1834:
45:
1846:
1886:
36:
1910:
1898:
1874:
213:
Further evidence of the prevalence of dark matter in dSphs includes the case of Fornax dwarf spheroidal galaxy, which can be assumed to be in dynamic equilibrium to estimate mass and amount of dark matter, since the gravitational effects of the Milky Way are small. Unlike the Fornax galaxy, there is
182:
may not be clearly separate and distinct types of objects. Other recent studies, however, have found a distinction in that the total amount of mass inferred from the motions of stars in dwarf spheroidals is many times that which can be accounted for by the mass of the stars themselves. Studies reveal
221:
A topic of research is how much the internal dynamics of dwarf spheroidal galaxies are affected by the gravitational tidal dynamics of the galaxy they are orbiting. In other words, dwarf spheroidal galaxies could be prevented from achieving equilibrium due to the gravitational field of the Milky Way
169:
For example, 98% of the stars in the Carina dwarf spheroidal galaxy are older than 2 Gyr, formed over the course of three bursts around 3, 7 and 13 Gyr ago. The stars in Carina have also been found to be metal-poor. This is unlike star clusters because, while star clusters have stars which formed
126:, they are much more difficult to find due to their low luminosities and surface brightnesses. Dwarf spheroidal galaxies have a large range of luminosities, and known dwarf spheroidal galaxies span several orders of magnitude of luminosity. Their luminosities are so low that
193:
Although at fainter luminosities of dwarf spheroidal galaxies, it is not universally agreed upon how to differentiate between a dwarf spheroidal galaxy and a star cluster; however, many astronomers decide this depending on the object's dynamics: If it seems to have more
138:, the known dwarf spheroidal galaxies with the lowest luminosities, have mass-to-light ratios (M/L) greater than that of the Milky Way. Dwarf spheroidals also have little to no gas with no obvious signs of recent star formation. Within the
656:
Koposov, Sergey E.; Belokurov, Vasily; Torrealba, Gabriel; Evans, N. Wyn (10 March 2015). "Beasts of the southern wild: Discovery of a large number of ultra-faint satellites in the vicinity of the
Magellanic clouds".
157:
has resulted in the discovery of 11 more dSph galaxies as of 2007 By 2015, many more ultra-faint dSphs were discovered, all satellites of the Milky Way. Nine potentially new dSphs were discovered in the
210:, which show little to no signs of dark matter. Because of the extremely large amounts of dark matter in dwarf spheroidal galaxies, they may deserve the title "most dark matter-dominated galaxies."
178:
Because of the faintness of the lowest-luminosity dwarf spheroidal galaxies and the nature of the stars contained within them, some astronomers suggest that dwarf spheroidal galaxies and
585:
1656:
234:
reveal that its orbital path does not correspond to the mass contained in
Hercules. Furthermore, there is evidence that the UMa2, a dwarf spheroidal galaxy in the
1703:
1353:
226:
has a velocity dispersion of 7.9±1.3 km/s, which is a velocity dispersion that could not be explained solely by its stellar mass according to the
206:
cosmological model, the presence of dark matter is often cited as a reason to classify dwarf spheroidal galaxies as a different class of object from
897:; Willman, Beth; et al. (2008). "The most dark matter dominated galaxies: Predicted gamma-ray signals from the faintest Milky Way dwarfs".
357:
1950:
1086:
163:
1769:
1935:
1930:
1688:
1069:
1774:
1501:
1940:
1671:
1864:
1789:
1744:
1552:
1141:
1136:
1109:
349:
603:(November 2007). "The kinematics of the ultra-faint Milky Way satellites: Solving the missing satellite problem".
1470:
261:; Willman, Beth; Walker, Matthew G. (2008-08-28). "A common mass scale for satellite galaxies of the Milky Way".
1754:
1666:
1661:
1567:
1463:
1421:
1131:
1104:
223:
166:, all of which consist of stars generally much older than 1–2 Gyr that formed over the span of many gigayears.
154:
766:
Bono, G.; Stetson, P.B.; Walker, A.R.; Monelli, M.; Fabrizio, M.; Pietrinferni, A.; et al. (2010-01-01).
426:
McConnachie, Alan W. (2012-06-05). "The
Observed Properties of Dwarf Galaxies in and Around the Local Group".
1945:
1749:
1734:
1681:
1340:
1328:
1323:
1237:
1202:
1163:
231:
99:
1252:
1151:
159:
131:
1779:
1676:
1378:
715:
Bonnivard, V.; Combet, C.; Daniel, M.; Funk, S.; Geringer-Sameth, A.; Hinton, J.A.; et al. (2015).
