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HUV 5NPF5HUV lMM H$ 5O5 H$ P UUe "  H$ 5PN5H$ lOO HH5QD HHAR  ` # Active Galaxies II H;` $ )More galaxies with high radiation output f` % 5Is there a common connection? ` &  ` ( BL Lacertae and similar things ` ) BL Lac objects ڀ` 0 Probably galaxies, but ... l` *  ` + UVSeyfert Galaxies 1` , Spirals with bright nuclei N` 1 %Sometimes  very  bright nuclei Uk` - UV ` . FQuasars ` / Once a big mystery €` 2 At the edge of the universe ߀` 3 *Just  very, very  bright nuclei ??? HH5RDUUHHlUQQ Hd5SUUHH5TS HHj U ` G IIRadio Galaxies ` $;` H s A summary X` I ˀ u` Q he Two classes nn` S *Compact: Radio image smaller than optical ` T gs Example: M87 ` U ob*Extended: Radio image larger than optical ` V ΀Example: Cygnus A ` R UV e#` L ҀRadio emitters Sp@` N nu,High radio output ( >10 33   W) ry]` O U&Spectrum falls quickly with frequency z` P ˀ Clear jets ` W ry  Lobes in extended class ed` M  ` J JuOptical properties br` K Elliptical galaxies  ` Y UUSome emission lines in spectra (` X QJets apparent in some cases 5E` Z  b` [ X-Ray emitters HHH5USHHlRXTT d5Vs $XXmmy HH5WV eTwHH0 image sXti ` ' ExBL Lac Objects ;` 4 nd Variable star #53 in Lacertae l X` 5 ˀ xu` 7 Rapid variability ` 8 Ԁ4D m  2-3  typical in   one month ut` 9 Evident at all wavelengths U` ; ui y` < Peculiar spectrum ` : No clear emission lines #` = edVery nonthermal continuum @` > OpPerhaps synchrotron emission ]` ? al lz` @ Polarized emission on ` A *Intensity polarized by  ~20 % or so ` B Strong! ` C "Polarization varies rapidly, too. ` D   ` E Images are starlike (` F TFuzz apparent? dHH5XVXHHlU[WW  ed5Y[[tiHH5ZY HHabe l X[ ` 6 RaSeyfert Galaxies ;` \ DActive spiral galaxies l iX` ] nt tu` ^ +Optical spectra show strong emission lines ` ;` _ Type 1:  Very broad lines ` p No#D v   10 6   m/sec ` =` a maMainly non-forbidden lines Op` b ro%Forbidden lines somewhat more narrow ` c Po!Type 2:  Lines not very broad A#` d la#Type 1.5:  Somewhere in between @` e  ]` f PoOptical images distinct tz` g DSpiral arms apparent E` h taVery bright center regions Fu` q "Short exposure just shows nucleus ` i   Active Galactic Nuclei ` m )Emission lines sensitive to image region  ` n BLR:  Broad line region (` o NLR:  Narrow line region abE` j  b` k Normal radio emission ` l Ga Not classed as Radio Galaxies veHH5[YtHHlX^ZZ d6\din^^DvHH6]\ aHHxdd` b ro^ne ` ` Quasars c;` r Li$Active galaxies at large distances? laX` s me ru` u Some history ` v f%Third Cambridge Radio catalog (3C) ` w al$  Look for optical counterparts Ve` x egSome looked like stars ` { usExamples: 3C48, 3C273 ` | ?Quas istell a r  R adio Object s  (QSOs) sen#` y giHowever:Radio stars ??? L@` } reStrange optical spectra! ]` z li rz` ~ The breakthrough `  al+Optical spectrum of 3C273 (m  = 13 ) sse` es(Typical emission lines at high redshift ߀` z  = 0.158  v/c ` /d  =  v / H 0  = 630  Mpc in` 'M  = -26 =  M M87   - 4 6` Forty times brighter than M87! S` &And its brighter still in the radio! p` And 3C273 is relatively nearby! arHH6^\HHl[a]] idgd6"_l aaerrtHH6#`_ srsHHxuseeaQu ` t RAGNs and Quasars ;` A common thread? oX` ? Lu h re4Consider a schematic representation of spectra: p` Th.Black hole engines with varying fuel sources? HH6%a_HHl^d`` d6Kbdd/HH6Lcb HH dy  d Weird Stuff with Quasars t;d in eXd %We identify quasars because they are yud ,Very energetic  and  Very far away d  d Apparent Superluminal Motion d /Does the 3C273 jet move faster than  c ? "l 1No, if the jet is moving close to  c : $ /  Light from jet reaches us one year later uasD +but it seems to have moved 14 light years!  Ld re od rDouble (or multiple) Quasars "l Th%Actually a gravitational lens: sHH6NdbHHlacc ``H6Re_Nf`$ 6Vfge$  X6Wgfhe dZdZdZ log (Intensity) wiZ6XhgkeZtifquZZfg,6ziste cfg, Wavelength (m)6ljqle ti 736\khnetheet 6nljpe KyFg Y72as'0power[num[10.00000000,"10"],num[2.00000000,"2"]]gh6vmrsey"ndg72'7power[num[10.00000000,"10"],minus[num[2.00000000,"2"]]]H6bnkoel26donqe2226rplre!y"ndg2'7power[num[10.00000000,"10"],minus[num[4.00000000,"4"]]]z6hqoje6Xzzz6trpme6ziy"ndgz'7power[num[10.00000000,"10"],minus[num[6.00000000,"6"]]]ql6ysmie72 72'num[1.00000000,"1"]6H26{tiue6n6H2 6Hz?-D6~utve[.0?.Dm@[2. 00??H?H?6--1666gVVlc 6vuwe[00lc  lӀccccc2MM)~6wvxe)x{D )_ _ lzzhTRfgIQ6xwye [m[TRfgIQTbTb NormalX#hEO6yxze X#hEOX#xdZX#xdZ Galaxyu9V6zy{e u9Vu u Radio,u'EO6{z|e u'EOu8u8 GalaxyD6|{}e u1.D SeyfertiuěEO6}|~e ěEO Galaxyl@C6~}e l@ClQlQ Quasar 6~e 6 $cfg9V6e cfg9Vcc Radioz 6ez 6z z$ 6e  $ 6e   "dZ "dZ IRfg%XF6e 6[Fll OpticalxdZfg"6e fg" UVH6e6H H9~6bc1.;?6eu;?6;z$66eaxy$66Z$-6eQu-QQ6QQZ--6gVZ--ZZ-ZZ6ZZzZZZ--6---ZH-6H- dZHHh%R[6 h%R[h6h6 To Earthfg6fg^6 fg6fg^66  Jet movesl_fg6 l_fglolo  100 light years-)fg6 .-)fg-9-9  101 light years706 70HH 14 lyHH6bcQu66 7 C??:66 :??CHHLQQLHHC666zH-6zH--zHHh$R[6 h$R[h4dZh4dZ To Earthhfgw6 hfgwxx Dim (but massive) galaxy$-6$-_fg$?-;-$?6$?s$?Z;Zd6HH6 HH Confirmation: Quasars are C @ Active Galactic Nuclei f` Ѐ!Recent observations with the HST `  ` 4Quasars are rare, but very bright, distant objects. `   3If they are just extra-bright active galaxies, you  0should see the galaxy if you can collect enough [@ 'light and have good enough resolution. h1`  N` 6  Made for the HST k`  ` m-Clear observations that quasars have fuzz. `  ` 2Some cases show spiral arms with  HII regions! 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