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1974ApJ. . .192. .581K trate theimportantspectroscopiccharacteristicsthat which canbeclassifiedasSeyferts.Discussionsofsome relations amongthevariousparametersthatcanbe them asastatisticalgroupinthehopeoffindingcor- few werefoundbyothermeans.Asthesampleof tained intheZwickylistsofcompactgalaxies,anda in abright,semistellarnucleus.Thisdefinitionincludes used inthispaperissimplyagalaxyrecognizableon structed usingmeasuresofgalaxydiametersmadeon diameter- diagramforSeyfertgalaxiesiscon- data areincludedfor18galaxies,andtheangular- aid inclassifyingthesegalaxies.Newt/5Fphotometric the datathatnowexistforasampleof71galaxies measured forthesegalaxies.Inthispaperwesummarize were detectedinMarkarian’ssurveyofgalaxieswith The primarynewdatapresentedareasetof37spectra strong ultravioletcontinua.Anumberwerealsocon- have propertiesresemblingthoseoftheclassical N galaxiesiftheirspectrahavebroademissionlines Sky Surveyprintsthathasbroademissionlinesarising obtained withimage-tubespectrographswhichillus- some respectoneoranotheroftheclassicalSeyferts. of theclassification,butallgalaxiesresemblein of thegalaxiesincludeaconsiderationvalidity Seyfert galaxiesincreases,itbecomespossibletostudy Sky Surveyprints. The AstrophysicalJournal,192:581-589,1974September15 search inAstronomy,Inc.,under contracttotheNational which isoperatedbytheAssociation ofUniversitiesforRe- Seyfert .Mostofthese“new”galaxies Science Foundation. © 1974.TheAmericanAstronomicalSociety.Allrightsreserved.PrintedinU.S.A. The workingdefinitionofaSeyfertgalaxywhichis A largenumberofgalaxiesarenowknownwhich t Visitingastronomer,KittPeak NationalObservatory, * NationalAcademyofSciences exchangescientist. © American Astronomical Society • Provided by theNASA Astrophysics Data System so itisconcludedthattheredshiftsarecosmological.ThemeanMfor40Seyfertnucleiwhoseproperties presented toillustratethespectralcharacteristicsofthesegalaxies,andnewUBVdataareincludedfor18 resemble theQSOsiscalculatedtobe-20.4,with21nucleihaving—20>—21.5. galaxies. Awell-definedangular-diameter-redshiftrelationisfoundtoexistforthetotalsampleofgalaxies, Subject headings:Seyfertgalaxies—galacticnuclei u Data nowavailablefor71Seyfertgalaxiesaresummarizedanddiscussed.Acollectionof37spectrais I. INTRODUCTION II. THEDATA Byurakan AstrophysicalObservatory,Armenia,USSR AN ATLASOFSEYFERTGALAXIES Received 1974March18;revisedApril12 Dyer Observatory,VanderbiltUniversity Edward Ye.Khachikian* Daniel W.Weedman*)* ABSTRACT AND 581 -1 _1 -1 classes ofSeyfertsaswellthe homogeneityofspectra and theyarenonstellarobjectsonSkySurveyprints. class 2Seyfertsthaninthenarrow-linegalaxies.There distinguished frommostnarrowlinegalaxiesbythe blend intheclass2Seyferts.ClassSeyfertsarealso rarely exceed200kmsintheselattergalaxies.In width thatdividestheclass2Seyfertsfromother tensity typicallybetween500and1000kmsare class 2galaxieshavefullwidthsathalf-maximumin- also correlatewiththeseclassifications(Khachikian width. Thisclassificationisconvenientbecausethe the forbiddenlinesandBalmeraresame