38:
247:
192:, but is much smaller. Giant spiral galaxies are typically 2–100 times the size of those spirals that exist in bulges. Where they exist, these central spirals dominate the light of the bulge in which they reside. Typically the rate at which new stars are formed in pseudobulges is similar to the rate at which stars form in disk galaxies. Sometimes bulges contain nuclear rings that are forming stars at much higher rate (per area) than is typically found in outer disks, as shown in
259:
304:
200:
2147:
2159:
98:
2187:
2211:
162:
2199:
145:). One study has suggested that about 80% of galaxies in the field lack a classical bulge, indicating that they have never experienced a major merger. The bulgeless galaxy fraction of the Universe has remained roughly constant for at least the last 8 billion years. In contrast, about two thirds of galaxies in dense
327:
Until recently it was thought that one could not have a supermassive black hole without a surrounding bulge. Galaxies hosting supermassive black holes without accompanying bulges have now been observed. The implication is that the bulge environment is not strictly essential to the initial seeding and
211:
Properties such as spiral structure and young stars suggest that some bulges did not form through the same process that made elliptical galaxies and classical bulges. Yet the theories for the formation of pseudobulges are less certain than those for classical bulges. Pseudobulges may be the result of
215:
Many astronomers suggest that bulges that appear similar to disks form outside of the disk, and are not the product of a merging process. When left alone, disk galaxies can rearrange their stars and gas (as a response to instabilities). The products of this process (called secular evolution) are
315:. Such black holes by definition cannot be observed directly (light cannot escape them), but various pieces of evidence suggest their existence, both in the bulges of spiral galaxies and in the centers of ellipticals. The masses of the black holes correlate tightly with bulge properties. The
224:
can result from secular evolution of galaxy disks. Secular evolution is also expected to send gas and stars to the center of a galaxy. If this happens that would increase the density at the center of the galaxy, and thus make a bulge that has properties similar to those of disk galaxies.
121:). These stars are also in orbits that are essentially random compared to the plane of the galaxy, giving the bulge a distinct spherical form. Due to the lack of dust and gases, bulges tend to have almost no star formation. The distribution of light is described by a
228:
If secular evolution, or the slow, steady evolution of a galaxy, is responsible for the formation of a significant number of bulges, then that many galaxies have not experienced a merger since the formation of their disk. This would then mean that current theories of
128:
Classical bulges are thought to be the result of collisions of smaller structures. Convulsing gravitational forces and torques disrupt the orbital paths of stars, resulting in the randomised bulge orbits. If either progenitor galaxy was gas-rich, the
212:
extremely gas-rich mergers that happened more recently than those mergers that formed classical bulges (within the last 5 billion years). However, it is difficult for disks to survive the merging process, casting doubt on this scenario.
319:
relates black hole mass to the velocity dispersion of bulge stars, while other correlations involve the total stellar mass or luminosity of the bulge, the central concentration of stars in the bulge, the richness of the
88:
have revealed that many bulges lie at the heart of a spiral galaxy. It is now thought that there are at least two types of bulges: bulges that are like ellipticals and bulges that are like spiral galaxies.
181:
These bulges have stars that are not orbiting randomly, but rather orbit in an ordered fashion in the same plane as the stars in the outer disk. This contrasts greatly with elliptical galaxies.
1313:
1229:
1164:
686:
1010:
Magorrian, J.; Tremaine, S.; Richstone, D.; Bender, R.; Bower, G.; Dressler, A.; Faber, S. M.; Gebhardt, K.; Green, R.; Grillmair, C.; Kormendy, J.; Lauer, T. (1998).
