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Double Line 5c>?=5e?>=66 zH q@=B7\AA Single Line5hA@HZqB@C7q TableFootnoteEGxR qCB7 9EGxR EPwEPw  TableFootnoteod5pDRRHH5xE5 HH Fe   HH5zFN5 HHlEE DHH5{G6 HH @>?HDoe   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 HHjAR  ` #  Galaxies ;` $ Begin studying the universe X` %  u` ' 5.Classification of Galaxies  (Morphology) ` * Elliptical galaxies ` + ԪWide range of sizes ` , Spiral galaxies ` / Ordinary and Barred spirals K` - Star birth and nuclei #` . UVIrregular galaxies @` 0 Tidal disruption ]` ( UU !z` ) Visible Spectra of Galaxies ` 2 )Mostly absorption but sometimes emission ` 1 Doppler shifts 5` 3  ` 4 Nonvisible Radiations  ` 5 "Radio, Infrared, X-Ray, Gamma-Ray (` 6  NE` 7 Rotation Curves b` 8 !The Dark Matter problem persists HH5RDHHlUQQ d5S $UUnirsHH5TS '5HHNlaZZUEl ` & Elliptical Galaxies ge;` 9  X` : al: Spheroidal shapes with  large variations  in size u` < - ` > uc1Nomenclature: E n  where n = 10(a-b)/a ` ? Ti a =  major axis ` @  b =  minor axis tr` = "Observe that  0  n  7 ` E si # h A 3 Brightness described by de Vancouleurs law: ` B le3(Proportionality is for large values of  r ) Ray` C  ` D  Composition appears peculiar b` F Th9+  Most stars appear quite old ( ~10 10  yr)  ` G ++  Most of the mass in lower mass stars )` H -+  Most of the light from red giant stars F` I +  Generally very little gas HH5USaHHlRXTT  d5V 9XXal HH5WV  HHT < uc1No__X  ` ; b)Comparison of M32 and M87 ;` M xi#Two well known elliptical galaxies  mX` J  u` K th Appearance is very similar ` N ,Types are  E2 (M32)  and  E1 (M87) V` O ˆ ` P le Brightness is very different alu` Q ay6+  Apparent visual magnitudes ( m V ) are ` R ar8.2 (M32) and 8.6 (M87) + #` S ea"+  Distances can be determined @` U M32: In orbit around M31 ]` T &  d M 32  = 690  kpc z` V nt$M87: Globular cluster luminosities ne` Z ga'  d M 87  = 16.6 M pc  h W E+  Use  m V  - M V  = 5log d  -5 to find L` L )  M87 is 400 times brighter than M32 HH5XV HHlU]WW ݀ 5YZnf $z~ >݀ 1 k'equal[(*q"Blue"q*)log[(*q"Blue"q*)over[(*q"Blue"q*)times[(*q"Blue"q*)char[(*q"Blue"q*)I],id[(*q"Blue"q*)char[(*q"Blue"q*)r]]],indexes[(*q"Blue"q*)0,1,char[(*q"Blue"q*)I],char[(*q"Blue"q*)e]]]],propto[(*q"Blue"q*)minus[(*q"Blue"q*)times[(*q"Blue"q*)num[(*q"Blue"q*)3.33000000,"3.33"],id[(*i1iq"Blue"q*)plus[(*q"Blue"q*)power[(*q"Blue"q*)id[(*q"Blue"q*)over[(*q"Blue"q*)char[(*q"Blue"q*)r],indexes[(*q"Blue"q*)0,1,char[(*q"Blue"q*)r],char[(*q"Blue"q*)e]]]],fract[(*q"Blue"q*)num[(*q"Blue"q*)1.00000000,"1"],num[(*q"Blue"q*)4.00000000,"4"]]],minus[(*q"Blue"q*)num[(*q"Blue"q*)1.00000000,"1"]]]]]],minus[(*q"Blue"q*)power[(*q"Blue"q*)char[(*q"Blue"q*)r],fract[(*q"Blue"q*)num[(*q"Blue"q*)1.00000000,"1"],num[(*q"Blue"q*)4.00000000,"4"]]]]]] tNsX5ZS 