1993Apjs ... 86 ...5K the Astrophysical Journal Supplement

Home , List of spiral galaxies, NGC 1433, NGC 1510, NGC 1553, NGC 1569, NGC 1614

1993ApJS ... 86 ....5K tween morphologicaltype,activity classbasedonopticalspec- ble class.Withthisatlasweaimtoclarifytheconnection be- that spiralgalaxiesoflaterHubbleclasshavemorefluxat the shortest UVwavelengthsthandospiralgalaxiesofearlierHub- servatory (OAO)(Pence1976)andofXhtAstronomicalNeth- picture basedonUVspectraoftheOrbitingAstronomical Ob- emission featuresofindividualobjects.Ourdatasupport the absolute fluxdistributions,tobettershowtheabsorption and according tomorphologyandactivityclassintheform of energy distributions,todemonstratetheoverallcharacteristics (LINER), starburst,bluecompact,compactdwarf, and data set.Thespectraforawidevarietyofgalaxies,including ity classusingasampledrawnfromuniformlyreducedIUE erlands Satellite{ANS)(Coleman,Wu,&Weedman1980) Seyfert 2galaxies,arepresented,bothintheformofspectral normal spiral,low-ionizationnuclearemission-hneregion star-forming galaxiesofdiflerentmorphologicaltypeandactiv- © 1993.TheAmericanAstronomicalSociety.Allrightsreserved.PrintedinU.S.A. The AstrophysicalJournalSupplementSeries,86:5-93,1993May of ESA. 2 1 We presentasystematicstudyoftheultravioletspectra AlfredP.SloanFoundationFellow. AffiliatedwiththeAstrophysicsDivision, SpaceSciencesDepartment 18506 a26±014 Space TelescopeScienceInstitute,3700SanMartinDrive,Baltimore,MD21218;andIstitutodiAstronomía,UniversitéCatania the extinctionlawisdiflerentorthatanydustpresentingalaxiesformofclumpsanddoesnot Subject headings:atlases—galaxies:ISMSeyfertspiralstarburst toF ocX--^. that areflatorincreasingtowardshortwavelengths,withawiderangeinspectralindex,goingfromFccx the longestUVwavelengths.Thestarbursting,bluecompact,andcompactdwarfgalaxieshaveUVcontinua contribute totheflux,owingveryhighopticaldepth. is notapparentinthesegalaxies.Thelackofandustfeature(e.g.,the2200Ábump)impheseitherthat show afeaturelessbluecontinuumplusemissionlines,withtheUVspectrumofhostgalaxyapparentonlyat spectra oflow-ionizationnuclearemission-lineregion(LINER)galaxieswiththenormalspiral shows thattheUVcontinuumofLINERsisdominatedbygalaxycontinuum.Incontrast,Seyfert2galaxies flux attheshortestUVwavelengthsthandospiralgalaxiesofearlierHubbleclass.Acomparison noise ratio. have beenextractedwithanoptimalalgorithmandco-addedtoproducespectrathebestpossiblesignal-to- starburst galaxiesisproducedbycombining387low-resolutionspectrafromtheIUEdataarchives.The Observatory andfromtheAstronomicalNetherlandsSatellitethatspiralgalaxiesoflaterHubbleclasshavehigher x x The spectralsignatureofdustwithawavelengthdependencetheextinctionsuchasisseeninMilkyWay An atlasofultravioletspectrathecentralregions143spiral,irregular,bluecompact,Seyfert2,and Our datasupportthepictureproposedearlieronbasisofUVspectrafromOrbitingAstronomical © American Astronomical Society • Provided by theNASA Astrophysics Data System Physics andAstronomyDepartment,JohnsHopkinsUniversity,HomewoodCampus,Baltimore,MD21218 1. INTRODUCTION AN ATLASOFULTRAVIOLETSPECTRASTAR-FORMIJNGGALAXIES ultraviolet: galaxies Space TelescopeScienceInstitute,3700SanMartinDrive,Baltimore,MD21218 A. L.Kinney,R.C.Bohlin,andD.Calzetti Received 1992April13;acceptedSeptember21 2 Rosemary F.G.Wyse 1 N. Panagía ABSTRACT AND 5 the activityobservedinoptical.TheIUEarchivesdonot tra, andtheultravioletionizingcontinuumthatoftendrives be made.However,acquisitionofawell-definedsample of of IUE. normal diskgalaxiesshouldbeahighpriorityinthelateryears about UVspectralpropertiesasafunctionofgalaxytype can chives containalargenumberofgalaxies,sothatconclusions the IUEaperture,sothatwavelength coveragefortheatlas currently beingobtainedinan aperturematchedtothesizeof fact thatthesampleisnotparticularlycomplete,IUEar- scientific communityhashadthemostinterest.Inspiteof contain acollectionoftheindividualgalaxiesinwhich contain acomplete,well-selectedsampleofgalaxies,butrather context ofalargerdataset.Ground-based opticalspectraare vidual objectsandtheirUV spectra arediscussedin§4.3. of dustupontheirspectraarediscussedin§4.2;andtheindi- characteristics ofthevarioustypesgalaxiesandimpact Wolf-Rayet stars,andlatertypeisdiscussedin§4.1 ; the such astheinterstellarmedium(ISM),earlyOandBstars, § 3;thespectralsignaturesofvariouscontributorsto UV, described in§2;digitaldistributionoftheatlasis in The ultravioletspectrainthis atlaswillbeanalyzedinthe The objectselection,datacompilation,andreductionare 1993ApJS ... 86 ....5K the disksofgalaxies,whichwe wishtoexclude.Theshort-and long-wavelength spectraareplotted togetherinFigures8-112 dict theopticalcolorsofstar-forminggalaxiesathighredshift will alsobeusedtoquantifyUVcolorsofgalaxiesandpre- background fromstar-forminggalaxies.Thetemplatespectra tra willbeusedtopredictthecontributiondiffuseUV tra willbeusedtoformtemplatespectraofstar-forminggalax- IUE ofHnregions,supernova remnants,andotherobjectsin ture. Aperturepositionisparticularly importantinproducing that theregionofLyaemissionUnecanbeobserved.The (z «1-2).Anumberofgalaxiesintheatlasareredshiftedso ies accordingtoHubbleclassandactivityclass.Templatespec- a uniformdatabase,sincemany spectrahavebeentakenwith ensure thatthecenterofgalaxywaswithinIUEaper- based ontheirsignal-to-noiseratio(see,e.g.,Kinneyet al. were selectedforinclusionintheatlas.Theirselection was axies. redshift star-forminggalaxiesforhigh-redshiftgal- lyzed inanattempttounderstandtheimplicationsofourlow- observations ofemissionandabsorptionatLyawillbeana- objects willeventuallygofrom1200to7800Â.TheUVspec- servers withinformationonoffsetsweretakenintoaccount to observers’ commentsregardingoffsetsandpublicationsby ob- persion IUEspectraofthegalaxies,387143galaxies towrites forthislistwereinspectedtoexcludespectrawith to havebroademissionlines(calleddwarfSeyfert1galaxiesby were excluded,exceptforthoselow-luminosityobjectsfound galaxies presentintheVéron-Cetty&Véroncatalog(1986) galaxies. ThenalistofobjectscommontoboththeIUEar- al. 1989,hereafterCPG)wasproduced.TheCPGcontains pact galaxiesintheCatalogueofPrincipalGalaxies(Paturelet length (LWRandLWP)camerastakeninthelarge(10"X nates ofagalaxyandthecoordinatesobservation.Both and othererrorsintheon-linearchive.Of^780low-dis- incorrect pointingsandtocorrectforerrorsinexposuretime list of~780low-dispersionspectragalaxies. (spiral andirregulargalaxies)cross-referencedwithlistsof cross-referenced withtheIUEarchivesobjectclasses80and82 Filippenko &Sargent1985).Ourinitiallistofgalaxieswas chives andtheCPGwasproduced,fromwhichSeyfert1 de Vaucouleurs,&Corwin1976)andtheMarkarianlistsof ond ReferenceCatalogueofBrightGalaxies(deVancouleurs, 73,000 galaxiesandincludes,amongothercatalogs,theSec- son 1984foracompletedescriptionofIUEdata). 20") aperture.Theresolutionisapproximately5Âforthe spectra fromtheshort-wavelength(SWP)andlong-wave- sitions ofobjects(±5')intheIUEarchivestoproduceamaster 240 candidategalaxieswerethencross-referencedwiththepo- starburst galaxies(Balzano1983;Mazzarella&Balzano SWP and8ÂfortheLWRLWP(seeTumrose&Thomp- 1991b). Agreementwasrequiredbetweenthecatalogcoordi- 6 1986 ),sothatmissingobjectswereadded.Thepositionsofthe The individualIUEspectra,observingscripts,andpho- First alistofthepositionsallspiral,irregular,andcom- The ultravioletdataarefromtheIUEarchivesandinclude © American Astronomical Society • Provided by theNASA Astrophysics Data System 2.1. ObjectSelection 2. THEDATA KINNEY ETAL. that areincludedintheatlas,alongwiththeirpositionsand tude, therightascensionanddeclination,and,finally,other generally wellmatchedbetweenthecameras,whichisevi- with nonormalizationbetweenthecameras.Thefluxlevelsare tabase [NED]),theactivityclassofgalaxy,heliocentric IUE apertureforallspectraco-addedagivenobject.We the 9fineextractionincludes81%offighta15line large, asevidencedbythefollowingfacts:(a)AnIUEslitof9 degrades thesignal-to-noiseratioinresultantspectra tral extractiontechnique,theaddednoisein15finesseriously ber offinesinthefile.Despiteoptimalnatureourspec- and othernames. other names;andTable3listsMarkarianobjectspositions names. Forcross-reference,Table2liststheMessierobjects (assuming q=\andH50),theGalacticreddening(Bur- velocity, thephotographicmagnitude,absolutemagnitude dence thatthecenterofgalaxywascontainedinlarge weighting withtheirrelativestatisticaluncertainty(Kinney et the absolutecalibrationofBohlinetal.(1990)isused. The persion, andexcessnoiseintheresult. extraction. Ingeneral,ourcurrentimplementationoftheopti- fines, (c)Foroneofthemoreextendedgalaxies,NGC7590, fines correspondsto19"4,or91%ofthe21"4highIUEslit.(b) fine optimalextractions.Thelossoffightina9slitisnot in themoremodemline-by-linefilesthathavetwicenum- This sht-weightedextractioncanchooseslitheightsofeither9 used toextractthespectrafromIUEline-by-Unedatafiles. mal extractiontechniqueofKinney,Bohlin,&Neill(1991c)is stein &Heiles1982,1984),theGalacticlatitudeandlongi- mann 1987,hereafterRSA]andtheNASAExtragalacticDa- length (LW)spectra,thegalaxyname,morphologicaltype Ceriello 1991,whoreportIUEfluxesfornormalgalaxies,and have comparedourfluxeswiththoseofLongo,Capaccioli,& are alsotakenintoaccount(Bohlin&Grillmair1988a,b), and net signal,afalselywidenedprofileperpendiculartothe dis- mal extractionalgorithmfor15finestendstotracksomeofthe In thecaseoftrailedspectra,87%fightisincentral9 many cases.Therefore,allspectrapresentedherearefrom9 or 15fines,wherethe9isunderstoodtobe1830fines from theRevisedShapley-AmesCatalog[Sandage&Tam- of thegalaxy(whereweusedsimplerclassificationthose of short-wavelengthspectra(SW),thenumberlong-wave- find thattheyagreetoabout5%. spectra ofgalaxiesobservedmultipletimesareco-added by noise outsideoftheslit,whichmayproduceanartificiallylarge grouped bytheiractivityclass, orderedbyobservedslope,and al. 1991c)toproducespectrawiththebestpossiblesignal-to- signal-to-noise ratioarepresented inFigures1,2,and3, short- andlong-wavelengthcoverage andwithrelativelyhigh erties ofthemanyclassesgalaxies inthisatlas,galaxieswith noise ratios. Q0 Changes ofsensitivityoverthedecadeIUEobservations In ordertominimizethenoiseinatlasspectra,opti- The fistofatlasgalaxiesisgiveninTable1withthenumber In anattempttogiveoverview ofthespectroscopicprop- 2.2. ExtractionandReduction 2.3. Methodology 1993ApJS ... 