1987ApJ. . .321. .233E The AstrophysicalJournal,321:233-250,19S7October1 © 1987.TheAmericanAstronomicalSociety.Allrightsreserved.PrintedinU.S.A. near-infrared wavelengths(A<10/mi;cf.Rieke1978,here- first far-infrareddetectionsofasignificantnumberactive after R78),theInfraredAstronomicalSatellite(IRAS)all-sky survey at12,25,60,and100/mionlyrecentlyprovidedthe galactic nuclei(AGNs).EdelsonandMalkan(1986,hereafter tral energydistributionsofaheterogeneoussample of EM) usedIRAS,IUE,andground-baseddatatostudyspec- 29 AGNsbetween0.1and100/mi.Miley,Neugebauer, and galaxies. Neugebaueretal.(1986)reportedIRASobservations wavelength), andEdelson(1986,hereafterE86)analyzedIRAS Soifer (1985)reportedthatfar-infraredcolorsof120active (1986), ImpeyandNeugebauer(1987),othershavestudied of 179quasars(ofwhich74weredetectedinatleastoneIRAS observations ofthebrightestPG/BQSquasars.Landauet al. of itstotalenergyatinfraredwavelengths. Insomecases,thisis the broad-bandpropertiesofblazars. the resultofpresence dust.Thedustcanabsorband by theUniversityofHawaiiundercontract totheNationalAeronauticsand Space Administration. 2 1 Although Seyfertgalaxieshavebeenstudiedextensivelyat Virtually everyknownSeyfertgalaxyemitsalargefraction VisitingAstronomerattheInfrared TelescopeFacility,whichisoperated PresidentialYoungInvestigator. Thus, thenear-andmid-infraredemissionfrommostSeyfert1galaxiesappearstobedominatedbynon- thermal radiation,althoughdustradiationisclearlyimportantforothers. is predominantlythermalinSeyfert2galaxiesandnonthermalquasars.Foropticallyselected1 spectra ofopticallyselectedSeyfert2galaxiesaresteep(a._=-1.56),insharpcontrastto of 48Seyfertgalaxies.Mosthavecompleteinfrareddetections,butnoneweredetectedat1.3mm.The selected quasars,whichhaveflatinfraredspectra(â_=—1.09).Thissuggeststhattheemission galaxies, a._=-1.15,and-70%haveflatspectrasimilartoquasarsunlikeSeyfert2galaxies. dominated byunreprocessedradiationfromasynchrotronself-absorbedsourceoftheorderlight-dayin shortward of100/un.Fortherelativelydust-freeSeyfert1galaxies,thissuggeststhatinfraredemissionis size, aboutthesamesizeashypothesizedaccretiondisks.ForSeyfert2galaxiesandotherdusty In manyoftheobjectswithundetectedturnovers,emissionfromcooldustingalacticdiskappearsto objects, itimpliesminimumdusttemperaturesof35-65K,significantlywarmerthaninnormalgalaxies. mask theturnover.Thisstrong“coolexcess,”whichdominates60-100/miemissionfromtheseobjects,is Subject headings:galaxies:Seyfert—infrared:spectraquasarsradiationmechanisms correlated withthe11/misourcesize,suggestingthatSeyfertnucleitendtoresideingalaxiesundergoing 225/an 2 25Aim strong starformation. 225/im © American Astronomical Society • Provided by the NASA Astrophysics Data System Observations between1.2jumand1.3mmarepresentedforanunbiased,spectroscopicallyselectedsample Half oftheobjectsdetectedatthreeormoreIRASwavelengthshavefar-infraredspectrawhichturnover BROAD-BAND PROPERTIESOFTHECfASEYFERTGALAXIES.II.INFRAREDTO I. INTRODUCTION radio sources:galaxies—spectrophotometry Owens ValleyRadioObservatory,CaliforniaInstituteofTechnology Department ofAstronomy,UniversityCalifornia,LosAngeles Received 1986November14;accepted1987March18 Steward Observatory,UniversityofArizona MILLIMETER PROPERTIES 1,2 M. A.Malkan R. A.Edelson ABSTRACT G. H.Rieke AND a thermally reradiateasignificantportionoftheopticaland ward atshorterwavelengths,owingtotheWiencutoff*below emission producesaverysteepspectrumwhichcurvesdown- ultraviolet continuum(RiekeandLebofsky1979).Thethermal the peakwavelengthofemissionfromhottestsurviving dust grains.Thermalfar-infraredemissionisalsofrequently associated withdustreddeningofthenuclearemissionlines steepness oftheinfraredspectraandinternalreddening and and nonstellarcontinuum.EMfoundcorrelationsbetween other dustindicators. continua bynonthermalprocesses.Inthecaseofviolentlyvari- the infraredandhighpolarizationconclusivelydemonstrate able quasarsandBLLacertaeobjects,therapidvariability in infrared spectra(ImpeyandNeugebauer1987).Inquasars and this (AngelandStockman1980).Theyalsotendtohave flat infrared (andoptical)emissionislessdirect,sincethecontin- luminous, unreddenedSeyfert1nuclei,thecasefornonthermal uum isneitherhighlypolarizednorviolentlyvariable. The strongest indicationisthe relatively flatshapeofthefar- infrared toopticalcontinuum, whichiswelldescribedbya power lawwitha>—1.3(F ocv,EM).Opticallyselected which wereidentifiedaspredominantly nonthermalemission. quasars haveflatinfraredspectra (â_^=—1.09E86), The correlationfoundbetween the3.5gmand2keVX-ray v 2i25 However, someactivegalacticnucleiproducetheirinfrared 1987ApJ. . .321. .233E uum emissionisdiscussedin§III,andthefar-infrared cussed inthenextsection.Thenatureofinfraredcontin- was incorrectlyclassifiedasaSeyfert2galaxyinPaperI). also describedtheirradioproperties.(Oneobject,NGC3227, discussed indetailEdelson(1987,hereafterPaperI),which tion effectsduetodustcontent.Theselectionofthesampleis by ultravioletexcess,thissamplehasnoknownbiasesorselec- and studyatotherwavelengthsaswell.Unlikeobjectsselected optical brightness,theseobjectsarerelativelyeasytodetect contains 26type1and222Seyfertgalaxiesselectedby optical spectroscopy(HuchraandBerg1987).Becauseoftheir deduce thepropertiesofclassasawhole.TheCfAsample well-defined, unbiased,spectroscopicallyselectedsample—to spectral energydistributionsoftheCfASeyfertgalaxies—a problem wasavoidedbyexaminingtheinfraredtomillimeter to biassamplesagainststronginfraredemitters(R78).This example, selectionbyultravioletexcess(suchasthatused mechanisms. PreviousAGNstudieshavebeenbiasedbythe Markarian 1972andSchmidtGreen1983)hasbeenshown selection techniquesusedtoconstructtheirsamples.For are studiedtodeterminetheimportanceofdifferentemission unbiased, spectroscopicallyselectedsampleofSeyfertgalaxies emission fromtheseobjectsisnonthermalinorigin(Malkan galaxies) suggeststhatthesameprocessisresponsibleforemis- sion atbothwavelengths,implyingthatthelowerfrequency flux ofquasarsandSeyfert1galaxies(butnot2 1984). 234 The near-infrared,IRAS,andmillimeter-wavedataaredis- In thispaper,theinfraredpropertiesofacomplete, © American Astronomical Society • Provided by the NASA Astrophysics Data System NGC 7682 Mkn 533 2237+07 NGC 5940 NGC 5929 1614+35 Mkn 686 IC 4397 NGC 5674 Mkn 461 NGC 5273 Mkn 266 NGC 5252 Mkn 789 NGC 5033 NGC 4388 1335+39 Mkn 766 NGC 4235 NGC 3982 Mkn 744 NGC 3362 NGC 3079 Mkn 1243 NGC 1144 0152+06 1058+45 Mkn 573 Mkn 993 0048+29 Mkn 334 a Source Mkn817hasameasured10pmflux densityofSio.e=220+38mJy. 11.0 ± 10.1 ± 11.3 ± 11.1 ±0.8 15.7 ± 12.9 14.6 ± 44.1 ± 11.6 ± 30.8 ± 23.1 ± 21.1 ± 31.0 ± 19.8 ± 22.0 ± 12.2 ± 13.8 ± 11.1 ±1.114.51.415.61.5 14.3 ±0.720.81.027.51.4 3.6 ± 4.4 ± 6.9 4.0 ± 7.7 ± 5.6 ± 9.2 ± 5.8 ± 5.8 ± 6.0 ± Sl.2fim (mJy) 0.5 0.6 0.2 1.1 0.3 0.6 0.8 1.3 0.5 0.5 1.0 0.5 3.5 1.0 2.0 2.0 2.0 0.9 2.0 0.5 2.2 0.6 2.4 0.4 2.0 0.6 EDELSON, MALKAN,ANDRIEKE CfA SeyfertGalaxyNear-InfraredData 14.9 ± 15.6 ± 17.8 ± 15.7 ± 25.0 ± 19.5 ± 17.4 ± 61.6 ± 48.5 ± 12.0 ± 42.6 ± 35.4 ± 25.9 ±2.0 71.3 ± 29.4 ± 29.5 ± 19.0 ± 6.8 ± 6.8 ± 7.4 ± 8.8 ± 8.1 ± 7.8 ± 6.8 ± 7.4 ± 8.0 ± (mJy) 0.8 0.9 1.4 0.7 0.5 0.5 1.0 1.4 1.0 1.5 0.6 0.6 1.0 1.0 5.0 2.5 