19 90ApJS. . .72. .231M -1 Adams (1977)foundthatnearlyallSeyfertshavespiralor galaxies. Theprimarymotivationistoextendtheeffortsof logical typeofthegalaxies.”WehingerandWyckoff(1977) prescient paper,Kalloglian(1971)notedthefrequentoccur- were classedaspossibleellipticals,butinnocasewasany (CCD) detectorandbycompilinganimprovedsampleof earlier authorsthroughtheuseofcharge-coupleddevice © 1990.TheAmericanAstronomicalSociety.Allrightsreserved.PrintedinU.S.A. ies andconcludedthattheir“spectradependsonthemorpho- passed nearlyallofthethen-recognizedSeyfertgalaxies.Ina with publishedmaterialon20additionalgalaxies,itencom- member ofthesampleclearlyanellipticalgalaxy.Adams barred spiralormorphologies.Severalgalaxies photographic studyof30Seyfertgalaxieswithredshifts less examined 12high-redshiftSeyfertgalaxieswithanelectrono- rence ofpeculiarmorphologiesandbarsinMarkariangalax- (1977) alsonotedthat“thereisapparentlyasurplusof Seyfert galaxies. The AstrophysicalJournalSupplementSeries,72:231-244,1990February remainder tohave“jetsorotherdistrubedfeatures.”From a graphic camera.Thesegalaxiesaregenerallymoreluminous survey consistedofimage-tubeplates60galaxies;together Seyfert nucleiindisturbedandinteractingsystems.”Adams’s possibly highercentralsurface brightnessintheSeyfertdisks. range oftheSITcamerausedinhisstudy,Yeefoundthat the (1983). Despitethedifficultiesposedbylimiteddynamic cleus, andsignsofthatprocessbecomeevidentinringlike and Wyckoff(1977)found60%tobespiralsmostof the than thoseincludedinthesurveyofAdams(1977).Wehinger mation onthestructureand kinematicsofSeyfertgalaxies. disk parametersandcolorsofSeyfertgalaxiesaresimilar to structures inthediskofgalaxy.Three-colorsurfacepho- an evolutionaryschemeinwhichgasissuppliedtothe nu- than 5000kms,Simkin,Su,andSchwarz(1980)proposed Heckman, Balick,andSullivan (1978)findapproximately those ofnormalspiralgalaxies, withtheexceptionofa tometry hasbeenobtainedfor20Seyfertgalaxiesby Yee This paperexaminesthemorphologiesandcolorsofSeyfert In aclassicstudyofthemorphologySeyfertgalaxies, Single-beam HI(21cm)observations alsoprovideinfor- nuclei. Imagesofthegalaxiesarepresentedalongwithaperturemagnitudes. which mayberemnantsofpastinteractions,constitutesapproximatelyone-fifththesample.Thecolorsand exponential diskparametersofSeyfertgalaxiesaregenerallysimilartothosespiralwithoutactive Subject headings:galaxies:nuclei—photometrySeyfertstructure tidally interacting,orbarredgalaxies).AsubsetofSeyfertgalaxieswithamorphousmorphologies,some that Seyfertgalaxiesnearlyalwayspossessmechanismsfortransportingmaterialintotheirnuclei(e.g.,peculiar, CCD imagesofavolume-andluminosity-limitedsample51MarkarianNGCSeyfertgalaxiesshow © American Astronomical Society • Provided by theNASA Astrophysics Data System SEYFERT GALAXIES.I.MORPHOLOGIES,MAGNITUDES,ANDDISKS I. INTRODUCTION Institute forAstronomy,UniversityofHawaii,andSpaceTelescopeScience Received 1987March18;accepted1989July31 John W.MacKenty ABSTRACT 231 have “stronganomahes”intheirHIspectra.Alargersurvey pecuharities attributedtoeitherclosecompanionsinthe one-third ofasample58Seyfertand“Seyfert-like”galaxies years towardanunderstandingofthehostgalaxiesAGNs of 91SeyfertsbyMirabelandWilson(1984)shows40%with part bythedebateovertruedistancesofQSOs.Stockton comes fromstudiesoflow-redshiftQSOs.Thiswassparkedin neutral gasinthegalaxies. Malkan, Margon,andChanan(1984)havedetectedfaint Hutchings etal(1981,1982),Hutchings,Crampton,and (1978) demonstratedthatQSOsdohavecosmologicalred- telescope beamortidalinteractionsthathaveperturbedthe by whichthecentralmassiveobjects(incurrent-epochAGNs) with neighboringgalaxies.Stockton(1982)notedthepresence shown thatthisnebulosityhasthecorrectcolors,magnitudes, Campbell (1984),Wyckoff,Wehinger,andGehren(1981), shifts andseemtopreferresideinsmallgroupsofgalaxies. mal continua,respectively. near severalQSOsandproposedthatinteractionsareameans nucleus ofanactivegalaxywith“fuel”mightbeinteractions QSO hostgalaxiesthatshowstellarabsorptionlinesatthe etal (1984)havesucceededinobtainingspectraofseveral QSO nuclei.BorosonandOke(1982),MacKentyStock- and scalelengthsforgalaxiesattheredshiftofresident “fuzz” underlyingmostofthelow-redshiftQSOsandhave redshift QSOs3C48(Boroson andOke1982)Markarian galaxies) appearstobeinteracting andthatone-fourthisin fueling radiogalaxiesandemission-linewithnonther- (1982) alsodiscussedtheputativeroleoftidalinteractions in of veryclose(andprobablytidallytruncated)companions same redshiftastheQSOnuclei. ton (1984),Boroson,Persson,andOke(1985),Heckman compact groupsorclusters of galaxies.Spectrathelow- and Campbell(1984)findthat one-thirdoftheirsample(78 QSOs tendtosupportthisconcept.Hutchings,Crampton, are suppliedwithgas.Fosburyetal.(1982)andStauffer 1014 (MacKentyandStockton 1984)showBalmerlineab- Images andspectraofthehostgalaxieslow-redshift Somewhat surprisingly,muchoftheprogressinrecent Gunn (1979)suggestedthatameansofsupplyingthe 19 90ApJS. . .72. .231M _1- 232 ing themorphologiesofgalaxiesinsurveyandnotes vations ofthissamplearedescribedin§III,andtheir ies isdefinedin§II,anditscompletenesscomparedtothe have consideredthepossibilitythatinteractinggalaxies would sufficetoincreasetheinputof“fuel”nucleus luminous Seyfertgalaxies,thesampleiscloselyakinto the § VII. nuclear activity.Roos(1981,1985^,6)andGaskell(1985) behavior oftheQSOluminosityfunctionconsistentwith bars, orinfallofgasclouds,deRobertis(1985)findsthe low-redshift QSOs(StocktonandMacKenty1983,1986). paper assumei/=75kms Mpc,^r=0.5.Whendis- with LINER(Heckman1980û)orstarburstcharacteristics more luminousQSOsandisclearlydistinctfromgalaxies discussed in§VI,andtheconclusionsaresummarized on selectedgalaxiesarepresentedin§V.Theresults observations inascenariowheregalaxyinteractionstrigger considered byseveralauthors.NormanandSilk(1983)note quite asymmetric.Photoionizedgasstructuressuggestiveof magnitude oftheavailablecatalogs. must bechosentoinaccord withthelimitingapparent objects arefluxlimited,theapparentmagnitudeconstraint directly coupledtothespatialresolutionorscalethat is analysis isexplainedin§IV.Thesystemdevisedforclassify- actually responsiblefortheactivityarerathersmallgalaxies. and suggestthatsuchdistortionsmightarisefrommergers, galaxy mergersandinteractionsonactivegalaxieshavebeen (1972) andGunn(1979),thetheoreticalconsequencesof Keel (1985)andMacKenty(1986)reportSeyfertgalaxieswith star formation;furthermore,Markarian1014’smorphologyis sorption inthehostgalaxies,indicatingarecentepisodeof (Balzano 1983).And,sincemostcatalogsofastronomical achievable forthemostdistantobjects.Byselectingrather samples usedinpreviousmorphologicalsurveys.CCDobser- that anygeneraldistortioninthecentralregionofgalaxy tidal tails. tidal featureshavebeendiscoveredassociatedwithluminous have accountedformostofthecurrentlycatalogedSeyfert recently reviewedthemethodsofdiscoverySeyfertgalaxies galaxies tobeincludedinthesample.Thelimitingdistance is nosities, and(3)theminimumapparentbrightnessesof the and someoftheassociatedselectioneffects. Huchra, Wyatt,andDavis(1982),Osterbrock(1984)have galaxies: surveysofUV-excessobjectsanddirectspec- ods usedinthediscoveryofSeyfertgalaxies.Twomethods cataloged Seyfertgalaxiesisprimarilytheresultofmeth- difficulties inherentintheirdiscovery.Itisinterestingtonote (1) themaximumdistances,(2)minimumabsolutelumi- Seyfert galaxiesareknown.Therelativelysmallnumberof 1980; Veron-CettyandVeron1984),whileonly200-300 that -3000QSOshavebeencataloged(HewittandBurbidge troscopy. Weedman(1977),BalickandHeckman(1982^), 0 o A volume-andluminosity-limitedsampleofSeyfertgalax- All distancemeasuresand absolute luminostiesinthis Following theinitialsuggestionsofToomreand Any surveyofSeyfertgalaxiesmusttakeintoaccountthe For thepresentstudy,threecriticalconstraintsare © American Astronomical Society • Provided by theNASA Astrophysics Data System II. SELECTIONOFTHESAMPLE MACKENTY -1 preferable tokeepthesample selectioncriteriacloselycou- have publishedmagnitudesofsignificantlygreateraccuracy more severebiases.Keel(1980)andLawrenceElvis included intheMarkarianfists.Thesamereasoningapplies to related tothemorphologiesofSeyfertgalaxies.Since only known tobeuncertain-0.5mag.Themostimportant NGC galaxies)arethosefromtheMarkarianfistswhich based onthedataavailableatthattime.Theonlymagnitudes ian survey.Themedianredshiftofthesampleis9450kms. pled toMarkarian’sdiscovery datasincethissampleisin- rather thanontheirnuclearmagnitudes.Tohaveselected the magnitudes wereusedforallMarkariangalaxies,and