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Double Line} w5c>?=5e?>=66 H q@=B7AA Single Line~5hA@HZqB@C7q TableFootnoteEGxR qCB7 9EGxR EPwEPw  TableFootnoteod5pDRRHH5xE5 HH gFe   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 BHHAR  ` # Active Galaxies I ;` $ ,Galaxies with more luminosity than normal X` % 5 u` ( tnExtreme star forming activity ` * Result of tidal interactions? ` ) oExamples:M82 ` - NGC 253 ` 2 *Moderately active. Maybe conventional. ` 3  1` +  N` , Radio Galaxies k` . 4L RADIO  greater than  ~10 33   W ` / FExamples:M87 (aka Virgo A) ` 0 Cygnus A €` 1 Centaurus A ` ' )Very active. Truly something special. HH5RDHHlUQQ d5SUUHH5TS HHRU ` & alRadiations from M87 $;` 4 h A summary X` 5  u` 7 Optical Properties Ex` = a@M V  -22.3  L   6.310 10   L SUN ` B pl 2.510 37  W ` 8 ˀ)Size  7  arcmin  30  kpc ` 9 Ѐ*Internal  jet  1.5  kpc long ` :  a#` ; ՀRadio Emissions L@` < er Compact core ]` > ˀ;Jet is clear:  L  10 34   W and polarized ` 0z` C ̀Falls rapidly with frequency ` ?  e` @ soX-Ray Observations H` A 5DL XRAY  510 35   W   L OPTICAL  /50 HH5USHHlRXTT d5VXXHH5WV &HHlM8  A summkkX  ` U 7Radio Galaxies per;` V General radiation properties X` W   0u` X 'Enormous emission at radio wavelengths W ` Y ˀ" Greater than  10 33  W ` [ 0(Normal optical output  ~10 36   W) g ` Z 2 Typically  10 6  times normal galaxies  h \ ac* Steeply falling frequency spectrum: )  ` ] 34 *` ^ ed Distinct optical emission lines piG` _ Some lines are forbidden d` ` y &  Emitting area has low densities HH5XV HHlU[WW d5Y[[HH5ZY XHH }V|}[  ` 6 Synchrotron Radiation ;` D  X a 7,If a charged particle accelerates, it emits rau@ a tielectromagnetic radiation. u` b En o c io(If this acceleration is due to circular ea c 3+motion (e.g. in a magnetic field), we call ou@ c  $this  synchrotron radiation . pi` d  i# h e s 4The flux (intensity) goes like a power law:  . tr h f 8Very different from thermal (i.e. blackbody)!  - n HH5[YefoHHlX^ZZ  ded5\^^HH5]\ HH5  [[^  ` E The Jet Mechanism ;` F  X` g ,Similar to jet production in star formation u h h ro$but a lot more power generated: / b` i If c` j ce(Synchrotron radiation means the disk is el` k at Ionized (electrons emitting) ` l If Spinning at high speed o` m  Low density ` n gn c` o ou"Similar to gases around a pulsar. -` p /  Recall the jet in the HST crab images. 4ThHH5^\ .HHl[a]]  bld5_aaHH5`_ ZHHa ` G Radiations from Cygnus A ;` H .One of the strongest radio sources in the sky X` q 5 u` r Je%Radio output  10 38   W  s Si9This is  ~100  times the  total  output from h@ s re our Galaxy ted` t  i` u Most emission from lobes on ` { elExternal jets #` v le!  