579:
135:
1809:
1759:
1594:
1506:
1242:
1126:
1062:
1024:
973:
916:
857:
831:
789:
738:
717:"Dark matter annihilation and decay in dwarf spheroidal galaxies: The classical and ultrafaint dSphs"
676:
622:
559:
506:
445:
392:
280:
170:
more or less the same time, dwarf spheroidal galaxies experience multiple bursts of star formation.
1914:
1572:
1480:
1411:
1303:
1178:
103:
1845:
1902:
1890:
1804:
1799:
1784:
1739:
1708:
1693:
1611:
1579:
1416:
1368:
1358:
1014:
963:
932:
906:
893:
Strigari, Louie; Koushiappas, Savvas M.; Bullock, James S.; Kaplinghat, Manoj; Simon, Joshua D.;
875:
847:
813:
779:
728:
692:
666:
638:
612:
549:
522:
496:
469:
435:
408:
382:
312:
270:
1837:
1819:
1794:
1764:
1643:
1485:
1475:
1458:
1390:
1219:
1185:
1146:
1099:
805:
461:
353:
304:
296:
1849:
1651:
1626:
1606:
1601:
1589:
1443:
1264:
1197:
1032:
981:
924:
865:
797:
746:
684:
630:
567:
514:
510:
453:
400:
396:
288:
207:
203:
179:
147:
123:
95:
1698:
1621:
1313:
1286:
1257:
1209:
1055:
17:
1028:
977:
920:
861:
793:
742:
680:
626:
563:
449:
284:
198:, then it is likely that it is a dwarf spheroidal galaxy rather than an enormous, faint
1562:
1395:
1298:
1293:
1247:
1190:
227:
107:
75:
688:
1924:
1718:
1584:
1547:
1318:
1281:
1269:
1121:
1116:
870:
835:
817:
696:
526:
473:
162:
in 2015. Each dSph is named after constellations they are discovered in, such as the
153:
The first dwarf spheroidal galaxies discovered were
Sculptor and Fornax in 1938. The
936:
879:
457:
412:
1878:
1713:
1616:
1557:
1542:
1448:
1373:
1168:
1158:
642:
518:
341:
316:
199:
57:
44:
767:
540:
K., Grebel, E. (1998). "Star
Formation Histories of Local Group Dwarf Galaxies".
1814:
1631:
1521:
1511:
1308:
1274:
1214:
1094:
195:
139:
87:
1516:
1453:
894:
600:
571:
258:
235:
215:
127:
809:
465:
300:
86:
with very little dust and an older stellar population. They are found in the
1526:
986:
951:
751:
716:
257:
Strigari, Louis E.; Bullock, James S.; Kaplinghat, Manoj; Simon, Joshua D.;
143:
91:
79:
35:
1037:
1002:
308:
554:
501:
387:
111:
292:
404:
183:
that dwarf spheroidal galaxies have a dynamical mass of around 10
1363:
1348:
1078:
83:
53:
1873:
1019:
968:
928:
801:
733:
671:
634:
190:, which is very large despite the low luminosity of dSph galaxies.
1436:
1431:
1426:
1383:
911:
852:
784:
617:
440:
275:
1001:
Roderick, T.A.; Jerjen, H.; Da Costa, G.S.; Mackey, A.D. (2016).
1051:
950:
Battaglia, Giuseppina; Sollima, Antonio; Nipoti, Carlo (2015).
373:
Ferguson, Henry C.; Binggeli, Bruno (1994). "NASA/ADS Search".
768:"On the stellar content of the Carina dwarf spheroidal galaxy"
60:(right), two of the earliest known dwarf spheroidal galaxies.
1003:"Structural analysis of the Sextans dwarf spheroidal galaxy"
238:, experiences strong tidal disturbances from the Milky Way.
218:, experiences strong tidal disturbances from the Milky Way.
1047:
952:"The effect of tides on the Fornax dwarf spheroidal galaxy"
122:
Despite the radii of dSphs being much larger than those of
840:
Monthly
Notices of the Royal Astronomical Society: Letters
214:
evidence that the UMa2, a dwarf spheroidal galaxy in the
772:
1862:
27:
Low-luminosity galaxy of old stars & little dust
1727:
1642:
1535:
1494:
1404:
1339:
1230:
1085:
222:or other galaxy that they orbit. For example, the
102:in appearance and properties such as little to no
1007:Monthly Notices of the Royal Astronomical Society
956:Monthly Notices of the Royal Astronomical Society
836:"Globular clusters and dwarf spheroidal galaxies"
721:Monthly Notices of the Royal Astronomical Society
114:in shape and generally have lower luminosity.
