1819:
1831:
1871:
1895:
1883:
1859:
543:
and dark matter, form by merging with each other. Evidence suggests that the formation of galactic halos may also be due to the effects of increased gravity and the presence of primordial black holes. The gas from halo mergers goes toward the formation of the central galactic components, while stars
161:
which extends throughout the galaxy extending far beyond its visible components. The mass of the dark matter halo is far greater than the mass of the other components of the galaxy. Its existence is hypothesized in order to account for the gravitational potential that determines the dynamics of
457:
is a dimensionless constant. The invisible halo component cannot extend with this density profile indefinitely, however; this would lead to a diverging integral when calculating mass. It does, however, provide a finite gravitational potential for all
318:
133:. The halo stars of the Milky Way have an observed radial velocity dispersion of about 200 km/s and a low average velocity of rotation of about 50 km/s. Star formation in the stellar halo of the Milky Way ceased long ago.
538:
model of the universe in which the evolution of systems such as halos occurs from the bottom-up, meaning the large scale structure of galaxies is formed starting with small objects. Halos, which are composed of both
404:
141:
A galactic corona is a distribution of gas extending far away from the center of the galaxy. It can be detected by the distinct emission spectrum it gives off, showing the presence of
129:. In our stellar halo, stars tend to be old (most are greater than 12 billion years old) and metal-poor, but there are also halo star clusters with observed metal content similar to
202:
177:
is a widely accepted density profile of the dark matter halo determined through numerical simulations. It represents the mass density of the dark matter halo as a function of
455:
110:. A low amount (about one percent) of a galaxy's stellar mass resides in the stellar halo, meaning its luminosity is much lower than other components of the galaxy.
1641:
738:
347:
1688:
520:
500:
476:
424:
195:
526:: the fastest-moving stellar objects still gravitationally bound to the Galaxy can give a lower bound on the mass profile of the outer edges of the dark halo.
1338:
786:
761:
697:
482:, which state that if the shape of the halo is spheroidal or elliptical there will be no net gravitational effect from halo mass a distance
174:
1071:
1754:
1673:
1054:
478:. Most measurements that can be made are relatively insensitive to the outer halo's mass distribution. This is a consequence of
1759:
584:
1486:
352:
1656:
1849:
1774:
1729:
1537:
1126:
1121:
1094:
968:
578:
479:
1455:
1739:
1651:
1646:
1552:
1448:
1406:
1116:
1089:
876:
Navarro, Julio F.; Frenk, Carlos S.; White, Simon D. M. (May 1996). "The
Structure of Cold Dark Matter Halos".
714:
38:
which extends beyond the main, visible component. Several distinct components of a galaxy comprise its halo:
1734:
1719:
1666:
1325:
1313:
1308:
1222:
1187:
1158:
1148:
1237:
1136:
1764:
1661:
1363:
85:
A halo can be studied by observing its effect on the passage of light from distant bright objects like
1794:
1744:
1579:
1491:
1227:
1111:
1047:
990:
895:
840:
715:"The Andromeda galaxy's halo is even more massive than scientists expected, Hubble telescope reveals"
646:
162:
bodies within galaxies. The nature of dark matter halos is an important area in current research in
1899:
1557:
1465:
1396:
1288:
1163:
967:
Zolotov, Adi; Willman, Beth; Brooks, Alyson M.; Governato, Fabio; Brook, Chris B.; Hogg, David W.;
1830:
1887:
1875:
1789:
1784:
1769:
1724:
1693:
1678:
1596:
1564:
1401:
1353:
1343:
1014:
980:
919:
885:
830:
670:
636:
433:
167:
592: – Spiral-shaped regions of enhanced brightness within the galactic disc in spiral galaxies
522:. The only dynamical variable related to the extent of the halo that can be constrained is the
1915:
1822:
1804:
1779:
1749:
1628:
1470:
1460:
1443:
1375:
1204:
1170:
1131:
1084:
1006:
911:
858:
782:
757:
732:
693:
662:
118:
79:
1834:
1636:
1611:
1591:
1586:
1574:
1428:
1249:
1182:
998:
903:
848:
654:
650:
535:
154:
103:
64:
57:
325:
313:{\displaystyle \rho (r)={\frac {\rho _{\text{crit}}\delta _{c}}{(r/r_{s})(1+r/r_{s})^{2}}}}
1683:
1606:
1298:
1271:
1242:
1194:
1040:
572:
523:
427:
71:
49:
994:
899:
844:
581: – Celestial coordinate system in spherical coordinates, with the Sun as its center
82:, there is no sharp transition between the other components of the galaxy and the halo.