1969:
2016:
291:
satellite later confirmed the X-shape of the bulge. The X-shape makes up 45% of the mass of the bulge in the Milky Way. The boxy/peanut bulges are in fact the
1666:
624:
113:
are often called "classical bulges" due to their similarity to the historic view of bulges. These bulges are composed primarily of stars that are older,
188:) show that the bulges of many galaxies are not devoid of dust, but rather show a varied and complex structure. This structure often looks similar to a
173:
Many bulges have properties more similar to those of the central regions of spiral galaxies than elliptical galaxies. They are often referred to as
1399:
288:
37:
2082:
2001:
605:, H.C. Ferguson, R.F.G. Wyse. Cambridge, U.K.; New York : Cambridge University Press, 1999. (Cambridge contemporary astrophysics)
375: – the amount of stellar mass missing from the center of the galaxy, likely due to the action of a binary supermassive black hole
275:
Edge-on galaxies can sometimes have a boxy/peanut bulge with an X-shape. The boxy nature of the Milky Way bulge was revealed by the
1382:
311:
Most bulges and pseudo-bulges are thought to host a central relativistic compact mass, which is traditionally assumed to be a
2087:
367:
230:
1814:
2177:
1984:
2102:
2057:
1865:
1454:
1449:
1422:
349:
276:
1783:
1309:"Supermassive black holes in disk-dominated galaxies outgrow their bulges and co-evolve with their host galaxies"
957:
479:
287:
stars. The VVV survey also found two overlapping populations of red clump stars and an X-shape of the bulge. The
2067:
1979:
1974:
1880:
1776:
1734:
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1016:
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2047:
1994:
1653:
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1486:
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312:
295:
of a galaxy seen edge-on. Other edge-on galaxies can also show a boxy/peanut bar sometimes with an X-shape.
1285:
Discovery of a
Relationship between Spiral Arm Morphology and Supermassive Black Hole Mass in Disk Galaxies
1565:
1464:
805:"On the nature of bulges in general and of box/peanut bulges in particular: input from N-body simulations"
682:"On the nature of bulges in general and of box/peanut bulges in particular: input from N-body simulations"
185:
85:
2092:
1989:
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1295:
381:
316:
246:
2122:
2072:
1907:
1819:
1555:
1439:
1375:
1332:
1248:
1225:–σ relation between supermassive black holes and the velocity dispersion of globular cluster systems"
1183:
1092:
1035:
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992:
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951:
Xiao, T.; Barth, A. J.; Greene, J. E.; Ho, L. C.; Bentz, M. C.; Ludwig, R. R.; Jiang, Y. (2011).
933:
907:
816:
757:
695:
659:
633:
584:
556:
522:
488:
258:
166:
475:"Bulgeless Giant Galaxies Challenge Our Picture of Galaxy Formation by Hierarchical Clustering"
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1956:
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953:"Exploring the Low-mass End of the M $ _BH$ -$ \sigma$ $ _*$ Relation with Active Galaxies"
925:
834:
775:
713:
677:
651:
647:
574:
514:
506:
321:
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307:
ESO 495-21 may host a supermassive black hole, an unusual feature for a galaxy of its size.
199:
2011:
1934:
1626:
1599:
1570:
1522:
1368:
887:
732:
361:
31:
1127:
Supermassive Black Holes and Their Host
Spheroids. II. The Red and Blue Sequence in the M
324:
system orbiting in the galaxy's far outskirts, and the winding angle of the spiral arms.
1336:
1252:
1187:
1096:
1039:
980:
921:
830:
771:
709:
570:
502:
384: – Relationship between the mass of a galaxy bulge and the mass of the supermassive
358: – Spherical component of a galaxy which extends beyond the main, visible component
352: – Celestial coordinate system in spherical coordinates, with the Sun as its center
1875:
1708:
1611:
1606:
1503:
153:) do possess a classical bulge, demonstrating the disruptive effect of their crowding.
146:
142:
122:
105:, a galaxy with a classical bulge. The spiral structure ends at the onset of the bulge.
65:
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150:
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81:
69:
1284:
1205:
1160:"A new method for estimating dark matter halo masses using globular cluster systems"
1146:
1126:
1055:
588:
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2026:
1929:
1870:
1855:
1761:
1686:
1481:
1471:
937:
372:
663:
619:
1147:
A Correlation between Galaxy Light
Concentration and Supermassive Black Hole Mass
896:"A Fundamental Relation between Supermassive Black Holes and Their Host Galaxies"
68:. The term almost exclusively refers to the central group of stars found in most
17:
2127:
1944:
1834:
1824:
1621:
1587:
1527:
1407:
1308:
1070:
1011:
952:
895:
862:
474:
337:
130:
1829:
1766:
346: – Class of galaxy that has spiral structures extending from their cores.
