Revista Mexicana de Astronomía y Astrofísica ISSN: 0185-1101 [email protected] Instituto de Astronomía México

Higuera-G., Mario-A.; Ramos P., Andrés F. PAHS AS TRACERS OF LOCAL AGN-STARBURST CONNECTION Revista Mexicana de Astronomía y Astrofísica, vol. 49, núm. 2, octubre, 2013, pp. 301-309 Instituto de Astronomía Distrito Federal, México

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How to cite Complete issue Scientific Information System More information about this article Network of Scientific Journals from Latin America, the Caribbean, Spain and Portugal Journal's homepage in redalyc.org Non-profit academic project, developed under the open access initiative © Copyright 2013: Instituto de Astronomía, Universidad Nacional Autónoma de México eit eiaad srnmı Astrof´ısica Astronom´ıa y de Mexicana Revista is nvria ainld Colombia. de Nacional Universidad cias, a ainld Colombia. de Nacional dad amdu yterdaino h eta source, central is AGNs the in 2004; of dust Wada radiation nuclear the & The by Imanishi up 2007). warmed 2001; al. et Storchi- Davies al. 2000; et al. to et used (Clavel Bergmann processes be activ- stellar AGN and can between ity connection spec- that and origin IR wavelengths the The study many has emissions. bands atomic trum some and use to continuum diagrams formation quan- These of to luminosity. and IR order AGN the of in contribution built the diag- been tify many have and diagrams (AGNs), nostic Nuclei Galactic Active regions circumnuclear of and nuclear formation several al. star in et activity the im- quantify Maiolino made to have 2006; contributions 2012), portant Imanishi Rike & 2001; Diamond-Stanic 2007; al. et Spoon 1 2 ueossuis(i enne ta.2001; al. et Fernandez (Cid studies Numerous bevtroAto´mc ainl autdd Cien- de Facultad Nacional, Astron´omico Observatorio eatmnod ´sc,Fcla eCeca,Universi- Ciencias, de F´ısica, Facultad de Departamento ASA RCR FLCLANSABRTCONNECTION AGN-STARBURST LOCAL OF TRACERS AS PAHS lcmotmet elscaae aaisSyet1 efr o a gala las con 2 Seyfert 1- Seyfert LIRGs-ULIRGs. galaxias los y y brote, cuasares con los de comportamiento el nrroa Gs epooe uvsdarmsd ig´siobsdse l en diagn´ostico basados de diagramas gala formaci´on nuevos estelar, de discriminar proponen 7.7 brote en de Se PAH con emisi´on fin de circunnu- galaxias AGNs. de y el y conjunto nuclear espectrosc´opicos con infrarrojas un formaci´on estelar fotom´etricos y en de datos est´an vinculado procesos actividad usaron estos galaxias la Se de a n´ucleos activos debidos clear. los son de que actividad aquellos la a asociados L sdt iciiaebtenteepoessi apeo trus, starburst, 7.7 of the on sample based diagrams a diagnostic new in nucl propose we processes to Here, these due AGNs. and between those da spectroscopic to discriminate and related to Photometric are activity. used formation (AGN) star nuclei circumnuclear galactic or active with associated the fqaasadSyet1Syet2glxe rmsabrt n LIRGs-ULIRG and starbursts from Words: Key galaxies 2 1-Seyfert Seyfert objects. and quasars of oyylcaoai yrcro msinbn,the band, emission hydrocarbon aromatic polycyclic .INTRODUCTION 1. MR I)ye par´ametro el y FIR) (MIR, q lojtv eta eet rbj u netgrcoopoeo energ´eticos c´omo procesos investigar fue trabajo este de central objetivo El h anproeo hsrsac a oivsiaehweegtcprocesses energetic how investigate to was research this of purpose main The aaee.Tedansi igasalwu odsrmnt h behavior the discriminate to us allow diagrams diagnostic The parameter. aais cie—glxe:gnrl—glxe:nuclei galaxies: — general galaxies: — active galaxies: eevd21 oebr2;acpe 03Ags 5 August 2013 accepted 22; November 2012 Received ai-.Higuera-G., Mario-A. µ ,l a´netel ms´ne lifarj ei lejano y medio infrarrojo el emisi´on en la raz´on entre la m, q o igaa edanotc emtncomparar diagn´ostico permiten de diagramas Los . , 49 ABSTRACT RESUMEN 0–0 (2013) 301–309 , 1 n nre .RmsP. Ramos Andr´es F. and Br lrvoe U)poo,poiea nietmea- indirect an provide single photon, fluo- a (UV) IR by excitation through vibrational radiating following PAHs, star rescence trace The to (PAHs) formation. poly- use hydrocarbons others aromatic and (2006) cyclic al. Wada et & Schweitzer the Imanishi (2004), problem, by this mitigate 1) To dominated Type (i.e., sources. often unobscured for particularly are itself, AGN indicators SFR dard iheiso ie uha H as as well such as the lines infrared, of emission ranges far with two and in ultraviolet forma- luminosity continuum, calibrations star with These of linearly sequence. rates self- scale Hubble of a the along in estimates tion resulted of that set research consistent extensive out ried 2006). Imanishi 2006; al. et galax- the (Brand type infrared ies formation, and stellar starburst in with dominant latter associated 2008) ionized those al. the Mel´endez by et 1996; from and Mirabel coming & emissions (Sanders the gas by also and γ enct 19)adPnzoe l 20)car- (2003) al. et Panuzzo and (1998) Kennicutt n o rbblt f[ I ie.Teestan- These lines. II] [O of probability low and L MRFR nrrdrtoand ratio infrared (MIR,FIR) 2 α awere ta H , con s xias xias µ β ear m P , a s α P , β Br , 301 α , © Copyright 2013: Instituto de Astronomía, Universidad Nacional Autónoma de México 0 IUR-.