3.0 3.0 4.0 0.6 0.7 3.0 0.5 3.0 0.7 24.2 : 19.4 : 15.8 23.1 16.1 13.4 47.8 46.9 16.1 50.1 29.9 27.8 12.4 91.9 ± 31.5 ± 26.3 ± 16.0 ± 9.5 ±0.9 6.9 : 8.7 : 6.3 8.7 7.9 7.3 5.2 ± 7.9 ± 7.4 ± TABLE 1 ^2.2nm (mJy) ± 1.0 2.4 0.7 0.6 1.0 0.5 0.9 0.8 1.0 0.9 0.6 1.5 0.5 3.0 2.5 4.0 2.4 2.4 0.5 5.0 0.8 3.6 1.2 0.5 2.4 0.8 to providenear-infrareddataforatotalof44objects(95%), Devereux, Becklin,andScoville1987;Neugebaueretal1987), with thoseavailableintheliterature(R78;Rudy,LeVan,and Rodriguez Espinosa1982;Cruz-GonzalesandHuchra1984; also madeatL(3.5/mi)or(3.6/mi),and12objectswere infrared (1.1—2.2/mi).Measurementsof13brightobjectswere observed atN(10.6/mi).Theseobservationswerecombined etry wasobtainedfor29oftheSeyfertgalaxiesinnear- Campins, Rieke,andLebofsky(1985).Newinfraredphotom- (2.2 /mi)wereused,withabsolutefluxcalibrationsfrom The usualphotometricbands,J(1.2/un),JT(1.6/mi),andK Catalina 61inch(1.55m)reflectorandtheIRTF3mtelescope. single-element InSbdetectorsontheStewardObservatory nosity distanceorforevolution. corrections weremadeforcosmologicaleffectsinthelumi- is assumed.Asthelargestredshiftinthissamplez=0.06,no given intheAppendix. six SeyfertgalaxieswhichwerenotincludedinPaperIare of themajorresultsthispaperisgivenin§VII.Positions investigated in§V,andthe60fiminfraredluminosityfunction of Seyfertgalaxiesisderivedanddiscussedin§VI.Asummary red propertiesandthosederivedatotherwavelengthsare emission arediscussedin§IV.Therelationshipbetweeninfra- turnover andtherelationbetweenfar-infraredmillimeter 1- Near-infrared photometrywasobtainedwithstandard < 15 Throughout thispaper,avalueofH=75kms"Mpc 0 : 15 46 ± 16 ± 43 ± 16 ± 74 ± 22 +2 31+3 73+6 23 ± 10 ± $3.5 (im (mJy) 7 ± 3 <144 < 53 < 32 325 ± 288 ±28 210 ±20 158 ±34 167 ±15 82 ±12 SlQ.6(xm 18+4 (mJy) a) Near-InfraredData 25 15 Mar84 15 Mar84 04 Mar85 04 Mar85 04 Mar85 04 Mar85 04 Mar85 04 Mar85 13 Sep84 15 Apr84 04 Mar85 II. DATA 04 Mar85 16 Apr84 14 Apr84 15 Apr84 14 Apr84 15 Mar84 21 Dec86 26 Sep85 16 Sep84 13 Sep84 Mar 86 Mar 86 Mar 86 Mar 86 Mar 86 Mar 86 Mar 86 Date Vol. 321 1987ApJ. . .321. .233E No. 1,1987 measurements at3.5/¿mfor28objects(58%),and10.6/mi data for29objects(60%). galaxies. Sourcenamesarepresentedincolumn(1).Fluxden- Table 1weremeasuredwith8"5apertures.Thustheyrefer tains thedateofJ,if,andKobservations.Severalrepeated are presentedincolumns(2)-(6),respectively.Column(7)con- light, andtherewasoftensignificantGalacticlightoutsidethe primarily tothenucleus.InlessluminousSeyfertgalaxies, observations agreedtowithinabout10%.Thefluxeslistedin sities anduncertaintiesfortheJ,H,K,L,Nmeasurements these fluxesalsoincludeasubstantialcontributionfromstar- least oncebyIRAS.Twoobjects(NGC3362andMrk774)lay aperture. Table 1givesthenewnear-infrareddataforCfASeyfert Forty-six ofthe48CfASeyfertgalaxieswereobservedat © American Astronomical Society • Provided by the NASA Astrophysics Data System b) IRASData I Zw1 0048+29 Mkn 334 Mkn 335 NGC 4051 NGC 3982 Mkn 744 NGC 3516 0152+06 Mkn 573 Mkn 993 NGC 5033 Mkn 231 NGC 4388 Mkn 205 Mkn 766 NGC 4235 NGC 4151 NGC 3362 NGC 3227 NGC 3079 Mkn 1243 NGC 1144 NGC 1068 Mkn 590 NGC 5252 Mkn 789 IC 4397 Mkn 266 1058+45 Mkn 279 Mkn 461 NGC 5273 Mkn 270 NGC 5674 NGC 5548 1335+39 Mkn 817 Mkn 686 NGC 5929 Mkn 841 2237+07 NGC 5940 NGC 7682 Mkn 530 NGC 7469 Mkn 533 1614+35 Source S^m(mJy)^25^mSQmSioo/m»¿>1.2 0(i INFRARED PROPERTIESOFSEYFERTGALAXIES < 70 < 121 < 146 < 119 < 85 < 109 < 82 < 80 C 103 38300 ±2300 2080 1820 1000 1250 ± 1300 341 ± 212 ± 431 457 104 540 ± 780 828 384 562 ± 307 ± 306 186 ± 198 ± 130 169 ± 343 132 357 199 134 360 164 128 720 198 124 140 180 93 CfA SeyfertGalaxyFar-InfraredandMillimeterData ± 101 104 109 130 42 46 44 44 34 38 34 47 78 40 60 29 35 32 75 25 34 38 37 40 37 32 31 32 30 33 42 42 30 < 102 < 144 < 174 < 160 < 167 < 78 < 80 < 72 88600 ±5210 4600 2040 ±122 8560 3370 1260 ± 1070 ± 1430 1420 1750 ±175 1240 5500 ±550 1570 1930 ±231 420 ± 806 ± 755 680 ±52 247 ± 610 995 922 ± 976 138 ± 242 453 289 198 ± 273 765 168 151 392 112 191 ±56 80 ! ± : ± ' ± : ± ± 70 ± 38 ± ± ± ± 230 514 214 126 142 106 22 41 99 76 44 73 89 84 57 34 38 62 27 44 60 37 45 70 89 32 52 TABLE 2 186000 ±18600 42400 ± 33300 ± 10700 ± 13600 ± 26700 ± 4310 ± 4010 ± 2130 ± 6720 ± 8160 ± 6730 ± 5400 ±288 8030 ± 3720 ± 7320 ± 1200 ± 1840 ±107 1070 ± 2340 ± 9450 ± 1680 ± 1200 ± 1630 ± 1110 ± 5470 ± 414 ± 435 ± 467 ± 260 ± 931 ± 290 ± 374 ± 425 ± 631 ±60 328 ± 443 ± 991 ± 476 ± 605 ± 117 ± 481 ± 794 ± 900 ± 856 ± in the~2%ofskywhichIRASdidnotobserve.One 46 objectsobserved(NGC7682)laywithin4'ofa10Jysource, lengths. and couldnotbedetectedowingtostrongconfusion.Allofthe remaining 45objectsweredetectedwithIRAS,and32ofthe46 were measuredignoringallobservationsinwhichasourcewas tabulated incolumns(2)-(5).Forobjectsbrighterthan0.5Jyat source namesaregiveninthefirstcolumn.Thefluxdensities objects observed(70%)weredetectedinallfourIRASwave- mined fromsourceextractionsperformedonco-addedsurvey not detected,objectswithlowsignal-to-noiseratiostendto and errorsat12,25,60,100/mi,or3<7upperlimits,are IRAS fluxesforobjectsfainterthan0.5Jyat12/miweredeter- appear brighterthantheyactuallyare.Forthisreason,all Catalog (1985).SincetheIRASPointSourcefluxes 12 /mi,photometrywastakenfromtheIRASPointSource Far-infrared fluxesfromIRASarepresentedinTable2.The 3330 5950 1310 1070 3740 232 298 242 336 816 683 784 221 396 491 110 104 766 134 49 49 46 80 38 60 61 53 55 93 87 39 56 80 50 50 79 63 87 76 50 79 239000 ±23900 <323 < 350 < 257 42400 ± 20400 ± 30100 ± 87600 ± 17300 ± 15200 ± 16900 ± 11300 ± 10400 ± 34400 ± 12000 ± 4660 ± 2430 ± 5060 ± 8600 ± 2160 ± 2630 ± 5330 ± 1990 ± 2030 ± 1240 ± 1270 ± 1210 ± 3130 ± 1310 ± 1530 ± 1020 ± 1420 ± 2260 ± 3560 ± 1970 ± 1800 ± 2140 ± 8190 ± 1800 ± 1820 ± 1270 ± 1790 ± 736 ± 750 ± 456 ± 4360 3010 2440 2860 2370 8760 1550 1150 1090 6190 1450 1220 494 430 243 250 571 532 300 239 248 225 136 168 211 345 164 183 174 173 242 382 130 195 162 208 214 106 205 254 186 1350 1281 1431 1230 1185 1131 1041 1548 1296 1473 1269 1098 1050 (mJy) 462 468 465 852 699 933 456 834 930 342 318 537 744 495 309 591 915 672 816 900 615 738 564 615 306 735 765 801 762 822 903 585 768 303 507 235 1987ApJ. . .321. .233E an aan with “Q”orundeterminedspectra andsteepfar-infraredspec- (dusty orsteep)incolumn(6) (see§IIIc).Inaddition,sources spectra areclassifiedwitha“Q” (quasar-likeorflat)“D” the spectralindices«2.2-25^ dao„,theinfrared greater thanthisvaluearelabeled witha“C.”Onthebasisof unity arelabeledwitha“E” in column(5),whilethosewithR column (4)(see§IIW).SourceswithRmorethan3abelow measure ofthedegreeresolutionat~11/un)ispresented in marked withan“R.”Thecompactnessparameter(R, a a “B”incolumn(3),whilethosewithweakexcesses are mediate types(i.e.,Seyfert1.5galaxies)areclassifiedastype 1. Using slitspectroscopyoftheinner10"(EdelsonandWahl 12 Gm Seyfert galaxytype,takenfromHuchraandBerg(1987).Inter- Column (1)containsthesourcename,andcolumn(2) the 1/2 1987), sourceswithstrongultravioletexcessesaredenoted are presentedincolumns(2)-(6),respectively. 