An extended radio galaxy l@` w t  h]` x Optical image fuzzy z` y gn*Suggests elliptical galaxy with dust lane ` z Like Centaurus A ??? HH5a_hHHl^j`` ݀ 5bcl|]Z9݀ $'equal[(*q"Blue"q*)char[(*q"Blue"q*)M],over[(*q"Blue"q*)times[(*q"Blue"q*)char[(*q"Blue"q*)r],power[(*q"Blue"q*)char[(*q"Blue"q*)v],num[(*q"Blue"q*)2.00000000,"2"]]],char[(*q"Blue"q*)G]]]NT5cehfhe bbi *n e 5deJewh>$'equal[(*q"Green"q*)approx[(*q"Green"q*)char[(*q"Green"q*)r],cross[(*q"Green"q*)sin[(*q"Green"q*)id[(*q"Green"q*)times[(*q"Green"q*)over[(*q"Green"q*)num[(*q"Green"q*)1.00000000,"1"],num[(*q"Green"q*)3.00000000,"3"]],string[(*q"Green"q*)" arcsec"]]]],times[(*q"Green"q*)num[(*q"Green"q*)15.00000000,"15"],string[(*q"Green"q*)" Mpc"]]]],times[(*q"Green"q*)sn[(*q"Green"q*)num[(*q"Green"q*)7.50000000,"7.5"],num[(*q"Green"q*)17.00000000,"17"]],string[(*q"Green"q*)" m"]]]NO5ecghddi +j5fgb;<$'equal[over[times[char[Delta],char[lambda]],indexes[0,1,char[lambda],num[0.00000000,"0"]]],times[over[num[1.00000000,"1"],num[2.00000000,"2"]],over[num[20.00000000,"20"],num[5030.00000000,"5030"]]],over[char[v],char[c]]]5NH5gehffi ,5d5hjjeql[HH5ih rn"HHmq*  "Green"qcgjee  ` I [(The Central Mass of M87 ],;` J .0 0X h K *q1For motion in a circular orbit, we know that * G h L 0,:Find  r  from angular size and distance to M87: + 5 h M q"4Find  v  from Doppler shift of OIII line: , 0, N GrOso    v  = 6.010 5   m/sec.  (Actually more, since the +@ N inclination angle is nonzero.) ` O ˧ ` P M  M  = 410 39   kg  = 210 9   M SUN  (!) u` R ],#Enormous mass in a small distance! 0009` Q um(r   25  pc) [5e` T "]Must  be a black hole. HH5jhHHlaii H96kVql[wlzW ) 6 lmk Gre6 mlokI[(s oM8~fg*6nopk nn ~fg*~~ 0.01 6omnki a 7:   fg6pnqk OI fg 0.1 fg 6qprk (tufg  1NVfg6rqsk VfgVV 10fg=k6sruk 0fg=k Frequency (GHz)rmoqfgX6txyk Q log (Intensity)t 6usvkl6vuwkl6llH6wvxkHmHH$6xwtko$$$$~6ytzkp$~~fg$2u6#zyksm@ a܀D60{|ARxDE\KC/'(atop[(*j4jq"Red"q*)equal[(*q"Red"q*)times[(*q"Red"q*)char[(*q"Red"q*)F],id[(*q"Red"q*)char[(*q"Red"q*)nu]]],times[(*q"Red"q*)indexes[(*q"Red"q*)0,1,char[(*q"Red"q*)F],num[(*q"Red"q*)0.00000000,"0"]],indexes[(*q"Red"q*)1,0,char[(*q"Red"q*)nu],minus[(*q"Red"q*)char[(*q"Red"q*)alpha]]]]],equal[(*q"Red"q*)log[(*q"Red"q*)id[(*i1iq"Red"q*)times[(*q"Red"q*)char[(*q"Red"q*)F],id[(*q"Red"q*)char[(*q"Red"q*)nu]]]]],plus[(*q"Red"q*)minus[(*q"Red"q*)times[(*q"Red"q*)char[(*q"Red"q*)alpha],log[(*q"Red"q*)char[(*q"Red"q*)nu]]]],string[(*q"Red"q*)"constant"]]]]NsZ61|}Ym{{Z .H64}|YV~Z -Z )67~}pZ )fg6X68~} FdZFdZFdZ log (Intensity)Ǜ69} Ǜ log (Frequency)KCl6:}jReld"qtilu66<}d*)v 4ed" )i ~ ~2yDuDuQy_~_~zRQO6=} *ReRQOcc Thermal"q*fgv6>} R"qfgv''  