&RAMOS-P. & HIGUERA-G. 302 G 6(r50 .9191+800734E1 1.52E-28 Mrk334 3.43E-14 0.067 1.911E+38 0.29 3786(Mrk744) NGC 863(Mrk590) NGC G 2503 .7E3 .1 .6-41.15E-28 1144 NGC Mrk573 Mrk993 1.86E-14 0.110 1.979E+37 0.31 4253(Mrk766) NGC 4235 NGC G 5802 .8E3 .5 .1-42.65E-28 4388 NGC 5.51E-14 0.054 1.185E+38 0.27 Mrk817 5548 NGC G 5252 NGC 7469 NGC G 3700 .0E3 .3 .4-45.26E-29 1.19E-27 7.94E-14 3.78E-13 0.134 9.908E+37 0.04 1.64 8.364E+39 -0.80 5695 NGC 5347 NGC 5256(Mrk266SW) NGC 7603) Mrk530(NGC rsF35+0504 .7E3 .2 .1-43.05E-28 5929 1.25E-28 NGC 5.61E-14 1.41E-13 0.025 0.050 2.177E+38 2.022E+38 0.47 0.08 MCG-5-13-17 F03450+0055 Iras 931(Mrk1040) NGC G 7674 NGC 2639 NGC Mrk79 G 6205 .3E3 .3520E1 5.62E-28 2.04E-14 0.2335 2.839E+37 0.53 Mrk938 7682 NGC 2992 NGC G 6(r38 .8371+8014 .5-42.75E-27 6.15E-14 0.1045 3.701E+38 0.08 513 NGC 262(Mrk348) NGC UGC7064 04504 .7194+801 .3-43.00E-27 4.23E-14 0.14 1.984E+38 0.17 1125 NGC F01475-0740 4748) MCG-2-33-34(NGC C39 .2251+800686E1 6.24E-28 1320(Mrk607) NGC 8.69E-14 0.026 2.541E+38 0.42 3227 NGC Mrk478 Mrk509 IC4329A F04385-0828 4051 NGC Ark120 G 1667 NGC 4593 NGC G 3660 NGC Mrk279 G 1101 .2E3 .4 .2-33.60E-27 2.94E-28 1.23E-28 3.22E-13 8.57E-14 1.83E-14 4501-S1-2 NGC 0.049 0.048 0.017 3.627E+37 4.459E+37 6.143E+37 0.18 0.08 0.80 4151 NGC 3516 NGC 526a NGC G 4968 NGC MCG-3-34-64 G 5135 NGC MCG-2-40-4 G 7172 NGC MCG-3-58-7 IC3639 Mrk34 Mrk78 Mrk477 Mrk463 G 0800 .8E3 .0485E1 4.56E-26 8.55E-12 0.1034 2.881E+39 0.05 5033 NGC 1068 NGC RS23704 .9509+8026 .1-41.42E-28 5.81E-14 0.2465 5.079E+38 0.09 4579 NGC 22377+0747 IRAS G 7314 NGC G 1097 NGC G 1386 NGC Mrk3 G 3982 NGC G 4507 NGC efr log(L12 2 Seyfert log(L12 1 Seyfert AAFO IEAUEADORESTIMATIONS OUR AND LITERATURE FROM DATA − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − / / − 6)L L60) L L60) .6249+8002551E1 2.26E-28 5.07E-29 5.13E-14 2.64E-14 0.07205 0.126 2.489E+38 1.593E+37 0.06 0.34 .8237+9061 .6-32.62E-28 1.96E-13 0.6815 2.357E+39 0.58 1.75E-28 7.68E-14 0.489 1.326E+38 0.38 .8957+916 .5-31.45E-27 3.15E-13 1.66 9.577E+39 0.58 3.58E-28 1.90E-13 0.231 3.484E+38 0.32 .1727+804656E1 1.12E-27 5.60E-13 0.406 7.267E+38 0.31 1.05E-28 9.75E-14 0.061 5.176E+38 0.10 .7215+7000 .4-41.53E-28 7.44E-14 0.0209 2.135E+37 0.67 1.70E-27 1.28E-12 0.609 3.497E+39 0.58 .2565+704241E1 5.92E-29 4.11E-14 0.442 5.655E+37 0.02 2.29E-28 5.33E-14 0.077 1.020E+39 0.03 .1386+800878E1 1.93E-28 7.85E-14 0.068 3.876E+38 0.01 .3238+7046 .0-31.02E-27 4.70E-13 0.4665 2.368E+37 0.63 1.33E-28 7.06E-14 0.371 2.085E+38 0.10 .2583+903428E1 2.08E-27 2.84E-13 0.304 5.823E+39 0.22 1.08E-27 1.54E-13 0.845 2.905E+38 0.40 .2627+916575E1 6.29E-28 7.56E-13 1.665 6.217E+39 0.92 2.13E-27 4.05E-13 0.496 2.870E+38 0.37 .6125+906511E1 4.97E-28 1.14E-13 0.675 1.225E+39 0.36 1.57E-28 1.60E-13 0.781 1.134E+39 0.51 .2117+900230E1 4.89E-29 1.75E-28 3.01E-14 6.34E-14 0.052 0.071 1.127E+39 7.588E+38 0.02 0.07 .9407+812515E1 5.45E-28 1.57E-13 1.225 4.087E+38 0.59 1.32E-28 6.57E-14 0.448 2.118E+38 0.14 .9247+800134E1 1.16E-28 3.45E-14 0.011 2.417E+38 0.39 .1316+801810E1 5.64E-29 1.05E-13 0.198 3.196E+38 0.11 9.17E-28 4.87E-13 0.309 4.897E+37 0.37 .2602+8006512E1 1.79E-28 1.22E-13 0.07665 6.072E+38 0.12 8.87E-28 5.33E-13 0.119 1.094E+37 0.22 .4354+931 .9-37.12E-28 3.79E-13 3.16 3.594E+39 0.44 4.13E-29 1.74E-13 0.033 4.028E+37 0.25 .9660+830511E1 1.16E-28 1.18E-13 3.095 6.660E+38 0.29 2.18E-28 6.87E-14 0.034 2.206E+38 0.09 .3359+803211E1 2.79E-27 1.13E-12 0.322 3.549E+38 0.43 .9365+802511E1 3.24E-28 1.14E-13 0.285 3.625E+38 0.09 .3674+816 .1-32.58E-27 2.61E-13 1.61 6.764E+38 0.13 .2351+909991E1 1.88E-27 9.10E-13 0.989 3.521E+39 0.72 .7174+9007520E1 2.82E-28 2.01E-13 0.09725 1.714E+39 0.27 .1551+8044 .1-33.46E-28 3.41E-13 0.4245 5.551E+38 0.41 .4162+9003 .1-31.17E-28 1.21E-13 0.0839 1.642E+39 0.24 .7131+907737E1 8.26E-28 3.79E-13 0.717 1.361E+39 0.37 .6103+9013 .4-41.79E-28 3.64E-14 0.1035 1.003E+39 0.36 .7477+9001595E1 3.58E-27 9.51E-14 0.06185 4.717E+39 0.07 .3901+801350E1 3.43E-28 5.03E-14 0.153 9.051E+38 0.23 .6222+813510E1 1.14E-27 1.00E-12 1.315 2.272E+38 0.46 .3162+7000538E1 9.10E-28 3.82E-13 0.04085 1.662E+37 0.43 .5203+702930E1 2.91E-28 3.00E-13 0.209 2.013E+37 0.45 .5117+91825E1 2.34E-27 2.52E-12 1.8 1.187E+39 0.65 .4609+7020 .7-33.49E-28 2.97E-13 0.2805 6.069E+37 0.34 .2436+8019 .5-31.03E-26 1.65E-13 0.1395 4.356E+38 0.02 .1214+816 .5-35.30E-28 4.05E-13 1.61 2.164E+38 0.41 .8207+800 .8-36.21E-28 2.08E-13 0.04 2.017E+38 0.28 . .5E3 .4565E1 5.67E-28 6.59E-14 0.1435 8.556E+38 0.3 7 7 . . 