2.2-25 /xm?12-60,ini>5-60|imJ60-100/ím>d^iOO mm Column (1)containsthesourcename,andspectralindices tral indiceshavebeencalculatedandtabulatedinTable3. less luminousAGNshaveabumpinthenear-infrareddueto spectra. frequency turnoverisdetectableinabouthalfoftheinfrared starlight whichpeaksnear~1.5/mi.Afar-infraredlow- steep (a^-2,asinMrk533andNGC1968)toflat> wide varietyofspectralshapesandfeaturesareseeninFigure 1. Theoverallspectralenergydistributionsrangefromvery —0.7, asinMrk335and590).Thespectraofmanythe column (6)ofTable2. were detectedat1.3mm.The3aupperlimitsarelistedin of précipitablewatervaporalongthelinesight.Nosources time, thetimeofdayanobjectwasobserved,andamount The actualerrorswereastrongfunctionoftheintegration about 15minutes,yieldingtypical1aerrorsof~200mJy. scope hada30"beamwidth,andthepointingwasaccurateto effective noise-equivalentfluxdensityof-5Jys.Thetele- sideband). Theapertureefficiencywasabout15%,givingan typical systemtemperatureof~325Konthesky(double NRAO-Kitt Peak12mtelescopeon1984June9-16.The QMC-Oregon 0.3Kmillimeterbolometerwasusedwitha IRAS fluxobservedfromthisinteractingsystem.Theseobjects ~ 10".Mostsourceswereobservedforintegrationtimesof only 90"fromNGC5930,whichappearstoemitmostofthe line spectrum(KollatschnyandFricke1984).NGC5929is are excludedfromfurtheranalysis. nucleus, whilethecompanionhasalow-ionizationemission- galaxy (separation9").OneofthegalaxieshasaSeyfert2 a nearbyspiralcompanion.Mrk266isactuallyclosebinary appears extendedintheIRASbeambecauseitisonly41"from and 60¿zm15%at100jum. overall calibrationuncertaintyisestimatedtobe10%at12,25, because theseobjectshadpower-lawslopesneara=-1.The data. NospectralcorrectionstotheIRASdatawerenecessary, 236 Table 4containsparametersderivedfortheseobjects. To quantifythefollowingdiscussionofspectralshapes,spec- Figure 1containsvFplotsfortheCfASeyfertgalaxies.A v The CfASeyfertgalaxieswereobservedat1.3mmwiththe The infraredfluxesofthreeobjectsareconfused.Mrk279 © American Astronomical Society • Provided by the NASA Astrophysics Data System III. THEINFRAREDCONTINUUMEMISSION c) MillimeterData a) Introduction EDELSON, MALKAN,ANDRIEKE a and causes thespectrumtocurve downward steeplyfromthemid- to thenear-infrared. ^ range oftemperatures(EM). The high-frequencyWiencutoff by thesuperpositionofthermal emissionfromdustgrainsata “ dusty”anddenotedbyaD.” denoted bya“Q”inTable4andFigure2.Anyspectrumwith their indexsteeperthanthese boundary valuesisdesignatedas i2—óo/tm ^-1.25isdesignatedas“quasar-like,”and is § Ilia,anyinfraredspectrumwith«2.2-25^^-1.37 and selected quasarshavea._>-1.37and > segregates Seyfert2galaxiesfromquasars.Alloftheoptically distribution ofa_,evenstronger. «2.2—25 ftm^—1.37anda_>—1.25,whichcompletely removal ofthiscomponentwouldmakethedifferencein the ponents at2.2pmthanSeyfert1galaxies(see§Illb). The tively. Seyfert2galaxiestendtohavestrongerstellarcom- and type2Seyfertgalaxiesatthe99%97%levels,respec- «2.2-25 „m«12-60^distributeddifferentlyfortype1 parameter indifferenttypesofobjects(Siegel1956)showsthat -1.25, unlikeanyoftheSeyfert2galaxies.Asdiscussed in ^12—60 pm1.55+0.36.ThenonparametricKolmogorov- Smirnov (K-S)testfordifferencesinthedistributionofasingle 225/im160|im 2 25(m the Seyfert2galaxies,ä_=-1.56±0.34and «2.2—25„m =-1.15±0.29andôi_-1.080.44.For and â_,=—0.69+0.44.ForSeyfert1galaxies, 1260iim ^2.2—25 pm1.09+0.16(rmsscatterforindividualobjects) For bright,opticallyselectedquasars,E86foundthat object whichliesonthedottedlinehasa,, circles, andbrightPGquasars(takenfromE86)bystars.An Seyfert 1galaxiesaredenotedbytriangles,2 diagram. Figure2isaplotof._versus„ 2 5fim 1260lim 1260(m galaxies usuallyhavesteeper,curvedspectra. fitted byasimplepowerlaw.AscanbeseeninFigure1,Seyfert 225flm160m warm dustisasteep,curvedspectrum.EMfoundthatobjects usually hadsteepinfraredspectra(a«-2),whicharenotwell with largeinternalreddeningsandotherdustindicators sion tendstoproduceflat,smoothspectra.Thesignatureof 1 galaxiestendtohaveflat,power-lawspectra,whileSeyfert2 nucleus haveverydifferentspectralshapes.Nonthermalemis- systematic studyofthisfeaturewiththesedata. lack ofuniformcoveragebetween3.5and10/anpreventsa detectable insomespectra,asdiscussedbyEM.However,the fifth component,abroadbumpcenterednear5/an,isclearly component withasharplong-wavelengthcutoffnear80/an.A the nucleus);and(4)arelativelyflatnonthermalpower-law lying galaxy;(3)emissionfromwarmdust(probablycloseto far-infrared emissionfromcooldustinthediskofunder- starlight, whichisonlyimportantshortwardof3.5/an;(2) no companionshavean“N”(see§Vb). interacting objectshavean“I”incolumn(8),whilethosewith axies canbeexplainedasamixtureoffourcomponents:(1) (7) (see§IIIc).OnthebasisofDahari’s(1985)observations, flux duetonuclearnonstellaremissionarepresentedincolumn “(D)” appendedtothisclassification.Estimatesofthe2.2/an 1.2 /an-1.3mmspectralenergydistributionsofSeyfertgal- tral indices(a_<-Uoraioo^j,,,,,,^—2.0)havea The steepinfraredspectraof Seyfert 2galaxiesareproduced 2560/im The dashedlineinFigure2delineatesaregionwith This differencecanbeseenmosteasilyinacolor-color Thermal dustemissionandnonthermalfromthe As discussedinEM,themajorfeaturesofobserved b) InfraredSpectralShape 1987ApJ. . .321. .233E except fortheSeyfert2galaxies. objects atthetop.DataareplottedaslogvFvs.v,soahorizontalline would havea=—1(i.e.,equalpowerperoctaveoffrequency).Forthepurposedisplay sigma errorbarsareshown,andafactor of2isshownatthelowerleftforscale.Anarbitraryscalingconstant addedtothedatafordisplaypurposes,(b)Sameas(a) only, theIRASdataaregrayshifted by thecompactnessparameter{R),discussedin§IIIc,toaccountfor effectsofemissionfromtheunderlyinggalaxy.One v Fig. 1.—(a)PlotsofvFat1-100/zmfortheCfASeyfert1galaxies.The objectsarepresentedinapproximateorderoftheultravioletexcess,withbluest v © American Astronomical Society • Provided by the NASA Astrophysics Data System Frequency (Hz) Frequency (Hz) Fig. la 1987ApJ. . .321. .233E infrared spectraofmanyobjects. Continuumemissionfrom nated bythermalemission. suggesting thattheinfraredspectra oftheseobjectsaredomi- percent oftheSeyfert1galaxiesoccupy“dusty”region, the dominantmechanismformostSeyfert1galaxies.Thirty axies isgoodevidencethatthermaldustemissiondominates emission. ThisclearspectraldivisionfromtheSeyfert2 gal- the spectraofSeyfert2galaxies,whilenonthermalradiation is “ quasar-like”regionofFigure2,indicativeflatpower-law 238 Starlight makesasubstantial contributiontothenear- Seventy percentoftheSeyfert1galaxieslieinupperright © American Astronomical Society • Provided by the NASA Astrophysics Data System c) Starlight Frequency (Hz) (Hz) EDELSON, MALKAN,ANDRIEKE Fig. lb meaningful informationabout thestellarpopulationitself. to obtainabetterestimate of thespectrumnuclear source. Instead, thegoalistoremove its contributionsofaraspossible starlight tothespectrainthese objects.Thesedatagivelittle native methodshadtobeusedestimatethecontribution of Filippenko 1983;McAlaryandRieke1987).Therefore,alter- stellar andcompactnuclearsourcecomponents,butsuchdata aperture measurementscanbeusedtoseparatetheextended a Rayleigh-Jeansfallofftolongerwavelengths.Detailedmulti- galactic stellarpopulationspeaksnear1.5/miandhasroughly are availableforonlyafewobjectsinthissample(Malkan and The starlight-correctednuclear fluxwasestimatedat2.2/¿m Vol. 321 