86 ....5K rl8 Fig. r8 rl rl r7 49 50 53 48 47 46 45 rl rl 52 44 43 r2 r6 51 42 41 40 r5 39 38 37 36 35 r4 34 33 29 27 25 32 31 28 24 r2 30 23 22 21 20 19 18 17 16 15 14 13 12 11 10 8 9 3 2 2 1 1 1 1 3 1 1 1 1 1 1 2 1 1 1 1 1 3 1 1 1 7 2 1 2 1 2 3 2 4 4 1 2 2 1 1 1 1 1 1 1 1 1 2 1 1 1 1 3 1 2 12 5 1 1 SW LWGalaxy 1 1 1 1 10 NGC1068 1 NGC3396 NGC3448 NGC3432 NGC3395 MCG9-18-32 NGC3393 NGC3353 NGC3682 NGC3351 NGC3310 UGC5720 NGC3622 Mrk36 NGC3256 NGC3125 UGC5408 NGC3081 UGC6456 UGC6448 NGC3660 NGC3504 1050+04 NGC3077 NGC3049 NGC3031 NGC2997 IZw 18 NGC2903 NGC2820A NGC2841 NGC2798 MCG10-13-71 NGC2782 IC2184 NGC2681 NGC2639 Holmbergll NGC2537 NGC2403 UGC4483 NGC2415 UGC3838 NGC1800 NGC1705 NGC1667 NGC1672 NGC1614 NGC1569 NGC1553 NGC1510 NGC1433 NGC1313 NGC1140 NGC1023 IC214 NGC1097 NGC598 IC1586 Mrk357 ES0296-11 Harol5 NGC262 NGC224 Name American Astronomical Society •Provided bythe NASA Astrophysics Data System Irr. Am. IBm Sc Scdp Sep SBa Im Im SO/a SBb SAB(r)bc Sb(s) pec. pec. pec. SBbc Irr. Irr. Am. 10 S? SABab SBa SBbc Sb Sc(s) Irr. Sbc 10 pec. Sb SBa SAB(rs)a Sa Sa dim IV Irr. Sc Irr. pec. Sc Cl. Irr. Im IBm. Am. Irr. Am. Sbc SAB(s)bc SBb pec. Im SO pec. Am. pec. SBab SBdm Irr. Am. SBbc Sb SBO pec., 2-nuc. Scd I Type Class Pair? Pair SO Sb Morph. Activity SB nuc. SB nuc. Syl/NELG BCG SB nuc. Sy2 BCDG BCDG BCDG SB nuc. BCDG BCDG Hs SB nuc. SB nuc. BCDG BCDG BCDG Sy2 SB nuc. Lin Hs Hs BCDG SB nuc. SB nuc. Lin BCDG Lin BCDG BCDG HII BCDG BCG Lin+Sy BCG BCG HII Sy2 SB+Sy BCDG SB nuc. SB nuc. BCDG HII BCG Sy 2 Hs+Lin SB nuc. SB nuc. BCG Sy 2 BCG - 5780* -93* 616 991* 3678* 646* 2447* 3730* 995 779 1357 992 1648 2821 2602* -36 1543* 1306* 1628 1535 7 2413 1461* 441 1110 756* 550 4230* 637 2551 715 3187 3784* 3605* 723 1494* 3060* 4585 -83 1081 640 4778* 1534* 1741 158* 156* 131 989* 452 1335 -180 1236 1061 661 9061* 4507* -297 km s 1509 5572* 6407* 5821* 1319 1131 VH 15845* Atlas Galaxies : : 13.3* 12.15 14.7p* 14.66a 15.5 13.65* 11.73 12.6 15.Op* 13.10p 14.70a 15.69a 11.8 12.4 13.2 10.52 11.2 13.17a 7.86 11.98 13.12 14.84* 9.50 10.64 12.68 8.89 13.04p 10.32 16.28a 10.17 15.4* 13.0 15.6 12.15 15.0p* 11.10* 12.35 12.78* 14.0p* 11.09 12.65 14.3p* 13.10 12.80 12.75 11.03 13.63* 9.37 11.90 10.42 13.47* 9.55 10.68 6.26 12.85 10.16 4.38 10.36 14.7* Bt TABLE 1 15.7 14.5* 13.5 13.90* 14.9p* >* -19.42*o0.01 -19.39*o 0.00 -17.34*o -20.2 -14.6m -18.74c -19.10*o 0.00 -15.06*a 0.00 -21.11 -20.78* -19.50 -20.56 -20.58 -19.02*o 0.00 -21.59* -18.5 -20.66 -20.82 -19.02*o 0.00 -18.96*o 0.00 -22.80 -18.2 -17.2 -20.67 -20.75 0.04 -21.40 0.12 -15.07*a 0.01 -20.96 -16.77m -21.53 -17.57*o -19.81 -19.07c -22.06 -12.89m -18.13 -20.44* -20.09* -20.48 -22.18 -21.76* -19.47 -17.3 -17.00 -22.54 -21.37 -21.58* -16.22 -21.26 -17.66*o 0.00 -21.15 -19.66 -20.36 -22.30 -22.93 -21.17 -22.07* -19.07 -21.82c -20.79* -22.07b -20.53b -20.78* -21.61 M E(B-V)1 b = 50 0.01 0.00 0.00 0.02 0.00 0.03 0.00 0.00 0.02 0.08 0.00 0.01 0.00 0.13 0.07 0.05 0.03 0.02 0.04 0.00 0.00 0.03 0.00 0.02 0.04 0.01 0.00 0.02 0.03 0.03 0.04 0.04 0.02 0.05 0.00 0.04 0.05 0.51 0.00 0.00 0.02 0.03 0.02 0.01 0.06 0.03 0.04 0.05 0.04 0.02 0.06 0.02 0.08 246.2 269.1 201.8 270.7 204.6 234.0 135.3 153.1 184.8 192.9 277.4 365.3 127.8 137.3 192.9 156.7 259.0 135.8 152.3 227.6 262.6 156.6 156.2 152.7 208.7 141.9 142.1 234.4 160.5 261.1 204.1 166.9 179.5 145.0 268.8 204.4 149.8 155.6 182.2 143.1 142.6 248.8 167.3 168.9 144.3 173.8 184.1 150.6 265.6 255.7 283.4 143.7 226.9 188.3 282.2 172.1 145.0 157.8 133.6 132.2 120.1 122.3 121.7 121.2 48.5 47.5 55.4 53.9 63.2 63.2 44.7 37.3 50.6 48.4 66.5 63.1 56.0 25.0 66.0 29.9 53.4 56.4 46.8 54.1 52.8 41.7 20.6 40.9 44.8 44.5 11.7 44.1 40.3 44.3 -35.1 41.3 43.7 -38.7 -30.1 -38.9 16.8 39.7 38.2 34.4 32.7 33.0 29.2 28.6 28.5 -34.4 24.0 -43.7 -48.2 -51.2 -44.6 -56.3 -64.7 -51.9 -19.1 -52.0 -31.3 -74.7 -75.6 11.2 -39.1 -30.9 -40.5 -21.6 09 5210.2 10 5028.4 10 4708.9 10 5138.4 10 4942.9 09 5710.0 11 2446.1 11 2436.6 11 2355.8 11 2100.1 11 1710.3 11 0215.6 11 0028.1 10 4702.6 10 4603.8 10 4600.0 09 5921.9 09 5127.6 09 4328.0 10 4216.5 10 4119.6 10 3540.3 10 2922.9 09 3030.3 09 2919.9 10 2543.0 10 0419.0 10 0022.0 09 1726.1 09 1409.4 07 3339.5 09 1834.9 08 0942.5 07 2339.4 09 1253.5 09 1053.8 08 3201.3 08 1353.5 07 3205.5 07 2220.0 05 0433.0 08 4958.0 08 4003.1 04 5306.0 04 4611.0 04 4455.0 04 3135.5 04 2605.8 04 1505.0 04 0154.0 03 4027.0 03 1739.0 02 5207.0 02 4411.0 02 4006.5 02 3715.8 02 1128.8 01 3104.6 01 1956.6 01 1743.0 00 4604.8 00 4517.0 00 4604.4 00 4000.0 (h-m-s) c*(1950) -24 5348 -08 2301 -43 3900 -29 4130 -22 3506 -30 5736 -32 0112 -53 2630 -06 24 -59 2018 -08 4042 -55 5412 -43 3212 -47 2248 -66 4042 -10 1343 -30 2854 -00 1332 -41 2954 -12 5922 54 3423 (d-m-s) Names 6(1950) Other 66 5156 04 5352 36 5309 33 1518 33 1444 52 3550 79 1606 64 2446 29 2434 56 1323 54 3934 67 3053 28 1435 53 45 09 3032 59 4050 68 5833 69 1813 11 5800 21 4319 42 1234 65 4240 55 2746 40 1917 46 0832 51 1119 64 2657 59 5853 51 3014 69 5720 70 5213 35 2115 72 1355 72 4033 50 2308 64 4418 38 5055 04 5633 30 2340 22 5430 41 0006 31 4100 22 0607 UGC6024 Mrkl267 UGC5986 UGC5935 Mrkl53 VII Zw403 UGC5931 MCG-04-26-011 Mrk35, Haro3 UGC6459 Mrkl70 Mrkl291 UGCA225 M95 Mrk33, Haro2 MCG-07-022-010 IC2529 UGC6339 UGC6118 UGC5786 MCG-05-24-022 Mrk25 UGC5398 Mrk710 Mrk86 M81 UGCA181 Mrkll6, UGCA166 UGC5079 UGC4966 MrklOS, IC2458 UGC4905 Mrkl9 UGC4862 UGC4544 DDO 50 Mrk8 UGC4645 MCG+12-08-048 Haro 1 UGC3918 Mrk7 MCG-05-13-004 ESO 158-G013 MCG-01-13-013 ESO118-G043 UGC3056 Mrk617 ESO 157-G017 MCG-07-09-006 ESO 249-G014 ES0082-G011 Mrkl063 UGCA041 M77 UGC2154 Mrkl027 M33 MCG-07-03-016 Mrk960 Mrk347 Mrk348 M31 1993ApJS ... 86 ....5K rl0,rl2 1 Fig. SWLWGalaxy rl7 rll rl7 rl9 no. Name 103 102 101 100 r3 rl r3 r3 r9 69 r3 r9 96 1 95 94 93 92 91 90 99 89 88 87 97 86 85 84 83 82 81 80 79 78 72 77 76 75 71 70 68 67 66 65 64 63 62 61 60 59 57 74 73 58 56 55 54 7 5 1 1 ? 1 1 2 2 2 2 3 1 1 1 1 2 1 2 1 1 1 1 1 1 NGC6217 NGC6090 NGC6052 NGC5996 NGC5506 NGC5457 UGC8850 NGC5253 NGC5256 ES0383-44 UGCA410 NGC5860 UGC9560 NGC5728 IC4395 NGC5236 Mrk789 NGC5194 Mrk477 NGC5674 Mrk66 NGC5135 NGC5102 IC 3961 NGC5005 IC3639 NGC5643 1350-00 UGC8315N NGC4861+ NGC4853 MCG6-28-44 NGC4826 NGC4748 NGC4736 NGC4670 UGC7905S NGC4449 MCG8-23-35 NGC4388 NGC4385 NGC4594 NGC4569 NGC4382 NGC4350 NGC4321 NGC4314 NGC4258 NGC4214 NGC4194 NGC4111 NGC4102 NGC4579 NGC4500 ES0572-34 NGC3995 NGC3994 NGC3991 NGC3982 MCG-1-30-33 NGC3758 NGC3738 NGC3690 American Astronomical Society •Provided bythe NASA Astrophysics Data System Im Am. SBbc Sd pec.,pair Cl. Irr. SBd Sa pec. Sc 2-nuc. dE pair ofEs Irr. pec. 2-nuc. SAd SBc 2-nuc. Sbc SABb SBb SAO pec. S Sb Im Im Comp. SBb/Sc SBc S SO Am. IBm lABm Sb SAab, SBb Sm pec. Sab SBab SO pec. SO Sbc SBa pec. SBc Sm pec. SO Sb Sa Sab SABab SBa Sm Sc Im Sbc Sb SO, 2-nuc. Irr. IV Sc pec. Type Class Morph. Activity SB nuc. SB nuc. SB nuc. Sy2 HII Sy 2 SB nuc. Sy2+Lin SB nuc. SB nuc. SB ring SB nuc. SB nuc. BCDG Sy2 Sy 2 Lin BCG Sy2 SB nuc. SB nuc. BCDG Sy 2 Sy 2 Sy 2 Lin BCDG BCDG BCDG BCG Syl Lin Lin Sy 2 HII BCDG Sy2 SB nuc. BCDG BCG SB nuc. Hs Lin Lin BCG Lin Lin/HII HII HII Lin BCG Sy2 SB nuc. Syl &HII SB nuc. Lin Lin Lin BCG HII 395 8353* 3963* 520 464 4157 4729 251 9593 6525* 420 8785* 3304* 665* 5398* 831 2970 7472* 15230* 831 413 4110 1365 1815* 7595* 1143 1022 311 4875* -261 463 1213* 11379* 3309* 207 281* 2487 883 291 2506* 791 865 3353 3096* 3192* 5167* 1194 10946* 13421* 3115* 2142 739 8912* 224 2988 1076 1075* 1089 1805 1184 1568 1102 km s" v H TABLE 1—Continued 8.18 8.51 8.98 12.79* 14.4* 15.4 11.11 14.00p* 14.09p* 11.86 14.5 13.45 14.5 15.0 12.94 13.2* 15.45* 14.83* 10.64 15.2 9.37 14.20 12.1 15.4p* 10.89 14.67p* 10.64 12.8 8.92 9.85 13.70p* 12.8 14.41* 8.95 15.3* 9.28 12.3 13.3* 13.05 14.1 14.84a 11.83 11.88 11.35 10.22 13.01* 11.75 14.19p* 12.8 13.5* 11.91 14.5 13.01p* 10.56 13.1* 13.05 10.10 10.11 15.2p* 12.14 10.23 12.02 Bt -21.51 -22.94* -18.2 -21.11 -21.76c -21.69 -20.50*o 0.03 -22.24* -20.93* -21.12 -21.91c -21.60 -21.46* -16.63*a 0.01 -21.01c 0.01 -20.62c -22.55 -18.73 -17.95*o 0.00 -22.47 -21.39c -22.31* -21.20 -22.08* -16.60 -21.78 -18.64 -18.64 -21.67* -22.15* -20.61 -20.81 -19.01 -21.29b -18.84 -19.33 -19.80 -21.93 -20.81* -20.74* -21.23* -22.81 -21.69 -22.31 -21.05 -20.38 -21.60 -19.82 -21.91 -19.80 -22.05 -18.79 -20.71*c -20.30 -20.52c -21.21* -21.02* -17.21 -22.30 -17.44*o 0.02 H =bO M 0 b 0.00 0.01 0.02 0.05 0.03 0.00 0.03 0.02 0.00 0.03 0.03 0.00 0.00 0.00 0.06 0.05 0.09 0.00 0.02 0.12 0.00 0.00 0.00 0.00 0.00 0.02 0.01 0.04 0.00 0.00 0.00 0.00 0.00 0.00 0.06 0.04 0.00 0.03 0.02 0.01 0.01 0.01 0.02 0.00 0.00 0.00 0.00 0.01 0.01 0.01 0.00 0.01 0.03 0.02 0.00 0.00 0.00 0.00 E(B-V) 1 339.2 53.8 5.8 334.1 314.9 81.4 35.3 313.9 314.6 335.9 29.5 87.8 71.3 58.8 337.3 38.1 311.7 32.5 93.0 355.9 321.4 37.0 102.0 309.7 49.8 102.7 111.3 33.4 104.9 68.6 315.7 84.4 113.8 59.3 102.8 303.2 49.5 101.6 111.5 212.7 88.6 111.5 110.6 84.5 300.6 290.4 74.4 288.8 62.7 267.7 79.2 270.1 271.1 286.1 298.5 288.5 75.6 279.1 74.3 273.7 55.3 226.8 72.1 123.4 76.0 125.3 62.2 136.8 134.1 68.1 138.1 185.8 77.3 187.7 83.1 138.3 68.8 160.3 78.1 134.4 61.8 149.5 185.9 77.2 185.7 77.2 138.8 60.3 128.1 144.6 59.3 141.9 55.4 59.8 45.2 45.5 48.6 49.0 72.7 59.2 30.1 67.0 58.5 28.9 32.0 71.3 63.2 56.8 57.4 70.9 25.8 77.1 82.1 79.2 82.1 88.3 15.0 72.4 42.1 26.1 71.7 63.1 51.1 59.0 77.8 76.9 14 1039.1 14 0126.6 13 5339.8 13 5010.8 13 3705.0 13 3615.0 13 3436.0 16 3505.1 16 1024.5 16 0301.2 15 4437.8 15 3548.4 15 0444.3 14 4855.1 13 3411.0 13 2955.4 14 3937.2 14 3903.0 14 3122.3 14 2928.0 14 1506.1 13 2745.8 13 2357.8 13 2257.0 13 1907.0 13 1153.5 13 0838.6 12 5638.5 12 5638.5 12 5610.4 12 5432.6 12 5416.9 12 4935.1 12 4832.0 12 4249.8 12 4132.4 12 2545.9 12 3811.0 12 3512.6 12 2351.7 12 2314.8 12 2309.2 12 2125.1 12 2023.2 12 2002.0 12 1629.7 12 1308.0 12 1141.7 12 3724.2 12 3418.7 12 2902.6 12 2253.2 12 0431.0 12 0351.6 11 5625.0 11 5510.3 11 5502.3 11 5456.3 11 5352.3 11 4411.4 11 3352.5 11 3304.5 11 2544.2 a (1950) (h-m-s) -02 5826 -31 2330 -32 4506 -29 3648 -17 0230 -43 5712 -29 3424 -36 2212 -13 0834 -36 2900 -11 2059 -18 4454 -03 3354 (d-m-s) Names 6 (1950)Other 54 3525 48 31 42 4953 00 2237 47 2712 78 1805 52 3506 20 4043 55 2534 35 4636 53 42 05 4043 57 3039 27 0515 18 3640 39 2441 37 1923 35 0656 35 0656 27 5203 32 4304 21 5718 41 2327 44 2216 48 4613 18 0138 11 2143 27 2358 55 1008 00 5053 47 3451 43 2037 58 1426 30 1025 36 22 54 4821 52 5923 32 3424 32 3323 32 3654 55 2410 21 5224 54 4758 58 5023 12 5618 18 2803 16 5821 16 0600 12 0540 13 2618 Mrkl376 VIII Zw323 I Zw92 M101 Mrk463 Um619 HARO10 Mrk266a,b M83 Mrk829, IIZw70 UGC9369 MCG-05-32-052 M51a MCG+10-19-072 MCG-05-32-013 UGC10470 Mrk496 Mrk297 Mrk691 Mrk487 Mrk480S MCG-03-37-005 MCG-07-30-003 MCG-06-29-031 MCG+07-27-052 II Zw67 Mrk673 UGC8256 Mrk59 Mrk59 Mrk54 IRAS1249-131 M64 TOL1238-364 UGC7592 Mrk209 UGC7520 Mrk52 M94 UGC7930 M85 UGC7473 M100 M106 Arp248B Mrk220 M58 M90 Mrk213 UGC7443 UGC7208 Mrk201 UGC7103 UGC7096 POX 36 M104 UGC6944 UGC6936 UGC6933 UGC6918 Mrk739 UGC6565 Mrkl71 1993ApJS ... 86 ....5K the samescale.ThespectraarefromstellaratlasofFanelli in threelinesofsightthrough ourGalaxy.Table5liststhe et al.(1992)andareseparated byluminosityclass. Figure 3showsbluecompact,compactdwarf,andSeyfert and LINERgalaxies;Figure2showsstarburst and plotted intherestframe.Figure1showsnormalspiralgalaxies ent inthespectraofearly-type stars.Table6liststheabsorp- discrete features—absorption, emission,andPCygni—pres- 4 showsOandBstars,whileFigure5displaysA-Mall on 2 galaxies.Asanaidtotheinterpretationoftheseplots,Figure Table 4liststhestrengthsofUV interstellarabsorptionlines Q-1 _l 1-1 -1 the extinction-correctedB°. tions toderiveB%havebeentakenfromThuan&Martin1981;b—B%GordonGottesmanc—galaxiesforwhichBorv both the apparentmagnitudecorrectedforGalacticandinternalabsorption,B,assumingH=50kmsMpc.Forrecessionvelocities rl4,rl5 calculate anapproximatevalueforM.Thesymbolindicatesalso approximateMforgalaxieswithbothvandBfromRC3,butwithout range 500-3000kms,butnotbelongingtoacluster;m—thismarksthedistancescalculatedthroughdistancemodulus;a—Borcorrec- been obtainedfromB°(RC3),assumingasdistancetheofcluster. between 500and3000kms'Mhasbeencalculatedwiththeusualformulaaftercheckingthatitisnotnearacluster.Forv>s the general small).TheabsolutemagnitudeMisobtainedfromRC3usingthevelocityreducedwithrespecttoGalacticstandardofrest, u, Galactic andinternalabsorptionfromarecessionvelocityreducedtothecentroidofLocalGroup(cf.RSA). the apparentmagnitudeinBsystemofRC2,Misabsolutecalculatedfromancorrected for have beentakenfromNED(NASAExtragalacticDatabase),sincethey arenotreportedinRSAorRC3;thesamevalueshavebeenusedto formula hasbeenappliedwithoutproblem.Redshiftcorrectionswereforv>10,000kms.Forgalaxiesbelongingtoacluster,M has compact galaxiesandbluedwarf(whereagalaxyisconsideredtobeifithasMfainterthan-20);Sy2 are E{B -V)fromourGalaxyisBurstein&Heiles1984.Theactivityclassificationasfollows:BCGandBCDGare,respectively, blue tion. Specificsymbolsare:Am.