7 7 µ µ m m Wm (W m (W − − 2 2 AL 1 TABLE EQW ) EQW ) 7 7 . . 7 7 µ µ m m ( ( µ µ )Fu(I)( m (W Flux(FIR) m) m (W Flux(FIR) m) − − 2 2 F ) F ) 1 1 . . GHz 4 GHz 4 Wm (W m (W − − 2 2 Hz Hz − − 1 1 ) ) © Copyright 2013: Instituto de Astronomía, Universidad Nacional Autónoma de México C342 IC IRAS05189-2524 IRAS01572+0009(Mrk1014) IRAS11387+4116 IRAS00188-0856 6240 NGC 5728 NGC RS26+29323 .3133+9003210E1 5.1 1.03E-13 0.00352 Mrk52 1.363E+39 0.13 IRAS08559+1053 IRAS12540+5708(Mrk231) IRAS12265+0219(3C273) IRAS11506+1331 IRAS03250+1606 Iras23060+0505 5953 NGC G 0520 NGC IRAS13428+5608(Mrk273) IRAS15462-0450 IRAS13539+2920 1.74E-28 6.33E-13 0.01167 5.326E+39 0.11 IRAS08572+3915 253 NGC Iras20460+1925 7592 NGC G 1222 NGC IRAS13451+1232(PKS1345+12) IRAS14060+2919 IRAS09039+0503 828 NGC 4355) (NGC 4418 NGC G 1365 NGC IRAS17179+5444 IRAS15206+3342 IRAS09116+0334 Iras15250+3609 G 2146 NGC IRAS15225+2350 IRAS09539+0857 Iras17208-0014 G 2623 NGC IRAS16474+3430 IRAS10378+1108(9) Iras13126+2452 G 3310 NGC IRAS21208-0519 IRAS10485-1447 CGCG1510.8+0725 G 3556 NGC IRAS10494+4424 G 3628 NGC IRAS11095-0238 IRAS12112+0305 IRAS12127-1412 IRAS12359-0725 IRAS14252-1550 IRAS14348-1447 IRAS15327+2340(Arp220) IRAS16090-0139 IRAS16487+5447 IRAS17028+5817 IRAS17044+6720 IRAS21329-2346 LR-efr log(L12 2 ULIRG-Seyfert log(L12 1 ULIRG-Seyfert LR-IE log(L12 ULIRG-LINER LR-I log(L12 ULIRG-HII trus log(L12 Starburst efr log(L12 2 Seyfert IG log(L12 LIRGs ASADTEANSABRTCNETO 303 CONNECTION AGN-STARBURST THE AND PAHS − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − / / / / / / / − − 6)L L60) 6)L L60) 6)L L60) L L60) L L60) L L60) L L60) .8148+619 .8-11.79E-27 1.08E-11 2.71E-28 2.46E-28 5.88E-13 1.98 1.488E+36 9.94E-14 0.38 6.11E-29 0.16 8.346E+39 0.57 0.0612 5.22E-14 8.698E+39 0.57 1.78 1.237E+40 0.23 1.48E-28 1.27E-13 4.01E-27 1.416 6.58E-28 1.10E-12 2.592E+40 0.64 4.50E-13 1.62 1.467E+40 0.92 0.9385 3.584E+38 0.83 .3116+8087 .5-31.23E-28 2.25E-13 1.15E-28 2.90E-27 6.10E-14 0.8375 1.166E+38 1.42E-12 0.53 0.5465 1.27E-28 2.513E+40 0.08665 0.35 1.26E-13 1.436E+40 0.53 1.755 3.430E+40 0.71 8.93E-29 6.72E-14 6.30E-29 2.68 8.59E-28 1.842E+40 4.78E-14 0.44 5.64E-13 0.02805 1.266E+40 0.07 3.195 9.253E+38 0.57 .5385+926516E1 1.66E-27 1.36E-27 1.62E-12 1.20E-28 9.76E-13 2.655 3.895E+39 1.33E-13 0.85 1.09E-28 1.59 1.101E+40 0.189 1.26 9.39E-14 1.058E+40 0.77 4.62 1.698E+40 0.61 4.09E-29 2.99E-13 2.81E-26 1.264 3.78E-11 7.06E-28 6.346E+40 0.67 3.82E-13 5.85 1.304E+38 0.80 1.655 1.109E+40 0.74 .2493+820 .9-35.80E-28 6.19E-13 5.07E-26 8.84E-14 2.03 4.933E+38 0.72 0.0538 8.74E-29 3.343E+39 0.44 8.28E-14 2.245 2.337E+40 0.51 5.83E-29 7.41E-14 9.76E-28 2.455 3.85E-28 6.42E-13 1.563E+40 0.63 1.83E-12 2.455 1.430E+40 0.49 8.19 1.182E+39 0.95 .7502+8041 .5-23.53E-27 3.12E-27 5.15E-12 6.83E-14 0.4115 5.022E+38 0.57 0.239 1.01E-28 9.085E+39 0.53 8.14E-14 0.574 2.699E+40 0.65 9.87E-29 5.84E-14 1.36E-28 1.6455 3.11E-13 8.951E+39 0.38 11.455 2.200E+40 0.86 .3747+8472E1 1.01E-26 7.21E-12 4 7.437E+38 0.63 6.20E-29 6.09E-14 2.235 1.852E+40 0.57 7.99E-29 5.99E-14 7.69E-28 12.425 1.45E-12 1.175E+41 0.28 3.765 2.084E+40 1.49 .5433+924 .0-28.99E-28 1.10E-12 2.43 4.323E+39 1.35 1.04E-28 110E-13 0.8125 1.019E+40 0.54 7.89E-29 9.71E-14 2.89E-28 2.875 8.10E-13 1.868E+40 0.62 2.005 2.889E+38 1.60 .5957+718 .8-23.41E-27 1.68E-12 1.81 9.577E+37 0.65 6.01E-29 5.90E-14 3.595 1.144E+40 0.41 4.79E-28 1.05E-12 2.045 8.913E+38 1.66 .5290+728520E1 2.03E-27 2.03E-12 2.815 2.910E+37 0.45 1.99E-28 1.83E-13 5.62 1.605E+40 0.77 .4244+874531E1 2.73E-27 3.11E-12 7.485 2.434E+38 0.54 2.36E-28 1.38E-13 5.46 5.148E+40 1.03 .5153+033 .2-32.19E-28 4.02E-13 3.38 1.583E+40 1.15 .7220+0030 .3-47.46E-28 6.43E-14 0.3505 2.240E+40 0.37 .7106+012557E1 3.76E-29 5.73E-14 1.285 1.066E+40 0.47 .1122+015560E1 6.30E-29 6.08E-14 1.535 1.252E+40 0.41 .9254+032531E1 3.37E-28 3.12E-13 3.225 2.584E+40 1.29 .3813+975 .8-23.11E-27 4.78E-12 7.52 8.163E+39 1.63 .2621+929 .2-31.79E-28 1.32E-13 2.98 6.271E+39 0.92 .1112+044512E1 1.48E-28 1.28E-13 4.435 1.192E+40 0.91 .6237+003854E1 4.70E-29 5.40E-14 0.308 2.367E+40 0.56 .2158+024581E1 6.58E-29 8.16E-14 2.405 1.598E+40 0.82 . .2E4 .4 .2-43.90E-29 7.72E-14 3.245 1.828E+40 0.5 . .2E4 .417E1 1.96E-28 1.79E-13 2.34 5.526E+40 0.9 7 7 7 7 7 7 7 ...... AL (CONTINUED) 1 TABLE 7 7 7 7 7 7 7 µ µ µ µ µ µ µ m m m m m m m Wm (W Wm (W m (W Wm (W Wm (W m (W m (W − − − − − − − 2 2 2 2 2 2 2 EQW ) EQW ) EQW ) EQW ) EQW ) EQW ) EQW ) 7 7 7 7 7 7 7 ...... 