1704:List of the most distant astronomical objects
1063:
8:
584:: CS1 maint: multiple names: authors list (
489:Annual Review of Astronomy and Astrophysics
487:Mateo, Mario L. (1998). "NASA/ADS Search".
1070:
1056:
1048:
230:. Similar to Sextans, previous studies of
94:and as systems that are companions to the
1036:
1018:
985:
967:
910:
869:
851:
783:
750:
732:
670:
616:
553:
500:
439:
386:
274:
202:. In the current predominantly accepted
1869:
246:
577:
710:
708:
706:
336:
334:
332:
330:
328:
326:
252:
250:
142:, dSphs are primarily found near the
7:
164:Sagittarius dwarf spheroidal galaxy
25:
375:Astronomy and Astrophysics Review
82:applied to small, low-luminosity
1908:
1896:
1884:
1872:
1844:
1833:
1832:
871:10.1111/j.1745-3933.2008.00424.x
232:Hercules dwarf spheroidal galaxy
43:
34:
224:Sextans dwarf spheroidal galaxy
1775:Galaxy formation and evolution
1770:Galaxy color–magnitude diagram
519:10.1146/annurev.astro.36.1.435
344:; Gallagher, J.S. III (2016).
1:
1657:Galaxies named after people
689:10.1088/0004-637X/805/2/130
1967:
1951:Galaxy morphological types
1790:Gravitational microlensing
1745:Galactic coordinate system
350:Cambridge University Press
1936:Dwarf elliptical galaxies
1931:Dwarf spheroidal galaxies
1828:
899:The Astrophysical Journal
659:The Astrophysical Journal
605:The Astrophysical Journal
572:10.1017/S1539299600020190
458:10.1088/0004-6256/144/1/4
110:, they are approximately
100:dwarf elliptical galaxies
18:Dwarf spheroidal galaxies
1755:Galactic magnetic fields
1568:Brightest cluster galaxy
1464:Luminous infrared galaxy
428:The Astronomical Journal
346:Galaxies in the Universe
236:Ursa Major constellation
216:Ursa Major constellation
155:Sloan Digital Sky Survey
98:(M31). While similar to
1750:Galactic habitable zone
1735:Extragalactic astronomy
1324:Supermassive black hole
1238:Active galactic nucleus
542:Highlights of Astronomy
511:1998ARA&A..36..435M
397:1994A&ARv...6...67F
204:Lambda cold dark matter
174:Evidence of dark matter
68:dwarf spheroidal galaxy
1502:Low surface brightness
1253:Central massive object
1780:Galaxy rotation curve
987:10.1093/mnras/stv2096
832:van den Bergh, Sidney
752:10.1093/mnras/stv1601
90:as companions to the
1815:Population III stars
1810:Intergalactic travel
1760:Galactic orientation
1627:Voids and supervoids
1038:10.1093/mnras/stw949
352:. pp. 162–165.
1941:Elliptical galaxies
1805:Intergalactic stars
1694:Large quasar groups
1689:Groups and clusters
1553:Groups and clusters
1412:Lyman-alpha emitter
1304:Interstellar medium
1029:2016MNRAS.460...30R
978:2015MNRAS.454.2401B
921:2008ApJ...678..614S
862:2008MNRAS.385L..20V
794:2010PASP..122..651B
743:2015MNRAS.453..849B
681:2015ApJ...805..130K
627:2007ApJ...670..313S
564:1998HiA....11..125G
450:2012AJ....144....4M
293:10.1038/nature07222
285:2008Natur.454.1096S
269:(7208): 1096–1097.
1800:Intergalactic dust
1785:Gravitational lens
1740:Galactic astronomy
1709:Starburst galaxies
1449:blue compact dwarf
1405:Energetic galaxies
1369:BL Lacertae object
405:10.1007/BF01208252
348:. United Kingdom:
160:Dark Energy Survey
1860:
1859:
1820:Galaxy X (galaxy)
1795:Illustris project
1765:Galactic quadrant
1486:Wolf-Rayet galaxy
1476:Green bean galaxy
1471:Hot dust-obscured
1422:Luminous infrared
1186:Elliptical galaxy
834:(November 2007).