the km s~\(4)haveabsolutemagnitudeslessthan-19Af,and of anactivegalaxyanditsnuclear spectrum.Overall,itseems (1982) havediscussedtheconnection betweentheinclination RNGC magnitudeswereusedforthesevenNGCgalaxies not consideration inconstructingthiscatalogwastoavoidbias Table 1,columns(1)and(2).Aplotoftheirabsolutemagni- produce ascompleteasamplepossibleandstillretain in thepresentsample.Theseconstraintswerechosento sample basedon,forexample,[Om]fluxes,mighthaveadded the decisiontoselectgalaxiesbasedontheirtotalmagnitudes the more“interesting”)ofMarkarianSeyfertgalaxies a fraction(consistingmainlyofthemoststudiedandperhaps region ofthisfigurereflectstheincompletenessMarkar- Figure 1(themagnitudes,obtainedhere,are-1magbrighter (5) haveapparentmagnitudeslessthan16.5wareincluded many galaxiesidentifiedashavingLINERspectra.From than Markarian’s,inconstructingthesampleMarkarian then availablefortheentiresample(excludingbrighter able telescopetime. than Markarian’s).Theabsenceofgalaxiesintheupperright tudes inV(for30kpcapertures)versusredshiftisshown these requirementsandwasreasonableintermsoftheavail- statistical analysis.Asampleof~50galaxiesbothsatisfied sufficiently largenumberofgalaxiesonwhichtoperforma Markarian orNGCcatalogs,(2)havedeclinationsbetween (from avarietyofdiscoverymethods)tobeSeyfertgalaxies. galaxies brighterthan~13m(Markarian1967).However,a fainter than-15.5w(HuchraandSargent1973;Meurs General Catalog(RNGC;SulenticandTifft1973)areknown creasingly incompleteforgalaxiesofapparentmagnitude galaxies. From1967to1979theypublished15listscontaining catalog ofSeyfertgalaxiesduringtheirsearchforUV-excess their catalog,allSeyfertgalaxiesthatare(1)includedinthe that containsallidentifiedSeyfertgalaxiesand,inaddition, the publishedliterature(andafewobservationsoftheirown) significant numberofbrightgalaxiesfromtheRevisedNew and Wilson1984).Furthermore,theMarkarianfistsexclude Lipovetskii, andStepanian1979)havecompiledthelargest 1500 galaxies.TheMarkarianUV-excesssurveybecomesin- should beunderstoodthatthevalueshavebeenconvertedto this cosmologywhennecessary. tances ormagnitudestakenfromotherworksarecited,it pg pg pg pg -20° and+60°,(3)haveredshiftsbetween300013,000 The selectionofthesamplewasmadein1983September, The 51Seyfertgalaxiesselectedforthisstudyarefistedin Schinckel andPhillips(1982)havecompiledacatalogfrom Markarian andhiscoworkers(Markarian1967;Markarian, Vol. 72 19 90ApJS. . .72. .231M No. 2,1990 0514-001 1095 2325+083 2359+030 5437811 2302+222 2154+071 0922+523 0804+391 0739+500 0434-103 0331-052 0323-062 0239+070 0232-090 1048 0225+311 1040 2353+071 2316-000 1721+310 1606+123 1254+571 0752+392 0733+585 0204-003 1018 2301+084 1535+580 1439+534 1433+485 1343+561 1216+301 1202+204 0916+163 0446-062 0 0247+191 0236+014 0004+200 335 2041-105 1553+192 0339-013 0328-032 0228-091 1044 0212-010 590 0045+143 1146 1622+411 1557+351 1535+544 1502+104 1435+590 1416+252 1339+304 1221+030 1207+472 1124+353 Naae © American Astronomical Society • Provided by theNASA Astrophysics Data System 533 7674 315 516 506 871 291 477 541 530 7603 290 474 5683 509 699 493 273 231 766 4253 622 618 609 595 486 841 817 Mrk NGC 268 423 110 382 612 372 704 198 ... 7469 ... 5548 (i) (2)(3)(4)(5) 79 50 0 9 0 4074 1358 1667 1409 1019 985 931 863 11830 1.5 12981 10500 11220 12300 11400 12300 12300 10800 10200 12950 1.5 10650 10110 11700 12810 10930 12300 12040 10200 1 11850 8620 8545 9240 7800 9980 8800 6600 2 6580 1.2 5020 1 9900 3850 6925 9900 4071 4910 9450 9600 1.8 8400 4990 6910 9720 1.9 4578 7500 7220 8930 7380 6066 9300 7251 4920 1 8100 Type 1.5 1.5 1.2 1.5 1.5 1.5 1.5 2 1 1 2 1 1 2 1 1 1 1 1 1 1 1 1 1 1 1 16.0 15.0 16.0 15.0 15.5 -57.3 15.5 15.0 15.0 16.0 14.5 ■pg Resolu- 16.5 14.0 14.0 16.5 15.5 16.0 15.0 15.5 14.5 13.5 13.0 16.0 13.5 13.5 14.5 15.0 14.0 14.0 15.0 14.5 12.5 14.5 16.0 14.5 14.0 15.5 15.0 15.0 14.0 15.5 15.0 15.5 14.5 13.0 14.0 15.5 15.5 14.5 14.5 14.5 15.5 (Mrk) BIINightSeeingtion -48.8 -33.9 -35.4 -52.8 -54.7 -29.9 -45.5 -21.1 -34.7 -46.5 -59.5 -45.6 -47.8 -27.2 -57.7 -41.4 -30.1 -35.5 -51.2 -41.8 -45.0 -60.5 -56.9 -48.2 SEYFERT GALAXIES.I. 41.6 47.3 48.0 31.5 56.8 60.6 60.2 59.7 82.3 44.4 44.6 49.4 49.4 77.3 30.8 54.6 28.4 53.5 70.5 64.6 68.4 78.6 70.2 39.7 28.6 28.7 (6) Properties oftheSample (7) 20 13 13 13 30 30 30 30 13 13 13 30 30 13 13 23 23 23 23 23 23 20 19 20 30 30 30 13 23 20 19 13 30 30 30 13 13 23 23 23 23 13 13 23 23 23 20 13 19 TABLE 1 1.4 1.3 1.3 1.3 3.1 3.4 4.0 4.5 1.3 1.6 1.4 2.0 2.1 2.9 3.5 3.8 3.9 4.0 1.4 1.6 2.3 2.8 1.6 1.2 1.4 2.0 2.2 2.1 2.6 3.5 5.6 4.5 3.4 1.1 1.4 1.3 1.5 2.6 2.8 2.8 4.0 4.2 1.0 1.5 1.6 1.9 1.7 1.1 1.2 (8) 0.63 0.73 0.96 0.88 0.95 0.81 0.87 0.75 0.38 0.91 0.81 0.88 0.96 1.04 1.47 1.43 2.04 0.62 1.18 0.92 0.77 2.48 2.07 3.03 0.86 0.48 1.82 1.33 1.19 1.16 1.94 2.04 1.23 1.07 1.05 2.58 2.58 0.58 0.78 1.09 1.64 1.55 1.52 1.62 1.01 1.51 1.51 1.30 (9) 0.7 (10) (11) 3 0 2 2 0 3 1(3) 1(2) 1(2) 2 3 0(1) 0 0 2(3) 3 0 2(3) 3 0 3 3 0 3 2 0(3) 0(1) 0(3) 3 0(1) NC 1(2) 1 3 2 3 1 2 2 1(2) 1 0 0 0 0 2 3 0 0(1) 0 0 0 0 0 0 0 0 0 1 1 1(3) IC 155 119 107 105 165 165 101 173 144 175 127 170 115 165 131 159 135 (12) (13) 59 81 35 65 35 69 55 69 17 75 35 33 81 73 35 PA 73 3 5 9 9 13.9 10.3 10.9 10.2 11.5 11.5 10.3 16.0 16.8 12.3 14.5 11.9 10.0 12.6 12.4 6.5 4.3 6.2 5.5 5.8 6.4 8.3 5.1 4.2 9.0 5.8 5.1 6.7 6.4 6.1 9.9 3.1 7.0 4.8 5.1 6.8 4.1 6.1 6.7 7.5 7.2 6.6 8.6 6.9 6.9 9.6 4.0 9.9 a 0.66 0.55 0.94 0.86 0.69 0.74 0.52 0.85 0.64 0.60 0.86 0.69 0.89 0.90 0.86 0.47 0.78 0.74 0.25 0.65 1.00 0.98 0.84 0.61 0.72 0.65 0.96 0.54 0.95 1.00 0.59 0.73 1.00 0.92 0.75 0.76 0.85 0.69 0.95 0.78 0.81 0.57 0.59 0.61 0.77 0.78 0.84 0.70 b/a (14) 233 19 90ApJS. . .72. .231M 234 c b kiloparsecs; col.(14)ratiooftheminor andmajoraxislengthofthe24thRmagisophote;col.(15)exponential diskscalelengthinkiloparsecs; exponential diskcomponent. central surfacebrightnesses(not corrected forinclination);cols.(28)-(30)thefractionofluminosity within32kpccontainedinthe classification inparentheses;col.(11) interactionclass;col.(12)positionangleofthe24thRmagisophote; col.(13)semimajoraxeslengthin diameter apertures;cols.(22)-(24) sameascols.(16)-(18)foranannulusbetween5and10kpcin radius; cols.(25)-(27)theB,V,andR cols. (16)-(18)V,B-V,andV— Rmagnitudeandcolorsin30kpcdiameterapertures;cols.(19)-(21) sameascols.(16)-(18)for5kpc the B,V,andRphotometricobservations;col.(9)sameas (8) expressedinkiloparsecs;col.(10)morphologicalclasswithalternate type; col.(5)m,fromMarkarian;(6)Galacticlatitude;(7) nightofphotometricobservations;col.(8)meanseeinginarcseconds a 13.00 17.02 10.88 c b a -1 5.22 6.01 3.57 4.37 6.92: 3.74 2.84 2.07 6.85 6.60 4.22a 4.95 4.06 4.39 5.29 5.28 3.36 9.06° 3.92 7.63 4.97 r 2.55 6.60 5.65 2.50 3.89 3.84 2.97: 3.80 3.41 3.56 1.56 5.10 3.34 6.14 4.23 3.58 3.41 5.31 7.79 2.53 5.49: 3.04 2.58 5.72 (15) Peculiarprofile. No obviousdisk. Highlyinchned. Notes.—Key tocolumnheadingsisasfollows:col.(1)Markarian name; col.(2)NGC(3)redshiftinkms;(4)Seyfert 0 © American Astronomical Society • Provided by theNASA Astrophysics Data System -21.34 -22.22 -22.71 -21.21 -21.49 -20.58 -21.34 -21.39 -21.01 -21.14 -21.59 -22.87 -20.58 -20.67 -21.37 -20.58 -21.38 -22.26 -21.62 -21.31 -21.55 -22.05 -21.88 -21.38 -21.85 -21.74 -20.57 -21.55 -20.14 -20.80 -21.88 -21.34 -21.12 -21.45 -21.55 -21.70 -21.66 -20.61 -20.81 -22.09 -20.91 -22.05 -21.36 -20.81 -21.07 -20.14 -22.17 -21.46 (16) (17)(18) 30 kpcAperture 0.91 0.78 0.30 0.42 0.88 0.72 0.48 0.84 0.75 0.75 0.99 0.44 0.67 0.76 0.89 0.85 0.67 0.39 0.21 0.34 0.40 0.69 0.90 0.74 0.70 0.27 0.73 0.79 0.67 0.46 0.87 0.57 0.64 0.88 0.72 0.63 0.59 0.36 0.48 0.85 0.72 0.90 B-V 0.66 0.82 0.24 0.55 0.94 0.22 0.63 0.58 0.58 0.60 0.54 0.56 0.58 0.64 0.56 0.53 0.56 0.55 0.54 V-R 0.47 -20.24 0.50 0.59 0.56 0.41 0.53 0.96 0.58 0.52 0.53 0.55 0.60 0.59 0.52 0.50 0.55 0.53 0.63 0.57 0.57 0.61 0.58 0.53 0.60 0.63 0.43 0.53 0.55 0.65 0.60 0.55 0.55 0.53 0.59 0.45 -22.53 -20.47 -20.16 -21.14 -21.29 -20.70 -20.22 -20.44 -22.46 -20.00 -20.61 -20.55 -19.96 -20.68 -20.42 -19.91 -21.64 -20.99 -20.74 -19.58 -20.11 -19.98 -20.78 -20.85 -20.07 -20.50 -21.82 -20.57 -19.92 -20.10 -20.91 -20.12 -20.97 -19.55 -20.89 -20.06 -20.91 -20.69 -20.11 -20.93 -19.89 -19.73 -21.19 -20.27 -19.75 -19.57 -21.35 (19) (20)(21) 5 kpcAperture 0.90 0.26 0.57 0.63 0.41 0.88 0.88 0.36 0.87 0.80 0.70 0.32 0.08 0.24 0.70 0.87 0.80 0.78 0.68 0.17 0.76 0.31 0.43 0.33 0.96 0.80 0.58 0.21 0.38 0.68 0.76 B-V 0.47 0.97 0.78 1.02 0.77 0.48 0.56 0.21 0.60 0.66 0.22 0.84 0.69 0.54 0.22 1.08 1.00 TABLE 1—Continued MACKENTY 