7 7 7 7 7 7 7 µ µ µ µ µ µ µ m m m m m m m ( ( ( ( ( ( ( µ µ µ µ µ µ µ )Fu(I)( m (W Flux(FIR) m) )Fu(I)( m (W Flux(FIR) m) m (W Flux(FIR) m) )Fu(I)( m (W Flux(FIR) m) )Fu(I)( m (W Flux(FIR) m) m (W Flux(FIR) m) m (W Flux(FIR) m) − − − − − − − 2 2 2 2 2 2 2 F ) F ) F ) F ) F ) F ) F ) 1 1 1 1 1 1 1 ...... GHz 4 GHz 4 GHz 4 GHz 4 GHz 4 GHz 4 GHz 4 Wm (W Wm (W m (W Wm (W Wm (W m (W m (W 7E-25 − − − − − − − 2 2 2 2 2 2 2 Hz Hz Hz Hz Hz Hz Hz − − − − − − − 1 1 1 1 1 1 1 ) ) ) ) ) ) ) © Copyright 2013: Instituto de Astronomía, Universidad Nacional Autónoma de México 0 IUR-.&RAMOS-P. & HIGUERA-G. 304 te airtosfrtert fsa omto using formation star of 7.7 two rate the introduced for (2007) (2012) calibrations al. other Rike et & Maiolino Diamond-Stanic Recently, and 2007). carriers al. molecular et their (Yong modify or with destroy linked may AGN shocks from 2012). or Rike strength photons & high-energy field However, Diamond-Stanic radiation 2002; (Peeters UV the of surement I-I niao,adcluaethe calculate and indicator, MIR-FIR respectively. luminosities, (PAH) bon nodrt osrc w e igotcdiagrams. diagnostic new two construct to order in ad xrce yu rmteSizrdatabase. Spitzer the PAHs from the us and by NRAO, satellite, extracted from IRAS bands the continuum from radio continuum the sam- IR instru- the different the from table, came this ments: and in heterogeneous shown is As ple 1. Table in marize h aai tlctx hwuprlimits. upper show text italic in data The G191001 .8E3 0.02525 0.122 0.02015 0.0862 4.083E+38 0.01223 4.891E+39 0.08765 3C48 9.131E+38 3.045E+39 0.11 6.972E+38 0.51 1.590E+40 0.37 0.28 0.02285 0.28 0.24 3.182E+38 PG1351+640 PG1119+120 0.34 PG1115+407 PG0007+106 PG2349-014 PG1426+015 PG1302-102 PG1229+204(Mrk771) 4194 NGC C505 .5E4 0.10945 1.053E+41 0.55 0.0287 0.03 0.033065 0.0219 1.496E+39 1.280E+38 4.580E+38 1.449E+38 0.37 0.46 3C79 0.48 3C65 0.52 PG1613+658(Mrk876) PG1612+261 PG1534+580 PG1448+273 PG1404+226 4676 NGC G100902 .0E3 .27 .0-45.64E-29 2.50E-14 0.02375 1.102E+39 0.24 3C84 PG2130+099 4818 NGC C7 .5285+600517E1 1.30E-24 1.66E-25 5.70E-26 1.78E-14 4.49E-15 2.87E-14 0.055 0.0302 0.06 2.825E+36 0.000257 8.945E+35 4.527E+36 0.75 3.180E+37 0.22 1.05 0.14 3C293 3C274 3C272.1 3C270 3C249.1 7252 NGC C4 .3387+80.0171 0.0195 0.0126 0.03238 3.817E+38 0.1064 1.637E+36 1.928E+38 0.0344 1.071E+39 0.53 0.12005 7.048E+39 0.55 0.53 2.553E+39 0.28 1.317E+39 0.08 0.49 0.1 3C445 3C386 3C382 3C381 3C330 3C323.1 3C303.1 7714 NGC G 1614 NGC SSQAA C log(L12 3CR QSOS-QUASAR SSQAAsP log(L12 PG QSOS-QUASARs nti ae,w ecieteetmto fan of estimation the describe we paper, this In h aaydt olce o hswr r sum- are work this for collected data The µ ,ad11.3 and m, trus log(L12 Starburst .TESML N SOURCES AND SAMPLE THE 2. µ oyylcaoai hydrocar- aromatic polycyclic m − − − − − − − − − − − − / / / 6)L L60) 6)L L60) 6)L L60) .1399+9036 .6-43.07E-28 0.0522 3.76E-14 4.006E+40 0.34 9.46E-28 0.3965 3.979E+39 0.01 1.07E-12 1.935 1.484E+39 0.67 .4407+9002529E1 3.66E-29 2.96E-14 0.07533 7.999E+39 0.09 0.03245 2.46E-28 4.017E+39 0.14 1.52E-13 3.325 3.494E+39 0.69 .3917+6001232E1 2.15E-25 3.20E-13 0.00122 9.167E+36 0.13 4.28E-28 9.89E-13 0.892 1.970E+38 0.62 .9205+906815E1 3.84E-26 1.56E-14 0.688 2.055E+39 0.19 2.31E-28 2.18E-13 1.92 3.191E+39 0.52 .8755+811 .7-36.18E-28 5.17E-13 1.17 7.515E+38 0.68 .7475+919514E1 1.29E-27 1.48E-12 1.945 4.715E+39 0.67 7 7 7 . . . 7 7 7 µ µ µ m m m q Wm (W Wm (W Wm (W AL (CONTINUED) 1 TABLE parameter − − − 2 2 2 EQW ) EQW ) EQW ) 7 7 7 . . . 7 7 7 µ µ µ m m m ain t1,2,6 n 100 and 60 25, obser- 12, far-infrarred at and vations mid-infrarred 0.001878 The between 0.55. range and a have galaxies The rgtrta .4J t60 objects at extragalactic Jy all 5.24 of than sample (RBGS), brighter limited in Sample contained flux- Galaxy objects Bright a of Revised list IRAS complete the the of sample o.Fnly h A esrmnswr extracted were measurements Cata- PAH Source the the Faint Finally, contains IRAS the NVSS log. in The galaxies 1998). of majority al. et (Condon the Condon (NVSS) from Survey 1992; GHz, Sky 1.4 VLA se- NRAO of we complete densities objects, flux IR of corrected subsample lected same Wada the & of For sam- Imanishi presence 2004). the The 2003; by (Imanishi biased Malkan, 2003). starburst be Rush, nuclear to al. expected 1992; not et are Burg Sanders ples & Moshir 1993; Huchra 1989; Spinoglio 1990; & al. et catalogues Soifer al. IRAS 1984; et in al. condensed et are (Neugebauer data These Satel- Astronomical lite. Infrared the by surveyed sky tire ( ( ( µ µ µ )Fu(I)( m (W Flux(FIR) m) )Fu(I)( m (W Flux(FIR) m) )Fu(I)( m (W Flux(FIR) m) .4-41.68E-28 1.14E-14 .4-54.57E-26 8.84E-15 .9-42.82E-29 9.19E-28 1.51E-26 2.54E-29 6.68E-27 2.63E-29 2.49E-14 1.76E-14 1.25E-14 1.53E-14 1.55E-14 1.18E-14 .2-52.92E-26 4.51E-29 2.82E-29 2.52E-15 2.63E-29 1.29E-14 6.98E-15 9.38E-15 .5-41.51E-25 3.85E-14 .5-52.20E-26 3.05E-15 .9-45.79E-26 6.54E-26 5.16E-26 3.79E-26 6.57E-26 2.25E-26 2.29E-14 3.34E-15 7.32E-15 3.66E-15 8.91E-15 3.40E-15 .2-59.68E-30 8.92E-15 .3-51.77E-26 6.53E-15 − − − 2 2 2 F ) F ) F ) 1 1 1 . . . µ µ GHz 4 GHz 4 GHz 4 ,cvrn h en- the covering m, ,cm rmasub a from came m, Wm (W Wm (W Wm (W − − − 2 2 2 Hz Hz Hz − − − 1 1 1 ) ) ) © Copyright 2013: Instituto de Astronomía, Universidad Nacional Autónoma de México aais eegopdtgte ne h label the under together grouped here galaxies, in s h aa(C)o h pte Heritage Spitzer the of 5.3–14 (BCD) using data (SHA) Archive observa- the These use observations. tions satellite Spitzer from yMrym,Mui aiuh (2000), Taniguchi & adopted Mouri, that Murayama, to by MIR similar criterion the a in following emissions FIR, and the between differences find to of ( resolution low (LL) hsrao,w en h measure For the activity). define we stellar reason, or this (AGN origins and possible clouds represents molecular their of spectra, states far-infrared temperature and different mid- near-, the can conclusions major obtained. and be work, galax- this of for types selected different ies the of sub- particularities behav- and the the ior about complete, information statistically useful provide are samples samples the not infor- Although all 2MASS. The and database the from Simbad-VizieR features. Database-NED, selected PAH Extragalactic data NASA/IPAC the the with get complemented was to mation order by in extracted The galaxies us (2007). the show al. parentheses et of Yong in Burg work values and the (2006) 93 & from and al. taken Huchra PG et QSOs Schweitzer (14) and (1993), 108 quasars (2000); 3CR al. (16) al. et Clavel et 53 and (1992) Rush and Vie- (2003), 1 Rodr´ıguez-Ardila & gas (2004), Seyfert subsample Wada (2003), (27) & Imanishi second by Imanishi 41 published a galaxies published of and 2 Seyfert galaxies (2006), (47) composed starburst AGNs al. (16) of et 20 Brand et Imanishi by (2007); ULIRGs- and (5) (2006) Imanishi al. 7 (8) by y 12 published ULIRGs-Sy1 Sy2, ULIRGs-LINER, (4) (21) se- 7 LIRGs 24 ULIRGs-HII, (9) and (2006); (2006) 14 Maloney Imanishi & Dudley, galaxies: Imanishi, from emission lected IR typical of et (Smith 2007a,b). continuum emis- underlying PAH al. its of to behavior spectrum, relative overall MIR sions algo- the the an on of PAHFIT, focuses decomposition and which the set, for data pix- BCD rithm damaged images, the of from spectral mask els default a creates BCD which the spec- IRSCLEAN, using reconstructing environ- for cubes IDL method tral a the CUBISM, in algorithms ment: three using tracted ∼ The ti elkonta h msincniumin continuum emission the that known well is It composed subsample one of consists sample The 3.7 ′′ L n 10.5 and .TEMRFRINDICATOR MIR-FIR THE 3. 1.0 ausfrqaasadSyet1 Seyfert and quasars for values (12.60) L (12 , 0 log = 60) ′′ epciey h aawr ex- were data The respectively. R ∼ 0)mdlswt widths with modules 100) h ASADTEANSABRTCNETO 305 CONNECTION AGN-STARBURST THE AND PAHS L L µ (60 (12 S)ad14–40 and (SL) m µ µ L m) m) 1,0 norder in (12,60) i . Type µ (1) m qiaetwdhfrtecntuto fanwdi- new a of 2). (Figure construction diagram the agnostic for width equivalent n a-Reisos o h 7.7 the For mid-IR emissions. the far-IR between and differences significant showing h o afo h iga,wietebto half bottom the while diagram, the of half top the hi ereo ula ciiya ela oassess we to formation, the as star well selected with as associated activity contribution nuclear the of degree their sections. following the in alternatives discussed two These be will (a2). present nuclei are galactic activity 2007) active stellar in of al. stages et different (Yong or emissions (a1), di- X-ray are intense bands by PAH luted the either explanations: possible sample. our validation in formation differences statistical star observed provides the of test for existence KS the the the of Considering activity, tracer a emissions. is as PAH there latter the i.e., in hypothesis, isotropy null the no rejects also test the and n efr aais n h eut r shown are for P-values results The the and 2. Table galaxies, in 2 Seyfert and nodrt xlr hsbhvo,w ple the applied we to behavior, test this (KS) explore Kolmogorov-Smirnov to order In yteAN r oiatin dominant are heated mid- AGN, dust and the the consistent near- from is the by spectra in 1), (NIR-MIR) emissions (Figure that infrared galaxies fact the 2 with and in 1 observed Seyfert also galaxies, ULIRG-LIRG-Starburst o h te e fglxe:sabrt IG and range LIRGs the starburst, in lie galaxies: values of the ULIRGs, set other the for i.1. Fig. 1 viewed be can figure color LIRG The starburst, are online. galaxies. quasars 2, and Seyfert ULIRG galaxies the and 1 from Seyfert differentiated The well analysis. the in aais h auslebetween lie values the galaxies,