1987ApJ. . .321. .233E No. 1,1987 was performedwiththestellar spectrumandapowerlawwith estimates areindicatedbya “b” inTable4.Wherethespec- limit equaltothefluxat Kbandwasassigned.These detected fluxmightarisefrom thenuclearsourceandanupper Table 4.ComparisonwiththeuncorrectedKfluxesin 1 fit wasperformedusinganunreddenedstellarspectrum with the galaxieswhereJHKLdatawereavailable,aleast-squares because therearevirtuallycompleteJHKdataonthesample trum peaksatHorislevelbetween HandK,aleast-squaresfit spectrum rosefrom//toX, itwasassumedthatallthe these objects.WhereonlyJHKdatawereavailableand the shows thatstarlightcorrectionscanbeimportantinmany of to optimizethefit.Theseestimatesareindicatedbyan“a ”in and apowerlawwithspectralindexthatwasallowedtovary normal colors(i.e.,J—H—0.7,HK=0.2,andK—L 0.2) at Kforthesedata.TheseestimatesarelistedinTable4. For and theratioofnucleartostellarfluxisexpectedbelargest spectral indexa =—1.Ifthederivednuclear fluxwaslessthan © American Astronomical Society • Provided by the NASA Astrophysics Data System I Zw1 Mkn 590 0152+06 Mkn 993 0048+29 NGC 3362 NGC 3227 NGC 3079 Mkn 1243 NGC 1144 NGC 1068 Mkn 573 Mkn 335 Mkn 334 NGC 7682 Mkn 533 Mkn 530 2237+07 IC 4397 NGC 3516 NGC 7469 Mkn 817 NGC 5674 NGC 5548 NGC 4051 NGC 3982 Mkn 744 NGC 5940 NGC 5929 Mkn 841 Mkn 686 Mkn 279 Mkn 461 NGC 5273 NGC 5252 Mkn 789 Mkn 231 NGC 4388 Mkn 205 Mkn 766 NGC 4235 NGC 4151 1614+35 Mkn 270 Mkn 266 NGC 5033 1058+45 1335+39 Source > - > - > - > -I > -I • -0.75 -0.89 ±0.05 -1.27 ±0.06 -1.70 ±0.06 -1.77 ±0.03 -0.75 ±0.11 -1.38 ±0.04 -1.31 ±0.04 -2.23 ±i -0.84 ±i -1.57 +- -1.24 ± -1.00 -1.06 ±0.10 2.11 ±0.05 0.76 ±0.07 0.80 0.90 ±0.12 0.69 0.72 ±0.10 <*2.2—25/xm 0.90 0.97 0.66 0.98 1.27 1.27 ±0.06 1.25 1.41 ±0.05 1.24 ±0.06 1.13 ±0.05 1.29 ±0.06 1.28 ±0.03 1.51 ±0.04 1.32 ±0.03 1.17 ±0.07 1.11 ±0.05 1.31 ±0.10 1.05 1.95 1.26 INFRARED PROPERTIESOFSEYFERTGALAXIES 1.83 1.25 1.61 ± i ± ' ± 0.05 ± ' 0.09 0.12 0.06 0.05 0.06 0.11 0.07 0.09 0.05 0.05 0.05 < -1.07 < -1.20 < -0.81 < -0.03 < -0.82 < < -0.73 < -1.99 : -0.65 : -0.88 : -0.55 CfA SeyfertGalaxySpectralIndices -1.26 -0.97 -1.88 -1.16 -1.78 -0.98 -0.59 -1.12 -0.85 -1.15 -2.03 -0.55 -0.97 ±0.07 -0.98 ±0.15 -1.65 -2.19 -1.00 -0.12 -1.87 -1.17 -1.58 -0.73 -1.45 -1.12 -1.24 -1.97 -1.30 -1.74 -1.81 -1.47 -1.39 0.63 0.73 1.46 1.67 <*12-60/im ± 0.06 ± 0.07 ± 0.18 ± 0.14 ± 0.09 ± 0.13 ± 0.11 ± 0.09 ± 0.12 ± 0.14 ± 0.11 ± 0.07 ± 0.09 ±0.17 ± 0.14 ± 0.06 ± 0.11 ± 0.09 ± 0.07 ±0.06 ± 0.14 ± 0.09 ± 0.13 ± 0.10 ± 0.07 ± 0.07 ± 0.04 ± 0.16 ± 0.08 ± 0.15 ± 0.07 ± 0.07 TABLE 3 : -0.74 : -0.70 : -1.25 : -0.91 ; -2.08 ; -2.24 : -0.16 : -0.96 -2.37 -0.85 -0.65 -0.45 -0.60 -2.18 -1.59 -1.19 -1.71 -1.80 -0.95 -1.74 -3.47 -2.24 -2.05 -0.06 -2.50 -0.73 -2.04 -0.43 -1.32 -1.47 -1.18 -0.43 -2.00 -2.75 -1.63 -1.50 -1.61 -2.30 -2.11 -2.07 -2.99 -1.55 at -0.79 ±0.10 -1.32 ±0.22 0.02 makes theJ—Kcolorredder. increasingly dominantnucleusraisesthe12/anluminosity and nonparametric Spearmanrankcorrelationtest(Siegel1956) and Filippenko(1983)McAlaryRieke(1987). these methodsarenotexpectedtobeveryaccurate,theresults 20% ofthetotalatK,anupperlimitKflux was «25-60^m ^o.45—6o umthe98%confidencelevel.Asexpected, an shows thatthereisanegativecorrelationbetweenL and tion betweennuclear(12fim)luminosityanda_. The are generallyinroughagreementwiththosefoundbyMalkan assigned. Theseestimatesareindicatedbya“c.”Although and canconfuse thedeterminationofinfrared spectrumof some degreeintheinfraredspectra ofallnormalspiralgalaxies 12tim 0 4560Mm The importanceofstarlightcanalsobeseeninthecorrela- Thermal emissionfromdustin thegalacticdiskispresentto ± 0.21 ± 0.31 ± 0.19 ± 0.18 ± 0.14 ± 0.19 ± 0.31 ± 0.30 ± 0.09 ± 0.17 ± 0.16 ± 0.16 ± 0.10 ± 0.13 ± 0.26 ± 0.10 ± 0.09 ± 0.18 ±0.16 ± 0.17 ± 0.13 ± 0.25 ± 0.13 ±0.13 ± 0.33 ±0.10 ± 0.08 ± 0.35 ± 0.20 ± 0.10 ± 0.24 ± 0.13 ± 0.16 ± 0.13 ± 0.29 > -2.67 > 1.06 > 0.31 -0.79 -1.79 -0.50 -0.67 -2.57 -1.62 -0.47 -2.13 -2.22 -0.49 -2.32 -1.91 -0.31 ±0.23 -1.73 ±0.31 -1.46 -1.42 -1.45 -0.11 -3.01 -0.26 -1.49 -0.15 -1.53 -0.95 -1.22 -0.46 -0.48 -1.79 -1.59 -0.97 -0.06 -1.40 -0.94 -2.95 -1.33 -0.69 -1.11 -1.76 -0.70 -2.23 <*60-100/im 0.07 0.20 d) ExtendedInfraredEmission ± 0.21 ± 0.27 ± 0.21 ± 0.28 ± 0.37 ± 0.35 ± 0.30 ± 0.24 ± 0.33 ± 0.33 ± 0.42 ± 0.46 ± 0.33 ± 0.29 ± 0.27 ± 0.24 ± 0.25 ± 0.33 ± 0.22 ± 0.50 ± 0.29 ± 0.28 ± 0.22 ± 0.42 ± 0.26 ± 0.23 ± 0.23 ± 0.28 0.44 0.29 0.44 0.32 0.30 0.27 0.36 0.23 0.48 0.14 0.33 0.28 ^lOO/im —1.3mm > 0.51 > 0.16 > -0.47 > 0.70 > 0.04 > > 0.17 > 0.85 > 0.50 > 0.45 > -0.08 0.79 0.46 0.17 0.27 2.53 0.55 0.24 0.09 0.33 0.46 0.30 0.19 0.56 0.94 0.38 0.17 0.15 1.41 1.01 0.52 0.06 0.37 0.96 0.09 0.12 1.16 1.91 1.17 1.42 1.70 1.69 1.25 239 1987ApJ. . .321. .233E errors intheground-basedand IRASphotometry. ments anddonotappearto sufferconfusionwithnearby greater spatialextent.Forexample,sevenofthe38CfASeyfert objects. TheuncertaintyinR wasestimatedbycombiningthe the 22galaxiesinsamplewhich havetherequisitemeasure- as R,the“compactnessparameter.” ItislistedinTable4for This comparisonissimplifiedbythefactthatSeyfertgalaxies ments madewithsmallbeams(typically6"-9"indiameter). starlight canbeseparatedfromnuclearemissionbyitsmuch usually havelittlespectralstructure at10.6gm(Aitkenand the activenucleus.Thisthermalemissionfromdustheated by Roche 1985).Theratioofground-based toIRASfluxisdefined ed structureonangularscalesof>20"at12/un(IRASPoint solved byIRASbutcanbeidentifiedcomparingthe Source Catalog1985). galaxies intheIRASPointSourceCatalog(18%)showresolv- 12 gmmeasurementswithground-based10.6/immeasure- 240 In moredistantgalaxies,thegalacticemissionmaybeunre- © American Astronomical Society • Provided by the NASA Astrophysics Data System NGC 7682 Mkn 533 Mkn 530 NGC 7469 2237+07 NGC 5940 NGC 5929 1614+35 Mkn 841 Mkn 686 Mkn 817 IC 4397 NGC 5674 NGC 5548 Mkn 279 Mkn 461 NGC 5273 Mkn 270 Mkn 266 NGC 5252 Mkn 789 NGC 5033 Mkn 231 NGC 4388 Mkn 205 1335+39 Mkn 766 NGC 4235 NGC 4151 NGC 3982 NGC 4051 Mkn 744 NGC 3516 NGC 3362 NGC 3227 NGC 3079 Mkn 1243 1058+45 NGC 1144 NGC 1068 Mkn 590 0152+06 Mkn 573 I Zw1 Mkn 993 0048+29 Mkn 335 Mkn 334 Source TypeUVX 2 2 1 2 1 1 2 1 1 2 2 1 2 1 2 1 2 2 2 1 1 2 1 2 1 1 2 1 1 2 1 1 1 1 2 1 2 2 1 1 2 2 2 1 2 1 1 1 R B B B R B R B R B R B B B B R R R B R R B B R R R B B R B B R R R R R B B R R B R R R B B B B EDELSON, MALKAN,ANDRIEKE CfA SeyfertGalaxySpectralParameters : 0.11 0.65 ±0.11 0.53 ±0.16 0.72 ±0.09 0.85 ±0.28 0.76 ±0.15 1.03 ±0.23 1.10 +0.15 0.07 ±0.03 0.61 ±0.05 0.82 ±0.12 0.94 ±0.06 0.55 ±0.06 1.23 ±0.15 0.84 ±0.13 0.70 ±0.06 0.22 ±0.03 0.59 ±0.14 0.66 ±0.05 0.81 ±0.10 1.07 ±0.27 0.78 ±0.18 R TABLE 4 Extent SEDNuclearFlux(mjy)Interacting E E E C C C C C E E C E E E E c c C -1 extrapolate the12gmmeasurements to10.6gm. to theIRAS12and25gm measurementsandusingitto wavelengths oftheIRAS and ground-basedphotometric bands. Thiscorrectionwasdetermined byfittingapowerlaw a =—1.Thesecondcorrection allowsforthedifferingeffective This correctionisaweakfunction ofthespectralindexnear to thesamesourcespectrum,theymustbemultipliedby1.22. spectrum. Tocorrecttheground-based10.6/¿mmeasurements assumes colorcorrectionsappropriatetoavpower-law surements