1547:
1380:
1283:
1278:
1232:
1175:
1002:
566:
505:
485:
461:
409:
180:
107:
1909:
1703:
1569:
1532:
1303:
1254:
1106:
1101:
953:
923:
75:
1018:
1863:
1698:
1601:
1542:
1527:
1433:
1358:
1153:
1143:
674:
548:
43:
547:
On the other hand, the halo of the Milky Way Galaxy is thought to derive from the
502:
from the galactic center on an object that is closer to the galactic center than
1799:
1616:
1506:
1496:
1293:
1259:
1199:
1079:
560:
158:
122:
70:
The distinction between the halo and the main body of the galaxy is clearest in
27:
Spherical component of a galaxy which extends beyond the main, visible component
954:"Advances in Black Hole Physics and Dark Matter Modelling of the Galactic Halo"
609:
1501:
1438:
658:
589:
142:
1010:
915:
862:
666:
1511:
163:
130:
114:
17:
853:
818:
890:
126:
106:. It surrounds most disk galaxies as well as some elliptical galaxies of
1348:
1333:
1063:
540:
102:
The stellar halo is a nearly spherical population of field stars and
86:
35:
1858:
907:
1421:
1416:
1411:
1368:
985:
971:; Stinson, Greg (2009-09-10). "The Dual Origin of Stellar Halos".
835:
641:
74:, where the spherical shape of the halo contrasts with the flat
1036:
569: – Tightly packed group of stars within a larger formation
53:
627:
Helmi, Amina (June 2008). "The stellar halo of the Galaxy".
575: – Hot, ionised, gaseous component in the Galactic halo
1032:
89:
that are in line of sight beyond the galaxy in question.
779:
1847:
534:
The formation of stellar halos occurs naturally in a
508:
488:
464:
436:
412:
355:
328:
205:
183:
145:
and other features detectable by X-ray spectroscopy.
1712:
1627:
1520:
1479:
1389:
1324:
1215:
1070:
514:
494:
470:
449:
418:
398:
341:
312:
189:
713:August 2020, Meghan Bartels 31 (31 August 2020).
399:{\displaystyle \rho _{\text{crit}}=3H^{2}/8\pi G}
34:is an extended, roughly spherical component of a
1689:List of the most distant astronomical objects
1048:
544:and dark matter remain in the galactic halo.
8:
737:: CS1 maint: numeric names: authors list (
1055:
1041:
1033:
349:is a characteristic radius for the model,
984:
889:
852:
834:
640:
507:
487:
463:
441:
435:
411:
382:
376:
360:
354:
333:
327:
301:
291:
282:
261:
252:
238:
228:
221:
204:
197:, the distance from the galactic center:
182:
117:stellar halo contains globular clusters,
1854:
819:"Dark Matter Halos from the Inside Out"
601:
752:Setti, Giancarlo (30 September 1975).
730:
629:The Astronomy and Astrophysics Review
7:
143:HI gas (H one, 21 cm microwave line)
754:Structure and Evolution of Galaxies
25:
1893:
1881:
1869:
1857:
1829:
1818:
1817:
952:Worsley, Andrew (October 2018).
756:. D. Reidel Publishing Company.
168:galactic formation and evolution
166:, in particular its relation to
157:is a theorized distribution of
93:Components of the galactic halo
1760:Galaxy formation and evolution
1755:Galaxy color–magnitude diagram
781:. Cambridge University Press.
692:. Princeton University Press.
585:Galaxy formation and evolution
406:is the critical density (with
298:
270:
267:
246:
215:
209:
1:
941:. Princeton University Press.
804:The Physics of Galactic Halos
563: – Type of galactic form
1003:10.1088/0004-637X/702/2/1058
937:Binney and Tremaine (1987).
1642:Galaxies named after people
530:Formation of galactic halos
450:{\displaystyle \delta _{c}}
175:Navarro–Frenk–White profile
1932:
1775:Gravitational microlensing
1730:Galactic coordinate system
690:Astrophysics in a Nutshell
579:Galactic coordinate system
1813:
973:The Astrophysical Journal
878:The Astrophysical Journal
817:Taylor, James E. (2011).
659:10.1007/s00159-008-0009-6
1740:Galactic magnetic fields
1553:Brightest cluster galaxy
1449:Luminous infrared galaxy
1735:Galactic habitable zone
1720:Extragalactic astronomy
1309:Supermassive black hole
1223:Active galactic nucleus
777:Jones, Mark H. (2015).
651:2008A&ARv..15..145H
1487:Low surface brightness
1238:Central massive object
802:Lesch, Harold (1997).
516:
496:
472:
451:
420:
400:
343:
314:
191:
1765:Galaxy rotation curve
823:Advances in Astronomy
517:
497:
473:
452:
421:
401:
344:
342:{\displaystyle r_{s}}
315:
192:
1800:Population III stars
1795:Intergalactic travel
1745:Galactic orientation
1612:Voids and supervoids
610:"OpenStax Astronomy"
506:
486:
462:
434:
410:
353:
326:
203:
181:
1790:Intergalactic stars
1679:Large quasar groups
1674:Groups and clusters
1538:Groups and clusters
1397:Lyman-alpha emitter
1289:Interstellar medium
995:2009ApJ...702.1058Z
900:1996ApJ...462..563N
854:10.1155/2011/604898
845:2011AdAst2011E...6T
1785:Intergalactic dust
1770:Gravitational lens
1725:Galactic astronomy
1694:Starburst galaxies
1434:blue compact dwarf
1390:Energetic galaxies
1354:BL Lacertae object
688:Maoz, Dan (2016).