i nterange the in lie , Sources nodrt eaaetesml fglxe by galaxies of sample the separate to order In two have test KS the in found anisotropies The h eaainbetween separation The 10 15 20 0 5 L (12 L -1.5 Type 1Quasars-3CR Type 1Quasars-PG Type 1Seyfert Type 2Seyfert Type ULIRG Type Starburst Type LIRG 1,0 itga ltfralglxe included galaxies all for plot histogram (12,60) µ m)/ L 1,0 ai n h 7.7 the and ratio (12,60) L -1.0 (60 log[L(12 − µ 0 . )rjc h ulhypothesis, null the reject m) 3t .5 o l efr 2 Seyfert all For 1.05. to 63 -0.5 µ m)/L(60 ye1 Type ye1 Type L − 0.0 (12 0 µ . µ 2ad05,while 0.53, and 92 -A emissions m-PAH ye1 Type m)] µ bet n the and objects ye1 Type − bet occupy objects m), 1 . 0.5 3ad0.5. and 63 L µ (60 PAH m objects. objects 1.0 µ m) © Copyright 2013: Instituto de Astronomía, Universidad Nacional Autónoma de México IG n LRs hspteni u odiffer- to 12 due at emissions is observed pattern the galaxies, in This ences starburst ULIRGs. 2, and Seyfert LIRGs by occupied mainly is RAMOS-P. & HIGUERA-G. 306 saglx iharltvl on tla popula- stellar young relatively 1097 a NGC ( with 253. tion NGC galaxy and a 2) is Figure in labeled (not samples 1 Seyfert of 11% present. and Moreover, also 2, are Seyfert LINERs galaxies. the of ULIRGs of 78% and 43% located starburst are all ASFR and the In in (ASFR). as located us region particular box by a denominated square delimits quadrant The mainly right lower 2C the galaxies. Class starburst occupied and by composite are galaxies by activity) 1A-2A 1B-2B (AGN/SB Classes Classes AGNs, (2007), diagram, unobscured al. by our et Spoon in by defined but regions the to spond (2000). al. et Murayama by rived 0905 separates 1049-005, of values higher At LRsadsabrtglxe ntedarm val- the diagram, within the 253 in NGC galaxies and starburst 1097 and ULIRGs NGC of particu- a position AGN The is weak lar a 253 2010). and NGC (M¨uller-S´anchez starburst al. 2007); strong coexist et a al. which et in galaxy (Mason source heating the dust is Prieto, of which 2005; 2005), Reunanen al. & Maciejewski, et (Storchi-Bergmann nucleus the yANadselratvt.A oe ausof values lower At activity. heated stellar are L and clouds intermediate molecular AGN at the while by ratio, 2008), the of body al. values black et warm a (Pope produces emission and nucleus active the eaue ewe 05 Hs ta.20) The 2003). al. et (Hass lowest K 30–50 between peratures l Fgr )adi qa otesprto value ( separation galaxies the 2 to Seyfert and equal 1 is Seyfert and between 2) (Figure ple 1,0 h trcmoethasteds ttem- at dust the heats component star the (12,60) nteAF perteLNR:NC1097 NGC LINERs: the appear ASFR the In corre- 2 Figure in shown lines vertical dotted The ∼ L 10 1,0 au,ascae ihteqaa PG quasar the with associated value, (12,60) 6 er) tadsac esta cfrom pc 9 than less distance a at years), y 35 347 Reject 0.574095 Reject 53 0.975215 0.283724 1.306E-8 Reject 0.228102 5.2752E-35 53 1 5.30404E-37 0.228102 Reject 1.9598E-17 0.681925 Result 0.228102 p-value 53 Critical D Sy2 1 Type log[ α Test K-S ye1 Type L - ETDN OVER DONE TEST K-S 1,0,teds shae by heated is dust the (12,60), ciesa omto region formation star Active 6 6 6 57 0.05 169 0.05 169 0.05 169 0.05 rmters ftesam- the of rest the from L (12 µ µ ) log[ m)] n 60 and m − 0 . ) de- 6), YE1 TYPE µ L m. AL 2 TABLE (60 µ ) log[ m)] N EFR GALAXIES. 2 SEYFERT AND amn h ut hc srflce ntesmaller the in for reflected responsible for is values which factor dust, the group, the is ULIRG-starburst warming component the stellar In the galaxies. 2 Seyfert ettecnium ovsteoeetmto nthe in ob- overestimation every the 7.7 for solves continuum, adjusting the and ject tool PAHFIT the using (2000). fPHi 7.7 in new measurements PAH our with of and observations diagram IRAS (2007) from diagram data Spoon this Additionally existence the AGNs. the complements in validate activity to star diagram of the the confirms galaxies area, of Seyfert this usefulness in some appear that formation fact star with The zone). (ASFR LRs(SRrgo)adteohrof other starburst- the in of and sample consisting region) the one (ASFR separates objects, ULIRGs it of groups field; two this to tribution factor. dominant diagram, the (2007) is Spoon absorption the which in of local- area 3B and an region (2008), the al. in ized et star- Hatziminaoglou extinguished by cat- “heavily IRAS burst” as the classified in also object alogue, luminous The most intense 1998). the Ponman is with & second (Read system ex- radio triple and in bright infrared, a tremely the is in superluminal first formation, The star ULIRG-LINER and interact- 220. 