ortothenewonesreportedhere.TheIRASsystem tions havebeenappliedtothepublishedSeyfertgalaxymea- (Rayleigh-Jeans ;a=+2)spectraattheeffectivewavelength of calibration givesequivalentmonochromaticfluxesforstellar computing R.First,thecolorcorrectionsinground-based and IRASphotometrymustbereconciled.Theground-based 10.6 /¿m(Rieke,Lebofsky,andLow1985).Nocolorcorrec- Sources withRlessthanunity byatleast3stars.Anobjectwhichliesonthedottedlinehasa_25=«12-00ßm-Thedasheddelineatesregionwith_^>—1.37and > —1.25.All in Seyfertgalaxieswithlessluminous nuclei.Notsurprisingly, sources alsohavesignificantly bluerH—Kcolors,atthe95% shows thecorrelationof12jjmluminositywithR.TheSpear- fied asextended.Theclassificationsoftheseobjectsarenot as compact, andNGC1144,7469,Mrk530wereclassi- low signal-to-noise:Mrk841and2237+07wereclassified as of thequasarsand70%Seyfert1galaxiesliewithinthisregion,all2outside. the extendedinfraredemission ismostcommoninthosegal- reliable astheothers. to beextendedwiththistest.Fivesourceshadclassifications at 2 ßm25m160 ßm vsa The compactnessparameterisausefulindicatorofthepre- Fig. 2.—Color-colordiagramofct.2-2sum*i-eoßm-Seyfert1galaxiesaredenotedbyfilledtriangles,circles,andbright quasarsby 2 © American Astronomical Society • Provided by the NASA Astrophysics Data System INFRARED PROPERTIESOFSEYFERTGALAXIES a 2.^m 25}im 44-1 cannot bedetermined. emission fortheentirecomplete,unbiasedsampleofobjects axies withthelowestredshiftsinthismagnitude-limited from a4xTOergss(10L)energysource.Atthe dis- hence emitstronglyat10pmadistanceofroughly 2 pc observed at10.6pm,thefrequencyofstrongextendedinfrared sample. SincetheseSeyfertgalaxieshavebeenmoreextensively (i.e., >600pc)fromthenucleus.Thissuggeststhat“ E” will reach300Ksignificantlyfartherfromtheenergysource, tance ofthegalaxiesinthissample,2pctypicallycorresponds but anunusualwavelengthdependencewouldberequired to to 0"01.Grainswithrealisticwavelength-dependentemissivity The infraredslopesobserved innormalgalaxieswithhigh galaxies haveanextendedsource ofluminosityinadditionto account fortheemissionin“E”galaxiesfartherthan 3" the activeSeyfertnucleus. rates ofcurrentstarformation tendtobesteeperthanthoseof significant atthe99%confidence level,isshowninFigure3. active galacticnuclei(Miley, Neugebauer,andSoifer1985). 0 with A graydustgrainwillreachatemperatureof300Kand The correlationofa_6om compactnessparameter(R) 12ß 241 1987ApJ. . .321. .233E galaxies havecoolexcesses. cool dust.AllSeyfert2galaxies andabouthalfoftheSeyfert1 galaxies, wherethefar-infrared excessisthermalreradiationby from thegalaxieswithcoolexcesses, thespectraoftheiraddi- tional far-infraredemissionare verysimilartothoseofnormal Within theaccuracyofsubtraction ofaquasar-likecomponent “ quasar-like”nonthermalspectrumarelabeledwitha Q.” “ Q(D),”or(D)”inTable4.Thosewithnoexcessrelative to a “ cool”excessinthe60-100/unregionarelabeledwitha D,” spectra thatmorecloselyresemblequasars. better spatialresolutionwouldshowthatmanyofthe CfA measurements ofextentalsogenerateasignificantportion of parameters arecorrelatedatthe97%and99%confidencelevels,respectively. Conversely, itisexpectedthatfar-infraredmeasurementswith (Persson andHelou1987),soitwouldaccounteasilyforthe Seyfert galaxieswith“D”spectraactuallyhaveflatternuclear their infraredemissionthroughstarformationinthedisks. It issuspectedthatmanyofthe“D”galaxieswithoutdirect correlation ofextendedemissionwithinfraredspectralindex. Much ofthisenergyisgeneratedinthediskgalaxy 242 Fig. 3.—Correlationofcompactnessparameter(R)with12/miluminosityanda_ispresentedinthetopbottompanels,respectively. These 1260 ßm As describedin§Ilia,objectswhichshowevidencefor a © American Astronomical Society • Provided by the NASA Astrophysics Data System e) CoolExcess EDELSON, MALKAN,ANDRIEKE R warmer emissionfromcurrent star-formationregionsthat tends todominateat60pm. Thestrengthsofemissionat12 emission fromthediskthatusually dominatesat100pm,and red spectraconsistoftwocomponents: infraredcirrus-like this resultwillbedifficult. cold infraredexcessesandthereforewillgiveabiasedview of the prevalenceofextendedinfrared emission.Thusextensionof cussed, samplesofSeyfertgalaxiesselectedbyothercriteria measured signal-to-noiseratiobetterthan5.Asalready dis- such asultravioletexcesstendtoexcludegalaxieswithstrong this sample(Mrk334)withIRAS12pmmeasurements a sources. Unfortunately,thereisonlyoneobjectremaining in extension andacoolexcesssuggeststhatmanyoftheother compact. Thisstrongcorrelationbetweendetectablesource Seyfert galaxieswithcoolexcessesarealsoextendedinfrared extended andthree(Mrk573,Mrk766,231) are axies withcoolexcessesandmeasurementsofR,11 are compactness parameters(R),noneareextended.Ofthe14 gal- eight galaxieswithoutcoolexcesseswhichalsohavemeasured the observedextentofSeyfertgalaxiesat11pm.Of Models oftheIRAScolors galaxiesindicatethattheinfra- It isinterestingtocomparethespectralclassificationwith Vol. 321 1987ApJ. . .321. .233E -1 43-10 41-1 8 least sevenadditional objectswith“D”or “Q(D)”spectra more importantthannonthermal emissionintheseobjects.At No. 1,1987 where thecompactnessparametersinTable4aresignificantly polyaromatic hydrocarbonfeaturesinthe12/¿mband.Thus, and 100/¿marecorrelatedbecauseofthepresencestrong less thanunity,thegalaxiesareexpectedtohavestrongcool histogram abovethehorizontallineatiV=0showsluminositydistributionof“D”Seyfertgalaxies. curved lineshowsthefieldgalaxyluminosityfunction(RiekeandLebofsky1986)normalizedtonumberofgalaxiesinCfASeyfert sample.The excess fromtheirdisks. NGC 5674,7469,andMrk533)forwhichthecoolinfra- cantly higherthanwouldbeexpectedfromanunbiasedsample luminosities werecomputedbynormalizingavpowerlaw well removedfromthe“quasar-like” regionofFigure2,pro- red luminositiesaregreaterthan4x10ergss(10 L©). axies (NGC1068,NGC1144,4388,Mrk789,IC4397, of fieldgalaxies.Thisconclusionrestsprimarilyoneight gal- ing luminosityasdescribedbyRiekeandLebofsky(1986).All and Lebofsky1986)inFigure4.Thecoolfar-infraredexcess viding furtherevidencethatthermal emissionbydustismuch amount ofluminosityfromoutside thenucleus.Theyarealso ters areextended,givingdirect evidenceforasignificant All fiveofthesegalaxieswith measuredcompactnessparam- NGC 5929,eachofwhichmaybeconfusedinthelargeIRAS “ Q”galaxiesareexcluded,asMrk266,279,and the 60and100/mameasurements,calculatingremain- to the25fimmeasurementsofgalaxy,subtractingitfrom Seyfert galaxiesiscomparedwiththatoffield(Rieke beam withanearbygalaxy.Thecoldluminositiesofthe infrared luminositygreaterthan6x10ergss(1.5 10 malized insuchawaythatthetotalnumberofgalaxieswith luminosity functionfromRiekeandLebofsky(1986)was nor- remaining galaxiesareindicatedinthehistogramFigure4. Lq) isequaltothetotalnumberofSeyfertgalaxiesin the For thefieldgalaxies,indicatedwithsmoothline, the sample (includingthoserejectedorof“Q”type). 43-1 10 Fig. 4.