0.57 V-R 0.68 0.62 0.56 0.59 0.56 0.65 0.69 0.61 0.59 0.98 0.51 0.41 0.56 0.57 0.57 0.51 0.52 0.65 0.55 0.65 0.71 0.63 0.45 0.69 0.51 0.44 0.69 0.58 0.60 0.46 0.50 0.55 0.58 0.62 0.55 0.56 0.58 0.50 0.68 0.64 0.67 0.66 0.59 0.57 0.60 0.48 0.46 -20.25 -17.65 -18.49 -19.67 -20.87 -19.61 -19.73 -20.08 -20.71 -18.50 -19.76 -18.49 -18.65 -19.07 -20.95 -20.76 -20.13 -19.94 -18.06 -19.23 -19.75 -19.90 -20.11 -19.99 -20.54 -20.29 -20.46 -19.87 -18.73 -19.49 -19.38 -18.98 -19.99 -20.54 -17.98 -19.62 -20.70 -20.23 -18.18 -19.53 0.720.4422.722.021.5 -20.07 0.700.5220.219.519.0 -20.40 -18.85 -20.12 -19.20 -19.41 -18.54 -20.79 (22) (23)(24) 5-10 kpcAnnulus 0.93 0.93 0.66 0.80 0.99 0.55 0.60 0.45 0.54 0.66 0.83 0.75 0.97 0.84 0.77 0.64 0.87 0.72 0.58 0.67 0.64 0.95 B-V V-R 0.65 0.96 0.71 0.72 0.80 0.95 0.56 0.67 0.40 0.79 1.15 0.41 0.98 0.63 0.84 0.80 0.76 0.82 0.69 0.56 0.91 0.86 0.52 1.00 0.57 0.51 0.66 0.55 0.64 0.57 0.66 0.51 0.57 0.48 0.43 0.54 0.57 0.47 0.96 0.56 0.53 0.59 0.53 0.52 0.60 0.47 0.60 0.51 0.58 0.54 0.41 0.53 0.55 0.60 0.39 0.52 0.45 0.46 0.51 0.57 0.51 0.51 0.64 0.64 0.52 0.60 0.56 0.51 0.51 0.26 21.4 22.2 21.2 22.8 23.3 21.9 23.1 23.2 20.8 21.4 22.4 22.1 23.5 22.421.4 20.1 21.6 21.3 23.5 19.5 20.6 23.2 22.8 22.0 21.8 23.2 22.0 21.8 20.4 20.9 23.5 21.2 22.6 21.721.0 22.9 22.021.4 21.7 22.2 20.2 21.5 21.3 23.3 21.4 22.2 22.5 (25) (26)(27) B Central S.B. 20.8 20.9 20.6 21.5 22.0 21.6 20.4 22.1 21.3 22.4 20.3 20.2 20.4 21.5 22.9 19.5 19.3 21.5 20.4 21.1 21.4 21.2 21.5 20.0 22.1 21.6 21.0 20.9 22.7 22.1 20.5 21.9 22.4 20.0 20.6 20.6 19.4 19.5 21.3 20.9 20.3 20.0 20.8 21.6 20.0 20.9 22.5 20.6 20.3 21.6 19.9 19.0 19.9 19.6 18.4 20.6 20.7 22.4 22.0 21.1 20.7 21.4 20.6 21.5 21.7 21.0 20.5 20.0 20.2 21.6 19.8 19.7 19.6 18.8 19.5 19.1 R 0.12 0.40 0.48 0.41 0.12 0.09 0.160.25 0.18 0.440.46 0.64 0.85 0.64 0.24 0.58 0.13 0.67 0.35 0.17 0.10 0.70 0.35 0.42 0.450.44 0.37 0.410.49 0.41 0.06 0.25 0.27 0.20 0.21 0.43 0.26 0.59 0.13 0.33 0.29 0.350.39 0.56 0.620.74 0.93 0.49 0.46 0.64 0.53 0.56 0.440.43 (28) (29)(30) B Disk Fraction 0.60 0.83 0.45 0.19 0.51 0.21 0.69 0.17 0.65 0.16 0.70 0.32 0.50 0.30 0.67 0.41 0.13 0.15 0.65 0.22 0.50 0.39 0.85 0.27 0.28 0.54 0.53 0.66 0.00 0.28 0.50 0.45 0.24 0.67 0.18 0.65 0.21 0.59 0.31 0.44 0.00 0.50 0.56 0.76 0.27 0.43 0.00 0.51 0.08 0.85 0.51 0.09 0.33 0.65 0.46 0.21 0.00 0.34 0.43 0.22 0.28 0.69 Vol. 72 19 90ApJS. . .72. .231M -1 1 -1 1 only afterextendingtheapparent-magnitude-limited spectro- ies thathascometobeknownas“Seyfertgalaxies,” and of such“classical”Seyfertgalaxies willprobablybeacquired haps debatablewhichmethodofdiscoveringSeyfertgalaxies 1983), tofainterlimitingmagnitudes. scopic surveys,suchastheCfA redshiftsurvey(Huchraetal regions reflectthemajorityofthatpopulationactivegalax- is best,galaxieswithphotoionizedbroad-andnarrow-line inescapable atthepresenttimeinanySeyfertsampleof the furthermore suchgalaxiespossessthegeneralnuclearproper- galaxies mayrepresentadifferentclassofSeyfert equally goodorperhapssuperiorsampleofSeyfertgalaxies ties ofthemoreluminousQSOs. Largeandcompletesamples (see deGripetal.1985),although//MS'-selectedSeyfert order of50galaxies.TheIRASdatabasemayyield an virtually completeforthe85%ofgalaxiesbrighterthan ies withvelocitieslessthan3000kms)ontheSeyfert than “classical”MarkarianSeyfertgalaxies.Whileitis per- ian survey.Theresultsofa(K/F(max))test(usingMarkar- sample selectedforthispaperindicatethattheis ian’s magnitudeswherepossibleandincludingthefivegalax- Wilson (1984)reachedsimilarconclusionsabouttheMarkar- pleteness forgalaxiesfainterthanm~15.5.Meursand 15.5w. NGC 4258(537kms"),4388(2450and redshifts of332)andfoundincreasingsignificantincom- NGC 5728(2970kms).Althoughthesegalaxieswere observed, thesubtractionofnightskyfromimages galaxies: NGC1068(1090kms"),4151(990 the firstfourMarkarianlists(401galaxies,forwhichtheyhad these galaxiesprovedtoberatherunreliable. the sampleasdefinedabovewouldcontainfiveadditional obtained forthissurvey,arepresentedinpaper. magnitudes forallofthesegalaxies,derivedfromtheimages tended primarilytostudyMarkarianSeyfertgalaxies.New vs. redshift.Someincompletenessisevidentintheupperrightcomer. pg No. 2,1990 pg -1 The incompletenessatfaintmagnitudesappearstobe Huchra andSargent(1973)appliedthe(V/V(max))testto If thelowerredshiftlimitof3000kmswereremoved, Fig. 1.—TheabsolutemagnitudesinV(in30kpcdiameterapertures) 2 o cn -22.5 _ -20.5 _ -23 ^IL -22 _ -21 _ © American Astronomical Society • Provided by theNASA Astrophysics Data System 2000 400060008000100001200014000 Redshift • " SEYFERT GALAXIES.I. -1 bias duringeachexposuretopermitscalingoftheframe were obtainedfromtheaverage of2-6exposuresineachfilter prior toitspixel-wisesubtraction.Technicalproblemswithin ing 20-400.01sdarkexposures).Theusual“extendedregis- virtual-phase CCDcamera(Hhvak,Henry,andPilcher1983) with theUniversityofHawaii’s2.24mtelescopeatMauna were correctedwithflat-field frames.Theflat-fieldframes estimate ofthemeanbiaslevel to-16electronsrmsafter with nonphotometricconditionsweresubsequentlyscaledto photometric night.Thelongexposuresobtainedonnights least one“short”exposureofeachgalaxyinfilterona had bothphotometricconditionsandsatisfactorystandard was usedattheCassegrainfocusbehindafocalreducer, correction forday-to-daytrends. ining theskyatsunriseoruponhearingreportsofcirrus Kea Observatory.ATexasInstruments(TI)800x800pixel subtraction ofanaveragedbiasframe(obtainedfromaverag- working intheinfrared). exposure programwascarriedoutonnightsthatweresubse- cause (1)theymighthavebetterseeingand(2)forconditions exposures alsowereobtainedonnonphotometricnightsbe- observations weremadeisgiveninTable2.Onlyfivenights obtained ineachfilter.Alogofthenightsonwhichthese (typically 60s)andalongexposure600were giving afinalimagescaleof0'.'41pixel. the CCDcamera’selectronicslimitedrehabilityof this ter” offchipregionwasusedtoestimatetheDClevelof the clouds duringthenightfromobserversatothertelescopes quently determinedtohavebeennonphotometricafterexam- of cirruscloudsbothatduskanddawn(hencetheshort- star observations.Thestrategyemployedwastoobtainat filters oftheKittPeak“Mould”type.Bothashortexposure to havebeenconsideredphotometrictheskyhadbeclear the saturationofCCDdetectorintheirnuclei).Short the photometricobservationsusingouterregionsof Seyfert galaxies(toavoidthevariabilityoftheirnucleiand Variations inthesensitivityof theCCDfrompixelto The imageswerecorrectedforinstrumentaleffectsbythe Images ofeachSeyfertgalaxyinthesamplewereobtained Images wereobtainedthroughKron-CousinsB,F,andR III. OBSERVATIONSANDINITIALREDUCTIONS 1985 Apr16Photometry(night30) 1984 Nov17Photometry(night23) 1984 Oct23-24Longexposures 1984 Sep1Photometry(night20) 1984 Aug31Photometry(night19) 1984 Jun28-29Longexposures 1984 Jun27Photometry(night13) 1984 Feb25-27Longexposures 1983 Dec3-5Spectraofcompanions UT Date(s)ObservingProgram b) InstrumentalCorrections Log ofObservations a) Observations TABLE 2 235 19 90ApJS. . .72. .231M -1 -1 236 higher orderfittingfunctionsdidnotyieldmarkedlysuperior were typicallylessthan0.02.Ingeneral,thisprocedure re- image, definedas Watanabe, Koraira,andOkamura1982): regions surroundingtheSeyfertgalaxieswereextractedfor included inmostoftheregions fromwhichtheskylevelwas moved theskybackgroundtobetterthan1%.Theuse of were excludedfromthefit.Valuesforshadingacross the where I(x,y)isthenumberofcounts(1count=1.6elec- further analysis.Theseregionsrangedinsizefrom-15%to was availableoftheskylevel determination(andthesimplest results becausemostofthecurvatureinskybackground filled mostoftheframeonly anarrowregionneartheedges determined; inthoseinstances inwhichtheSeyfertgalaxy gnette thefieldofview).Theedgesdetectorwere not occurs neartheedgesofdetector(whereoptics vi- showed sources(stars,faintgalaxies,ortheSeyfertgalaxy) trons) atapoint(x,y)withintheimage.Allareasthat fit isdesirableinsuchcases). these regionsbyfittingaplanesurfaceoftheform(e.g., tor. Thecontributionfromthenightskywassubtracted After divisionbytheaveragedflats(containingatleast100,000 der ofthenight). dust particle,andthemorningflatswereusedforremain- used forthatpartofthenightpriortoappearance photoflood lamp.Eachframewasexposedtoapproximately phase CCD).Furthermore,theonlynotablefeaturesare has verysatisfactoryspatialuniformityevenpriortothe a filterduringthenight;inthoseinstances,eveningflatswere aged together(exceptwhenalargepieceofdustappearedon two-thirds offullwellcapacity(fullis~70,000elec- of theinsidedomeslitdoorilluminatedwitha75w not