=amorphous,Comp.compact,Cl.Irr.clumpyirregular,2-nuc.presenceoftwonuclei.Thereddening uncorrected apparentmagnitudefromtheRC3;visVorwhenfirstnotavailable(thedifferencebetweentwo isin Keel etal.1985.(rl9)Netzer,Kollatschny,&Fricke1987. (r9) Keel1983c.(rlO)DeRobertis&Osterbrock1986.(rl1)Huchra,Wyatt,Davis1982.(rl2)Heckmanetal.1983.(rl3)MoorwoodOliva Kollatschny &Fricke1986.(r5)Phillips,Charles,Baldwin1983.(r6)Lamb,etal.1985.(r7)ZamoranoRego(r8)Joseph1984. classification hasbeenusedforeachgalaxy.ThefirstcolumngivesthefigurenumbergalaxiestreatedindividuaUyinthispaper.Ifno spectra typicalofaHnregion. Seyfert 2galaxies;SBnuc.aregalaxiesexperiencingastarburstintheirnuclei;HshotspotLinLINERs;HII with otherwise comefromtheNASAExtragalacticDatabase(NED).ThemorphologicaltypefoUows,wherepossible,classicalHubbleclassifica- number isgiven,areferencefortheactivityclassificationgivenaslistedbelow: 1988. (rl4)Heckman1980.(rl5)Osterbrock&Cohen1982.(rl6)Véron-CettyVéron1986.(rl7)Lamb,Bushouse,Towns1989. (rl8) T TH T0 B BHT T T B B GSR TB B B H2lovX Fig. rl6 rl3 rl5 rl6 rl3 no. 112 111 110 109 108 107 106 105 104 Other notation:p—whenBhnotavailablefromRC3,thephotographicmagnitudehasbeenreported;o—marksgalaxieswithredshiftin An asteriskfoUowingavalueofv,BorMmeansthefollowing:Thevaluesandcorrespondtoheliocentricvelocity The recessionvelocity(v)andtheapparentmagnitude(BarefromRSAwhennomarksshown;vishelicoentricvelocity,B is The criterionfordefiningtheclassisnotbasedonphysicalconsiderationsbutcomesfromliterature,wheremostwidelyaccepted The names,cross-identifications,coordinates,andsomeofthemorphologicaltypesaretakenfirstfromRSAorliterature, References.—(rl) Thuan&Martin1981(BCDG).(r2)GordonGottesman(BCG).(r3)MazzareHaBalzano1986(Mrk).(r4) T HTB HrT SW LWGalaxy © American Astronomical Society • Provided by theNASA Astrophysics Data System NGC7496 NGC7793 NGC7714 NGC7582 NGC7552 TOL1924-416 Mrk542 NGC7673 NGC7590 Mrk309 NGC7250 NGC7130 NGC6764 NGC6221 Mrk499 1941-543 Name SAd Sdm pec. Comp. Cl. Irr. SAbc SBbc SBab SBc S/I Sa pec. Comp. pec. SBb SABbc pec. Type Morph. UV SPECTRAOFSTAR-FORMINGGALAXIES SB nuc. SB nuc. HII HII Sy2 Sy2+SB Sy2+HII SB nuc.? SB nuc. Sy2-|-SB nuc. HII BCG Sy2-fSB Lin/HII BCG Activity Class 217 3401* 7354* 2799* 4796 5625* 2869* 2416* 1509 1589 1472 7710* 1498 12636 1157* 1478 km s” v H TABLE 1—Continued Notes toTable1 9.65 15.8p* 13.00* 13.17* 12.20 11.46 11.40 11.78 15.3 13.22* 12.92 15.0* 13.3* 12.56* 11.52 14.9* Bt -21.49 -18.85 -20.04c -21.24* -21.47* -20.78 -21.75 -20.89 -20.11*o 0.15 -22.32c -22.27 -20.37* -20.79*o 0.07 -21.46*o 0.06 -21.55 -21.12* 0.00 M E(B-V) NED. Notethatsomegalaxiesareextended,sothe WE tion featuresduetomid-late-typestars.Table7listsemis- the WEaperturecontains entiregalaxydisk(forexample, are describedin§4.1. NGC 4385,witharadiusof 6"). Thusthefluxesinthistable a radiusof80'),whileothergalaxies aremuchsmaller,sothat aperture containsonlythebulge (forexample,NGC224,with object. Theradiusgivenishalfofthelargestdiameterfrom sion linesfromnebularregions.ThesecontributorstoUV flux represent variousportionsof thebulgeplusdiskdependingon b Table 8containsfluxesandanapproximateradiusforthe = 50 0.04 0.00 0.02 0.04 0.00 0.00 0.00 0.00 0.05 0.00 0.04 4.5 99.2 348.2 348.1 348.1 347.8 93.1 88.2 91.3 94.0 9.9 343.6 81.5 356.9 329.7 75.2 -65.2 -35.4 -65.8 -65.7 -63.8 -30.8 -13.5 -77.2 -61.8 -55.6 -50.4 -29.4 -24.1 -9.6 40.0 18.2 23 2511.8 23 1610.0 23 1538.0 23 0659.0 23 5515.0 23 5425.8 23 3341.0 23 1325.0 22 5009.9 22 1608.7 21 4520.0 19 4103.0 19 2429.0 19 0701.2 16 4826.0 16 4702.6 a (1950) (h-m-s) -42 3042 -42 5124 -43 4200 -32 5206 -02 2141 -42 3836 -35 1106 40 1841 -54 2218 -41 4036 -59 0800 6 (1950)Other (d-m-s) Names 23 1851 01 5242 24 2754 50 5108 48 4744 IC5294 MCG-06-01-009 UM 191 Mrk538 Mrk325 ESO 347-G033 ESO 291-GOOl ESO 291-G016 Mrk907 IC5135 ESO 185-IG013 ESO 338-IG004 ESO 138-G003 UGC11407 UGC10565 1993ApJS ... 86 ....5K ß hm their lowsignal-to-noiseratio;thesegalaxieshavenotbeen the endofthispaper),orderedbyrightascension.About 25% lines andfittingapowerlawtothecontinuum)arefound which arecommontothisatlasandtheworkofKinneyetal. tinction inthesegalaxiesmayhaveadifferentwavelengthde- wavelengths wheretheUVextinctioncurveofGalaxy[AJ the galaxysize.Theaverageobservedultravioletfluxisgiven curve andtheLMCextinctioncurve. eddening ofstarburstgalaxiesusingbothaGalacticextinction Cloud (LMC)extinctioncurve.Figure7demonstratesthe der- also dereddenedtwogalaxiesusingtheLargeMagellanic siderably lowerthanthatofthesolarneighborhood,wehave agree towithin1a. (1991a, whereslopesweremeasuredbyremovingtheemission on thetopofeachplot.TheslopesfourSeyfert2galaxies activity classinFigure6,withthemedianandvarianceshown uniform estimateforthetrueintrinsicUVslope. pendence fromthatofourGalaxy,butmethodproducesa correct whennoextinctionispresent.Ofcourse,theUVex- dent ofextinctionlikethattheMilkyWay,andisalso parameters areshowninTable9,orderedbyactivityclass.A wave bandswerechosentocorrespondthethreedifferent lengths 1482,1913,2373,and2700Â.Thefirstthreeofthese of thegalaxyspectrahavelittlespectralinformationbecause of slope thatisbasedonregionswithequalextinctionindepen- values havebeenfittedtoF=\,andtheresultsfor along withthevariancein100Âregions,centeredonwave- 10 M51 132745.8 M64 125416.9 M33 013104.6 M31 004000?0 particularly interesting.(Theentiredataset,includingobjects E(B- V);Seaton1979]hasthesamevalue.Thesethreeflux M106 121629.7 M104 123724.2 M101 140126.6 M100 122023.2 M95 104119.6 M94 124832.0 M90 123418.7 M85 122253.2 M83 133411.0 M81 095127.6 M77 024006.5 M58 123512.6 ground fluxnumberisshown atthebottomasadottedfine. tal formasdescribedbelow.) Thegrossfluxnumber(FN)is extracted butnotshowninthispaper,willbeavailabledigi- shown inthefiguresexceptcaseswhereobjectitself is age ofthetotalflux.Thespectrum itselfisplottedinunitsof Above thegrossandbackground FN,1aisplottedaspercent- shown atthebottomofeach plotasasolidfine.Theback- x0 Given thatmanyoftheatlasgalaxieshavemetallicitiescon- The distributionsofslopes,ß,areshownashistogramsby The spectraaredisplayedindividuallyinFigures8-112(at Galaxy Other Name «(1950)0(1950) © American Astronomical Society • Provided by theNASA Astrophysics Data System Messier Galaxies TABLE 2 -11 2059NGC4594 -29 3648NGC5236 -00 1332NGC1068 o 47 2712NGC5194 4100'06" NGC224 41 2327NGC4736 47 3451NGC4258 69 1813NGC3031 21 5718NGC4826 30 2340NGC598 54 3525NGC5457 13 2618NGC4569 18 2803NGC4382 12 0540NGC4579 16 0600NGC4321 11 5800NGC3351 KINNEY ETAL. -2-1 (1980); wavelengthsforabsorptionfinesfromthegalaxiesare lengths foremissionfinesshownontheplotsarefromUlrich Galaxy arefromMorton,York,&Jenkins(1989);wave- Galaxy. Thewavelengthsfortheabsorptionfinesfromour spectrum toflagsometypicalstrongabsorptionfinesfromour marked attheredshiftofgalaxy.Abarisdrawnbeneath plot withthelocationoftypicalabsorptionandemissionlines ergs cmsÁ.Ahorizontalbarisdrawnatthetopof Mrk 499. Mrk 496b Mrk 66.. Mrk 59.. Mrk 54.. Mrk 960. Mrk 907. Mrk 829. Mrk 799. Mrk 789. Mrk 739. Mrk 710. Mrk 691. Mrk 673. Mrk 617. Mrk 542. Mrk 538. Mrk 496a Mrk 487. Mrk 480S Mrk 477. Mrk 463. Mrk 357. Mrk 347. Mrk 116. Mrk 108. Mrk 86.. Mrk 52.. Mrk 36.. Mrk 35.. Mrk 33.. Mrk 8... Mrk 7... Mrk 1267 Mrk 1063 Mrk 1027 Mrk 348. Mrk 325. Mrk 309. Mrk 297. Mrk 266b Mrk 266a Mrk 235. Mrk 220. Mrk 213. Mrk 209. Mrk 201. Mrk 171. Mrk 170. Mrk 153. Mrk 25.. Mrk 19.. Mrk 1291 Mrk 1376 Galaxy Name hm 09 12 07 2339.4 072220?0 08 0942.5 04 3135.5 01 1956.6 00 4604.4 00 4517.0 09 1726.1 00 4604.8 09 52 23 3341.0 23 2511.8 09 3030.3 02 5207.0 02 1128.8 23 5425.8 22 5009.9 22 1608.7 23 2511.8 12 5638.5 12 5432.6 12 2309.2 11 02 13 2357.8 10 42 10 29 10 00 15 3548.4 15 0444.3 13 5339.8 14 15 16 4702.6 16 1024.5 16 1024.5 14 3903.0 16 0301.2 14 4855.1 13 5908.5 13 29 11 33 15 44 13 3615.0 13 3615.0 11 2355.8 10 4603.8 10 5028.4 12 4132.4 12 2902.6 12 2351.7 12 1141.7 11 2544.2 14 1039.1 11 2100.1 a (1950) Marrarían Galaxies 22.9 22.0 53.5 06.1 55.4 52.5 37.8 15.6 16.5 10.2 TABLE 3 -02 5826 -08 2301 -10 1343 -12 5922 -08 4042 -02 2141 ô (1950) 00 5053 46 0832 29 2434 72 1355 72°4033" 64 2657 57 3039 35 0656 32 4304 56 1323 54 3934 59 4050 59 5853 48 3154 48 3148 04 5352 04 5633 01 5242 42 4953 22 5430 22 0607 23 1851 24 2754 20 4043 23 1851 48 4613 64 2446 55 2746 40 1841 09 3032 48 4744 52 3550 21 5224 27 0515 53 4253 31 4100 55 1008 58 1426 54 4821 58 5023 59 3416 52 3508 52 3506 55 2534 35 4636 18 3640 11 2143 18 0138 NGC 4861 MCG 6-28-44 NGC 4385 UGC A225 NGC 3353,H3 UGC 5720,H2 UGC 5408 UGC 3838 NGC 2820A NGC 2537 MCG 10-19-072 MCG 10-13-71 IC2184 UGC 6448 UGC A166 NGC 4194 NGC 3690 MCG 9-18-32 UGC 9560 NGC 3758 NGC 3049 NGC 6052 NGC 7673 UGC 7905 NGC 4500 MCG 8-23-35 NGC 3660 NGC 1140 Haro 15 NGC 7250 NGC 5430 VIII Zw323 NGC 5996 NGC 1614 NGC 7714 UGC 10565 NGC 6090 NGC 6090 UGC A410 NGC 5860 UGC 8850 NGC 262 IC 1586 NGC 7*673 NGC 5256 Mrk 266a NGC 5506 IC214 IC 4395 1050+04 Name Other Vol. 86 1993ApJS ... 86. lß a2ß the unitsofabscissaareHz.Thegalaxiesdisplayedattheirrest wavelengths,andtheMgnX2800,Cm]XI909,ivXI550featuresaremarked. Because spectralslopeiscommonly quotedasFocy“,wegive vF ocv~~. of flux,F,versuswavelength, X.SlopesarequotedinFocX^. quency, logv,whiletheplots ofindividualobjectsareinunits F ozv=v~~ No correctionismadeforextinction. et al.(1984),andFanelli (1987,1990). from Panek&Savage(1976),Nussbaumeretal.(1982),Heck theconversionbetweenthesethreesystemshere: v v x x ß No. 1,1993UVSPECTRAOFSTAR-FORMINGGALAXIES -2-1 Fig. 1.—SpectralenergydistributionofLINERsandnormalspiralgalaxies orderedbyspectralslope.Theunitsoftheordinateareergscms,while Figures 1-5areinunitsof energy,log(vF),versusfre- F ocX, v x © American Astronomical Society • Provided by theNASA Astrophysics Data System Liner GalaxiesNormal 15.0 15.1515.3 15.0 15.1515.3 Log (l/) il 1993ApJS ... 86 ....5K l -2 wavelengths. Likewise,“red” isusedtoreferspectrathat have weakfluxatshortUVwavelengths comparedtotheflux short UVwavelengthscompared withthefluxatlongUV Hz. as arelativetermtorefer spectrathathavestrongfluxat and vFccv~Andiscussions concerningslopes,“blue”isused i.e., withaslopeofß=0,hascorrespondingslopesofF,,oc y, v 12 21 Fig. 2.—Spectralenergydistributionofstarburstgalaxies,orderedby slope.Theunitsoftheordinateareergscms,whileabscissa A spectrumofapproximatelyconstantfluxinFversus X, x © American Astronomical Society • Provided by theNASA Astrophysics Data System J k 0 Ö0 à à _ NGC7793SAd r 15.0 15.1515.3 15.0 15.1515.3 NGC3690 Scpec NGC7673 ClIrr NGC5253 ImAm NGC4214 lABra NGC4449 ffim cm civ i Starburst Galaxies KINNEY ETAL. S||k^ NGC3440 IrrAm,, Mgii Icmciv i NGC7714 SdmPec Log (y) digital formthroughseveral routes.TheNationalSpace 0 (a=-2)isredderthanaslopeofß-1). at longUVwavelengths.Inthisterminology,aslopeof ß= The atlaswillbeavailabletothe astronomicalcommunityin 3. DIGITALDISTRIBUTIONOF THEATLAS NGC6052 ClIrr cm civ i Vol. 86 : No. 1, 1993 UV SPECTRA OF STAR-FORMING GALAXIES 13

