1989AJ 98. .367F 1 8 367 Astron.J.98 (2),August1989 0004-6256/89/020367-52$00.90 © 1989Am. Astron. Soc.367 bution ofmasswithinclustersgalaxies.Byvirtuesheer within clusters.Furtherinformationonthedynamicalhis- numbers, dwarfgalaxiesofferimprovedstatisticsonthera- verse, theyareusefulastestparticlesforstudyingthedistri- indicators ofthelarge-scaledistributionmatterinuni- galaxies inbothhigh-andlow-densityregionsofthelocal nous galaxieshasonlyrecentlybecomebothtechnicallyfea- nized formanyyears,findingandcatalogingtheless-lumi- luminous, massivegalaxies.Whilethisbiashasbeenrecog- galaxies inclusters,andisno doubt duetoenvironmental ments). Typesegregationis observed amongluminous ies arenottheproductsofcollisions (eithermergersorfrag- ent ifaclusterisdynamicallyrelaxed andmostofthegalax- on thebasisofequipartition energyandshouldbeappar- of galaxiesbymassandtype. Mass segregationisexpected tory ofclustersmaybeobtained bystudyingthesegregation dial distributionofmassandontheextentsubclustering universe. universe. Testingthispossibilityrequiresacensusofdwarf that theywillmoredirectlytracethemassdistributionin peaks intheinitialfluctuationspectrum,thenitispossible tic constituentoftheuniverse.While“characteristic” sible andscientificallyinteresting. side theLocalGrouphavebeenstronglybiasedinfavorof clusters ofgalaxies.Ifthedwarfgalaxiesformatsmaller have fl=1inspiteoftheinsufficientmassmeasured function is—10L,anaveragegalaxyshineswith,at luminosity ofagalaxy(L*)atthebreak the underlyingmassdistributioninuniverse(Kaiser that brightgalaxiesaremuchmorestronglyclusteredthan terest intheseaveragegalaxiesstemsfromthespeculation most, afeeble10L.Fromcosmologicalviewpoint,in- THE ASTRONOMICALJOURNAL 1985; BardeenDavisa/.1985),makingitpossibleto 0 0 0 POPULATION STUDIESINGROUPSANDCLUSTERSOFGALAXIES.II.ACATALOGGALAXIES Even iflow-luminositygalaxiesturnoutnottobeusefulas Dwarf galaxies,bynumber,arefarthedominantgalac- Until recently,investigationsofgalaxypopulationsout- © American Astronomical Society • Provided by the NASA Astrophysics Data System Department ofPhysicsandAstronomy,CenterforAstrophysicalSciences,TheJohnsHopkinsUniversity,Baltimore,Maryland21218 -1 hm M —13.0,assumingadistancemodulusofm—AT=31.9)andcontainslikelymembersdowntoB background galaxies.Forclustermembers,thislistingshouldbecompletetoR—18(corresponding large-scale (10.9"mm)platestakenwiththeduPont2.5mreflectoratLasCampanasObserva- are few,ifany,clustermemberscontainedinthesampleofbackgroundgalaxies. from backgroundgalaxies.Radialvelocitiesareincludedfor89galaxiesinthesurvey,providinga surface brightness,dwarfgalaxiesintheclustercanbedistinguishedwithahighdegreeofcertainty the sky.Thecatalogisessentiallydiameterlimited,withalimitingof17"atanisophoteB tory, andfromdigitalphotometryofanESO/SRCbluesurveyplatecoveringroughlythesamearea This paperpresentsacatalogof2678galaxieswithinanarea~40°sq.centeredontheFornax spatial distributions,wefindacoreradiusof0.7°forKingmodelfittothecluster,andshowthatthere cluster componentsuperimposedonauniformbackground.Usingmaximum-likelihoodfitstothese galaxies, wemodelthespatialdistributionofvarioustypesgalaxiesassumaKing reliable indicatorofmembershipinthesecases.Asadditionalsupportforourrejectionbackground Cluster ata~335and—35.7°.Thedatahavebeenobtainedfromvisualinspectionof26deep 5tT T — 20.Clustermembershipisforthemostpartbasedongalaxymorphology.Byvirtueoftheirlow — 26.5.Withinthissurveyregion,thecatalogincludes340likelyclustermembersand2338 T I. INTRODUCTION IN THECENTRAL3.5°OFFORNAXCLUSTER Received 12January1989;revised23February1989 Henry C.Ferguson VOLUME 98,NUMBER2 ABSTRACT -1 -1 telescope, therecentlycompletedVirgoClusterSurvey number ofexposures.BasedonplatestakenwiththeduPont with reasonableintegrationtimesanda mann, andTarenghi. permutations andcombinations ofBinggeli,Sandage,Tam- from 1984to1987inTheAstronomical Journal,byvarious Virgo Clusteritselfweresetout inaseriesofsevenpapers dwarfs. Theobservedproperties ofthesegalaxiesandthe the observedgalaxiesinVirgo surveyareclassifiedas toward luminous,massivegalaxies.Approximately80%of to asBST85)hasdonemuchremedythepre-existingbias nearby clusterscanbesurveyedtofaintlimitingmagnitudes brightnesses ofthegalaxiesandlargeangularextent a largefieldofview(1.5°X1.5°).Giventhisview, panas combineshighspatialresolution(10.9"mm)with Vaughan 1973),theduPont2.5mtelescopeonLasCam- lution iscrucialforweedingoutbackgroundcontaminants. ily determinedonthebasisofmorphology,additionalreso- the clusters.Searchesforsuchgalaxiesoverlargeareasof nearby clustersstemsfromthesmallsizesandlowsurface cesses thatmaybeinvolved. ments arethereforenecessarytoidentifythephysicalpro- of bothbrightandfaintgalaxiesinawidevarietyenviron- axy massandclusterproperties.Studiesofthepopulations observed typesegregationdependindifferentwaysongal- or later.Mechanismsthathavebeenproposedtoexplainthe influences, operatingeitheratthetimeofgalaxyformation Because clustermembershipforthefaintgalaxiesisprimar- nax andVirgoclustersarereadilyapparentondeep48" small formatofCCDdetectors.DwarfgalaxiesintheFor- sky usingCCDsarecurrentlyimpracticalbecauseofthe ESO/SRC skysurveys;however,thesmallscale Schmidt plates,suchasthosetakenforthePalomarand (Binggeli, Sandage,andTammann1985,hereafterreferred (67" mm)makesmorphologicalclassificationdifficult. While theVirgoClusterSurvey hascontributedgreatlyto The technicaldifficultyinsearchingfordwarfgalaxies By virtueofitsuniqueopticaldesign(Bowenand AUGUST 1989 1989AJ 98. .367F lating theseresultsfromoneclustertotheuniverseatlarge. intrinsic propertiesofdwarfgalaxies,andthedynamical our knowledgeoftheluminosityfunctiongalaxies, by Shapley(1943),anddeVaucouleurs(1956),who function andthepropertiesofdwarfgalaxiesvaryfromclus- The nextobviousstepistoseewhetherthegalaxyluminosity state oftheVirgoCluster,onemustbecautiousinextrapo- few decades.Hodge(1978)publishedphotographicsurface gave itthedesignationG53inhiscatalogofnearbygroups schePs visittoSouthernAfricain1835.Thegroupwasnoted Fornax haspresumablybeenknownsinceSirJohnHer- the radiosourceFornaxA.Theconcentrationofgalaxiesin collection ofglobularclusters,andneartheoutskirtsby tration ofearly-typegalaxies,dominatednearthecenterby dage (1989). plates) isbeingundertakenbyBinggeli,Tarenghi,andSan- plementary investigationforthefield(basedonSchmidt data directlycomparabletotheVirgoClusterdata.Acom- additional nearbyclustersandgroupsofgalaxies,basedon of thisseriespapersistobeginsuchaninvestigationon ter toclusterorbetweenclustersandthefield.Thepurpose 368 HENRYC.FERGUSON:THEFORNAXCLUSTER berts andSadler(1984).Morphologicalstudiesofgalaxies photometry for13ofthebrightgalaxies,andphotoelectric members oftheclusterhavebeencarriedoutoverlast NGC 1316,abrightanddustyshellgalaxyassociatedwith NGC 1399,aluminousEOwithanextendedhaloandlarge Cluster. Thisclusterisnotableasasmallbutdenseconcen- aperture photometryhasbeenobtainedbySandage(1975) the successofrecentstudiesVirgoCluster,anumber and Griersmith(1982),amongothers.Ausefullistofthese group atCardiffandCambridgehasusedtheAutomatic dwarf galaxiesintheclusterbasedontheirmorphology ter. Thesesurveysareall,coincidentally,comingtofruition which hadverylowsurfacebrightnesses.Amoreextensive though thepresenceofthesegalaxieswasnotedbyShapley Chincarini, andRood(1975),Jones1980), ic andspectroscopicsurveyshavebeencarriedoutbyWelch, in theclusterhavebeenpublishedbyWirthandGallagher and otherphotoelectricobservationswascompiledbyLau- morphological-type distribution, andsurface-brightness- the region(Cawsonetal.1987;PhillippsDavies and CCDphotometryofselectedindividualgalaxies.A Schmidt plates,andhavefollowedthisupwithspectroscopy Bothun (1987,hereafterreferredtoasCB)haveidentified at aboutthesametime.Caldwell(1987)and of groupshaveundertakennewsurveystheFornaxClus- catalog compiledbyDuus(1979)hasneverbeenpublished. absolute magnitudesintherange—13.8to16.0,mostof as early1943.Thefirstcatalogofdwarfsintheregion ter beganwithHodge(1959,1960)andReaves(1964),al- Richter andSadler(1985). magnitude relationforthesample presentedinthepresent et al.1988).Finally,inPaperI ofthisseries(Fergusonand surface-brightness galaxiesfoundonaU.K.Schmidtplateof Plate Measuring(APM)machinetocatalogandstudylow- and thetwoothersisthat,inthis catalog,clustermember- paper. Theprimarydifference between thepresentcatalog Sandage 1988),wehavediscussed theluminosityfunction, (de Vaucouleurs1974).Extensivestudiesofthebrighter ( 1980,1984)andWirth1983),extensivephotograph- (Hodge, Pyper,andWebb1965)contained50objectswith This paperpresentsacatalogofgalaxiesintheFornax Spurred onbytherenewedinterestindwarfgalaxiesand Studies ofthelow-luminositydwarfmembersclus- © American Astronomical Society • Provided by the NASA Astrophysics Data System -2 their appearanceonlarge-scaleplates.Thefullcatalogcon- there werefarfewerdwarfspergiantinFornaxthanVir- This apparentdearthofdwarfsledCaldwelltoconcludethat survey, orbecausetheywerejudgedtobeinthebackground. missed, becausetheywerebelowthemagnitudelimitofhis not listedbyCaldwell(1987),eitherbecausetheywere tains 131additionallikelydwarfclustermembersthatwere ship forthefaintgalaxiesismostpartdeterminedby ranging from23.5to22.5Barcsec,galaxiesthatareap- cally compelling(seePaperI). number ofgalaxiesinFornaxthedifferencewasnotstatisti- difference inthegiant-to-dwarfratio,butwithsmall go. Basedonthecatalogpresentedhere,wealsofounda classifications ofthegalaxiesbasedonhigher-resolution parently exceedinglyrareinthelocalneighborhood.With galaxies, withabsolutemagnitudesMintherange—14.5 the principalobservationalverificationoftheory fact ofselectioneffects.Thisconclusioncallsintoquestion bution acrossthefaceofclusterasshowninPaperItends per IthatDaviesetalwereledtotheirconclusionbythe plate materialusedforthepresentsurvey,wearguedinPa- to —13andrelativelyhighcentralsurfacebrightnesses dwarf galaxyformationproposedbyDekelandSilk(1986). relation fordwarfgalaxies(Binggeli,Sandage,andTarenghi Fornax thatthewell-knownsurface-brightness-magnitude difficult todistinguishfromclusterdwarfsontheSchmidt presence intheirsampleofbackgroundgalaxiesthatwere If true,italsointroducesintoFornaxanewclassofdwarf present catalogis,onaverage,correct. plate material.Whileredshiftsarenotyetavailableforthe to confirmthattheirassignmentthebackgroundin putative backgroundgalaxies,theirprojectedspatialdistri- brightness spirals,suchasMalin1(Bothun,Impey,Malin, background galaxies.Inparticular,compactellipticalgalax- the importanceofcarefulclassificationbasedonlarge-scale tion. Furthermore,thediscoveryoflarge,low-surface- with large-scaleplates,however,certainclassesofcluster plates forweedingoutthebackgroundcontaminants.Even The actualcatalogislistedinSec.IV,withlikelycluster and Mould1987),indicatesthattheremaybebackground tainty inthefaintendofgiantellipticalluminosityfunc- ground giantellipticals.Thisisthemajorsourceofuncer- ies, suchasM32,arevirtuallyindistinguishablefromback- galaxies aredifficult,ifnotimpossible,todistinguishfrom sented inSec.II.ThephotometryisdiscussedIII. members byexaminingtheprojectedspatialdistributionof as clusterdwarfs.Whilemembershipinsuchambigu- giants lurkingamongthegalaxiesthathavebeenidentified 1984; Kormendy1985;Caldwell1987)waslargelyanarti- tion isthatthedistributionofbackground galaxiesappears ter componentamongthegalaxies thathavebeenrelegated catalog isanalyzed,totestwhetherthereadetectableclus- V, thespatialdistributionofgalaxiesvarioussubsets members andbackgroundgalaxieslistedseparately.InSec. the galaxiesinthissurvey. possible tosetconstraintsonthenumberofcluster ous casescan,inprinciple,beresolvedbyspectroscopy,itis to decreasetowardthecenter oftheFornaxCluster.We to thebackground.Anunexpected resultofthisinvestiga- B intergalactic dust.Acomparison toothercatalogsandalist discuss thepossibilitythatthis maybeduetoextinctionby Davies etal(1988)concludedfromtheirAPMsurveyof The differencesamongthevarioussurveysdemonstrate Details ofthegalaxyselectionandclassificationarepre- 368 1989AJ 98. .367F - -1 background galaxiesaredescribedindetailBinggeli,San- brightness, resolutionintoknots,luminosityclass,andradi- dage, andTammann(1985).Thesecriteriaincludesurface eters asbestwecouldwhenonlyoneplatewasavailable. of skypossiblewiththedataset,estimatinggalaxyparam- the twosetsofdata,buthaverathercoveredlargestarea not restrictedthiscatalogtotheoverlappingregionbetween ric parametersforthegalaxies.Forcompleteness,wehave whether ornottheyareclustermembers.TheSRCplatewas galaxies, themorphologicalcriteriaweremostfrequently al velocity.Becauseradialvelocitiesarelackingformost used todeterminethetotalmagnitudesandotherphotomet- used primarilyforclassifyingthegalaxiesanddeciding the surveyisshowninFig.1.TheLasCampanasplateswere corresponding to1.68".Theresultingimagecontained of selectingguidestarsfortheHubbleSpaceTelescope.The tized attheSpaceTelescopeScienceInstituteforpurpose plate #358,takenontheU.K.SchmidtTelescopeanddigi- with asuccessrateof98%whenradialvelocitiesbecame arrays fordisplayonavideomonitor.Theregioncoveredby SRC platecoversroughlythesameareawithascaleof supplemented withacopyoftheblueESO/SRCsurvey observations ispresentedinTableI.Thesedatahavebeen a side,withplatescaleof10.9"mm\Asummarythese Cluster, wheremembershipclassificationswereconfirmed used. ThesecriteriaprovedtobequitereliablefortheVirgo 67.3" mm.Itwasdigitizedwithapixelsizeof25/¿m, sion withexposuretimesof75min,eachcoverafield1.5°on scope. The50X50cmplates,takenonbaked103-aOemul- segrain cameraoftheLasCampanas2.5mduPonttele- obtained bySandagebetween1980and1981usingtheCas- VII, specialtypesofdwarfgalaxiesarelistedanddiscussed. 369 HENRYC.FERGUSON:THEFORNAXCLUSTER of crossreferencesispresentedinSec.VI.Finally, 14000 Xpixelsandwasbrokenupinto800pixel The criteriausedtodistinguishclustermembersfrom Photographs ofa6°XregiontheFornaxClusterwere © American Astronomical Society • Provided by the NASA Astrophysics Data System Fornax field b) Cluster-MembershipCriteria CD 1728-S CD 1717-S CD 171&-S CD 1655-S CD 1722 CD 1727-S CD 1702-S CD 1695-S CD 1674-S CD 1686-S CD 1708-S CD 1660-S CD 1661-S Plate a) Observations II. THESURVEY 3 4237.0 3 2417.7 3 3630.6 3 1811.3 3 1204.8 3 4238.1 3 3025.2 3 3631.7 3 4239.2 3 1812.3 3 2418.8 3 3026.3 3 3632.7 R.A. Dec. Plate center (1950) -33 0549 -33 0642 -33 0629 -33 0603 -33 0654 -34 2103 -34 2049 -34 2142 -34 2129 -34 2116 -35 3616 -35 3603 -35 3549 Table I.Summaryofobservations. 1981 Jan9 1981 Jan9 1981 Jan11 1981 Jan11 1981 Jan9 1980 Dec30 1981 Jan5 1981 Jan4 1981 Jan7 1981 Jan6 1980 Dec31 1981 Jan2 1980 Dec31 Exposure Date 1 -1 Fornax bership determinationwasopentoquestion.Galaxyclassifi- be clustermembersdowntotheplatelimit.Inaddition,we plates, weattemptedtoincludeallgalaxiesthatappeared duced. Differentcriteriawereusedforselectinggalaxies be nostrongevidencethatthesegalaxiesformadynamically based onthetwosetsofdataagreed,althoughtherewerea were alsocataloged.Morphologicalclassificationsas- potential clustermembership.Numeroussmallergalaxies image) werecataloged,regardlessoftheirmorphologyor solved tobeeasilyclassified,andgalaxieswherethemem- included backgroundgalaxiesthatwerewellenoughre- each catalog.InchoosinggalaxiesfromtheLasCampanas ed separately,andtwodistinctcatalogswereinitiallypro- as clustermembers. separate entityatadifferentdistance,wehaveincludedthem with radialvelocitiescomesfromthepossibilitythatNGC based onvelocities.Onepotentialambiguityforgalaxies number ofgalaxiesthatcouldberejectedaspossible panas plate.Inmostcases,themembershipclassifications significantly disagreedwerereinspectedontheLasCam- galaxies wheretheclassificationsfromtwosetsofplates log andtheLasCampanascatalogswerethenmerged, on theLasCampanasdata.Thediameter-limitedSRCcata- fications mustberegardedaslessreliablethantheonesbased signed tothegalaxiesbasedontheseimages,butclassi- larger than~17"(basedonvisualinspectionofalinearized galaxies ontheSRCplate,hereallwithamajoraxis sequence. Incontrast,becauseofthedifficultyclassifying author, andtypicallyagreedtowithinonemembershipclass cations wereperformedindependentlybySandageandthe subclump (deVaucouleurs1974).Becausethereappearsto is verylittleambiguityincluster-membershipassignments al velocitiesbetween2123kms~and4540sothere fact, therewerenogalaxiesintheregionwithmeasuredradi- members iftheyhadvelocitieslessthan2500kins.In in theFornaxfields,galaxieswereassumedtobecluster available. Whereradialvelocitieswereavailableforgalaxies 1316, NGC1365,andtheircloseneighborsformaseparate (see TableIV)andtowithinonedivisionintheHubble field The LasCampanasplateandtheSRCwereinspect- CD 1654-S CD 1687-S CD 1681-S CD 1680-S CD 1668-S CD 1667-S CD 1673-S CD 1713-S CD 1696-S CD 1703-S CD 1707-S CD 1712-S c) SelectionofGalaxiesfortheCatalog Plate 3 2419.8 3 4240.3 3 1813.3 3 3633.9 3 3027.3 3 2420.9 3 1814.4 3 3028.5 3 3635.0 3 4241.5 3 1815.5 3 2422.0 R.A. Dec. Plate center (1950) -36 5049 -35 3642 -35 3629 -36 5103 -36 4816 -36 5142 -36 5129 -38 0549 -38 0642 -38 0629 -38 0616 -38 0603 1981 Jan4 1981 Jan3 1980 Dec30 1981 Jan3 1981 Jan1 1981 Jan1 1981 Jan6 1981 Jan2 1981 Jan5 1981 Jan7 1981 Jan8 1981 Jan8 Exposure Date 369 1989AJ 98. .367F -2 jority ofbackgroundgalaxieshavebeenclassifiedfromthe ed bylow-surface-brightness dwarfs(dEand Im galaxies), within thattype.Atfaintmagnitudes, theclusterisdominat- pends ontherangeofsurface brightnessesanddiameters magnitude limitofourcatalog foragivengalaxytypede- to clustermembers,butnot backgroundgalaxies.The southern andeasternedgesof thesurvey,whereonlyLas greater than17"atanisophoteof27Bmagarcsec.Atthe log isbelievedtobecompleteforgalaxieswithdiameters lar. IntheregioncoveredbySRCplate,presentcata- Campanas plateswereused,this completenesslimitapplies extremely lowsurfacebrightnessesdisappearintothenight apparent surfacebrightnessesanddiameters.Galaxieswith classified basedontheLasCampanasplates,whilema- members withintheLasCampanassurveyregionhavebeen sky, whilegalaxieswithsmalldiametersbegintoappearstel- SRC platealone. du Pontplates.Thus,inthefinalcatalog,alllikelycluster survey. Thesegalaxieswerereinspectedandclassifiedonthe in theSRCsurveywhereitoverlapswithLasCampanas Only afewadditionallikelyclustermemberswereturnedup from dwarfirregularsandfaintbackgroundspirals. scale imageswasusefulfordistinguishingdwarfellipticals members (class3)basedontheirappearancethelarge- For faintergalaxies,theadditionalresolutionoflarge- of theseimageswerecompletelysaturatedontheSRCplate. Las Campanasplateswasessentialbecausethecentralparts scale plates.Forthebrightergalaxies,classificationon 370 HENRYC.FERGUSON:THEFORNAXCLUSTER The detectionofgalaxiesinanysurveydependsontheir © American Astronomical Society • Provided by the NASA Astrophysics Data System d) CompletenessLimits brighter thani?=19shouldbevisible. for thedwarfellipticals,butitis notpossibletoestimatethe face-brightness-magnitude relation similartotherelation to belostthenightskyati?~18,andbyB—20most slope orspreadintherelation with anydegreeofcertainty. ies thatappearunambiguously tobeirregulardisplayasur- have beenassignedtheclassification “dEorIm.”Thegalax- tremely difficult,andanumberofgalaxiesinthecatalog nesses, distinguishingbetweenadEandanImbecomesex- dwarfs areinvisible.Morethan90%ofthedEgalaxies the central2.4°ofFornaxCluster.Dwarfellipticalsbegin tude isindependentofmagnitude.Thecompletenesscorrec- brightness-magnitude relation,byassuming(a)thatthere- gulars intheluminosity profilesandsurfacebrightnesses, a Given thesimilaritiesbetween dwarfellipticalsandirre- luminosity (BothunetaL1986).Atlowsurfacebright- tions basedonthisassumptionwerecalculatedinPaperIfor lation extendsdowntothefaintestmagnitudesobservedand that theirregulargalaxieshavelargerscalelengthsatagiven Binggeli, andTammann1984),thereissomeindication the flatteningdistributionsarequitedifferent(Sandage, in thecluster.Thesurface-brightnessprofilesofImgal- dwarf ellipticalscanbemadebasedontheobservedsurface- axies arequitesimilartothoseofthedEgalaxies,although cult toestimatebecausesofewofthesegalaxiesareobserved face-brightness ellipticalgalaxiesandbluecompactdwarfs accompanied byasmallpopulationofcompact,high-sur- T (b) thatthespreadinsurfacebrightnessatagivenmagni- T (BCDs). The completenesslimitsforthedwarfirregularsarediffi- An estimateofthecompletenesscatalogfor tometer spots. regions oflowersensitivityneartheSensi- right-hand cornersoftheSRCplateare insets nearthelowerleft-handandupper plate aremarkedwithadashedline.The as solidlines.TheboundariesoftheSRC dividual LasCampanasplatesareshown marked asdots.Theboundariesofthein- axies fromTableIII(nonmembers)are members )aremarkedassquares,andgal- ies fromTableII(FornaxCluster Fig. 1.Mapoftheregionsurveyed.Galax- 370 1989AJ 98. .367F Bj imagewasconstructedfromtheCCDimagesbyapplying The imageswerethencomparedpixelforpixel.intensi- is thezero-pointdensityofphotographic emulsion.A,B, which thephotographicimage becomes saturated,andD where /istheCCDintensityin ADU,Z>isthedensityat els) removed.Thesedatawere then fitusingthefunction fitting withthecontributionfromdeviantpoints(badpix- pixel intervalstoprovideanequallyweightedsamplefor ty dataweresortedandthemedianvaluestakenin50 SRC imageusingthepositionsofseveralstarsinfield. this correction.TheCCDwasalignedandrescaledtothe for convertingfromthephotometrictoBbandpass.A between theBandVphotometricbandpasses.BlairGil- C, andDwereallowedtovary asfreeparameters.Tests for more (1982)havedeterminedacolorcorrectionof GG395 filter.Thebandpassofthiscombinationliesin sources compiledbyLaubertsandSadler(1984). lished photoelectricaperturephotometryfromnumerous the CCDimageswereobtainedbycomparingfluxesin tracted fromtheimageatallpoints.Thefluxzeropointsfor level ofthepeakinhistogrampixelintensitiesfor The skybackgroundlevelwastakentobethebrightness brightest galaxiesthatwerecatalogedfromtheSRCplate, but itisnotpossibletodetermineonmorphologicalgrounds circles ofvarioussizescenteredonthenucleuswithpub- several regionsawayfromthegalaxy.Thisvaluewassub- entire image.Thisagreedwithin\showedthatthefinalfitwasquite b, andc.Aniterativeapproachwasusedtoremovethecon- 1381. fog ± 0.3mag.TestsoftherepeatabilitySRCplatepho- Stars thatweresuperimposed on thegalaxieswerenot 4ky (*¿0=ax+byc, The backgroundlevelwasdeterminedfromarectangular An empiricalvignettingcorrectionfortheU.K.Schmidt Comparison ofthephotometrytopublished Each imagewasconvertedtoalinear-intensityscalebe- b) AccuracyofthePhotometry d) BackgroundSubtraction c) VignettingCorrection e) StarSubtraction 371 1989AJ 98. .367F 1/4 1/4 curate tobetterthan+3",onaverage. final rightascensionanddeclinationareestimatedtobeac- the platedeterminedforHSTguide-starcatalog.The celestial coordinatesbyapplyingtheastrometricsolutionfor this relationwasusedtoextrapolateinwardthecenterof rated. Inthiscase,anrlawwasfittothesurface-bright- light) wascalculatedfromthegrowthcurves.Thisisavery the galaxy.Theeffectiveradius(thatwhichcontainshalf ness profilewithin10"oftheoutermostsaturatedpixel,and The profilesofmostthedwarfgalaxiesarereasonablywell play profilesforninearbitrarilychosengalaxiesinFig.2. weighted firstmomentofthepixelswithinthisaperture,and while ensuringthatallthegalaxylightwasconsidered.The define amaximumaperturesizeforfurtherphotometry,in procedure describedbelow.Thisgrowthcurvewasusedto Any saturatedpixelswerefilledinatthispoint,usingthe wards fromthevisuallydeterminedcenterofgalaxy. diameters Z>largerthan17" areshowninTableIII.The members areshowninTableII. Backgroundgalaxieswith ten independentresolutionelements.Column9inTablesII the galaxyiscircularandfollowsanrlaw,fitto crude correction,becauseitisbasedontheassumptionthat approximated byanexponential. ative ofthegrowthcurves.Forillustrativepurposes,wedis- at itsouter,asymptoticlimit. total magnitudewastakentobethelevelofgrowthcurve a newgrowthcurvewasproducedbasedonthiscenter.The center ofthegalaxywasthenrecomputedfromintensity- order tominimizethecontributionfrombackgroundnoise grating theintensityincircularannuli1arcsecwidthout- first agrowthcurveforeachgalaxywascomputedbyinte- data listedinTableIIareasfollows: the surface-brightnessprofileistypicallybasedonlessthan applied. and IIIindicateswhetherthesaturationcorrectionhasbeen used forthesegalaxies. mated magnitudesfromtheLasCampanasplateshavebeen been removed.Forhighlyelongatedgalaxieswithastarnear that itwasoftennotpossibletodetectwherethestarhad star thatitwasnotpossibletomakeacorrection.Eye-esti- contaminated bythediffractionpatternfromanearbybright ceeded. threshold, oruntilamaximumnumberofiterationswasex- deviation inthesixsurroundingpixelvaluesfellbelowaset center movedawayfromthemaskedpixeluntilstandard the center,radiusofcirclewasincreasedand not highlyelongated,thisproducedverygoodresults,such masked pixelandthegalaxycenter.Forgalaxiesthatwere center andwitharadiusequaltothedistancebetween pixels oneithersideinacirculararccenteredatthegalaxy was replacedwiththemeanofnearestthreeunmasked 372 HENRYC.FERGUSON:THEFORNAXCLUSTER 26 5 The pixelpositionsofthegalaxycenterswereconvertedto For thebrightergalaxies,centerofimagewassatu- Column 1.Fornax ClusterCatalog(FCC)number. To determinepositionsandmagnitudesofthegalaxies, Surface-brightness profilescanbederivedfromthederiv- Galaxies classifiedasclustermembers andlikelycluster There wereafewcaseswherethegalaxywassobadly © American Astronomical Society • Provided by the NASA Astrophysics Data System f) GalaxyTotalMagnitudesandPositions IV. THECATALOG -1 -2 beginning withtheprefix“B”. listed inorderofrightascension,andhavecatalognumbers in thecatalog.BackgroundgalaxiesTableIIIarealso km s. mined towithin —2mm.Theaveragedifference betweenthe cataloged onlyfromtheLasCampanas platesweredeter- tions areaccurateto3".Platepositions forgalaxiesthatwere moment ofthesurface-brightness distribution.Theseposi- tometry, positionsweredetermined fromtheweightedfirst sured fromeithertheSRCplateorLasCampanasplate, taken fromtheliterature. source forthemagnitudeandeffectiveradius,iftheywere the galaxyinthissurvey,whiletensdigitindicates Table V.Theonesdigitindicatestheplatematerialusedfor fective radii.Themeaningsofthesourcecodesarelistedin 0.1 'atanisophoteof26.5Bjarcsec. appeared ontheSRCplateand werenottoobrightforpho- or havebeentakenfromthe literature. Forgalaxiesthat Catalog numberinorderofrightascensionastheyarelisted galaxy, dependingonthespaceavailable. ies arelistedattheendofTableII. from theSRCplatesorliterature. system (BST85). when determinedfromtheSRCplate,and—15"de- below. termined fromtheLasCampanasplates. seconds. Theaccuracyofthecoordinatesis~3"orbetter minutes, andseconds. in thenotescolumn13. Table IIwehaveindicatedsuchbackgroundcontamination the catalognumberinTableIIIindicatethatavelocityor press it,andhaveinsteadlistedalternatenamesveloc- star ),andthereforethemagnitudeestimateisuncertain.For uniform (usuallyduetothepresenceofanearbybright sky backgroundontheSRCplateneargalaxywasnon- from TableIIistheclassification(nb),whichindicatesthat alternate nameislistedinthenotes.Onefurtherdifference columns arethesameasinTableII.Asterisksatendof ities inseparatenotesattheendofTableIII.Thefirstnine (1985), 2=Jonesand(1980),3Lauberts (1982). -1 The celestialcoordinatesforeachgalaxyhavebeenmea- All likelyclustermembersareassignedaFornaxCluster Column 12.Sourceofthevelocity:1=RichterandSadler Column 11.Uncertaintyoftheobservedvelocityin Column 10.Heliocentricvelocityofthegalaxyinkms. Column 13.Notes.Additionalnotesonindividualgalax- Column 15.IAUcoordinatedesignation. Column 14.Names.Uptofournamesarelistedforeach Column 9.Sourceofthecoordinates,magnitudes,andef- Column 8.Decimallogarithmofthediameterinunits Column 7.Effectiveradiusinarcsecondsasdetermined Column 6.Totalblueapparentmagnitude. Column 5.MorphologicaltypeintheextendedHubble Column 4.Membershipstatusofthegalaxy.SeeTableIV. Column 3.Declination(1950)indegrees,minutes,and Column 2.Rightascensionfortheepoch1950inhours, The individualparametersarediscussedinmoredetail We haveleftoffcolumns10-14inTableIIIsoastocom- b) Coordinates(Columns2and3) a) FCCNumbers(Column1) 372 1989AJ 98. .367F 373 HENRYC.FERGUSON:THEFORNAXCLUSTER © American Astronomical Society • Provided bythe NASA Astrophysics Data System 73 w .