beenthinned.Athighspatialfrequenciesthedevice the nightandalsoinmorning.Theseframeswereaver- trons). Flatfieldswereusuallyobtainedatboththestartof precision towhichtheareaphotometrycanbeconducted(see —the deepestexposureshave~3000skyelectronspixel). columns withenhancedsensitivityevery20-25that departs fromuniformityby-2%(comparedto8%forthe flat-field correctionsincethisfrontsideilluminateddevicehas are satisfactorilycorrectedwiththedomeflat-fieldframes. § IIIc).TheTIvirtual-phaseCCDgeneratesverylittle,ifany, However, largerscalenonuniformitiesinthedevicelimit electrons pixel),thepixel-to-pixelvariationsarelessthan thinned Galileo/InstituteforAstronomyTI500x500three- 1% (considerablybetterthanthephotonstatisticsinsky of 60-600sisgenerallyinsignificant. dark current,andthecosmic-raydetectionrateoverperiods - 75%oftheoriginalarea800x800pixelCCDdetec- The imageswereexaminedonanimagedisplaysystemand The TIvirtual-phaseCCDdetectorusedforthisproject © American Astronomical Society • Provided by theNASA Astrophysics Data System I{x,y) =a+(ax)(ay, 012 (l ^l-^maxI^llmax)/^0 c) SkySubtraction MACKENTY -1 by 0.38maginordertoforcethemeanofF—Rcolors of nights 20and30wasusedfornight23.Itsubsequently because ofextremelypoorseeing;afittotheremaining color term,andVistheairmassofobservation.Similar magnitude, aisthezeropoint,extinction, procedure wasthenusedtosolvefortherelationship: photometric nightsbymeansofobservationsstandard probably rehableto0.05mag. extinction termsseveraltimesgreaterthanthetypicalextinc- mass standardstarobservationsonnight23areunusable were between1.5and1.8airmasses.Regrettably,thehigh extinction wereobtainedforeachnight.Unfortunately,night dard starobservationsforeachphotometricnightwerethen (these beingjudgedthemostreliableobservations).Thestan- standard starobservationsobtainedonnights13and30 forms wereusedfortheVandRpassbands. where bistheinstrumentalmagnitude,Bcorrected mass) andallobservationswereobtainedatlessthan1.8 color timesairmasstermsappeartobesmall(<0.05mag for eachgalaxyusingconcentric circularannuli.Inthepre- regarded withcaution.Theremainderofthephotometry is masses, thisprocedureprobablyresultsinafinaluncertainty mean oftheV—Rcolors(whichhaveverylittlescatter) of found tobenecessarycorrecttheRzeropointfornight23 sion) andconditionsappearedphotometricatbothsunset (three Landoltstarseachobserved5timesinquicksucces- complete thephotometryofthoseSeyfertgalaxiesvisiblein following night(night20)wasusedinstead.Inaneffortto reliable extinctionterm;therefore,thefrom star; themedianofouteraperturewasusedtodetermine each filter.Twoconcentricapertureswerecenteredon M92 (Christianetal1985;Heasley1984)wereobservedin sent instance,themostimportant considerationistheuni- of -0.1magfornight23,buttheseobservationsshould be all ofthenight23observationswereobtainedatsimilar air sunrise, ameanextinctionobtainedfromtheaverageof standard stars(withamaximumairmassof1.4)yields fitted (usingthesemeancolorterms),andazeropoint air masses,thosetermsweresettozero.Aleast-squaresfitting the skycontribution)wasmeasured.Sincesecond-order and, whenpossible,aselectedregionintheglobularcluster stars. BothindividualstarsfromthelistofLandolt(1983) the Seyfertgalaxiesobservedonnight23toagreewith the tion. Sincethestandardstarobservationsaresomewhatsparse the autumn,mostofobservationsobtainedonnight23 19 hadtoofewstandardstarobservationstodeterminea the localskylevel,andfluxininneraperture(minus the Seyfertgalaxiesobservedonothernights.Sincenearly 0x2 A meancolortermforeachfilterwasdeterminedfromthe A photometriccalibrationwasobtainedforeachofthe Profiles ofintensityasafunction ofradiusweremeasured b —B=Oq+a-^X, d) PhotometricCalibration IV. ANALYSIS a) Profiles Vol. 72 19 90ApJS. . .72. .231M -2 position ofthenuclearpeakwasdeterminedfromatwo- not providearehableindicatoroftheinclinationdisk pixel wereaddedintotheprofileinsuchamannerthatfluxis positions offieldstars(withanuncertainty~1pixel)for obtained fromellipticallyaveragedisophoteswasabandoned, components. Thereforetheusualpracticeoffittingaprofile galaxies inthesample,ellipsefitstoanouterisophotemay formity inthetreatmentofsamplepopulation.Because for theshort-exposureimagesandwasestimatedfrom dimensional parabolicfit(withanuncertaintyof~0.1pixels) No. 2,1990 conserved. Regionswithfieldstarsorgalaxies(exceptfor determined foreachpixelintheimage,andcountsatthat nuclei). Thedistancefromthecenterofnucleuswasthen and magnitudeswereobtainedfromcircularapertures.The the peculiarmorphologiesofasignificantfraction that annulus. and eachannuluswascorrectedfortheexcludedfractionof tightly interactingsystems)wereexcludedfromtheprofile, the long-exposureimages(whichgenerallyhavesaturated better fit(especiallytothepeakofstarimages),itfailed ysis becauseofthebetterbehaviorwingsprofiles. more usefulthantwo-dimensionalfitsinthesubsequentanal- determined frommeasurementsofunsaturatedstarsoneach nent Lorentzian(Diego1985)andatwo-componentgaussian When possible,allstarswerefittedwithbothatwo-compo- CCD frame.Fitsofsimplefunctionstotheirprofilesproved (Thompson 1986).WhiletheLorentzianusuallyprovideda detector particularlywell. or imagescontaminatedbydefectivecolumnsontheCCD converge forstellarimagesobtainedunderpoorseeingcondi- tions (worsethan~2").Neitherfunctionfittedtrailedimages nights arefistedinTable1,column(8).Shortexposureswere R images)oftheshort-exposureimagesfromphotometric Obtained fornearlyallofthegalaxiesundernonphotometric sured fullwidthsathalf-maximum[FWHM]ofthe5,V,and were usedforthemorphologicalclassificationsandFigures on nights23and30.Whilenotrequiredfortheanalysisof conditions onnightswithmuchbetterseeingthanprevailed exponential diskparameters,theimageswithbetterseeing 2-5 (Plates73-83). sight, anellipsecenteredoneachgalaxy’snucleuswasfitted of thegenerallyredcolorsouterpartsgalaxies to the24thmagnitudearcsecisophote.Becauseof the were generallynotobtained underphotometricconditions, superior signal-to-noiseratioresultingfromthecombination at wavelengthsintheRpassband,ellipsefitswere per- and thepeakinquantumefficiencyofCCDdetector long exposuresareusuallysaturated andsinceSeyfertnuclei formed onthelong-exposureRimages.Sincetheseimages over regionsexternaltothe nucleus (sincethenucleiin their profileswerescaledto the short,calibratedRprofiles are frequentlyvariable).The ellipseswerefittedtothelong- The pointspreadfunctionor“seeing”foreachimagewas The measuredpointspreadfunctions(averagingthemea- To estimatetheinclinationofeachgalaxytoourfine © American Astronomical Society • Provided by theNASA Astrophysics Data System b) PointSpreadFunctions c) EllipseFitting SEYFERT GALAXIES.I. l/4 law forthebulge).See,example,workofBurstein where /isthesurfacebrightnessataradiusrand fight distributionoftheouterpartsspiralgalaxies become meaninglessforb/a=1.0. position anglesbecomeprogressivelylesswelldeterminedand (1979a, b)andBoroson(1981).Kormendy(1977)discusses nuclei, thepracticehasbeentofitsimultaneouslyboth distance tothegalaxy.Itsprincipalunfortunatepropertyis profiles thatarefreeofcontaminationbythenucleusorbulge some potentialdifficultieswiththisapproachandlimits disk andthebulgecomponents(usingdeVaucoleursr a fittoradialprofileexpressedinmagnitudesislinearand scale length.Thisfunctionhastheconvenientpropertiesthat peated. Thepositionangles(“PA”),majoraxislengths(“tf”), images andfromfitstotheselectedregionsinphotomet- ing thescalelengthsobtainedfromlong-exposure R lar tothatemployedin§IVa.Forthosegalaxieswith b/a were extendeduntiltheprofilesbecamenoisybecauseoflack brightness (expressedinmagnitudes)versusradiusplotsand disk componentparametersistheselectionofregionsin to thevalidityofexponentialdiskmodel. the profiletoassigndisk.Ingalaxieswithoutactive form: axes weredeterminedto-1pixel(0741),andtheposition for useinthefit—typically<0.1mag),allpointslying or minusafactorsufficienttoyieldtotalof100-200pixels exposure Rimagesaftersmoothingthetwicewitha because theycoveralarger region ontheCCDdetectorand ric (short-exposure)profiles.Thelimitingfactorsarethechoice of -[2-f(a/6)]/3thanthoseobtainedfromcircularlyaver- b/a greaterthan0.5,theexponentialdiskscalelengths ob- each smoothedlongRpassbandexposureinamannersimi- components. Theregionsselectedwerelinearinsurface the resultsaredependentoncorrectchoiceofregionin that anexponentialwillfitalmostanyprofile,andtherefore that thecentralsurfacebrightnessisindependentof angles to~4°.Fornearlyface-ongalaxies(b/a>0.9),the are reportedinTable1,columns(12)-(14).Thelengthsofthe and theratioofminortomajoraxis(“b/a”)eachfit significantly offthefitwerediscarded,andwasre- all pixelsintheimageat24thmagnitudeRisophate(plus image fordeterminationofthe sky.Forafewofthesmaller aged profiles.) greater than0.8,circularlyaveragedprofileswereused.