2623 two Arp NGC ASFR, the appear, of systems half ing lower the In ceased. psd fwihbegan recent which most of the starburst, episode the intense of an was few there a AGN within of that found distribution and stellar galaxy et nuclear this Davis the frame); resolved ASFR (2007) 3227 the of al. NGC limit galaxy, upper 1 the in in Seyfert Also (just the heating, nucleus. appears dust active region the of this of cause role the the minimizes as and formation star idates h iga fFgr sa rgnlcon- original an is 2 Figure of diagram The µ A qiaetwdhsonb lvle al. et Clavel by shown width equivalent PAH m L (12 L 1,0,adtevle fPH7.7 PAH of values the and (12,60), , 0]log[ 60)] µ .Fnly u pcr extraction, spectra our Finally, m. ∼ L 0Mrao u a now has but ago, Myr 40 (7 . 7 µ m)] ye1 Type µ m - © Copyright 2013: Instituto de Astronomía, Universidad Nacional Autónoma de México qaebx ttergt ensthe defines right, the at box, square fselratvt stesoeo h orlto be- correlation the of slope the quantifier A is 1985). activity stellar al. et of Jong (de source emissions the radio are of stars super- young massive while of stars, explosions massive nova by heated dust of mission diinlsucsfo cwizre l 20)adYn ta.(07.Teclrfi color The (2007). al. et Yong and (2006) al. et Schweitzer from sources additional au .5(adr iae 96 o trus aais h ih lesym blue light labeled The line galaxies. dotted starburst blue for The 1996) Mirabel estimations. & (Sanders 2.35 value h apehsaredshift a has sample The i.3 (26)idctrpotdaantthe against plotted indicator L(12,60) 3. Fig. the of plot Diagnostic 2. Fig. h nrrdeisosaelreydet h ree- the to due largely are emissions infrared The .TEFRRDOCORRELATION FIR-RADIO THE 4.

log[L(12 µm)/L(60 µm)] Log[L(12µm)/L(60µm)] -1.5 -1.0 -0.5 0.0 0.5 1.0 -1.5 -1.0 -0.5 0.0 0.5 1.0 1A 2A z ewe .013 o h trus C32 n .5frterdosuc C3.Teviol The 3C330. source radio the for 0.55 and 342, IC starburst the for 0.000103, between Type 13CR Type 1PG Type Starburst Type LIRGs Type ULIRGs-S2 Type ULIRGs-S1 Type ULIRGs-HII Type ULIRGs-Liner Type 2Seyfert Type 1Seyfert ASADTEANSABRTCNETO 307 CONNECTION AGN-STARBURST THE AND PAHS L Type LIRG Type starburst Type ULIRG-Liner Type ULIRG-HII Type ULIRG-Sy2 Type ULIRG-Sy1 Type 2Seyfert Type 1Seyfert Type 13CR Type 1PG (12 -2 -3 µ ASFR m)/ RR q L 3C273 A (60 q ein h oo gr a evee online. viewed be can figure color The region. Log[EW(7.7 A PG1049-005 -1 µ ( q − )lmnst ai safnto fte7.7 the of function a as ratio luminosity m) IRAS 13451+1232 aaee.Terddte iemre ihtelabel the with marked line dotted red The parameter. 1 -2 . 8 ersnstema falvalues all of mean the represents 38)

q Mrk1014 NGC4151 parameter 0 µ aaee Hlu ofr oa-oisn1985; 1992), Rowan-Robinson Condon & or Soifer, emission (Helou, far-infrared parameter and emission radio tween Mrk231 IRAS 17179+5444 m-PAH) -1 Mrk 3 2B 1B 3C231 q 1 PG1351+236 ≡ NGC4151 PG1351+640 log µ NGC6240 3C293 PG0157+001 NGC6240 NGC7714 m] F osrpeetqaaswt pe limit upper with quasars represent bols GreaterPAHemission 0 ν Mrk273 (1 F NGC 2623 2 FIR . uecnb iwdonline. viewed be can gure Mrk 273 H)Wm GHz)(W 4 PG2130+099 ARP220 q / (3 S PG1119+120 < q . NGC253 NGC253 75 µ ARP220 NGC4418 A qiaetwidth. equivalent PAH m .Tegahcincludes graphic The 0. × NGC4418 1 3

1C

2C 10

Warm dust continuum dust Warm − continuum dust Hot 12 2 Hz) Hz q − S 1 ) hw the shows , (2) et q © Copyright 2013: Instituto de Astronomía, Universidad Nacional Autónoma de México 0 IUR-.&RAMOS-P. & HIGUERA-G. where 308 and where 100 (Jy). adr iae 19)etbihd sn IRAS using established, a (1996) observations, Mirabel 1994). Volk & pop- & stellar Sanders Lisenfeld, older Xu, 1992; to (Condon younger ulations from increase to tends e ihecs ai msina G candidates. AGN as (2008) emission radio galax- identify excess al. to with correlation et ies F(1.4Ghz) Sabater FIR, a and used formation, star intense n odds (60 dust ac- mid-infrared cold between discriminated and intensity, are emission sources to On the cording emission. axis, dominant vertical the the by sample the separate the region vertical indicating mation the drawn, is along frame sample a the axis of distribution the ing nrrdeiso rgt.Tedse ielabeled line far- dashed the The radio in (right). dominance strong emission with infrared with those those and (left) into emission separated are objects oe ecnutdarve fthe of review There- a conducted 2001). we Condon radio-FIR fore, & the Reddy, by (Yun, predicted value correlation the luminosity than radio the greater which is forma- in (AGNs) star those strong and have tion that sources between inator niao safnto fthe of function a as indicator nomsiebakhlslctdi in litcl is 10 ellipticals than giant in less located holes black massive onto Region Radio u ape iue3sostegaho the of graph the shows 3 Figure sample. our 1910adP 