Synchrotron*)nH6H\(*@] /lp],-u6Kg*q-uc 6Lc - 66N4- 6-??HQQcQQ$6R XTQ gcc Z2Q2Q2c2u2u pllgl 66Pl 6ncyC~~lޥ6U ޥ$$ Rotating accretion diskZQ$6T ]Qz hmmvm[[_ddhu;fg#6[ fgu;fg#uKuK Jets)nQ=6Z (*Q=QNQN l--6^l-- ~~luF6_ NuFuu Centralu?6` u?uu engined6yHH6z HH7 ` S The Black Hole Engine ;` | ԛ&More efficient than nuclear reactions X` }  u` ti/Probable source of energy for active galaxies. `   ~ 2A mass m falls from a large distance onto a black  H ~ ˀ5hole of mass M. Gravitational energy release is 1 9` fgB(For nuclear reactions typically get  1 % of mc 2 .) V`   *s` /  Enormous potential for energy generation ` $if  you can feed it fast enough! ` ˛  h /Output luminosity is (for 100% efficiency) 2 /` 웦(where dm/dt is the mass feeding rate. HH6|HHlj 6tޡ6$'equal[times[char[Delta],char[U]],over[times[char[G],char[M],char[m]],char[R]],times[over[num[1.00000000,"1"],num[2.00000000,"2"]],char[m],indexes[1,0,char[c],num[2.00000000,"2"]]]] NP6gax 1 6 rgx06e$'Pequal[(*q"Red"q*)char[(*q"Red"q*)L],times[(*q"Red"q*)over[(*q"Red"q*)num[(*q"Red"q*)1.00000000,"1"],num[(*q"Red"q*)2.00000000,"2"]],over[(*q"Red"q*)times[(*q"Red"q*)char[(*q"Red"q*)d],char[(*q"Red"q*)m]],times[(*q"Red"q*)char[(*q"Red"q*)d],char[(*q"Red"q*)t]]],indexes[(*q"Red"q*)1,0,char[(*q"Red"q*)c],num[(*q"Red"q*)2.00000000,"2"]]]]NH6)2 2wh isd5Leftd6RightHd7 ReferencedDdSdVdYta[Ud\[M[md_[100dh],],d00 a 5 f a Body. f b 00] vBulleted\t". )cf c CellBody. f d  CellHeading. f e V Footnote. f fT Heading1Body. f gT  Heading2Body. f hT   HeadingRunInBody. f i l yIndented. f j g Numbered.\t. f kE  Numbered1.\tNumbered. f l f TableFootnote. f mT   TableTitleT:Table : .  f nP TitleBody. f o T   TableTitleT:Table : . f p   CellHeading. f q  CellBody. f r   CellFooting. f s  Body. @ t  lHeader. @ u  blaFooter. f v g.Body. f w Body. $f x Body. $f y Body. f z .Body. f { $ Body. $f |  Body. Hf }  Body. f ~  Body. f    Body. f  Body. f  .Body. $f .Body. $f .Body. $$f Body. f .Body. f $ Body. $f .Body. f  Body. f  Body. $f Body. f  Body. f  Body. f  Body. $$f  Body. $f  Body. $$f  Body. $f  Body. f  Body. Hf  Body. f Body. $$$f Body.  $  Emphasis  EquationVariables )   ڝ  ڝ ڝ tu  [  tu ڝ ڝ w w $)  tu )  tu ڝ w w  ڝ ڝ  ڝ ڝ tu  ڝ w ڝ w ڝ tu ڝ w ڝ w w  Z Z Z  Z Z Z Z Z Z Z  Z  Thin Medium Double Thick@  Very Thin     oH p q rH p q rH p q rH p q rH p q rFormat A   oH p q rH p q rH p q rH p q rH p q rFormat B U e V UComment d BlackT!WhiteddAReddd Greendd  Blued Cyand Magentad Yellow  Times-Roman Times-Bold Times-ItalicHelvetica-BoldSymbolSymbolTimes HelveticaSymbol RegularRegulary BoldRegularItalicQjq8/OlM%"#hm-,ڵktQD/WA 8h5V L5AxҮf_C<];JBm4Q>Lmᰫ/Ip| 8