(For of signal.Ellipticalisophoteswithasingle,fixedposition 3x3 kernel.Anellipsecenteredonthenucleuswasfittedto Larger galaxiesaremorelikely tohavegreaterskyresiduals of regionstofitandtheprecision oftheskysubtraction. tained fromellipticallyaveragedprofilesarelargerbyafactor angle andelfipticitywereusedtoconstructaprofilefrom also maynotprovideadequate regionsneartheedgesof 0 An importantfactorforthereliabledeterminationof Freeman (1970)popularizedanexponentialmodelforthe The centralsurfacebrightnesseswerethendeterminedus- d) ExponentialDiskFits r=e/r I() hr=V)~°’ 237 19 90ApJS. . .72. .231M where indicated).Inallimagesnorth isatthetopandeastonleft.Inmostimagesbrightstars andtheSeyfertnuclei“wraparound”inimage MacKenty (see 72, 237) (Mrk 372),600s, V\(d)0323-062(Mrk609),600 s,V;(e)0804+391(Mrk622),300 s,R(poorseeing). display, producingaconfusedwhite andblackregion.OftenthebrighteststarsSeyfertnucleihave saturatedtheCCDresultinginchargebleeding(to the west).Foreachimageexposure timeandfilterisindicated,{a)0004+200(Mrk335),600s,R\ (b)0239+070(Mrk595),600s,R\(c)0247+191 Fig. 2.—Amorphousandunresolved galaxies(MC=0).InFigs.2-5thescaleofeachimageisindicated byahorizontalbar30"inlength(except © American Astronomical Society •Provided bythe NASAAstrophysics Data System PLATE 73 19 90ApJS. . .72. .231M PLATE 74 600 s,R;(h)1339+304(Mrk268), 600s,R(scalemark=60");(/)1435+590(Mrk817),R; (/) 1439+534(Mrk477),600s,B. MacKenty (see72,237) Figs. 2/-2y.—Amorphousandunresolvedgalaxies(MC=0)continued. (/)1202+204(NGC4074),400s,R(poorseeing);(g)1221+030(Mrk50), © American Astronomical Society •Provided bythe NASAAstrophysics Data System 19 90ApJS. . .72. .231M MacKenty {see72,237) 1622+411 (Mrk699),480s,R(scalemark=60");(n)2041-105 509),600s,V. Figs. 2/c-2Amorphousandunresolvedgalaxies(MC=0)continued,(k)1502+104(Mrk841)480 © American Astronomical Society •Provided bythe NASAAstrophysics Data System s, K;(/)1535+580(Mrk290),480/?;(m) PLATE 75 19 90ApJS. . .72. .231M PLATE 76 MacKenty (see 72, 237) 0446-062 (NGC1667),600s,V; (d) 0916+163(Mrk704),1200s,R. Fig. 3.—Spiralgalaxies(MC=1). (a)0212-010(Mrk590,NGC863),600s,V;(ft)0225+311 1040, NGC931),600s,B(scalemark=60"),(c) © American Astronomical Society •Provided bythe NASAAstrophysics Data System 19 90ApJS. . .72. .231M Mac Kenty{see72,237) 600 s,V;(h)2301+084(NGC7469),V(scalemark=60"); (/')2353+071(Mrk541),600s,V\(j)2359+030543,NGC7811),720V. Figs. 3e-3y.—Spiralgalaxies(MC=1)continued,(e)1207+472(Mrk 198),600s,R;(/)1606+123(Mrk871),V;(g)2154+071516), © American Astronomical Society •Provided bythe NASAAstrophysics Data System PLATE 77 19 90ApJS. . .72. .231M MacKenty (see 72, 237) 1019), 600s,V;(d)0328-032(Mrk 612),600s,V. PLATE 78 Fig. 4.—Spiralgalaxieswithbars orrings(MC=2).(a)0045+143(Mrk1146),600s,R;(b)0228-091 (Mrk1044),600s,V;(c)0236+014(NGC © American Astronomical Society •Provided bythe NASAAstrophysics Data System 19 90ApJS. . .72. .231M MacK 1 0739+500 (Mrk 79), 1200s,V(scaleuncertain);(h) 0752+392(Mrk382),600s,R; (i)1216+301(Mrk766,NGC4253), 600s,V. ©American Astronomical Society• Providedby theNASA Astrophysics DataSystem Figs. Ae-Ai.—Spiral galaxieswithbarsorrings(MC =2)continued,(e)0331-052 (NGC1358),600s,V\(/)0434-103 (Mrk618),600s,R\(g) PLATE 79 19 90ApJS. . .72. .231M MacKenty (see72,237) K; (/)1557+351(Mrk493),600s,V;(m)1721+310506),900 s,V. PLATE 80 Figs. 4y-4m.—Spiralgalaxieswithbarsorrings(MC=2)continued, (j)1433+485(Mrk474,NGC5683),600s,V;(k)1553+192291),480 © American Astronomical Society •Provided bythe NASAAstrophysics Data System 19 90ApJS. . .72. .231M (NGC 1409),600s,R\(d)0514-001 (Mrk1095),400s,V\(e)0733+5859),1200(/) 0922+523(Mrk110),900s,R(scalemark=60"). MacKenty (see72,237) Fig. 5.—Peculiarandinteracting galaxies(MC=3).(a)0204-003(Mrk1018),600s,V;(b)0232-090 (Mrk1048,NGC985),600s,R;(c)0339-013 © American Astronomical Society •Provided bythe NASAAstrophysics Data System PLATE 81 19 90ApJS. . .72. .231M PLATE 82 MacKenty (see72,237) 1343+561 (Mrk273),600s,V;(j)1416+252(NGC5548),R (scalemark=60";theimagesareatslightlydifferentscales). Figs. 5g-5y'.—Peculiarandinteractinggalaxies(MC=3)continued, (g)1124+353(Mrk423),600s,(h)1254+571231),B;(/) © American Astronomical Society •Provided bythe NASAAstrophysics Data System 19 90ApJS. . .72. .23IM MacKenty (see72,237) NGC 7603),1200s,V(scalemark=60");(m)2325+083(Mrk533, NGC7674),700s(5700-6200ÀpassbandfilterwithTIthree-phase500x500CCD; scale markindicates60”). Figs. 5/c-5m.—Peculiarandinteractinggalaxies(MC=3)continued. (/:)1535+544(Mrk486),480s,V(scalemark=60"),(/)2316-000530, © American Astronomical Society •Provided bythe NASAAstrophysics Data System PLATE 83 19 90ApJS. . .72. .231M -1 238 Table 1,columns(10)and(11). Table 3.Theclassifications for eachgalaxyareindicatedin presence ofmechanismscapabletransportingmaterial into better than175. the innerpartsofgalaxy. Thetwosequencesareshownin ing nightswithseeingconditionsbetterthan270andusually sequences, oneformorphologiesandasecondinterac- pressed inkiloparsecsistabulatedTable1,column(9). The tions. Bothprovidesomeindicationofthelikelihood the classifications werebasedonadditionalimagesobtained dur- resolution element(theFWHMofstarsintheimage) ex- central surfacebrightness.Afewcasesfailedtoyieldaccept- short photometricexposures.Nearlyallofthemorphological each oftheclassificationspresentedinthisstudy,size of a classifications. Todemonstratethelimitationinresolutionfor component. Thelattereffectwilltendtoincreasethereported galaxies thediskcomponentisbarelyevidentinprofiles, seeing diskestimateswereobtainedfromtheaverageof the compared togalaxiesintheexistingcatalogsofmorphological able fits;theseareindicatedinTable1,column(15). and thefitmaybecorruptedbyinclusionofbulge galaxies andthegreaterdistanceofmostSeyfert morphological classificationschemes.Theprincipaldifficulties are thecontributionofnucleitocentralregions outer features)ithasbeennecessarytopresenttwoimagesof defects (specificallyblockedcolumnsintheCCDdetector), image thefilterusedandexposuretimearenotedin associated withclassifyingSeyfertgalaxieswithintraditional (especially galaxieswithsmallbarsandfaint filter. Thehalosseenaroundverybrightstarimagesaredue figure legends.Imageshavegenerallybeencleanedofvisible nology. motivated inpartbythedevelopementofnewdetectortech- image tube,WehingerandWyckoff(1977)usedanelectrono- be higherthanin“normal”galaxies.SinceSeyfertgalaxies a singlegalaxy. spot nexttoacomplementarydarkisduedustonthe “best” representation.Thedefectthatgivesrisetoabright and theircontrasthasbeenadjustedinteractivelytoyieldthe nuclei arenearlyalwaysfoundinspiralgalaxies.Thefraction to reflectionsintheopticalpath.Inanumberofcases stricted themselvestoalimitedsample(30galaxiescloser graphic camera,andSimkin,Su,Schwarz(1980)re- of Seyfertgalaxieswithpeculiarmorphologiesalsoappearsto than 5000kmsinredshift).Thepresentstudyhasbeen available observationalmethods.Adams(1977)exploitedthe galaxies (Adams1977;WehingerandWyckoffSimkin, are relativelyrare,mostfairlydistantandrequirethebest Su, andSchwarz1980;Dahari1984)demonstratedthatSeyfert Each galaxyinthesamplehasbeenclassifiedalongtwo Adams (1977)hasdiscussedatsomelengththedifficulties The CCDimagesarepresentedinFigures2-5.Foreach Several previoussurveysofthemorphologiesSeyfert © American Astronomical Society • Provided by theNASA Astrophysics Data System a) ClassificationSequences V. MORPHOLOGIES MACKENTY -1 _1 _1 -1 galaxy totheNE.Adams(1977) hastheidentificationsre- JWM). galaxy witharedshiftgreaterby3200kms(Dahari1985; redshift oftheSeydfert(JWM). to theSW,andcompanion (Mrk610)isthedisturbed with slightlyasymmetricarmsexceptforthesmallgalaxy to the north.Theapparentcompanionactuallyisabackground Wilson (1978)reportavelocitydifferenceof160kms. has asmallcompanionthatappearsdistorted.Wardand with filamentaryarms.Thereisasmallgalaxytothewestof shows emissionlineswitharedshiftwithin200kmsof the de Vaucouleursand(1975)Theys and galaxy hasabarlikeextensiontothesouthanddistor- This galaxyislikelytobeamerger. the east.Amoderate-qualitygrismspectrumofthisgalaxy appear inthering.Thisgalaxyhasbeendiscussed by ted ringlikefeaturetotheeast.Severalbrightcondensations unknown redshift. here forthefirsttime. Spiegel (1976). in narrow-band[Om]images,itismostlikelyabackground barely resolvedgalaxiesdominatedbyitsnucleus.Thefeature galaxy seenedge-on. extending severalarcsecondstowardtheNWisintriguing observations havethereference“JWM”andarepresented only to-200-300kms.Redshiftsobtainedfromthese December 4-5UT.AgrismspectrographandtheTI500X Balick andHeckman1981,1982h),butsinceitisnotvisible (and withinthebumed-outregioninimagepresentedby several galaxiesbytheauthorduringnightsof1983 tail totheSSE.Thereisanouter“arc”ofmaterialNE. three-phase CCDwereemployed,yieldingredshiftsaccurate 0323—062 (Mrk609).