° .-S •O £- Æ .Sià 2 5-g Dû rS o *- Ç £ . 4J-y te 43 £ N 1 dE2,N 1 dEO 1 E3 1 dEO 2 dEO^N? 1 E0 2 dEl,NorE(cD)16.7 2 dE4 1 dE6 1 dS0(5),N 1 dEO 1 dEO 2 dE318.8 1 dE3/ImV ImV dSO dE4 dE3 +ImV SBbc(s)I dS0(5),N E0 dE4,N dE4,N dE SO(cross) dE3 dE6,N dE0,N? dEl 80.(9) dEl,N dE3JSÎ dE3,N dE3,N S0(9)(boxy) dE2 dEO SO/a dSO S0(9)(cross) SBa(s) Sa 2 Type (5) 20.4 20.3 16.7 17.3 10.2 18.7 18.0 19.7 19.8 18.2 16.8 18.6 16.9 14.8 15.5 11.21.06412541202 18.5 19.0 14.4 18.5 19.7 19.2 14.3 11.9 19.5 19.6 15.7 19.9 13.6 Bq* 20.0 14.1 18.0 16.8 16.60.93 18.3 11.50.70 17.2 12.10.86 18.3 19.2 13.0 (6) 18.1 11.80.67 20.4 11.7 20.91.35351405181 17.7 10.60.80 19.8 17.5 16.4 18.0 13.0 17.2 18.7 11.3 18.1 17.2 13.2 17.9 18.0 13.7 12.4 24.7 0.97 r DSIVel.Err.S2N (7) (8)(9)(10)(11)(12)(13) 17.3 0.75 13.4 0.94 14.2 1.27 16.3 1.23 26.9 1.3715730 24.0 1.21351386 21.4 1.34 11.8 1.20 12.3 0.73 11.3 1.40 e 26.0 1.3531465 39.8 1.4215 11.1 0.813 10.1 0.873 12.6 1.3941495 18.0 0.783 12.9 1.3525 9.6 0.83 4.5 0.49 4.2 0.37 9.0 0.61 9.3 0.68 5.3 0.44 5.0 0.59 6.8 0.54 9.0 0.87 3.7 0.39 6.2 0.55 9.5 0.62 2.1 0.29 4.7 0.413 4.4 0.44 6.6 0.47 6.5 0.904 5.6 0.413 6.7 0.62 7.9 0.53 7.3 0.533 7.7 0.603 7.2 0.854 6.9 0.653 3.9 0.373 8.3 0.883 9.0 0.753 8.3 0.633 8.3 0.703 Table IL(continued) 1.93 15163851NGC1365,ES0358-G17,G117,D73 0.29 5 0.79 5 1.48 15839 3 3 3 11941502 3 3 1854302 3 3 3 1376 3 3 3 1639 3 1465 3 3 3 3 3 3 3 3 1827 111NGC1380,ES0358-G28,G57,D103 1793 141NGC1381,ES0358-G29,G76,DI04 25 1 23 45 15 20 13 1 NGC1375,ES0358-G24,G82,D89 1 NGC1374,ES0358-G23,G83,D90 2 NG82, D77 NG84, D74 NG66, D75 NG121 HPW17 NG18, D83 NG52, D79 ESO358-G20, G10,MCG-5-9-15,D84 ES0358-G19, G46,D80 NG122, D85 G99, NG24,D82 NG54, D86 NG123, D88 NGC1373, ES0358-G21,G84 ES0358-G25, G8,MCG-5-9-17,D92 NG88, D91 NG58, D94 IC1963, ES0358-G26,G45,10335 NG57, D96 NG17, D95 NGC1379, ES0358-G37,G81,D97 NG16, D98 NG19 D99 NG20, D100 NG35, D101 NG65, D105 D102 NGC1386, ES0358-G35,G98,D1070334-3609 NG62, D1080334-3426 NGC1380A, ES0358-G33,G54,DI060334-3454 ES0358-G34, Gl14JD110,NGC1392?0334-3625 NG116 NG115 Names (14) 0331-3601 0331-3235 0331-3618 0331-3600 0331-3420 0332-3445 0332-3531 0332-3557 0332-3523 0332-3540 0332-3614 0332-3637 0332- 3 526 0331- 3 430 0332-3629 0332-3427 0332-3601 0332-3542 0333- 3521 0332- 3248 0333-3522 0333-3512 0333-3529 0333-3520 0333-3522 0333-3529 0333-3525 0333-3523 0333-3237 0333-3631 0333-3615 0333-3540 0333-3530 0333-3458 0333-3524 0333-3436 0333-3620 0333- 3459 0333-3609 0334- 3533 0334-3536 0334-3535 0334-3600 0334-3604 0334-3619 0334-3532 0334-3527 0334-3457 0334-3522 0334-3508 0334-3719 0334-3310 0334-3419 0334-3731 0334-3535 0334-3623 IAU (15) 376 1989AJ 98. .367F 377 HENRYC.FERGUSON:THEFORNAXCLUSTER © American Astronomical Society • Provided by the NASA Astrophysics Data System (1) (2) 181 185 183 182 200 33558.8-3502361dE2 186 184 205 33616.0-3815241dElJi? 204 33615.4-3317161dS0(8),N 203 33612.8-3440461dE6,N 202 33611.4-35031d:E6,N 201 33601.2-3726281dE4 187 208 33623.8-3541291dE2^ 207 33623.7-3517231dE2^I 206 33621.1-3727031dEOpec 195 209 33624.9-3349152dE5,N 196 33539.3-3559271dE6 194 190 189 188 212 33627.3-3634271dEl? 211 33626.1-3525142d:E2,N 210 33625.0-36131dEO 198 33550.1-3722131dE5 197 33545.6-3527281dE3 193 192 191 213 33634.2-35461EO 199 33550.4-3653172ImV 215 33643.0-3555032dE,N? 214 33642.1-3559401dEO 231 230 228 222 217 33648.4-3653152dE/ImV19.7 216 33645.8-3643072dEO19.2 233 232 229 227 226 225 224 223 221 220 33659.8-3523491dE219.5 219 33657.4-3545201E210.9 218 33650.1-3525351dE418.5 236 235 234 240 238 237 239 # RA(1950) 3 3457.2 3 3459.1 3 3459.0 3 3527.4 3 3506.7 3 3501.8 3 3507.0 3 3523.1 3 3517.0 3 3509.6 3 3508.4 3 3515.5 3 3514.7 3 3513.4 3 3512.0 3 3732.8-315705 3 3812.5-362334 3 3807.9-341936 3 3805.4 3 3800.7 3 3756.3 3 3755.4 3 3744.4-364247 3 3725.0-355305 3 3718.3-353152 3 3711.7-361532 3 3814.7-354701 3 3808.2-322842 3 3754.7 3 3827.5 3 3815.6 3 3813.7-343620 3 3826.8 3 3823.9 3 3821.3 Dec(1950) M -36 3855 -35 0602 -35 0343 -35 5428 -35 3212 -35 5138 -36 0301 -35 4013 -35 3256 -35 2126 -38 1748 -35 0215 -34 5336 -35 4508 -34 4555 -34 5502 -35 2853 -35 4055 -35 4918 -35 1055 -35 5943 -31 5039 -37 3931 -36 4138 -33 3450 (3) (4) dE5,N dE3 SBO (5) dEO dE3 dE2N SBO dE4,N dEOJSÎ dE3 dS0(7),N SBOpec dE5 dE4 SBO ImBI ImV dE7,N dEOJN? dE5JM dEO dEO dE0,N? dE? dE4 19.6 ImVordE 16.9 ImlV dE2 dE5JN dE0,N 16.2 dEO^Î 15.6 dE4,N 17.7 dE5 dE5,N dE3 > Type (5) 16.7 18.2 12.8 17.9 19.1 17.7 19.6 19.3 13.5 16.1 17.5 19.5 17.2 14.9 17.2 15.3 16.7 17.4 19.0 18.8 17.8 12.3 14.9 15.5 16.9 18.7 15.9 15.8 18.7 17.3 17.6 15.20.833 16.3 5.60.873 19.0 6.20.583 10.6 37.21.57351430 18.4 17.2 19.1 18.8 19.3 19.2 7.40.463 b 19.2 13.4 17.2 19.6 17.4 17.8 16.5 18.9 18.7 17.8 (6) t 20.1 1.49 50.1 1.5215 10.2 0.753 11.4 0.89 16.3 1.35 12.1 0.98 12.3 0.84 11.4 0.853 11.4 1.133 12.9 0.95 (7) 12.9 1.11 13.0 1.12 20.0 1.45351944 18.6 1.083 11.7 0.843 36.3 1.46 14.5 1.09 18.5 0.84 14.2 0.91 16.6 1.06 13.3 0.88 11.9 0.97 6.4 0.62 6.3 0.46 9.0 0.783 7.9 0.703 5.0 0.49 7.1 0.573 6.3 0.533 8.3 0.39 5.6 0.523 9.8 1.06 8.5 0.823 7.9 0.523 6.7 0.543 8.5 0.963 9.2 0.61 7.3 0.50 7.6 0.673 6.7 0.55 6.8 0.62 5.7 0.42 6.0 0.68 6.2 0.513 6.9 0.513 9.0 0.83 8.2 0.75 5.6 0.503 5.7 0.53 8.3 0.66 5.4 0.56 8.9 0.59 8.9 0.73 Table IL(continued) 0.66 0.93 (8) (9)(10)(11)(12)(13) D SIVd.Err.S2N 3 3 3 3 2023 3 3 3 3 3 1 1784 391NGC1380B,ES0358-G37,G77 1337 161NGC1387,ES0358-G36,G78,DI12 1823 902G79,Dili 1372 602ES0358-G43,G18,D125 1042 1502ES0358-G42,G43,D126 999 291NGC1389,ES0358-G38,G97,DI16 894 1202NGC1396,G75.D124 953 1502 15 1NGC1404,ES0358-G46,G73,DI37 10 1 9 1NGC1399,ES0358-G45,G74 5 ES0358-G44r,D129,NG2,HPW24 3 D127 NG56, HPW19,D109 NG112, D113 NG113 HPW20, NG8,DI14 NG23, DI19 HPW21, NG55,DI18 DI 22 NG34, D121 NG114, DI20 D117 NG120 HPW23, NG33,DI23 NG7, DI30 D131 HPW25, NG21,D132 NG119 NG71.D349 NG117 NG118, DI34 HPW29, NG76 NG87 NG91.D142 NG72, D136 D135 NG78 NG111 HPW28, NG6,D141 G72, DI39 NG43 D138 NGC1427A, ES0358-G49,G68,D149 NG109 D144 D148 D145 Names (14) 0334-3506 0335-3502 0335- 3 540 0334- 3 638 0334-3532 0335-3817 0335-3545 0335-3445 0335-3554 0335-3532 0335-3521 0335-3453 0335-3503 0335-3603 0335-3722 0335-3527 0335-3559 0335-3551 0335- 3502 0335-3653 0336-3317 0336-3440 0336-3536 0336- 3726 0336-3815 0336-3349 0336-3517 0336-3727 0336-3613 0336-3541 0336-3634 0336-3525 0336-3559 0336-3536 0336-3555 0336-3653 0336-3643 0338-3455 0338- 3549 0337- 3528 0337-3540 0337-3642 0337-3157 0337-3553 0337-3531 0337-3615 0336-3523 0336-3545 0336-3525 0338-3419 0337-3510 0338-3547 0338-3436 0338-3623 0338-3228 0338-3559 0338-3150 0338-3739 0338-3641 0338-3334 IAU (15) 377 1989AJ 98. .367F 378 HENRYC.FERGUSON:THEFORNAXCLUSTER © American Astronomical Society • Provided by the NASA Astrophysics Data System 241 244 243 242 (1) (2) 248 33849.2 247 33847.8 246 33843.8 245 264 263 262 261 260 33917.6 259 33912.8 258 33912.7 257 33909.6 256 33908.3 255 33906.4 254 33906.4 253 33904.1 252 33856.0 251 33854.2 250 33852.4 249 33850.3 265 267 33948.5 266 33946.2 273 34019.7 272 34016.4 271 34010.7 270 34008.6 269 34002.5 268 33956.9 292 34156.6 291 34144.9 277 34027.7 276 34024.6 275 34024.5 274 34022.8 297 296 295 34235.2-3519592dEO 294 34233.2-3549141dEl,N? 293 34231.4-3600411dEl,N 290 289 288 287 286 285 284 283 282 281 280 34043.1 279 34033.6 278 34030.4 299 298 300 # RA(1950) 3 3828.3 3 3836.5 3 3833.7 3 3829.1 3 3945.1 3 3936.8 3 3927.4 3 3838.4 3 3937.3 3 3924.4 3 4245.7 3 4238.2 3 4048.8 3 4044.7 3 4306.9 3 4250.4 3 4143.2 3 4127.6 3 4126.1 3 4119.1 3 4117.0 3 4108.6 3 4100.2 3 4049.0 3 4306.5 Dec(1950) M -36 2825 -37 0256 -35 5017 -36 0814 -35 2102 37 4811 35 2605 33 5538 35 5054 35 4820 35 0646 37 5947 35 5424 35 1053 36 0211 36 3928 33 3831 35 4449 35 0250 36 0623 35 1859 35 4023 33 5613 35 5401 35 1055 37 34001dEl 37 40091E0 36 01102dE3 35 49111dE3/Im? 36 16471dE2 33 56 35 1940 36 50381dE0,N 34 3643 35 3603 35 0024 37 4729 35 2658 36 4715 34 0436 36 0128 36 06451dEl 34 01392dE6,N 35 18401E5(boxy) 35 33061E4 35 4304 35 4151 33 11481dE6,N? 35 22172dE5 36 00381Sell 34 51041dEO 35 40292dEO 34 47571dE0,N? 36 2539 35 2959 38 2312 34 05411dS0(9),N (3) (4) 2 dE2 2 dE0,N? 2 dE2 2 dE 2 dEl 2 dEl 2 dE2 1 dEl 1 dE3pecj'í/ImlV15.8 1 dE0,N 1 dE2 1 dE3 1 dEO^N 1 dE5JN? 1 dEOJM 1 dEO 1 dE0,N 1 dEO^J 1 dE 1 dEl 1 dEO 1 SmIV 1 ImIV/dEpec 1 dEl 1 dE 1 Sdin? dE6/ImIV? dEIJÍ dE5 dE0,N dEO^J dSO (8),N dE5 SBcdlII dE4,N dE2J'J dEl dEl,N Sd(on edge) Type (5) 20.1 18.2 16.5 17.8 16.6 17.0 17.8 19.6 18.1 13.7 17.6 16.3 16.0 19.0 16.0 14.6 17.8 17.1 13.6 18.7 17.8 19.1 18.1 16.8 17.8 18.9 17.2 17.6 17.1 18.8 19.2 18.7 19.7 18.3 18.3 16.0 15.9 16.1 17.1 16.6 16.3 19.4 12.8 18.7 15.4 18.0 19.0 17.8 14.5 17.9 18.6 16.7 16.8 13.8 11.8 19.3 16.5 18.1 14.2 b (6) t r 20.5 1.2331708 11.7 0.94 11.0 0.81 15.9 0.96 14.9 0.953 13.6 0.713 13.8 1.3241217 11.8 0.873 10.8 0.953 11.1 0.993 13.8 1.3931521 12.9 1.01 t 28.7 1.34 32.4 1.24351454 15.6 1.123 (7) 13.1 0.853 10.4 0.793 12.2 0.75 13.2 0.783 16.4 1.07 13.3 0.79 10.8 0.94 10.0 0.833 14.0 1.003 12.0 0.963 12.3 1.06 10.4 0.55 10.5 1.17 10.4 0.75 10.1 1.2541620 4.5 0.413 4.9 0.513 6.8 0.493 6.7 0.613 6.0 0.63 8.6 0.583 9.4 0.833 7.6 0.88 7.1 0.613 7.5 0.523 7.7 0.503 7.1 0.533 7.5 0.543 7.1 0.64 7.7 0.803 9.2 0.783 8.0 0.703 8.5 0.563 7.6 0.84 7.3 0.543 9.9 0.553 5.4 0.44 5.6 0.87 9.8 1.043119060 6.0 0.784 9.2 0.723 6.3 0.673 8.3 0.603 Table II.(continued) 0.60 1.55 151217 (8) (9)(10)(11)(12)(13) D SIVel.Err.S2N 895 83 30 1 25 1 21 3 1 NGC1437,ES0358-G58,G95 1 NGC1427,ES0358-G52,G67,DI72 NG137 NG39, D161 D158 NG4, DI57 NG73, D163 NG37, D162 HPW32 ESO358-G50, G24,HPW34?,DI60 NG22, D159 HPW33, ESO301-G24,NG48,D155 NGC1419, ESO301-G23,G131,D156 D154 NG40, D153 NG3, D152 DI 50 HPW31, NG44,D151 NG51, D147 NG5, D146 NG81.D165 NG79, DI64 NG101, DI69 ES0358-G51, G53,DI68 NG98, DI85 NG42 NG99 HPW42, NG75 DI 84 NG105 NG108 NG104 HPW37, NG80 HPW36?, NG74 NG11, D188 D187 NG83, D186 NG103 NG45, D175 NGC1428, ES0358-G53,G80,D174 HPW39, NG15,D173 NG102 ES0358-G56, G22,DI81 NG107, D176 NG38, DI80 NG77 NGC1437A, ES0358-G54,GUI G23, D177 NG41, D178 Names (14) 0338-3510 0339-3540 0339-3550 0339-3548 0339-3506 0339-3356 0339-3554 0339- 3 759 0338- 3 554 0338-3734 0338-3740 0338-3601 0338-3602 0338-3639 0338-3748 0338-3526 0339-3518 0338-3549 0338-3616 0338-3510 0339-3606 0339-3355 0339-3338 0339-3544 0339-3502 0339-3356 0339-3519 0342-3549 0341- 331 0341-3540 0341-3447 0341-3625 0341- 3529 0340- 3823 0340-3401 0340-3518 0340-3533 0340-3543 0340-3541 0340-3436 0340-3536 0340-3500 0340-3747 0340- 3526 0339- 3647 0342-3521 0342-3519 0342- 3600 0341-3522 0341-3600 0341-3451 0341-3405 0340-3404 0340-3650 0343-3628 0343- 3702 0342- 3550 0342-3608 0340-3601 0340-3606 IAU (15) 378 1989AJ 98. .367F 379 HENRYC.FERGUSON:THEFORNAXCLUSTER © American Astronomical Society 302 34318.2-35291Sdm(onedge)15.7 301 34310.1-3607371E4 305 34342.0-3714111dSO^Ô) 304 34335.2-3439321dEl 303 34322.0-370527 (1) (2)(3)(4) 315 34508.1-3351421Sab(re)II 312 34424.1-3505471Scd(onedge)13.51.7225193212 311 34421.6-3354591dS0(8),N16.910.60.90 309 34416.1-3658331dE2 308 34402.0-3630421Sd(onedge) 307 34353.0-3512501dE3 306 34352.5-3629581SBrnHI 316 314 34446.0-3718431dE2¿í 313 34438.2-3450191dS0(9) 310 34421.5-3650591SB0 340 339 338 336 323 34544.9-3630551dE2/ImV 322 34544.0-3843601Sd 321 34540.8-3606211dE 320 319 318 317 337 335 34843.8-3603291E14.212.91.26146025 334 34829.2-3523492dE(boxy)18.66.80.571 332 34756.0-3605421EorSO15.78.30.9821326120 331 34721.1-3707271dE17.119.20.94 330 34720.7-3604372dE19.44.60.44 329 34702.5-3606112dE18.25.50.62 327 34618.9-3740351dE3?17.411.70.86 325 34607.7-3510401dE3 324 34600.3-3637231dSO(8) 333 34805.8-36141EorSO16.86.00.862 328 34629.1-3615301dE18.410.90.74 326 34612.2-3653511dEl18.67.40.60 # RA(1950)Dec(1950)M 3 4517.8-322715 3 4515.4-362844 3 4508.9-363523 3 4536.0-322423 3 4511.2-325534 3 5127.9-375847 3 5013.3 3 4858.5-351913 3 5004.7 3 4909.5-3655 -38 0119 -33 3657 2 dE5,N? 2 dE 2 dE,N 1 dE6,N 1 dE3,N 1 dE2»N 1 dEl 1 SO 1 dEpec 1 dE/ImV dEl,N Type (5) 14.2 15.5 13.8 15.7 18.8 16.3 15.41.02 12.6 38.31.52 16.5 14.70.98 13.5 17.7 15.6 16.4 14.80.96 16.1 15.81.07 17.7 8.90.74 17.4 17.5 18.8 12.20.621 17.3 6.60.77 17.5 18.2 14.3 17.6 17.5 12.5 17.8 18.2 7.80.66 15.3 18.91.16 (6) 20.4 1.163 25.8 1.4431352 27.2 1.423 12.4 1.223 20.0 1.31 13.5 1.083 r DSIVel. 15.3 0.853 16.6 1.133 19.1 0.853 10.4 0.74 11.4 0.72 (7) (8)(9)(10) e 9.7 0.613 3.8 0.793 7.8 0.74 9.3 0.79 5.7 0.68 9.0 0.77 Table IL(continued) 1.43 Provided bythe NASA Astrophysics Data System 3 3 3 3 1004 3 3 5 3 3 3 3 3 1856150 1020 201 1597 151 (11) (12)(13) Err. S2N 29 1 39 1 3 NG50,D211 1 ES0358-G63,G52,DI97 ES0358-G59, G94,DI89 NGC1437B, ES0358-G61,G109,DI940344-3630 NG47, DI91 ESO358-G60, DI90 NGC1460, ES0358-G62,G108,D1960344-3650 NG89, DI930343-3512 HPW43?, NG46,D192 NG97, D222 NG92, D202 HPW45, NG12,D201 D195 ESO359-G03, G150,D220 D216 NG96, D213 NG14, D206 ESO419-G07, NG90,D204 HPW46, NG13,D203 ICI993, ES0358-G65,G21,D200 NG49, DI98 D218 ESO359-G02, G91,D217 G92, D215 NG95, D212? NG93, D209 ES0358-G66, G142,D208 ES0302-G09, D207 Names (14) 0343-3543 0343-3607 0344- 3658 0343- 3629 0343-3714 0343-3439 0343-3705 0344-3505 0344-3354 0345-3606 0345-3227 0345-3628 0345-3255 0345-3635 0345- 3351 0344- 3718 0344-3450 0350- 3801 0348- 3519 0345- 3630 0345-3843 0345-3224 0351- 3758 0350- 3336 0349- 3649 0348-3523 0348- 3614 0347- 3605 0347-3604 0346-3740 0346-3510 0346- 3637 0348-3603 0347-3707 0347- 3606 0346- 3615 0346-3653 IAU (15) 379 1989AJ 98. .367F 380 HENRYC.FERGUSON:THEFORNAXCLUSTER B0001 30931.0 B0024 B0023 B0022 B0021 B0020* B0019 B0018 B0017 B0016 B0015 B0014 B0013 B0012 B0011 B0010 B0009 B0008 B0007* B0006 B0005 31020.0 B0003 30940.0 B0002 30934.0 B0026 B0025 B0004 30950.0 B0027 B0031* B0030* 31512.0-324559 B0029 B0028 © American Astronomical Society • Provided by the NASA Astrophysics Data System B0039 B0038 B0037 B0036 B0035 B0034 B0033 B0032 B0040 B0041 31622.0-341230 B0045 31638.0-341406 B0044 31636.0-332454 B0043* 31634.0-331760 B0042 31625.0-361912 B0061 B0060 B0059 B0058 B0057 B0056 B0055 B0054 B0053 B0052 B0051 B0050 B0049 B0048 B0047 B0046 B0065 B0064 B0063 B0062 O) (2)(3)(4) # RA(1950)Dec(1950)M 3 1229.0 3 1159.0 3 1036.0 3 1442.0-374706 3 1440.0-351736 3 1437.0-373148 3 1436.7 3 1436.0 3 1421.0 3 1415.0 3 1414.0 3 1313.0 3 1307.0 3 1303.0 3 1232.0 3 1217.0 3 1207.0 3 1448.0-381842 3 1444.0-352448 3 1232.0 3 1501.0-325348 3 1501.0-382454 3 1451.0-3654 3 1504.0-374354 3 1532.0-344548 3 1520.0-365242 3 1520.0-335224 3 1603.0-383536 3 1553.0-331430 3 1553.0-380448 3 1621.0-365848 3 1621.0-383412 3 1536.0-380148 3 1528.0-334748 3 1645.0-383524 3 1639.0-375700 3 1758.0-342342 3 1729.0-335930 3 1723.0-325548 3 1720.0-325636 3 1718.0-343630 3 1716.0-323860 3 1709.0-375512 3 1705.0-380812 3 1705.0-350448 3 1704.0-362136 3 1704.0-383612 3 1810.0-332106 3 1805.0-352348 3 1802.0-375800 3 1802.0-341048 3 1802.0-345812 3 1735.0-354300 3 1733.0-381200 33 3054 33 2318 32 3730 32 5312 37 3138 37 1960 33 3730 33 4236 32 2848 33 0218 33 4318 32 2618 33 4318 33 1442 33 2848 32 4954 32 3812 33 0148 32 5418 33 2206 4 S 5 Sb 5 S 5 S 5 S(onedge) 5 S 4 SordEN 4 pec 5 S 5 S 3 dEJiorS 5 S 3 SorImV,N 5 S 5 S 3 Sbc(onedge) 5 (interacting) 5 Sab(r)I-n/SBab(r)I-II 5 S 5 E 5 S 5 S0(9) 5 S 5 SBab(r)n 5 SB 3 BCD? 4 S 5 S 5 Sab(s) 5 5 S 5 E 5 S 5 S(Seyfert?) 5 S ImV pec? Im orS S S S ImlV? BCD(High SB)orS Imin? S S S S S S S S S orImlII Sc(s)llpec Type (5) Table III.Possiblemembersandlikelybackgroundgalaxies. 17.4 16.6 16.5 17.0 17.9 18.0 18.3 16.7 17.9 17.1 17.0 17.0 17.0 16.7 17.8 15.7 18.3 17.0 16.7 17.3 17.0 16.8 18.3 16.3 18.1 16.8 17.0 17.0 17.9 16.2 17.0 18.5 17.2 14.9 18.0 16.0 16.9 18.5 16.6 14.7 13.0 16.4 16.8 17.1 16.5 17.0 16.9 16.5 16.1 17.2 15.8 16.6 17.3 17.2 18.3 16.0 17.4 17.2 16.5 16.8 16.7 16.9 16.0 16.6 17.5 Bj rDS (6) (7)(8)(9) e 0.86 0.71 0.64 0.72 0.73 0.70 0.76 0.64 0.61 0.84 0.77 0.60 0.73 0.71 0.63 0.68 0.70 0.64 0.71 0.59 0.75 0.93 0.54 0.67 0.80 0.58 0.61 0.80 0.90 0.80 0.78 0.68 0.52 0.55 0.84 0.80 0.75 0.85 0.81 0.68 0.57 0.65 0.85 0.59 0.65 0.69 0.79 0.71 1.23 0.81 0.70 0.63 0.95 0.65 0.78 0.70 0.81 0.73 0.71 0.75 0.64 0.88 0.75 0.72 1.49 20 B0071 31840.0-322442 B0070 31840.0-330312 B0069 31839.0-374948 B0067 31827.0-344330 B0066 31825.0-352048 B0087 B0086 B0084* 31918.0-350230 B0083* 31915.0-362100 B0081 31908.0-340506 B0080* 31908.0-365412 B0079 B0078 B0077 B0075 31859.0-354624 B0074* 31855.0-335342 B0072 31842.0-374130 B0068* 31838.0-384254 B0088 B0085 31925.0-335524 B0082 31909.0-380442 B0076 B0073 31854.0-345742 B0090 B0089 B0093 B0092 B0091 B0105 B0104 B0103 B0102 B0101 B0100 B0099 B0098 B0097 B0096 B0095 B0094 B0112 32043.7-3729244(interacting)ordEpec18.64.90.58 B0111 32041.7-3623214S0 B0110 B0109 B0108 B0107 B0106 B0115 B0114 B0113 B0124 B0123 B0122 B0121 B0120 B0119 B0118 B0117 B0116 B0130 32100.9-373919 B0128 32059.2-335109 B0127 32059.2-342749 B0126* 32057.7-365636 B0125 B0129 32059.9-350222 (1) # RA(1950) Dec(1950)M 3 1931.0-375200 3 1928.0-354048 3 1946.0-372312 3 1945.0-3448 3 1939.0-365442 3 1932.0-352418 3 1904.0-355224 3 1951.0-365800 3 1948.0-342906 3 1947.0-324924 3 1907.0-363042 3 1904.0-340454 3 1903.0-363542 3 2030.6-362604 3 2029.6-364745 3 2025.7-375017 3 2025.0-375310 3 2019.0-3554 3 2016.2-374312 3 1957.0-350448 3 1954.0-322818 3 2036.0-362459 3 2033.0-331542 3 2032.2-362243 3 2039.4-380146 3 2039.0-364038 3 2037.9-362643 3 2037.0-351142 3 2036.6-363501 3 2047.7-353142 3 2046.5-3635185S 3 2045.6-35585E 3 2045.0-3837485S 3 2051.1-350753 3 2050.8-370958 3 2047.0-363659 3 2054.0-350260 3 2054.0-361642 3 2052.8-350231 3 2050.8-363145 3 2057.3-374211 3 2056.7-355425 (2) (3)(4) 5 S 5 Sc(s)III 5 (interacting) 4 SorSmIV 4 SBc 5 S 5 S 4 SordSO 4 SordE5 5 S 4 S 5 S 5 S 3 dS0(6),NorS 3 SBcd(onedge) 4 E 5 S 5 S 5 SBb(s)I-n 5 S 4 Smin? 5 3 E? 5 S 5 S 5 5 S 5 Spec 5 S 5 S 4 E(cD)?ordEN 5 E 5 S 5 E(cD) 4 ImlV? 4 dSd? 5 5 E 5 5 S 5 S 5 E 5 SBbc(s)I-B 5 Sc(s)I 3 dE4 El E(M32?) S S SBab(r)I S Merger(interacting) Sm S S S S S Type (5) 16.0 14.9 15.3 17.3 17.3 15.3 15.8 16.8 15.7 14.0 15.3 16.9 15.4 16.2 15.1 15.1 18.2 17.1 15.3 16.2 15.5 17.5 16.6 18.3 18.2 17.8 17.0 18.3 17.1 18.9 16.2 17.8 16.5 17.3 16.8 18.2 18.0 18.0 18.4 17.6 17.0 17.6 17.6 17.6 18.8 18.0 17.5 17.8 17.0 18.0 17.6 15.6 18.6 3.40.491 18.0 4.80.651 18.1 0.575 17.3 10.10.831 B 18.3 16.9 15.7 19.1 18.3 18.2 17.8 15.7 (6) (7)(8)(9) t 4.6 0.511 4.7 0.631 7.7 0.793 4.8 0.541 4.3 0.603 3.5 0.481 4.5 0.611 4.0 0.581 4.5 0.593 4.6 0.54 7.3 0.78 6.7 0.733 3.8 0.543 8.0 0.904 4.5 0.513 3.2 0.471 5.1 0.63 2.6 0.51 3.3 0.74 5.1 0.854 3.3 0.461 5.6 0.533 3.8 0.561 3.8 0.503 8.9 1.004 0.91 5 0.91 5 0.62 5 0.64 5 0.90 0.88 0.87 0.91 0.68 5 0.88 5 0.56 5 0.65 5 0.90 5 0.77 0.68 0.90 0.88 5 0.99 5 0.56 5 0.70 5 0.72 5 0.62 5 0.67 5 0.58 5 0.69 5 0.55 5 0.58 5 0.83 5 1.12 1.01 1.12 5 1.14 0.53 5 0.69 5 0.72 5 D 380 1989AJ 98. .367F 381 HENRYC.FERGUSON:THEFORNAXCLUSTER B0148 B0146 B0145 B0144 B0143 B0142 B0141 B0140 B0139 B0138 B0137 B0136 B0135 B0134 B0133 B0132 B0131 B0153 B0152 B0151 B0150 B0149 B0147 B0160 B0154 B0162 B0161 B0159 B0158 B0157 B0155 B0163 B0156 B0165 B0164 B0167 B0166 B0183 B0182 B0181 B0180 B0177 B0175 B0170 B0169 B0168 B0185 B0184 B0179 B0178 B0176 B0174 B0173 B0172 B0171 B0190 32144.1-370159 B0188 32143.8-352646 B0187 32143.3-370345 B0186* 32143.2-370444 B0195 32147.0-352539 B0192* 32144.7-370501 B0189 32143.9-370659 B0194 32146.3-351035 B0193 32146.1-325507 B0191 32144.6-364555 © American Astronomical Society • Provided by the NASA Astrophysics Data System (1) (2)(3)(4) # RA(1950)Dec(l950)M 3 2111.0-323213 3 2108.5-360326 3 2108.4-360317 3 2108.0-330018 3 2107.8-370444 3 2107.4-361620 3 2102,7-3310 3 2102.7-342654 3 2102.0-381254 3 2121.3-373016 3 2121.0-372618 3 2120.6-380604 3 2120.3-332432 3 2120.0-323237 3 2117.4-371419 3 2114.0-384300 3 2112.1-344832 3 2109.9-353235 3 2106.2-323911 3 2104.3-343706 3 2102.2-372257 3 2129.0-3753 3 2122.8-361054 3 2122.1-351547 3 2129.7-374240 3 2129.4-354927 3 2129.0-374548 3 2128.8-324019 3 2128.3-343403 3 2125.2-353809 3 2129.8-354425 3 2127.4-334115 3 2125.4-362455 3 2129.9-333953 3 2129.9-3645 3 2134.8-324147 3 2133.2-362429 3 2133.1-340123 3 2139.9-3557 3 2139.3-364750 3 2139.1-324855 3 2138.6-333812 3 2137.8-334025 3 2137.8-344802 3 2137.0-323254 3 2136.3-323726 3 2136.2-322706 3 2135.9-355428 3 2135.6-334738 3 2133.6-342940 3 2130.3-363607 3 2141.5-3616 3 2141.0-351724 3 2138.6-325006 3 2141.3-353922 5 Sc(s)II-m 4 (interacting)? 5 ? 5 S 5 E 5 S 5 E(incluster) 5 3 dElorfilament 5 5 E 5 E 5 S 5 E 5 E 3 Sm? 3 dE2? 5 S 5 E 5 S 5 S 4 E 5 Sc(onedge) 5 S 5 5 S 5 S0? 4 ? 4 S 5 S 4 S 4 (interacting)?orIm 4 S 5 S 4 E(M32?) 5 S 5 E 5 5 5 S 5 S 5 5 S 4 E(cD) 5 S 5 3 SmIV? 3 dEO/ImV 3 Spec^N 5 S 5 S 4 E 4 dSO? 5 S 5 E 5 5 E 5 Sbc(s)II ImIV-V? E Type (5) 18.4 6.00.571 17.3 6.30.723 18.3 3.40.473 18.4 4.60.533 18.0 18.1 3.70.533 18.5 16.9 18.0 4.70.571 19.1 3.80.463 18.4 4.00.501 17.7 4.70.591 18.7 3.90.481 18.4 18.3 0.545 17.1 3.70.752 18.2 17.4 18.6 4.60.561 18.0 18.7 18.5 3.70.471 16.8 5.40.75 17.2 4.40.62 18.1 17.9 17.3 5.40.683 18.2 3.30.491 19.0 4.30.471 17.6 3.80.56 17.5 5.20.71 17.7 19.0 4.30.493 18.2 3.50.461 18.2 4.30.541 17.2 18.4 17.5 4.50.704 18.7 5.90.531 18.2 5.10.611 17.8 5.90.623 17.6 17.3 5.50.613 18.5 19.1 18.9 18.3 Bj rDS 17.3 7.10.773 18.2 3.50.531 18.3 3.30.461 18.9 4.70.481 16.3 2.40.572 19.3 7.60.511 18.2 15.9 4.30.833 14.5 5.10.883 17.5 4.80.642 (6) (7)(8)(9) 18.3 3.50.491 15.1 4.30.753 18.9 3.70.471 19.0 5.10.463 18.5 3.80.531 18.5 3.90.461 17.7 *4.60.651 18.3 3.20.461 e 7.1 0.774 3.7 0.481 9.9 0.631 2.8 0.471 3.3 0.49 3.7 0.501 3.5 0.471 3.2 0.47 4.0 0.46 4.5 0.47 3.3 0.461 5.0 0.583 3.7 0.65 3.8 0.47 3.5 0.45 Table III.(continued) 0.57 5 0.64 5 0.60 0.69 5 B0203 B0201 B0199 B0198 B0208 B0207 B0206 B02Q5 B0204 B0202 B0200 B0197 B0196 B0210* B0209 B0211 B0217 B0216 B0214 B0213 B0212 B0225 B0223 B0222 B0221 B0220 B0219 B0218 B0215 B0227 B0226 B0224 B0232 B0230 B0228 B0235 B0234 B0233 B0231 B0229 B0248 B0247 B0245 B0244 B0242 B0240 B0238 B0237 B0250 B0249 B0246 B0243 B0241 B0239 B0236 B0252 32236.2-324440 B0255* 32238.0-341641 B0253 32236.6-334641 B0251 32235.1-350845 B0260 32244.6-345434 B0258 32242.6-354421 B0257 32241.8-322153 B0256 32241.4-380739 B0254 32237.0-333152 B0259 32242.8-331103 d) (2)(3)(4) # RA(1950)Dec(1950)M 3 2152.0-3550 3 2150.7-372029 3 2150.6-360955 3 2150.3-373400 3 2149.2-325546 3 2148.8-333501 3 2148.1-325605 3 2147.2-333149 3 2153.9-351603 3 2153.7-372533 3 2153.4-341544 3 2153.3-354922 3 2150.3-352926 3 2157.1-355419 3 2158.8-350458 3 2158.2-360926 3 2157.4-371200 3 2159.1-374922 3 2158.5-334059 3 2204.9-335826 3 2204.5-3738 3 2204.2-345348 3 2202.7-345343 3 2202.3-331318 3 2200.3-343009 3 2159.5-3728 3 2207.9-324155 3 2205.5-330652 3 2204.0-362614 3 2203.6-361426 3 2210.6-334612 3 2208.4-315903 3 2212.9-344957 3 2210.2-351425 3 2210.2-344403 3 2208.0-351732 3 2227.3-343254 3 2219.4-324652 3 2213.3-343202 3 2210.9-333825 3 2232.0-375251 3 2229.9-373104 3 2228.3-351356 3 2227.9-351719 3 2226.8-323729 3 2226.4-335109 3 2225.7-335105 3 2224.1-335249 3 2223.8-360458 3 2220.5-334034 3 2215.4-330838 3 2214.2-3249 3 2213.4-355131 3 2231.3-364555 3 2223.4-345207 4 SO/a 4 E(M32?) 