494:
2491:
2489:
2486:
2484:
2481:
2479:
2478:Ultra diffuse
2476:
2474:
2471:
2470:
2468:
2464:
2458:
2455:
2453:
2450:
2448:
2445:
2443:
2440:
2436:
2433:
2431:
2428:
2426:
2423:
2421:
2418:
2417:
2416:
2413:
2409:
2406:
2404:
2401:
2399:
2396:
2395:
2394:
2391:
2389:
2386:
2384:
2381:
2380:
2378:
2374:
2368:
2365:
2363:
2360:
2356:
2353:
2351:
2348:
2347:
2346:
2343:
2341:
2338:
2336:
2333:
2331:
2328:
2326:
2323:
2321:
2318:
2317:
2315:
2313:
2312:Active nuclei
2309:
2301:
2298:
2297:
2296:
2293:
2291:
2288:
2286:
2283:
2281:
2278:
2276:
2273:
2271:
2268:
2266:
2263:
2259:
2256:
2255:
2254:
2251:
2247:
2244:
2243:
2242:
2239:
2237:
2234:
2230:
2227:
2226:
2225:
2222:
2220:
2217:
2215:
2212:
2210:
2207:
2206:
2204:
2200:
2192:
2189:
2188:
2187:
2184:
2182:
2179:
2175:
2172:
2171:
2170:
2167:
2163:
2160:
2159:
2158:
2155:
2151:
2148:
2146:
2143:
2141:
2138:
2136:
2133:
2132:
2131:
2128:
2124:
2121:
2119:
2116:
2114:
2111:
2109:
2106:
2104:
2101:
2099:
2096:
2094:
2091:
2090:
2089:
2086:
2082:
2079:
2077:
2074:
2073:
2072:
2069:
2067:
2064:
2063:
2061:
2059:
2055:
2051:
2044:
2039:
2037:
2032:
2030:
2025:
2024:
2021:
2002:
1998:
1992:
1977:
1971:
1956:
1950:
1935:
1929:
1914:
1908:
1893:
1889:
1883:
1868:
1864:
1858:
1852:
1846:
1838:
1834:
1829:
1824:
1820:
1816:
1811:
1806:
1802:
1798:
1794:
1787:
1779:
1775:
1771:
1767:
1763:
1759:
1754:
1749:
1746:(1): 192–98.
1745:
1741:
1737:
1730:
1722:
1718:
1714:
1710:
1706:
1702:
1695:
1687:
1683:
1679:
1675:
1671:
1667:
1660:
1651:
1646:
1642:
1638:
1635:(1): 246–55.
1634:
1630:
1626:
1619:
1611:
1607:
1603:
1599:
1595:
1591:
1586:
1581:
1577:
1573:
1566:
1558:
1554:
1550:
1546:
1542:
1538:
1533:
1528:
1524:
1520:
1513:
1505:
1501:
1497:
1493:
1489:
1485:
1480:
1475:
1471:
1467:
1460:
1454:
1448:
1440:
1436:
1432:
1428:
1424:
1420:
1415:
1410:
1406:
1402:
1401:
1396:
1390:
1384:
1378:
1370:
1366:
1362:
1358:
1354:
1350:
1345:
1340:
1336:
1332:
1325:
1317:
1313:
1308:
1303:
1299:
1295:
1290:
1285:
1281:
1277:
1273:
1266:
1258:
1254:
1249:
1244:
1240:
1236:
1231:
1226:
1222:
1218:
1217:
1212:
1205:
1199:
1193:
1187:
1177:
1169:
1165:
1161:
1157:
1153:
1149:
1144:
1139:
1135:
1131:
1123:
1121:
1119:
1103:
1099:
1093:
1078:
1072:
1064:
1060:
1055:
1050:
1046:
1042:
1038:
1031:
1025:
1019:
1013:
1007:
1001:
995:
987:
983:
979:
975:
971:
967:
962:
957:
953:
949:
942:
940:
938:
936:
934:
932:
925:
919:
910:
905:
901:
897:
893:
889:
885:
878:
870:
868:0-691-02565-7
864:
860:
853:
851:
849:
847:
845:
843:
836:
830:
822:
818:
814:
810:
806:
802:
797:
792:
788:
784:
776:
768:
762:
758:
751:
747:
731:
727:
716:
713:
712:
703:
697:
692:
688:
684:
678:
673:
669:
663:
658:
654:
648:
643:
639:
635:
629:
624:
620:
616:
609:
604:
600:
596:
590:
585:
581:
575:
570:
569:
561:
558:
557:constellation
554:
551:
549:
546:
543:
540:
538:
535:
533:
530:
527:
524:
522:
518:
515:
514:
508:
506:
502:
491:
484:
480:
471:
469:
465:
461:
456:
454:
446:Faded spirals
443:
441:
437:
433:
432:galaxy merger
429:
425:
415:
406:
397:
394:
390:
385:
383:
374:
370:
356:
353:
349:
345:
338:
333:
324:
322:
318:
298:
294:
285:
276:
272:
263:
254:
250:
241:
232:
229:
225:
205:
202:
198:
188:
162:
157:
154:
143:
134:
127:
123:
119:
113:
108:
104:
90:
88:
84:
80:
79:disc galaxies
76:
72:
71:spiral galaxy
68:
64:
60:
52:
48:
44:
39:
33:
19:
2854:Edwin Hubble
2821:
2809:
2544:fossil group
2466:Low activity
2300:Ultramassive
2130:Dwarf galaxy
2113:intermediate
2108:grand design
2070:
2005:. Retrieved
2003:. ESA/Hubble
2000:
1991:
1979:. Retrieved
1970:
1958:. Retrieved
1949:
1937:. Retrieved
1928:
1916:. Retrieved
1907:
1897:12 September
1895:. Retrieved
1891:
1882:
1870:. Retrieved
1866:
1857:
1845:
1800:
1796:
1786:
1743:
1739:
1736:Zabludoff AI
1729:
1704:
1700:
1694:
1669:
1665:
1659:
1632:
1628:
1618:
1575:
1571:
1565:
1522:
1518:
1512:
1469:
1465:
1459:
1447:
1404:
1398:
1389:
1377:
1334:
1330:
1324:
1279:
1275:
1265:
1220:
1214:
1204:
1192:
1176:
1133:
1129:
1105:. Retrieved
1101:
1092:
1080:. Retrieved
1071:
1044:
1040:
1030:
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947:
918:
891:
887:
877:
858:
829:
786:
782:
775:
756:
750:
730:
687:James Dunlop
599:Coma Cluster
501:LEDA 2108986
497:
488:
457:
449:
440:LEDA 2108986
421:
412:
386:
378:
341:
315:
289:
267:
245:
211:
201:Sérsic model
194:
158:
152:
149:
58:
56:
2603:void galaxy
2566:cannibalism
2551:Interacting
2507:Interaction
2493:Blue Nugget
2483:Dark galaxy
2388:Lyman-break
2280:Protogalaxy
2246:Disc galaxy
1913:"Busy bees"
344:ellipticals
2838:Categories
2643:Polar-ring
2488:Red nugget
2430:faint blue
2290:Spiral arm
2145:spheroidal
2135:elliptical
2118:Magellanic
2103:flocculent
2071:Lenticular
2058:Morphology
2007:12 January
1960:2 November
1872:7 December
1707:: 351–65.
742:References
668:Messier 84
619:Ursa Major
483:Messier 85
359:Kinematics
337:ESO 381-12
67:elliptical
2578:Satellite
2573:Jellyfish
2561:collision
2498:Dead disk
2415:Starburst
2330:Markarian
2202:Structure
2169:Irregular
2140:irregular
1610:118326756
1585:1110.4384
1439:118629605
1414:1205.6183
1407:(1): 68.