—TheSeyfert istheamorphousgalaxy 0239+070 (Mrk595).—TheSeyfertisthelargergalaxyto 0236+014 (NGC1019).—Anunremarkablebarredspiral 0232-090 (Mrk1048,NGC985).—Thishighlypeculiar 0225+311 (Mrk1040,NGC931).—Thiswell-knowngalaxy 0212—010 (Mrk590,NGC863).—Tightlywoundspiral Redshifts ofpossiblecompaniongalaxieswereobtainedfor 0204-003 (Mrk1018).—Highlypeculiarwithashortstubby 0004+200 (Mrk335).—Thisgalaxyisoneofaclass imately thesamesizeasSeyfertgalaxyandarewithin known redshiftsareclassifiedasIC=1iftheyapprox- 0 Amorphous/unresolvedIsolated 2 Barand/orringDisturbedcompanion Seyfert galaxy. 3 PeculiarordistortedBridge,tail,jet 1 SpiralCompanion ~ 5diameters,oraresmallerbutwithin1diameterofthe Class Morphology(MC)Interaction(IC) Notes.—Seyfert galaxieswithcompanionsun- b) NotesonIndividualGalaxies Classification Sequences TABLE 3 or atsamez Vol. 72 19 90ApJS. . .72. .231M -1 _1 _1 -1 No. 2,1990 jetlike tailextendingtotheWNW.Thereisadiffuseregionat Wilson 1984). versed (seeMarkkarianandLipovetskii1974;Mirabel interacting pairbetterknownasIIIZw55.Therehasbeen 480 kms,althoughthedistortedappearanceconvincingly difference of130kms(Dahari1985;JWM). spiral galaxy.Ithasfaintdistortedandfragmentedouter NNE hasanemission-lineredshiftwithin200kmsofthe arms. ThecompanionbarredspiraltotheSSEhasaredshift demonstrates thephysicalassociation. some confusionastowhichnucleusistheSeyfert(seeWilson and Meurs1982).Dahari(1985)findsavelocitydifferenceof of thebarbeingmorediffuse(seeWehingerandWyckoff end ofthebar)andextendingtoNEthenaround Seyfert galaxy(JWM). an anomalousarmbeginningatthenucelus(ratherthan have ananomalousarmalongitssouthernedgeoppositea pears tohaveanasymmetric armonitsnorthernsideanda with abrighterarmtotheNE. small degreeofisophotetwistingandadustlanesouth the difference of130kms. of thegalaxyisaforegroundstar(Adams1977;Wehinger spiral. Thereisaspiralgalaxyofunknownredshift~3'to 1977). and showssignsofhavingspiralarms. ring attheendsofbar. nucleus extendinginaneast-westdirection. star obtainedasapartofthisstudyaddstheHaline in second extensiontotheSSE,againpossessingadiffuseregion the endoftailextendingtosouth.Thereisalsoa the WNW. the SE.Thegalaxyisalsoasymmetric,withnorthernside beyond thishalo.An[Om]narrow-bandimageshowsan extending totheNE.Theslightlybrighterstareasthas nearly stellarwithanextensiontotheWNWandafaintwisp acting companionhasaNELGspectrumwithredshift absorption atzeroredshifttotheaccumulatedevidence. and Wyckoff1977;Dahari1985;JWM).Thespectrumof this at theend.Thestellarobjectembeddedindisturbedbody cated bythepresenceofanearbybrightstar.Thegalaxyis small amorphousgalaxywhoseredshiftisunknown. similar haloshouldbepresent(butsomewhatfainter)around a “halo”duetoreflectionsinthefocalreducer’soptics.A armlike featureextendedtotheSE. the Seyfertgalaxy;extendedmaterialclearlyextendswell 0328-032 (Mrk6/2).—TheSeyfertisthenorthernbarred 0434—103 (Mrk618).—Thesmallspiralcompaniontothe 0339-013 (NGC1409,NGC1410).—Ahighlydistorted 0739+500 (Mrk79).—Thisbarredspiralgalaxymayhave 0804+391 (Mrk622).—Thisamorphousgalaxymightbea 07333-585 (Mrk9).—Thisgalaxyappearstobedisturbed 0922+523 (Mrk110).—Thishighlypeculiargalaxyhasa 1124+353 (Mrk423).—Dahari(1985)findsthattheinter- 1207+472 (Mrk795).—Thisgalaxymaybeasymmetric 1202+204 (NGC4074).—Thisfeaturelessgalaxyexhibits a 0446-062 (NGC7667).—Thisspiralgalaxyappearsto 1216+301 (Mrk766,NGC4255).—This barredspiralap- 0514-001 (Mrk1095,Akn720).—Theimageiscompli- © American Astronomical Society • Provided by theNASA Astrophysics Data System SEYFERT GALAXIES.I. -1 -1 -1 images inthe[Oni]À5007linefor-25ofgalaxies the paper; seeMacKenty1986for imagesofit.) will thereforebeconsidered “normal”inthecontextof present study.(Animageof this galaxyisnotincludedin present sample.Mrk315wastheonlygalaxytoshowsuch a length of~80kpc(MacKenty1986).Thisfeaturewas dis- ing approximatelyattheendofextension.Exceptfor peculiar galaxyinthesample.Theextensiontosouth galaxy doesnotappearpeculiar inthebroad-bandimagesand dramatic feature.WhileMacKenty(1986)interpreted this irregular companionwithafainttailtothewest. redshift differenceof600kms(Adams1977). with faintouterarms.TheellipticalgalaxytotheSWhasa plume, thisgalaxymightbeclassifiedasanedge-onspiral. panion hasabrighttailextendingtothenorthandredshift pears tobeassociatedwiththegalaxy.Thereisalsofaint redshift differenceof-890kms(Dahari1985). feature asaprobableremnantoftidalinteraction, this covered intheprocessofobtainingnarrow-band(80 A) asymmetric halotothesouth. difference of220kms(Dahari1985). most luminousgalaxiesintheIRAScatalog(seeFairclough distored aswell.DiesmallsegmentpointingtowardtheSE its high-infraredluminosity(RiekeandLow1975), plume extendingtothenorth. extraordinary ionizedgasjetlikefeatureextending60kpc to spiral galaxy.Theredshiftofthecompanionisunknown. The companion(IZw121-2;Adams1977)isprobablya example ofatidalinteractionwithbridgeconnectingthe (see e.g.,WilsonandUlvestad1982)hasadistortedinnerarm diffuse materialextendingtotheNE.Thisgalaxyisoneof defies easyclassification.Thecompaniontotheeasthasa unusual morphologyhasbeenrecentlynotedbyHutchings the NWandthenbendingbacktowardSEforatotal de RobertisandPooge1986;Heckmanetal.1986)hasan to theNNWwithasickle-shapedplumeeastoriginat- system andafaintouterarmthatendsindiffuseregionto 1986). approximately one-thirdofthewayalongextensionap- the nucleus.Thebodyofgalaxyitselfissignificantly appears tocomeanabruptendanddoesnotpointback and Neff(1986). diffuse extendedregiontotheSSE.Thisgalaxyisknownfor Seyfert (thesouthwesterngalaxy)toitscompanion.Diecom- appearance totheSWandatailNNE.Thereisalso tinguished spiralincontinuumimages.However,thereis an the NNE. 2041—105 (Mrk509).—Thisamorphousgalaxyhasan 2302+22 (Mrk375).—Thegalaxyappearstobeanundis- 1721+310 (Mrk506).—Thisgalaxyhasaprominentring 1535+544 (Mrk486).—Thisgalaxyhasajetlikeextension 1439+534 (Mrk477,1Zw92).—Thissystemisagood 1416+252 (NGC5548).—Thiswell-studiedSeyfertgalaxy 1343+561 (Mrk273).—Thisgalaxyisperhapsthemost 1339+304 (Mrk268).—Thisgalaxyispossiblyaspiralbut 2301+084 (NGC7469).—Thiswell-studiedSeyfert(e.g., 1254+571 (Mrk231).—Thispeculiargalaxyhasa“lumpy” 1221+030 (Mrk50).—Thisamorphousgalaxyhasafaint 239 19 90ApJS. . .72. .231M _1 -1 _1 240 ing the“companion”galaxyandextendingbeyondit.The original assertionbyArp(1971)thatthe“arm”endedat redshift 7700kmsgreaterthanthatoftheSeyfert(Arp recently bySharp(1986).ThesmallgalaxytotheSEhasa long “tidaltails,”oneextendingtotheENEandother Toomre 1972)interactioninthissample.TheSeyfertisthe difference of—270kms(Dahari1985;JWM),andboth extending totheNW.Theellipticaleasthasaredshift “companion” galaxyisnotborneoutbythedeeperimages. the CCDimagesobtainedhereshowtwoarmsortailscross- 1971; Dahari1985;JWM).InagreementwithSharp(1986), spiral galaxyhasbeendiscussedbyArp(1971)andmore prevalance ofdisturbed,interacting,orpeculiargalaxies.Many spiral galaxytothewestinthissmallgroup.Itdisplaystwo of theremaininggalaxieshavebarsorrings.Half the twosmallergalaxieshaveredshiftswithin300kmsof the bestexampleofa“classical”Toomre-type(Toomreand images aresuggestiveofthepresencespiralarms,abaror bars. (either intrinsicallyorastheresultofresolution galaxies (27%ofthesample)asbelongingtoaspecialclass galaxies inthissamplehaveeitheradisturbedmorphologyor to bedistortedandhasemissionlines. the Seyfertgalaxy(JWM).ThesmalltoSEappears ation, then35%ofall“spiral”Seyfertgalaxiesinthesample sequences isshowninTable4.Ifwetreatalltheamorphous a bar.Thetwo-dimensionaldistributionoftheclassification given inparentheses.Withthealternativeclassifications,65% ring, oradistortedmorphology,analternativeclassificationis (11), representfairlyconservativeassignments.Wherethe are peculiarand70%haveeitherdisturbedmorphologiesor available images;see§Yld)andexcludethemfromconsider- either abarordisturbedmorphology. of allgalaxiesand79%nonamorphoushave 13 andperhapsasmany17havebars(25%-33%).In the “normal” galaxies.Ofthe51galaxiesinthissample,atleast 2316-000 (Mrk530,NGC7603).