280:
138:
102:
848:
789:
1839:
1345:
284:
97:
49:
42:
165:
Astronomers refer to the distinctive spiral-like bulge of galaxies such as
404:
233:
greatly over-predict the number of mergers in the past few billion years.
1087:
1030:
912:
821:
700:
638:
265:
204:
193:
133:
can also cause inflows to the newly merged galaxy nucleus. Following a
161:
620:"Secular Evolution and the Formation of Pseudobulges in Disk Galaxies"
518:
1676:
1661:
1391:
451:
2198:
1327:
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1047:
929:
762:
561:
1749:
1744:
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1696:
1243:
1178:
971:
493:
302:
198:
160:
96:
36:
61:
1364:
545:"Survival of Pure Disk Galaxies over the Last 8 Billion Years"
364: – Hot, ionised, gaseous component in the Galactic halo
1360:
137:, gas clouds are more likely to convert into stars, due to
1012:"The Demography of Massive Dark Objects in Galaxy Centers"
27:
Tightly packed group of stars within a larger formation
1307:
Simmons, B. D.; Smethurst, R. J.; Lintott, C. (2017).
746:"The X-shaped Bulge of the Milky Way Revealed by WISE"
2175:
1296:
SPACE.com - Even Thin
Galaxies Pack Hefty Black Holes
386:
Pages displaying wikidata descriptions as a fallback
377:
Pages displaying wikidata descriptions as a fallback
2040:
1955:
1848:
1807:
1717:
1652:
1543:
1398:
84:around them, but high-resolution images using the
1314:Monthly Notices of the Royal Astronomical Society
1230:Monthly Notices of the Royal Astronomical Society
1165:Monthly Notices of the Royal Astronomical Society
809:Monthly Notices of the Royal Astronomical Society
687:Monthly Notices of the Royal Astronomical Society
473:; Drory, N.; Bender, R.; Cornell, M. E. (2010).
109:Bulges that have properties similar to those of
41:Artist's impression of the central bulge of the
538:
536:
465:
463:
461:
459:
2017:List of the most distant astronomical objects
1376:
8:
1071:"On the Black Hole Mass-Bulge Mass Relation"
863:"Hubble Observes Tiny Galaxy with Big Heart"
30:For the center of the Milky Way galaxy, see
625:Annual Review of Astronomy and Astrophysics
601:The formation of galactic bulges edited by
207:, a galaxy with a star-forming nuclear ring
1383:
1369:
1361:
744:Ness, Melissa; Lang, Dustin (2016-07-01).
252:The X-shape of the bulge of the Milky Way.
76:). Bulges were historically thought to be
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1260:
1242:
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1177:
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820:
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435:, Washington: Carnegie Institution, 1961
2182:
405:"The Peanut at the Heart of our Galaxy"
396:
279:satellite and later confirmed with the
1158:Spitler, L. R.; Forbes, D. A. (2009).
1125:Giulia A.D. Savorgnan, et al. (2016),
656:10.1146/annurev.astro.42.053102.134024
264:The prominent X-shape of the bulge of
237:Boxy/peanut bulge for edge-on galaxies
216:often observed in such galaxies; both
169:as disc-type bulges, or pseudobulges.
117:, and hence have a reddish hue (see
7:
25:
1075:The Astrophysical Journal Letters
900:The Astrophysical Journal Letters
549:The Astrophysical Journal Letters
2209:
2197:
2185:
2157:
2146:
2145:
1262:10.1111/j.1745-3933.2012.01321.x
1197:10.1111/j.1745-3933.2008.00567.x
840:10.1111/j.1365-2966.2005.08872.x
719:10.1111/j.1365-2966.2005.08872.x
257:
245:
1069:Häring, N.; Rix, H.-W. (2004).