broader thantheforbiddenlines,orclass2,inwhich are eitherclass1,inwhichtheBalmerlines into twogroupsdependingontherelativewidthsof Proceeding fromthis,theSeyfertgalaxiesareseparated . Thespectroscopicdistinction betweenthetwo have nuclearcolorslikethose forclustersofyoung have ultravioletexcessesthat cannotbeexplainedby line galaxies(Weedman1973).BothclassesofSeyferts among class1Seyferts,2andnarrow- are alsosignificantdifferencesintheUBVcolors ally becauseitimpliesadifferentionizingsourceinthe not consideredSeyferts.However,theselinestendto are sharpandclearlyresolvedinobjectslikeMarkarian not consideredtobeSeyfertsalthoughlinewidths galaxies withstrongnuclearemissionlineswhichare thousand kmswide.Thereisnoclearlydefinedline those oftheforbiddenlinesinclass1objects,but generally asymmetric.Thesewidthsaregreaterthan and Weedman1971a;1973).Thelinesin forbidden linesandBalmerlines.TheSeyfertgalaxies stellar radiationwhereasnarrow-line galaxiesgenerally spectra suchasthoseinfigure2theHaand[Nn]lines only datarequiredarespectraofmoderatedispersion Seyferts. Thisisanimportantdistinctionastrophysic- 308 and313(numbers2325,infig.2),whichare Balmer linesinclass1objectsareusuallyseveral although photometricandmorphologicalproperties [O m]:Hßratio,whichisextremelyhighinclass2 1974ApJ. . .192. .581K 582 primarily Ngalaxies.Thoseobjectsincludedwhich pact galaxies,theclassicalSeyferts,andafewothers, with otherpropertiesofthegalaxiessuchastheir within agivenclassisillustratedinfigures1and2 first fiveMarkarianlistsofgalaxieswithultraviolet table 1.TheseincludetheSeyfertsdiscoveredin contained inthenotestotable1. colors orluminosities.Commentsontheindividual among theclass1spectra,suchasvariationsin continua (Markarian1972,1973),thosefound spectra ofSeyfertgalaxiesinfigures1and2are Balmer linewidths,thatmayprovetobecorrelated (1972a); numbers1,class1Seyfertgalaxiesfromtable;2,21. in theliteratureofbroadlinesitsspectrum.Sources the compilationbyBurbidgeandO’Dell(1972).An were initiallyclassifiedasNgalaxiesaretakenfrom (primarily bySargent)fromtheZwickylistsofcom- (plates 6and7).Thereareinterestingdifferences maximum diameters6"ofthegalaxiesintable1were N galaxyisincludedhereifmentionhasbeenmade which mightbeassociated with activityinagalaxy. galaxies. Theimageswerecarefullystudiedforevidence the onlysourceofhomogeneousphotographsforthese measured onSkySurveyprintssincethesearesofar central diskspresentinsome galaxies,soshorter- of spiralstructureorthepresence ofjetsandfilaments, of thetabulateddataarecontainedintable.The structure wouldnotbedetected intheoverexposed These featuresarealsonoted inthetable;butspiral The totalsampleof71Seyfertgalaxiesislistedin Fig. 3.—Angular-diameter-redshiftdiagramforSeyfertgalaxiesandellipticalgalaxies.Filledcircles,ellipticalsfromSandage © American Astronomical Society • Provided by theNASA Astrophysics Data System EDWARD YE.KHACHIKIANANDDANIELW.WEEDMAN -1 exposure photographswithalargescalemightshow table 1isthatanangular-diameter-redshiftrelation spiral featuresinmoreofthegalaxies. where thegalaxiesintable1areplottedusing exists forSeyfertgalaxies.Thisisillustratedinfigure3, The meanrelationfortheSeyfertsfollowscloselythat (fUled circles),butthesamelinefitsSeyfert for giantellipticalgalaxiesdeterminedbySandage angular diametersd"measuredfromSkySurveyprints. galaxies. Theellipticalsplottedareallofthoselisted angular-diameter-redshift relationfortheellipticals (1972