—Normalizedluminosityfunctionof“D”Seyfertgalaxies.Integratedinfraredluminosities,L,aregiveninunits4x10ergss (10 L).The The luminositiesoftheSeyfertgalaxiestendtobesignifi- The distributionofluminositiesforthecoolexcessesin 0 © American Astronomical Society • Provided by the NASA Astrophysics Data System INFRARED PROPERTIESOFSEYFERTGALAXIES Log(L) 43-1 a anz 43- (Mrk 334,0048+29,Mrk231,133539,NGC5940, 4 x10ergss,althoughforvariousreasonstheluminosity that only1.4galaxiesinthissampleshouldhavefar-infrared of theunderlyinggalaxyislesscertainfortheseobjects. function ofjusta2_o^6-ioo ^-Atzeroredshift,itis given bytheformula (v,) isdeterminedbyfittingaparabolainlogv-logFspace to which risefrom1to~80/mi.However,noneweredetected (100 /¿m)intheobservedframe. EMcontainsadetaileddis- which a=0astheturnover,providedthatv,>3THz spectra oftheseobjects.EMstudiedthisturnoverinaheter- tral turnovermustoccurinthefar-infrared-submillimeter above ~500mJyat1.3mm.Thismeansthatadramaticspec- sources (Sâ:1Jy),withspectralenergydistributions luminous infraredgalaxies,presumablywithhigherthan it appearsthatSeyfertnucleitendtobefoundinrelatively plotted inFigure4isgeneratedthediskofgalaxy.Thus luminosities largerthan4x10ergss\rathereightto cussion ofthismethod.The turnover frequencyisactuallya the 25,60,and100/miIRASdata,takingpoint at seen toturnoverbefore100/mi. selected quasars.Overhalfoftheobjectsinthosestudieswere ogeneous sampleofAGNs,asdidE86foraoptically average ratesofstarformation. 1614 +35/andMrk530)haveluminositiesgreaterthan 15. Inbothcases,itisexpectedthatthebulkofluminosity 56 v 60 The normalizedfieldgalaxyluminosityfunctionpredicts The CfASeyfertgalaxiesaregenerallystrongfar-infrared In EM,E86,andthepresentstudy,turnoverfrequency IV. LOW-FREQUENCYTURNOVER 2.63 —1.71(0C5_6O/im/^60—100 pm) 2 243 1987ApJ. . .321. .233E filled stars.Anobjectwhichliesonthe dottedlinehasa_=.Sourceswithdetectedturnovers lieintheregionaboveandtorightofdashed line. column (1),andturnoverfrequencies(inTHz)in(2). with higherfrequencyIRASdata.Table5containstheturn- detected at100/an(Mrk335andMrk841)weremeasured objects withdetectedturnovers.Sourcenamesaregivenin over frequenciesandotherparametersforthe15unconfused 244 2560Mm60100/im 12.48). Theturnoverfrequenciesoftwoobjectswhichwerenot provided thatthespectrumisconcavedownwardandlogv> t Fig. 5.—Color-colordiagramofa_ vs.a_.Seyfert1galaxiesaredenotedbyfilledtriangles, 2galaxiesbyfilledcircles,andbrightquasars Of the34unconfusedobjectsdetectedatthreeormore 25 6010 Mm © American Astronomical Society • Provided by the NASA Astrophysics Data System NGC 7469 IC 4397.... NGC 3516 NGC 3079 NGC 1068 I Zw1 Mrk 841... Mrk 817... Mrk 461... Mrk 789... Mrk 231... Mrk 766... Mrk 573... Mrk 334... Mrk 335... Source (1) EDELSON, MALKAN,ANDRIEKE 1210 (THz) (10cm)K)(G)(K) 4.0 4.6 4.1 4.5 7.3 5.0 3.9 3.6 3.5 5.1 3.6 3.5 3.0 3.7 7.9 (2) (3)(4)(5)(6) v rTB f5bd Derived TurnoverParameters 22000 9400 2600 3500 5700 8800 8300 3900 3100 1200 1800 1100 1500 720 720 -2 0 TABLE 5 a 60/um 100/xm millimeter region. the dottedlinewouldhavea_=oMm*Sources require thatthespectraoftheseobjectscutoffinsub- overs whichcouldnotbedeterminedbecausetheyapparently occurred longwardof100/¿in.However,the1.3mmlimits ward of100/un.Theother19unconfusedsourceshadturn- IRAS wavelengths,15(44%)hadturnoversdetectedshort- 2560Min61 4.3 4.5 4.3 4.5 4.2 2.4 4.2 3.6 5.2 3.7 2.1 3.7 2.3 3.3 1.8 A Figure 5isaplotof_versuso_ioom-sourceon 260/iin6M 2700 2000 1600 1500 1000 910 400 440 470 490 620 930 880 390 670 44 48 42 47 44 43 44 88 61 97 56 62 36 50 55 18 (10 cm)(M) 0 430 270 360 700 340 150 100 130 120 160 (7) (8) 44 37 58 79 25 2300 2100 1000 940 470 270 680 360 630 520 730 190 100 130 54 Yol. 321 1987ApJ. . .321. .233E 10 10 21 lying galaxy. these objects,thefar-infraredspectrumofnucleusmayturn ably duetocooldustemissionfromtheunderlyinggalaxy.For below thedottedlinehavestrongexcessesnear80¿un,prob- of thedashedlineinFigure5.Sourceswhichliesignificantly with detectedturnoverslieintheregionaboveandtoright over, butitcannotbeseenbecauseofemissionfromtheunder- effect wasnotsignificantwiththeK-Stest. detected, asdidthreeof12redobjects(25%).However,the blue ultravioletcolors(55%)hadlow-frequencyturnovers with Seyfertgalaxytypeortheshapeofinfraredspectrum. No. 1,1987 from asynchrotronself-absorbedsource(asappearstobethe continuum emissionisknown.Ifitnonthermal parameters, whenthemechanismresponsibleforinfrared case inmostSeyfert1galaxies),thenitoccursatthefrequency frequency andultravioletcolor.Twelveofthe22objectswith had detectedturnovers,asdid50%oftheobjectswith“D” galaxies. Thirty-eightpercentoftheobjectswith“Q”spectra detected shortwardof100/mi,asdid42%theSeyfert2 15 spectra. Theremaybeaweakcorrelationbetweenturnover Forty-five percentoftheSeyfert1galaxieshadturnovers galaxies (suchasfree-freeabsorptioninthebroad-lineregion) at whichthesourcebecomesopticallythick.EMshowedthat magnetic field(Æ),andsourcesize(r)canbecalculated(see required toderivesourceparameters.IftheX-rayfluxis are unlikelytobecorrect.Inthiscase,onemoreassumptionis other explanationsoftheturnoverinlow-reddeningSeyfert1 higher frequencies:E86foundthatsixofninequasars(67%) turnovers thanextendedsources.Moreluminousactivenuclei “ C”incolumn[5]ofTable4)aremorelikelytohavedetected (3H5) ofTable5,respectively.Thetypicalinferredbrightness Compton-scattered radiation,thebrightnesstemperature(T) had v,>5THz,whileonlytwoof34theCfASeyfertgal- are alsomorelikelytoshowdetectableturnovers,andat AGNs, theturnovercanbemaskedbysteep-spectrumemis- axies (6%)did.Thisindicatesthat,especiallyinlow-luminosity child radiuscanbeestimatedbyassumingthatthesourceis temperature T*æ3xIOKimpliesasourcesizer« E86 fordetails).Theseparametersaretabulatedincolumns sion fromcooldustintheunderlyinggalaxy. red sourcesizesræ100Schwarzschildradii,thatis,about the accreting attheEddingtonlimit.Thesecalculationsyieldinfra- most compactregionsofradioselectedsources,usingdifferent temperatures andmagneticfieldsarealsoreasonablefor the size ofthehypothesizedaccretiondisk.Thederivedbrightness ness temperaturesof7J,«3x10Karealsofoundin the accretion diskregion.Itisinterestingtonotethatpeakbright- from nucleardust(asappearstobethecaseforSeyfert 2 assumptions (Readhead1986). can beusedtodeterminetheminimumcharacteristicdusttem- perature (7^),size(r)andmass(m).Thesequantitiesare pre- galaxies andsomeSeyfert1galaxies),theturnoverfrequency emissivity €oc1/2isassumed, withmassabsorptioncoefficient s sented incolumns(6)-{8)of Table5,respectively.Adust b9 is alowerlimit.Itcouldbemuch largerifthesourceisoptically size ofthethermallyemitting region(discussedfurtherinEM) k =60cmg"at100/un(Draine andLee1984).Thederived s thin. FormostSeyfert2galaxies, typicalminimumdustsizes s and temperatures ofr«100pcand7^ 50Karefound. d d x 10cmandamagneticfieldB«300G.TheSchwarzs- The turnoverfrequencymaybeusedtodeterminesource There werenotrendsforturnoverfrequencytobecorrelated Objects withcompactinfraredemission(i.e.,thosea If theinfraredcontinuumisdominatedbythermalemission © American Astronomical Society • Provided by the NASA Astrophysics Data System INFRARED PROPERTIESOFSEYFERTGALAXIES -12 a anci s mm upperlimits.ThesourceNGC1068hasa^o/im-i.3^ line regionorthegalacticdisk. This iswarmerthandustinnormalgalaxies(deJongetal. limits whichcanbesetforanyothersourcesare dependence oftheemissivitydust,spectralindices sizes r^100pcsuggestthatthedustresidesinnarrow- ous infraredgalaxiessuchasArp220(Sandersetal1987).The low-frequency sideofthecutofftobequitesharp. for theturnoverintheseobjects,theyalreadyconstrain absorption, isresponsibleforitscutoff.Duetothe22“ sufficiently sensitivetodiscriminatebetweendifferentcauses io/im-i.3mm ^+L5.Whilethemillimeterdataarenotyet a ä—3to—4couldbeexpected.However,themoststringent 1984), butsimilartothetemperatureofdustinhighlylumin- for correlations. All weredetectedat6cm.Thehighdetectionrates(100% axies detectedat60pmwithIRASwerediscussedinPaperI. 