803:Athanassoula, E. (2005-04-01).
618:; Kennicutt, Jr. R. C. (2004).
543:Sachdeva, S.; Saha, K. (2016).
328:growth of massive black holes.
60:) is a tightly packed group of
2088:Galaxy formation and evolution
2083:Galaxy color–magnitude diagram
1219:Sadoun, R.; Colin, J. (2012).
368:Galaxy formation and evolution
231:galaxy formation and evolution
184:Subsequent studies (using the
1:
733:SAO Encyclopedia of Astronomy
340: – Type of galactic form
452:The Galactic Bulge: A Review
433:The Hubble Atlas of Galaxies
1970:Galaxies named after people
1283:Seigar, M., et al. (2008),
2248:
2103:Gravitational microlensing
2058:Galactic coordinate system
989:10.1088/0004-637X/739/1/28
781:10.3847/0004-6256/152/1/14
580:10.3847/2041-8205/820/1/L4
511:10.1088/0004-637X/723/1/54
350:Galactic coordinate system
29:
2141:
958:The Astrophysical Journal
480:The Astrophysical Journal
2068:Galactic magnetic fields
1881:Brightest cluster galaxy
1777:Luminous infrared galaxy
1017:The Astronomical Journal
750:The Astronomical Journal
80:that happened to have a
2063:Galactic habitable zone
2048:Extragalactic astronomy
1637:Supermassive black hole
1551:Active galactic nucleus
648:2004ARA&A..42..603K
313:supermassive black hole
1815:Low surface brightness
1566:Central massive object
1145:Graham et al. (2001),
867:www.spacetelescope.org
308:
208:
186:Hubble Space Telescope
170:
106:
86:Hubble Space Telescope
45:
2093:Galaxy rotation curve
1346:10.1093/mnras/stx1340
306:
202:
164:
100:
40:
2128:Population III stars
2123:Intergalactic travel
2073:Galactic orientation
1940:Voids and supervoids
299:Central compact mass
2118:Intergalactic stars
2007:Large quasar groups
2002:Groups and clusters
1866:Groups and clusters
1725:Lyman-alpha emitter
1617:Interstellar medium
1337:2017MNRAS.470.1559S
1253:2012MNRAS.426L..51S
1188:2009MNRAS.392L...1S
1097:2004ApJ...604L..89H
1040:1998AJ....115.2285M
981:2011ApJ...739...28X
922:2000ApJ...539L...9F
831:2005MNRAS.358.1477A
772:2016AJ....152...14N
710:2005MNRAS.358.1477A
571:2016ApJ...820L...4S
503:2010ApJ...723...54K
115:Population II stars
111:elliptical galaxies
78:elliptical galaxies
2113:Intergalactic dust
2098:Gravitational lens
2053:Galactic astronomy
2022:Starburst galaxies
1762:blue compact dwarf
1718:Energetic galaxies
1682:BL Lacertae object
309:
268:as seen by Hubble.
209:
203:Central region of
171:
107:
46:
2173:
2172:
2133:Galaxy X (galaxy)
2108:Illustris project
2078:Galactic quadrant
1799:Wolf-Rayet galaxy
1789:Green bean galaxy
1784:Hot dust-obscured
1735:Luminous infrared
1499:Elliptical galaxy
409:ESO Press Release
283:with the help of
119:stellar evolution
74:galactic spheroid
18:Bulge (astronomy)
16:(Redirected from
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1794:Hanny's Voorwerp
1704:Relativistic jet
1578:Dark matter halo
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1321:(2): 1559–1569.
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1088:astro-ph/0402376
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1031:astro-ph/9708072
1024:(6): 2285–2305.
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815:(4): 1477–1488.
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701:astro-ph/0502316
694:(4): 1477–1488.
678:Athanassoula, E.
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382:M–sigma relation
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322:globular cluster
317:M–sigma relation
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157:Disk-like bulges
93:Classical bulges
64:within a larger
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1571:Galactic Center
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1357:External links
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1276:
1237:(1): L51–L55.