359:978-0-521-67186-6
208:globular clusters
180:globular clusters
124:globular clusters
16:(Redirected from
1958:
1913:
1912:
1911:
1901:
1900:
1899:
1889:
1888:
1887:
1877:
1876:
1868:
1848:
1836:
1835:
1481:Hanny's Voorwerp
1391:Relativistic jet
1265:Dark matter halo
1072:
1065:
1058:
1049:
1043:
1042:
1040:
1022:
998:
992:
991:
989:
971:
962:(3): 2401–2415.
947:
941:
940:
914:
890:
884:
883:
873:
855:
828:
822:
821:
787:
763:
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736:
712:
701:
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653:
647:
646:
620:
596:
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589:
583:
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557:
555:astro-ph/9806191
537:
531:
530:
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502:astro-ph/9810070
484:
478:
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423:
417:
416:
390:
388:astro-ph/9409079
370:
364:
363:
338:
321:
320:
278:
254:
96:Andromeda Galaxy
47:
38:
21:
1966:
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1961:
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1959:
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1955:
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1919:
1909:
1907:
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1883:
1871:
1863:
1861:
1856:
1824:
1723:
1638:
1531:
1490:
1400:
1335:
1314:Galaxy filament
1258:Galactic Center
1226:
1081:
1076:
1046:
1000:
999:
995:
949:
948:
944:
892:
891:
887:
830:
829:
825:
765:
764:
760:
714:
713:
704:
655:
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598:
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539:
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372:
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339:
324:
256:
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244:
189:
186:
176:
120:
64:
63:
62:
61:
56:(left) and the
50:
49:
48:
40:
39:
28:
23:
22:
15:
12:
11:
5:
1964:
1962:
1954:
1953:
1948:
1946:Dwarf galaxies
1943:
1938:
1933:
1923:
1922:
1918:
1917:
1905:
1893:
1881:
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1857:
1855:
1854:
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1817:
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1797:
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1777:
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1737:
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1716:
1711:
1706:
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1696:
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1684:
1679:
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1669:
1664:
1659:
1648:
1646:
1640:
1639:
1637:
1636:
1635:
1634:
1624:
1619:
1614:
1612:Stellar stream
1609:
1604:
1599:
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1597:
1592:
1587:
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1575:
1570:
1565:
1560:
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1366:
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1337:
1336:
1334:
1333:
1332:
1331:
1321:
1316:
1311:
1306:
1301:
1299:Galactic ridge
1296:
1294:Galactic plane
1291:
1290:
1289:
1279:
1278:
1277:
1267:
1262:
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1260:
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1234:
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1077:
1075:
1074:
1067:
1060:
1052:
1045:
1044:
993:
942:
929:10.1086/529488
905:(2): 614–620.
885:
846:(1): L20–L22.
823:
802:10.1086/653590
758:
727:(1): 849–867.
702:
648:
635:10.1086/521816
611:(1): 313–331.
591:
532:
479:
418:
365:
358:
322:
245:
243:
240:
228:Virial Theorem
187:
184:
175:
172:
119:
116:
108:star formation
52:
51:
42:
41:
33:
32:
31:
30:
29:
26:
24:
14:
13:
10:
9:
6:
4:
3:
2:
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1715:
1714:Superclusters
1712:
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1700:
1697:
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1647:
1645:
1641:
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1630:
1629:
1628:
1625:
1623:
1620:
1618:
1617:Superclusters
1615:
1613:
1610:
1608:
1605:
1603:
1600:
1596:
1593:
1591:
1588:
1586:
1583:
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1581:
1578:
1574:
1571:
1569:
1566:
1564:
1561:
1559:
1556:
1555:
1554:
1551:
1549:
1548:Galactic tide
1546:
1544:
1541:
1540:
1538:
1534:
1528:
1525:
1523:
1520:
1518:
1515:
1513:
1510:
1508:
1507:Ultra diffuse
1505:
1503:
1500:
1499:
1497:
1493:
1487:
1484:
1482:
1479:
1477:
1474:
1472:
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1397:
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1380:
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1375:
1372:
1370:
1367:
1365:
1362:
1360:
1357:
1355:
1352:
1350:
1347:
1346:
1344:
1342:
1341:Active nuclei
1338:
1330:
1327:
1326:
1325:
1322:
1320:
1317:
1315:
1312:
1310:
1307:
1305:
1302:
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19:
1915:Solar System
1850:
1838:
1573:fossil group
1495:Low activity
1329:Ultramassive
1173:
1159:Dwarf galaxy
1142:intermediate
1137:grand design
1013:(1): 30–43.