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© American Astronomical Society • Provided by the NASA Astrophysics Data System 1974ApJ. . .192. .581K present intheclass2prototypeNGC1068.Anexten- resolved withfurtherquantitativedatafortheoptical, if any,relationexistsbetweentheclass1and2 fainter thanforthenucleialoneofclass1.Alsoas cannot bemeasureddirectly,theMforclass2 magnitudes oftheclass2nucleiarecertainlyfainter has demonstratedthatexcessivedustreddeningis , andradiospectra. those ofclass2.Itisnotyetpossibletodecidewhat, have beendiscoveredtomuchhigherredshiftsthan than class1(althoughtheymayonlybedimmedmore magnitudes ofbothclassesSeyferts.Theabsolute stantial correctionsmayberequiredfortheabsolute Adams andWeedmantoconsiderthisproblem;sub- galaxies intable1isnowbeingmadebyThomas which thenucleiaresubject,becauseWampler(1968) proach theminluminosity.ThoseSeyfertswithvery it istheclass1SeyfertsthatresembleQSOsintheir may notbethesame.Hopefullythisquestioncan by dustabsorption).Whilethenuclearmagnitudes sive studyoftheHa:HßratiosinmanySeyfert those SeyfertsbluerthanB—V=+0.6,U quasi-stellar objectssothatanexplanationofthe shown bythespectrainfigures1and2,classSeyferts Seyfert galaxiesthemselves(Weedman1973)are continua, likeQSOs,aredominatedbynonthermal conclusion fromtheUBVcolorsisthatclass1Seyfert broad permittedlines(liketheQSOs)areclass1,and two groupsofobjects,itisimportanttorealizethat basis oftheirangulardiametersthattheredshifts a veryusefulworkinghypothesissincethebrighter nuclei ofSeyfertgalaxiesarescaled-downmodels Seyferts. Thefundamentalsourceofnuclearactivity certain (Arp1971a;LyndsandMillikan1972). figure 1)andKazarian102(number1).Bothobjects figure 1.TheseareMarkarian205(number3in radiation.) Forcomparisonwithclass1spectra,the spectroscopic andphotometricappearanceap- attempting torelatetheenergeticphenomenain cosmological. Wehavealreadyconcludedonthe luminosity, iftheredshiftsofSeyfertsandQSOsare 588 portant relativetopossiblemodels forthequasi-stellar appear stellaronSkySurveyprintssoareconsidered spectra oftworadio-quietQSOsareillustratedin Seyfert galaxieswouldalsoexplaintheQSOs.Thisis trum isrepresentativeofthoseencounteredinQSOs blue stellarobjectsdiscoveredinanobjective-prism Seyfert galaxiesarecosmological(fig.3).When the interpretationofQSOs as highlyactivenucleiin with ^0.1. Kazarian 102iscontainedinanunpublishedlistof QSOs althoughthenatureofMarkarian205isun- Seyferts dooverlapthefainterQSOsinabsolute giant ellipticalgalaxies.The only nearbySeyfertgalaxy survey withtheByurakan1-mSchmidt,anditsspec- objects. Sandage(1972&)has givenevidencefavoring u — 0.4(liketheQSOs)arealsoclass1.