6 cmand4500Â,97%at60pm)makesitpossibletosearch tion ofinfraredluminositySeyfert1galaxiesaredenotedby line forSeyfert1galaxies,andbythedotted2 triangles, andSeyfert2galaxiesbycircles.Aproperleast- d galaxies. squares fittotherelationLocLJisindicatedbydashed + 2.53,whichindicatesthatdust,andnotsynchrotronself- fidence level,forbothtypesofSeyfertgalaxies.Assumingthe although thecorrelationappearsstrongerforSeyfert1gal- power-law relationLocLJ,s=0.90+0.10forSeyfert1 two fluxes(SopmS)arecorrelatedatthe99.9%con- axies. TheSpearmanrankcorrelationtestindicatesthatthe integrated opticalluminosity.Seyfert1galaxiesaredenotedby galaxies, whileforSeyfert2galaxiess=1.06+0.14. line forSeyfert1galaxies,andbythedotted2 triangles, andSeyfert2galaxiesbycircles.Aproperleast- fitted regressionlineissteeperthanthatforLversus. The squares fittotherelationLocisshownbydashed weaker. ForSeyfert1galaxies,s=1.73+0.13(significant at corelation intheopticalandinfraredfluxesisalsosomewhat galaxies. correlated withnonthermalluminosity. the opticalandinfraredluminosityoflow-luminositySeyfert galaxies isdominatedbytheunderlyinggalaxy,which not (Paper I),isconsistentwiththehypothesisthatnonthermal s =1.71+0.15(significantatthe99%confidencelevel). The the 99.5%confidencelevel)andforSeyfert2galaxies, steep slopeseeninthisrelation,andtheL-Lrelation radio, infrared,andopticalemissionareallcorrelated,but that mation, leadingtolargeinfrared luminosities(i.e.,Weedman IRad galaxies forthepresenceofclose companiongalaxiesatnearly IRad 6 cm the samplehave close(physicallyassociated) neighboringgal- the sameredshift.Asindicated inTable4,16ofthegalaxies IRrad IRopt 1983). Dahari(1985)hasclassified manyoftheCfASeyfert radopt Table 3containslimitsto,basedonthe1.3 Six centimeterobservationsof39the45CfASeyfertgal- 3 mm L andarecorrelatedforbothtypesofSeyfertgalaxy, Figure 6isaplotofnonthermalradioluminosityasfunc- Figure 7isaplotofinfraredluminosityasfunction A clearcorrelationisalsoseenbetweenLand,butthe irrad It hasbeensuggestedthatinteractions cantriggerstarfor- IRopt V. RELATIONTOOTHERPROPERTIES a) RadioandOpticalLuminosity b) Companions 245 1987ApJ. . .321 . .233E s IRLF. dusty Seyfert2galaxiestoallow theconstructionofareliable method ofselectingSeyfertgalaxies producesasamplewhichis too deficientinhigh-luminosity blueSeyfert1nucleiandin significant limitsforoc_ lieoutsidethisrange.This tifying Seyfertgalaxiesbyselectingobjectswith identified portionsoftheIRASsurveytendtohavearather De Grijpetal.(1985)obtainedaveryhighdetectionrateiden- small percentageofSeyfertgalaxies(RiekeandLebofsky1986). the 40CfASeyfertgalaxies (83%) withmeasuredvaluesor sample ofSeyfertgalaxieswiththeIRASdata.Completely complete infraredsurveysuchastheIRASPointSource (IRLF) oughttobedeterminedfromasampleidentified in a Catalog. However,itisverydifficulttoidentifyacomplete filled circles.Aproperleast-squaresfittotherelationL,ocLforSeyfert1galaxies(forwhichs=0.90),andbydottedline2 (s=1.06). formation inthebodyofgalaxy. 2560fim —0.5 >a25_o—1.25.However,Table3showsthat33 of emission fromcooldust,whichmaybepoweredbynewstar confidence level.The60fimluminosity(L)isalsolargerfor the interactingSeyfertgalaxies,at95%confidencelevel. infrared slopesthantheisolatedSeyfertgalaxiesat95% interacting Seyfertgalaxieshavesignificantlysteeperfar- Evidently thegalaxyinteractionisassociatedwithstronger axies arepresentedinFigure8.TheK-Stestindicatesthatthe tograms ofa_forinteractingandnoninteractinggal- which Daharifoundnocompanionsaredenotedby“N.”His- axies, whicharedenotedby“1.”The15Seyfertgalaxiesnear RTad 6 IR 1260Aim 246 Ideally, theSeyfertgalaxyinfraredluminosityfunction Fig. 6.—PlotofLvs.forthe39objectsobservedat60//mand6cm.Seyfert1galaxiesaredenotedbyfilledtriangles,while2 are denotedby radIR © American Astronomical Society • Provided by the NASA Astrophysics Data System VI. INFRAREDLUMINOSITYFUNCTION EDELSON, MALKAN,ANDRIEKE LerS rad (g/) is givenhere. method isdiscussedindetailPaperI,onlyabriefsummary method suggestedbySchmidtandGreen(1983).Since this the CfASeyfertgalaxyIRLFisbasedonmodifiedV/V unbiased, opticallyselectedsampleareused.Thederivation of selection byultravioletexcessisalsounsatisfactory. the redandblueobjectsat97%confidencelevel.Thus, The K-Stestshowsthata_isdistributeddifferently for summed overallnobjectswith LineachbinofwidthÀL dispersion), whilefortheredobjectsa_^=—1.51±0.45. the blueobjectsa_=-1.39±0.42(individual have flatterinfraredspectrathanthosewithweakexcesses. For within whichanobjectcould havebeendetectedaboveboth violet excesses.Objectswithstrongultravioletexcessestendto survey limits.Thedifferential IRLF, 0(L),isgivenby histogram offorobjectswithstrongandweakultra- between ultraviolet-excessandinfraredspectra.Figure9isa and Wahl1987),makingitidealforstudiesoftherelationship ultraviolet colors(Huchra,Wyatt,andDavis1982;Edelson ultraviolet-excess selectioncriterion,hasabroadrangeof red objects.TheCfASeyfertgalaxysample,whichusedno m quasar surveysbiasedthesesamplesagainsttheinclusionof tion criteriausedintheMarkarianSeyfertgalaxyandPG 1260Aim IR 1260 1260Ail? IR In thispaper,infraredmeasurementsofacomplete, The maximumaccessiblevolume(FJistheofspace R78 foundgoodevidencethattheultraviolet-excessselec- (I>(Lir) = Q/AL 4n Vol. 321 1987ApJ. . .321. .233E No. 1,1987 filled circles.Aproperleast-squaresfittotherelationLocL'isshown by galaxies aredenotedbyfilledtriangles,whileSeyfert2 line forSeyfert2galaxies(s=1.71). the dashedlineforSeyfert1galaxies(forwhichs=1.73),andbydotted IRad p 7.—plotofLvs.forthe45objectsdetectedat60/mi.Seyfert1 IGoptir © American Astronomical Society • Provided by the NASA Astrophysics Data System 42.2- 42.6 42.6- 43.0 43.4-43.8 43.0-43.4 43.8-44.2 44.6- 45.0 44.2- 44.6 1-3 3x Lers (ergss") (Gpcmag"N(Gpc"mag- (Gpc mag)N opt (ê/) log LlogO logO ir (1) (2)(3)(4)(5) (6) (7)^ INFRARED PROPERTIESOFSEYFERTGALAXIES Seyfert GalaxyFar-InfraredLuminosityFunction 4.47 3.79 3.81 2.98 3.51 2.81 3.64 Type 12BothTypes TABLE 6 2 0 4 42645-1 45731 42245-1 -1 42245 0 42 091 41 96 (Huchra andSargent1973).Inthisequation,Qistheamount The quantityListhemonochromaticluminosity(47trvF)at of skysurveyedoptically(Q=2.66sr),and/isthefraction AL =IO,correspondingtoonemagnitude. optically selectedobjectsobservedintheinfrared(/=0.94). 