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Double Line 5c>?=5e?>=6X6\ H q@=B7AA Single Line5hA@HZqB@C7q TableFootnoteEGxR qCB7 9EGxR EPwEPw  TableFootnoteod5pDRRHH5xE5 HH +Fe   HH5zFN5 HHlEE DHH5{G6 HH @>?He   HH5}HJ6HHlGG HUV 5~I6 HUV AAJUU`   HUV 5JLH6HUV lII H$ 5K6 FtnH$ ELUU` tn oH$ 5LJ6H$ lKK HUV 5M5 HUV N UUe !  HUV 5NPF5HUV lMM H$ 5O5 H$ P UUe "  H$ 5PN5H$ lOO HH5QD HH[AR  ` # Large Scale Structure C ` ' of the Universe f` $  ` & 5Clusters of Galaxies n` (  The Local Group ` )  Virgo cluster ` * tn Coma cluster ` ] Dynamics of clusters "` e  Cannibalism ?` -  Luminosity function \` .  Velocity dispersion ` + Superclusters and Voids ` / UUIntergalactic Matter Ѐ` 0 F Hot gas ` 1  More dark matter ` 2 Very Distant Galaxies 6` 3  Galaxy morphology S` 4  The Hubble Deep Field HH5RDHHlUQQ d5SUUHH5TS HH0 ` #Ual ` % 'Clusters of Galaxies ;` 7 'Obvious groupings of (bright) galaxies axiX` 5 ( u` 8 p Abell Classification: ` 9 Regular clusters ` : ؀4Large (  1000  or more with M  -15 ) e` ; m Spherical symmetry  ` < n Mainly elliptical galaxies ity` =  #` > stIrregular clusters @` ? rgMixtures with no clear pattern F]` @ Variation in size and shape erz` A 2 ` B ax Examples: ` C laLocal group Irregular ` G bbOthers nearby ` E Virgo cluster Irregular  ` F Coma cluster Regular U(` D  HH5USUHHlRXTT  d5VXXalHH5WV i HHObht) galaX ` 6 The Virgo Cluster ;` H A regular irregular cluster X` I ˀ au` K )Distance  16  Mpc and  Dq 7 ` L l   Diameter   2  Mpc Ma` M la s` N =Hundreds of bright galaxies Ir` O Four giant ellipticals tur` P atM87 at the center @#` S sM100 a prominent spiral @` Q  ]` R : X-Ray emission apparent l z` T  ` U OtBigger than local group and ` X Bright ellipticals dominate ` V Rbut U` W Not spherical and  ` Y Many spirals and irregulars HH5XVHHlU[WW d5Y[[HH5ZY HH+  ter ;[  ` J usThe Coma Cluster I;` Z Nearest regular cluster X` [ ˻  u` ^ l *Giant elliptical (NGC 4881) at the center ` c HST to map globular clusters r` d   Distance determination l` _  ` ` heSpherical symmetry ` a ro e#` b  HH5[YsonHHlX^ZZ d5\Br^^HH5]\ NoHHls and ice^ ` \ Dynamics of Galaxy Clusters P` f Cannibalism [m` g .The source of the giant, central ellipticals? ` h  ` j Luminosity function Ā m )The number of galaxies in a cluster with  H m 7luminosities between  L  and  L+dL  isf Y` k cl9and  L C  corresponds to  M B  = -19.4 v` n 81'  Lots of low luminosity galaxies! to` o te r` l Velocity dispersion mi p .Peculiar motion: Important for interpreting  H p redshifts. Findg [` q 0  Must be accounted for in Hubble Expansion x` , )for distances less than  20  Mpc HH5^\^HHl[a]]  d6_aaHH6`_ yluHH faso d i eSuperclusters and Voids h;d r %How are galaxy clusters distributed? Xd s nu rud u clIs the Universe Isotropic? d v weProfound question! L+dd  d w  Prior to   1950 o d x 19$Yes!  (Hubble believed it was.) f d y ax 1950 to 1970 #d z Thorough galactic maps y d@d {   Maybe yes, maybe no ]d | iSince the 1970s zd } hiNO! Fid ~ (Clusters are grouped in Superclusters ubd  Large, spherical voids appear ssd M d Imprint of the Big Bang? ^HH6a_HHl^h`` @tHEk6 bctHEk@tHEk3'equal[times[char[Phi],id[char[L]],char[d],char[L]],times[id[(*i1i*)times[over[num[0.00500000,"0.005"],power[string["Mpc"],num[3.00000000,"3"]]],power[id[over[indexes[0,1,char[H],num[0.00000000,"0"]],num[50.00000000,"50"]]],num[3.00000000,"3"]]]],power[id[over[char[L],indexes[0,1,char[L],char[C]]]],minus[fract[num[5.00000000,"5"],num[4.00000000,"4"]]]],power[char[e],minus[over[char[L],indexes[0,1,char[L],char[C]]]]],id[over[times[char[d],char[L]],indexes[0,1,char[L],char[C]]]]]]N1Z6 ce\ bb]f B7h4N6de }e"J B7h4N0 a'equal[indexes[0,1,char[sigma],char[p]],sqrt[sum[over[power[indexes[0,1,char[v],char[p]],num[2.00000000,"2"]],plus[char[n],minus[num[1.00000000,"1"]]]],string["Galaxies"]]],times[num[400.00000000,"400"],string[" to "],num[1500.00000000,"1500"],string[" km/sec"]]]N:T6ec\dd]g@td62f,[chhim[iHH63gf ,weHH00ver[indeh], ` t 0.Intergalactic Matter 0;` we dX` xe No intergalactic reddening actu` "]: r DUST   < 410 -30   kg/m 3  ` ha$< 10 -15  r DUST (ISM) ],` ], r`  Little absorption in UV ` b  Not much neutral gas h`  #` e X-Ray emission from clusters  a@` s[+  Some hot gas  inside  clusters ind]` ha ]z` 2"" Galactic motion predicts masses ` al0  M/L   100 - 300  Dark Matter! o HH65hfc]]HHlakgg ]d68ikkhHH69ji HH  kde  ` Looking Back in Time g;`  X` %Time for light to reach us  = d/c eu 2  Look for faint, red objects to get close to @ the age of the universe. ` ST ` What shapes are the galaxies? ` io n` "Will return to this later  ... 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