—Thishighlydisturbed 23253-083 (Mrk533,NGC7674).—Thisgalaxyisprobably The moststrikingresultofthissurveyisthewidespread The classificationsassignedinTable1,columns(10)and The fractionofbarredspiralsisthesameasfoundin © American Astronomical Society • Provided by theNASA Astrophysics Data System 0 92114 MC 0123Total Total ...3275 51 3 910313 2 81313 1 6320 11 Two-Way MorphologyClassifications a) Morphologies VI. DISCUSSION TABLE 4 IC MACKENTY barred spiral(MC=2)orthe spiral(MC=1)galaxies. (MC =3)galaxiesmoreoften havebluenucleithaneitherthe (0.54, 0.10).TheB-Vcolorsofthenuclei(0.61,0.26)and of nuclei (mean=0.59,standarddeviation0.09)andthedisks shown inFigure7.Theamorphous (MC=0)andpeculiar distribution oîB-Vcolors forthenucleianddisksis referred toasthe“nucleus”and“disk”apertures. The 5kpcdiameteraperturewasselectedasthesmahest region between5and10kpcinradiusfromthenuclei(i.e., the disks(0.75,0.17)show a muchgreaterdispersion.The system (oraforegroundstarinthecaseofMrk110).While galaxies (MC=3)aregenerallybrighter.Inthreeinstances essentially theentiredetectedgalaxyinnearlyallcases),fora profiles (§IVû)aretabulatedinTable1,columns(16)-(24), ies (e.g.,MalinandCarter1983).Probablyonlyafewpercent 3 galaxies. these galaxesareamongtheleastluminousofMC = this wouldacttoincreasethetotalmagnitudeofsystem, the nucleusandbulge.Theseapertureswillhenceforthbe annulus waschosentobeoutsideoftheregiondominatedby for eachgalaxya30kpcdiameteraperture(encompassing When thatfractioniscomparedtothe25%-35%of be foundinpeculiarordisturbedsystems.Determiningthe the photometryincludessecondnucleusofaninteracting tudes forthe30kpcapertures.Thepeculiaranddisturbed the observationswithpoorestresolution.The5-10kpc achievable withoutbecomingsmallerthantheseeingdisksof the annulushasinnerandouterdiametersof1020kpc). 5 kpcdiameteraperture,andforanannuluscoveringthe warranted. liarities, amorecarefulstudyofthesegalaxiesisclearly in factdonothaveundetectedbarsormorphologicalpecu- evident thattheSeyfertgalaxiesarestrikinglyunusual. (1984) usedtheworkofArpandMadore(1977)toestimate of allspiralgalaxieswouldbeclassifiedaspeculiaronthe gies issomewhatdifficult.Suchclassificationsdependonboth fraction ofallgalaxieswithpeculiarordisturbedmorpholo- infrared luminosityofnucleiisenhancedinbarredgalaxies. ited bars.Thepresenceofabarisnonethelessinterestin revised Shapley-Amescatalog(SandageandTammann1981), Excluding thosewithcompanions(IC=2orIC3)de- galaxies inthesampleareundisturbedspiralswithoutbars. galaxies inthissamplethatexhibitpeculiarmorphologies,itis system usedinthisstudy.Lonsdale,Persson,andMatthews for example,the“shells”foundaroundsomeellipticalgalax- creases thisfractionto18%(10%).Ifthefewisolatedspirals that 3%-6%ofallgalaxiesmightbeclassifiedaspeculiar. the limitingsensitivityofobservationsandresolution; references therein).Hawardenetal(1986)reportthatthe rial intotheinnerregionsofgalaxies(Heckman19806,and 26% ofallspiralgalaxiesand36%SaO-Sbcexhib- the contextofthispapersincebarsappeartochannelmate- There isverylittlevariationintheK-Æcolorsofboth Figure 6showsthedistributionofabsoluteVmagni- Magnitudes andcolorsderivedfromthecircularlyaveraged Only 22%(18%inthealternativeclassifications)of Seyfert galaxiesaremorelikelythannon-Seyfertto b) MagnitudesandColors Vol. 72 19 90ApJS. . .72. .231M -2 -2 The peculiargalaxies(MC=3)tendtobebrighterthanaverage.key Table 1,columns(15)and(25)-(27).Galaxieswithb/a< 0.5 kpc (Boroson1981).Theresultsoffittinganexponential disk inclination andextinctionwithinourGalaxyby model tothegalaxiesinpresentsamplearereported in nesses ofthediskstendtoclusteraround21.85magarcsec at thetopofthisfigurealsoappliestoFigs.8-10and12-13. are shownwitheachmorphologicalclass(MC)asindicatedbythekey. brightness is21.9Bmagarcsec (withaladispersionof1.0 fall withintherangeof1to5kpc(Freeman1970)and10 (this valueisindependentofdistance).Thediskscalelengths extensively (Freeman1970;Burstein1979a,b\Boroson1981) mag). Thecorrectionforthe useofcircularlyaveragedpro- are indicatedinTable1,column(15),andexcludedfrom and galaxieswhoseprofileslackanidentifiable“disk”region and displaysomeconsistentproperties(butseeKormendy b/a =0.6-0.8.Thisvaluefor themeancentralsurfacebright- the followinganalysisofdiskparameters. 1977). Boroson(1981)foundthatthecentralsurfacebright- files wasfoundempiricallyto belessthan0.2maginRfor are showninFigure8.The meancorrectedcentralsurface No. 2,1990 The diskcomponentsofspiralgalaxieshavebeenstudied The centralsurfacebrightnessesinÆ,correctedfortheir Fig. 6.—TheabsoluteVmagnitudeswithin30kpcdiameterapertures n £(0) =B(0)+2.5log(a/b)-0.2esc|Z>| c © American Astronomical Society • Provided by theNASA Astrophysics Data System c) Decompositions 0 123 Morphological Class M (30kpc) v SEYFERT GALAXIES.I. -2 images. Adams(1977)discussed fourofthese(Mrk335 Mrk 509[2041+105])and considered themunresolvedor in resolutionandredshift.Thepresenceoftheamorphous [0004+200], Mrk50[1221+030], Mrk290[1535+580],and galaxies isevidentlynotdue to anylimitationsintheavailable classification cannotbeexplainedbypoorresolution.Figures resolution, anditisthereforedifficulttoclassify(although its kind offeaturebutaredifficulttoclassify(i.e.,Mrk 372 11 and12showthedistributionofmorphologicalclasses amorphous galaxiesinthesamplewhoselackoffurther CCD images).Evenwithoutthesefivegalaxies,thereareeight companion ofthesamesizehasvisiblestructurein Mrk 268[1339+304],and817[1435+590]).Furthermore the observationsofMrk609(0323—062)haverelativelypoor [0247T191], Mrk622[0804+391],NGC4074[1202+204], (e.g., Adams1977).Thesegalaxiesconstitutebetween18% and 27%ofthesample.Severalthesegalaxiesshowsome or unresolved”havedrawnonlylimitedattentioninthepast lengths lessthan-2kpc.Theimplicationoftheobserved larger thanaverage.Freeman(1970)foundthattherangeof lengths andmajoraxisofthepeculiargalaxiestobe early-type spirals. distribution isthatSeyfertgalaxiesaregenerallyfoundin inverse correlationbetweenthefractionofluminosityin profiles insideof10"andtypicallybegin15"ormorefrom A comparisonoftheregionsYee(1983)selectedforhisdisk 7 kpc),whilelate-typespiralgalaxiesgenerallyhavescale generally smaller.Theremaybeatendencyforboththescale mag arcsecisophoteoftheamorphousgalaxiesarealso correlation isseenwiththe5-Fdiskcolors. within a32kpcdiameteraperture(seeYee1983)isshownin brightnesses thannormalspirals(hefoundanaveragevalue ness isingoodagreementwiththevaluesofFreeman(1970) spiral galaxieshavealargerrangeinscalelengths(upto the scalelengthsiscorrelatedwithmorphology.Early-type a resultofthebluecolorsSeyfertnuclei,thereisan Figure 9.Thereisapossibletendencyforboththepeculiar nuclei ofthegalaxiesinhisfitsto“disk”components. of 21.3).Thatfindingisnotconfirmedbythepresentresults. the othergalaxies.Thelengthsofmajoraxesat24th amorphous galaxiesgenerallyhaveshorterscalelengthsthan the diskcomponentandR—Fcolorsofnucleus;no the spiralandbarredgalaxies.Asmightbeexpectedas detector usedinhisstudy.Itseemsprobablethatthisinadver- 25" fromthecloseronesduetolimitationsofSIT found. Thefitsreportedhereseldomincluderegionsofthe fits mayexplainthehighercentralsurfacebrightnesseshe and theamorphousgalaxiestohavelessdominantdisksthan and 15"fromthemoredistantgalaxiesbetween10" and Boroson(1981).Yee(1983)tentativelyconcludedthat tently includedasizablecontributionfromthebulgesor the centersofgalaxies.Yee(1983)fitprofilesbetween5" Seyfert galaxiesmighthavesomewhatbrightercentralsurface The classofSeyfertgalaxiesclassifiedhereas“amorphous The diskscalelengths(r)areshowninFigure10. The fractionoftheluminosityindiskcomponent 0 d) AmorphousGalaxies 241 19 90ApJS. . .72. .231M 242 second. Noparticulartrendwithmorphological classisevident. exponential diskcomponentsare shown inmagnitudespersquarearc- morphological class. Fig. 8.—Thecentralsurfacebrightness inBobtainedfromfittingthe Fig. 7.—TheB-Vcolorswithina5kpcdiameterapertureareshownagainsttheB © American Astronomical Society • Provided by theNASA Astrophysics Data System > ÛQ < Lf) CD Cl O) O Û. i 0.2 0.4 0.6 0.8 0.4 0.6 0.8 0.2 1.2 1.2 i 1 0 0.20.40.60.811.2 J IL MC =2 MC =0 T ■ MACKENTY Disk B-V in Figure13.Althoughtheamorphous galaxiespreferentially potential ellipticals.TheB-Vcolbrsofthe“disk”regions of axial ratios(6/0)atthe24th magnitudeRisophoteisshown shorter exponentialdiskscale lengths.Thedistributionofthe these galaxiesarenotparticularly redcomparedtotherestof the sample.Thesegalaxies tend tohavesmallersizesand (MC =1)andpeculiargalaxies=3)appeartohavesomewhatless of their totalluminosityindisks. V passbandisshownbymorphologicalclass.Bothamorphousgalaxies Fig. 9.