1344:0708.0422
1063:0035-8711
961:0908.3017
796:0710.0893
595:PGC 83677
409:galaxies.
183:, and SB0
2810:Category
2699:See also
2623:Galaxies
2350:X-shaped
2181:Peculiar
2123:unbarred
2081:unbarred
2050:Galaxies
1939:18 April
1837:15159305
1778:13813083
1578:(1): 2.
1369:15229921
986:16543920
821:14312626
709:See also
683:NGC 6861
634:NGC 4111
615:NGC 5308
580:NGC 1222
553:NGC 1533
548:NGC 5866
542:NGC 4608
537:NGC 3632
532:NGC 3115
526:NGC 2787
521:Sculptor
511:Examples
373:NGC 4866
321:NGC 1175
317:NGC 1375
297:NGC 1460
275:NGC 1533
253:NGC 2787
228:NGC 1460
224:NGC 1460
171:, and S0
122:NGC 1387
107:NGC 2787
2670:Quasars
2638:Nearest
2633:Largest
2534:cluster
2367:Seyfert
1815:Bibcode
1758:Bibcode
1709:Bibcode
1674:Bibcode
1637:Bibcode
1590:Bibcode
1557:1429279
1537:Bibcode
1504:7757634
1484:Bibcode
1419:Bibcode
1349:Bibcode
1316:9274153
1294:Bibcode
1257:6872442
1235:Bibcode
1168:8602518
1148:Bibcode
1107:21 July
1082:13 July
966:Bibcode
896:Bibcode
801:Bibcode
653:Mrk 820
566:Gallery
474:Mergers
327:Content
146:ratios.
2822:Portal
2653:Spiral
2556:merger
2335:Quasar
2320:Blazar
2258:corona
2174:barred
2150:spiral
2098:barred
2093:anemic
2088:Spiral
2076:barred
1981:8 June
1918:16 May
1835:
1776:
1608:
1555:
1502:
1437:
1367:
1314:
1255:
1166:
1061:
984:
865:
819:
763:
601:Survey
560:Dorado
2690:Voids
2615:Lists
2593:Walls
2529:group
2514:Field
2408:ELIRG
2403:HLIRG
2398:ULIRG
2355:DRAGN
2345:Radio
2325:LINER
2219:Bulge
2191:Polar
1833:S2CID
1805:arXiv
1797:MNRAS
1774:S2CID
1748:arXiv
1606:S2CID
1580:arXiv
1553:S2CID
1527:arXiv
1500:S2CID
1474:arXiv
1435:S2CID
1409:arXiv
1365:S2CID
1339:arXiv
1312:S2CID
1284:arXiv
1253:S2CID
1225:arXiv
1164:S2CID
1138:arXiv
982:S2CID
956:arXiv
888:MNRAS
817:S2CID
791:arXiv
722:Notes
393:21-cm
179:, SB0
137:arms.
2648:Ring
2253:Halo
2241:Disc
2186:Ring
2066:Disc
2009:2015
1983:2015
1962:2015
1941:2016
1920:2016
1899:2016
1874:2016
1109:2013
1084:2015
1059:ISSN
863:ISBN
761:ISBN
319:and
208:Bars
195:The
167:, S0
41:The
2425:pea
2214:Bar
1823:doi
1801:362
1766:doi
1744:616
1717:doi
1705:236
1682:doi
1645:doi
1633:621
1598:doi
1576:198
1545:doi
1523:495
1492:doi
1470:124
1427:doi
1405:754
1357:doi
1335:671
1302:doi
1280:373
1243:doi
1221:371
1156:doi
1134:665
1049:doi
1045:229
974:doi
904:doi
892:258
809:doi
787:671
391:or
290:SB0
268:SB0
246:SB0
218:SB0
213:SB0
112:HST
73:in
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