512:
492:
468:
447:
416:
396:
339:
310:
187:
1845:
1844:
1805:Galaxy X (galaxy)
1780:Illustris project
1750:Galactic quadrant
1471:Wolf-Rayet galaxy
1461:Green bean galaxy
1456:Hot dust-obscured
1407:Luminous infrared
1171:Elliptical galaxy
939:Galactic Dynamics
788:978-1-107-49261-5
763:978-90-277-0325-5
699:978-0-691-16479-3
515:{\displaystyle r}
495:{\displaystyle r}
471:{\displaystyle r}
419:{\displaystyle H}
363:
308:
231:
190:{\displaystyle r}
104:globular clusters
80:elliptical galaxy
16:(Redirected from
1923:
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1884:
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1872:
1862:
1861:
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1833:
1821:
1820:
1466:Hanny's Voorwerp
1376:Relativistic jet
1250:Dark matter halo
1057:
1050:
1043:
1034:
1023:
1022:
988:
979:(2): 1058–1067.
964:
958:
957:
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943:
942:
934:
928:
927:
893:
891:astro-ph/9508025
873:
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536:cold dark matter
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155:dark matter halo
149:Dark matter halo
65:dark matter halo
21:
1931:
1930:
1926:
1925:
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1299:Galaxy filament
1243:Galactic Center
1211:
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1061:
1031:
1026:
966:
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729:
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712:
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626:
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621:
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573:Galactic corona
557:
532:
524:escape velocity
504:
503:
484:
483:
460:
459:
437:
432:
431:
428:Hubble constant
408:
407:
372:
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329:
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323:
297:
287:
257:
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224:
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201:
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151:
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137:Galactic corona
121:stars with low
100:
95:
72:spiral galaxies
50:galactic corona
28:
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22:
15:
12:
11:
5:
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1597:Stellar stream
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1296:
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1284:Galactic ridge
1281:
1279:Galactic plane
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1274:
1264:
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1262:
1252:
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1029:External links
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908:10.1086/177173
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680:
635:(3): 145–188.
619:
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594:
593:
587:
582:
576:
570:
567:Galactic bulge
564:
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1699:Superclusters
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1602:Superclusters
1600:
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1533:Galactic tide
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1492:Ultra diffuse
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1327:
1326:Active nuclei
1323:
1315:
1312:
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1307:
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1300:
1297:
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1900:Solar System
1835:
1823:
1558:fossil group
1480:Low activity
1314:Ultramassive
1266:
1144:Dwarf galaxy
1127:intermediate
1122:grand design
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31:
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1888:Outer space
1876:Spaceflight
1617:void galaxy
1580:cannibalism
1565:Interacting
1521:Interaction
1507:Blue Nugget
1497:Dark galaxy
1402:Lyman-break
1294:Protogalaxy
1260:Disc galaxy
884:: 563–575.
561:Disc galaxy
159:dark matter
115:Milky Way's
18:Galaxy halo
1657:Polar-ring
1502:Red nugget
1444:faint blue
1304:Spiral arm
1159:spheroidal
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1132:Magellanic
1117:flocculent
1085:Lenticular
1072:Morphology
969:Quinn, Tom
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724:2020-09-01
597:References
590:Spiral arm
426:being the
131:disk stars
1592:Satellite
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1575:collision
1512:Dead disk
1429:Starburst
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1216:Structure
1183:Irregular
1154:irregular
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719:Space.com
667:0935-4956
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439:δ
391:π
358:ρ
236:δ
226:ρ
207:ρ
164:cosmology
127:subdwarfs
56:, i.e. a
1916:Galaxies
1910:Category
1824:Category
1713:See also
1637:Galaxies
1364:X-shaped
1195:Peculiar
1137:unbarred
1095:unbarred
1064:Galaxies
1019:16591772
733:cite web
614:OpenStax
555:See also
541:baryonic
119:RR Lyrae
78:. In an
1850:Portals
1684:Quasars
1652:Nearest
1647:Largest
1548:cluster
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991:Bibcode
896:Bibcode
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430:), and
108:type cD
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1629:Lists
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1543:group
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1422:ELIRG
1417:HLIRG
1412:ULIRG
1369:DRAGN
1359:Radio
1339:LINER
1233:Bulge
1205:Polar
1015:S2CID
981:arXiv
920:S2CID
886:arXiv
831:arXiv
671:S2CID
637:arXiv
52:(hot
1662:Ring
1267:Halo
1255:Disc
1200:Ring
1080:Disc
1007:ISSN
912:ISSN
859:ISSN
827:2011
783:ISBN
758:ISBN
739:link
694:ISBN
663:ISSN
362:crit
230:crit
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