1222:
1211:
1150:
1138:
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1118:
1105:10.1086/383567
1081:(2): L89–L92.
1061:
1048:10.1086/300353
1002:
943:
930:10.1086/312838
879:
854:
795:
736:
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669:
632:(1): 603–683.
607:
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429:Sandage, Allan
421:
395:
393:
390:
389:
388:
379:
370:
365:
359:
353:
347:
341:
333:
330:
300:
297:
263:
256:
255:
251:
244:
243:
242:
241:
240:
238:
235:
158:
155:
143:star formation
123:Sersic profile
94:
91:
66:star formation
54:galactic bulge
26:
24:
14:
13:
10:
9:
6:
4:
3:
2:
2244:
2233:
2230:
2229:
2227:
2217:
2207:
2205:
2200:
2195:
2193:
2183:
2179:
2166:
2165:
2160:
2156:
2154:
2153:
2144:
2143:
2140:
2134:
2131:
2129:
2126:
2124:
2121:
2119:
2116:
2114:
2111:
2109:
2106:
2104:
2101:
2099:
2096:
2094:
2091:
2089:
2086:
2084:
2081:
2079:
2076:
2074:
2071:
2069:
2066:
2064:
2061:
2059:
2056:
2054:
2051:
2049:
2046:
2045:
2043:
2039:
2033:
2030:
2028:
2027:Superclusters
2025:
2023:
2020:
2018:
2015:
2013:
2010:
2008:
2005:
2003:
2000:
1996:
1993:
1991:
1988:
1986:
1983:
1981:
1978:
1976:
1973:
1971:
1968:
1967:
1966:
1963:
1962:
1960:
1958:
1954:
1946:
1943:
1942:
1941:
1938:
1936:
1933:
1931:
1930:Superclusters
1928:
1926:
1923:
1921:
1918:
1916:
1913:
1909:
1906:
1904:
1901:
1899:
1896:
1895:
1894:
1891:
1887:
1884:
1882:
1879:
1877:
1874:
1872:
1869:
1868:
1867:
1864:
1862:
1861:Galactic tide
1859:
1857:
1854:
1853:
1851:
1847:
1841:
1838:
1836:
1833:
1831:
1828:
1826:
1823:
1821:
1820:Ultra diffuse
1818:
1816:
1813:
1812:
1810:
1806:
1800:
1797:
1795:
1792:
1790:
1787:
1785:
1782:
1778:
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1768:
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1728:
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1702:
1698:
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1689:
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1680:
1678:
1675:
1673:
1670:
1668:
1665:
1663:
1660:
1659:
1657:
1655:
1654:Active nuclei
1651:
1643:
1640:
1639:
1638:
1635:
1633:
1630:
1628:
1625:
1623:
1620:
1618:
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1601:
1598:
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1478:
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1433:
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1428:
1424:
1421:
1419:
1416:
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1414:
1411:
1409:
1406:
1405:
1403:
1401:
1397:
1393:
1386:
1381:
1379:
1374:
1372:
1367:
1366:
1363:
1356:
1347:
1342:
1338:
1334:
1329:
1324:
1320:
1316:
1315:
1310:
1303:
1300:
1297:
1292:
1289:
1286:
1280:
1277:
1272:
1268:
1263:
1258:
1254:
1250:
1245:
1240:
1236:
1232:
1231:
1226:
1215:
1212:
1207:
1203:
1198:
1193:
1189:
1185:
1180:
1175:
1171:
1167:
1166:
1161:
1154:
1151:
1148:
1142:
1139:
1136:
1122:
1119:
1114:
1110:
1106:
1102:
1098:
1094:
1089:
1084:
1080:
1076:
1072:
1065:
1062:
1057:
1053:
1049:
1045:
1041:
1037:
1032:
1027:
1023:
1019:
1018:
1013:
1006:
1003:
998:
994:
990:
986:
982:
978:
973:
968:
964:
960:
959:
954:
947:
944:
939:
935:
931:
927:
923:
919:
914:
909:
906:(1): L9–L12.