BCG k BCDG BCG k BCDG Seyfert II ft cm civ cm civ :«ii I cm civ i i i MK477 Comp.

NGC4861 Im

NGC3353 Im,

NGC1705 Irr Am

UGC5720 Im

UGCA166 Irr

NGC3125 Irr Am

UGC9560 Irr Pec NGC24I5 Irr pec NGC1068 Sb

bfl NGC3991Im ^ 0 , NGC4500 Sba lUv NGC3081 1

1050+04

wf IC3639 SBb

MCG6-28-44 NGC4194 Sm pec

15.0 15.15 15.3 15.0 15.15 15.3 15.0 15.15 15.3

Log M Fig. 3.—Spectral energy distribution of blue compact, blue compact dwarf, and Seyfert 2 galaxies, ordered by slope

Science Data Center (NSSDC) will contain the Atlas in their sent to the SPAN address NCF: ¡Request or to the Internet Astrophysics Data Catalogues (ADC). Requests can be di- address [email protected].nasa.gov. The tape format is the rected to Requests, National Space Science Data Center, Code IUE format with character header and 16 bit integer data, ex- 933, Greenbelt, MD 20771. International requests can be di- cept that the usual group of seven quantities (wavelength, data rected to Requests, World Data Center A for Rockets and Satel- quality, gross, background, FN, s-1, and flux) have been sup- lites, Code 930.2, NASA/Goddard Space Flight Center, plemented by an error array and an exposure time array. The Greenbelt, MD 20771. Requests via electronic mail can be fifth quantity is just FN on a standard IUE tape, and the correc-