60 jum.Thedataweresummedusinglogarithmicbinsofwidth values ofL.Columns(2}-{3),(4H5),and(6)-{7)givethespace separately andforbothtypestogether,ispresentedinTable6 densities andnumberofobjectsineachbinrespectivelyfor and Figure10.Column(1)ofTable6containsthebinned type 1,2,andbothtypestogether. tion wasusedmakestheIRLFsubjecttoincompletenessfor most Seyfert2galaxies,andmany1have by theopticalandinfraredsurveylimits.Thus,thisIRLFcan infrared spectrathissteeporsteeper,effectcanbequite be systematicallydeficientinobjectswitha_<-1.3.Since objects withinfraredspectralindicessteeperthanthatdefined limit totheIRLFofallSeyfertgalaxies. luminosities of10*-10°ergss.TheIRLFSeyfert1 severe, andthederivedIRLFshouldbeconsideredalower IRy galaxies andbothtypestogetherweredeterminedforlumin- (Mrk 231,L=10-ergss“,andNGC5273, Nothing canbeconcludedfromthepresentdataabout osities of10*-10°ergss.TwoSeyfert1galaxies ir ergs s. IRLF ofSeyfertgalaxieswithLoutside10'-10 optIR 10 ergss"),andoneSeyfert2galaxy(Mrk270,L= This sampleconsistsofthe48SeyfertgalaxiesinCfAred- properties ofacomplete,unbiasedsampleSeyfertgalaxies. 10 g-i)haveinfraredluminositiesoutsidethisrange. shift survey.Forthesegalaxies,thefollowingdatahavebeen tinua between1.1/miand1.3mmtobestudied.Seyfertgal- of 45,LandNphotometryabout60%thesample, obtained :IRASmeasurementsof46objects,JHKphotometry irIR red spectrumtosteepenfromquasarsSeyfert1galaxies axies havethefollowingcharacteristics: of thermaltononthermalinfraredemissionalong this Seyfert 2galaxies.Thisiscausedbyanincreasinglylargeratio IR 1.3 mmupperlimitsforall.Theseobservationsallowthecon- IR erS s 4.43 4.35 4.39 2.89 3.17 3.37 The differentialIRLF,derivedforSeyfert1and2galaxies The factthatabivariateoptical-infrareddistributionfunc- The IRLFoftype2Seyfertgalaxieswasdeterminedfor For thefirsttimeitispossibletodetermineinfrared There isahighlysignificanttrendfortheslopeofinfra- VII. CONCLUSIONS 4.47 4.46 4.52 4.44 3.77 3.15 3.52 12 4 2 7 8 247 1987ApJ. . .321. .233E 95% significancelevel. objects. Thetwodistributionsaredifferent atthe95%confidencelevel. Fig. 8.—Histogramsofa_oforSeyfertgalaxiesclassifiedbyDahari(1985)asinteracting(I)ornoninteracting(N).Thetwodistributionsare different atthe F. 9—Histogramofa_based onultravioletexcess.Top:datafor“blue”objects(i.e.,thosewithstrong ultravioletexcesses);bottom:datafor“red” 126Mm IG1260;im © American Astronomical Society • Provided by the NASA Astrophysics Data System B rO ¡2¡ rO (U ß (U Íh 0 3 - 4 1 - -2 -2 -1 0 a “iSjim 60fim 12pm ecjim -1 Type N Type I 12 Objects 10 Objects 0 1987ApJ. . .321. .233E IRLF ofSeyfert1galaxies;middle:2bottom: of bothtypestogether.Errorbarsare1 Fig. 10.—InfraredluminosityfunctionoftheCfASeyfertgalaxies.Top: ro O CD 'o Q. O E 1000 r- 1000 - 1000 ^ © American Astronomical Society • Provided by the NASA Astrophysics Data System 1(F ^ 10^- 10*^ _i in.iJ1—i—iMini n—i—i i11111—i—i11il1—r-=i I »iilI—1ll1—u 1 }í L (ergs^ ir J jtypes INFRARED PROPERTIESOFSEYFERTGALAXIES 1 Type 2: Type 1 Both Ï T — 45 from theseobjects.Theturnoversinthepower-lawspectraof like spectra,indicatingthatnonthermalradiationis low-frequency turnoversaround80/¿m. the Seyfertgalaxyspectralenergydistributionshavesharp which have(*2.2-25pm^1-25anda_60/un37.Halfof radii. absorption, andimplysourcesizesof~100Schwarzschild unreddened Seyfert1nucleiareattributedtosynchrotronself- responsible fortheobservednear-andmid-infraredemission sequence. NoSeyfert2galaxyhasaninfraredslopeasflat any oftheopticallyselectedquasarsstudiedbyE86,all infrared spectraandone-thirdoftheSeyfert1appears nosity functionsarenotdistinguishableupto10ergss"^ tively morethermalfluxthanSeyfert1galaxies,theirlumi- 12 nantly thermalfar-infraredcontinua,theturnoverfrequency to comefromdust.AlloftheSeyfert2galaxiesandabouthalf with theIRASdata,M.J.LebofskyandW.F.Kailey for galaxies likeArp220.Seyfertnucleiappeartoresideingal- those ofnormalspiralgalaxiesbutsimilartoinfrared gives minimumdusttemperaturesof~50K,warmerthan appear tobespatiallyextended.Inthoseobjectswithpredomi- of theSeyfert1galaxieshavecoldfar-infraredexcesseswhich This indicatesthatSeyferthostgalaxiesoftenareunusually axies withhigherthanaveragefar-infrareddiskluminosities. reading themanuscript.J.Huchrakindlyreleasedlist of and N.Scoville,A.Readhead,M.Schmidtforcritically assistance inobtainingsomeofthemeasurementsreported, active instarformation.AlthoughSeyfert2galaxiesemitrela- IRAS datawassupportedbyNationalAeronauticsandSpace CfA Seyfertgalaxiesinadvanceofpublication.Analysis of (1986), thentheunblockedsolidangleisapproximatelynstera- galaxies inthiscompletesample.IfalloftheSeyfert2 at CaltechissupportedbyNSFgrantAST84-12473.Infrared Administration grantNAS7-918.Millimeter-waveastronomy dians. an obscuringtorus,assuggestedbyKrolikandBegelman are simplydustySeyfertl’swithbroad-lineregionsblockedby the NationalScienceFoundation.Thisworkwasalsopartially astronomy atStewardObservatoryispartiallysupported by supported byNSFgrantsAST85-52643and83-14134. About two-thirdsoftheSeyfert1galaxieshaveflat,quasar- The thermalemissionwhichcharacterizesalloftheSeyfert2 The authorswouldliketothankW.Riceforinvaluablehelp There isonedustySeyfert1foreverythree2 249 1987ApJ. . .321. .233E M. A.Malkan:DepartmentofAstronomy,Math-Sciences Building,UniversityofCalifornia,LosAngeles,CA90024 Kollatschny W.,andFricke,K.J.1984,Astr.Ap.,135,171. IRAS PointSourceCatalog.1985,JointScienceWorkingGroup, Impey, C,andNeugebauer,G.1987,Ap.J.,inpreparation. .1987,Ap.J.,313,651(PaperI). Huchra, J.,andSargent,W.L.1973,Ap.186,433. Huchra, J.P,Wyatt,W.F.,andDavis,M.1982,A.J.,87,1628. Huchra, J.,andBerg,R.1987,Ap.inpreparation. R. A.Edelson:CenterforAstrophysicsandSpaceAstronomy, CampusBox391,UniversityofColorado,Boulder,CO80309 Edelson, R.A.,andWahl,T.1987,Ap.J.Suppl.,inpreparation. Edelson, R.A.,andMalkan,M.A.1986,Ap.J.,308,59(EM). Edelson, R.A.1986,Ap.J.(Letters),309,L69(E86). G. H.Rieke:LunarandPlanetaryLaboratory,StewardObservatory, UniversityofArizona,Tucson,AZ87581 Dressei, L.L.,andCondon,J.1976,Ap.Suppl.,31,187. Draine, B.T.,andLee,H.M.1984,Ap.J.,285,89. Devereux, N.A.,Becklin,E.E.,andScoville,Z.1987,Ap.J.,312,529. de Jong,T.,Clegg,P.E.,Soifer,B.Rowan-Robinson,M.,Habing,H.J., de Grijp,R.H.K.,Miley,G.Lub,J.,andJong,T.1985,Nature,314,240. de Bruyn,A.G.,andWilson,S.1976,Astr.Ap.,53,93. Dahari, 0.1985,A.J.,90,1772. Cruz-Gonzalez, andHuchra,J.1984,AJ.,89,441. Condon, J.1987,preprint. Clements, E.D.1984,M.N.R.A.S.,204,811. Campins, H.,Rieke,G.andLebofsky,M.J.1985,A.J.,90,541. Angel, J.R.P.,andStockman,H.S.1980,Ann.Rev.Astr.Ap.,18,321. Aitken, D.K.,andRoche,P.F.1985,M.N.R.A.S.,213,111. in column(6). positions aspossible.Thequotederror(inarcseconds)isgivenincolumn(5).referencefortheastrometricmeasurement column (4).Anattemptwasmadetousepositionsmeasuredwithradiointerferometers,inorderhaveasconsistentasetof (1), andtherightascensiondeclinationincolumns(2)(3),respectively.Thetypeofastrometricpositionusedisgiven 1 (seePaperI).Fortheremainingsixobjects,publishedpositionsarecompiledinTable7.Thesourcenameispresentedcolumn 250 (Washington, DC:GPO). L67. Houck, J.R.,Aumann,H.H.,andRaimond,E.1984,Ap.(Letters),278, Forty-two ofthe48CfASeyfertgalaxiesstudiedinthispaperhavepositionsmeasuredwithVLA,whicharegenerallygoodto © American Astronomical Society hms and Wilson1981;(4)CresselCondon1976;(5)Clements1984. IC 4397141543.70263833.9O0.15 NGC 4388122314.85619R31 NGC 3982ll5352355°24'09"R3"1 Mrk 461134504.8343255O4 Mrk 789132955.53112149.8R1.53 Mrk 205121933.67753515.2R1.02 Note.—In col(4),O=opticalandRradio. 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