4 S(interacting) 4 Epec 5 E 5 S 4 S 5 E 5 E(nb) 5 E 5 E 5 group 5 S 5 S 5 S 4 SordSO 4 SorImV 5 SB 5 E 5 4 S? 5 E 5 S 5 E(incluster) 4 E(M32?) 5 E 5 5 S 5 3 dE2? 4 S0 4 EordE2,N 5 SBbc(r)I 4 S? 5 S(nb) 5 Sc(s)II 5 5 E 5 E 5 S E ImlV? E E3(M32?) E S S S ordE2,N Sc(s)I S E E S? orImlV? S orImV S Type (5) 18.7 3.90.481 16.8 5.60.852 18.4 3.80.493 17.9 4.30.551 16.8 17.3 18.4 18.2 18.1 18.7 5.30.513 17.2 17.0 18.6 18.3 17.8 3.60.532 17.8 16.3 3.50.813 18.2 3.80.513 18.1 17.5 16.2 17.8 4.20.513 16.6 6.30.903 18.9 18.4 18.4 17.4 18.0 18.4 17.7 17.9 17.7 18.7 18.6 18.3 B rDS 18.9 19.1 18.5 17.7 18.5 18.9 18.4 15.8 17.9 18.8 18.7 18.2 18.8 18.4 18.7 17.6 18.3 (6) (7)(8)(9) 18.5 3.20.481 17.3 5.60.683 17.7 16.4 15.8 17.9 18.2 18.5 17.7 17.9 17.6 17.0 19.0 te 4.2 0.571 4.7 0.55 4.1 0.62 4.0 0.63 5.7 0.713 5.9 0.79 3.6 0.463 19 0.574 3.2 0.471 5.3 0.62 4.8 0.58 4.6 0.53 4.1 0.542 2.0 0.46 5.3 0.63 3.7 0.82 9.5 0.681 4.0 0.531 3.9 0.541 3.7 0.493 8.2 0.601 4.3 0.561 4.0 0.463 5.3 0.571 3.3 0.461 4.2 0.511 4.9 0.491 4.1 0.493 4.7 0.531 4.2 0.521 4.3 0.51 5.0 0.591 3.6 0.483 3.7 0.513 4.8 0.661 2.8 0.582 5.4 0.51 6.2 0.653 7.0 0.85 3.7 0.461 3.4 0.521 3.3 0.511 3.7 0.501 3.7 0.541 4.5 0.804 4.3 0.631 7.2 0.64 5.9 0.80 3.8 0.51 5.6 0.59 3.4 0.511 3.6 0.463 3.6 0.542 381 1989AJ 98. .367F 382 HENRYC.FERGUSON:THEFORNAXCLUSTER B0261 B0280 B0276 B0275 B0272 B0264 B0263 B0262 B0285 B0284 B0283 B0282 B0281 B0279 B0278 B0277 B0274 B0273 B0270 32252.0-363854 B0269 32251.1-3542 B0268 32250.6-350244 B0267 32250.3-3323 B0266 32250.2-363007 B0265 B0288 B0287 B0286 B0271* B0290 B0289 B0295 B0294 B0293 B0292 B0291 B0304 B0303 B0302 B0301 B0300 B0299 B0298 B0296 B0306 B0305 B0297 B0316 B0312 B0311 B0308 B0307 B0320 B0317 B0315 B0314 B0313 B0310 B0309 B0322 B0321 B0319 B0318 B0325 B0324 B0323 © American Astronomical Society • Provided by the NASA Astrophysics Data System (1) (2)(3)(4) # RA(1950)Dec(1950)M 3 2247.4-332644 3 2246.4-354441 3 2249.8-365313 3 2249.2-350559 3 2246.0-345044 3 2310.8-351018 3 2309.5-361538 3 2308.2-353017 3 2307.0-362430 3 2306.0-382500 3 2303.0-372251 3 2300.6-320158 3 2300.3-345743 3 2259.2-345455 3 2258.5-344943 3 2257.6-351216 3 2257.6-371458 3 2257.4-350403 3 2252.4-362840 3 2252.3-344639 3 2312.2-331528 3 2312.1-371500 3 2311.8-361514 3 2318.6-321645 3 2315.7-323839 3 2314.9-332507 3 2323.7-331354 3 2323.6-333960 3 2323.3-360360 3 232Z8-323103 3 2321.5-352035 3 2319.1-341506 3 2315.8-361625 3 2326.6-333854 3 2324.9-363825 3 2324.3-373119 3 2337.7-321130 3 23314-335413 3 2329.8-340221 3 2329.3-372619 3 2329.0-340314 3 2328.5-355548 3 2327.3-350233 3 2337.7-345247 3 2337.6-353411 3 2337.4-322015 3 2337.3-333605 3 2335.5-340245 3 2333.8-334417 3 2333.0-350232 3 2332.4-352814 3 2338.7-342931 3 2338.4-36W08 3 2343.4-340904 3 23412-353826 3 2341.4-363421 3 2340.9-324210 3 2340.1-330908 3 2339.5-360510 3 23415-321054 4 E 4 S? 4 4 E(M32?) 4 S?ordSO 4 ? 4 E 5 E 5 E 5 E 4 SordSO 5 S 5 S 5 S 5 S 5 S 5 S 5 S0 5 S 5 S 5 S 5 S+flaw 4 SordSO 5 S 3 ? 3 EordE(M32?) 3 dE2pec? 4 E 4 SorE(M32?) 4 E 4 (onedge)pec 5 E 5 E 5 S 5 S(onedge) 5 S 4 E 4 E(incluster) 5 S(interacting) 5 E 5 5 E 5 S 4 SorImV 4 S 4 E(M32?) 4 E 4 E(M32?) 5 Sc(r)MI(interacting) 3 SordEN 5 Sc(s)I 5 Sc(s)MI 5 S(onedge) 3 E(M32?) 5 S 5 S 4 S 5 5 E 5 E(nb) 5 E 5 E 5 S0 5 E 3 dEO Type (5) 18.5 3.80.471 17.4 3.10.572 17.2 100.502 18.0 4.10.511 18.0 4.80.581 17.8 18.2 17.4 17.2 17.2 18.8 5.20.541 16.9 10.40.821 18.2 4.10.54 17.2 17.8 17.7 17.3 17.9 17.7 18.7 17.2 19.2 4.50.481 18.5 3.80.491 18.6 4.20.49 18.9 3.90.50 16.5 5.50.783 18.9 3.70.461 17.9 3.90.513 18.5 18.1 18.4 18.9 16.3 3.50.663 18.9 3.40.471 19.0 18.2 18.2 18.5 17.6 17.3 18.8 17.8 17.1 18.1 15.6 17.8 18.5 By DS 17.3 4.00.621 17.0 6.20.694 18.7 5.40.501 18.1 4.10.513 16.2 4.80.674 18.1 16.9 16.8 18.5 4.10.533 18.9 4.00.473 18.4 3.40.471 17.7 5.80.681 17.9 7.20.721 (6) (7)(8)(9) 18.2 18.5 18.4 17.9 17.8 10.6 0.79 4.0 0.50 4.3 0.61 5.4 0.643 6.4 0.741 2.7 0.56 6.9 0.61 4.8 0.52 3.8 0.481 3.5 0.662 3.6 0.491 3.1 0.61 4.1 0.63 4.1 0.55 4.8 0.54 4.1 0.46 5.4 0.52 3.3 0.50 3.8 0.48 3.1 0.50 3.4 0.50 3.9 0.50 8.9 0.78 3.9 0.53 6.4 0.83 3.7 0.59 3.7 0.55 3.6 0.75 3.4 0.52 3.8 0.51 8.8 0.86 4.3 0.67 5.4 0.52 3.9 0.48 3.8 0.49 Table III.(continued) 0.66 5 0.59 5 0.65 5 B0347 B0344 B0343 B0342 B0341 B0337 B0329 32349.3-3635195SBb(s)I B0328 32348.5-3409205(interacting) B0327 32347.0-3525515S B0326 32344.0-3336594E(M32?) B0346 B0345 B0340 B0339 B0338 B0336 B0335 B0334 B0332 B0331 B0330 32349.5-3639055E(cD) B0350 B0349 B0333 B0353 B0352 B0351 B0348 B0358 B0357 B0356 B0355 B0360 B0359 B0354 B0365 B0364 B0361 B0369 B0368 B0367 B0366 B0363 B0362 B0370 B0377 B0376 B0375 B0374 B0373 B0372 B0371 B0385 B0384 B0383 B0382 B0381 B0380 B0379 B0378 B0386 B0388 B0387 B0390 B0389 (1) (2)(3)(4) # RA(1950)Dec(l950)M 3 2403.2-361205E0(M32?) 3 2351.4-37465S 3 2349.6-374149E(M32?) 3 2403.7-3416585Sb(r)I 3 2402.4-3659465S0 3 2402.2-3248135E 3 2402.1-3805365S 3 2359.3-3246185S 3 2358.5-3646395E 3 2357.7-34415E 3 2357.1-3550375S 3 2356.1-3538354S 3 2355.5-3430155Sbc(onedge) 3 2354.6-3353605SBbc(r)II 3 2354.1-3537295E 3 2352.6-3444144(interacting)? 3 2352.3-3635474Epec 3 2409.7-362546 3 2408.3-3804075E 3 2406.1-3526415S 3 2404.5-3700165E 3 24112-370325 3 2412.1-351904 3 2411.2-333455 3 2414.9-3753305 3 2414.3-3506075 3 2413.8-3729095 3 2412.8-334020 3 2420.4-3752485S 3 2419.8-3354275E 3 2418.5-3339035S 3 2417.6-3343235E(incluster) 3 2417.5-3326415S(nb) 3 2415.6-3714105E 3 2415.5-3459015S 3 2420.4-354756 3 2423.5-320923 3 2422.4-351606 3 2421.5-343234 3 2421.3-343204 3 2429.0-3509465SBc(s) 3 2427.8-3446475S 3 2425.5-335704 3 2425.1-3415 3 2424.5-335934 3 2424.0-380436 3 2424.0-381812 3 2423.8-334442 3 2429.9-3316225E 3 2429.9-3447595 3 2426.5-3432385S 3 2426.2-323360 3 2425.8-365827 3 2425.6-351249 3 2424.2-344948 3 24317-325025 3 2432.0-370010 3 2430.5-355618 3 2434.0-334527 3 2433.9-362042 4 E 4 E(cD)? 5 S0 5 E 5 S 4 ? 4 E 5 S 5 E 5 E 5 S 4 S 4 E(M32?) 4 dE? 4 E(M32?) 4 E 5 E 5 S 4 E 5 S 3 dSO? 5 S 5 (interacting) 5 S 3 dE? Type (5) 18.5 16.5 18.3 6.00.601 17.8 4.40.593 17.5 5.80.641 18.1 17.7 17.0 17.6 18.1 18.7 18.1 16.0 16.6 16.5 17.7 17.8 18.3 17.1 17.2 17.7 17.2 17.8 18.1 18.7 17.6 17.9 17.9 18.7 18.2 18.4 18.0 18.1 16.1 12.50.994 17.1 5.80.752 17.8 16.0 17.3 18.6 16.9 17.7 17.6 18.2 18.1 Bj rDS 17.4 17.8 18.0 18.6 18.8 16.5 (6) (7)(8)(9) 17.2 4.50.703 18.8 3.80.461 16.5 6.40.913 18.4 4.60.493 18.0 5.00.651 17.7 5.50.613 18.7 4.40.561 18.8 4.10.471 17.9 7.80.623 17.6 3.80.572 16.4 6.80.752 18.2 3.30.481 18.3 4.00.541 18.4 17.2 9.80.831 e 4.4 0.513 4.1 0.581 4.5 0.591 4.0 0.471 4.0 0.493 4.1 0.553 4.1 0.69 4.6 0.724 4.0 0.513 2.3 0.542 5.6 0.713 2.9 0.702 3.6 0.561 3.3 0.451 3.3 0.763 3.0 0.654 2.2 0.462 2.7 0.563 2.7 0.56 7.8 0.47 7.8 0.71 3.9 0.49 3.4 0.46 3.1 0.57 3.6 0.53 3.4 0.53 6.4 0.771 5.1 0.784 2.3 0.502 3.2 0.491 3.7 0.511 3.3 0.50 4.7 0.621 2.4 0.462 3.2 0.491 4.3 0.56 3.9 0.633 4.7 0.51 4.8 0.79 5.0 0.531 5.3 0.613 3.2 0.471 3.5 0.501 2.9 0.46 3.5 0.481 0.63 382 1989AJ 98. .367F 383 HENRYC.FERGUSON:THEFORNAXCLUSTER B0391 32435.9-3340415Sb B0393 32436.1-3329045E B0392 32435.9-3430595S0? B0395 32437.0-32185E B0394 32436.9-3351284E B0399 32441.2-3714134E B0398 32441.1-3521134E B0397 32440.1-3756305S B0396 32439.5-3343395S B0400 32441.3-3344295E © American Astronomical Society • Provided by the NASA Astrophysics Data System B0405 32445.1-3512194E(M32?) B0404 32444.9-3247505E B0403 32444.5-3509554E(M32?) B0402 32442.6-3438314SO/a B0401 32441.6-3246315E B0408 32446.3-3629345S B0407* 32445.7-3512475S0(5)/E5(incluster) B0406 32445.6-321411dE? B0410 32448.4-3534045E B0409 32447.1-3425355S B0411 32448.5-3458385E B0417 324526-351738S B0414 32451.1-3258074S0(incluster) B0413* 32450.5-3425314group B0412 32448.8-3254025S B0418 B0416 32452.3-3548065S B0415 32451.7-3513485 B0420 32453.5-3432435Sbc(s)I-II B0419 B0421 32454.5-362959E(M32?) B0423 32455.0-3638605group B0122 32454.7-35565S B0424 32455.2-3430235Sc(s)I-II B0425 32455.4-3217044E(M32?) B0426 32455.8-3500374? B0429 32456.4-3257535 B0428 32456.2-3455515S B0427 32456.0-3518014E(M32?) B0431 32457.0-3253205E B0430 32456.7-3527084E(M32?) B0434 32501.7-3250354S(interacting)? B0432 32457.7-3637365S B0440 32510.7-3450285S B0439 32507.8-35385S B0438 32505.4-3646015S B0437 32505.2-3348045 B0436 32502.6-3646205S0(6) B0435 32501.9-374311dEl B0433 32458.9-3259544E B0445 32513.7-333433E(M32?)? B0444 32512.8-3639475S B0443 32511.9-3457595SBbcE B0442 32511.5-3648304E B0446 32515.1-3719294E(M32?) B0441 32511.4-3252345S B0447 32517.0-3829245S B0449 32518.0-35024E(M32?) B0448 32517.9-3738104S0(M32?)? B0450 32520.0-3452054Epec? B0452 32521.9-362453ImV B0451 32521.6-3502285S B0453 32522.2-3702154 B0455 32525.1-3649125S B0454 32524.1-3406575S0(9) (1) (2)(3)(4) # RA(1950)Dec(1950)M 3 2453.2-323910ImVorS 3 24526-364921S Type (5) 18.5 3.60.461 18.4 3.50.491 16.7 3.70.704 17.7 17.8 18.4 4.50.541 17.8 2.80.492 18.3 18.2 18.5 17.8 3.50.552 17.3 2.90.542 16.7 4.80.743 17.6 3.20.514 18.9 3.50.461 14.9 16.51.224 19.5 5.20.461 17.5 6.20.713 18.4 3.60.501 17.9 4.60.583 16.3 11.90.914 17.3 4.40.642 18.2 4.30.561 18.8 4.70.563 18.5 18.2 18.0 17.8 4.20.592 B DS 16.3 19.1 (6) (7)(8)(9) 16.2 17.5 17.9 17.0 19.2 18.9 18.0 17.4 18.0 18.3 18.2 17.4 18.7 16.9 18.2 17.6 16.5 18.2 18.4 17.0 18.5 T 16.7 17.0 16.6 18.1 17.2 18.3 16.3 16.0 18.8 18.6 17.7 16.8 17.2 18.7 4.0 0.531 4.4 0.591 5.9 0.641 3.0 0.463 3.6 0.481 4.2 0.483 4.9 0.68 6.9 0.914 3.7 0.493 3.5 0.501 3.6 0.521 4.8 0.61 7.4 0.79 4.0 0.62 2.8 0.59 5.1 0.46 4.9 0.543 3.9 0.56 3.8 0.53 3.7 0.50 4.3 0.46 9.2 0.663 6.9 0.811 5.7 0.792 3.4 0.461 4.2 0.742 4.2 0.543 4.5 0.55 5.7 0.61 2.8 0.59 3.5 0.66 4.5 0.70 2.6 0.542 2.4 0.553 3.1 0.674 5.6 0.63 5.2 0.82 3.4 0.46 4.2 0.483 5.3 0.563 3.2 0.622 3.3 0.461 3.8 0.693 Table III.(continued) 0.77 0.78 B0456 B0460 B0459 B0458 B0457 B0469 B0468 B0467 B0466 B0465 B0464 B0463* 32534.9-3655265Sbc(r)I(HighSB) B0462 B0461 B0470 B0472 B0471 B0474 B0473 B0475 B0476* 32541.0-334345 B0477* 32542.9-373738 B0478 32543.1-370319 B0481 B0480 32545.8-3455 B0479 32544.6-351024 B0483 B0482 B0485 B0484 B0486 B0490 B0489 B0488 B0487 B0494 B0492 B0491 B0495 B0493 B0496 B0501 B0500 B0499 B0498 B0497 B0504 BQ503 B0502 B0510 B0509 B0508 B0507 B0506 B0505 B0512 B0511 B0513 B0515 B0514 B0517 B0516 B0519 B0518 B0520 (1) (2)(3)(4) # RA(1950)Dec(1950)M 3 2527.4-374635 3 2525.9-332451 3 2530.7-374936 3 2529.5-361007 3 2528.0-335054 3 2531.2-3418205S(onedge) 3 2537.8-355322 3 2537.6-3746 3 2537.1-340702 3 2537.1-332629 3 2536.0-364519 3 2535.4-3314204E(incluster)orE(M32?)17.64.00.622 3 2535.1-3318455E 3 2531.6-350708? 3 2538.0-325619 3 2538.5-325713 3 2538.3-361056 3 2538.8-335124 3 2539.0-335841 3 2546.6-3343194SordE?,N 3 2549.2-3502175E 3 2547.0-3503425E 3 2546.7-3512054E(M32?) 3 2548.2-3500465 3 2550.6-374522 3 2549.8-341416 3 2551.1-361950 3 2552.1-374631 3 2551.8-362829 3 255Z4-354335 3 2555.2-3554 3 2554.9-361706 3 2554.7-374603 3 2554.6-345559 3 2555.6-364636 3 2601.4-334206 3 2559.8-371508 3 2558.3-355659 3 2556.7-355638 3 2602.4-361408 3 2609.5-371758 3 2607.8-363016 3 2604.8-3358 3 2604.4-362138 3 2603.1-3638 3 2603.0-343728 3 260Z7-360649 3 2610.2-341440 3 2608.1-3607 3 2611.0-354903 3 2611.1-351259 3 2611.1-362005 3 2613.1-330857 3 2614.0-320841 3 2617.1-362837 3 2617.0-344852 3 2615.4-342247 3 2618.1-350702 3 2618.0-344641 4 dE(M32?) 5 E(incluster) 5 S 5 5 Epec? 4 ? 4 E(M32?) 5 5 E 4 E(M32?) 5 S 5 E 5 E(incluster) 4 EordE,N 5 E 5 S 5 E 5 (interacting) 5 S 4 SBbc(s)II 4 S 5 E 4 5 E(nb) 5 S 5 E 4 E(nb) 3 dENorS 5 E 5 S(interacting) E(M32?) S orImlVN S S S BCD(High SB)orS E(M32?) S orImlV S S S E SBbc(rs)II Spec E(cD) S0 Sc S E6(M32?) E SbcI-II pec ? Type (5) 17.7 4.40.622 17.9 3.90.553 18.8 4.50.541 18.3 3.30.461 17.0 4.00.643 19.1 5.20.503 18.8 3.70.461 18.2 6.70.621 15.8 5.60.844 16.9 7.00.744 16.9 4.10.623 17.4 3.70.622 18.2 4.10.523 17.1 3.00.562 18.0 4.20.543 16.8 3.50.682 18.6 4.30.471 18.4 4.20.493 17.3 3.30.602 16.3 2.60.594 15.6 3.90.813 Br r,DS 18.3 4.20.471 (6) (7)(8)(9) 18.2 18.0 18.4 16.6 18.6 18.1 4.30.523 18.6 3.40.461 19.0 18.8 18.6 18.0 16.3 18.2 18.5 18.0 18.8 17.8 18.2 18.4 17.0 18.0 16.4 3.60.653 17.7 18.3 3.30.523 18.5 4.80.461 18.0 4.10.543 18.1 3.60.463 18.5 4.20.501 18.6 6.30.481 17.7 4.80.613 17.1 3.20.583 17.9 4.30.553 18.3 18.3 17.3 4.10.722 16.7 8.00.863 18.0 4.60.691 16.4 4.80.784 17.7 3.00.483 17.7 4.50.551 18.6 5.00.571 19.1 4.00.463 4.6 0.56 4.2 0.50 5.7 0.82 4.8 0.54 4.2 0.48 3.9 0.48 4.9 0.51 3.8 0.52 4.3 0.56 8.3 0.84 4.1 0.50 6.9 0.67 2.8 0.59 6.6 0.64 3.3 0.52 3.3 0.48 3.2 0.58 3.0 0.48 3.9 0.54 5.9 0.64 5.3 0.551 3.3 0.471 383 1989AJ 98. .367F 384 HENRYC.FERGUSON:THEFORNAXCLUSTER B0541 32637.8-3306525E B0539 32636.5-3641245E B0527 32622.9-3542325 B0526 32622.1-3745555S0 B0525 32622.1-3534185E B0524 32621.6-3324554 B0523 32621.2-3520185E B0522 32620.1-3613605S B0521 32618.9-3S1204SE B0547 32644.3-3255064S0ordS0(6) B0546 32643.1-3304515E B0545 32641.6-35535SO B0544 32639.7-3745594S(interacting)? B0543 32639.5-3401584S B0542 32638.6-3259505E(incluster) B0540 32637.8-3452425S B0538 32633.8-3610165S B0537 32632.9-3443555E B0536 32631.3-3603244E B0535 32630.6-3505595Sab(r) B0534 32630.2-3602324E B0533 32629.5-3413045E B0532 32627.2-3502395SBc(s)II B0531 32626.9-3559024S0 B0530 32626.1-3700295E B0529 32624.5-3433445S B0528 32623.0-3359474SBbcïï(LSB) B0548 32645.1-3410024ScII(HighSB) B0556 32652.8-3723475S B0558 32654.0-3646074Sb(inteiacting) B0557 32653.3-323445dE3,N? B0555 32651.6-3246525(interacting)? B0552 32648.6-3422025E B0550 32646.8-3447125 B0549 32646.7-3603194EordE2,N B0554 32650.8-3254284SO B0553 32649.9-3410435S(onedge) B0551 32647.4-3306325E B0579 32711.7-3259554E B0578 32711.0-3410064S0(2),NordS0(2),N B0577 32708.6-3424034? B0576* 32708.6-3529465SBcI-II B0575 32707.1-3207354E B0574 32706.8-35535E B0573 32706.7-3752134? B0571 32704.7-3541195S B0570 32704.5-3753034E(M32?) B0569 32704.5-3521285S B0566 32701.3-3615175Sc B0564 32701.1-3309365E B0563 32700.8-3424075Sc(s)I-II B0562 32700.8-3438215? B0561 32659.3-3644595S B0560 32656.6-3252155E B0559 32656.6-3632085 B0572 32704.9-3255255E B0568 32704.3-3354535S B0567 32704.0-3814305Sbc B0565 32701.2-3515114E B0583 32715.2-3445285E B0581 32713.9-3755525E(nb) B0580 32713.3-3507535SO/a B0585 32717.5-3631395E B0584 32715.7-334450EordEN B0582 32714.4-3602475EorS0 © American Astronomical Society • Provided by the NASA Astrophysics Data System (1) (2)(3)(4) # RA(1950)Dec(1950)M Type (5) 19.0 4.50.471 17.1 3.50.644 18.6 4.80.531 18.0 16.2 3.80.714 18.4 4.10.531 18.0 8.80.633 18.4 3.20.461 17.6 4.80.633 18.9 3.50.481 18.9 4.40.471 18.1 3.60.471 17.5 5.70.793 18.0 18.4 3.90.513 18.1 17.7 16.5 5.10.852 18.6 4.20.531 17.3 4.90.673 18.2 17.9 17.2 18.5 18.1 18.5 18.8 18.2 3.70.491 19.4 4.50.463 16.8 2.20.483 16.8 4.70.733 18.1 3.70.571 18.1 18.6 19.0 18.1 17.9 19.2 17.1 17.6 18.3 17.1 14.8 18.0 17.0 18.5 18.8 16.7 0.86 16.2 2.70.54 18.0 17.8 17.4 18.4 17.1 18.5 17.5 17.8 16.7 6.00.84 18.7 3.80.46 18.6 4.40.51 18.0 18.0 18.3 17.5 18.2 Bj rDS (6) (7)(8)(9) e 4.0 0.551 4.3 0.621 4.2 0.60 4.3 0.50 5.8 0.691 5.3 0.59 4.8 0.63 4.3 0.54 3.9 0.551 4.3 0.52 4.1 0.53 4.7 0.72 3.4 0.48 3.4 0.47 4.1 0.60 4.6 0.47 4.7 0.66 4.6 0.58 2.3 0.50 3.8 0.50 4.2 0.55 5.5 0.58 5.6 0.63 6.8 0.85 2.1 0.47 6.4 0.59 5.5 0.70 5.5 0.63 3.7 0.51 3.8 0.50 7.4 0.63 3.2 0.47 3.6 0.53 3.5 0.46 5.0 0.64 7.7 0.74 2.6 0.51 3.7 0.51 8.5 0.58 Table III.(continued) B0586 B0607 B0606 B0605 B0604 B0603 B0602 B0601 B0600 B0591 B0590 B0589 B0588 B0587 B0599 B0598 B0597 B0596 B0595 B0593 B0592 B0609 B0608 BQ594 B0612 B0611 B0610 B0613 B0616 B0615 B0614 B0646 32824.0-335333 B0645 32821.8-355447 B0644* B0643 B0642 B0641 B0640 B0639 B0638 B0637 B0636 B0630 B0627 B0626 B0625 B0624 B0623 B0622 B0621 B062Û B0619 B0618 B0617 B0649 32826.3-341138 B0648 32825.8-323315 B0647 32824.9-360925 B0635 B0633 B0631 B0629 B0628 B0634 B0632 B0650 32826.8-334900 (1) # RA(1950) Dec(1950)M 3 2718.4-364521 3 2741.8-3531 3 2741.6-360512 3 2737.7-3738415S 3 2737.5-3629095S 3 2735.0-3823425SBab 3 2734.4-3726335Sc(s)II 3 2732.7-3232124E 3 2730.6-3439215E 3 2730.0-3731395S 3 2726.2-370955 3 2725.7-350802 3 2721.9-352141 3 2720.7-344842 3 2719.2-375107 3 2719.1-360408 3 2746.1-321029 3 2744.1-324210 3 2743.3-343803 3 2729.3-3518404E(M32?) 3 2729.3-3628295 3 2728.8-360937 3 2728.5-371710 3 2728.4-351556 3 2729.1-360856 3 2753.8-361052 3 2751.3-360906 3 2747.1-363448 3 2746.7-344507 3 2756.8-351211 3 2755.5-365618 3 2755.3-365309 3 2753.7-365711 3 2752.1-325743 3 2751.8-360946 3 2820.3-3524 3 2820.0-354432 3 2820.0-381060 3 2818.8-334929 3 2817.9-3545 3 2816.4-351244 3 2759.2-375643 3 2758.0-350401 3 2757.9-345137 3 2755.8-325434 3 2816.0-381906 3 2815.6-355032 3 2813.1-335245 3 2813.0-320339 3 2805.5-354634 3 2803.5-375059 3 2802.8-324506 3 2802.4-322730 3 2800.2-375653 3 2759.3-355321 3 2758.4-344942 3 2813.0-342512 3 2810.4-365713 3 2810.3-365811 (2) (3)(4) 4 SordE0,N 4 E(M32?)orBCD 4 E(M32?) 5 5 S 4 S 4 E(M32?) 5 E 5 E 5 S 5 S 5 S 5 S 5 S 3 dE0,NorSmV 5 E 5 E 3 dE/ImV 4 S0 5 E 5 E 5 E 4 ? 5 S 5 S 5 E 5 S 5 E 4 S 5 SBb(r)HI 5 S 5 E 3 S(LSB)orSdV 4 ? 4 E4(M32?) 5 E 5 (interacting) 5 S 5 S 5 pec 5 S 5 S 5 S 5 S 5 E 5 S 5 E 5 E 5 S E s S S S ordSO Type (5) 18.1 18.7 15.9 18.3 17.2 15.3 17.3 17.1 5.30.743 17.4 4.80.733 16.3 4.00.804 17.9 4.50.601 18.5 4.80.561 19.1 3.60.471 18.4 4.50.553 17.8 3.20.492 18.8 3.60.461 17.1 18.3 3.80.521 18.8 3.80.483 16.8 5.00.803 18.5 3.70.471 18.0 3.90.593 17.9 4.10.621 18.6 19.2 5.10.543 18.6 3.20.473 17.8 19.0 17.3 18.0 4.50.531 18.5 17.5 6.50.781 17.6 3.10.494 18.1 3.50.493 16.1 4.10.794 18.7 3.60.461 18.0 3.80.503 18.0 5.40.701 18.3 3.70.481 18.7 18.6 18.3 3.50.473 17.6 4.10.622 14.5 1.145 18.2 3.50.531 18.1 16.9 18.5 18.3 17.6 4.00.594 18.1 4.00.501 18.4 4.30.503 17.5 4.50.581 18.0 18.7 3.60.471 18.4 5.00.623 17.5 4.90.701 17.9 4.40.583 17.9 17.7 17.7 18.6 B rDS 18.5 17.6 18.5 (6) (7)(8)(9) Te 4.6 0.56 4.0 0.47 2.7 0.573 2.3 0.502 4.2 0.62 3.4 0.49 3.9 0.583 3.6 0.683 2.7 0.56 9.9 0.803 5.1 0.491 4.3 0.52 4.3 0.50 3.8 0.521 4.2 0.59 4.7 0.56 4.5 0.533 4.6 0.601 5.4 0.511 3.5 0.51 4.9 0.593 4.6 0.583 3.2 0.461 3.8 0.481 3.9 0.481 0.72 5 0.81 5 384 1989AJ 98. .367F 385 HENRYC.FERGUSON:THEFORNAXCLUSTER B0651 32827.7-3409015S0(nb) B0654 32830.2-3450225Sc(s)I B0652 32829.5-3333265S B0656 32833.0-3644105S B0655 32830.6-3554204S B0653 32829.7-3632425Sc(s)II B0664 32842.3-343448dSO?orS B0663* 32839.6-320609dE,N B0661 32837.4-3230264 B0660 32836.3-3322485E B0659 32834.8-3311214E(M32?) B0658 32834.5-36105S B0657 32834.3-3532154S B0665 32842.7-3204414E B0662 32838.0-3204075S(interacting)? B0669 32845.1-3312475E B0667 32843.3-3658445E(nb) B0666 32843.3-3705425S B0670 32845.7-3620505E B0668 32843.7-3405395S B0675 32849.0-3626195S B0673 32847.9-3409535S B0672 32847.3-3448515E(interacting) B0671 32846.8-3741275S B0679* 32853.0-3821305SBb(s)IIpec B0676 328525-344851(interacting) B0674 32848.0-3705224 B0678 328527-3345325S(onedge) B0677 328527-3349534Sbc(s)II B0680 32854.4-3224304E(nb)? B0684 B0683 B0682 B0681 B0685 B0688 32903.0-3509165S B0687 „32859.9-3248105S B0686 32859.6-3254535S B0689 32903.2-3510155 B0700 32911.9-3719135S B0698 32909.5-3430484E B0697 32909.1-3333474? B0696 32908.9-3414105S B0695 32906.4-3410125E B0694 32906.0-3731244S B0693 32904.4-37065S B0692 32904.1-3538144E(M32?) B0691 32903.7-3433345Sb(r)II B0690 32903.3-3203105E B0704 32915.7-3356164 B0703 32915.1-3717145E B0702 32912.2-3805364SorSm(onedge) B0701 32912.1-3735094E(M32?) B0699 32909.8-3405105E(incluster) B0705 32916.0-3843065S(onedge) B0706 32917.5-3635335 B0709 32921.3-3543064S B0708 32919.2-3352555S B0707 32917.8-3624304ScI-II(LSB) B0712 32923.8-3545054E(M32?) B0711 3292Z0-3648145 B0710 32921.9-3311265E B0715 32926.8-3410555E B0714 32925.3-3233515E B0713* 32925.0-3539345SO/apec © American Astronomical Society • Provided by the NASA Astrophysics Data System (1) (2)(3)(4) # RA(1950)Dec(1950)M 3 2854.7-3622055S 3 2857.9-3503485SBcII 3 2855.7-3357005S? 3 2859.2-3406305S(onedge) 3 2857.5-3204174? Type (5) 18.2 4.50.641 19.1 17.5 16.1 16.1 19.0 4.10.511 18.5 16.2 17.9 18.3 18.7 18.1 18.2 16.4 18.6 3.70.471 18.8 18.8 4.50.501 18.4 4.80.563 17.9 4.40.621 18.3 5.50.561 17.0 11.20.921 18.2 3.40.481 18.5 16.0 18.7 3.70.463 17.2 18.8 16.3 Bj rDS 18.1 16.2 17.9 (6) (7)(8)(9) 18.2 18.2 18.0 17.6 18.9 5.10.511 17.9 4.30.571 19.3 6.60.511 17.9 5.40.721 18.2 3.30.461 17.4 17.7 18.0 19.0 17.8 18.0 18.1 18.4 18.7 17.3 18.4 16.8 17.2 17.1 17.9 16.8 18.1 17.9 19.1 18.6 18.5 17.1 18.1 18.3 15.5 e 12.6 0.98 4.2 0.521 4.4 0.53 4.1 0.51 2.9 0.692 5.1 0.783 2.5 0.584 4.7 0.48 5.9 0.73 3.1 0.532 3.7 0.531 3.8 0.461 3.6 0.561 4.5 0.543 4.0 0.511 4.1 0.521 7.3 0.713 2.7 0.602 5.7 0.774 4.7 0.653 2.8 0.483 5.5 0.621 3.3 0.471 3.9 0.501 4.7 0.66 4.3 0.491 4.4 0.613 4.8 0.611 4.1 0.481 4.1 0.511 6.4 0.76 2.2 0.58 6.6 0.803 3.5 0.511 3.9 0.49 3.2 0.60 4.9 0.46 4.9 0.61 4.5 0.54 3.9 0.471 9.8 0.87 3.6 0.581 7.0 1.00 3.4 0.46 3.5 0.62 3.4 0.52 3.6 0.52 3.4 0.48 Table III.(continued) 0.97 5 0.58 5 B0716 B0719 B0717 B0720 B0718 B0725 32936.8-343510 B0723 32933.4-372052 B0722 32931.7-352257 B0721 32931.7-362016 B0729* 32940.0-381354 B0728 32939.5-332300 B0727* 32937.6-375207 B0726* 32936.9-330052 B0724* 32935.1-321841 B0734 B0732 B0731 B0730 32941.2-330033 B0737 B0735 B0733 B0736 B0740 B0739 B0738 B0746 32953.9-3445574E B0745 B0744 B0743 B0742 B0741 B0749 32958.4-3735504 B0747* 32955.9-3714175Sc(s)I B0750 32958.5-3425515E B0748 32956.8-3313054? B0752 32959.8-3517095 B0755* 33001.8-3734034S B0754 33001.0-3631085E B0753 33000.0-3824545S B0751 32959.3-3232415E B0760 B0759 B0758 B0756 B0767 B0765 B0762 B0761 B0757 B0770 B0769 B0768 B0766 B0764 B0763 B0772 B0771 B0775 B0774 B0773 B0777 B0776 B0780 B0778 B0779 (1) # RA(1950) Dec(1950)M 3 2929.8-344910 3 2929.1-323849 3 2928.0-354208 3 2931.0-315325 3 2929.8-351511 3 2947.0-373215 3 2944.0-342705 3 2942.8-375519 3 2942.3-345943 3 2942.0-324406 3 2947.5-373160 3 2947.4-340127 3 2946.2-343558 3 2945.2-320852 3 2950.9-3433484S 3 2953.3-3751dE4 3 2951.5-343756SordSO 3 2950.8-3305554E 3 2949.3-3431185Sc(s)II 3 2947.5-335909 3 3003.7-343738 3 3003.5-353437 3 3003.1-330945 3 3005.3-354214 3 3005.0-363518 3 3005.0-330439 3 3004.1-330647 3 3006.5-352718 3 3006.4-362139 3 3005.7-360858 3 3005.5-342610 3 3005.1-340116 3 3007.6-322402 3 3009.8-341609 3 3009.5-353534 3 3008.1-323722 3 3012.3-364004 3 3012.0-380960 3 3011.6-320723 3 3011.6-350916 3 3015.7-3757224E 3 3017.4-3454575 3 3016.8-3213514? 3 3013.2-3714315E 3 3017.1-3412195E (2) (3)(4) 4 ? 5 S 5 S 5 S 5 pec 5 E 5 S 5 Sc(s)I 3 dE 5 S 5 Sc(LSB) 3 dE 3 dSO 4 grouporIm 3 dSOorSO 5 S 3 E(M32?) 3 ImV? 5 E 5 E 5 S 5 S 5 E 5 S 5 SBc(s)MI 4 E(M32?) 4 (interacting)? 4 5 E(M32?) 5 E 5 S 5 S 5 E 5 S 5 S 5 SBa(r) 5 S(onedge) 5 S 3 dE/Im? 5 S ImV? S Type (5) 18.8 3.90.461 17.2 4.40.574 17.8 5.30.631 18.2 3.90.561 18.4 4.20.463 18.4 3.80.501 17.6 4.50.661 18.6 4.30.483 17.9 8.40.681 16.3 4.00.673 17.6 3.40.512 16.9 7.30.753 19.0 4.50.511 16.5 0.875 17.4 4.40.643 18.3 3.80.491 18.7 3.50.483 16.2 2.80.722 18.8 4.30.491 17.9 2.60.462 19.0 6.20.501 18.4 3.80.481 16.8 2.40.584 17.2 5.60.704 B rDS 17.9 3.90.543 16.7 6.50.763 17.1 3.40.621 18.2 6.10.643 17.6 4.30.641 18.7 3.60.471 17.5 5.30.643 17.6 1.90.462 (6) (7)(8)(9) 17.1 4.80.723 18.0 3.90.493 17.7 4.70.561 16.4 0.935 19.1 4.40.463 18.7 3.80.461 18.0 4.90.593 17.1 4.60.693 18.2 17.3 18.9 18.8 17.3 18.8 18.0 17.9 18.5 17.7 18.9 17.6 18.6 18.8 te 18.2 3.50.471 19.3 16.7 2.90.624 17.8 6.10.701 19.0 3.60.483 16.4 8.10.902 17.9 5.10.651 18.3 4.20.531 18.4 3.70.491 17.1 270.542 18.2 4.50.561 4.5 0.68 4.4 0.70 4.2 0.60 5.9 0.53 5.4 0.71 6.7 0.60 4.4 0.61 3.3 0.54 5.3 0.49 5.0 0.59 5.0 0.51 3.6 0.47 3.7 0.49 3.5 0.49 5.3 0.52 385 1989AJ 98. .367F 386 HENRYC.FERGUSON:THEFORNAXCLUSTER B0785 B0784 B0783 B0782 B0781 B0787 B0786 B0797 33035.4-3328194E(incluster)or(M32?)17.24.80.692 B0795 33035.1-371816 B0794 33033.3-325556 B0792 33031.7-375814 B0790 33031.5-315909 B0789* 33029.9-354418 B0788 B0800 33041.5-3509014S0 B0799 33041.3-3804445S B0798 33038.2-3546315S B0796 33035.3-3755564E B0793* 33033.0-381548 B0791 33031.6-373116 B0805 33049.8-325006 B0804 33049.5-3238 B0803 33043.4-371936 B0802 33042.4-321944 B0801 33041.7-364309 B0807 33051.0-351726 B0806 33049.9-325457 B0810 33051.7-361529 B0809 33051.7-343744 B0808 33051.3-315344 B0812 B0815 B0814 B0813 B0811 B0821 B0820 33059.0-324125 B0817 33054.5-350105 B0816 33054.4-343928 B0819 33058.7-334555 B0818* 33057.5-351822 B0829 B0825 B0824 B0823 B0822 © American Astronomical Society • Provided by the NASA Astrophysics Data System B0834 33106.2-3246 B0826 B0836 33107.4-324142 B0835 33106.2-344316 B0833 33106.1-375811 B0831 33105.3-354633 B0830 B0828 B0827* B0832 33106.1-330319 B0841 B0839 33111.6-325100 B0838 33111.1-371711 B0837 33110.0-331607 B0840 33112.5-351543 B0844 B0843 B0842 B0845 (1) # RA(1950) Dec(l950)M 3 3020.5-375702 3 3023.8-364613 3 3023.6-375805 3 3020.3-325855 3 3023.9-373242 3 3021.3-331600 3 3028.6-3515 3 3025.0-354709 3 3054.3-331820 3 3052.6-373210 3 3052.1-353610 3 3053.3-360644 3 3052.9-331915 3 3059.8-332107 3 3101.8-362745 3 3100.4-335440 3 3101.4-372422 3 3104.9-353705 3 3102.4-354145 3 3102.4-372813 3 3101.9-3429 3 3105.2-330340 3 3102.8-342648 3 3113.3-330251 3 3113.9-315702 3 3113.8-380005 3 3116.0-371914 3 3115.9-372010 (2) (3)(4) 4 E? 4 SorlmlV 4 SordEJN 5 S 4 grouporIm 4 E(M32?) 5 S 4 S 5 E 5 S 5 Sc 5 S 4 E 5 E 5 5 S 5 S 5 S 5 S 3 BCD(HighSB)? 5 S 5 S 5 S 5 S? 4 E(M32?) 4 E 5 E 5 S 5 S 4 E 4 S0(6)(M32?) 5 S 5 S 5 Sa(Seyfeit?) 