4YYT d6[]]HH6\[ HHn ] k ` [ g[Spiral Galaxies *q;` X "BOne example is the Milky Way *X` Y "B "u` ] q" Two separate classes "q*` ^ q*.Ordinary designated as  S  or  SA ` b (*Bulge, disk, spiral arms ]` _ )pBarred designated as  SB ` ` veArms branch off the bar ` c Bl q#` a e"# Sub-classes describe spiral arms q"B@` d e"0Subclass a     tightly wound arms ]]]` f )n' b   arms somewhat clearer [(*z` g q"' c   pronounced, open arms e"q` e 1. 0` h Bl Strong dust lanes in disk ` m 5Apparent in edge-on views ` j   ` n ) OB Associations and HII in spiral arms ](` o Star formation! E` i  b` k 5 Central bulge follows log I   - r 1/4 k` l #Similar evolution to ellipticals?? HH6][HHlXb\\ "q*6&^_ #yJ lZdBBu'atop[(*j4j*)equal[(*l-131072ll-131072ll-131072lr-458752r*)plus[times[indexes[0,1,char[M],char[V]],id[times[char[M],num[87.00000000,"87"]]]],minus[times[indexes[0,1,char[M],char[V]],id[times[char[M],num[32.00000000,"32"]]]]]],plus[num[8.60000000,"8.6"],minus[num[8.20000000,"8.2"]],times[num[5.00000000,"5"],log[over[num[0.69000000,"0.69"],num[16.60000000,"16.6"]]]]]],uequal[minus[num[6.50000000,"6.5"]]]]%@{6'_V ro^^Wd6,`bb nHH6-a` r ]HHSt` ib ` \ lgOddball Galaxies ;` p k X` r SiDwarf Galaxies o eu` s &Small, irregular collections of stars ` x  ` t Irregular Galaxies "q*` u )Isolated and large, but no regular shape ` y Results of tidal disruption? [` w 2l 3#` v usCollisions and Cannibalism ar[@` z M]Proximity and velocity ,mi]` { 0,  Collisions iz` | m[ cD Galaxies 2"` } 60Extended ellipticals [` ~ ,tMultiple nuclei 0,`  0.  Cannibalism HH6/b`600HHl]eaa rod6UceeHH6Vdc HHeW ` The Morphological Mix ;` Ga iX` p"Of the  observed  galaxies, u` 77% are spirals l,` io20% are ellipticals ` 3% are irregulars `   at0However: Large, bright spirals most easily seen y@ idat large distances! #`  @` isOf the galaxies out to 9.1Mpc, ]` y 33% are spirals z` 13% are ellipticals ` al(54% are irregulars (lots of small ones) ip`  ~` le*Is this a better measure of the universe? ` Is the universe isotropic? H ` Later ... HH6XecHHlbhdd Hd6zfhhHH6{gf HHMo` h d q bsInvisible Radiations C d 77from Galaxies fd io 0d Continuum Radio d s More on this later. d at od ht 21-cm Radio ead Outlines spiral arms dd Determines rotation curves ` 1d ie uNd Infrared kd alFlux correlates with radio ard  d arX-Ray and  g -Ray l d Nuclei and other hot spots eHH6}hf HHlekgg ` d6ikkHH6ji HH6z  mmk  ` Galactic Rotation Curves ;` The Missing Mass problem X`  u q)Remember the result from gravitation and  H s motion in circular orbits: ` m Bwhere  M(r)  is the mass contained within radius  r . %`  B` ea5Is  M(r)  well described by the luminous mass? _` es t| 3For both ellipticals and spirals, the answer seems k@ Flto be  NO . 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