© American Astronomical Society • Provided by the NASA Astrophysics Data System 1993ApJS ... 86 ....5K tion forchangingIUEsensitivityisappliedtothefluxarray mous FTPatnodestsci.edu( 130.167.1.2).Thedataresidein the atlaswillbeavailablevia theDataManagementFacility/ the directoryobserver/catalogs/iue galaxyatlas.Eventually file. only. Theon-lineformatisheaderanddata,allinoneASCII STScI. DMF/DADS doesnotnowhavethe capabilityforon- Data ArchivingandDistribution System(DMF/DADS)at 14 KINNEYETAL.Vol.86 The atlaswillalsobeavailable foralimitedtimeviaanony- © American Astronomical Society • Provided by theNASA Astrophysics Data System Fig. 4.—SpectralenergydistributionofOandBstarsfromtheFanelli etal.(1992)atlas 0-B ClassI1II-1VV Log(n) the ISMofourGalaxy,in ISMofthegalaxyitself,orin stellar atmospheres ofstarscontributingto the UVfluxof ity inthefuture. line accesstoarchiveddatabutisexpectedhavesuchcapabil- The absorptionfeaturesingalaxy spectracanoriginatein 4.1. UVAbsorptionandEmission Signatures 4. DISCUSSION 1993ApJS ... 86. fines, andfineswithPCygni profilefromearly-typestarsare gions produceemissionlines. Table4summarizestheequiva- sight throughourGalaxy.Typical absorptionfines,emission lent widthsofISMabsorption linesdetectedinseveralfinesof absorption (PCygniprofiles), andcoolstarscanproduceab- produce emissionlinesandfeatureswithboth and galaxy. Inadditiontoproducingabsorptionlines,hotstars can sorption linessimilartothose producedintheISM.Hnre- No. 1,1993 © American Astronomical Society • Provided by theNASA Astrophysics Data System A-M Class1III-IVV UV SPECTRAOFSTAR-FORMINGGALAXIES type starsaresummarizedinTable6.Typicalemissionfines from nebularregionsaresummarized inTable7. summarized inTable5.Typicalabsorptionfinesfromlate- sorbs bothdiscreteandcontinuous radiationfromexternal The diffusemediumassociated withourownGalaxyab- 4.1.1. InterstellarAbsorptionLines 15 1993ApJS ... 86 ....5K 2906 2733 2530 2511 2385 2297 2009, 2010 1907, 1909 1719 1640 1600-1630 blend 1548,1551 1486 1465 1453 1428 1394, 1403 1371 1336 1333 1300 1255 1239,1243 References.—(1) Panek&Savage 1976;(2)Nussbaumeretal.1982;(3)Heck1984. Note.—In cols.(3)-(6),a=absorption (W^>0);e=emission0.66 >0.50 <1.64 0.53 0.20 0.73 0.22 0.53 0.75 0.10 0.18 0.39 0.60 0.14 0.58 0.24 0.39 1.05 ^x(A) e e e e WC e e e e e e/p e/p (6) SN 1980K 3.3 3.7 1.6 1.6 1.9 References 2 2 2 2 2 2 2 2 2 3 3 3 3 3 3 3 3 1,2,3 1,2 1 1,2,3 1,2,3 1,2 (7) 1993ApJS ... 86 ....5K -1 galaxies. Thedustcomponentisresponsibleforthecontinuum tected onlyinIUEspectrawithmuchhighersignal-to-noise wavelengths, bothinthediskandhaloofourGalaxy. the interstellargasisresponsibleforabsorptionatdiscrete if afullwidthathalf-maximumof7ÂisadoptedfortheSW discussed in§2.2anddemonstratedFigure7.Inaddition, for thiseffectintheestimationoftruespectralslopesis absorption, whichreddenstheoriginalspectrum.Allowance ratios thanthosepresentedhere. camera, anabsorptionlinewithintrinsicequivalentwidth appear inthelow-resolutionspectrathisatlas.Forexample, mode (^1000kms).Therefore,onlythestrongestISlines much narrowerthantheIUEresolutioninlow-dispersion fact, withtheexceptionofLyaline,theirintrinsicwidthis of —7%thecontinuumlevel.Suchfaintlinescanbede- of 0.5Âwillappearasaweakfeaturewithtroughminimum 2852 Mgia2 2800 Mgii...a2 2600 Fen...a2 2400 Fen...a2 3000 FeIa2 1855,1863 Aima1 1671 Aina1 Main DiscreteFeaturesinSpectraofMid-toLate-TypeStarsUnesandlinestrengthsexpectedthespectrumextragalac- In general,interstellar(IS)absorptionUnesarenarrow. Note.—In cols.(3)-(6),a=absorption(W^>0). References.—(1) Fanellietal.1987;(2)1990. X (À)IonAFGKReferences (1) (2)(3)(4)(5)(6)(7) © American Astronomical Society • Provided by theNASA Astrophysics Data System 2796, 2803 2325-2329 2837 2837,2838 2733 2470 2423, 2425 3133 3023 3043, 3047 1335,1336 1882,1892 1747-1754 1658-1666 1640 1548, 1550 1483, 1487 1397-1407 1394, 1403 1239, 1243 1907, 1909 Wavelength 1 -- -=ticobjects,Table4presentsacompilationofthestrongestIS (A) TABLE 6Ratherthanresortingtotheoreticalmodelsestimatethe Nv N rv] O iv] Si rv C n Cn] N in] Om] Hen C rv Om O m Cn Mgn C m] Si m] O m O m He ii [On] [Ne rv] Ion UV SPECTRAOFSTAR-FORMINGGALAXIES17 Main EmissionLinesfromNebularObjects Regions H ii TABLE 7 PNs 1 their Galacticlatitudesdifferby97°(b73=64°b tic origin. taken fromtheIUEhigh-dispersionobservationsofBladeset km s“,whichBladesetal.(1988b)haveshowntobeofGalac- Hubble SpaceTelescope(observedwiththeFaintObjectSpec- ground sources. the spectrumofSN1980KinNGC6946(b=126°;Pettiniet distribution oftheabsorbinggasrelativetoourGalacticplane. zation ionsarestrongertoward3C273thantheLMC, al. (1988a),includingallcomponentswithvelocitiesupto80 trograph [FOS]ataresolutionof1300intheinterval1150- absorption Unesdetectedinthespectraof3C273andSN suggesting thatthereisasizableasymmetryinthelarge-scale However, theequivalentwidthsoffewISUnesdetectedin observed withtheGoddardHighResolutionSpectrograph al. 1982)areaboutafactorof3.4higherthanthosetoward3C and ataresolutionof15,000intheintervals1522-1556, (GHRS) ataresolutionof1500intheinterval1175-1452Â, values (sin64°/sin12°=4.3). 273, i.e.,approximatelytheratiooftheirrespectivecosecant -33° ).Theabsorptionsfromboththelow-andhigh-ioni- high-resolution mode(Burksetal.1991). spectra takenwiththeSWPcamera(1200-2000Á)in 3300 Á,withagapfrom1600to1650byBahcalletal.1991; 3C25LJAC 1987A, whichareamongthebrightestextragalacticback- 1991) withtheresultsobtainedIUEbyco-adding10 1775-1813, 2572-2617,and2777-2821ÂbyMorrisetal. The twoUnesofsightprobedifferentpartsthedisk,since The ISUneintensitiesfortheofsighttoSN1987Àare For 3C273wehavecombinedtheresultsobtainedwith Crab O-rich N-rich SNR Cygnus Loop 1993ApJS ... 86 ....5K IZW18 IC2184 NGC1140 IC214 IC1586 NGC3081 NGC3049 NGC3031 NGC2997 NGC2903 NGC2841 NGC2820A NGC2798 MCG10-13-71 NGC2782 NGC2681 NGC2639 UGC4483 Holmbergll NGC2537 NGC2415 NGC2403 UGC3838 NGC1800 NGC1705 NGC1667 NGC1672 NGC1614 NGC1569 NGC1553 NGC1510 NGC1433 NGC1313 NGC1097 NGC1068 NGC1023 NGC598 MRK357 ES0296-11 HAR015 NGC262 NGC224 Galaxy MCG9-18-32 NGC3353 NGC3351 NGC3310 UGC5720 NGC3256 NGC3125 UGC5408 NGC3077 NGC3432 NGC3396 NGC3395 NGC3393 UGC6448 NGC3660 NGC3622 MRK36 NGC3504 NGC3448 1050+04 81421 NGC3758 NGC3738 NGC3690 NGC3682 UGC6456 b NGC3994 NGC3991 NGC3982 MCG-1-30-33 NGC3995 Fluxesareinunitsof10ergscmsÄ^ RadiusishalfthelargestdiameterforgalaxyasgiveninNED. 6 Radius 1432-1532Â1863-1963Ä2323-2423Á2650-2750Á , © American Astronomical Society • Provided by theNASA Astrophysics Data System , , 1 , 1057" SOÔ" 1327" 242" 3'42" 3'24" I'SS" 154" 2'48" I'SS" I'OS" l'Oô" 4'Z3" l^l" 4'27" ÔS" I'OS" e'is" 3'57" l^l" i'oe" S'lS" ^lö" S'lö" Z'ZS" l15" 1'09" I'IS" 1'45" 1'48" IMS" 124" 30" 33" 24" 39" 15" 42" 36" 45" 51" 30" 15" 54" 33" 51" 27" 24" 60" 57" 54" 39" 39" 51" 24" 30" 15" 27" 15" 9" 10.18 ±1.29 16.84 ±1.49 4.42 ±0.59 2.76 ±0.29 0.93 ±0.29 3.23 ±0.41 0.23 ±0.15 3.92 ±0.46 0.78 ±0.22 0.49 ±0.19 1.96 ±0.40 1.32 ±0.25 1.20 ±0.28 2.75 ±0.40 0.93 ±0.19 4.02 ±0.46 0.85 ±0.27 0.51 ±0.22 0.32 ±0.21 1.34 ±0.24 0.17 ±0.15 2.33 ±0.27 0.66 ±0.38 1.50 ±0.31 1.03 ±0.16 5.22 ±0.47 0.72 ±0.21 0.75 ±0.17 1.02 ±0.46 4.91 ±0.51 0.96 ±0.22 0.33 ±0.19 0.37 ±0.23 0.59 ±0.24 0.69 ±0.27 0.67 ±0.18 0.57 ±0.21 0.97 ±0.18 2.24 ±0.33 0.36 Ï0.20 0.71 ±0.10 0.91 ±0.20 2.50 ±0.35 0.44 ±0.23 0.63 ±0.33 0.97 ±0.20 0.30 ±0.18 3.01 ±0.31 0.56 ±0.22 0.19 ±0.13 2.51 ±0.23 0.59 ±0.23 0.82 ±0.17 2.03 ±0.38 6.64 Ï1.06 0.69 ±0.21 0.58 ±0.22 2.11 ±0.32 0.19 ±0.13 0.59 ±0.14 0.83 ±0.14 1.07 ±0.21 1.39 ±0.19 1.55 ±0.17 1.74 ±0.29 1.56 ±0.33 1.62 ±0.49 1.17 ±0.16 1.12 ±0.17 1.36 ±0.27 2.95 ±0.35 0.75 ±0.09 0.60 ±0.11 0.30 ±0.23 2.47 ±0.25 2.03 ±0.19 1.89 ±0.19 0.65 ±0.10 0.51 ±0.09 0.35 ±0.09 0.88 ±0.13 7.45 ±0.53 1.29 ±0.12 0.31 ±0.16 0.35 ±0.21 0.52 ±0.10 0.86 ±0.10 0.39 ±0.17 0.45 ±0.10 0.51 ±0.09 0.63 ±0.19 0.93 ±0.12 2.15 ±0.18 0.66 ±0.09 1.82 ±0.18 1.00 ±0.12 0.64 ±0.09 0.29 Ï0.07 0.39 ±0.07 0.90 ±0.17 0.57 ±0.08 0.26 ±0.07 0.40 ±0.12 0.62 ±0.12 0.94 ±0.14 8.46 ±0.50 0.26 ±0.09 2.77 ±0.18 0.43 ±0.08 0.81 ±0.12 0.15 ±0.08 0.42 ±0.10 0.53 ±0.10 3.02 ±0.18 0.44 ±0.09 0.88 ±0.08 0.36 ±0.20 2.37 ±0.24 0.57 ±0.15 0.62 ±0.11 0.28 ±0.09 0.24 ±0.08 1.81 ±0.20 1.95 ±0.26 7.53 ±3.00 0.28 ±0.18 0.23 ±0.09 0.48 ±0.05 3.00 ±0.19 0.51 ±0.11 0.53 ±0.10 1.47 ±0.16 1.60 ±0.15 1.89 ±0.31 1.01 ±0.07 0.61 ±0.07 0.90 ±0.17 0.97 ±0.12 1.68 ±0.15 1.32 ±0.11 4.84 ±1.62 0.27 ±0.17 2.09 ±0.33 1.30 ±0.171.200.10 0.20 ±0.10 0.20 ±0.12 1.48 ±0.37 1.85 ±0.17 0.23 ±0.10 0.78 ±0.15 0.38 ±0.27 0.63 ±0.20 0.46 ±0.13 0.57 ±0.140.580.05 0.53 ±0.110.510.06 0.55 ±0.13 0.18 ±0.070.230.03 0.54 ±0.340.590.13 0.32 ±0.170.720.08 0.13 ±0.070.170.04 0.19 ±0.10 0.35 ±0.21 0.40 ±0.21 5.43 ±0.42 2.85 ±0.67 0.69 ±0.13 0.15 ±0.11 0.38 ±0.14 5.51 ±1.54 0.13 Ï0.10 0.76 i0.15 0.39 ±0.21 2.07 ±0.261.710.16 0.46 ±0.280.500.10 0.15 ±0.090.230.04 0.71 ±0.390.620.17 1.77 ±0.28 1.40 ±0.341.280.10 1.03 ±0.13 1.65 ±0.21 0.45 ±0.171.090.14 0.50 ±0.100.520.06 1.86 ±0.322.000.18 1.44 ±0.18 0.69 ±0.110.650.07 1.54 ±0.211.320.07 1.08 ±0.311.020.15 8 Observed Fluxesin100ÂBins 2.23 ±0.18 5.07 ±0.45 0.21 ±0.04 1.74 ±0.07 1.40 ±0.12 4.79 ±0.20 0.22 ±0.03 0.73 ±0.04 0.56 ±0.07 0.62 ±0.08 0.38 ±0.06 2.25 ±0.18 0.42 ±0.07 4.08 ±0.15 0.40 ±0.05 0.29 ±0.08 0.15 ±0.05 0.24 ±0.05 0.41 ±0.10 0.39 ±0.10 2.90 ±0.24 0.40 ±0.08 0.95 ±0.05 0.57 ±0.05 0.91 ±0.06 0.33 ±0.10 1.75 ±0.12 1.56 ±0.08 1.33 ±0.07 TABLE 8 6 18 Galaxy Radius1432-1532Ä1863-1963Â2323-2423Â2650-2750Â NGC4314 NGC4214 NGC4194 NGC4111 NGC4102 ES0572-34 NGC4350 NGC4321 NGC4258 IC3961 IC3639 NGC4594 NGC4579 NGC4569 NGC4500 NGC4449 NGC4385 NGC4382 NGC5102 NGC5005 NGC4861 NGC4853 MCG6-28-44 NGC4826 NGC4748 NGC4736 NGC4670 UGC7905S MCG8-23-35 NGC4388 IC4395 NGC5236 NGC5135 UGC8315N NGC5728 MRK477 NGC5674 NGC5643 NGC5506 NGC5457 UGC8850 NGC5253 NGC5256 ES0383-44 MRK789 NGC5194 MRK66 NGC5860 UGC9560 1350-00 NGC5996 UGCA410 MRK499 NGC6217 NGC6090 NGC6052 TOL1924-41 NGC6221 NGC7590 NGC7582 NGC7552 MRK309 NGC7250 NGC7130 NGC6764 MRK542 NGC7714 NGC7673 NGC7496 1941-543 NGC7793 , , , , , , , , 1424" ÎS" 9'1S" 342" 2'06" 3'33" Tl8" Ï30" 2'48" I'SO" 42l" 445" 2'57" s'oe" ^SO" 42l" s'oo" s'se" 439" I'OO" 2'54" ÔO" ÔO" l^l" 142" 1'45" s'se" 2'18" 2'W" I'IS" 1'33" 124" 1 30 54" 30" 48" 24" 42" 36" 45" 45" 24" 36" 51" 24" 57" 39" 12" 42" 