3 dE3 4 E 4 ImlV? 5 S(nb) 5 S(onedge) 5 S 5 5 S 5 S(onedge) 5 E 3 dE3? E(M32?) E(in cluster) S ordE3JV E S (onedge) E S0 S S S Type (5) 18.1 4.40.513 17.3 2.70.522 18.3 4.80.541 17.6 2.00.482 18.2 4.90.591 16.3 8.10.934 18.4 4.30.543 19.9 5.50.501 18.0 5.00.573 15.9 17.8 4.10.573 18.7 3.10.461 17.9 3.80.531 17.2 3.20.612 18.2 3.60.491 16.6 0.855 16.6 4.10.724 18.1 4.50.591 17.8 6.50.653 18.1 3.60.493 18.1 15.8 17.9 18.1 18.2 4.00.523 18.5 4.30.501 18.4 18.5 3.90.511 17.8 16.9 2.60.643 17.2 4.90.672 19.1 7.60.543 18.0 4.60.641 18.3 4.60.541 17.4 4.70.673 Br rDS 17.2 2.10.472 18.3 4.60.523 15.8 9.70.953 16.0 3.10.744 (6) (7)(8)(9) 18.8 17.6 4.40.653 18.6 4.70.483 18.1 18.3 5.30.553 18.6 3.90.463 18.4 3.60.501 19.0 3.80.463 17.3 7.10.731 18.9 4.10.471 17.2 3.50.632 18.5 4.40.521 17.1 3.20.602 18.4 4.20.523 14.7 4.70.803 16.3 2.40.583 18.5 3.80.471 18.1 3.90.491 18.8 3.80.511 17.3 2.30.512 18.2 3.50.481 17.8 3.80.591 17.5 3.50.582 16.7 4.00.704 17.1 2.30.504 e 4.2 0.52 4.4 0.58 2.9 0.65 5.9 0.87 3.5 0.49 5.0 0.701 3.5 0.521 4.1 0.471 5.6 0.511 Table III.(continued) B0847 33117.1-3514254E(M32?) B0850 33118.1-3258355S0 B0849 33118.1-380510ring B0848 33117.5-3347215 B0846 33116.3-3157395S0 B0851 B0860 B0859 B0855 B0854 B0853 B0852 B0865 33133.2-3151564? B0864 33132.7-3525574E B0863 3313Z1-3521105S B0862 33126.4-3525415S B0861 33125.6-3348374S0 B0858 B0857 B0856 B0867 33136.8-355218 B0866 33135.0-352733 B0872 B0870 33139.3-380054 B0869 33138.8-325448 B0871 B0868* 33138.5-371806 B0873 B0877 B0875 B0874 B0880 B0879 B0878 B0876 B0882 33149.7-3429394E(M32?) B0884 33150.0-3250024E B0883 33150.0-38485S B0881 33149.6-3249214E B0885 33150.9-3402085S B0889 B0888 B0887 B0886 B0899 B0890 B0904 B0903 B0902 B0901 B0900 B0898 B0897* B0896 B0895 B0891 B0905 B0894 B0893 B0892 B0906 B0908 B0907 B0909 B0910 (1) # RA(1950) Dec(1950)M 3 3118.4-325742 3 3125.2-324821 3 3124.2-355029 3 3123.6-353037 3 3123.5-353028 3 3123.3-335704 3 312Z7-324652 3 3119.1-375926 3 3120.0-364400 3 3119.9-325732 3 3141.3-324910 3 3140.1-351959 3 3142.9-325729 3 3141.6-331050 3 3141.5-325952 3 3145.9-344859 3 3143.0-382648 3 3149.4-331241 3 3146.7-343006 3 3148.9-334945 3 3151.8-353555 3 3158.9-353510 3 3158.8-325520 3 3158.0-322030 3 3157.1-321036 3 3154.3-325114 3 3154.0-320235 3 3152.5-315155 3 3151.9-320205 3 3159.3-344338 3 3159.1-324456 3 3158.9-360139 3 3157.0-324932 3 3156.0-324320 3 3154.6-324859 3 3200.4-344638 3 3156.0-383412 3 3155.9-335245 3 3155.4-325827 3 3154.7-320527 3 3201.5-335308 3 3203.3-353943 3 3203.7-340519 3 3203.3-340403 3 3204.7-330454 (2) (3)(4) 4 S 3 dE? 5 S(onedge) 4 E(M32?) 5 E 5 Sa(s) 4 E(M32?) 5 E 5 E 5 4 E E E(M32?) E? S S S ordS S S S S S S dE2? orE s S (interacting)? orBCD so s ? E(M32?) S0 S? E S(interacting)? ■dE Type (5) 16.9 6.50.844 18.0 3.80.541 18.5 3.30.481 17.0 6.40.723 18.7 3.60.471 17.7 4.60.621 18.2 3.40.481 17.1 4.80.762 19.0 4.30.481 18.4 3.90.563 16.3 18.2 17.8 5.00.671 18.4 4.40.561 18.6 17.6 160.493 17.6 4.50.582 18.0 4.90.613 17.2 17.3 17.6 18.4 18.3 18.3 15.4 18.7 16.9 17.0 18.7 18.2 18.0 18.0 17.8 4.50.601 18.3 17.9 18.9 (6) (7)(8)(9) 17.8 4.90.581 16.1 0.885 17.2 3.10.622 18.3 3.80.533 17.8 17.9 3.90.563 18.4 4.10.483 18.2 18.3 18.8 18.5 17.3 16.1 0.925 18.2 3.00.471 18.3 3.40.481 17.3 170.533 17.4 19.5 15.4 18.1 17.2 5.00.694 18.3 3.30.461 16.7 4.90.713 17.0 8.70.843 17.8 17.6 16.9 18.4 18.8 14.4 0.72 10.7 1.08 4.8 0.85 4.1 0.63 4.8 0.57 5.4 0.70 4.2 0.53 3.4 0.65 3.5 0.50 3.3 0.51 8.4 1.01 3.6 0.69 4.7 0.561 4.8 0.681 3.1 0.49 16 0.64 3.7 0.46 3.5 0.50 5.5 0.641 3.7 0.491 4.5 0.671 4.5 0.511 3.8 0.531 3.4 0.471 3.7 0.541 6.1 0.65 16 0.55 3.7 0.48 3.8 0.46 4.2 0.46 5.9 0.64 6.5 0.75 17 0.61 3.4 0.54 0.57 5 D S 386 1989AJ 98. .367F 387 HENRYC.FERGUSON:THEFORNAXCLUSTER B0916 33208.8-3404264E(HighSB) B0912 B0921 B0919 33209.9-3348415S B0917 33209.6-3347175S0 B0915 B0914 B0913 B0911 B0924 B0922 B0920 33210.4-3729365S B0918 33209.7-3241074E B0923 B0929 33217.1-345942 B0928* 33213.0-354148 B0927 33212.2-320133 B0926 33212.2-341544 B0925 B0930 33218.0-370729 B0934 B0931 B0939 33226.6-3555025S B0938 33226.0-3314224S B0937 33224.2-3709405S B0936* 33222.5-3529515S B0935 B0933* B0932 B0942* 33231.0-3600235S0 B0941 33229.9-3558334E(M32?) B0940 33228.0-3350365E B0944* 33234.0-325955dE,N B0943 33232.4-3659035S B0945 33234.5-3227095E B0947 33235.4-3303194E(M32?) B0946 33234.8-3703195E B0954 33246.9-37265S(interacting)? B0951 33242.4-354327E(M32?) B0949 33236.7-33014E B0948* 33236.4-3513485S B0962 33251.8-3631434E(M32?) B0961 33251.0-3816545S B0958 B0956 B0953 33244.2-3642315E B0950 33238.1-3702135S B0964 33254.7-3414065S B0963 33252.6-354323E(M32?) B0960 B0959 B0957 B0955 33246.9-3800175E? B0952 33243.3-3400485 B0968 B0966 B0965 33254.8-3537025S B0967 B0969 B0973 B0972 B0971 B0970 B0975 B0974 © American Astronomical Society • Provided by the NASA Astrophysics Data System O) # RA(1950) Dec(1950)M 3 3206.6-374640 3 3205.6-3544 3 3208.5-350727 3 3208.3-342223 3 3205.0-382718 3 3210.8-350636 3 3210.6-344217 3 3211.2-330542 3 3211.1-321133 3 3211.9-334908 3 3219.4-375844 3 3219.8-3421 3 3222.3-325149 3 3222.1-333534 3 3220.4-372731 3 3248.9-361853 3 3246.9-365455 3 3250.6-332314 3 3249.1-330222 3 3248.0-383706 3 3255.4-373849 3 3256.2-361155 3 3256.1-331724 3 3258.8-375727 3 3301.3-332559 3 3300.1-323615 3 3303.0-385118 3 3302.2-334606 3 3302.0-382824 3 3304.0-344201 (2) (3)(4) 4 S0 4 S 5 E 5 S 5 4 SB0(M32?) 5 S 4 5 5 E 4 E(M32?) 3 S?orImV 3 S? 5 E 5 S 5 E 5 S(onedge) 5 S 5 S 5 Sa 4 E 5 S 5 S 5 S(onedge) 3 (interacting)orBCD? 4 E(incluster) 5 S 4 S 5 S(onedge) 5 E 5 S 5 E 5 S 5 S 3 dE5pecorE(cD) Type (5) 18.2 3.60.541 18.2 3.30.471 17.4 3.00.524 17.6 3.60.572 16.3 4.80.884 17.8 3.50.491 18.5 3.70.511 17.5 18.2 3.40.531 16.9 3.80.674 17.1 2.40.523 18.3 3.90.461 18.5 5.00.541 16.4 5.80.872 16.8 2.40.642 18.3 3.10.471 16.7 5.90.804 16.8 2.20.513 18.8 5.60.511 18.1 4.80.553 18.5 3.10.461 18.5 3.30.521 18.2 4.90.561 16.1 5.10.843 17.9 3.90.592 17.9 3.50.512 17.1 3.00.564 18.0 6.80.691 18.0 18.0 4.40.571 17.5 4.20.562 Bj rDS 18.0 16.8 15.5 16.7 18.2 (6) (7)(8)(9) 17.7 17.2 17.1 17.9 18.2 18.5 17.3 15.9 17.1 4.60.742 16.7 3.90.783 17.4 0.695 16.5 17.9 18.3 17.4 18.8 18.2 18.3 3.70.461 18.5 3.50.491 17.7 4.30.581 18.4 3.50.461 17.9 4.00.513 18.2 4.10.511 18.4 3.40.471 18.4 4.00.541 17.7 18.6 3.30.471 17.7 9.80.793 16.6 e 7.4 1.00 3.6 0.51 2.7 0.62 4.9 0.683 5.7 0.853 3.5 0.57 8.7 0.69 4.2 0.551 5.9 0.571 6.2 0.70 5.2 0.732 5.2 0.642 3.7 0.662 5.7 0.85 3.4 0.46 3.6 0.481 3.4 0.773 3.8 0.54 3.3 0.461 Table III.(continued) 0.80 5 0.64 0.80 5 0.64 5 B0984 33308.7-3226065S B0981 33308.0-334803EordSO B0980 33307.2-34415S B0978 33306.5-3642135S B0977 33306.0-3722274E B0976* 33304.4-3514304S B0989 33312.7-315622 B0986 33311.0-360122 B0985 33309.1-3442375 B0983 33308.5-3353235S B0982 33308.4-3643465E B0979 33306.8-3624315S B0991 B0990* 33313.0-333216 B0988 33312.0-361200 B0987 33311.7-334406 B0994 B0992 B0996 33314.9-3335015E B0995 B0993 B0997 33316.0-3757455Epec B1000 33317.2-3750295E B0999 33317.0-3614545S B0998 33316.4-3555224E(M32?) B1004 B1002 B1001 B1003 B1007* 33322.1-3453 B1006 33321.1-3438 B1005* 33321.0-324558 B1010 33323.4-333840 B1009 33323.2-362457 B1008 33323.1-365160 B1011 B1023* B1020 B1019 B1018 B1017 B1016 B1015 B1014 B1013 B1012 B1028 B1027 B1026 B1025 B1024 B1022 B1021 B1031 B1030 B1029 B1034 B1033 B1032 B1036 B1035 B1039 B1038* B1040 B1037 (1) # RA(1950) Dec(1950)M 3 3314.1-380442 3 3313.7-364021 3 3313.4-334904 3 3313.7-323516 3 3314.2-323223 3 3318.8-333453 3 3319.8-332301 3 3320.6-331631 3 3320.2-372531 3 3324.5-335745 3 3335.4-353217 3 3325.3-360920 3 3325.0-385006 3 3342.5-3317 3 3340.2-362843 3 3339.4-380610 3 3337.3-350450 3 3337.2-343918 3 3335.1-364540 3 3332.6-332558 3 3331.1-332345 3 3330.6-332950 3 3330.4-365512 3 3330.0-363925 3 3329.4-352559 3 3329.0-353859 3 3325.4-363229 3 3346.1-360942 3 3345.2-362737 3 3346.2-345107 3 3348.7-330830 3 3348.2-325949 3 3347.0-3555 3 3354.9-351708 3 3351.7-370318 3 3351.5-344129 3 3355.8-334257 3 3353.3-324845 3 3355.9-344247 (2) (3)(4) 4 E(M32?) 4 S0? 5 5 S 5 S 5 S 5 (interacting) 5 S 5 S 3 SorBCD? 4 E(cD)? 4 E(M32?) 5 S 5 S 5 E(interacting) 5 S 5 S 3 dE? 5 SorE 4 SordES^N 4 E(M32?) 5 S 5 E 4 S? 4 E(M32?) 5 5 S 5 S(HighSB) 4 E 5 S 5 (interacting) 5 Sbc(s)I-II 3 dSOorS 4 E(M32?) 5 S 5 S 5 S 5 SabI 4 E(incluster)orE(M32?)16.710.80.94 5 S 5 E(nb) 5 E 5 S 5 E 5 S 5 18.43.50.49 5 E 3 ? 5 ? Type (5) 18.9 4.40.561 18.3 5.30.553 18.5 3.80.503 18.8 3.50.463 16.6 3.50.723 17.9 4.90.611 17.3 7.60.782 18.4 6.20.651 17.0 6.70.812 17.9 4.40.551 18.5 3.00.481 18.2 3.40.492 17.2 0.655 17.8 3.40.462 17.0 5.20.703 18.2 3.50.483 17.9 3.90.503 15.6 7.00.932 19.1 3.80.521 16.5 3.20.702 18.1 3.70.532 18.5 4.30.531 17.7 3.90.513 17.5 6.80.791 17.9 18.2 4.20.551 19.1 Bj rDS 13.7 17.5 18.3 17.6 (6) (7)(8)(9) 18.1 17.2 17.3 18.1 17.5 0.625 18.7 4.10.541 18.2 4.80.601 16.9 2.20.483 17.3 2.80.584 17.0 7.20.732 18.0 3.90.521 18.6 4.00.513 17.2 2.60.553 18.0 4.10.611 17.0 3.60.682 19.6 6.30.561 18.2 3.60.541 17.9 4.10.611 18.2 3.60.503 17.3 2.60.534 16.3 4.30.863 18.5 4.70.543 15.9 4.40.813 18.3 3.50.511 18.8 5.30.55 17.6 6.00.74 18.7 3.40.50 e 18.4 19.4 18.3 18.0 17.8 22.0 1.32 4.0 0.45 5.5 0.64 8.8 0.59 5.3 0.73 5.7 0.75 3.6 0.49 5.3 0.65 3.8 0.55 3.8 0.50 4.0 0.53 4.6 0.52 5.1 0.47 3.6 0.48 3.4 0.48 387 1989AJ 98. .367F 388 HENRYC.FERGUSON:THEFORNAXCLUSTER B1104* 33447.9-3405 B1101 33446.4-351229 B1105 33450.6-345902 B1103 33446.7-345519 B1102* 33446.5-353319 B1100* 33445.7-350912 B1099 B1098 B1097 B1096 B1095* 33442.8-3504 B1094 B1093 B1092 B1089 B1088 B1087 B1091 B1090 B1086* 33434.2-345212 B1085 B1084 B1083 B1082 B1081 B1074 B1066 B1065 B1064 B1061 B1080 B1079 B1078 B1077 B1076 B1075* 33428.4-352154 B1073 B1072 B1071 B1070 B1069 B1068 B1067 B1063 B1062 B1060 B1059 B1058 B1057 B1056 B1055 B1054 B1053 B1052 B1051 B1050 B1049 B1048 B1047 B1046 B1045 B1044 B1043 B1042 B1041 © American Astronomical Society • Provided by the NASA Astrophysics Data System 0) (2)(3)(4) # RA(1950)Dec(1950)M 3 3445.7-375540 3 3445.4-330319 3 3444.9-344226 3 3443.3-321337 3 3441.5-343241 3 3440.9-351058 3 3437.2-330914 3 3437.0-340806 3 3436.1-380711 3 3435.8-321330 3 3434.9-332619 3 3434.8-372529 3 3432.8-333711 3 3432.5-335347 3 3431.9-370316 3 3431.3-341352 3 3418.5-321041 3 3417.5-374543 3 3413.1-345616 3 3412.4-335731 3 3428.2-340046 3 3427.3-341013 3 3426.2-3302 3 3423.9-3358084E 3 3421.8-3230484EordE,N 3 3418.7-3728525S 3 3411.2-324002 3 3431.0-382006 3 3426.2-341833 3 3423.5-3701295S 3 3422.1-3154304S 3 3410.8-322919 3 3431.0-315900 3 3430.1-372027 3 3429.8-340500 3 3429.2-335838 3 3410.4-340914 3 3410.1-315010 3 3409.7-341033 3 3430.5-340814 3 3408.9-333349 3 3408.7-355625 3 3408.1-335022 3 3407.0-330849 3 3406.8-362749 3 3405.7-322529 3 3403.8-322858 3 3402.3-330754 3 3402.2-315631 3 3400.5-344741 3 3400.4-342124 3 3358.5-375453 3 3358.6-324700 3 3357.0-381718 3 3356.2-330754 3 3356.0-330126 4 S 4 EorS0 4 S 4 SorSmIV 5 S0 5 S 4 S 5 Sc(r)I 5 E(incluster) 5 E 5 (interacting) 5 S 4 E(M32?) 4 SOordSO 4 S 3 E(M32?) 5 E 5 Sc(r)I 5 S 5 SBc(s)I 5 Sc(r)I 5 Sa 4 E 5 E 5 E 5 S 5 S 5 S? 5 S0 4 E 5 E 4 E 5 E 5 5 5 E 5 5 E 5 S(onedge) 3 SorBCD 5 pair 3 ? 5 S0(incluster)? 5 E 4 ? 4 S 5 E 4 S? 5 E 5 E SB0? S Sa ordS0„ E E(in cluster) E(M32?) dE3 S? Type (5) 15.6 9.50.98 19.0 4.30.48 18.1 5.80.661 16.7 18.1 3.70.501 17.7 3.20.52 17.8 3.60.54 15.4 3.40.682 18.4 7.30.611 18.3 4.00.521 18.2 3.90.513 15.9 18.0 18.7 17.4 15.9 18.2 18.6 16.6 19.0 16.4 4.50.74 17.2 3.10.61 17.1 5.70.76 17.7 4.90.65 16.6 18.1 4.20.471 17.1 4.10.632 18.2 5.40.573 18.2 18.5 4.50.461 17.5 6.80.753 18.1 18.5 18.1 18.9 4.40.54 19.3 18.8 18.1 18.4 15.0 18.3 17.3 18.5 18.9 18.7 17.6 3.50.612 18.2 3.60.461 18.5 3.90.541 18.4 4.80.581 16.1 2.50.602 18.6 18.4 18.9 18.7 17.9 17.0 17.7 19.3 19.2 4.50.481 16.3 18.0 18.6 3.40.461 18.0 0.635 19.1 6.50.511 18.4 3.60.511 Bj rDS (6) (7)(8)(9) e 9.7 0.83 5.1 0.62 2.6 0.61 3.4 0.49 2.9 0.46 6.2 0.92 4.5 0.47 3.9 0.53 3.9 0.47 3.1 0.66 5.2 0.51 4.2 0.541 4.1 0.501 4.3 0.58 4.0 0.48 4.4 0.50 2.3 0.46 3.3 0.531 5.0 0.97 3.8 0.46 4.0 0.56 3.4 0.521 3.7 0.51 3.2 0.47 3.8 0.47 4.1 0.47 4.6 0.47 3.8 0.47 3.1 0.47 2.9 0.48 5.2 0.60 2.4 0.62 3.3 0.51 1.9 0.53 Table III.(continued) 0.79 5 B1168 33538.9-364221dE5 B1167 33538.0-3802095 B1166* 33536.2-3616445 B1165* 33536.1-345233 B1164 33536.1-365654 B1163 33535.1-321109 B1160 B1170 33539.4-3604305 B1169* 33539.0-3449335E(incluster) B1162 33534.0-323056 B1161 33533.3-320356 B1159 B1158 B1156 B1157 B1155 B1154 B1152 B1153 B1151 B1150 B1142 33520.4-3327364E B1149 B1148 B1147 B1146 B1145 33522.1-3739175S B1144 33521.7-3325035S B1143* 33521.7-3519094S? B1141 33519.7-3236465E(incluster) B1140 B1139 B1138 B1137 B1136 B1130 33513.1-340926 B1129* 33512.7-320941 B1128 33511.8-323057 B1127 33511.4-344627 B1126 33511.0-323203 B1125 33510.0-3237475E B1124 33508.8-3427425S(onedge) B1135 B1134 B1133 B1132 B1131 B1123 33507.7-325818dEOJí B1122 33507.5-32154E B1121 33503.9-3150264S(onedge) B1120* 33503.7-375920 B1119 33502.4-3442 B1118 33502.3-351610 B1116 33458.9-354536 B1117 33500.4-345918 B1115 B1114 B1113 B1112 Bllll B1110 33455.3-3343015S B1109 33454.5-3309044E(M32?) B1107 33451.5-3332314E(M32?) B1106 33451.0-3442145Sc(r)I-II B1108 33451.7-333724dSOorS0 (1) # RA(1950) Dec(1950)M 3 3533.0-341651 3 3532.7-333719 3 3532.7-3244 3 3531.1-374451 3 3531.1-370722 3 3530.2-331228 3 3529.2-380824 3 3528.5-315944 3 3527.5-380914 3 3519.5-323902 3 3518.8-315601 3 3516.7-372443 3 3526.7-375116 3 3518.4-330124 3 3516.5-321101 3 3513.4-323815 3 3526.3-331117 3 3526.0-323627 3 3525.5-345131 3 3524.0-331216 3 3523.0-323415 3 3516.4-321406 3 3515.4-365952 3 3515.3-321332 3 3514.1-335239 3 3458.4-3317 3 3458.1-320360 3 3457.0-383148 3 3456.5-340755 3 3456.4-351219 (2) (3)(4) 4 S? 4 E(M32?) 5 E 5 S(onedge) 3 dS0,NorS 5 S(onedge) 4 EordE 4 E 5 S 4 E 4 E(M32?) 4 ? 4 E(incluster) 4 E(M32?) 5 E 5 S 5 E 5 SBc(s)I 4 S 4 E(incluster) 4 S 5 E 5 S(incluster) 5 S 5 E 5 E 5 S 5 S 5 S 5 (interacting) 5 5 S 3 ImV? 5 S 5 S 4 S 5 S(onedge) 5 E(incluster) 5 S 5 S Type (5) 18.1 3.60.491 16.6 9.70.914 19.3 6.50.493 18.1 4.80.581 16.5 18.7 4.30.511 17.7 5.50.603 16.8 3.50.643 17.2 18.2 3.60.491 18.0 17.4 15.5 17.8 16.8 6.40.832 18.3 4.10.521 17.6 6.40.743 18.2 3.60.513 17.0 10.70.872 18.0 18.2 18.5 17.8 18.3 18.3 17.3 18.8 18.7 18.1 18.7 16.5 17.2 18.4 18.2 16.4 17.9 17.4 16.6 16.4 18.0 17.9 17.2 17.5 18.3 16.6 16.8 18.2 17.0 18.3 14.5 18.9 18.5 18.5 18.8 16.7 18.2 18.5 17.4 17.8 18.8 17.0 2.40.523 17.4 6.10.712 16.6 7.80.864 17.4 4.10.592 16.0 3.70.724 B rDS (6) (7)(8)(9) Te 4.3 0.54 4.8 0.63 4.1 0.672 4.3 0.541 4.0 0.48 4.8 0.501 4.0 0.57 4.3 0.51 2.9 0.57 2.3 0.51 4.6 0.57 5.0 0.691 4.7 0.593 4.5 0.513 4.4 0.49 4.2 0.78 3.2 0.59 2.3 0.47 5.1 0.942 3.7 0.632 5.8 0.68 4.1 0.533 4.2 0.611 5.7 0.733 2.6 0.562 3.4 0.491 3.1 0.461 2.9 0.462 3.5 0.542 5.8 0.782 9.4 0.852 5.7 0.561 3.6 0.491 5.0 0.493 2.7 0.66 3.8 0.53 5.0 0.742 3.2 0.482 3.7 0.541 2.1 0.533 3.8 0.491 3.9 0.501 6.3 0.821 3.8 0.461 5.0 0.633 3.6 0.473 0.72 5 388 1989AJ 98. .367F 389 HENRYC.FERGUSON:THEFORNAXCLUSTER B1180* 33548.8-350424 B1178* 33547.3-352854 B1181 33549.6-361934 B1179 33548.6-335503 B1177 33547.1-315626 B1176 33546.4-323742 B1175 B1174 B1173 B1172 B1171 B1184 33550.8-341121 B1183* 33550.8-352750 B1182 33549.6-315842 BU 8933553.6-323736 B1187 33552.8-320519 B1186 33551.8-332138 B1185* 33550.9-344754 B1191 33554.3-353651 B1190 33554.1-381011 B1188* 33552.9-361832 B1195* 33556.6-355717 B1194 33556.2-330317 B1193 33554.4-343858 B1192 33554.3-334626 B1199 B1196 B1200 B1198 B1202 336028 B1201 336028 B1197 B1205 33604.5 B1204 33604.0 B1203 336029 B1206 33605.2 B1221 B1211 33607.2 B1210 33607.0 B1209 33606.6 B1208 33606.4 B1207 33606.4 B1223 B1222 B1217 33610.1 B1216 33609.9 B1215 33609.5 B1214 33609.3 B1213 33609.2 B1212* 33607.8 B1225 B1224 B1220 33611.5 B1219 33610.6 B1218 33610.5 B1226 33614.6 B1228 33615.2 B1227 33614.8 B1230 33615.3 B1229* 33615.3 B1234 33616.7-334823 B1233 33616.3-323746 B1232 33615.8-330959 B1231 33615.5-354626 B1235 33617.3-334521 © American Astronomical Society • Provided by the NASA Astrophysics Data System (1) (2)(3)(4) # RA(1950)Dec(1950)M 3 3544.8-380659 3 3541.2-380312 3 3539.6-323322 3 3539.6-362808 3 3544.9-3238 3 3601.2-333951 3 3601.6-365333 3 3601.1-333802 3 3558.6-381108 3 3558.6-334837 3 3612.2 3 3614.2 3 3612.9 3 3612.9 3 3614.2 33 4357 32 1704 37 5853 33 1454 38 0103 33 4311 33 5112 32 3512 37 5316 33 2235 31 5158 32 3522 32 3510 36 0939 36 0827 33 3631 33 2659 33 2318 33 1450 33 2312 32 5937 33 5024 36 2904 33 0137 32 1457 35 3847 34 5359 37 1604 37 4033 33 0120 4 S 4 S 4 E 4 E? 5 S 5 S 5 S 5 E 5 S 5 S(onedge) 5 S 5 E 5 Sc(s) 5 S 3 dE? 4 E 5 Sc(s)II 4 E(M32?) 5 S 5 E 5 S 3 SorBCD? 5 E 5 E 5 5 S(onedge) 5 E 5 Sb(r)I 3 E 5 Sa(r) 5 S 3 E(M32?) 5 5 S 3 dE? 3 dE2 5 E(incluster) 5 S(onedge) 5 S0 5 4 S? 4 ? 5 S 4 SordESN 4 5 E 5 S(onedge) 5 E? 5 S0(7) 5 E 4 E(M32?) 5 5 S 5 S 5 S E? S (interacting)? S (incluster) S E S S orImV Spec S Type (5) 16.7 18.3 18.6 16.6 17.6 17.4 17.3 19.4 16.2 18.9 18.5 18.2 4.50.551 18.9 17.1 7.80.753 18.3 18.2 18.3 4.40.511 16.7 4.70.782 16.6 6.50.893 18.4 3.40.471 18.2 17.7 18.2 18.9 19.2 17.5 17.3 17.2 16.5 17.3 16.3 6.80.854 18.2 3.40.491 18.3 4.10.521 19.4 7.20.471 18.3 9.90.663 18.6 3.20.461 Bj rDS 18.5 3.40.471 16.8 6.40.722 18.0 3.80.531 18.9 5.00.551 18.6 17.7 18.4 17.1 18.7 18.5 3.80.531 16.5 5.70.722 18.1 4.60.611 (6) (7)(8)(9) 17.1 2.80.583 17.4 5.90.752 17.8 3.30.532 18.0 4.10.531 17.4 2.40.482 17.8 4.80.622 17.7 4.40.544 18.6 5.50.553 18.2 3.50.483 18.3 6.30.643 18.3 4.40.471 18.2 3.30.481 17.5 17.9 16.5 2.20.594 18.0 4.60.621 18.3 3.50.481 e 4.7 0.684 2.6 0.60 2.4 0.54 4.1 0.521 2.4 0.692 6.7 0.51 3.9 0.51 3.6 0.46 4.2 0.471 5.3 0.623 3.3 0.612 3.6 0.501 4.6 0.601 3.6 0.461 4.9 0.531 2.2 0.502 5.6 0.682 3.9 0.543 3.7 0.481 3.2 0.504 5.7 0.753 5.1 0.613 3.8 0.531 8.0 0.834 4.9 0.72 4.6 0.49 6.8 0.59 3.4 0.45 3.0 0.61 5.7 0.652 3.9 0.533 Table III.(continued) B1237 B1236 B1248 33627.0-3300034E B1246* 33625.4-3455165Sc B1245 B1244 B1243 B1242 B1241* B1240 B1239 B1238 B1250 33628.3-3314504SordSO B1249 33627.3-3345435E(incluster) B1247 33626.8-3317564E B1256 B1260 B1258 33632.8-3430555E B1257 B1254 33630.9-3328225E B1253 33630.5-3314515S B1252 33629.7-3344325S B1251 33628.5-3323115E B1261 33633.5-3154144E? B1259 B1255 33631.2-3442115S B1263* 33636.0-3523585(interacting) B1262 33635.4-3203455E B1265 3637.9-3212415 B1264 33636.9-3803255E B1267 33638.5-3203265S B1266 33638.3-3251535 B1270 33640.0-3728545S B1269 33639.9-3614344 B1268 33638.8-3646325S B1271 33640.6-330415 B1273 33642.3-361353 B1272 33641.0-375726 B1286* B1279 33646.4-3257324E(imeracting)ormlV17.07.90.892 B1276 33645.4-3248564E(M32?) B1275 33645.1-322637 B1274* 33643.6-360732 B1288 B1287 B1285 33649.6-3702425S B1284 33649.2-3251435E(cD) B1283 33648.3-3740505S(onedge) B1282 33648.0-3345425RSa B1281 33647.5-354248filament? B1280 33646.4-3623135E B1278 33646.1-3430145S B1277 33646.0-324008S?ordEpecN B1291 B1290 B1289 B1293 B1292 B1295 B1294 B1299 B1297 B1296 B1298 B1300 (1) (2)(3)(4) # RA(1950)Dec(1950)M 3 3618.8-3540 3 3621.6-354007 3 3619.8-331655 3 3619.2-350035 3 3618.9-341634 3 3617.5-374037 3 3624.9-322101 3 3622.5-374415 3 3622.4-332457 3 3624.6-374313 3 3631.8-332606 3 3633.4-332335 3 3632.9-331104 3 3632.1-344728480^9) 3 3649.6-345723 3 3651.3-361912 3 3651.1-343758 3 3650.1-321552 3 3653.6-350560 3 3652.9-344920 3 3652.7-362230 3 3654.2-344424 3 3653.0-365908 3 3654.6-320428 3 3700.9-373946 3 3659.8-321250 3 3659.1-3412 3 3657.7-37231 3 3701.3-335653 4 5 E 4 E(M32?) 5 S 5 S(interacting)? 5 E 5 S 4 S? 5 E 5 pec 5 S 3 dE? Im E ordE,N dE3pec? E S (HighSB) S S? (interacting) Sc(s)II (interacting)? S E Sc(rs)I E ? SO? ordSO E(M32?) E ordE(M32?) S S pec orBCD Type (5) 18.5 5.20.561 18.7 4.60.473 17.3 8.30.793 16.7 9.10.902 16.0 3.60.622 16.0 2.90.594 18.0 18.8 18.0 3.90.551 17.8 4.00.642 18.3 3.30.501 17.9 3.40.483 15.0 4.00.832 18.0 4.80.611 18.4 4.50.511 18.2 17.9 18.0 6.10.651 19.0 18.6 18.0 18.1 3.40.471 16.7 7.60.873 18.1 4.30.521 18.7 3.40.471 18.5 5.00.561 17.2 4.60.681 18.0 3.90.482 18.5 5.30.491 18.2 4.00.491 17.8 3.90.521 15.9 3.20.662 B rDS 17.7 0.635 18.6 3.30.491 17.6 2.90.592 16.8 2.50.603 18.2 5.20.591 17.4 5.30.742 18.0 5.50.583 19.5 6.10.493 18.8 5.00.481 17.2 5.50.673 17.7 5.60.662 18.3 3.30.461 17.7 4.50.594 (6) (7)(8)(9) 17.5 2.40.512 17.9 4.20.531 18.2 4.70.583 17.6 5.00.633 16.8 8.70.853 18.6 3.90.521 17.7 4.70.651 17.8 5.10.591 18.6 3.90.471 18.8 6.50.491 17.8 7.70.673 19.3 3.80.461 18.6 18.4 17.0 3.60.684 18.2 3.50.491 17.3 3.10.633 18.2 4.20.491 17.9 4.00.582 Te 4.0 0.463 3.8 0.531 5.6 0.651 3.8 0.503 3.8 0.451 3.8 0.541 3.8 0.491 5.1 0.511 3.3 0.491 389 1989AJ 98. .367F 390 HENRYC.FERGUSON:THEFORNAXCLUSTER B1304 B1303 B1302 B1306 B1305 B1301 B1319 33716.0-341645 B1318 33714.7-335255 B1317* 33714.1-334129 B1316* 33713.8-360153 B1309 B1308 B1325 B1324 B1322 B1321 B1320 33719.2-330102 B1315 B1314 B1313 B1312 B1311 B1310 B1307 B1330 B1327 B1326 B1323 B1332 B1329 B1328 B1331 B1335* 33732.0-382148 B1334 B1333 B1337 B1336 B1340 B1343 B1342 B1341 B1339 B1338 © American Astronomical Society • Provided by the NASA Astrophysics Data System B1345 B1344 B1348 B1347 B1346 B1358 B1353 B1350 B1349 B1360 B1357 B1356 B1355 B1354 B1352 B1351 B1365 B1364 B1363 B1362 B1361 B1359 (1) (2)(3)(4) # RA(1950)Dec(1950)M 3 3709.3-355357 3 3705.2-362440 3 3705.0-362450 3 3701.5-320943 3 3711.8-333560 3 3708.0-382806 3 3707.3-321511 3 3713.0-382618 3 3712.0-324327 3 3710.7-333952 3 3710.6-331154 3 3725.8-323101 3 3725.4-331150 3 3719.4-334906 3 3719.4-352524 3 3713.2-331251 3 3712.9-323444 3 3712.7-3251 3 3712.0-323510 3 3726.6-380412 3 3723.6-3414 3 3730.6-350128 3 3729.4-342853 3 3728.7-332654 3 3728.5-350635 3 3727.1-332243 3 3729.9-332302 3 3732.0-335524 3 3731.7-321900 3 3730.6-344530 3 3732.7-325534 3 3732.5-314954 3 3734.7-325453 3 3734.2-372034 3 3734.1-324605 3 3733.4-331618 3 3734.8-324052 3 3735.8-352201 3 3735.7-350106 3 3739.2-324644 3 3738.8-370253 3 3737.5-3549 3 3736.7-323509 3 3740.1-345546 3 3744.8-324731 3 3744.5-340211 3 3744.5-333101 3 3744.3-323523 3 3744.1-332603 3 3744.0-353448 3 3743.7-370022 3 3740.7-325911 3 3745.8-370104 3 3745.4-342643 3 3748.9-353620 3 3748.7-341547 3 3748.2-335327 3 3747.6-345801 3 3749.3-331253 4 S 4 SordEpec,N 4 E 4 E(M32?) 5 S(pair) 5 S(interacting)? 4 5 S 4 SordE,N 5 S 5 S 5 S(onedge) 5 S 5 E 5 S 5 S 5 (interacting) 5 S 5 S 5 pec 3 dEO 5 5 ? 3 dE3,NorS 5 E 4 E(M32?) 5 E(cD)? 3 SordEpecN 4 E 5 E 5 S 5 group 4 E 4 (interacting)? 4 ? 4 SorBCD 5 Sb 4 S0 5 E 5 E 5 E 5 E 5 E 5 S 4 S(HighSB)orBCD 5 (interacting) 4 E 4 E 5 S 5 E 4 SBordSBO 4 E 5 (interacting) 5 S 4 E 5 SBb(rs)I 5 S0 5 S 5 E 3 dS0(8)N 4 Im? 5 E 5 S(onedge) 5 S 5 Type (5) 18.5 17.1 17.6 17.7 17.4 16.4 16.3 18.1 18.7 17.2 18.4 18.3 17.7 17.3 17.9 3.00.482 15.3 11.51.093 16.6 3.20.672 17.4 17.1 18.4 18.2 18.0 17.4 16.7 17.2 17.4 18.8 18.2 19.0 16.9 18.0 18.3 15.9 16.5 18.1 15.7 19.0 18.7 16.8 18.1 18.5 18.6 18.8 18.9 17.9 17.7 Bj rDS 16.9 16.6 18.1 (6) (7)(8)(9) 17.6 16.0 16.8 17.9 16.8 17.9 17.7 18.0 18.6 19.1 18.2 16.8 17.4 18.4 18.5 18.1 e 4.5 0.491 6.5 0.471 4.6 0.61 4.5 0.50 4.3 0.563 6.6 0.793 5.7 0.621 5.8 0.693 5.7 0.862 5.0 0.684 6.0 0.593 4.2 0.48 4.6 0.55 5.6 0.56 5.9 0.74 5.5 0.723 2.6 0.56 3.5 0.50 3.5 0.632 4.2 0.56 7.5 0.66 7.7 0.771 6.0 0.71 3.9 0.72 4.3 0.471 4.4 0.681 3.9 0.48 4.3 0.511 4.8 0.541 4.2 0.523 5.5 0.812 3.8 0.742 2.9 0.632 1.9 0.47 5.2 0.722 7.0 0.83 4.3 0.56 6.3 0.631 6.9 0.651 3.3 0.491 3.2 0.481 4.6 0.58 7.8 0.85 5.2 0.48 4.1 0.471 4.1 0.521 4.7 0.541 4.2 0.621 2.9 0.602 5.7 0.651 5.8 0.683 3.0 0.652 2.6 0.501 3.5 0.501 3.0 0.471 3.4 0.723 3.2 0.622 3.6 0.541 9.4 0.653 Table HI.(continued) 0.73 5 0.72 0.98 5 B1371 33750.6-331141 B1368 B1367 B1366 B1387 B1386 B1384 338022-3602505S B1383 33759.8-370916BCD? B1382 33758.3-3353235(interacting)? B1381 33757.6-3216464SorBCD B1380 33756.8-323423 B1379 33756.8-331243 B1378 33754.5-380015 B1377 33754.4-332246 B1376* 33754.2-362733 B1375 33753.8-372535 B1374* 3375Z8-353318 B1373* 33752.1-362021 B1372 33751.5-322853 B1370 B1369 B1385 33802.3-3409114S B1390 B1389 B1388 B1391 B1392 B1395 B1394 B1393 B1400 338129-354117 B1397 33810.8-315920 B1396* 33810.7-375704 B1405 33814.6-3245365E B1404* 33813.8-3757055Sb(interacting) B1402 33813.6-3430185E B1401 33813.2-3336565S0 B1399 33812.0-362645 B1398 33811.1-343633 B1410 33818.9-3649515S B1409 33817.3-3806305S(onedge) B1408 33816.3-3353145RSa? B1407 33815.0-3615275S B1406 33814.7-371833BCDorE(M32?) B1403 33813.8-364308dE4,N B1413 B1412 B1411 B1420 B1418 B1417 B1416 B1415 B1414 B1429 33835.8-3234235E B1428 33835.4-3236205E B1427 33835.3-3436285(interacting) B1419 B1426 33834.6-3314444E(M32?) B1425 B1424 B1423 B1422 B1421 B1430 33836.1-3759255S O) # RA(1950) Dec(1950)M 3 3750.0-320807 3 3749.3-372606 3 3750.6-3417 3 3750.3-375629 3 3749.8-341542 3 3803.8-3216 3 3803.3-3249 3 3805.4-330626 3 3805.8-380450 3 3804.1-371455 3 3807.5-340355 3 3810.6-324411 3 3810.3-330027 3 3809.6-334418 3 3806.6-321439 3 38221-343017 3 3819.2-341509 3 3819.0-3759 3 3824.5-324231 3 3822.3-381047 3 38326-371055 3 3829.7-320114 3 3828.8-320123 3 3827.3-372349 3 3827.3-374518 3 3826.0-324417 3 3825.9-324544 3 3825.7-380255 3 3824.9-333704 3 3834.3-320057 (2) (3)(4) 4 E 4 S 5 ? 5 E 5 E 4 E? 5 S 5 Sel 5 S 5 E 5 S 5 E 4 E 5 E 5 3 S0ordSO 5 5 E 5 E(nb) 5 5 E(M32?) 