905:
901:
897:
893:
889:
888:Ferrarese, L.
883:
880:
868:
864:
858:
855:
850:
846:
841:
836:
832:
828:
823:
818:
814:
810:
806:
799:
796:
791:
787:
782:
777:
773:
769:
764:
759:
755:
751:
747:
740:
737:
734:
729:
726:
720:
715:
711:
707:
702:
697:
693:
689:
688:
683:
679:
673:
670:
665:
661:
657:
653:
649:
645:
640:
635:
631:
627:
626:
621:
617:
611:
608:
604:
598:
595:
590:
586:
581:
576:
572:
568:
563:
558:
554:
550:
546:
539:
537:
533:
528:
524:
520:
516:
512:
508:
504:
500:
495:
490:
486:
482:
481:
476:
472:
466:
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462:
460:
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453:
448:
446:
444:
442:
438:
434:
430:
425:
422:
410:
406:
400:
397:
391:
383:
380:
374:
371:
369:
366:
363:
360:
357:
356:Galactic halo
354:
351:
348:
345:
344:Spiral galaxy
342:
339:
336:
335:
331:
329:
325:
323:
318:
314:
305:
298:
296:
294:
290:
286:
282:
278:
267:
260:
248:
236:
234:
232:
226:
223:
222:galactic bars
219:
213:
206:
201:
197:
196:(see photo).
195:
191:
190:spiral galaxy
187:
182:
180:
179:disky-bulges.
176:
168:
163:
156:
154:
152:
151:Virgo Cluster
149:(such as the
148:
144:
140:
136:
132:
126:
124:
120:
116:
112:
104:
99:
92:
90:
87:
83:
82:disk of stars
79:
75:
71:
67:
63:
59:
55:
51:
44:
39:
33:
19:
2163:
2151:
1886:fossil group
1808:Low activity
1642:Ultramassive
1560:
1472:Dwarf galaxy
1455:intermediate
1450:grand design
1318:
1312:
1302:
1291:
1279:
1234:
1228:
1214:
1172:(1): L1–L5.
1169:
1163:
1153:
1141:
1121:
1078:
1074:
1064:
1021:
1015:
1005:
962:
956:
946:
903:
899:
882:
870:. Retrieved
866:
857:
812:
808:
798:
753:
749:
739:
728:
691:
685:
672:
629:
623:
616:Kormendy, J.
610:
603:C.M. Carollo
597:
552:
548:
487:(1): 54–80.
484:
478:
471:Kormendy, J.
432:
424:
414:14 September
412:. Retrieved
408:
399:
373:Mass deficit
326:
310:
274:
227:
218:spiral disks
214:
210:
183:
178:
175:pseudobulges
174:
172:
135:major merger
131:tidal forces
127:
108:
101:An image of
57:
53:
47:
2216:Outer space
1945:void galaxy
1908:cannibalism
1893:Interacting
1849:Interaction
1835:Blue Nugget
1825:Dark galaxy
1730:Lyman-break
1622:Protogalaxy
1588:Disc galaxy
892:Merritt, D.
338:Disc galaxy
56:(or simply
1985:Polar-ring
1830:Red nugget
1772:faint blue
1632:Spiral arm
1487:spheroidal
1477:elliptical
1460:Magellanic
1445:flocculent
1413:Lenticular
1400:Morphology
1328:1705.10793
763:1603.00026
562:1602.08942
519:2152/35173
392:References
281:VVV survey
167:ESO 498-G5
103:Messier 81
2192:Astronomy
1920:Satellite
1915:Jellyfish
1903:collision
1840:Dead disk
1757:Starburst
1672:Markarian
1544:Structure
1511:Irregular
1482:irregular
1271:117185846
1244:1204.0144
1179:0809.5057
1113:119431361
997:118444825
972:1106.6232
965:(1): 28.
849:0035-8711
790:0004-6256
756:(1): 14.
555:(1): L4.