15" 21" 33" 30" 51" 12" 12" 6" 6" 9" 6" 10.34 ±0.93 13.14 ±2.14 23.43 ±3.97 14.11 ±1.10 0.96 ±0.63 2.28 ±0.33 0.15 ±0.10 2.22 ±0.261.170.12 0.17 ±0.12 0.62 ±0.14 1.58 ±0.32 2.14 ±0.25 1.91 ±0.27 1.56 ±0.36 0.29 ±0.11 0.99 ±0.28 0.15 ±0.10 0.28 ±0.20 0.86 ±0.37 0.92 ±0.18 3.81 ±0.25 0.45 ±0.16 0.25 ±0.19 0.41 ±0.24 0.98 ±0.23 6.39 ±0.62 0.46 ±0.27 3.70 ±0.41 2.29 ±0.37 0.41 ±0.19 8.85 ±0.85 9.92 ±0.98 0.19 ±0.12 2.01 ±0.36 1.51 ±0.19 1.06 ±0.25 0.72 ±0.25 1.72 ±0.28 1.43 ±0.21 1.27 ±0.18 0.96 ±0.27 2.47 ±0.21 0.44 ±0.18 0.32 ±0.20 1.01 ±0.28 1.31 ±0.26 0.67 ±0.18 0.32 ±0.20 0.28 ±0.21 0.41 ±0.20 0.26 ±0.19 0.50 ±0.21 0.39 ±0.20 0.44 ±0.20 0.84 ±0.30 0.35 ±0.20 0.64 ±0.24 0.74 ±0.21 3.16 ±0.31 0.36 ±0.18 1.03 ±0.21 1.09 ±0.18 1.06 ±0.16 1.74 ±0.21 1.07 ±0.34 1.31 ±0.28 1.57 ±0.35 1.18 ±0.35 17.09 ±1.22 10.58 ±1.19 0.56 ±0.31 6.34 ±0.39 0.13 ±0.05 4.09 ±0.29 0.46 ±0.09 0.12 i0.07 0.87 ±0.08 0.75 ±0.14 0.28 ±0.09 0.33 ±0.13 0.79 ±0.12 1.66 ±0.11 1.79 ±0.20 1.46 ±0.16 0.42 ±0.11 0.31 ±0.06 0.90 ±0.13 0.70 ±0.19 0.53 ±0.07 2.25 ±0.33 0.46 ±0.07 0.19 ±0.08 5.04 ±0.67 5.47 ±0.86 0.18 ±0.10 0.38 ±0.18 0.92 ±0.25 1.44 ±0.45 1.17 ±0.11 2.55 ±0.26 0.22 ±0.08 2.41 ±0.12 0.30 ±0.07 0.22 ±0.12 1.26 ±0.17 7.09 ±0.76 0.90 ±0.14 0.44 ±0.10 1.91 ±0.19 1.06 ±0.08 1.13 ±0.15 1.52 ±0.11 0.38 ±0.07 0.64 ±0.21 0.61 ±0.07 1.03 ±0.17 0.36 ±0.19 0.67 ±0.24 0.28 ±0.09 0.56 ±0.25 0.38 ±0.31 0.19 ±0.18 0.38 ±0.07 0.17 ±0.12 0.75 ±0.10 0.47 ±0.14 0.19 ±0.09 0.72 ±0.07 0.87 ±0.11 0.76 ±0.15 0.50 ±0.11 1.08 ±0.13 1.78 ±0.14 1.55 ±0.15 1.01 ±0.14 16.43 ±2.60 4.34 ±0.34 0.76 ±0.18 0.15 ±0.07 0.12 ±0.11 0.28 ±0.15 0.13 ±0.07 1.24 ±0.26 0.85 ±0.22 1.72 ±0.29 1.16 ±0.25 0.67 ±0.310.740.15 0.49 ±0.310.12 0.21 ±0.160.360.09 0.28 ±0.21 3.34 ±0.32 2.89 ±0.37 0.23 ±0.10 0.80 ±0.14 0.51 ±0.18 0.54 ±0.16 0.46 ±0.19 0.30 ±0.13 0.20 ±0.12 0.76 ±0.220.700.10 0.80 ±0.451.090.24 2.81 ±0.25 0.56 ±0.11 0.26 ±0.15 1.00 ±0.14 1.41 ±0.111.190.05 0.32 ±0.14 0.48 ±0.14 0.59 ±0.220.730.10 1.55 ±0.252.120.19 1.13 ±0.23 0.27 ±0.08 0.70 ±0.23 5.81 ±0.91 0.58 ±0.160.610.09 1.03 ±0.16 1.94 ±0.56 0.39 ±0.080.320.06 7.41 ±0.77 1.18 ±0.21 1.88 ±0.27 0.36 ±0.12 0.24 ±0.19 0.12 ±0.10 0.15 ±0.110.130.07 0.83 ±0.160.05 0.93 ±0.250.860.14 0.37 ±0.11 0.21 ±0.11 1.13 ±0.16 15.22 ±1.24 0.39 ±0.05 3.55 ±0.12 0.21 ±0.04 0.69 ±0.07 0.87 ±0.05 0.57 ±0.10 0.22 ±0.03 1.45 ±0.13 1.43 ±0.10 0.30 ±0.05 0.29 ±0.04 2.32 ±0.23 0.37 ±0.05 0.81 ±0.08 1.80 ±0.12 2.00 ±0.13 0.33 ±0.05 0.21 ±0.08 0.18 ±0.03 6.54 ±0.23 0.29 ±0.04 0.44 ±0.06 1.00 ±0.07 0.46 ±0.08 0.91 ±0.13 0.27 ±0.03 0.43 ±0.07 2.56 ±0.20 2.45 ±0.19 0.25 ±0.03 0.71 ±0.06 0.69 ±0.07 2.37 ±0.12 4.46 ±0.37 0.54 ±0.05 2.20 ±0.24 0.62 ±0.05 0.49 ±0.08 0.35 ±0.02 0.70 ±0.09 1.41 ±0.15 1993ApJS ... 86 ....5K © American Astronomical Society Galaxy NGC1553 NGC1433 NGC224 NORMAL TOL1924-41 NGC2403 NGC598 NGC2681 LINER NGC4382 NGC3682 NGC4111 NGC3994 NGC3031 NGC2841 IC3961 NGC4853 NGC4579 NGC4314 NGC4258 UGC9560 NGC4861 MCG6-28-44 NGC4500 STARBURST NGC5194 NGC5005 NGC4826 NGC4736 NGC4594 NGC4670 NGC4449 NGC4194 NGC3738 IC2184 NGC1569 NGC3995 NGC3991 NGC3353 UGC5720 NGC2415 UGC3838 NGC3504 NGC3448 NGC3310 NGC3049 NGC2782 NGC3125 UGCA166 NGC2820A NGC1705 NGC1510 NGC1313 BCDG, BCG,HII NGC7250 1050+04 NGC7714 NGC7552 NGC6052 NGC5996 NGC5860 NGC5253 ES0383-44 NGC5236 NGC5102 NGC4385 NGC4214 NGC3690 3 Reddening-free SpectralIndicesListedbyActivityType Provided bythe NASA Astrophysics Data System -2.10 ±0.05 -2.20 ±0.09 -2.06 ±0.07 -2.57 ±0.09 -1.74 ±0.07 -0.94 ±0.21 -0.48 ±0.15 -1.62 ±0.13 -1.75 ±0.12 -0.89 ±0.14 -2.06 ±0.07 -2.03 ±0.10 -1.12 ±0.18 -1.90 ±0.12 -1.87 ±0.09 -1.56 ±0.10 -2.44 ±0.13 -1.62 ±0.24 -2.04 ±0.29 -1.22 ±0.10 -1.20 ±0.38 -1.89 ±0.08 -0.90 ±0.17 -1.75 ±0.63 -2.41 ±0.06 -1.49 ±0.08 -1.28 ±0.14 -1.32 ±0.07 -0.82 ±0.89 -1.02 ±0.16 -1.52 ±0.18 -1.20 ±0.26 -0.57 ±0.08 -1.85 ±0.06 -1.26 ±0.18 -1.22 ±0.27 -0.77 ±0.13 -1.28 ±0.16 -1.31 ±0.11 -1.21 ±0.35 -0.58 ±0.50 -0.95 ±0.28 -0.82 ±0.13 -0.07 ±0.35 -1.23 ±0.44 -1.29 ±0.14 -1.31 ±0.16 -1.98 ±0.37 -1.17 ±0.13 -0.41 ±0.49 -1.25 ±0.45 -1.40 ±0.15 -1.35 ±0.13 -1.25 ±0.11 -1.25 ±0.14 -0.93 ±0.11 0.06 ±0.40 0.26 ±0.14 0.14 ±0.42 0.79 ±0.36 0.06 ±0.28 0.20 ±0.42 0.07 ±0.48 0.17 ±0.40 0.06 ±0.93 0.08 ±0.31 0.27 ±0.17 1.04 ±0.47 TABLE 9 ß±tß 19 logô) ±6log(F) 0 -15.16 ±0.04 -14.76 ±0.06 -15.13 ±0.07 -14.66 ±0.28 -15.33 ±0.06 -15.07 ±0.09 -14.64 ±0.05 -14.77 ±0.15 -14.37 ±0.09 -14.18 ±0.11 -14.70 ±0.11 -14.99 ±0.06 -15.08 ±0.07 -14.98 ±0.13 -14.98 ±0.09 -14.88 ±0.06 -14.84 ±0.07 -15.83 ±0.10 -15.85 ±0.22 -14.59 ±0.07 -15.23 ±0.28 -15.37 ±0.18 -14.79 ±0.05 -15.16 ±0.06 -14.87 ±0.12 -15.22 ±0.36 -15.12 ±0.13 -14.66 ±0.06 -13.54 ±0.11 -14.95 ±0.11 -14.49 ±0.20 -14.18 ±0.23 -15.00 ±0.11 -14.38 ±0.35 -14.41 ±0.29 -14.00 ±0.33 -14.12 ±0.30 -15.46 ±0.26 -15.04 ±0.21 -14.64 ±0.10 -14.70 ±0.11 -15.06 ±0.13 -15.13 ±0.19 -13.94 ±0.06 -15.06 ±0.20 -14.52 ±0.05 -14.15 ±0.23 -14.88 ±0.36 -13.81 ±0.24 -13.74 ±0.12 -15.41 ±0.32 -14.70 ±0.10 -14.71 ±0.30 -15.81 ±0.28 -13.30 ±0.09 -14.05 ±0.06 -14.85 ±0.12 -14.91 ±0.10 -14.71 ±0.08 -14.10 ±0.10 -14.89 ±0.08 -14.70 ±0.10 -14.33 ±0.08 -15.16 ±0.11 1993ApJS ... 86 ....5K medium andforsometypes of stars. Mg nA2800,whicharestrong featuresbothfortheinterstellar provided bytheabsorptions of SirvA1400,CA1550,and to Simandadditionalunidentified ionsasdiscussedbelow (e.g., Hecketal.1984).Even moreconfusingexamplesare also characteristicofO-typestellarspectra,wheretheyare due by theISMgas,wheretheyareduetoOi,Sin,andCbut are tion features.Forexample,theabsorptionlineswhichoccur around 1300and1335Áareproducedinmeasurablestrength tinction inthe2200Áabsorptiontrough,deepinterstellar al> tude. SincelowGalacticlatitudealsomeansstrongdust ex- sometimes theyfallatthesamewavelengthasstellarabsorp- depressions inthespectrumofagalaxy. sorption featuresshouldcorrelatewithstrong2200 Á highly ionizedspeciesareapproximatelyindependentof lati- duced predominantlyintheGalacticdisk,whilethose of by ISabsorptionsatleastasstrongthosemeasuredfor3C of theexpectedstrengthlow-ionizationlines,whicharepro- 273 andSN1987A.Acosecantlawprovidesaroughestimate 20 KINNEYETAL.Vol.86 The importanceofknowingthestrengthISfeaturesisthat Therefore, thespectraofmostgalaxiesareprobablyaffected © American Astronomical Society • Provided by theNASA Astrophysics Data System a those galaxieswithbothshort-andlong-wavelengthspectraareincluded. to minimizetheeffectsofreddeningonslopedetermination.Only The ß±ößvaluereportedadjacenttoeachactivityclassisthemedian value fortheclass.TheconversionintoFocvisgivenbya=-2-ß. points whichhaveequalcontributionsfromMilkyWay-typereddening, p Galaxy SEYFERT 2 NGC2903 NGC1097 HOTSPOT NGC7793 NGC7673 BCDG, BCG,HII NGC1068 NGC4321 NGC3351 NGC2997 IC3639 NGC3393 NGC3081 NGC6221 Composite NGC5135 NGC4388 NGC3982 NGC7582 NGC7496 NGC7130 NGC6764 NGC5728 MK477 NGC5643 NGC5506 UGC8850 NGC5256 NGC3758 NGC1672 NGC7590 NGC5674 8 Thefullequationislog=ßA±f.Slopesarebasedon3flux 0 TABLE 9—Continued -0.32 ±0.11 -0.45 ±0.12 -1.67 ±0.18 -1.75 ±0.10 -0.93 ±0.22 -1.09 ±0.30 -0.64 ±0.39 -0.42 ±0.14 -0.76 ±0.47 -0.97 ±0.56 -0.71 ±0.34 -0.16 ±0.28 -1.34 ±0.17 -0.52 ±0.48 -1.64 ±0.28 -0.12 ±0.50 -1.18 ±0.28 -0.87 ±0.10 -0.78 ±0.34 -0.51 ±0.53 -0.69 ±0.49 -0.36 ±0.83 -0.55 ±0.35 -0.76 ±0.44 -1.55 ±0.58 -0.24 ±0.11 0.04 ±0.13 0.13 ±0.14 0.21 ±0.28 0.61 ±0.49 0.28 ±0.38 ß±6ß based onlow-dispersionIUE data(seealsoWalbom,Nichols- the worksbyPanek&Savage (1976),basedonOAO2data, were sufficient,contributesignificantlytotheIUEflux. We Bohlin, &Panek1985forhigh-dispersion IUEdata).The and Nussbaumeretal.(1982) andHecketal.(1984),both are fistedinTable5,whichhas beencompiledonthebasisof shall concentrateonmassivehotstarsforthepresent. phases ofstellarevolutionthatpassthroughtheOstarregion of theH-Rdiagramandthatcould,providedluminosity no effectonitscontinuumslope,andthereareshort-lived discussed furtherbelow,theevolutionarystateofahotstar has and Astarsbecomeprogressivelyflatter(seeFigs.45). As slopes areessentiallythesameforallOandW-Rtypes(ß ~ increase inFtowardshorterwavelengths.Inpractice,their WN andWC)arecharacterizedbyhightemperatures(T> -2.5 ),whilethespectralenergydistributions(SEDs)oflater B 10,000 K),resultingincontinuousfluxdistributionswhich x cS The maindiscretespectralfeaturesseeninearly-typestars Early-type starswithspectraltypesB,O,andW-R(both \og(F) ±6log(F 0 -13.72 ±0.09 -15.26 ±0.13 -14.98 ±0.16 -15.00 ±0.28 -14.00 ±0.08 -13.60 ±0.10 -14.06 ±0.09 -15.08 ±0.08 -15.43 ±0.41 -14.14 ±0.21 -15.08 ±0.12 -15.06 ±0.22 -15.02 ±0.35 -13.52 ±0.11 -14.10 ±0.20 -15.13 ±0.32 -15.51 ±0.21 -14.66 ±0.37 -15.85 ±0.42 -15.24 ±0.20 -14.58 ±0.08 -14.72 ±0.24 -15.05 ±0.39 -14.98 ±0.35 -14.80 ±0.26 -14.25 ±0.36 -14.14 ±0.28 -13.73 ±0.08 -14.94 ±0.25 4.1.2. Early-TypeStars 1993ApJS ... 86 ....5K stellar evolution,suchaspost-asymptoticgiantbranch rable tothatofthestellarfeatures,e.g.,finesoccurringaround occur atthesamewavelengthandwithastrengththatiscompa- stellar fines.Thereareinstancesinwhichtheinterstellarfines atlas, someofthestellarfeaturesmaybeconfusedwithinter- dispersion foreachclassshownabove therespectivehistogram.Blueslopes plays astrongPCygniprofileinthecaseofsupergiants. absorption, withtheexceptionofSirvdoublet,whichdis- ionization thanthoseofO-typestars.Thefinesaregenerallyin plotted accordingtotheiractivity class,withthemedianvalueand Cygni profile,whichismoreprominentforsupergiantsbe- teristic emissionofHenXI640doesconstituteauniqueflag giants havesimilarlystronglines.Ontheotherhand,charac- are ontheleft;redslopes right. cause oftheirhighratemassloss. These lineseithermaybeinabsorptionordisplayaP for thepresenceofW-Rstars. substantial populationofW-RstarsbecauseO-typesuper- the varioustypesfromeachother: of astrongPCygnilineCrvisnotclearevidencefor Cygni profileorappearessentiallyinemission.Thedetection of highlyionizedionswhicheitherdisplaya“classical”P tral types,therearesomecharacteristicsthatclearlydistinguish several angstromseach. respective blueabsorptionsandredemissionsmayamountto lent widthisaroundzero,whiletheequivalentwidthsoftheir stars arepresent.InthecaseofPCygnilines,totalequiva- easily detectableinthespectrumofagalaxy,ifmanyearly-type 1300 and1335Á,SiivX1400,CrvX1550. equivalent widthsoftheseUnesmaybe10Äormore,whichis -0.82 +/-0.89 -1.25 +/-0.45-1.750.63-0.760.47 No. 1,1993 ß As mentionedabove,thereexistseveralOstarphasesof In low-dispersionspectrasuchastheonescontainedinthis 2. O-typestellarspectracontainlinesofhighlyionizedions. 