4 E 5 E 5 S 5 S 5 E 5 S(interacting) 5 (interacting) 5 S 3 Im?orBCD dE6pec E ordE2N E S Im E(M32?) Sb(interacting) pec SB cl E(in cluster) E(M32?) E(in cluster) E S (onedge) Type (5) 18.8 19.2 18.0 15.8 3.20.672 16.9 5.80.764 17.0 3.10.613 18.1 4.70.573 17.4 18.4 17.9 17.9 3.40.473 17.6 4.20.572 17.7 4.10.541 18.0 4.20.521 16.5 4.30.844 16.5 240.59 18.2 15.6 16.4 18.6 16.8 18.5 16.3 18.5 17.8 2.60.532 18.6 3.70.491 17.9 18.0 3.30.531 18.1 3.20.481 18.4 5.60.581 15.8 6.21.043 18.4 4.20.471 16.9 290.603 18.2 3.80.491 B rDS 16.7 250.523 17.4 4.40.702 17.5 4.70.652 18.1 3.90.521 15.3 20.71.144 18.5 4.30.531 17.7 4.90.653 18.1 4.30.581 18.7 4.20.561 18.0 3.80.541 18.9 7.60.523 18.3 18.4 16.5 (6) (7)(8)(9) 16.9 17.9 17.0 18.5 4.00.551 17.1 8.80.812 16.7 3.50.702 17.0 3.20.603 18.9 16.8 18.7 17.9 18.1 3.20.481 18.4 3.40.471 17.9 6.60.661 18.4 3.80.531 16.6 6.40.742 17.4 2.60.513 te 4.4 0.471 4.8 0.651 4.0 0.473 7.4 0.771 4.3 0.74 4.2 0.51 24 0.47 5.7 0.86 3.5 0.46 3.4 0.502 4.4 0.63 4.2 0.51 21 0.51 3.9 0.51 26 0.62 4.3 0.50 4.0 0.49 4.7 0.68 5.9 0.87 7.8 0.94 5.3 0.73 3.4 0.48 9.3 0.84 5.2 0.47 3.9 0.51 390 1989AJ 98. .367F 391 HENRYC.FERGUSON:THEFORNAXCLUSTER B1432 B1431 B1440 B1438 B1437 B1436 B1435 B1434 B1433 B1442 B1441 B1439 B1444 B1443 B1447 B1446 B1445 B1450 B1448 B1453 B1452 B1451 B1449 B1454 B1457 B1456 B1455 B1459 B1458 B1461 B1460 B1463 B1462 B1465 B1464 B1467 B1466 B1471 B1470 B1469 B1468 © American Astronomical Society • Provided by the NASA Astrophysics Data System B1481 33918.2-3238185S B1475 B1473 B1472 B1483* 33919.8-3319144S? B1479 B1477 B1476 B1474 B1485 33920.5-3219404S? B1482 33919.5-3706134SorBCD B1480 B1478 B1487 33922.7-3754375S B1486 33921.3-3553505E B1484 33920.4-324930dE? B1488 33922.9-3711005S B1490 33924.0-3230095S B1489 33923.1-3426245E B1493 B1491 B1495 B1494 B1492 (1) (2)(3)(4) # RA(1950)Dec(1950)M 3 3839.0-3436285E 3 3837.9-3430375 3 3837.4-3452344 3 3837.1-3415335SO? 3 3836.5-34465(interacting) 3 3839.1-3759125Sc(interacting)? 3 3845.6-322725 3 3845.2-350627 3 3843.3-374505 3 3843.2-342940 3 3843.0-3800 3 384Z6-3310235S 3 3841.9-3425205 3 3840.5-3744395E 3 3839.7-3313234E 3 3845.8-3405185Sc(s)I 3 3850.6-3431274E 3 3846.4-3746205E 3 3846.0-3327245S 3 3855.1-3542514S 3 3854.1-3612395E5 3 3847.0-3240074S 3 3856.9-3434575S 3 3856.6-3222604? 3 3857.9-331929 3 3857.6-321835dSO 3 3860.0-351851 3 3858.8-374849 3 3904.4-335827 3 3902.7-351929 3 3900.2-364931 3 3906.2-323013 3 3905.4-342446 3 3905.2-341540 3 3906.5-3210 3 3907.3-342445 3 3907.1-343002 3 3908.8-380626 3 3908.6-324636 3 3907.5-344311 3 3910.8-332229 3 3909.7-342348 3 3915.2-380151 3 3914.3-332260 3 3913.7-324844 3 3911.4-342855 3 3911.0-342242 3 3909.9-345957 3 3914.3-323227 3 3917.6-332501 3 3927.3-3726 3 3927.0-320634 3 3925.3-371103 3 3924.3-371060 3 3927.1-345328 4 dE? 4 ImV? 5 E 3 dE?,N 5 S 4 E? 4 E(M32?) 5 E 4 E 5 S 5 E 4 E 4 ? 5 S(onedge) 3 dE4? 4 E 4 E 4 E 4 E 4 ? 5 E 5 S 5 S 5 S 5 E 5 E(incluster) 5 S 5 E 5 E 5 S 5 E 5 S 5 E 5 S 5 E Type (5) 17.9 3.40.511 18.0 4.90.571 18.6 3.60.461 18.3 3.40.471 18.2 4.30.571 17.4 2.00.502 16.8 5.90.753 18.1 6.20.681 19.5 6.60.463 18.8 6.10.573 18.6 3.30.461 18.4 3.80.471 18.0 4.80.671 18.9 3.30.481 18.1 0.565 16.0 2.90.684 18.4 3.50.501 19.2 7.10.503 17.7 4.50.611 17.3 3.40.612 18.4 3.40.493 19.1 5.30.501 16.8 2.10.573 17.1 2.60.542 17.4 3.30.562 18.7 4.90.493 18.6 4.90.591 17.8 6.30.661 Bj rDS 18.5 3.40.463 17.6 3.80.6*3 18.6 3.90.513 (6) (7)(8)(9) 19.1 4.90.471 17.3 8.70.832 18.2 4.20.521 18.8 3.50.461 18.6 5.40.571 18.2 3.50.521 18.2 3.40.501 17.1 7.60.842 17.8 4.90.612 18.3 5.10.541 17.7 18.8 18.9 17.4 4.30.702 18.1 3.70.493 17.4 18.0 18.3 6.10.633 17.9 3.30.481 18.6 6.00.591 18.2 4.10.591 16.5 7.80.862 18.1 3.70.531 17.4 1.90.482 18.6 3.10.471 19.0 3.60.461 17.5 5.30.683 18.3 3.80.471 e 18.4 3.50.481 18.3 3.60.511 19.0 3.80.471 18.7 4.30.513 18.7 4.50.501 18.3 4.70.531 4.3 0.47 6.5 0.75 3.7 0.56 3.9 0.54 3.9 0.46 Table III.(continued) B1501 33929.4-3445315E B1503 33931.9-3748575 B1502 33930.1-3710235E B1500 33928.5-3721054S? B1499 33928.3-3206084E B1498 33928.2-3650315S B1497 33927.8-3806335S B1496 33927.7-3738564? B1507 33933.4-3806175S B1506 33933.3-375546dE?,N B1505 33933.2-3801365S B1504 33932.0-3223455S B1509* 33933.7-3552444(interacting)ordEpec18.56.10.61 B1508 33933.7-3202584S B1513 B1511 B1510 33934.7-3753384E B1517 33938.4-3247005? B1516 33938.0-3513505E B1515 B1514 B1512 B1522 B1521 B1520 33939.3-3350255E? B1519 33939.2-3613435S B1518 33938.6-3444025 B1525 B1523 B1526 33943.3-3718265S B1524 B1529 33945.8-353035dE2,N? B1528 33945.7-3810215SBa(r)+E B1527 33944.4-3151425E(interacting) B1530 33945.8-3632295E B1535 33948.9-375828 B1533 33947.4-3408 B1532* 33946.4-341653 B1531 33946.1-364529 B1538 B1536 B1534 33948.0-334258 B1546 B1544 B1540 B1539 B1537 B1548 B1547 B1545 B1543 B1542* B1541 B1550 B1549 B1552 B1551 B1555 B1554 B1553 B1556 B1559 B1558 B1557 B1560 (1) (2)(3)(4) # RA(1950)Dec(1950)M 3 3936.8-371023 3 3935.3-342546 3 3937.3-342648 3 3937.2-320507 3 3936.2-322757 3 3942.5-323551 3 3941.5-362618 3 3941.3-372234 3 3940.4-375602 3 3941.8-3153 3 3950.1-375644 3 3957.4-340306 3 3957.1-372819 3 3955.5-354134 3 3954.9-325234 3 3953.0-342330 3 3951.2-380456 3 3950.9-3503 3 3957.1-371228 3 3956.5-363237 3 3955.5-365818 3 4003.0-381106 3 3959.3-381052 3 3958.8-325434 3 3957.4-321255 3 4004.6-353021 3 4004.3-362523 3 4003.8-371253 3 4003.8-353951 3 4005.2-321228 3 4007.0-335825 3 4005.8-371812 3 4005.6-321302 3 4007.4-3810 3 4007.0-380519 4 ? 4 S?orBCD 5 E 5 S 5 S(onedge) 4 SorSmin 4 S? 5 E 5 S 5 S 4 pec 5 4 ? 5 S 5 Sc(rs)I 5 E 4 S0 4 E(incluster) 4 S 4 E(M32?) 5 (interacting) 5 S 5 S 5 S 5 S 5 E(nb) 4 S 5 S 3 dE4 4 E(M32?) 5 S(tides) 5 5 E 5 S 5 E(incluster) 5 E 5 S? 5 E 5 S(onedge) 3 SorlmlV Type (5) 18.8 3.90.503 17.1 7.20.832 17.4 6.10.701 19.1 4.10.461 18.8 3.70.491 18.7 4.40.571 17.2 3.00.683 17.4 2.90.523 18.9 3.90.461 17.0 8.50.883 17.1 6.80.802 18.5 3.70.461 19.5 4.60.461 18.5 3.80.471 19.1 9.10.571 18.3 4.50.501 17.5 7.00.742 17.8 8.60.763 16.5 2.50.562 17.7 18.5 16.9 4.10.674 18.4 3.80.581 17.2 18.6 18.4 18.2 3.90.511 18.3 4.40.561 18.8 4.30.483 B 16.9 2.30.524 19.5 5.60.513 15.1 4.70.903 18.2 4.60.601 18.6 2.90.471 17.3 5.10.643 17.0 7.90.793 (6) (7)(8)(9) 19.2 3.90.493 18.1 3.60.481 17.8 18.0 3.70.503 16.7 270.612 16.9 7.10.882 18.0 4.00.543 18.5 18.6 18.8 16.7 18.2 18.1 16.2 19.1 15.6 5.30.994 18.2 4.10.503 18.2 18.6 3.50.471 17.8 3.20.482 17.5 6.30.663 18.4 4.30.483 17.2 3.50.672 17.9 4.20.573 17.9 4.00.572 17.7 5.40.672 t 16.6 3.00.753 18.0 3.80.581 4.0 0.49 4.8 0.56 2.5 0.47 3.4 0.48 5.8 0.70 4.2 0.51 4.1 0.58 4.3 0.643 4.4 0.601 4.0 0.521 5.8 0.493 23 0.61 3.3 0.52 22 0.533 3.8 0.47 D S 391 1989AJ 98. .367F 392 HENRYC.FERGUSON:THEFORNAXCLUSTER B1563 34009.4-3624475E B1562* 34009.1-3811235SBb(s)I-II(interacting)14.75.00.97 B1565 34010.1-3422474S(onedge) B1564 34009.4-3222255 B1561 34008.0-3717345E18.73.40.491 B1581 B1580 B1579 B1578 B1577 B1576 B1575 B1574 B1573 B1572 B1571 B1570* 34010.7-365807 B1569 B1568 B1567 B1566 B1585 B1583 B1582 B1584 B1589 34029.1-3215515 B1588 34028.5-3159565E B1587 34027.7-3211034E(nb) B1586 34025.5-3156594S?ordEpec,N B1590 34031.0-3731565S B1593 B1592 B1591 B1596 B1595 B1594 B1597 B1601 B1599 B1598 B1610 B1607 B1604 B1603 B1600 B1616 B1614 B1612 B1611 B1609 B1608 B1606 B1605 B1602 B1618 B1615 B1613 B1625 B1624 B1623 B1622 34059.0-3443355 B1621 34058.6-345714S0 B1620 B1619 B1617 © American Astronomical Society • Provided by the NASA Astrophysics Data System (1) # RA(1950) Dec(1950)M 3 4010.4-322135 3 4016.1-324541 3 4011.1-321341 3 4010.7-353322 3 4010.5-324730 3 4010.3-375559 3 4019.5-325043 3 4019.5-354837 3 4017.7-315310 3 4017.6-361413 3 4013.7-364746 3 4012.5-331531 3 4011.7-344957 3 4011.0-383848 3 4010.8-325626 3 4010.5-321327 3 4024.7-323452 3 4020.7-344118 3 4020.2-321146 3 4035.0-380946 3 4032.6-324944 3 4031.9-370623 3 4031.7-362115 3 4038.5-380109 3 4037.7-332316 3 4034.8-332141 3 4040.6-335548 3 4039.6-332120 3 4038.9-331037 3 4038.7-332425 3 4041.8-353916 3 4041.2-321336 3 4039.7-370015 3 4039.0-320107 3 4050.1-351803 3 4050.0-362531 3 4048.7-335618 3 4047.0-345905 3 4044.6-320352 3 4055.0-351720 3 4053.4-351732 3 4053.1-323912 3 4052.1-363303 3 4050.9-3244 3 4050.2-342742 3 4047.7-332439 3 4042.2-350551 3 4059.1-3215205E 3 4058.0-374756 3 4057.3-342123 3 4100.8-3719605E(interacting) 3 4100.7-3345035 (2) (3)(4) 4 S(LSB) 4 SOordSO 4 E(M32?) 4 S(LSB)? 5 E(incluster) 5 SBb(s)II 5 SBbc(s)I 5 5 E 5 S 5 E 5 S 5 SBbcïï 5 ? 5 S 5 E(incluster) 5 pair 5 Sc 3 dE3? 4 E 5 E? 5 5 E 4 ? 5 group 5 E 5 E? 5 5 S 3 dE3,N? 5 S 5 SO 5 E 5 S 4 SO 5 E 4 S0? 5 S07 4 5 E 5 S 5 E(incluster)? 5 S 5 E 5 E 5 S 5 SBbl-II 5 S Type (5) 17.6 6.00.64 18.1 4.60.651 17.8 2.60.47 18.5 4.50.571 18.6 3.80.48 15.3 3.70.73 18.6 3.20.471 17.5 8.40.822 17.0 0.785 18.7 4.30.481 14.9 4.50.794 18.9 5.50.501 17.3 5.00.732 18.0 4.40.561 18.6 3.70.491 17.7 4.80.583 18.0 4.90.583 17.4 4.90.662 18.1 3.40.521 18.4 4.40.51 18.6 3.40.48 18.1 3.10.46 18.8 3.90.471 17.9 4.70.571 19.0 3.00.461 18.3 2.80.462 16.7 5.10.852 18.1 4.60.553 18.2 3.30.492 18.6 3.40.491 17.4 3.60.582 18.1 19.7 18.5 18.4 18.2 18.8 5.70.511 15.8 5.50.802 17.4 2.30.462 18.7 3.30.481 19.6 4.40.493 18.6 3.30.463 Bj rDS 17.6 2.50.492 18.5 4.00.493 18.0 4.10.511 18.5 3.50.461 18.7 18.7 3.70.481 18.0 5.50.641 18.1 18.2 3.90.561 16.0 6.30.834 18.7 4.70.491 18.3 18.4 3.90.491 17.4 2.50.552 18.5 17.4 4.30.662 16.9 3.00.604 (6) (7)(8)(9) 18.1 3.10.492 17.8 2.50.472 18.3 4.20.501 18.6 3.40.471 e 6.2 0.49 3.5 0.48 3.5 0.47 3.4 0.46 3.7 0.54 3.9 0.471 3.6 0.521 3.6 0.531 3.7 0.471 Table III.(continued) B1628 B1626 B1630 B1629 B1627 B1647 B1646 B1645 B1639 B1635 34108.7-3250575 B1631 3410Z7-3720244S(interacüng)orBCD16.28.70.94 B1644 B1643 B1642 B1641 B1640 B1638 B1636 B1634 34104.2-37255E(nb)pec B1633 34103.2-3716245S B1632* 34103.0-3737515Merger B1650 B1649 B1648 B1637 B1651 B1655 B1654 B1653 B1652 B1657 B1656 B1660 B1658 B1664 B1662 B1661 B1659 B1666 B1665 B1663 B1681 B1669 B1686* 34144.2-3449264SBb(s)I-II B1685 B1684 B1683 B1632 B1680 B1679 B1678 B1677 B1676 B1675 B1674 B1673 B1672 B1671 B1670 B1668 B1667 B1688 34146.7-3442085E B1687 34145.6-3733225E B1689 34146.9-3804125E B1690 34146.9-3214195E (1) # RA(1950) Dec(1950)M 3 4115.7-3803525S? 3 4113.3-3527494E(M32?) 3 4113.1-324735 3 4111.9-343315 3 4111.2-343156 3 4109.9-332653 3 4108.7-361350 3 4102.3-372047 3 4102.1-324508 3 4102.1-371660 3 4101.7-370816 3 4101.3-362716 3 4112.9-321539 3 4110.9-324853 3 4110.4-330600 3 4108.8-373309 3 4117.8-3634265E 3 4116.6-3650085E 3 4116.3-3716594SordSO 3 4108.8-325944 3 4118.9-344251 3 4119.2-334714 3 4119.1-373412 3 4119.0-372013 3 4126.8-372624 3 4119.5-344437 3 4127.8-362739 3 4127.6-345812 3 4127.0-315358 3 4123.2-370531 3 4131.1-372110 3 4128.3-352146 3 4128.0-351020 3 4127.8-323614 3 4141.0-3557205S 3 4139.0-315204 3 4135.8-3434255 3 4132.3-3400524E 3 4132.3-3336224E(interacting) 3 4132.2-334754 3 4142.3-3655255E 3 4141.8-3246455E 3 4140.3-362749 3 4139.8-373348 3 4139.3-322952 3 4138.9-364827 3 4135.8-3639375E 3 4132.5-3350234E(incluster) 3 4143.9-3224034S 3 4142.4-3726244E(M32?) 3 4138.7-325006 3 4138.7-315213 3 4138.6-3727 3 4138.6-373234 3 4136.6-355003 (2) (3)(4) 4 SordSO 4 (interacting) 4 E 4 E(M32?) 5 E 5 S 5 E 5 S 5 S 5 S 5 S 5 E 5 ? 5 S(onedge) 4 S 4 S(onedge) 4 S 4 SorBCD 5 E 4 (interacting)orBCD 5 E 5 RSa 5 E 4 E 4 E(incluster) 5 5 S 5 S(interacting)? 5 S 5 5 S 5 E 5 S? 4 E(M32?) 4 S? 5 S 5 (interacting)? 5 E 5 E(incluster) Type (5) 18.7 4.10.481 18.7 3.20.501 18.3 4.40.571 18.7 5.00.551 17.2 210.471 17.5 5.40.692 18.0 4.20.531 16.9 2.40.534 18.1 4.10.523 18.7 4.70.511 17.8 5.20.642 18.5 17.9 17.2 2.60.522 18.4 3.80.621 17.1 3.40.602 18.1 4.80.553 17.0 2.20.552 17.4 4.40.574 18.1 5.20.591 18.5 4.40.501 16.1 2.80.763 18.7 3.70.501 18.9 4.80.511 17.8 4.60.582 18.6 4.50.533 16.5 250.644 17.2 6.80.784 18.1 3.40.512 19.0 18.0 18.2 4.00.523 13.9 18.2 18.3 17.2 290.65 18.5 16.9 Bt 17.9 5.30.671 18.6 3.80.473 17.6 7.10.682 17.9 19.1 18.0 16.8 18.5 4.60.541 17.4 6.30.733 18.1 3.60.521 18.5 3.80.471 17.4 5.80.702 16.6 5.10.773 17.2 17.9 16.4 17.1 19.0 18.0 3.30.481 18.8 17.4 (6) (7)(8)(9) 18.4 17.2 18.6 17.7 18.1 4.2 0.491 5.2 0.481 4.1 0.501 4.6 0.563 4.5 0.553 6.5 0.832 4.7 0.561 5.9 0.513 4.8 0.591 7.2 0.852 20 0.542 4.8 0.561 3.6 0.541 5.5 0.471 3.7 0.684 4.1 0.561 4.8 0.471 6.4 0.673 28 0.512 24 0.552 3.2 0.461 3.6 0.603 26 0.512 3.3 0.491 1.9 0.592 D S 392 1989AJ 98. .367F 393 HENRYC.FERGUSON:THEFORNAXCLUSTER B1691 B1704 B1702 B1701 B1699* B1698 B1697 B1696 B1695 B1694 B1693 B1692 B1705 B1703 B1700 B1706 B1710 B1709 B1707 B1720 B1718 B1717 B1716 B1715 B1714 B1713 B1712 B1711 B1708 B1721 B1719 B1724 B1723 B1722 B1725 B1727 B1726 B1743 B1742 B1741 B1734 B1733 B1729 B1728 B1745 B1744 B1737 B1735 B1732 B1731 B1730 B1748 B1746 B1740 B1739 B1738 B1736 © American Astronomical Society • Provided by the NASA Astrophysics Data System B1750 B1749 B1747 B1753 B1751 B1755 B1752 B1754 (1) (2)(3)(4) # RA(1950)Dec(1950)M 3 4203.1-3626585S 3 4150.3-373145 3 4148.3-353818 3 4147.8-321050 3 4147.1-324028 3 4202.0-3433555 3 4157.0-3756145E 3 4150.8-340413 3 4204.1-3556014groupordE(+g.cl?),N18.06.60.591 3 4156.1-3243254E 3 4154.6-354650 3 4152.8-325015 3 4151.1-315833 3 4206.3-330644 3 4206.1-325031 3 4205.7-354946 3 4204.6-362139 3 4154.9-374703 3 4154.6-323324 3 4209.1-3149275S 3 4208.2-325051 3 4206.4-354447 3 4206.2-320657 3 4205.7-373041 3 4205.1-321907 3 4204.5-3703 3 4211.0-3551085S 3 4210.4-3336434E 3 4216.4-325258 3 4215.9-375209 3 4215.8-354411 3 4214.0-3516? 3 4211.1-3509355S 3 4217.4-333933 3 4217.3-375250 3 4217.5-365256 3 4220.6-341826 3 4220.4-341355 3 4220.1-371653 3 4231.2-331130 3 4229.6-333633 3 4229.6-3159 3 4226.7-354114 3 4226.3-320658 3 4222.9-352209 3 4221.9-325154 3 4221.5-323718 3 4233.6-332015 3 4232.5-353945 3 4228.4-3613 3 4226.6-375157 3 4224.7-375309 3 4224.3-340033 3 4222.6-320358 3 4221.7-354320 3 4236.6-343422 3 4234.4-343448 3 4234.2-343210 3 4236.8-372034 3 4236.8-370526 3 4237.8-3349024EordEN 3 4240.0-3249055S 3 4239.0-3813005S 3 4240.6-31594E 3 4240.0-3826065E 4 E 4 S(nb)orBCD 4 E 5 (interacting)? 5 S0 4 S 5 E(incluster) 5 S 5 E(incluster) 3 Im 5 5 E 4 ImlV? 5 S 5 S(nb) 5 E 5 S 5 S 5 RSa 5 S 4 S 5 E 5 E 4 S? 5 S 5 (interacting)? 5 E 5 E(incluster) 5 E 5 S 5 E 5 5 E 3 pecorBCD 5 E 5 E(cD)? 5 E 5 5 SblI 5 E E Im dE2? E E(M32?) S? S S? pec Type (5) 18.7 5.00.531 16.9 18.3 18.5 3.80.481 17.3 1.80.462 17.0 7.00.902 18.0 18.1 16.2 2.50.592 17.3 4.60.712 16.8 19.3 17.9 18.0 18.6 18.3 17.8 17.9 17.6 16.7 17.8 18.9 17.7 7.10.791 18.0 4.30.563 17.8 5.50.601 18.6 18.6 18.0 16.4 6.60.844 18.0 16.9 18.5 18.2 19.1 18.5 18.6 18.6 17.5 18.5 3.40.491 18.2 3.60.551 18.3 3.60.551 17.4 7.10.772 17.3 4.30.652 18.0 7.20.623 19.1 18.0 4.50.60 18.2 4.20.54 18.1 4.70.56 18.9 4.00.461 18.5 3.20.471 18.2 3.60.551 18.1 5.00.561 17.8 5.10.691 17.6 3.20.553 18.3 17.7 2.60.49 16.8 17.6 5.00.761 18.2 3.10.471 18.3 4.60.61 17.1 9.60.74 Bj rDS 17.5 16.7 16.2 4.10.75 (6) (7)(8)(9) e 4.1 0.541 4.0 0.531 4.2 0.53 7.6 0.54 4.0 0.52 7.7 0.77 3.1 0.684 7.6 0.72 6.1 0.50 4.0 0.50 4.0 0.57 4.2 0.551 3.7 0.581 2.9 0.63 3.6 0.53 3.3 0.52 3.7 0.59 4.4 0.49 5.4 0.59 3.3 0.461 3.0 0.47 3.6 0.51 4.6 0.51 3.1 0.46 2.0 0.51 5.6 0.72 3.7 0.51 3.7 0.50 3.5 0.501 3.1 0.461 3.6 0.64 Table III.(continued) 0.73 0.68 B1767 B1758 B1757 B1756 B1776 B1775 B1774 B1772 B1771 B1770 B1769 B1768 B1766 B1765 B1764 B1762 B1759 B1777 B1773 B1763 B1761 B1760 B1783 B1781 B1780 B1778 B1784 B1782 B1779 B1785 B1789 B1788 B1787 B1786 B1790 B1794 B1792 B1791 B1807 B1806 B1799* 343120-383212 B1798 B1797 B1796 B1795 B1793 B1815 34329.9 B1811 34321.9 B1810 B1809 B1808 B1805 B1804 B1803 B1802 B1801 B1800 343124-341714 B1813 34328.8 B1812 343221 B1818 B1816 B1814 34329.4 B1820 B1817 B1819 (1) (2)(3)(4) # RA(1950)Dec(1950)M 3 4242.4-3428224S 3 4240.9-3338165? 3 4240.8-3637275E 3 4243.5-3622575E 3 4241.1-35405E 3 4257.3-3151074E(nb) 3 4252.3-3647585Sc 3 4251.1-3306515E 3 4250.6-35045S 3 4249.8-3511445S 3 4248.2-3508585 3 4247.6-355047 3 4243.6-3646434 3 4259.2-3634445S 3 4259.0-3648125S 3 4254.7-3253455E 3 4253.9-3253475E 3 4253.2-3751375Epec 3 4252.9-3653055E 3 4252.8-3515435E 3 4249.7-3150565 3 4248.0-3847245 3 4300.4-3411345E(cD) 3 4300.3-3224265E(nb) 3 4300.2-381008dESN 3 4302.1-3306564? 3 4302.0-3806ImV? 3 4301.3-3258205E 3 401.0-3827305S 3 4302.0-38485S 3 4306.7-3555285 3 4305.0-3812185 3 4304.5-3252205 3 4304.3-3436445 3 4308.0-340439 3 4307.2-323615 3 4307.1-340817 3 4307.0-375225 3 4306.8-3412165 3 4316.4 3 4315.9 3 4314.7-340423 3 4310.9-353936 3 4309.6-374540 3 4309.3-332230 3 4308.1-3540485E 3 4318.5 3 4318.0 3 4317.3 3 4317.0 3 4316.2 3 4315.9 3 4313.1-380717 3 4330.9-341551 3 4330.8-361022 3 4330.6-342459 3 4333.0-3818 3 4332.7-370055 32 2159 37 3327 37 3335 31 5630 36 5838 32 0056 37 0060 32 0216 37 3311 36 1922 34 5522 35 5511 32 1849 4 S? 4 ? 4 E(M32?) 4 SordE3N 4 E 5 (interacting) 5 S 5 S 4 S0 5 S 5 SBa(r)pec 5 E 5 S 5 E 5 E 5 E 5 E 5 Sb(Seyfert?) 4 E(M32?) 5 S(incluster) 4 E 5 SBa(r) 5 E 5 S S S S ordE3N S (onedge) (interacting) E E(in cluster) S S0 S E(M32?) E(M32?) S(nb) ? ? Type (5) 17.6 6.10.673 18.5 3.60.461 18.0 5.50.652 16.9 17.1 18.2 4.00.563 16.6 0.815 17.2 3.20.584 17.7 4.60.562 18.8 280.473 18.4 3.90.491 17.7 18.9 18.6 18.9 3.40.481 18.4 16.3 17.7 17.0 18.1 18.2 18.2 17.4 16.7 18.2 17.7 15.2 18.0 18.6 18.2 3.50.481 18.0 3.70.511 18.9 18.2 18.5 18.0 6.50.661 16.1 0.735 17.7 210.482 17.7 18.3 18.7 B rDS 16.8 18.5 18.7 19.3 18.4 18.4 3.80.501 17.8 3.50.532 18.8 3.30.463 16.6 2.50.543 17.4 3.00.542 14.9 1.215 17.6 5.80.691 16.9 240.504 18.7 4.50.471 17.8 16.8 18.5 4.30.501 (6) (7)(8)(9) 16.8 17.6 16.7 18.7 16.8 17.0 18.7 18.5 te 4.0 0.471 4.7 0.862 6.6 0.461 7.0 0.751 5.8 0.631 5.5 0.663 3.2 0.594 3.2 0.612 4.2 0.54 4.9 0.68 9.8 0.802 5.0 0.581 3.4 0.47 3.4 0.49 4.1 0.471 3.8 0.481 3.2 0.59 4.3 0.47 4.3 0.53 5.5 0.57 4.5 0.471 5.6 0.68 3.4 0.48 4.9 0.531 4.1 0.622 4.0 0.521 5.2 0.501 4.2 0.702 2.2 0.602 3.1 0.461 5.9 0.73 2.5 0.692 29 0.59 6.5 0.803 8.2 0.88 3.2 0.531 0.77 0.80 5 0.85 0.51 5 393 1989AJ 98. .367F 394 HENRYC.FERGUSON:THEFORNAXCLUSTER B1826 B1824 B1821 B1841 B1840 34354.3-3414174Im? B1838 34350.5-3650155 B1837 34350.0-3748395E B1834 B1832 B1830 B1829 B1828 B1827 B1825 B1823 B1822 B1844 B1843 B1842 B1839 34351.2-3230335S B1836 34348.8-3648055 B1835 B1833 B1831 B1847 B1845 B1850 B1848 B1846 B1855 B1851 B1849 B1858 B1857 B1856 B1854 B1853 B1852 © American Astronomical Society • Provided by the NASA Astrophysics Data System B1863 B1862 B1861 B1860 B1859 B1867 B1866 B1865 B1864 B1880 B1878 B1876 B1875 B1872 B1870 B1869 B1868 B1883 B1882 B1881 B1879 B1877 B1874 B1873 B1871 B1885 B1884 (1) # RA(1950) Dcc(l950)M 3 4338.7-323915 3 4334.4-320644 3 4346.5-375349 3 4344.8-334805 3 4339.8-365644 3 4339.0-341309 3 4338.8-335323 3 4335.4-324407 3 4334.3-322947 3 4354.3-332023 3 4347.5-331629 3 4345.1-343603 3 4342.1-335227 3 4341.8-320915 3 4339.8-335308 3 4358.3-315859 3 4356.9-321315 3 4356.6-363622 3 4355.7-380452 3 4340.3-321619 3 4358.7-365130 3 4358.9-321142 3 4400.7-360226 3 4400.6-330960 3 4400.0-381748 3 4405.1-343919 3 4403.4-320132 3 4401.6-344232 3 4409.4-363659 3 4405.8-354126 3 4405.6-351621 3 4404.0-344315 3 4403.4-380742 3 4411.6-372722 3 4410.6-343540 3 4408.4-341849 3 4407.9-343825 3 4407.6-320559 3 4413.1-341301 3 4412.1-341204 3 4412.0-345601 3 4411.6-314934 3 4415.8-320725 3 4414.3-315420 3 4427.5-365132 3 4427.1-330522 3 4426.0-362659 3 4423.6-330750 3 4419.3-315114 3 4419.3-334017 3 4417.5-375731 3 4417.3-353331 3 4428.3-322808 3 4428.0-383106 3 4427.9-324837 3 4427.0-320415 3 4421.0-330546 3 4431.0-383312 3 4430.6-354603 3 4429.0-370614 (2) (3)(4) 4 BCD? 5 4 EordE 5 S 5 E 5 5 S 5 E 5 E 5 E 5 S 4 E 5 S0 5 E 5 E 5 ? 5 E 5 S(onedge) 5 S 5 S? 4 S(HighSB)? 5 S 5 E 4 E(M32?)? 5 RSa 4 E(incluster) 5 E 5 Epec 5 E 5 S 5 S0 5 S 5 E 5 E 5 S 5 E 5 E 4 filament? 4 S(incluster)? 4 E 5 E 3 ? 5 E 5 S(incluster) 5 E(incluster) 5 S0 5 E(imeracting) 5 E 5 E group orIm S S S S Type (5) 17.9 4.40.561 17.6 17.9 18.6 3.30.481 18.0 4.00.523 18.6 3.00.491 18.7 18.2 4.10.611 18.7 16.8 8.10.881 18.1 3.30.511 18.3 3.60.503 18.3 3.60.471 17.3 2.30.554 18.4 3.70.481 18.4 3.90.501 18.6 4.30.501 17.8 2.60.502 17.8 4.00.573 18.5 3.60.481 18.2 3.50.501 17.4 16.3 17.3 17.4 18.9 3.70.491 18.0 3.50.501 18.6 3.50.471 16.4 18.2 18.6 4.10.511 15.8 0.765 18.2 17.5 18.1 18.2 18.2 16.8 17.2 18.1 4.10.581 17.9 18.8 18.5 17.8 17.7 8.10.701 18.0 5.30.681 18.4 3.40.471 18.0 3.80.511 16.7 5.80.842 18.5 3.60.461 16.7 2.20.524 19.1 19.3 18.9 4.70.531 17.1 2.70.572 18.2 3.30.461 18.1 4.20.521 18.2 3.70.561 18.6 5.50.501 18.9 4.30.461 Bj rDS 18.9 3.70.49 18.9 4.10.50 16.2 1.13 18.1 18.5 (6) (7)(8)(9) e 2.1 0.492 3.6 0.522 5.5 0.77 3.3 0.46 3.1 0.461 2.2 0.51 2.5 0.55 3.3 0.54 4.2 0.56 4.8 0.51 4.3 0.54 2.2 0.61 5.8 0.61 3.3 0.46 2.4 0.48 3.7 0.55 2.6 0.49 3.5 0.51 3.5 0.65 3.5 0.47 3.9 0.53 3.5 0.46 3.5 0.50 3.9 0.511 Table III.(continued) 0.58 5 5 3 3 B1890 B1889 B1888 B1887 B1907 B1905 B1904 B1891 B1886 B1909 B1906 B1903 B1902 B1900 34437.3-320248 B1899* 34436.6-370331 B1897 34434.8-354130 B1895 B1894 B1893 B1910 B1908 B1901 B1898 34434.9-343156 B1896 34434.7-333248 B1892 B1917 B1916 B1915 B1914 B1913 B1912 B1911 B1918 B1922 34449.1-364554 B1921* 34449.1-370552 B1920 B1919 B1926 B1924 34449.8-315725 B1923 34449.7-342855 B1930 B1929 B1928 B1927 B1925 34451.3-364015 B1932 B1931 B1934 B1933 B1949 B1947 B1946 B1945 B1944 B1941 B1940 B1938 B1935 B1950 B1948 B1943 B1942 B1939 B1937 B1936 (1) # RA(1950) Dec(1950)M 3 4438.4-320314 3 4433.1-320643 3 4432.1-3240 3 4431.5-330609 3 4442.5-320100 3 4440.7-334133 3 4440.1-370251 3 4440.0-360449 3 4439.0-343211 3 4437.4-330403 3 4434.6-330456 3 4433.7-331059 3 4433.7-380641 3 4433.5-343331 3 4432.6-343023 3 4431.7-321134 3 4431.3-341949 3 4445.0-343156 3 4444.8-325018 3 4442.9-330218 3 4445.9-373852 3 4445.9-325753 3 4446.4-335302 3 4446.4-325725 3 4446.2-342423 3 4446.0-332624 3 4447.3-330139 3 4447.2-332524 3 4448.8-370728 3 4448.0-3600 3 4454.1-3341 3 4453.6-335802 3 4454.3-355013 3 4455.1-373731 3 4454.5-355630 3 4455.2-352648 3 4502.9-355525 3 4457.5-320137 3 4456.9-375330 3 4456.7-363553 3 4511.4-320915 3 4509.4-333440 3 4507.5-315754 3 4505.9-3435 3 4505.5-363236 3 4503.6-315260 3 4503.4-332956 3 4502.5-352412 3 4501.2-375156 3 4500.6-315843 3 4459.7-365343 3 4459.4-314946 3 4508.5-3451 3 4503.2-345707 3 4501.6-3523 (2) (3)(4) 4 E(M32?) 5 S 5 E? 5 E(incluster) 5 5 5 S 5 Shell 5 E(cD) 5 E(incluster) 5 S 5 ? 5 E(incluster) 5 S(nb) 5 E(incluster) 5 E(incluster) 5 E? 4 E(incluster) 5 Sc(r)I-II 5 E 5 E(incluster)? 4 E 4 SordEO 4 EordE,N 4 E(M32?) 5 S 5 S 5 E 5 E(incluster) 5 S0? 5 E 5 S0(incluster) 5 E(M32?) 5 SBb(s)I-n 4 EordE,N 4 E 5 4 S(incluster)orBCD 4 SordSO 4 S 5 E 5 S 5 ring 5 E 4 (interacting)? 5 Sell 5 E 5 S 5 S(incluster) 5 S 5 SO 5 S 5 S 5 E 5 E 3 E(M32?) 5 S 5 S 3 E(cD)ordE 3 E6(M32?) Im(in cluster)? group E(in cluster) S0 Sel-H Type (5) 18.6 18.5 16.5 19.1 15.8 5.90.833 18.8 6.10.591 16.4 14.41.002 17.8 5.50.691 18.1 5.40.611 17.4 4.70.702 16.1 10.71.014 15.9 11.11.042 18.3 3.40.481 17.3 1.80.502 18.9 18.4 17.8 15.8 17.9 17.2 17.5 18.6 18.2 17.6 16.0 16.6 2.30.564 17.9 4.60.581 17.8 4.00.571 18.0 4.10.631 18.7 4.30.471 16.4 15.51.054 17.8 5.10.593 17.7 4.90.573 18.3 3.30.521 19.4 4.00.501 18.4 3.40.461 16.4 6.20.833 17.9 18.0 3.00.522 17.7 2.80.512 15.5 16.7 18.6 18.0 17.9 18.1 19.0 18.3 4.40.511 16.9 18.6 17.3 18.6 18.0 18.7 3.70.471 16.6 4.10.804 16.7 17.1 (6) (7)(8)(9) 18.4 3.70.511 18.6 6.50.561 16.7 2.30.593 18.6 3.30.491 17.8 3.90.543 18.8 4.20.461 15.3 14.61.182 15.6 8.81.044 4.7 0.56 2.3 0.512 7.6 0.621 5.4 0.702 3.3 0.471 3.4 0.521 2.9 0.46 3.5 0.55 2.9 0.65 2.0 0.54 3.9 0.45 3.5 0.49 9.2 0.85 3.4 0.46 2.9 0.52 4.1 0.54 4.2 0.50 4.6 0.54 5.1 0.56 4.9 0.63 2.7 0.46 5.4 0.65 5.0 0.58 3.8 0.56 2.4 0.51 3.2 0.60 3.7 0.49 3.4 0.61 3.9 0.55 1.7 0.46 D S 394 1989AJ 98. .367F 395 HENRYC.FERGUSON:THEFORNAXCLUSTER B1951 34511.4-3258295S B1958 B1955 34513.8-3205585E B1953 34512.1-3738505E B1952 34511.8-3337114Spec B1961 B1960 B1959 B1957 B1956* B1954 34512.4-3732565 B1963 B1962 B1965 B1964 B1966 B1968 B1967 B1972 B1971 B1970 B1969 B1974 B1973 © American Astronomical Society • Provided by the NASA Astrophysics Data System B1977 B1976 B1975 B1979 B1978 B1980 B1982 B1981 B1984 B1983 B1985 B1987 B1986 B1992 B1990 B1989 B1988 B2002 B2000 B1999 B1997 B1996 B1995 B1994 B1993 B1991 B2004 B2003 B2001 B1998 B2005 B2007 B2006 B2009 B2008 B2010 B2014 B2012 B2011 B2015 B2013 (1) (2)O)(4) # RA(1950)Dec(1950)M 3 4517.2-370331 3 4515.1-373147 3 4524.2-315800 3 4523.1-364351 3 4523.0-323018 3 4521.4-371343 3 4517.2-315939 3 4524.0-380458 3 4524.2-342160 3 4524.2-330011 3 4524.6-3153595S? 3 4527.9-3639534E 3 4526.8-355557dE0,NorS 3 4526.2-355843S?orImlV 3 4524.9-3533424EordEN 3 4529.2-3329085E 3 4529.0-3831545E 3 4528.8-345553dE6 3 4528.5-3729094EordEJí 3 4528.0-3627435E(cD) 3 4532.0-333013 3 4534.8-353214 3 4532.7-333602 3 4531.3-373134 3 4536.2-330040 3 4536.8-3315565E(interacting) 3 4536.5-3446405E(cD)pec 3 45424-3430324S 3 4541.8-3426015S 3 4544.2-3554145E 3 4546.1-353407 3 4544.9-373837 3 4548.6-324457 3 4548.3-315747 3 4548.1-351529 3 45525-332754 3 4551.2-361752 3 4550.2-330521 3 4549.8-320756 3 4556.0-3301325E 3 4555.2-3450275S 3 4555.0-3737425S 3 4554.7-3425184SordS0pec,N 3 4553.1-314844 3 4559.0-3237174 3 4557.0-3646355(interacting) 3 4556.2-3652264 3 4556.0-3317065E 3 4559.4-3616055E(nb) 3 4558.6-3302115? 3 4603.1-363717 3 46020-3306 3 4601.3-333545 3 4559.9-374732 3 4559.5-361354 3 4603.7-3313114E 3 4604.2-3305285(interacting)? 3 4605.1-3205495S 3 4604.2-3305574(interacting) 3 4606.0-3303125E 4 S 5 5 ? 5 E 5 S 4 E 4 S 5 E 5 E 5 S(onedge) 4 E 4 S0(M32?) 