527:119303368
494:1009.3015
285:red clump
50:astronomy
43:Milky Way
2232:Galaxies
2226:Category
2152:Category
2041:See also
1965:Galaxies
1692:X-shaped
1523:Peculiar
1465:unbarred
1423:unbarred
1392:Galaxies
1206:16818778
1056:17256372
894:(2000).
680:(2005).
589:14644377
332:See also
266:NGC 1175
205:NGC 4314
194:NGC 4314
2178:Portals
2012:Quasars
1980:Nearest
1975:Largest
1876:cluster
1709:Seyfert
1333:Bibcode
1249:Bibcode
1184:Bibcode
1135:Diagram
1093:Bibcode
1036:Bibcode
977:Bibcode
938:6508110
918:Bibcode
872:17 June
827:Bibcode
768:Bibcode
706:Bibcode
644:Bibcode
567:Bibcode
499:Bibcode
2164:Portal
1995:Spiral
1898:merger
1677:Quasar
1662:Blazar
1600:corona
1516:barred
1492:spiral
1440:barred
1435:anemic
1430:Spiral
1418:barred
1269:
1204:
1111:
1054:
995:
936:
847:
788:
664:515479
662:
587:
525:
139:shocks
2204:Stars
2032:Voids
1957:Lists
1935:Walls
1871:group
1856:Field
1750:ELIRG
1745:HLIRG
1740:ULIRG
1697:DRAGN
1687:Radio
1667:LINER
1561:Bulge
1533:Polar
1323:arXiv
1267:S2CID
1239:arXiv
1202:S2CID
1174:arXiv
1133:*,sph
1109:S2CID
1083:arXiv
1052:S2CID
1026:arXiv
993:S2CID
967:arXiv
934:S2CID
908:arXiv
817:arXiv
758:arXiv
696:arXiv
660:S2CID
634:arXiv
585:S2CID
557:arXiv
523:S2CID
489:arXiv
141:(see
72:(see
62:stars
58:bulge
1990:Ring
1595:Halo
1583:Disc
1528:Ring
1408:Disc
874:2019
845:ISSN
786:ISSN
416:2013
289:WISE
277:COBE
220:and
52:, a
1767:pea
1556:Bar
1341:doi
1319:470
1257:doi
1235:426
1192:doi
1170:392
1101:doi
1079:604
1044:doi
1022:115
985:doi
963:739
926:doi
904:539
835:doi
813:358
776:doi
754:152
714:doi
692:358
652:doi
575:doi
553:820
515:hdl
507:doi
485:723
293:bar
177:or
48:In
2228::
1504:cD
1339:.
1331:.
1317:.
1311:.
1265:.
1255:.
1247:.
1233:.
1227:.
1223:BH
1221:"M
1200:.
1190:.
1182:.
1168:.
1162:.
1131:-M
1129:BH
1107:.
1099:.
1091:.
1077:.
1073:.
1050:.
1042:.
1034:.
1020:.
1014:.
991:.
983:.
975:.
961:.
955:.
932:.
924:.
916:.
902:.
898:.
890:;
865:.
843:.
833:.
825:.
811:.
807:.
784:.
774:.
766:.
752:.
748:.
712:.
704:.
690:.
684:.
658:.
650:.
642:.
630:42
628:.
622:.
583:.
573:.
565:.
551:.
547:.
535:^
521:.
513:.
505:.
497:.
483:.
477:.
458:^
440:^
431:,
407:.
125:.
2180::
1384:e
1377:t
1370:v
1349:.
1343::
1335::
1325::
1273:.
1259::
1251::
1241::
1208:.
1194::
1186::
1176::
1115:.
1103::
1095::
1085::
1058:.
1046::
1038::
1028::
999:.
987::
979::
969::
940:.
928::
920::
910::
876:.
851:.
837::
829::
819::
792:.
778::
770::
760::
722:.
716::
708::
698::
666:.
654::
646::
636::
591:.
577::
569::
559::
529:.
517::
509::
501::
491::
418:.
34:.
20:)
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