1009lei h einwith region the in lie 2130+099 positive PG and 1119+120 Mirabel & Sanders by determined (1996). value the shows hw,alresml fglxe i nteregion the in lie galaxies of with sample also associated diagram large the con- a as the However, shows, AGN. increasing the of of to expense tribution falls the formation at star post- of mid-infrared, sequence, contribution evolutionary the an where of IR, repre- part they last that the suggest sent and sources three these cuss RmsAmia20) hsgahi particularly is graph heating dust This and 2009). formation Almeida star reduc- (Ramos of and activity ad- it cooling In the gas, ing the 2011). ionize jets al. radio et dition, (Dicken activity formation star FIR tlwI uioiis h vrg au of value average the luminosities, IR low At nti otx,the context, this In nFgr ,treQO:P 3160 PG 1351+640, PG QSOs: three 3, Figure In F µ ≡ FIR adflxdniismaue nJanskys in measured densities flux band m F F 1 60 . ν q 26 stefrifae u acltdas, calculated flux infrared far the is 14Gz steflxdniya . GHz, 1.4 at density flux the is GHz) (1.4 aaee.Fra ta.(09 lodis- also (2009) al. et Farrah parameter. µ × − m 10 3 R) nrdoglxe,teaccretion the galaxies, radio In (RR). and M ra h otdlnsa h origin the at lines dotted The area. − q q 14 ⊙ au qa o23 o bet with objects for 2.35 to equal value aaee values parameter µ F (2 yr ) ntehrzna xs the axis, horizontal the On m). 100 . − 58 1 q µ F n hscniinrestricts condition this and , aaee sas discrim- a also is parameter m 60 r h RS60 IRAS the are µ m q + aaee.Follow- parameter. F 100 q < ciesa for- star Active ,hr called: here 0, aaee for parameter µm m W ) L µ (12,60) and m − (3) 2 q , q s tog14Gzeiso rma ciencesde- nucleus negative with active region The an new a from fines LIRGs. emission GHz and 1.4 ULIRGs strong starbursts, for (as- holds type GHz that galaxy 1.4 events) at -type with emission far- sociated the the and between emission relationship infrared the validates rameter lte gis h qiaetwdho h 7.7 the of width equivalent the against plotted efr ,o h etsd fteAF region, ASFR an the and of formation side star nucleus. of left active coexistence the 3227, the on NGC validates and 1, middle Seyfert the side, in a right LINER, the on a relative AGN, 1027, weak The NGC a 253, NGC method. of our position of power the demonstrates discriminatory this the and in similar, galaxies is of space used parameter distribution study the one, studies, each our this though of including all even in 2006; Nevertheless, 2009), variables. al. different et Koulouridis al. 2003; et al. Farrah et Haas 2001; al. (Storchi-Bergmann et authors previous of sampling the remaining dominant. the is for component while, AGN dust, the responsi- of galaxies, heating factor the dominant for the the ble that is verifying component region, galaxies stellar ASFR (AGN ULIRG-starburst the activity The in of concentrate formation). source star and discriminating or strength for tool by original galaxies an is emission, PAH ience ihlwselractivity. ac- stellar ques- are low they final open with that nuclei a an confirms tive are graph is the they scenario However, not evolutionary tion. or an Whether of di- stage not literature. are presented the scenarios RR evolutionary in The region the to radio linked the clouds. rectly in dense located with sources associated intense with emissions those from FIR material galax- density low radio with noisy ies highly discriminating for suitable trh-egane l 20) ase l (2003), (2009). al. by et al. suggested Haas et location Farrah (2001), sequences relative evolutionary al. its et the Storchi-Bergmann and of of scenario one predominance other in the the determines or ac- galaxy one dominant a The in diagrams. tivity diagnostic the in exist bet,acrigt hi ee fnceractivity, nuclear of surveys. of identification observational level large the their in for to useful like according is diagram, objects, This one, lower. previous is the ac- galaxies stellar radio the for There, (PG) tivity quasars located. the are ULIRG-SY2 of a some and sources, radio 3CR where h igotcdarmof diagram diagnostic The with overlap study this in sampled galaxies The h igotcdarm nwhich in diagram, diagnostic The h cnro a)ad(2,pooe in proposed (a2), and (a1) scenarios The .CONCLUSIONS 5. q L aus(einRR) (region values 1,0 vs (12,60) L 1,0 is (12,60) § q ,co- 3, µ pa- m © Copyright 2013: Instituto de Astronomía, Universidad Nacional Autónoma de México nre eieRmsPdla eatmnod ´sc,Fcla eCiencias, F´ısica, de de Facultad Departamento Padilla: Andr´es Ramos Felipe ai rad iur azo:Osraoi srnoioNcoa,Facult Astron´omico Garz´on: Nacional, Observatorio Higuera Armando Mario M., Elitzur, C., Packham, A., N. 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