5 E 5 Sbc(s)II 5 S 5 E 5 S 5 S 5 S? 5 E E S S0 Sc(s) S dE(nb) S S? S S Type (5) 17.4 4.10.622 18.6 3.50.471 18.3 3.40.461 19.1 4.80.513 17.5 250.55 15.0 1.114 17.6 2.30.512 16.6 17.7 17.9 18.1 18.2 18.3 18.2 18.8 16.2 18.4 18.9 19.3 18.6 17.8 18.5 18.4 16.9 18.1 17.9 19.0 17.9 18.7 18.5 (6) (7)(8)(9) 18.4 18.2 15.9 17.4 18.0 17.1 17.4 18.2 17.3 15.5 lYs 0.645 18.5 4.50.511 17.8 17.1 17.7 19.1 18.4 18.6 4.00.461 19.4 3.10.471 17.5 9.40.791 17.7 3.00.513 18.4 3.20.461 19.0 4.40.503 17.4 4.60.562 17.1 5.60.752 17.6 5.00.711 16.7 9.10.822 18.4 3.80.531 18.5 6.30.561 19.0 4.20.473 17.7 4.30.541 17.6 3.60.592 17.5 6.20.641 17.9 5.10.581 18.0 6.80.631 4.6 0.63 4.3 0.511 4.4 0.54 5.0 0.661 3.1 0.673 3.5 0.46 2.5 0.582 3.4 0.48 3.4 0.47 5.1 0.593 5.3 0.583 6.3 0.561 6.1 0.461 6.3 0.721 8.9 0.591 4.4 0.511 4.3 0.611 4.7 0.553 5.7 0.663 3.3 0.511 4.0 0.501 3.5 0.491 3.5 0.511 5.9 0.531 3.0 0.703 3.7 0.583 3.9 0.611 4.6 0.60 4.9 0.47 5.1 0.561 2.2 0.492 8.9 0.844 3.4 0.574 2.4 0.58 2.9 0.51 3.2 0.613 3.6 0.50 Table III.(continued) 0.67 5 D S B2025* 34615.0-3651115Sbc(s)II B2023 34613.9-3343324E? B2022 34613.2-3150044E? B2021 34611.8-3334255E(incluster) B2020 34609.9-3359045S(interacting) B2018 34609.0-3500535S B2017 34607.8-3212415E(nb) B2016 34606.4-3212544E(incluster) B2026 34616.0-3332605E(incluster) B2024 34614.5-3207504E B2019 34609.5-3425314? B2028 34616.6-3151505E B2027 34616.6-3155505E(nb) B2031 34619.5-3303364S? B2030 34619.0-3148385E B2029 34617.3-3654525E B2033 34620.3-3602105S B2032 34620.2-3439174S B2035 34621.0-3412045E(incluster) B2034 34620.5-3208454S B2037 34623.4-3614295E B2036 34622.0-3213345E(incluster) B2039 34624.3-3337325E(cD)pec B2038 34624.0-3654455E B2042 34625.2-3459095E(cD)? B2041 34625.1-3217555S0(incluster) B2040 34625.0-3549134E(M32?) B2044 34626.9-33075S B2043 34626.1-3532545E B2047 34630.5-3214234S0(incluster) B2045 34626.9-3610544S B2050 34632.0-332847E(M32?) B2049 34630.9-3334535E(incluster) B2048 34630.6-3342444? B2046 34628.0-3817124SorSm B2052 34632.9-3335505E(incluster) B2051* 34632.3-32235S(onedge) B2053 34635.6-3336155E(incluster) B2057 34637.0-3204364? B2056 34636.9-3226324? B2055 34636.8-3404275E B2054 34635.7-3414554E(cD)? B2058 34638.5-3352574EorBCD B2063 34643.1-3353155S B2062 34641.7-3215174? B2060 34641.2-3306365S(onedge) B2059 34639.1-3759185E(incluster) B2067 34647.6-360347dE?,N B2066 34646.9-3754045S(nb) B2065 34644.0-3207164E B2064 34643.4-3411494E(cD) B2061 34641.2-3332085S(onedge) B2069 34648.1-3444554E B2068 34647.8-3149295E B2070 34648.5-3335305S B2072 34650.9-3311325E+flaw B2071 34649.1-3754105S(onedge) B2076 34652.2-3409225S B2075 B2074 B2073 B2079 34658.8-3523015 B2078 34654.5-3617505E B2077 34653.8-3438315E B2080 34659.4-32174E(incluster) (1) (2)(3)(4) # RA(1950)Dec(1950)M 3 4651.1-3538325S0 3 4652.0-3226304group 3 4651.0-3323104? Type (5) 18.2 3.10.491 16.1 8.10.992 17.5 10.00.791 17.3 5.30.632 18.2 4.20.511 19.3 4.30.471 18.4 17.9 14.1 17.3 18.4 17.7 18.0 18.4 17.6 17.8 18.6 16.2 18.2 17.0 18.0 18.7 17.4 B 18.0 17.3 18.5 17.5 18.6 16.5 18.3 4.80.611 18.2 4.70.531 16.5 16.9 17.7 (6) (7)(8)(9) 18.4 4.00.531 16.6 6.30.862 17.0 7.50.872 17.8 9.30.811 17.6 17.9 5.70.611 18.0 18.2 18.9 16.5 17.9 18.4 4.80.491 17.1 16.3 18.0 17.4 17.5 17.8 18.5 17.7 t 18.3 18.7 17.6 18.7 18.3 18.7 19.2 18.0 16.9 18.8 17.9 4.0 0.481 4.1 0.581 5.9 0.631 6.1 0.954 9.5 0.791 25 0.522 3.2 0.461 4.5 0.501 3.6 0.481 4.2 0.511 5.8 0.812 3.7 0.491 3.5 0.491 3.0 0.512 3.0 0.58 3.4 0.58 7.6 0.69 9.3 0.85 2.8 0.46 4.3 0.52 5.9 0.53 20 0.49 25 0.54 6.3 0.72 3.4 0.702 4.7 0.611 4.7 0.611 4.7 0.671 4.2 0.611 4.4 0.701 3.3 0.511 26 0.562 9.0 0.862 5.7 0.772 3.4 0.471 5.8 0.662 28 0.592 3.3 0.612 4.6 0.59 4.1 0.49 22 0.49 4.0 0.48 3.9 0.501 3.5 0.491 4.3 0.481 9.3 0.63 3.9 0.491 3.6 0.491 6.1 0.802 3.3 0.522 0.74 5 D S 395 1989AJ 98. .367F 396 HENRYC.FERGUSON:THEFORNAXCLUSTER B2084 34701.7-3246234E(incluster) B2082 34700.5-3156274E B2086 34702.5-3216405E(interacting) B2085 3470Z3-3201355E B2083 34701.1-3314085(interacting)? B2081 34700.0-3245094E(incluster) B2091 34707.8-362815 B2090 34707.6-33565E B2088 34704.2-3545215E(M32?) B2087 34703.3-355960? B2099 B2097 B2094 34709.7-352608 B2093 34708.9-324133 B2092* 34708.2-352958 B2089 34704.7-3514225 B2101 B2100 B2098 B2096 B2095* 34709.7-360134 B2105 B2104 B2103 B2102 B2106 B2108 B2107 B2109 B2114 B2113 B2112 B2110 B2116 B2115 B2111 B2121 B2120 B2119 B2118 B2117 B2123 B2122 B2129 B2127 B2125 B2124 B2133 B2131 B2130 B 2128 B 2126 B2135 B2134 B2132 B2136 B2139 B2138 B2137 B2144 B 2143 B2142 B2141 B 2140 B2145 © American Astronomical Society • Provided by the NASA Astrophysics Data System (1) (2)(3)(4) # RA(1950)Dec(1950)M 3 4711.1-354514 3 4712.3-340138 3 4712.2-364031 3 4712.2-352331 3 4711.5-324438 3 4710.3-363509 3 4710.2-353018 3 4709.9-354521 3 4715.1-330854 3 4714.8-320214 3 4715.2-334555 3 4716.9-325435 3 4716.7-333719 3 4717.2-343023 3 4723.2-360724 3 4723.1-351237 3 4720.4-3227 3 4719.7-364240 3 4717.2-335256 3 4724.6-335053 3 4724.7-335528 3 4726.1-341523 3 4725.8-363746 3 4734.6-373117 3 4734.2-341732 3 4733.6-334525 3 4733.3-325060 3 4727.1-320437 3 4741.7-333500 3 4740.7-370032 3 4736.5-334650 3 4734.7-341805 3 4749.3-345314 3 4743.8-362905 3 4743.0-362710 3 4742.3-320749 3 4741.2-335659 3 4739.8-334830 3 4748.5-373405 3 4747.0-362753 3 4743.5-375814 3 4751.3-363117 3 4749.6-362637 3 4751.8-362923 3 4755.0-322430 3 4753.8-334426 3 4753.7-342714 3 4753.5-363256 3 4755.1-323922 3 4754.5-345031 4 S 4 E(incluster) 5 E(M32?) 5 E 5 (interacting) 5 S 5 5 SO 5 (interacting) 5 E 4 EordE,N 4 ? 5 5 S 4 S? 4 EordSO 5 (interacting)? 5 4 4 ? 5 S0 4 E 4 EordE 5 S 4 E(M32?) 5 S0? 3 ? 3 dEN?orS 5 E 5 S(onedge) 5 S 3 SordEJSÎ 5 E 5 E 4 E 5 S 5 E(incluster) 5 E(interacting) 4 E(M32?) 5 E 4 (interacting)? 4 SordSO 5 S 5 E 5 S 5 E 5 E 5 S 5 5 E 5 5 E 4 S 5 S 3 EordE(M32?) Type (5) 17.9 4.70.621 17.5 2.30.542 18.1 4.90.561 17.9 5.80.671 18.0 8.70.671 18.2 3.50.471 17.0 3.20.592 17.6 3.50.602 18.5 3.30.451 18.2 3.50.501 18.5 2.80.471 16.7 7.10.802 18.4 3.10.461 17.6 17.0 17.4 16.2 19.0 4.40.471 18.7 3.60.451 18.8 17.2 14.5 4.90.972 18.1 18.0 2.80.462 18.5 4.50.511 18.0 5.90.621 18.6 4.10.491 19.7 5.10.541 18.2 3.70.461 16.3 15.9 17.4 2.30.512 Bj rDS 17.8 18.2 17.9 18.5 17.9 18.1 18.0 18.3 18.9 19.0 (6) (7)(8)(9) 18.0 4.20.541 18.6 4.60.481 18.7 18.4 18.8 18.2 18.3 17.2 18.4 18.6 18.3 18.3 3.70.511 18.6 3.70.571 17.4 2.80.532 17.8 17.8 17.1 17.9 4.40.681 17.9 4.50.562 18.1 18.4 16.5 17.4 2.70.612 e 7.4 0.772 6.5 0.682 5.6 0.691 9.2 0.902 6.0 0.531 2.5 0.592 3.9 0.521 4.6 0.54 4.4 0.61 4.5 0.57 2.6 0.68 3.3 0.68 5.4 0.621 4.1 0.461 3.3 0.471 3.5 0.521 3.8 0.542 3.2 0.48 4.4 0.511 3.8 0.46 3.8 0.552 4.0 0.562 2.5 0.512 3.2 0.47 3.7 0.47 3.3 0.501 3.4 0.511 3.7 0.47 5.5 0.682 5.0 0.792 3.3 0.471 3.6 0.512 6.1 0.862 3.7 0.521 Table III.(continued) B2147 34755.5 B2149 34758.2 B2148 34756.7 B2146 34755.3-3344454(interacting) B2164* 34814.4 B2162 34813.4 B2158 34806.5 B2153 34802.3 B2151 34759.2 B2150 34758.6 B2163 34814.3 B2161 34813.1 B2160 34811.8 B2159 34806.6 B2157 34806.3 B2156 34805.6 B2155 34804.2 B2154 34802.7 B2152 34800.9 B2166 34815.8-37045S B2165 B2170 34822.3-3514354E B2168 34819.5-3518204E B2167 34819.4-3315555E B2171 34823.0-3743165E B2169 34821.6-3738064S B2173 34824.9-33564? B2172 34823.5-3328175 B2174 34826.3-3405464S B2179 34833.3-3159285E B2177 34830.6-3545474E B2176 34829.7-3356055S B2175 34829.7-3219145S(onedge) B2180 34834.0-3424085 B2178 34830.8-3420465pec B2183 34837.4-3545294E B2182 34837.2-3317015S(onedge) B2181 34836.7-314743EordE B2188 34845.6-3302035E B2186 3484Z8-3545495E B2185 34841.3-3543544S0(boxy)? B2184 34839.0-3801095 B2194 34851.9-3652275S B2192 34848.5-3653465 B2191 34847.4-3638575S B2190 34846.9-332644E(M32?)ordE,N B2189 34846.4-3317294? B2187 34843.7-380517EordE,N B2198 34852.3-3755105E? B2196 34852.1-3405404E B2195 34852.0-3302445E B2193 34850.4-3359315S B2201 34853.2-33244E(M32?) B2200 34852.8-3313115E B2199 34852.7-3342544BCD? B2197 34852.2-3605214? B2204 34854.5-3746574E? B2203 34853.6-3731254SorBCD B2202 34853.6-3724375S B2205 34857.3-3228224 B2207 34858.2-3409025S(interacting) B2206 34857.8-3333075 B2209 34858.6-375931EordE,N B2208 34858.3-3332315E B2210 34859.0-3334425E? (1) # RA(1950) Dec(1950)M 3 4814.5-3727225 (2) (3)(4) 35 40534 34 50585E 32 18455 32 00585S 33 03315E 34 54125S 32 10265 34 564E 32 55403? 33 17025E 38 06345S(onedge) 32 36234EordE3? 36 28325 32 38603E?ordEN 35 57314E(M32?) 32 00264E 33 515 37 58345S(onedge) Type (5) 17.3 18.5 17.9 18.4 17.8 19.0 18.1 16.8 18.6 18.0 18.4 18.1 18.8 17.5 16.7 18.4 17.3 18.9 18.4 18.3 18.2 18.5 17.6 17.8 18.4 17.6 17.6 19.0 18.4 18.2 18.2 18.1 17.4 B rDS 17.7 17.4 18.0 18.1 18.6 18.4 18.7 17.8 18.4 18.5 18.0 (6) (7)(8)(9) 18.8 18.1 18.1 17.8 15.8 16.11.16 18.6 18.6 16.4 19.4 18.4 17.5 17.0 17.9 16.7 18.8 18.1 17.5 18.2 17.7 17.8 19.2 xe 4.1 0.481 4.3 0.571 4.4 0.471 4.9 0.662 4.3 0.692 4.3 0.511 4.4 0.501 ZI 0.492 3.3 0.551 5.5 0.461 4.1 0.49 4.0 0.481 4.3 0.521 4.4 0.561 5.6 0.661 6.5 0.701 3.0 0.47 Z4 0.56 3.7 0.491 3.1 0.481 4.3 0.571 3.1 0.46 8.0 0.88 3.7 0.562 3.3 0.642 3.6 0.461 4.5 0.561 6.8 0.701 Z7 0.472 3.5 0.482 4.3 0.551 4.2 0.561 5.4 0.571 3.4 0.51 4.4 0.551 4.0 0.471 Z5 0.50 3.9 0.51 3.7 0.51 6.6 0.64 4.3 0.55 3.5 0.501 3.6 0.49 3.7 0.50 4.2 0.541 7.2 0.541 3.4 0.471 5.4 0.651 6.2 0.571 3.9 0.521 3.8 0.511 4.1 0.632 4.4 0.551 5.3 0.511 3.5 0.481 Z7 0.542 Z2 0.542 4.5 0.591 5.2 0.511 3.9 0.632 Z8 0.462 3.4 0.511 1.6 0.512 3.8 0.471 396 1989AJ 98. .367F 397 HENRYC.FERGUSON:THEFORNAXCLUSTER B2216 B2219 B2218 B2217 B2215 B2214 B2213 B2212 B2211 B2229 B2228 B2227 B2226 B2221 B2220 B2230 B2225 B2224 B2223 B2222 B2234 B2231 B2240 B2239 B2238 B2236 B2235 B2233 B2232 B2242 B2241 B2237 B2244 B2243 B2269 B2268 B2267 B2266 B2264 B2263 B2262 B2261 B2260 B2259 B2258 B2257 B2256 B2255 B2254 B2252 B2250 B2249 B2245 B2271 B2270 B2265 B2253 B2251 B2248 B2247 B2246 B2275 B2274 B2272 B2273 © American Astronomical Society • Provided by the NASA Astrophysics Data System (1) # RA(1950) Dec(1950)M 3 4860.0-353243 3 4859.7-330322 3 4859.2-322346 3 4859.2-331203 3 4913.0-355142 3 4901.8-322210 3 4900.5-330215 3 4906.0-321005 3 4905.6-360334 3 4915.9-335902 3 4915.4-375738 3 4910.6-380648 3 4910.6-325150 3 4907.4-322842 3 4906.1-332637 3 4906.0-3756 3 4923.4-325452 3 4919.3-335754 3 4919.0-343419 3 4919.0-333106 3 4917.9-315830 3 4917.7-371244 3 4909.2-361032 3 4908.9-374428 3 4907.9-331011 3 4907.7-374550 3 4924.0-341930 3 4921.5-340535 3 4920.0-324543 3 4919.5-332343 3 4924.9-3720 3 4924.9-373546 3 4925.7-323953 3 4925.3-364455 3 4927.3-373824 3 4944.3-330528 3 4944.0-350024 3 4943.0-350302 3 4942.9-371920 3 4938.7-364439 3 4937.8-325910 3 4935.8-323639 3 4944.8-340443 3 4942.9-324224 3 4942.2-341636 3 4941.8-373646 3 4940.8-323142 3 4939.5-321950 3 4936.1-374826 3 4935.3-345637 3 4934.1-372914 3 4927.8-343406 3 4954.9-3300 3 4954.5-321611 3 4950.1-331519 3 4945.3-370554 3 4933.9-375435 3 4933.7-315716 3 4931.1-371631 3 4928.2-375040 3 4956.3-344705 3 4955.7-324601 3 4956.7-331423 3 4958.7-323336 3 4958.1-322910 (2) (3)(4) 4 ? 4 S 4 E 4 ImordSO 4 E 5 S 5 E 5 S 5 S(onedge) 4 E 4 4 E(M32?) 4 E 5 3 dE?,N 4 E 5 S 4 5 S 5 5 E 4 S 4 E 5 5 S(nb) 5 E 5 S0 3 dSO?orS? 5 E? 3 E(M32?) 5 E 5 (interacting)? 4 E 4 E(M32?) 4 S0 3 E 4 S? 4 E 5 E 4 5 S 4 E(M32?) 5 S 5 S 5 S 5 S 5 5 E 5 S 5 S 5 E(interacting) 4 S(LSB)ordSO 4 ? 4 S 5 S 5 E 5 S(onedge) 5 E 5 S 4 ? 4 E 5 S(onedge) 5 S 5 S 5 E Type (5) 18.2 18.0 4.20.581 16.8 18.5 18.4 16.5 15.9 3.20.692 17.7 4.40.632 18.5 18.5 19.0 4.10.481 18.2 3.30.491 15.7 17.5 18.1 18.9 16.5 17.5 16.8 18.4 18.3 18.1 19.0 18.3 17.3 17.5 18.4 17.9 17.8 18.4 17.4 18.4 18.5 18.7 17.7 18.5 19.1 15.8 17.6 18.1 18.2 4.40.581 19.1 3.60.461 16.8 3.10.612 16.8 18.3 18.5 18.4 18.5 3.50.491 18.7 3.30.491 18.0 3.50.561 18.0 3.90.581 18.1 3.60.461 17.5 5.70.721 18.6 3.60.471 17.4 18.0 18.9 4.20.461 17.8 18.1 18.2 18.0 17.2 5.30.631 17.5 3.90.512 18.3 3.50.511 18.3 4.00.561 Bj rDS (6) (7)(8)(9) A 4.9 0.561 4.0 0.46 4.8 0.56 5.5 0.531 2.3 0.552 5.7 0.742 3.3 0.461 4.5 0.66 4.1 0.51 7.7 0.47 4.0 0.50 3.5 0.49 3.1 0.491 2.0 0.47 3.7 0.54 3.1 0.58 4.0 0.47 4.9 0.79 5.4 0.652 5.0 0.541 3.4 0.461 2.6 0.46 2.2 0.53 3.6 0.50 3.0 0.57 3.9 0.50 3.2 0.71 3.4 0.52 5.3 0.61 4.2 0.55 5.0 0.531 3.6 0.461 3.7 0.49 3.5 0.47 3.1 0.66 2.1 0.48 5.5 0.66 3.5 0.47 3.3 0.46 3.8 0.55 3.7 0.52 3.7 0.51 3.5 0.48 3.9 0.53 3.0 0.45 Table III.(continued) B2290 B2289 B2298 B2297 B2295 B2294 B2293 B2292 B2291 B2288 B2287 B2286 B2276 B2304 B2303 B2300 B2296 B2285 B2284 B2282 B2281 B2280 B2279 B2278 B2277 B2306 B2305 B2302 B2301 B2299 B2283 B2308 B2307 B2309 B2330 B2329 B2328 B2327 B2326 B2325 B2324 B2321 B2318 B2312 B2311 B2310 B2334 B2333 B2332 B2331 B2323 B2322 B2320 B2319 B2317 B2316 B2315 B2314 B2313 B2337 35211.9-3741245? B2336 35203.1-3743125S B2335 B2338 35216.4-3734494E (1) # RA(1950) Dec(1950)M 3 4959.7-374515 3 5025.1-332956 3 5025.0-373855 3 5022.5-375428 3 5022.3-374824 3 5020.9-375514 3 5018.8-333014 3 5018.8-332951 3 5018.5-3757 3 5018.1-321611 3 5016.7-333358 3 5013.1-323105 3 5012.5-344700 3 5011.4-374833 3 5009.9-322905 3 5008.6-320218 3 5008.0-334008 3 5004.4-331108 3 5004.3-320901 3 5003.5-343727 3 5002.3-323638 3 5032.9-3738 3 5032.8-375322 3 5032.0-323330 3 5026.3-341258 3 5005.7-380110 3 5005.0-333118 3 5040.6-372908 3 5039.7-323047 3 5038.8-370947 3 5038.7-371027 3 5036.1-372207 3 5036.0-332410 3 5033.2-373258 3 5139.7-380621 3 5133.6-345030 3 5129.9-343728 3 5119.0-335712 3 5041.1-373612 3 5142.8-372636 3 5140.3-373945 3 5136.1-3438 3 5115.6-374113 3 5114.3-342658 3 5112.8-343540 3 5111.6-372352 3 5110.8-373038 3 5105.0-322554 3 5104.0-375248 3 5102.5-331918 3 5059.7-321014 3 5058.0-3412 3 5048.0-323936 3 5046.5-370140 3 5159.0-374111 3 5158.0-375317 3 5150.1-375752 3 5057.4-335702 3 5048.4-321532 3 5047.3-332221 (2) (3)(4) 4 E 4 EordEJM 4 E(M32?) 4 S 4 S 4 ? 4 SordSO 5 S 5 E 4 E 4 Im? 4 E 4 E 5 5 E 5 E 5 S(incluster) 3 (interacting)orBCD 4 S 4 ? 5 E 5 E(nb) 5 S 5 E 5 5 E 3 E(M32?) 3 E(M32?) 5 S 5 5 E 4 EordE,N 4 RS 4 E?ordE 4 E 4 EordE 5 E 5 E 3 dE 5 S 5 S 5 S 5 S 5 4 ? 4 E 5 E(pair)? 5 5 ? 5 S 5 E 5 S 5 S 5 S(onedge) 5 S 5 E 5 E? 3 ? 5 E 3 (interacting)?orIm Type (5) 17.0 3.40.612 18.4 3.80.541 18.0 3.50.521 18.8 17.9 15.6 17.2 4.40.692 17.7 3.00.572 16.4 6.40.742 18.2 3.80.471 16.0 6.50.902 16.6 6.30.832 18.6 4.10.481 18.7 3.20.461 18.2 5.70.651 18.9 5.70.531 18.1 3.70.571 17.4 17.5 18.0 18.9 18.3 18.0 9.60.611 16.8 18.8 16.7 5.00.702 18.8 5.70.571 17.6 4.40.631 18.5 18.8 18.4 3.80.541 17.3 5.70.722 18.1 3.40.481 17.6 3.60.542 18.8 17.9 4.40.621 17.8 5.70.611 18.0 17.1 18.1 18.7 4.70.501 16.8 2.70.572 18.4 17.8 4.10.581 18.7 18.0 18.7 17.7 18.3 3.70.511 18.0 3.30.481 18.4 3.50.531 18.3 18.1 18.6 4.00.491 17.7 3.90.531 17.9 3.70.512 17.6 3.40.512 18.8 4.90.551 17.9 4.50.561 18.7 18.1 17.3 18.0 Bj rDS (6) (7)(8)(9) e 4.8 0.65 4.1 0.46 7.6 1.00 5.3 0.72 4.3 0.481 5.3 0.461 5.4 0.67 3.8 0.591 3.2 0.461 5.6 0.541 2.1 0.502 3.1 0.461 3.6 0.481 4.3 0.531 4.8 0.521 4.3 0.581 7.9 0.751 4.0 0.461 3.5 0.521 2.9 0.592 3.8 0.491 5.0 0.711 3.2 0.471 5.8 0.591 6.8 0.651 3.3 0.501 3.3 0.471 397 1989AJ 98. .367F 398 © American Astronomical Society HENRY C.FERGUSON:THEFORNAXCLUSTER B0020 ES0300-G22 B0007 ESO357-G08 B0030 velocity4540±11ref.1 B0030 NGC1288,ES0357-G13 B0043 ES0357-G15 B0031 ES0357-G14,IC1909 B0083 ESO357-G20 B0074 ES0357-G17 B0068 ES0301-G06 B0210 NG32 B0186 G137a,D302 B0186 velocity12234±90ref.2 B0126 ES0357-G24 B0084 HPW3 B0080 ES0357-G18 B0407 velocity15623±120ref.2 B0271 NG132 B0255 G146 B0192 G137b B0463 ESO358-G07 B0463 velocity10022±190ref.3 B0413 ESO358-G03 B0407 G89,D303 B0476 G31,D304 B0476 velocity9353±30ref.2 B0576 HPW6 B0477 ESO301-G16 B0663 D48 B0644 D45 B0713 velocity16583±60ref.2 B0679 ESO301-G17 B0726 D57? B0724 D56 B0713 G102,D305 B0729 ESO301-G18 B0727 HPW9 B0747 HPW11 B0755 HPW12? B0789 HPW14 B0793 HPW15 B0818 G85,D306 B0818 velocity15233±120ref.2 B0827 velocity5125±60ref.2 B0827 G101,D307 B0868 velocity19196±120ref.2 B0868 G121,D308 B0897 G153 B0928 D78 B0933 velocity14037±120ref.2 B0936 D310 B0933 G120,D309 B0948 D312 B0944 D81 B0942 G100,D311 B0942 velocity14395±60ref.2 B0976 D313 B0990 velocity13974±60ref.2 B1005 velocity6562±0ref.1 B0990 G20,D314 B1038 D319 B1007 D316 B1005 ES0358-G22,G9,MCG-5-9-16 B1023 D317 Notes forTableIII Provided bythe NASA Astrophysics Data System B1075 D321 B1095 ES0358-G31 B1086 D323 B1102 D326 B1100 D325 B1104 G25,D327 B1104 velocity15922±60ref.2 B1129 velocity11900±60ref.2 B1120 NG135 B1229 D347 B1212 D345 B1195 HPW22,,D341,H5 B1188 ESO358-G40 B1183 D339? B1180 D338 B1178 D339? B1169 D333 B1166 D335? B1165 D332 B1143 D330 B1129 G4,ES0418-G14,D328 B1241 D128 B1185 D340 B1274 D351 B1246 D348 B1286 D352 B1263 D350 B1335 HPW26 B1317 G157,ES0358-IG47 B1317 velocity16004±51ref.1 B1316 D355 B1373 D143 B1374 velocity18533±60ref.2 B1376 D143 B1374 G69,D358 B1404 ESO301-G22b B1396 ESO301-G22a B1483 NG100 B1509 D166 B1542 D170 B1532 HPW38 B1570 velocity15177±120ref.2 B1562 ESO301-G25 B1632 ES0302-G03 B1570 G113,D359 B1686 HPW41? B1799 ES0302-G04 B1699 D183,NG106 B1899 ES0358-G64 B1921 HPW44? B1956 velocity5758±150ref.2 B1956 G130,ES0302-G07,D360 B2025 G105,ES0358-G67,D210? B2025 velocity5224±43ref.1 B2051 ESO419-G08 B2095 velocity5393±60ref.2 B2092 ES0358-G68 B2095 G93,ES0358-G69 B2164 ESO359-G01 398 1989AJ 98. .367F 399 estimated; thesourcesforpositionsthesegalaxiesare that appearedtobemoreaccuratethanthepositionswehad A fewofthebrightergalaxieshadpositionsinliterature positions fromtheSRCandLasCampanasplateswas11.3". shown inthenotescolumn13. computed heretothoseinthetwootherrecentcatalogsof here andthoselistedinhisTableIis7.4arcsec.Forgalaxies the FornaxCluster.ForgalaxiesincommonwithCaldwell on averageby7.5arcsec. in commonwithDaviesetal.(1988),thepositionsdiffered of theSRCplate,unbiasedwithrespecttoclustermember- essentially independentsurveys:Adiameter-limitedsurvey bership codesaredefinedinTableIV. cluster members.Theassignmentofmembershipwas the LasCampanasplates,highlybiasedtowardapparent ship, andamorphologicallyselectedsampleofgalaxiesfrom discussed brieflyaboveandextensivelyinBST85.Themem- system, setoutintheHubbleAtlas(Sandage1961),Re- ments onanindividualgalaxythatcouldnotberesolvedbya panas platematerialhavebeenusedforclassifications.Gal- Binggeli 1984;BST85).BoththeSRCandLasCam- ship class(describedabove).Wherethereweredisagree- of galaxies,theclassificationsagreedtowithinonesubclass pendently bytheauthorandSandage.Forvastmajority axies intheLasCampanasplatesurveywereclassifiedinde- (1987), themeanseparationbetweenpositionslisted vised Shapley-AmesCatalog(SandageandTammann 1981), andtheVirgoClusterSurveypapers(Sandage (e.g., SavsSab,ImIVV)andtowithinonemember- 20 Jonesand1980. 30 Burstein1987. 10 Welch,Chincarini,andRood, 1975. 2 SRCplateonly.Imagesaturated. 4 SRCandLasCampanasplates. SRCimagesaturated. 3 SRCandLasCampanasplates.imagenotsaturated. 5 LasCampanasplateonly. 1 SRCplateonly.Imagenotsaturated. The galaxylistsinTablesIIandIIIarebasedontwo It maybeofsomeinteresttocomparethecoordinates All galaxieshavebeenclassifiedintheextendedHubble © American Astronomical Society • Provided by the NASA Astrophysics Data System HENRY C.FERGUSON:THEFORNAXCLUSTER d) MorphologicalType(Column5) c) MembershipStatus(Column4) Table V.Sourcesofgalaxyparameters. codes. Table IV.Cluster-membership Code Meaning Literature sourcesformagnitudes 4 likelybackground 2 likelymember 6 likelyplateflaw 3 possiblemember 5 definitebackground 1 definitemember Plate material -2 the classification,asdescribedinSec.IVgbelow. cluster membersinTableIIontheLasCampanasplates, bright E’sfromSO’s.Second,forfaintergalaxies,the where possible.Thenotesincolumn9indicatethesourceof these reasons,wehavebasedourclassificationsoflikely tures necessaryfordistinguishinglow-surface-brightness from theSRCplatewereperformedbyauthoralone,and and cluster-membershipclasswasadopted.Classifications re-examination oftheimage,anintermediateHubbletype bandpass havebeenconvertedtoBmagnitudesbyapplying dwarf ellipticalsfromirregularsandbackgroundspirals.For low spatialresolutionoftheSRCplatewashesoutfea- galaxy fromabackgroundelliptical,ortodifferentiate ample, todistinguishahigh-surface-brightnessclusterBCD SRC platesaturatesatarelativelylowsurfacebrightness must beregardedaslessreliablefortworeasons.First,the of brightgalaxies.Thismakesitextremelydifficult,forex- ors assignedtothegalaxiesaccordingGriersmith the BlairandGilmore(1982)passbandcorrection,withcol- the colorcorrectionswill,ingeneral,belessthan0.1mag. SRC platedata,whereavailable.MagnitudesfromtheIIIa-J in 0.3mag.Theprincipalverificationcamefromacompari- literature (seePaperI)showedageneralagreementtowith- Fornax Cluster.Thiscomparisonfor42galaxiesyieldedthe from CaldwellandBothun(1987)fordwarfgalaxiesinthe son ofourSRCplatemagnitudeswithCCDphotometry Comparison tophotoelectricandCCDphotometryfromthe ples: following linearrelationbetweenthetwophotometricsam- ( —20.55arcsec),eliminatingallcontrastinthecenters ( 1982)color-magnituderelation.Theerrorsintroducedby where JreferstotheIIIa-Jbandpassinwhichcompari- U.K. SchmidtplatewithaCambridgeAPMmachine.Our number ofgalaxiesintheregionbasedonmeasurementsa mag. Daviesetal.(1988)havepublishedmagnitudesfora magnitude systemsis0.2mag,withanrmsdeviationof0.3 son wasmade.ThemeandifferenceSBbetweenthetwo magnitudes agreewellwiththeirsforthe176galaxiesin catalog. UsingtheSRCplatephotometry, rwasmeasured rated ontheSRCplate.Forthesegalaxies,wehavetaken for therelationbetweenthem. linear least-squaresfityields cating apossiblescaledifferencebetweenthetwosystems.A 0.34 mag.Thereisaslightcorrelationoftheresiduals,indi- common, withameanAi?of0.09magandanrmsscatter magnitudes fromtheliterature,asindicatedincolumn8. have beenestimatedbycomparingthemtogalaxiesinthe that fallofftheSRCplate.Magnitudesforthesegalaxies center oftheclusterforwhichSRCmagnitudeshavebeen appears tobeclosethatattained bythedigitalphotome- computed. Theaccuracyoftheseeye-estimatedmagnitudes try. T e x Total magnitudeshavebeencomputedfromthedigitized Bj(CB) =(1.10±0.02)5(SRC)-1.37+0.38, i? (Daviesetal.)—1.14i?(SRC)—2.37 y The effectiveradiusrislisted formostgalaxiesinthe There areanumberofgalaxiesattheedgessurvey Cluster membersbrighterthan~13.5i?arelargelysatu- T e f) EffectiveRadii(Column7) e) Magnitudes(Column6) 399 400 HENRY C. FERGUSON: THE FORNAX CLUSTER 400 from the growth curve that was used to compute the total indicate the appearance of the galaxy on either the SRC plate magnitude. It was taken to be the radius of a circular aper- or the Las Campanas plate. ture containing half of the total flux from each galaxy. These The ones digit of the code in column 9 indicates the plate effective radii are not expected to be terribly precise, because material for this survey, as shown in Table V. Galaxies with a of the small sizes of the galaxies, the low precision of the total 3, 4, or 5 in this column have been classified on the Las magnitudes, and the low resolution of the SRC plate. None- Campanas plates. The SRC plate emulsion was often satu- theless, they may be useful for statistical purposes, because rated at the centers of the images of bright galaxies, making they have been measured for a large number of galaxies. An photometry more difficult and less accurate. Thus, we have indication of their accuracy can be obtained by comparison also indicated whether or not the saturation density was with CCD photometry from Caldwell and Bothun ( 1987). reached in the galaxy image. These authors derived effective radii from fits of ellipses to Where possible, the positions of the galaxies were deter- the isophotes of the galaxies in their sample. They have thus mined from the SRC plate. If photometry of the galaxy was explicitly taken galaxy flattening into account, while we not possible on the SRC plate ( i.e., the galaxy was too bright, have accounted for it implicitly by using circular apertures. too near a bright star, or off the plate), positions were taken The results would therefore differ slightly from ours even if from the literature, as indicated in the notes in column 13. If the photometry in both cases were perfect. The relation accurate positions were not available in the literature, they between the two sets of effective radii is shown in Fig. 3. For were measured from the Las Campanas plates. 42 galaxies in common between the two surveys, we find a Where possible, magnitudes were obtained from the SRC mean Are of 0.7", with an rms scatter of 3.54". For these plate photometry. Because the photometry is less precise for small galaxies, the scatter amounts to —25% of the effective galaxies where the emulsion was saturated, we have noted radius. A linear least-squares fit to the relation between the whether or not this occurred. We have listed magnitudes and effective radii in the two systems yields effective radii for the bright galaxies where these data were r (CB) = (0.82+ 0.11)^ (SRC) + 1.78 + 1.60. available in the literature. The sources of these data are e shown in the tens digit of column 9, and are interpreted in Effective radii for galaxies that were too bright for SRC Table V. plate photometry were taken from the literature. Table VI summarizes the order of preference for the var- ious sources of the data in columns 1-8. g) Sources of Galaxy Parameters (Column 9) Each galaxy in the catalog appeared on at least one plate. h) Diameters (Column 8) However, a number of galaxies at the edges of the survey Diameters were measured from the digitized data, where region appeared either only on the SRC plate or only on the possible, and were otherwise estimated from the Las Cam- Las Campanas plate. We have set the codes in column 9 to panas plates. To compute the isophotal diameter from the

Fig. 3. Comparison between effective radii derived from the SRC plate photom- etry and effective radii from the CCD pho- tometry of Caldwell and Bothun ( 1987). The solid line is the expected result if they were identical, the dashed line shows the best fit to the points in the figure.