1010:
1006:
996:
959:
955:
945:
902:
898:
888:
843:
839:
826:
778:(892): 651.
775:
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724:
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662:
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580:cite journal
545:
541:
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345:
342:Sparke, L.S.
266:
262:
220:
212:
200:star cluster
192:
177:
168:
152:
121:
71:
67:
65:
58:Fornax Dwarf
1903:Outer space
1891:Spaceflight
1632:void galaxy
1595:cannibalism
1580:Interacting
1536:Interaction
1522:Blue Nugget
1512:Dark galaxy
1417:Lyman-break
1309:Protogalaxy
1275:Disc galaxy
895:Geha, Marla
601:Geha, Marla
548:: 125–126.
495:: 435–506.
381:(1–2): 67.
259:Geha, Marla
196:dark matter
140:Local Group
104:gas or dust
88:Local Group
1925:Categories
1672:Polar-ring
1517:Red nugget
1459:faint blue
1319:Spiral arm
1174:spheroidal
1164:elliptical
1147:Magellanic
1132:flocculent
1100:Lenticular
1087:Morphology
1020:1604.06214
969:1509.02368
734:1504.02048
672:1503.02079
665:(2): 130.
242:References
128:Ursa Minor
112:spheroidal
106:or recent
1607:Satellite
1602:Jellyfish
1590:collision
1527:Dead disk
1444:Starburst
1359:Markarian
1231:Structure
1198:Irregular
1169:irregular
912:0709.1510
853:0711.4795
818:119301603
810:1538-3873
785:1004.2559
697:118267222
618:0706.0516
527:119333888
474:118515618
466:0004-6256
441:1204.1562
301:0028-0836
276:0808.3772
144:Milky Way
118:Discovery
92:Milky Way
80:astronomy
1839:Category
1728:See also
1652:Galaxies
1379:X-shaped
1210:Peculiar
1152:unbarred
1110:unbarred
1079:Galaxies
937:11415491
880:15093329
434:(1): 4.
413:18879556
309:18756252
188:☉
84:galaxies
1865:Portals
1699:Quasars
1667:Nearest
1662:Largest
1563:cluster
1396:Seyfert
1025:Bibcode
974:Bibcode
917:Bibcode
858:Bibcode
790:Bibcode
739:Bibcode
677:Bibcode
643:9715950
623:Bibcode
560:Bibcode
507:Bibcode
446:Bibcode
393:Bibcode
317:4373541
281:Bibcode
74:) is a
1851:Portal
1682:Spiral
1585:merger
1364:Quasar
1349:Blazar
1287:corona
1203:barred
1179:spiral
1127:barred
1122:anemic
1117:Spiral
1105:barred
935:
878:
816:
808:
695:
641:
525:
472:
464:
411:
356:
315:
307:
299:
263:Nature
134:, and
132:Carina
54:NGC147
1879:Stars
1719:Voids
1644:Lists
1622:Walls
1558:group
1543:Field
1437:ELIRG
1432:HLIRG
1427:ULIRG
1384:DRAGN
1374:Radio
1354:LINER
1248:Bulge
1220:Polar
1015:arXiv
964:arXiv
933:S2CID
907:arXiv
876:S2CID
848:arXiv
814:S2CID
780:arXiv
729:arXiv
693:S2CID
667:arXiv
639:S2CID
613:arXiv
550:arXiv
523:S2CID
497:arXiv
470:S2CID
436:arXiv
409:S2CID
383:arXiv
313:S2CID
271:arXiv
136:Draco
1677:Ring
1282:Halo
1270:Disc
1215:Ring
1095:Disc
806:ISSN
586:link
462:ISSN
354:ISBN
305:PMID
297:ISSN
146:and
76:term
72:dSph
1454:pea
1243:Bar
1033:doi
1011:460
982:doi
960:454
925:doi
903:678
866:doi
844:385
798:doi
776:122
747:doi
725:453
685:doi
663:805
631:doi
609:670
568:doi
515:doi
454:doi
432:144
401:doi
289:doi
267:454
148:M31
78:in
1927::
1191:cD
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578:{{
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325:^
311:.
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295:.
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279:.
265:.
249:^
150:.
130:,
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1064:t
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1035::
1027::
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687::
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633::
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517::
509::
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456::
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415:.
403::
395::
385::
379:6
362:.
319:.
291::
283::
273::
185:M
70:(
20:)
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