(Theimportant The suggestionhasbeenmadefrequentlythatthe The morphologicalnatureof Seyfertgalaxiesisim- c) RelationbetweenSeyfertGalaxiesandQSOs © American Astronomical Society • Provided by theNASA Astrophysics Data System EDWARD YE.KHACHIKIANANDDANIELW.WEEDMAN class 1Seyferts.Theforbiddenlinewidthsandthe which mightbeexpectedforthenucleusofanelliptical class 2Seyferts,buttheemissionlinesareveryweak considered asevidenceforaconnectionbetween properties ofNGC1275arenotthoseexpectedif explanation forthis,suchasascarcityofgasinthe relative tothecontinuum.Theremaybeasimple class 1Seyferteventhoughthelatterareobjects mini-, accordingtoSandage’smodel.Butthe therefore bethebestexampleamongSeyfertsofa the brightestgalaxyinPerseusclusterandisalso which canbeclassedasagiantellipticalbecauseitis internal physicalconditions. galaxy. Buttheempiricalresultremainsthatspectral nucleus ofNGC1275comparedwithotherSeyferts, of thebroad,intenseBalmerlinesthatcharacterize spectrum ofNGC1275doesnotresemblethatany a strongradiosource(3C84).NGC1275should in table1thatresemblesthisdescriptionisNGC1275, Seyferts andQSOs.NGC1275showsnoindication representative spectraillustratingtheirpropertieshave investigations oftheseobjects.Itisconcludedonthe been presentedasaguideforanalysisandfuture determine theextentofnonthermalcontinua. basis oftheangulardiametersthesegalaxiesthat the Seyfertphenomenonisrestrictedtoparticulartypes logical classificationsthatitcouldbedecidedwhether necessary toobtainbolometricluminositiesand reddening onthebasisofBalmerdecrement.Ob- may bethebestparameterrepresentinganintrinsic than this,dependingonthedustabsorptionwithin magnitudes canbecalculated.TheMforthose their redshiftsarecosmological,soabsolute [O in]:HßratioinNGC1275aresimilartothose nuclear luminositysincethesecanbecorrectedfor in thenuclei,andstudiesofBalmer-lineluminosities give unambiguousinformationconcerningconditions galaxies. Severalimportantobservationalprojects the 107-inchtelescopeatMcDonaldObservatory; of galaxiesmightleadtosufficientlyrefinedmorpho- Finally, acarefulphotographicstudyofthissample servations oftheinfraredandradiocontinuaare spectra resemblethoseofQSOsis—20.4.Theintrin- 1275, class1Seyfertgalaxies,andQSOshavesimilar exchange programsponsored bytheNationalAcad- should bepursuedforthesegalaxies.Theemissionlines sic luminosityofSeyfertnucleimaybemuchgreater Seyfert nucleiwhoseemission-lineandcontinuous work throughgrantGP-38738. the NationalScienceFoundation forsupportofthis we expressappreciation.D. W. alsoacknowledges emies ofSciencestheU.S.A. andtheUSSR,towhom D. W.alsothanksDr.RayWeymannforguest of galaxies. United Stateswasmadepossiblebythescientific Steward Observatory.ThevisitbyE.Ye.K.tothe observing privilegeswiththe90-inchtelescopeat u Collected dataon71Seyfertgalaxiesalongwith We thankDr.HarlanSmithforgrantingustimeon IV. SUMMARY Vol. 192 1974ApJ. . .192. .581K Disney, M.J.1973,Ap.