© American Astronomical Society • Provided by the NASA Astrophysics Data System 1989AJ 98. .367F -2 -2 401 HENRYC.FERGUSON:THEFORNAXCLUSTER brightness profilewassmoothedwitha3"runningmean,to function ofradiusin1"-widecircularannuli.Thissurface- found fromthissmoothedprofile.Aswasthecasefor SRC plate,wecalculatedthemeansurfacebrightnessasa precise. CaldwellandBothun(1987)listdiametersfor reduce theeffectsofnoiseslightly.ThediameterDwas ies fallexponentiallythroughthetwoisophoteslistedbyCB assumed thatthesurface-brightnessprofilesforthesegalax- comparison withourdiametersat26.5Barcsecwehave dwarf galaxiesatisophotesof25and27Barcsec.For effective radii,thediametersmustberegardedasfairlyim- The relationbetweenourdiametersandthosecomputed from theCBdataisshowninFig.4,andbestfitby and haveinterpolatedalongtheexponentialtofindD. Membership Positions SRCplate. 26 5 Type 26 5 B SRCplate. Diameter r SRCplate. t e © American Astronomical Society • Provided by the NASA Astrophysics Data System Table VI.Orderofpreferenceforgalaxyparameters. Velocity. Las Campanasplates. Literature asindicatedinnotes(wheremoreaccuratethan15"). Las Campanasplates. Las Campanasplates. Las Campanasplates. Literature asindicatedincolumn9. SRC plate. Literature (sameasBt). SRC plate. Las Campanasplates. SRC plate. between oureye-estimateddiametersandthe ation intheresidualsfromlinearrelationshownaboveis in TablesIIandIIItoaccountforthisoffset.Thermsdevi- face brightnesses.Wehavenotcorrectedthediameterslisted cating aslightdifferenceinourcalibrationsattheselowsur- Our diametersareonaverage14%largerthantheirs,indi- diameters aresubjecttoacertainamountofsubjectivebias, ters fromtheSRCplate,wemeasureddiameterson the numberslistedinTablesIIandIII. ter, magnitude,andsurfacebrightnessofthegalaxy.The measured. Theresultingcalibrationdependsonthediame- computed fromtheSRCplateforgalaxieswherebothwere which wehaveattemptedtocalibratebyfindingtherelation Las Campanasplatesbyeyeusingamagnifiedreticle.These the calibrationtooureye-estimateddiametersproduce scatter aboutthisrelationis7.5",or22%.Wehaveapplied relation betweenourcalibrated,eye-estimatedZ>diame- means ofindependentmeasurementsfromseveraldifferent ters andtheSRCdiametersisshowninFig.5.Therms observers, withtheuncertaintiescompoundedfrom from thecompilationofRichterandSadler(1985),where The codingofthevelocitysourceslistedincolumn12isas galaxies notlistedbyRichterandSadlerarealsoincluded. quoted errorsofthedifferentsources.Velocitiesforafew they were,forthemostpart,derivedfromweighted 13.4 arcsec,whichamountsto16%,onaverage. 26 5 D (SRC)=(1.03+0.01)D'(CB) For galaxieswhereitwasnotpossibletoestimatediame- The heliocentricvelocitieslistedincolumn10aremostly 26 5 i) Velocities(Column10) + (8.094.58). ameters derivedfromtheCCDphotome- of diameterswereidentical;thedashed solid lineistheexpectedresultiftwosets try ofCaldwellandBothun(1987).The ameters A6.5fromtheSRCplateanddi- Fig. 4.Comparisonbetweenisophotaldi- figure. line showsthebestfittopointsin 401 402 HENRY C. FERGUSON: THE FORNAX CLUSTER 402

Fig. 5. Comparison between diameters de- termined from the Las Campanas plate and isophotal diameters from the SRC plate. Las Campanas diameters measured with a reticle from the plate have been em- pirically calibrated so that, on average, they match the Z>26 5 isophotal diameters. The figure shows the scatter left in the di- ameter measurements after the calibration has been applied.

follows: 1 = Richter and Sadler (1985), 2 = Jones and tive nature of galaxy classification, it is possible that certain Jones ( 1980), and 3 = Lauberts ( 1982). The galactocentric classes of cluster members may actually masquerade as velocities listed in Ref. 2 have been converted back to helio- background galaxies, while other classes of background gal- centric velocities so that they are consistent with the rest of axies may appear to be cluster members. Such misclassifica- the catalog. tion can most obviously occur in the case of compact (M32- like) elliptical galaxies, which would most likely be j) Notes (Column 13) relegated to the background, and in the case of low-surface- Additional notes for a few galaxies are indicated in col- brightness background spiral galaxies, which appear similar umn 13. The meaning of these notes is as follows: to nucleated dE or dSO galaxies. ( 1 ) Galaxy position taken from Jones and Jones ( 1980). While radial velocities, and hence definitive measures of (2) Contamination from a nearby star may affect the cluster membership, are available only for the brightest gal- magnitude estimate. axies in this catalog, some information on cluster member- ( 3 ) The nucleus is displaced from the center of the galaxy. ship can be extracted from the distribution of galaxies on the (4) Globular clusters appear to be visible around this gal- sky. In particular, we may use this distribution to set con- axy. We did not explicitly search for globulars; absence of straints on the maximum and minimum allowed number of this note should not be taken to mean that the galaxy has no cluster members in a given subset of the catalog. To do this, globular clusters. This note is included because globular we model the spatial distribution as a King (1962) model clusters around dwarf ellipticals may be of potential interest cluster-density profile superimposed on a uniform back- in future investigations. ground, and we allow the contributions of the two compo- ( 5 ) Galaxy appears to have multiple nuclei. nents to vary to find the best fit and the allowed range. Before fitting such a two-component model, we first need k) Names (Column 14) to find the cluster center and estimate its characteristic radi- us. We shall briefly discuss our selection of these parameters, while reserving a detailed discussion of the cluster morphol- As many names as will fit in the space allotted are shown ogy to Paper III. To determine the cluster center and core for each galaxy. If more names are known, the order of pre- radius, we have fit to the galaxy spatial distribution a King ference is as follows: NGC, IC, ESO, G (Jones and Jones model of the form 1980), HPW (Hodge, Pyper, and Webb 1965), NG (Cald- well 1987), MCG, D (Duus 1979). V. SPATIAL DISTRIBUTIONS OF GALAXIES leaving rc and the position of the cluster center (a0,<50) as Selection of cluster members on the basis of morphology free parameters, and adjusting the central surface density 70 alone is clearly a biased process, and is subject to selection such that the total number of galaxies produced by the fit effects that are not easily quantifiable. Because of the subjec- equals the number observed in the same area of sky.

© American Astronomical Society • Provided by the NASA Astrophysics Data System 1989AJ 98. .367F o hm S= —2lnLandweminimizeS.Parameterspaceis parameters canbeobtainedfromthepropertythat,in searched viathedownhillsimplexalgorithm(Neiderand find themaximumlikelihood,wedefinestatistic plates; theentirefitisrestrictedtoaregionofradius4.6°.To the numberofparametersthatareheldconstantattheirtrue limit oflargeN,theSstatisticisdistributedasx]>whereg and isrestrictedtoregionsoftheskythatfallonsurvey The integralinthedenominatorisevaluatednumerically distance roftheTVgalaxiesfromclustercenterata,0is technique similartothatdescribedbyMalumuthandKriss values (Cash1979). Mead 1965).Estimatesofconfidenceintervalsforthefitted 403 HENRYC.FERGUSON:THEFORNAXCLUSTER axies, andtheirdistributionprobablydoesnotfollowaKing for tworeasons.First,thelate-typegalaxies(spiralsand The best-fitcoreradiusislikelytobeaslightoverestimate from thissample,itfallswithinthe99%confidencecontour. not coincideexactlywiththebestfitforclustercenter circle of0.2°radius.WhilethepositionNGC1399does and the99%confidencecontourforcenterisroughlya dence intervalforthecoreradiusextendsfrom0.5Ito1.01°, profile. Second,anycontaminationbybackgroundgalaxies of 0.72°,andiscenteredat35,—35°43.The99%confi- Im’s) arelesscentrallyconcentratedthantheearly-typegal- ( 1986).Inourcase,thelikelihoodLofobtainingradial tQ0 /rg|S2 The modelfittingwasdoneviaamaximum-likelihood L=T\ (,’c’o,o)(”)afr The bestfitforallgalaxiesinTableIIhasacoreradiusr © American Astronomical Society • Provided by the NASA Astrophysics Data System c 1 '.= fK™‘i(r,a,0)(2Trr)dr ric0 -.5 O .5 Likely clustermembers Log(r) (degrees) core radiusof0.67°.Themaximumnumberbackground in theclustersamplewillincreaseapparentcoreradius as 0.6°.Themainpurposeofdisplayingthissamplehereisto galaxies allowedwithinthe99%confidencerangeis26,or Fig. 7.Thebestfithasnobackgroundgalaxies,anda the coreradiusofclusterforrestthisdiscussion. ple. Thebestfithasacoreradiusof0.7°,whichweadoptas dence—“3cr”) numberofbackgroundgalaxiesinthesam- we adoptaslightlysmallercoreradiusforthecluster,but a single-componentfit.Fromthetwo-componentfitsbelow, could alwaysfitaflatbackgrounddistributionwithKing galaxies, wenowholdthecoreradiusfixed(becauseone without requiringacorrectionforbackgroundgalaxies. show thatthissubsetofthecatalog,definedpurelyonmor- models givingthemaximumandminimum(to99%confi- ies. Thebest-fitmodelisshowninFig.6,alongwiththe adjusted sothatthefitproducescorrectnumberofgalax- degree. ThefreeparametersarerandC,/isonceagain core radiusoflessthan0.2°. results ofthissectionareratherinsensitivetochangesinthe phological grounds,canbewellfitbyourclustermodel so thatICisthenumberofbackgroundgalaxiespersquare spatial distributionas fit, wenowaddauniformbackgroundandmodelthegalaxy 11 %ofthesample,ifcoreradiusisallowedtogoaslow c0 0 The fittothedwarfellipticalsfromTableIIisshownin I(r) =I To searchforaclustercomponentamongthebackground Taking thecenterdeterminedfromsingle-component 0 2 [\ +(r/r)] c 1 bined distribution,whilethelighterlines cluster model,”i.e.,themodelwith fit, whichhasnobackgroundcontribu- The variouslinesshowtheresultoffitsto binned data. are binnedfordisplaypurposesonly.The the bestfit.Theheavylineshowscom- lowed withinthe3aconfidencelimitsof minimum numberofclustermembersal- tion. Thedottedlinesshowthe“minimum ground. Thesolidlineindicatesthebest a two-componentmodelconsistingof cating thepossibilityofy¡Ñfluctuations. least tengalaxies,withtheerrorbarsindi- maximum-likelihood techniqueontheun- model fittingwasperformedusing the that thedatainthisandfollowingplots show theindividualcomponents.Note King profileclusterandauniformback- the cluster.Eachannularbincontainsat the distance,indegrees,fromcenterof and thehorizontalaxisislogarithmof lowing figures,theverticalaxisisloga- Fig. 6.Radialsurface-densityprofileofall rithm ofthegalaxiespersquaredegree, likely clustermembers.Inthisandthefol- + C 403 1989AJ 98. .367F The agreementisworseifoneconsidersthattherearealso50 thus appearstobeconsistentwiththeclusterclassifications. best fitrequires158clustermembers,andtheallowedrange fied 242early-typegalaxiesaslikelyclustermembers.Thefit is from61to293members.Withinthisregionwehaveclassi- sample ofallgalaxiesinthisregionisshownFig.8.The quired thatthegalaxiesfallonSRCplate.Acomplete Figs. 8-14.Inordertohaveauniformsample,were- range ofC.TheresultsaresummarizedinTableVIIand model ofinfinitecoreradius),andexaminetheallowed 404 HENRYC.FERGUSON:THEFORNAXCLUSTER O © American Astronomical Society • Provided by the NASA Astrophysics Data System All members334 All galaxies2339158 Bkgd galaxieswith<££> .<24.5 10680_ Bkgd galaxieswith<££?> .5>25 2140 Bkgd galaxieswith<££?>6.5>24.5 9780 Possible compactEandSO(class 3)305 E andSO(class3+4) 338 0 Possible members(class3)1369 Background (class3-5)20460 dE anddSOmembers243 26 6 26 2 -.5 0 Subset dE anddSOgalaxies Log(r) (degrees) Table VII.Resultsoftwo-componentmodelfits. N ^duster Best ute significantlytotheapparentclustercomponent. axies haveamuchflatterdistributionandwouldnotcontrib- late-type clustermembersintheregion;however,thesegal- members inoursurveycouldhavebeenmisclassifiedas criteria. Inparticular,nomorethan15%ofthecluster could havebeenexcludedbyourmorphologicalselection tight constraintonthenumberofclustermembersthat and nomorethan45areallowed.Alreadythissetsarather shown inFig.9.Thebestfitproducesnoclustermembers, fit The distributionofbackgroundgalaxies(classes3-5)is Nbkgd 2046 2181 1068 214 978 338 127 25 .5 0 0 Max. Background ^cluster Nbkgd 217 286 61 0 0 0 0 0 0 0 bined cluster+backgrounddistribution, background. Themaximumsurfaceden- of theindividualcomponents. and thelighterlinesshowcontribution The heavydottedlineindicatesthecom- ground” fitisshownasthedottedline. per squaredegree.This“maximumback- in thecontextofthismodelis0.5galaxies sity ofbackgroundgalaxiesallowedwith- component, withnocontributionfromthe the solidline,isapureKingmodelcluster and dSOgalaxies.Thebestfit,shownas Fig. 7.RadialdensityprofileofclusterdE 2046 2278 1068 214 978 338 136 30 48 26 Nçiugter Nbkgd Max. Cluster 293 243 334 49 29 34 20 23 39 45 2001 2046 1019 944 315 185 97 10 0 0 404 1989AJ 98. .367F 405 HENRYC.FERGUSON:THEFORNAXCLUSTER o 00 © American Astronomical Society • Provided by the NASA Astrophysics Data System 2.5 1.5 2 1 -.5 0 Likely backgroundgalaxies Complete sample Log(r) (degrees) .5 dotted linesshowthemaximumcluster meanings ofthedifferentcurvesareasfol- plete samplefromTablesIIandIII.The background components. imum clustermodel;theheavylinesindi- model, andthedashedlinesshowmin- lows: thesolidlinesshowbestfit, Fig. 8.Radialdensityprofileofthecom- lines indicatetheindividualclusterand cate thecombinedprofile,andlighter tains noclustermembers.Codingforthe curves isthesameasinFig.7. ies inTableIII.Thebest-fitmodelcon- Fig. 9.Radialdensityprofileofallgalax- 405 1989AJ 98. .367F 406 HENRYC.FERGUSON:THEFORNAXCLUSTER © American Astronomical Society • Provided by the NASA Astrophysics Data System -.2 0.2 .4.6 E andSOgalaxies(classes34) Possible clustermembers Log(r) (degrees) more than~20areallowed.Codingfor to explaintheradialdistribution,andno show thatnoclustermembersareneeded fall intothissubset.Theresultsofthefit the curvesissameasinFig.6. type galaxiesinthecluster,theywilllikely If thereisasignificantpopulationofM32- SO galaxiesinmembershipclasses3and4. Fig. 11.RadialdensityprofileofallEand Fig. 6. The codingforthecurvesissameasin cluster members(membershipclass3). ies inTableIIIthatarelistedaspossible Fig. 10.Radialdensityprofileofallgalax- 406 1989AJ 98. .367F 407 HENRYC.FERGUSON:THEFORNAXCLUSTER © American Astronomical Society • Provided by the NASA Astrophysics Data System Low—surface—brightness backgroundgalaxies -.5 E andSOgalaxies(class3) Log(r) (degrees) O .5 2 judged morelikelytobeclustermembers, are fewergalaxiesinthissubsetthan axies inmembershipclass3.Whilethere ness andtheircontrastwiththesurround- on thebasisoftheirhighsurfacebright- Fig. 10,thegalaxiesplottedherewere Fig. 12.RadialdensityofallEandSOgal- ing background.Becauseofthesmall in densitytowardtheclustercenteris number ofclustermembersarenobetter number ofgalaxies,theconstraintson curves isthesameasinFig.6. somewhat suggestive.Codingforthe than inthelargersample,althoughrise tribution withnoclustercomponent.Cod- background galaxiesfromTableIIIwith ing forthecurvesissameasinFig.6. are bestfitbyauniformbackgrounddis- fainter than24.5magarcsec~.Thedata mean surfacebrightnesswithinD Fig. 13.Radialdensityprofileoflikely 265 407 1989AJ 98. .367F 408 HENRYC.FERGUSON:THEFORNAXCLUSTER basis oftheshapeluminosity profile,spiralfeatures, magnitudes. Theresultsofthetwo-componentfitareshown in Fig.12.Thebestfitincludesfiveclustermembers,butthe clusters, theirhighsurfacebrightnesses,andbrighter candidates, byvirtueoftheirisolationfrombackground this sample,30galaxiesappearedtobeparticularlygood by thefit.Thissetsaquantitativelimitonfaintendof association withanobviousbackground cluster,etc.Thereis for theFornaxClusterdwarfs, and mustbeexcludedonthe galaxies overlapthesurface-brightness-magnitude relation not auniqueindicatorofcluster membership.Background luminosity functionofhigh-surface-brightnessellipticals.Of with noclustermembers.Atmost,23membersareallowed 3cr constraintsarenobetterthan forthelargersample. shows thattheirspatialdistributionisbestfitbyamodel hiding amongthebackgroundellipticals.Wehaveclassified the faintestofthesehasaluminositywellabovelimits background galaxies.Figure10showsthedistributionof or likelybackgroundgalaxies(classes3and4).Figure11 our survey.IfthereareadditionalcompactE’s,theywillbe ed intheFornaxCluster(WirthandGallagher1984),but ter members,butnumbersbetween0and39areallowed. high-surface-brightness ellipticalsthatcouldbeM32-type reason oranotherdonotappeartobedE’s,areisolated these areeitherlow-surface-brightnessgalaxiesthatforone galaxies thatwehaveclassifiedaspossiblemembers.Mostof galaxies. Thebestfittothespatialdistributionhasnineclus- 338 EandSOgalaxiesontheSRCplateaspossiblemembers We arguedinPaperIthatsurface brightness,byitself,is A fewM32-likecompactellipticalshavealreadybeennot- © American Astronomical Society • Provided by the NASA Astrophysics Data System -.2 O.2.4.6 Lower—surface—brightness backgroundgalaxies Log(r) (degrees) o o -2 -2 the annulioutside Ifallabovethemean.This isexactlythe the clustercenterfallbelow meandensity,whilemostof toward theclustercenter;majority ofpointswithinI density ofbackgroundgalaxies actuallyappearstodecrease lation oftheclusterdwarfs. minosity functionandthesurface-brightness-magnitude re- significantly affectourconclusionsinPaperIaboutthelu- surface-brightness rangeby,atmost,17%,andwouldnot background sample.Weobtainsimilarresultsifwesetthe ter members,itwouldexclude12%ofthedEanddSOgalax- surface brightnesseswithin^26.5arefainterthan24.5 objects. InFig.13,weshowonlythosegalaxieswhosemean members. Thiswouldincreasetheclusterpopulationinthis there couldbe,atmost,29additionallow-surface-brightness brightness cutoffwouldexcludeallEandSOgalaxies,81% mag arcsec.IfthislimitwereappliedtotheFornaxClus- sample. Wenowlimitthissampletolow-surface-brightness members thatcouldbelurkinginourcompletebackground mold. Wehavesetlimitsaboveonthenumberofcluster brightness-magnitude relationandhavethusarbitrarilyex- dSO galaxies.Theresultsfromthefit(Fig.14)suggestthat of thespirals,38%irregulars,anddE threshold at(SB)>25magarcsec.Thissurface- that therearefew,ifany,clustermembersmixedinwiththis cals andSO’s.Theresultsfromthetwo-componentfitsshow ies, 47%ofthespiralsandirregulars,91%ellipti- cluded fromtheclustergalaxiesthatdonotconformto oped apersonalbiastowardsgalaxiesthatfallonthesurface- always theworry,however,thatwehavesomehowdevel- 265 A somewhatsurprisingfeature ofFigs.9-15isthatthe -2 same asinFig.6. ies overlap.Codingforthecurvesis the clusterdwarfsandbackgroundgalax- in therangeofsurfacebrightnesswhere inating againstbackgroundgalaxies,even selection criteriaareeffectiveindiscrim- background galaxiesfromTableIIIwith ure demonstratethatourmorphological results shownhereandinthepreviousfig- are bestfitbyauniformbackgrounddis- fainter than25magarcsec.Thedata tribution withnoclustercomponent.The mean surfacebrightnesswithinZ> Fig. 14.Radialdensityprofileoflikely 265 408 1989AJ 98. .367F o o independent oftheirpositionin thecluster.Itisnonetheless classification ofbackgroundgalaxies.Clustermembership obscuration. Incomparison,thereisa20%differenceinthe conceivable thatsomebiasmight creepintowardthecluster of thegalaxieswasdecidedonbasistheirmorphology, central Iandtheouterregions. density ofbackgroundgalaxiesshowninFig.9betweenthe in thisisophote,islikelyanupperlimitontheamoutof surface-brightness backgroundgalaxiesarestillvisiblewith- all clustermembersinthecentralI.Thisturnsouttobe ies, wehaveaddeduptheareawithinZ>isophotesof cribed simplytogeometricobscurationbyforegroundgalax- cluster membersinthebackground,orifvignettingon opposite ofwhatonewouldexpectiftherewereadditional more stronglyinthedistribution oflow-surface-brightness center, asonestartstoseeahigher concentrationofgalaxies. tribution ofbackgroundgalaxies. the intergalacticmedium;orlarge-scalestructureindis- of galaxiestowardtheclustercenter;extinctionbydustin decrease: obscurationofbackgroundgalaxiesbybrightgal- vey. tion. About75%ofthegalaxies intheclusterhave(SB) galaxies, becausetheseconstitute mostoftheclusterpopula- axies inthecenterofcluster;systematicmisclassification SRC platewereaffectingthecompletenesslimitofsur- If suchmisclassificationwere a problem,itwouldappear 409 HENRYC.FERGUSON:THEFORNAXCLUSTER 10% ofthetotalareaskywithinthisregion.Becausehigh- Normal andhigh—surface—brightnessbackgroundgalaxies 26 5 It isunlikelythatthedecreasecanbeduetoselectivemis- To estimatetheportionofthisdecreasethatcanbeas- A numberoffactorscouldpotentiallyaccountforthis © American Astronomical Society • Provided by the NASA Astrophysics Data System background galaxies. in thedistributionsofbothhigh-andlow-surface-brightness show thatthedeclinetowardsclustercenterisapparent greater than24.5withinD.However,Figs.13and15 crease inthedensityofbackgroundgalaxies.Foracomplete galaxies willhavetheform magnitude-limited survey,themagnitudedistributionof amount ofextinctionrequiredtoproducetheobservedde- interesting possibility.Wecanmakeacrudeestimateofthe intracluster mediumisveryshort (BurkeandSilk1974;Bar- small, bothbecausethelifetime ofgrainsembeddedinahot probably anoverestimateofthe amountofobscurationby extinction couldbeslightlylower. Ontheotherhand,10%is would fallbelowourthreshold. Thustheactualvalueof if itfollowedastandardgalacticextinctioncurve.Because foreground galaxies. lost duetoextinctionbecausetheirapparentdiameters our surveyisdiameterlimited,additionalgalaxieswouldbe the Bband.TheextinctioninFbandwouldbe0.06mag, we needanextinctionof0.08mag.Thisisthein For a10%reductioningalaxycounts(assumingtheother 26 5 (ignoring variouscosmologicalcorrections).Ifwehave^4^ 10% comesfromobscurationbyforegroundgalaxies),then, mag ofextinction,thenweexpecttofind logAfm) =logN(m)—0.6A. log N(m)=0.6m+const. The extinctionduetodustin clusters isexpectedtobe Obscuration bydustintheintraclustermediumisamore 0B 0 -2 brighter than24.5magarcsec.Once background galaxiesfromTableIIIwith background distributionwithnocluster again, thedataarebestfitbyauniform mean surfacebrightnesswithinZ) Fig. 15.Radialdensityprofileoflikely same asinFig.6. component. Codingforthecurvesis 265 409 410 HENRY C. FERGUSON: THE FORNAX CLUSTER 410 [u KOr" ^ low 1978; Draine, and Salpeter 1979), and because the uni- Fig. 16. The contour plot shows the density of galaxies from œ verse is known to be optically thin out to large redshifts. The Table II, while the grey scale reflects the density of back- only reported detection of intergalactic dust was by Kara- ground galaxies, with darker regions signifying higher densi- chentsev and Lipovetskii (1969), who found AB ties. There is clearly a decrease behind the cluster. Indeed, ^ = 0.22 + 0.05, from counts of distant clusters behind near- the galaxy surface density varies by a factor of 2 over the g by Zwicky clusters. They also pointed out that one can es- region surveyed. However, the position of the minimum 2 cape the problem of large optical depths at high redshift by does not coincide with the cluster center, and the back- postulating that the dust has a nonprimordial origin, and ground distribution in general gives the impression of being thus has a density that varies with redshift. Indeed, it is most clumpy. It thus appears that the decrease in background reasonable to suppose that the dust, if present, comes from counts toward the center of the Fornax Cluster is most likely material injected into the intracluster gas by the cluster gal- due to large-scale inhomogeneities in the galaxy distribution axies. From such considerations, Hu, Cowie, and Wang behind Fornax. Because of the dumpiness of the back- (1985) estimated the dust density one might expect in a rich- ground-galaxy distribution, it is not possible to set interest- cluster cooling flow tobe 10-32 g cm-3, a result that is sensi- ing limits on the dust content of the intergalactic medium tive to models for galaxy evolution, as well as to the tempera- from this survey. However, it is likely that good limits could ture and density of the intracluster gas. The reddening be obtained from a deeper survey of the region, where the inferred from this model is EB_ v = 0.02(R /10 Mpc), background-galaxy distribution should be more uniform, where R is the radius to which the intracluster gas extends. and contribution to the galaxy counts from the cluster The infrared luminosity from this dust would be too faint should be negligible. (by about an order of magnitude) to have been detected by IRAS. Application of this result to the Fornax Cluster is difficult because the x-ray emission observed by the Einstein VI. CROSS REFERENCES TO OTHER CATALOGS IPC (Killeen and Bicknell 1988) is concentrated on the two galaxies NGC 1399 and 1404, and does not extend far out This section presents cross references to several previous into the cluster. Given the small number of galaxies in the catalogs of the Fornax Cluster. Table VIII shows the galax- cluster and its low velocity dispersion, one would expect that ies from Hodge, Pyper, and Webb ( 1965 ) that we believe we any gas that does pervade the cluster would have a lower have identified in our survey. These authors list positions to temperature than in rich clusters, allowing longer grain life- a precision of 1.5 arcmin, and often there was no obvious times. correspondence to a galaxy in our catalog. Identifications for In order to assess whether the decrease is really associated the galaxies with question marks in Table VIII are less cer- with the cluster, we display the galaxy counts graphically in tain than those without.