—Thefractionoftheluminosityinexponentialdisks 0 0.20.40.60.811.2 i V colorswithina5-10kpcradiusannulusforeach MC =3 MC =1 ~i r Disk Fraction Vol. 72 19 90ApJS. . .72. .231M 1 kiloparsecs. Itisclearthattheamorphous classificationdoesnotreflect The resolutionisdefinedhereas the sizeofseeingdiskexpressedin merely inferiorimagery. shown fortheobservationsof galaxiesineachmorphologicalclass. other Seyfertgalaxiesatthesameresolutionwereclassified,it confirmed. entire rangeofobservedratios.Keel’s(1980)findingthat No. 2,1990 Seyfert galaxiesgenerallyhaveratiosofgreaterthan0.5is appear circularor“face-on,”theyoccupyessentiallythe shorter scalelengths. by morphologicalclass.Theamorphousgalaxies(MC=0)generallyhave Fig. 11.—Theresolutionoftheshort-exposure photometricimagesis In lightofboththeaboveandrelativeeasewithwhich Fig. 10.—Theexponentialdiskscalelengths(inkiloparsec)areshown © American Astronomical Society • Provided by theNASA Astrophysics Data System MC=0 MC=1 RESOLUTION (kpc) r o (kpc) SEYFERT GALAXIES.I. colors oftheMC=0galaxies.NoreauandKronberg(1986) blue compactgalaxies(seeSandageandBrucato1979;Thuan into thelifetimeofSeyfertphenomena.Tosomeextent interactions ormegers.Ifthisisindeedthecase,astudyof interpretation isthatthesegalaxiesaretheremnantsofprior redshift. Thisfurtherillustratestherealityofamorphousclass probably theresultofbar’sinfluence ontheellipsefittingprocedure. discuss anamorphousgalaxyininteractingsystem.Several (1979) reportmeanB—Vcolorsof~0.6inaccordwiththe galaxies. the amorphousgalaxiesresembleclassIIirregularor are intrinsicallyamorphous.Sincetheircolorsindicatethat appears thatamajorityoftheamorphous(MC=0)galaxies round, asignificanttailexistsof more ellipticallyshapedgalaxies.The 1983; NoreauandKronberg1986).SandageBrucato tendency forthebarredspirals(MC =2)toavoidappearingface-onis function ofmorphology.Although mostoftheamorphousgalaxiesare the stellarpopulationofthesegalaxiesmightprovideinsight these galaxiesareunlikelytobeellipticalgalaxies*apossible Fig. 12.—Themorphologicalclassesaredisplayedasafunctionof Fig. 13.—Theminortomajor axis ratios(b/a)areshownasa : 0 500010000 — 1IIII1111II:;:j:T-F- i 1r Redshift (km/s) b/a 243 19 90ApJS. . .72. .231M 244 John W.MacKenty: SpaceTelescopeScience Institute,3700SanMartin Drive,Baltimore,MD21218 represent asignificantfractionofallSeyfertgalaxies.Ifthe bations ormergersisindeedcorrect,thenanevenlarger Wehinger andWyckoff(1977),Simkin,Su,Schwarz star formationinthesegalaxies(e.g.,Gondhaleharetal.1986). authors haverecentlydiscussedthepossibilityofsignificant disruptions. fraction oftheSeyfertgalaxieshaveevidenceforlarge-scale material intotheirnuclei(i.e.,abarorexternalperturbation) speculation thatthesegalaxiesaretheresultofearlierpertur- appears thatSeyfertgalaxieswithoutamechanismformoving (1980), andYee(1983)intwomajordimensions.First,it are theexceptionratherthanrule.Second,classof Seyfert galaxieswithamorphousmorphologiesappearsto .19826,Ap.J.,256,798. .1982û,Arm.Rev.Astro.Ap.,20,431. .19796,Ap.J.,234,435. Arp. H.C,andMadore,B.F.1977,Quart.J.R.A.S.,18,234. Arp, H.1971,Ap.Letters,1,221. .1985,Ap.J.Suppl.,57,643. Adams, T.F.1977,Ap.J.Suppl.,33,19. Balick, B.,andHeckman,T.M.1981,Ap.J.,247,32. Boroson, T.A.,andOke,J.B.1982,Nature,296,397. Boroson, T.1981,Ap.J.Suppl.,46,177. Balzano, V.A.1983,Ap.J.,268,602. Christian, C.A.,Adams,M.,Barnes,J.V.,Butcher,H.,Hayes,D.S., Burstein, D.1979û,Ap.J.Suppl.,41,435. Boroson, T.A.,Persson,S.E.,andOke,J.B.1985,Ap.J.,293,120. .19806,Astr.Ap.,88,365. de Grijp,M.H.K.,Miley,G.Jub,J.,andJong,T.1985,Nature, de Vaucouleurs,G.,andA.1975,Ap.J.(Letters),197, de Robertis,M.M.,andPogge,R.W.1986,A.J.,91,1026. de Robertis,M.1985,A.J.,90,998. Dahari, O.1984,Ph.D.thesis,UniversityofCalifornia,SantaCruz. Hutchings, J.B.,andNeff,S.G.1987, inIAUSymposium121,Observa- Hutchings, J.B.,Crampton,D.,Campbell, B.,andPritchet,C.1981,Ap. Hutchings, J.B.,Crampton,D.,andCampbell,B.1984,Ap.J.,280, 41. Gaskell, C.M.1985,Nature,315,386. Freeman, K.C.1970,Ap.J.,160,811. Fosbury, R.A.E.,etal.1982,M.N.R.A.S.,201,991. Fairclough, J.H.1986,M.N.R.A.S.,219,IP. Diego, F.1985,Pub.A.S.P.,97,1209. Hutchings, J.B.,Crampton,D.,Campbell, B.,Gower,A.C,andMorris, Huchra, J.P.,Wyatt,W.F.,andDavis,M.1982,A.J.,87,1628. Huchra, J.,andSargent,W.L.1973,Ap.186,433. Heasley, J.N.1984,privatecommunication. Gunn, J.E.1979,inActiveGalacticNuclei,ed.C.HazardandS.Mitton Gondhalekar, P.M.,Morgan,D.H.,Dopita,andEllis,R.S.1986, Heckman, T.M.1980a,Astro.Ap.,87,152. Hawarden, T.G.,Mountain,C.M.,Leggett,S.K.,andPuxley,P.J.1986, Heckman, T.M.,Beckwith,S.,Blizt,L.,Skrutskie,andWilson, A. S. Heckman, T.M,Balick,B.,andSullivan,W.T.,III.1978,Ap.J., 224, Huchra, J.,Davis,M,Latham,D.,andTonry,J.1983,Ap.Suppl., 52, Hlivak, R.J.,Henry,J.P.,andPilcher,C.B.1984,Proc.SPIE,445, 122. Hewitt, A.,andBurbidge,G.1980,Ap.J.Suppl.,43,57. Heckman, T.M.,Bothun,G.D.,Balick,B.,andSmith,E.P.1984, A.J., J., 247,743. 314, 240. Mould, J.R.,andSiegel,M.1985,Publ.A.S.P.,97,363. (Cambridge: CambridgeUniversityPress),p.213. LI. The resultsofthisstudyextendtheworkAdams(1977), tional EvidencesofActivityGalaxies, ed.E.Ye.Khachikian,K.J. S. C.1982,Ap.J.,262,48. M.N.R.A.S., 219,505. 89, 958. M.N.R.A.S., 221,41P. 1986, Ap.J.,305,157. 745. 89. © American Astronomical Society • Provided by theNASA Astrophysics Data System VII. SUMMARY MACKENTY REFERENCES Yee, H.K.C.1983,Ap.J.,272, 473. Wyckoff, S.,Wehinger,P.A.,and Gehren,T.1981,Ap.J.,247,750. Wilson, A.S.,andUlvestad,J.S. 1982, Ap.J.,260,56. Watanabe, M.,Kodaira,K.,andOkamura,S.1982,Ap.J.Suppl.,50, 1. Wilson, A.S.,andMeurs,E.J. 1982,Astr.Ap.Suppl.,50,217. Wehinger, P.A.,andWyckoff,S. 1977, M.N.R.A.S.,181,211. Weedman, D.W.1977,Ann.Rev. Astr.Ap.,15,69. Ward, M.J.,andWilson,A.S.1978,Astr.Ap.,70,L79. Toomre, A.,andJ.1972,Ap.J.,178,623. .1987,Ap.J.,316,584. Veron-Cetty, M.P.,andVeron,P.1984,ESOSei.Rept.,No.1. Thuan, T.X.1983,Ap.J.,268,667. Thompson, L.A.1986,Ap.J.,300,639. Theys, J.C,andSpiegel,E.A.1976,Ap.J.,208,650. .1982,Ap.J.,257,33. .19856,Ap.J.,294,486. .1985a,Ap.J.,294,479. Sulentic, J.W.,andTifft,W.G.1973,TheRevisedNewGeneralCatalogue Stockton, A.,andMacKenty,J.W.1983,Nature,305,678. Stockton, A.1978,Ap.J.,223,747. .1985,A.J.,90,1449. Stauffer, J.R.1982,Ap.J.,262,66. Simkin, S.M.,Su,H.J.,andSchwarz,M.P.1980,Ap.237,404. Norman, C,andSilk,J.1983,Ap.J.,266,502. Sharp, N.A.1986,Ap.J.,302,245. Schinckel, A.,andPhillips,M.1983,ACatalogueofActiveGalaxies, Sandage, A.,andTammann,G.A.1981,ARevisedShapley-AmesCata- Sandage, A.,andBrucato,R.1979,T.7.,84,472. Roos, N.1981,Astr.Ap.,104,218. Rieke, G.H.,andLow,F.J.1975,Ap.(Letters),200,L67. Osterb rock,D.E.1984,Quart.J.R.A.S.,25,1. Noreau, L.,andKronberg,P.1986,A.J.,92,1048. lege ScientistsFoundationandNationalScience preparation. TheSTScIartdepartmentaidedintheconstruc- his support,encouragement,andguidance.JimHeasley,Laird Mirabel, I.F.,andWilson,A.S.1984,Ap.J.,277,92. Meurs, E.J.A.,andWilson,A.S.1984,Astr.Ap.,136,206. providing acomputertapeofhisunpublishedcatalog indebted toCarlPilcherforprovidingmewithhisfilterwheel helpful commentsonthismanuscript.Ihavehad Thompson, GarethWynn-Williams,andAndrewWilsonmade Markarian, B.E.,Lipovetskii,V.A.,andStepanian,D.A.1979,As- Markarian, B.E.,andLipovetskii,V.A.1974,Astrofizika,10,307. Markarian, B.E.1967,Astrofizika,3,55. Malkan, M.A.,Margon,B.,andChanan,G.A.1984,Ap.J.,280,66. Malin, D.F.,andCarter,1983,Ap.J.,274,534. MacKenty, J.W.1986,Ap.J.,308,571. Kormendy, J.1977,Ap.J.,217,406. grants AST83-17457and80-22203toAlanStockton. Bob Fflivak,CarlPilcher,andPatHenrymadetheGalileo/ discussions withOvedDahari,GaryHill,andBrentTully. MacKenty, J.W.,andStockton,A.1984,Ap.J.,283,64. Lonsdale, C.J.,Persson,S.E.,andMatthews,K.1984,Ap.287,95. Lawrence, A.,andElvis,M.1982,Ap.J.,256,410. Landolt, A.U.1983,A.J.,88,439. Keel, W.C.1980,A.J.,85,198. active galaxies.LouiseGoodhelpedwiththemanuscript assembly. FrankCheighandthestaffofUH88inch IfA CCDcamerasystemaveryusefulinstrument.Iam Kalloglian, A.T.1971,Astrofizika,7,521. the HonoluluChapterofAchievementRewardsforCol- tion ofthefigures.Financialsupporthasbeenprovidedby telescope weremosthelpful.IamgratefultoA.Schinckelfor of NonstellarAstronomicalObjects(Tucson:UniversityArizona Press). (Anglo-Australian Observatory),unpublished. ington), p.91. log ofBrightGalaxies(Washington,DC:CarnegieInstitutionWash- trofizika, 15,549. Fricke, andJ.Melnick(Dordrecht:Reidel),p.399. I amdeeplygratefultomythesisadvisorAlanStocktonfor Vol. 72