{Letters),181,L55. Byurakan AstrophysicalObservatory,Byurakan,Armenia,USSR Edward Ye.Khachikian Daniel W.Weedman Dyer Observatory,VanderbiltUniversity,Nashville,TN37235 Huebra, J.,andSargent,W.L.1973,Ap.186,433. .19736,preprint. .1972,Ap.Letters,12,1. Khachikian, E.Ye.,andWeedman,D.W.1971a,Astrofizika, de Vaucouleurs,G.,andA.1964,Reference .1973a,Ap.J.,181,31. de Vaucouleurs,G.1961,Ap.J.Suppl,5,233. .19716,ibid.,1,221. .1971,ibid.,1,111. Dibai, E.A.1970,Astrofizika,6,350. Burbidge, G.R.,andO’Dell,S.L.1972,Ap.J.,178,583. Arp, H.C.1971a,Ap.Letters,9,1. .19706,Astrofizika,6,357. Burbidge, E.M.,andG.R.1971,Ap.J.{Letters), Burbidge, G.R.1970,Ann.Rev.Astr.andAp.,8,369. Arakelian, M.A.,Dibai,E.Esipov,V.F.,andMarkarian, .19736,ibid.,9,319. .1973a,ibid.,9,325. .1972c,ibid.,p.329. Collin-Souffrin, S.,Alloin,D.,andAndrillat,Y.1973,Astr. Braccesi, A.,Lynds,C.R.,andSandage,A.R.1968,Ap.J. Arp, H.C.,andKhachikian,E.Ye.1973,Astrofizika,9,509. .19726,ibid.,8,177. Arakelian, M.A.,Dibai,E.andEsipov,V.F.1972a, Anderson, K.S.1971,Ap.J.,169,449. .19726,ibid.,176,LI. Adams, T.F.,andWeedman,D.W.1972,Ap.J.{Letters), .1973,Ap.J.,179,417. Adams, T.F.1972a,Ap.J.{Letters),172,LI01. No. 3,1974 7, 389. Press). and Ap.,22,343. B. Ye.1970a,Astr.Tsirk.,No.586. Astrofizika, 8,33. Catalogue ofBrightGalaxies(Austin:UniversityTexas 163, L21. {Letters), 152,L105. 173, L109. © American Astronomical Society • Provided by theNASA Astrophysics Data System ATLAS OFSEYFERTGALAXIES REFERENCES — .1973,IAUSymposium,58,inpress. Zwicky, F.,Oke,J.B.,Neugebauer,G.,Sargent,W.L.W., .1973,ibid.,183,29. .1972,/.,174,483. Zasov, A.V.,andLyutyi,V.M.1973,SovietAstr.—AJ,11, .1972,ibid.,173,7. .19706,ibid.,160,405. .1972a,Ap.J.,173,485. Weedman, D.W.,andKhachikian,E.Ye.1969,Astrofizika, Weedman, D.W.1970,Ap.J.,159,405. 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Chuvaev, K.1973,Astr.Tsirk.,No.755. 589 1974ApJ. . .192. .581K Khachikun andWeedman(see page582) (17) Markarian79,(18)NGC7469, (19)Markarian352,(20)NGC4051. 374, (10)Markarian231,(11) 110,(12)and(13)3C120,(14)NGC7603,(15)Markarian 279,(16)Markarian335, 102, (2)IIIZw2,(3)Markarian205,(4)Markarián304,(5)II 136,(6)IZw1,(7)II(8)Markarian506,(9) Fig. 1.—SpectraofQSOsandclass1Seyfertgalaxies;redtothe right.AllspectraarealignedonnightskyA5577.(1)Kazarian © American Astronomical Society •Provided bythe NASAAstrophysics Data System 17 14 13 MMNi.»œjUbc-mimj-mêi 11 20 12 18 16 15 19 Mr 10 8 IltoicaitoatolWtoNttoMVIMtoMllin 4 3 9 ■ 7 toa 6 toa |«M1IS i h • II ***•' ff 5 y--,1 MHato*aa*'-4' MKP § I , mé i I f i f*4»i PLATE 6 1974ApJ. . .192. .581K Khachikian andWeedman(see page582) Markarian 270.(35)NGC3227. (36)and(37)NGC1068. (21) Markarian501,(22) 315,(23)Markarian308,(24)198,(25) 313,(26)Markarian268,(27) Markarian 372,(28) 176, (29)IIIZw55,(30)NGC1275,(31)Markarian1,(32) 348,(33)Markarian3,(34) 1 Fig. 2.—Spectraofclass2Seyfert galaxiesandnarrowlinegalaxies;redtotheright.Allspectra alignedonnightskyA5577. 26 37 M « 36 4•§ 4 28 ^^ÊÊ^ÊttÊÊÊÊÊÊtÊÊÎÊÊÊÊÊIÊÊtÊÊÊÊtKÊÊKIIK^ÊÊtÊÊIKKÊtK^^9 35 It'-.aMIMIHHMNMÄ v*• PLATE 7 27 4.4.■•»îiwmi 25 24 21 © American Astronomical Society •Provided bythe NASAAstrophysics Data System 23 22 # * 4 II«».- 4 i tè&MiWlÊÊÊ: ^ i mma«ma I MMIN«IIIa MPiw-1 4 M Hl*Iml It HI*'I *£-- « » * « « I