D E Fig. 16. Isopleths based on galaxy counts C from Tables II and III. The contours show L the density of cluster members at intervals I of ten galaxies per square degree. The posi- N tions of the individual cluster galaxies are A marked with + signs. The grey scale T shows the density of background galaxies, I which varies from 30 to 150 galaxies per 0 square degree, with darker regions indi- N cating higher densities. The image was constructed by counting galaxies in 0.7° X 0.7° cells, separated by 1.4', and then smoothing these cells with an 11 cell run- ning mean.

03 50 45 40 35 30 25 RIGHT ASCENSION © American Astronomical Society • Provided by the NASA Astrophysics Data System 1989AJ 98. .367F most ofwhichappeartobeclustermembers,basedonour membership. TableIXshowstheFCCnumbersforallof on alistthatCawson(1984)compiledfromAPMmachine a copyoftheSRCskysurvey/plate,field#358,andbased classified asdwarfs(seeTableX)basedonhisinspectionof galaxies intheirsurvey. galaxies intheirsurveyforthepurposeofconfirmingcluster scans ofaplatethesamefield.Thecataloglists137entries, III-aJ Schmidtplate.Theyobtainedspectraformostofthe Cluster, completetoi?=16.0mag,basedoninspectionofa 411 HENRYC.FERGUSON:THEFORNAXCLUSTER Jones and(1980)publishedasurveyoftheFornax Caldwell (1987)presentedacatalogofgalaxiesthathe © American Astronomical Society • Provided by the NASA Astrophysics Data System Jones HPW HPW 12? HPW 11 HPW10 HPWI? HPW14 HPW13 HPW15 G10 G12 HPW9 G14 HPW 8 HPW7 HPW6 HPW5 HPW3 G18 G24 G22 G20 G26 G25 G23 G21 G28 G29 G32 G31 G45 G43 G46 G51 G47 G8 G4 G9 B1129 B1005 B0990 B1104 B0476 FCC 204 139 152 255 282 288 315 203 119 153 135 106 43 63 88 76 53 55 B0727 B0747 B0789 B0755 B0576 B0084 B0793 FCC 100 102 82 68 85 3 Jones Table VIII.DwarfsfromHodge,Pyper,andWebb(1965). Table IX.GalaxiesfromJonesand(1980). FCC HPW27? HPW HPW22 HPW25 HPW24 HPW23 HPW21 HPW20 HPW19 HPW29 HPW26 HPW17 HPW31 HPW28 i? =16thatwerenotlistedbyCaldwell.Theradialdistri- includes 131additionallikelyclustermembersfainterthan Virgo isnotstronglysupportedbyourdata. bution oftheseadditionaldwarfscomparedtoCaldwell’s other catalogs.Itisworthnoting,however,thatourcatalog survey. Caldwellalsolistsanadditionaleightdwarfsfrom tio forearly-typegalaxiesismuchsmallerinFornaxthan particular, Caldwell’sconclusionthatthedwarf-to-giantra- dwarf ratioandluminosityfunctionneedtobemodified.In the cluster,thenCaldwell’sconclusionsaboutgiant-to- the same.Iftheseadditionaldwarfsareindeedmembersof dwarfs isshowninFig.17;thedistributionsareessentially T Jones G100 G101 G102 G103 G105 G104 G109 G108 Gill G114 G113 G87 G86 G89 G88 G91 G93 G92 G97 G94 G99 G98 G95 B1195 B1335 FCC F12 230 208 206 243 223 201 181 128 195 188 B0407 B2095 B0942 B0827 B0713 B2025 B1570 FCC 332 335 100 301 290 193 136 179 308 310 285 176 95 67 47 32 HPW34? HPW44? HPW43? HPW41? HPW36? HPW HPW39 HPW37 HPW33 HPW45 HPW42 HPW38 HPW32 HPW46 Jones G119’ Gl37a G137b G118 G117 G119 G122 G121 G120 G126 G129 G128 G127 G131 G130 G135 G139 G142 G150 G146 G153 G159 G157 B0868 B0933 B1956 B0186 B0192 B0255 B1317 B0897 B1686 B1921 B1532 FCC FCC 121 249 324 338 116 316 305 296 274 267 318 266 255 250 256 90 37 39 62 22 29 33 21 28 26 411 1989AJ 98. .367F 412 HENRYC.FERGUSON:THEFORNAXCLUSTER central 1.7core radii ofFornaxand6.83+0.87 forthecen- it, wefindadE+dSO/ESO ratioof4.65+1.07forthe not distinguishbetweendE’sand dSO’s.Usingthesamelim- Fornax and6.01forVirgo(for B<18.25).Caldwelldoes the same.CaldwellreportedadE/(E -fSO)ratioof1.93for degree ofconfidence,rejectthe possibility thattheratiosare ference intheratiotwoclusters, wecannot,withahigh nax andVirgoclusters.Whiletheredoesappeartobeadif- In PaperIweshowedthedwarf/giantratiosforFor- © American Astronomical Society • Provided by the NASA Astrophysics Data System NG4 NG3 NG2 NGl NG6 NG5 Caldwell NG7 NG8 NGll NG10 NG9 NG12 NG13 NG14 NG15 NG16 NG17 NG18 NG19 NG20 NG21 NG22 NG23 NG24 NG25 NG26 NG27 NG28 NG29 NG30 NG31 NG33 NG32 Notes: 2. NG86andNG110werejudgedtobeplateflawson the SRCplate.Theywerenotvisibleon 3. NG94andNG136donotfallnearthepositionsof anydwarf-likegalaxiesinoursurvey. 1. ThepositionreportedforNG36mostcloselycorrespondstoabackgroundellipticalwith is possiblethatwehavecataloguedthesameplateflaw. the LasCampanasplates.BecauseCaldwell’ssurveywas also basedonSRCplatecopies,it diameter of15.8",belowthelimittableIII. in hissurvey. Caldwell listsNG136ashavingalargerpositionuncertainty thanmostoftheothergalaxies B0210 FCC 245 206 241 252 207 223 116 316 300 188 318 100 323 274 160 208 137 156 158 254 165 196 136 101 110 112 201 50 85 56 38 25 NG34 NG37 NG35 NG39 NG38 Caldwell FCC NG40 NG41 NG42 NG44 NG43 NG45 NG48 NG47 NG46 NG50 NG49 NG51 NG52 NG53 NG54 NG55 NG56 NG57 NG59 NG58 NG61 NG60 NG63 NG62 NG64 NG66 NG65 NG67 Table X.Caldwell’sdwarfs(Caldwell1987). 287 259 257 247 281 166 198 221 293 243 279 303 305 250 314 242 327 133 142 195 181 159 118 155 178 173 124 86 48 52 99 82 66 tral 1.7coreradiiofVirgo.Theseresultsareslightlydifferent from thosepresentedinPaperI,becausetherewedidnot tude ofCaldwell’ssurvey,some ofthedifferenceisdueto the differencecanbeascribedto thebrighterlimitingmagni- apply amagnitudelimittothe comparison.Whilemuchof slightly differentregionsoftheclusters usedforthecompari- classification ofthebrightergalaxies. NineofCaldwell’s son inthetwosurveysandsome ofitisduetodifferencesin Fornax EandSO galaxiesfelloutsidethe2.4°region weused NG69 NG68 NG72 NG71 NG70 NG73 Caldwell NG74 NG77 NG76 NG75 NG78 NG79 NG81 NG80 NG83 NG82 NG84 NG85 NG87 NG88 NG90 NG89 NG91 NG92 NG93 NG95 NG97 NG96 NG99 NG98 NG101 NG100 NG102 B1483 FCC 218 211 260 266 230 296 111 261 231 286 267 262 297 125 228 123 105 319 307 151 224 317 325 328 339 331 295 292 265 289 61 76 NG105 NG104 NG103 NG107 NG106 Caldwell NG108 NG109 NGlll NGl 12 NG114 NGl 13 NGl 16 NGl 15 NG118 NG117 NG119 NG120 NGl 21 NGl 22 NG123 NG124 NG125 NG126 NG127 NG128 NG129 NG131 NG130 NG132 NG133 NG134 NG135 NG137 B1699 B0271 B1120 FCC 291 269 271 280 270 238 229 215 197 185 187 214 171 212 175 199 127 140 145 258 89 87 69 98 40 23 41 42 72 60 412 1989AJ 98. .367F 413 HENRYC.FERGUSON:THEFORNAXCLUSTER brightness (LSB)backgroundspiralgalaxies.Cluster membership forthesegalaxiesisparticularlyuncertain; ies, bluecompactdwarf(BCD)galaxies,andlow-surface- rate listsofcandidatecompactelliptical(M32-like)galax- that deservespecialmention.Inthissectionwepresentsepa- als mayperhapsbemistakenfornucleateddwarfellipticals. certain classesofbackgroundgiantgalaxies,whileLSBspir- compact E’sandBCDgalaxieslookvirtuallyidenticalto galaxies inthecluster.TableXII showsthecandidateswe very fewhigh-surface-brightness, compact,star-forming show evidenceofactivestarformation, thereappeartobe portionate numberofdwarfswouldbeexcludedaswell,but for thecomparison(ofcourse,onemightexpectthatapro- cataloged. ies, weexcludednineasbeingeitherdwarfsorothertypes. that mightnotactuallybethecase).Ofremaininggalax- galaxies, notincludedinthispaper,and2930were these galaxiesarelikelytobeinthebackground.Additional the twoclusters. geli etal.(1985),oursislikelytobeafairercomparisonof Because ourclassificationsareconsistentwiththoseofBing- to belistedinTableIII.Ofthese,6,10,32,84,88,106,129, Davies etal.galaxies,notlistedinTableXI,weretoosmall vies etal.(1988).Asmentionedbefore,alargefractionof 130, 145,150,and156allappearedinourlistofsmaller There areseveralclassesofgalaxiesinTablesIIandIII While anumberoflow-surface-brightness dwarfgalaxies Table XIshowstheidentificationofgalaxiesfromDa- © American Astronomical Society • Provided by the NASA Astrophysics Data System VII. GALAXIESOFSPECIALINTEREST -.4 —.2O.2.4 a) BlueCompactDwarfs Log(r) (degrees) -1 been classifiedontheLasCampanasplates. are asfollows:(1)catalognumberfromTableIIor the galaxyhasone. liocentric velocityinkms,and(7)analternatename,if magnitude andclassification,asdefinedinTableV,(6)he- fined inTableIV,(4)totalmagnitude,(5)sourceofthe have identifiedontheLasCampanasplates.Thecolumns are afewsimilargalaxiesamongstthesamplethathasnot didate compactellipticalgalaxy.Itisthuspossiblethatthere and wasinitiallyclassifiedasabackgroundellipticalorcan- that thisgalaxyiscompletelyburnedoutontheSRCplate, surrounded byaringofbrightHnregions.Itisworthnoting a small,veryhigh-surface-brightnessgalaxy,withnucleus III, (2)morphologicaltype,(3)clustermembershipasde- be quiterare,andwouldpresumably showsomepreference for closeassociationwithgiant galaxies.Kimble,Davidsen, tidal strippingofagiantgalaxy. Inthelattercase,theymust different stellarinitialmassfunctions, oraretheremnantsof have mass-to-lightratiosdifferent fromthediffusedwarfs, this isthecase,thencompactE’scannotexistunlessthey supernova-driven windsintheearlyphasesofevolution.If structure ofthedwarfellipticalsisaresultgasstrippingby Dekel andSilk(1986)iscorrect.Inthisscenario,thediffuse ants. Thisistobeexpectedifthedwarfgalaxymodelof showed thattheyarelikelytobelesspopulousthanthegi- date compactellipticalandSOgalaxiesinthecluster sibility inthe4000Abreakstrengths ofthecandidateslisted and Sandage(1989)havefound someevidenceforthispos- The mostinterestingofthesegalaxiesisFCC24,which In Sec.V,weexaminedthespatialdistributionofcandi- b) Compact(M32type)EllipticalGalaxies .6 ble IIofthispaper(closedsquares).The ed byCaldwell(1987)inhisTableI(open well, andthatCaldwellunderestimated identical indicatesthatthesenewdwarfs fact thatthetwodistributionsarevirtually tion oftheadditionaldwarfslistedinTa- squares), comparedtotheradialdistribu- Fig. 17.Radialdistributionofdwarfslist- counts. core radius,normalizedtotheCaldwell the numberofdwarfs(byaboutafactor are likelytobemembersoftheclusteras 2 ).ThesolidcurveisaKingmodelof0.7° 413 1989AJ 98. .367F 414 HENRYC.FERGUSON:THEFORNAXCLUSTER © American Astronomical Society • Provided by the NASA Astrophysics Data System Davies 21 20 15 13 12 11 23 22 18 17 16 14 24 19 25 26 27 28 31 33 34 35 36 37 38 40 39 41 42 43 44 46 45 47 49 48 4 8 7 5 3 2 9 1 B0789 B0537 B0524 B0513 B0510 B0667 B0641 B0636 B0585 B0695 B0695 B0928 B0721 B0707 B0748 B0738 B0756 B0787 B0797 B0815 B0830 B0847 B0850 B0855 B0859 B0907 B0904 FCC 100 102 110 112 113 115 116 123 120 65 61 86 82 81 76 90 99 Davies 61 60 54 52 51 50 65 64 63 62 59 58 57 56 55 53 66 68 67 69 70 72 71 73 74 75 76 77 78 79 80 81 82 83 86 85 87 89 90 92 91 93 94 95 Table XI.GalaxiesfromDaviesetai(1988). B1143 B1180 B1195 B1020 B1006 B1084 B1082 B0986 B0958 B0960 B1022 B1241 B1108 B1109 B1112 B1116 B1127 B1148 B1157 B1159 B1186 B1199 B1200 B1202 B1221 B1240 FCC 137 133 134 128 164 158 156 135 136 174 178 181 187 183 188 195 196 203 Davies 109 107 105 104 103 102 101 100 108 111 110 113 112 114 115 117 116 119 118 120 122 121 123 124 125 126 128 127 131 132 133 135 134 137 136 138 139 140 142 141 99 98 97 96 B1317 B1532 B1306 B1292 B1284 B1284 B1279 B1278 B1271 B1256 B1248 B1285 B1320 B1319 B1321 B1349 B1327 B1379 B1345 B1351 B1419 B1477 B1518 B1553 B1565 FCC 207 221 222 223 230 237 234 243 241 245 247 252 260 261 262 264 267 274 278 Davies 160 159 158 157 155 154 151 149 148 146 144 143 162 161 153 152 147 164 163 166 165 168 167 170 169 171 172 173 174 175 176 178 177 179 180 181 182 184 183 185 186 187 B1686 B1715 B1665 B1651 B1627 B1610 B1747 B1701 B1656 B1759 B1751 B2092 B1773 B1770 B1790 B1794 B1816 B1867 B1905 B1920 B1969 B1979 B1987 B2087 B2141 FCC 292 285 279 293 296 295 297 298 299 299 300 302 303 311 316 318 324 414 1989AJ 98. .367F 1/4 giants) thanisolatedellipticalsofthesameluminosity. members tendtohavestrongerbreaks(i.e.,appearmorelike in BST85.Compactellipticalsthatlienearbrightcluster them. have normalbreakamplitudes,indicatingthatthetidal- However, thereareisolatedcompactellipticalsinVirgothat stripping hypothesisprobablydoesnotaccountforallof 415 HENRYC.FERGUSON:THEFORNAXCLUSTER lated compactE’sdoexist,theymaynothavesuchhigh fied bytheirhighsurfacebrightness.Whiletheprototype, is probablydueprimarilytoitsinteractionwithM31.Ifiso- M32, hasanunusuallyhigheffectivesurfacebrightness,this between E’sanddE’s.CaldwellBothun(1987)have face brightnessandmagnitudecontrastrelativetothesur- ellipticals fromourcatalog.ThislistincludesallEandSO below aboutM=—19.Inanycase,thecentralregionsof lation thatappearstoexistforgiantellipticals(Kormendy surface brightnesses.Thesurface-brightness-luminosityre- pointed outsomeadditionalintermediatecases. isolated backgroundellipticals.Afewofthegalaxieslisted rounding background.Mostofthesegalaxiesarelikelytobe also includesadditionalpossibleclustermembers(classes1- and arenotobviouslycontainedinabackgroundcluster.It fall within8arcminofabright(B<15)clustermember galaxies inmembershipclasses3and4fromTableIVthat brightnesses ashighthatofM32. most rlawellipticalsarecompletelysaturatedonphoto- 3 )thatappeartobegoodcandidatesbyvirtueoftheirsur- none ofthegalaxiesinoursamplehaveeffectivesurface highly uncertain.Asbestwecantell,giventhisuncertainty, graphic plates,makingsurface-brightnessmeasurements clusters isnowapparentfromthe VirgoandFornaxcluster spirals mightexistinthefield.That suchgalaxiesarerarein that asignificantpopulationof large, low-surface-brightness and GP1444(Daviesetal1988) pointtothepossibility (G92 andNGC1396)areprobablyintermediatecases 1985; Schombert1987)hasnotbeenshowntoextenddown B T It isnotatallclearthatcompactellipticalscanbeidenti- In TableXIII,welistthebestcandidatesforcompact The accidentaldiscoveriesofMalin 1(Bothune/ö/.1987) © American Astronomical Society • Provided by the NASA Astrophysics Data System c) Low-Surface-BrightnessSpiral Galaxies B0035 BCD?316.05 FCC B0037 BCD(HighSB)orS314.95 B0477 BCD(HighSB)orS316.34 B1348 S(HighSB)orBCD416.6 B0801 BCD(HighSB)?315.94 32 dEpec/BCD115.431433 24 BCD116.14 B1660 (interacting)orBCD416.5 B1631 S(interacting)orBCD416.2 35 SmIV/BCD?115.34 33 Sdinpec/BCD?114.241956 12 BCDorS217.05 Type Table XII.Bluecompactdwarf(BCD)galaxiesandcandidates. Memb. B? nesses weredetected. surveys, wherenospiralswithextremelylowsurfacebright- best candidatesforsuchbackgroundgalaxiesfromthecata- brightness, andthelastcolumnlistsmeansurfacebright- fact, wehavere-examinedthosegalaxiesclassifiedas nent bulgessurroundedbyveryfaintdisks.Inlightofthis brightnesses thanMalin1andGP1444,theyaresignificant- log. Thesecond-to-lastcolumnliststheeffectivesurface have alargebulge-to-diskcontrast.InTableXIV,welistthe disk. Whileallofthesecandidateshavehigherdisksurface giving aroughindicationofthesurfacebrightness ness betweenthe2?=26.5isophoteandeffectiveradius, candidates maybetestedbyCCDimagingonaverydark most likelytobegalaxiesinTableXV.Therealityofthese bulge-to-disk contrast,andshowsahintofspiralpattern interested shouldsendablank 600 fttapetotheauthor,or mat, eitheronmagnetictapeor viaelectronicmail.Anyone magnitude of16.5. which hasamajor-axisdiameter of1arcmin,andatotal only oneexample.Thatisgalaxy 123inTableII(NG84), appear tobesomewhatrarerinFornax,aswehavefound surface brightnesseswerefoundintheVirgoCluster.These night. panas plates.Wehavelistedthe“plateflaws’’thatappear brightnesses thattheywouldnotbevisibleontheLasCam- bles IIandIII.However,afewpotentialgalaxieseitherfell panas plates,wehaveincludedthemasrealgalaxiesinTa- on theLasCampanasplate. galaxies. ThebestcandidateisB1310,whichhasthehighest ly lowerthanthesurfacebrightnessesthataretypicalofdisk “dE, N,orS““dSOS”galaxies,toseewhetherthey send arequesttohcf@hutspa, or SCIVAX::FERGUSON. out oftheLasCampanasfields,orhadsuchlowsurface peared ontheplatesthatmightactuallybegalaxies.Where such galaxieswerevisibleonboththeSRCandLasCam- Both Malin1andGP1444arecharacterizedbypromi- A numberofexceptionallylargedwarfswithverylow The cataloginTablesIIandIII isavailableinasciifor- There wereafewlow-surface-brightnesssmudgesthatap- 1 S (kms”)Othername Velocity d) PlateFlaws? NGC1316C G104 415 1989AJ 98. .367F 416 HENRYC.FERGUSON:THEFORNAXCLUSTER © American Astronomical Society • Provided by the NASA Astrophysics Data System B0069 B0346 B0331 B0300 B0276 B0266 B0097 B0446 B0421 B0509 B0517 B0731 B0598 B0566 B0523 B0951 B1006 B0981 B0963 B1193 B1102 B1195 B1373 B1376 B1398 FCC B1611 B1621 B1916 B1817 B1922 B1941 B1946 B1947 B2144 B2050 B2162 B2187 B2181 B2190 B2209 B2217 B2234 B2235 B2283 B2289 B2290 B2293 332 G92 202 NGC1396 119 G26 182 G79 143 NGC1373 26 ES0357-G25 90 G118 names Other Table XIII.Compact,low-luminosityE(M32-type)galaxiesandcandidates. E3® S0 pec E4 pec SB0(8) E orS0 El E orS0 SBO pec E(M32?) E E ordE(M32?) E E? E(M32?) E0(M32?) E(M32T) d:E6,N E E(M32?) E6(M32?) E(M32?) E E E ordSO E(M32?) E(M32?) E(M32T) E(M32?) S0 E(M32?) o 2 E ordE2,N E E(M32?) SOg ordS0 E S0? E(M32?) SO E E(M32?) E6(M32?) E(cD) ordE E(M32?) E? ordE,N E ordE(M32?) E ordE,N E ordE g E(M32?) ordE,N E E ordE,N E(M32?) E E E(M32?) E(M32?) E Type Additional candidates Likely members Br 15.0 15.0 16.0 15.7 15.3 14.9 14.3 16.9 16.8 16.8 18.2 17.4 18.9 15.6 17.2 16.5 16.7 17.5 18.4 16.4 18.3 16.2 16.3 18.0 17.1 17.3 17.8 17.6 16.6 17.1 16.7 16.4 18.1 17.4 18.2 17.4 17.9 17.6 18.4 16.6 15.3 15.6 17.0 16.5 17.5 18.0 17.7 17.7 15.8 17.5 18.3 18.0 15.7 16.6 16.0 17.7 Memb. (km/s) 3 3 3 3 4 4 3 5 4 3 3 3 3 3 3 3 3 3 3 4 5 3 3 3 4 Velocity 1376 1554 1916 1823 1326 1823 894 NGC1399 NGC1381 NGC 1375 NGC1374 NGC1326A? ESO358-G05 NGC1326A? NGC1341 NGC1351A NGC1361A NGC1351A ICI 962 G99 G99 NGC1381 NGC1387 G79 ES0358-G59 NGC1437A IC1993 NGC1460 ESO359-G03 ESO359-G02 ESO359-G03 ESO359-G03 Near Distance (arcsec) 298 282 394 408 389 312 297 369 381 230 477 243 367 455 112 167 225 283 300 450 265 233 196 97 416 1989AJ 98. .367F Binggeli, B.,Sandage,A.,andTammann, G.A.(1985).Astron.J.90,1681 Blair, M.,andGilmore,G.(1982).Publ. Astron.Soc.Pac.94,742. Barlow, M.J.(1978).Mon.Not.R.Astron. Soc.183,367. especially BarryLasker,ConradSturch,BrianMcLean,and ing outthesurvey.ThanksarealsoduetoGuideStar Bardeen, J.(1985).InInnerSpace/Outer Space,editedbyE.W.Kolb, Brad WhitmoreandMarijnFranxforofferingtheirCCD Ray Lucasforprovidingthedigitaldatathissurvey,to Operations GroupattheSpaceTelescopeScienceInstitute, Las Campanasplates,andforhishelpguidanceincarry- 417 HENRYC.FERGUSON:THEFORNAXCLUSTER cago, Chicago),p.258. M. S.Turner,D.Lindley,K.Olive,and D.Seckel(UniversityofChi- (BST85). I ammuchindebtedtoAllanSandageforprovidingthe © American Astronomical Society • Provided by the NASA Astrophysics Data System * F12iscoincidentwithNG86,andpossiblyHPW27. F07 F05 F04 F02 F01 F08 F06 F03 F10 F09 Fll F12* F14 F13 (1) # FCC B0513 B1320 B1319* B1277 B1090 101 * Bestcandidate. RA(1950) 3 3324.4 3 3027.7 3 2954.3 3 3342.6 3 2536.5 3 2455.7 3 2325.3 3 2103.6 3 3558.3 3 3528.2 3 3643.0 3 3702.2 3 4522.0 3 3709.9 Table XIV.Possiblelow-surface-brightness(Malin1-type)backgroundspirals. (2) dEOJ^ orS dEJ^orS dE3J4 orS S? ordEpec,N Sa ordS0 S ordEpec,N 2 Type -35 3409 -34 07 -32 4244 -35 3203 -32 0136 -35 3026 -35 5904 -37 1523 Dec(1950) -33 2600 -33 2660 -35 2041 -36 1830 -32 1324 -34 4707 Table XV.Plateflawsthatmaybegalaxies. (3) Memb. BlogD6.5 T2eouter ill M REFERENCES 2 2 2 2 1 1 1 1 1 ImV orflaw dE,N? dE,N orflaw dE dE,N orflaw dE orflaw dE dE,N? orflaw dE dE orflaw dE orflaw ImV? orflaw dE dE orflaw 16.7 17.2 17.7 15.9 17.2 17.3 Bothun, G.D.,Mould,J.R.,Caldwell, N., andMacGillivray,H.T.(1986). Bothun, G.D.,Impey,C,Malin,and Mould,J.(1987).Astron.94, Binggeli, B.,Tarenghi,M.,andSandage, A.(1989).Astron.Astrophys.(in Binggeli, B.,Sandage,A.,andTarenghi, M.(1984).Astron.J.89,64. searchers Program. for theirfinancialsupportundertheGraduateStudentRe- thank theNationalAeronauticsandSpaceAdministration support withtheobservations.Finally,itisapleasureto Campanas, FernandoPeraltaandAngelGuerra,fortheir images forcalibration,andtothenightassistantsonLas Type press). 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