3. B-typestellarspectraarecharacterizedbyfinesoflower Although anumberoflinesarecommontothevariousspec- Fig. 6.—Histogramsofspectralindex ß,whereFocX.Galaxiesare 1. Wolf-RayetspectraarecharacterizedbyprominentUnes x -8 02 I ]..LIJJ.L1 normal nuc BdD-i-Bd+HII $y2 © American Astronomical Society • Provided by theNASA Astrophysics Data System 0.06 +/-0.93 -2 02 Liner UV SPECTRAOFSTAR-FORMINGGALAXIES -0.24 +/-0.83 norm+Lin -2 02 Ü both theMilkyWaydereddeningcurveandLMCcurve. tude (NGC1569),togetherwitharedstarburst7552)and blue Note thattheGalacticlatitudeofNGC 7552is-65?2. The dereddeningresultsinarelativelysmoothslopeforthecaseofNGC starburst (NGC4214).NGC1569and7552aredereddenedusing 1569, whiledereddeningcausesabroademissionfeatureinNGC7552. Fig. 7.—SpectralenergydistributionsofagalaxyatlowGalacticlati- 15.0 15.1515.3 Log (y) 21 1993ApJS ... 86 ....5K o elli etal.(1990)havedeveloped sophisticatedspectralsynthe- ground-state doublettransition andisthestrongestforF8-G1 mid-A stars,reachingthemaximum strengthforK0-K3.Fan- stars. Theresonancetransition MgiX2852startstoappearin predominantly fromG5-K5 stars. MgnX2800comesfroma ably wide(—60ÁinstarsofspectraltypeK).FeiX3000arises Fe iX3000originatesfromaquartetoflinesandcanberemark- maximum valuefordwarfsandgiantsofspectraltypeF9-G2. et al.1987).TheblendsofFenX2400andX2600reach a their equivalentwidth(EW)islargerthanexpectedforIS ab- ous, sinceboththestarsandISMcontributetoline. been compiledonthebasisofstudybyFanellietal.(1987, sorption (seeTable4).Otherwise,theidentificationisambigu- XX1855, 1863increasesinstrengthfromB2tomid-A(Fanelli absorption-Une equivalentwidthisthemaximum.Thelist has tra obtainedwithIUEandthepresentgalaxysample,since trend willcomphcatethecomparisonbetweenstellarspec- are listedinTable6,alongwiththespectraltypewhere stellar templatesarepredominantlysolarmetallicity. believed tobeameasureofthemetallicitysystem.This those ofopticalabsorptionfeaturessuchasMg,whichare cluded thatthestrengthsofUnesinUVincreasedwith residual (afterremovalofhotterstars)spectra.Theycon- studied thestrengthsofabsorptionUnesinresulting from theirIUEspectraofearly-type(EandSO)galaxies al. (1988)attemptedtoremovethesignaturesofhotterstars strongest linestendtobeatthelongerwavelengths.Bursteinet which appearexclusivelyinabsorption,withtheUnesofFe and Mgbeingparticularlystrong.Inlaterspectraltypesthe continuum emissionlongwardof2600Á(Wuetal.1991). but thecontributionatX<2000Ábecomesnegligibleforstars 1990 ).Thehuescanbeidentifiedashavingstellaroriginwhen of typelaterthanF3.StarsspectralGcontributeonly practically flat{FocX)atwavelengthslongerthan1600Á, length IUEcamera.ThecontinuumemissionofAOstarsis inates theUVemissionofnormalgalaxiesinlong-wave- 2 Greggio &Renzini(1990)foracomprehensivediscussionof al. withthisinterpretationoftheshortestIUEflux.Seealso which isinthepresentsample,wasalsoanalyzedbyBursteinet the bulgesofspiralgalaxies.Ithasbeenreportedthatam- greater thansolarmetallicity),characteristicsbelievedtode- toward shorterwavelengthsjustasdomassiveOstars.Ithas x hot phasesofstellarevolution. rising branchflux(Bursteinetal.1988).ThebulgeofM31, plitude oftheshort-wavelength“risingbranch”inIUE been shown(Barbaro&Olivi1989)thatthisphaseofstellar dwarfs. ThesestarswillhaveaUVcontinuumwhichincreases a wayastosuggestthatPAGBstarsmaybethesourceof spectra ofellipticalgalaxiescorrelateswithmetallicity,insuch scribe thedominantstellarpopulationinellipticalgalaxiesand are bothold(agegreaterthan~10Gyr)andmetal-rich(of evolution couldbeveryimportantinstellarpopulationswhich (PAGB) starswhichareontheirwaytobecomingwhite 22 Lines ofAlnX1671appearinstarslaterthanB8,whileA1 m The mostfrequentlyobservedcoolstarfeaturesinouratlas Lines fromA-Kstarsarecharacterizedbylowionization, Thermal emissionfromstarsinthespectralrangeA-Kdom- © American Astronomical Society • Provided by theNASA Astrophysics Data System 4.1.3. Mid-toLate-TypeStars KINNEY ETAL. 46-1 their low-ionizationemissionfines,theLINERspectra are axy, withlittleevidenceofactivity. JustasHeckman(1980) dominated intheUVby spectrumoftheunderlyinggal- entiate themselvesfromnormalspiralgalaxiesintheoptical by duces ahigh-excitationfinespectrum(Kinneyetal.1991b). which ismademostlyofswept-upmaterial.Thedetailedinfor- LINERs hadbeenclassified based ontheUVspectra,most uum, wefindnoevidencefor itintheUV.Indeed,if and LINERsareshowninFigure1.Althoughdiffer- an “activenuclearregion,”inwhichapowerfulnonthermal Crab Nebula,fromBlairetal.(1984b)forO-richSNRs, ring toyoungremnantsinwhichtheemittinggasismainly For SNRswepresentfourdifferentcases,thefirstthreerefer- the mostprominentPNfinesisfromFeibelmanetal.(1988). by Dufour(1987)forHnregions,Koeppen&Aller found noevidenceintheoptical forafeaturelessbluecontin- source (upto10ergss)ionizeshigh-densitygasand pro- mation onSNRspectraisfromDavidsonetal.(1982)forthe one correspondstotheCygnusLoop,whichisanoldSNRand constituted bymaterialejectedintheSNexplosion.Thelast PNs, andBlair&Panagia(1987)forSNRs.Theactualfistof Raymond etal.(1980)fortheCygnusLoop. R. A.Fesen(privatecommunicationcitedinBlair&Panagia tions theircontributiontotheintegratedspectrummaybe nebular objects.ItisbasedmostlyonthereviewsofIUEdata orders ofmagnitudelowerthanthatHnregions. far belowthatofHnregions,sounder“normal”condi- hand, theirindividualluminosityandnumberdensityare type, massivestars),planetarynebulae(PNs)(regionsmade ized species,suchasNv,Crv,Hen,andNerv.Ontheother than twiceionized,andHeisnevermoreonceionized. region gasisonlymoderatelyionized;C,N,andOarenomore tures definitelylowerthan50,000Kand,therefore,theHn dwarf, arebrightandhot),supernovaremnants(both Planetary nebulaeandSNRsmaydisplayfinesofhighlyion- clouds, mostoftheirionizingradiationgoesintothe about 1%oftheentireGalacticluminosityisproducedbyO- heated andionized). ejecta andinterstellargassweptbytheejecta,whichareshock- end oftheirevolution,inthetransitionfromredgianttowhite of gasejectedandionizedbymoderate-massstars,whichatthe H nregions(heredefinedastheionizedaroundearly- axy spectrum. surrounding gas.O-andB-typestarshaveeffectivetempera- and B-typestars,and,sincetheyareassociatedwithmassive regions accountformostofthenebularfineemission.Infact, 1987) forPupAasaprototypeofN-richSNRs,andfrom sis techniqueswhichcandeterminethestellarmixfromagal- The spectralenergydistributions(SEDs)ofnormalgalaxies In addition,onemayexpectemissionfinesoriginatingfrom Table 7fiststhemostprominentfinesthatareobservedin Emission finesfrom“ordinary”ionizedgasmayarise In atypicallate-typegalaxysuchasourownGalaxy,Hn 4.2. CharacteristicsofUVSpectraGalaxies 4.2.1. NormalSpiralGalaxiesandLINERs 4.1.4. NebularEmissionLines Vol. 86 1993ApJS ... 86 ....5K lent widths,anddifferentfines presentinthespectrum.Of course, oneimportantfactor is thatthestarburstshavealarge individual hotstarshavevery differentabsorptionfeatures galaxies asawayofperformingcrudespectralsynthesis. from thestarbursts,withdifferent lineratios,differentequiva- a naturalexplanationforthe largerangeinUVslopes,the rable totherangeinslopesofstarburstsandwouldserve as tion features.Withinthestarburstgalaxies,slopesrange While theOandBstarshavearangeinslopesroughlycompa- ß =-1.85±0.06).Thespectralenergydistributions(SEDs) from red(NGC7552,ß=0.26±0.14)toblue4214, denced bytheirbluespectraandstrong,hotstarabsorp- of OandBstarswitharangeinluminosityclass(Fanelliet al. galaxies toberedderthantheScandSdgalaxies.Forexample, the coolstarspectrum,whichdominatesfluxatlongwave- the galaxiesshowanexcessinshort-wavelengthfluxrelativeto galaxies showatrendforearlyHubbleclassestohavelessflux when orderedbyslope,thereisatendencyfortheSaandSb bottom. TheSEDsarenotcorrectedforinterstellarreddening. by slope,withthebluestontopandreddest with differentlevelsofactivity. taining opticalspectratoclarifytherelationbetweengalaxies IUE spectraoftheLINERNGC3998).Wearecurrentlyob- would havebeenclassifiedasnormalspiralgalaxies,sinceonly hot stars,asexpectedforgalaxieswithmoreactivestarforma- length. Meanwhile,thelaterspiralgalaxies(forexample,NGC pared withtheAandFstarsinFigure5.Incaseswherecool era. Forexample,theSAabgalaxyNGC4736canbecom- while thebluestgalaxyisScNGC3994.Thenormalspiral among theLINERs,reddestgalaxyisSaNGC2681, Although thegalaxiesdonotstrictlyseparatebyHubbleclass a few(e.g.,NGC4579)showevidenceofemissionlines(see the distributionofHubbletypesinIUEarchivesand,there- star featurescanbeclearlyseeninthelong-wavelengthcamera, features oflateAorearlyFstarsinthelong-wavelengthcam- at shortwavelengththanlaterHubbletypes(cf.Colemanetal. Reichert etal.1992foradetailedtwo-dimensionalanalysisof fore, ouratlas. der slopes.Infact,themedianvalueofHubbletypes ble type(Heckman1980),LINERsareexpectedtohavered- tion. Themassivehotstarspectrum,whichcanbeseenatthe of asignificantdifferenceinslopesbetweenthetwoisdueto value ofHubbletypethenormalspiralgalaxies,solack LINER galaxiespresentintheatlasissameasmedian known toresidepreferentiallyinspiralgalaxiesofearlyHub- the normalgalaxies(seeFig.6andTable9).SinceLINERsare 598, Scd)showshort-wavelengthfeatureswhichcomefrom 1992, Fig.5)canbecomparedwiththeSEDsofstarburst axies. star signaturesseenatlongerwavelengthsintheearly-typegal- shortest wavelengthsforthelate-typespirals,dilutescool 1980). No. 1,1993 The activestarformationofstarburstinggalaxiesisevi- The earlierspiralgalaxiesshowtheSEDsandspectral In Figure1thenormalgalaxiesandLINERsareordered The LINERsdonothavesignificantlydifferentslopesfrom 4.2.2. Starburst,BlueCompact,andCompact © American Astronomical Society • Provided by theNASA Astrophysics Data System Dwarf Galaxies UV SPECTRAOFSTAR-FORMINGGALAXIES ultraviolet. (Notethatthisbehavior contrastswiththatofqui- forming galaxiesthatareoptically bluearealsointhe between UVslopeandmetalficity. on averagethantheslopeof the starburstgalaxies.Thus,star- starburst galaxies.Indeed,they haveUVslopesthatarebluer dwarf galaxiesareknownto have lowermetalficitiesthanthe sure metalficitysoastodeterminethenatureofrelation spectra inan/UE-sizedaperturewhichwillenableustomea- known (seealso§4.1).Wearecurrentlycollectingoptical metalficity ([O/H]=0.02[O/H])bluecompactgalaxies of youngmassivestars:infact,IZw18isonethelowest in itsUVspectrum,althoughthisgalaxyhasalargepopulation I Zw18showsveryweakabsorptionfinesfromearly-typestars ficity contentwillcorrespondtolowerequivalentwidths.Thus ity ofthegalaxy.Indeed,someopticalfeatures,lesssensitiveto tion finesinthespectrumofagalaxyisaffectedbymetalfic- the dispersioninslopes:redstarburstgalaxies(cf.NGC “metalficity indicators”—forexample,Mg(MgH+ 6, other parameterssuchastemperatureorgravity,areused (cf. NGC4214and5253).Thestrengthoftheabsorp- equivalent widthsatshortwavelengthsthanthebluegalaxies tion, theremaybeasubstantiveunderlyingpopulationofcool E(B-V) valuefromBurstein&Heiles(1982),usingboththe with b=11?2,is(Æ-F)=0.51mag,andstrongabsorptionat the typeofextinctionseeninourGalaxy.Asanexample, dust extinction.However,thegalaxiesshowlittleevidenceof large, oldspiralundergoingjustanotherburstofstarforma- the redstarburstwithanyknownreddeninglawbecauseof the GalaxycurveandLMCcurve,untilithasapproxi- to dereddenNGC7552,averyredstarburstgalaxy,withboth NGC 1672),shownoabsorptionfeatureat2200A.Ifdustis have thestrongestextinction(forexample,NGC7552and extinction oftheMilkyWayisseeninFigure2forNGC1569, restricted tolocalstars. stars withmetalficitiestypicalofthesolarneighborhood,being range inmetalficity,whiletheatlasofFanellietal.contains 5156-5197 Â;Bursteinetal.1984).Generally,alowermetal- stars toreddenthespectrum. is dominatedbyarecentburstofstarformationafterperiod laws. Thisdemonstratesthattheslopedifferenceisdifficultto slope ofthebluestarburstcannotbeproducedbydereddening reasonable SED,althoughthereissomedeviationfromthe ing curveofFitzpatrick(1986).Bothdereddeningsproducea average GalacticcurveofSeaton(1979)andtheLMCredden- as demonstratedinFigure7.NGC1569isdereddenedwiththe ferent wavelengthdependencethànthedustinMilkyWay, causing thedispersioninUVslope,thatdustmusthaveadif- of quiescence,theslopemaybeveryblue.Butifgalaxyisa versus coolstarpopulationspresentinthegalaxy.Ifgalaxy completely differentfromanymeasuredtodate. explain withsimpledereddeningunlesstheextinctionlawis mate slopeofNGC4214,averybluestarburst.Infact,the standard dereddening.Forcomparison,anattemptwasmade 2200 Á.Thereddeststarbursts,whichmightbeexpectedto excess of2200Áemissionproducedbythesetwodereddening o 1672 andNGC7552)tendtohavelargerabsorption-fine 2 As agroup,thebluecompactgalaxiesand One additionaltraitcomplicatesanysimpleexplanationof The rangeinslopesofthestarburstsmaybeduetointernal The rangeinslopesmayalsobeduetothehotstar 23 1993ApJS ... 86 ....5K understand thedustinthese galaxies. that thespectralsignatureofdustisveryrarelyseeningalaxies, gion toapowerlaw. follow-up workwealsoplan to lookatIRASfluxesbetter an aperturematchedtothesize oftheapertureIUE,andin galaxies actuallycontainnodust,themostlikelyexplanation expected becauseofitsGalacticlatitudeè=11°andcorre- starburst galaxies.Theonlyunambiguous2200Âdustfeature even whentheirspectraareintrinsicallyred,aswiththe red known emissionlinesandfittedtheremainingcontinuumre- Thus, theslopeshereareingoodagreementwiththoseofKin- raised slightly,butthevalueforßwillnotbegreatlyaffected. the FqvalueinTable9(wherelogT=ßA+F)willbe flux. Wearecurrentlyobserving thegalaxiesininfrared is notseenintheUVspectraexcepttolowerdetected UV parent oropaque(Heisler&Ostriker1988).Theeffectof dust around unity.Thusdustislikea“picketfence,”eithertrans- dust isinclumps,sothatrarelyhasanopticaldepth of for thisapparentlackofdustintrinsictothegalaxiesisthat the sponding E{B-V)of0.51.Althoughitispossiblethat the seen inFigures1,2,and3isthatNGC1569,which is ney etal.(1991a),whoexcludedallspectralregionswith in the2323-2423Aregion.Oftheseemissionlines,onlyCm] gion, Cm]A1909inthe1863-1963Âregion,andn]A2326 cludes anemissionline:Niv]A1485inthe1432-1532Àre- three 100Awavebandsusedinthederivationofslopein- A1909 hasappreciableflux,andsinceCm]isinthecenterbin, here issomewhataflectedbythistrend,becauseeachofthe lines arenotresolved.Themethodusedtodetermineslope to havebluercontinuathantheyactuallyiftheiremission galaxies wouldlooklikewithhighersignal-to-noiseratio.A wavelengths isfromtheemissionlines.Therefore,UVspectra than 2magbrightertheothers.ThemanyemissionUnes of Seyfert2galaxieswithlowersignal-to-noiseratiowillappear significant percentageoftheNGC1068fluxatshortestUV of NGC1068presumablyshowwhatthespectraother wavelengths. Theimplicationisthattheremaybeasequence begin tobedominatedbythehostgalaxyatlongestUV the featurelessbluecontinuumplusemissionUnes(Kinneyet featureless bluecontinuumandthegalaxycontinuum. ratios, showninFigure3,bothNGC3982and3081 al. 1991a).OftheSeyfert2galaxieswithhighersignal-to-noise galaxy continuumplusemissionlinesspanningabroadrange of activegalacticnucleiorderedbytherelativestrengths of ionization,whileintheUVcontinuumisdominatedby In theoptical,aSeyfert2spectrumismadeupofanunderlying compact galaxies,andbluerthannormalspiralsLINERs. spiral galaxies,areredderintheUVthanstarburstorblue discussed byBursteinetal.1988.) escent ellipticalgalaxies,wherethegalaxieswhichareredder optically tendtohavebluershort-wavelengthUVcolors,as x0 24 One surprisingresultofthiscompilationgalaxyspectrais Among theSeyfert2galaxiesinFigure3,NGC1068ismore Seyfert 2nuclei,whichresidepreferentiallyinearly-type 4.2.4. TheRoleofDustintheUVSpectraGalaxies © American Astronomical Society • Provided by theNASA Astrophysics Data System 4.2.3. Seyfert2Galaxies KINNEY ETAL. -1 1 _1 5 0 1A±5 blocked fromourlineofsight. photoionizing continuumisobscured.Thus,Mrk348displays the numberofrecombinationphotonsislargerthanpredicted although Lyaisconsidered an actualfeaturebyHartmann, is someuncertaintyinthestrength oftheLyaemissionfine, taminated byanartifactonthe IUEcamera(1280Á),sothere C rvabsorptionfeature.TheregionaroundLyaisoftencon- they estimatethat3A/©yrofgasisbeingconverted into sion linesandwithsomeoftheultravioletcontinuumflux evidence ofharboringaSeyfert1galaxywithbroadHaemis- within theerrorsofKinneyetal.(1991a)valuea= were firstreportedbyFerland&Osterbrock(1986),who with aFWHMforHaof-7400kms“./UEdataonMrk348 to havebroadSeyfert1typeemissionlinesinpolarizedflux, Huchra, &Geller(1984).This comparativelydistant(z= starburst galaxy,andindeedthespectrumshowsaverystrong massive {M>10M©)stars. formation. FromtheirspectralsynthesisoftheIUEspectrum compact dwarfgalaxy(BCDG)tobeundergoingintense star ([O/H] ^0.3[O/H]^;Hunter&Gallagher1986)brightblue Fanelli, O’Connell,&Thuan(1988)foundthismetal-poor §4.1, andamoderate-strengthintrinsicLyaemissionline. features indicatingthepresenceofhotstarsasdiscussed in from thenumberofionizingphotons,implyingthat found avalueof=-0.9fortheUVspectralindex,whichis tions ofthesteadystateUVfluxLequeuxetal.(1981).The M© yr,bycomparingthefar-UVluminositywithpredic- spiral, whichhasacompanion,NGC266(Garcia-Vargasetal. lines. ThisSeyfert2nucleusresidesinaface-onearly-type(Sa) quence turnoffandisdominatedbylateFstars(seethestellar longer wavelengthfluxispresumablyduetothemain-se- derived anupperlimitforthestarformationrateof7.4X10“ spectrum ofMrk348isflat(FocA)withstrongemission spectra inFig.5forcomparison). Galactic andfromM31)MgiA2850. -1.4 ±0.5(Focv~‘).Kinneyetal.(1991a)foundthat file intheUVwiththatoptical.Deharvengetal.(1982) red giants,basedonacomparisonofthecross-dispersionpro- cause oftheweakabsorptionfeaturesSirvandCnear but withalessprominentrisingbranch.Welsh(1982)ob- present between1200and1350Â,aswellasMgnA2800(both wavelengths. AbsorptionfeaturesofSin,Oi,m,andCnare stars aremorecentrallyconcentratedthanthemetal-rich rising branchdidnotcomefromyoung,metal-richstarsbe- served thecenterofM31withIUEandconcludedthat with thecenterdominatedbybulgepopulation(Burstein et al.1988);thespectrumresemblesthatofanellipticalgalaxy, 2000 Âandanincreaseinfluxtobothlongershorter M31 isbasicallyconcave,withaminimuminfluxataround 15 isslowlyrisingfrom2000to1200Á,withstrongabsorption 1989 ).Mrk348hasbeenshownbyMiller&Goodrich(1990) x v 1300 Á.Inthecentralregion,Welshalsofoundthatblue Mrk 357;starburst.—Balzano(1983)classifies357as a Haro 15(Mrk960);I,BCDG.—TheUVspectrumof M31 isthebestexampleinatlasofaspiral(Sb)galaxy NGC 262(Mrk348);SO,Seyfert2.—Theshort-wavelength NGC 224(MSI,Andromeda);Sb.—TheUVspectrumof 4.3. IndividualObjects Vol. 86 1993ApJS ... 86 ....5K 4 7 10 o ing thenucleus(a“hotspot” galaxy)ataradiusof~10",or which placesthenucleusofNGC1097inlowactivity would bepredictedbasedonthenumberofphotonsavailable more activeLINERssuchas NGC 3031or4579). range amongtheclassofLINERs (cf.theemissionfinesof fines. TheUVspectrumisflatwithstrongabsorptionfeatures, called aLINERbyKeel(1983b)basedonopticalemission NGC 1068appearstobeobscuredfromdirectview. to ionizethegas.ThussourceofUVcontinuum of number ofrecombinationphotonsmeasuredwaslargerthan Osterbrock (1986)andKinneyetal.1991a)foundthat the emission finesandbroadfeaturesofFen.Ferland & Boksenberg (1986),whofoundbroadwingsonthepermitted a review). ple ofaSeyfert2galaxy.ThishighlystudiedSbgalaxywas found toharboraSeyfert1nucleus(seeKinneyetal.1991for observed byAntonucci&Miller(1985)inpolarizedfightand is anintrinsicMgicomponent. likely tobefromjusttheMilkyWayISM,implyingthatthere high ionization.NGC1068isthenearestandbrightestexam- (i\ xX°)continuumwithemissionfinesofbothlowand the IUEarchives. were studiedbyBlair,Kirshner,&Raymond(1984a);andthe tral regions.TheOBstarsofM33werestudiedbyMassey, galaxy, asopposedtothegeneralstellarpopulationofcen- from ourGalaxy.Incontrast,Mgiissostrongthatitun- b =19°,thestrongabsorptionfineofMgnisverylikelytobe axies (Tully1980).SinceNGC1023liesatGalacticlatitude normal SBOgalaxyinagroupof13gravitationallyboundgal- and onelong-wavelengthspectrumofthecenterM33arein al. (1984).Surprisingly,onlythreeshort-wavelengthspectra work concernsthepropertiesofindividualconstituents tional model,withayoungcomponentofage~10yrandan luminosity activenucleushasbeensuggestedbyTrinchieri, IUE waveband.Atshorterwavelengthsthecontinuumisrich to detectmanyofthecomplexabsorptionfeaturescommon 0.053) galaxyisobservedwithtoopoorasignal-to-noiseratio M3 3Hubble-SandagevariableswerestudiedbyHumphreyset Hutchings, &Bianchi(1985);theM33supernovaremnants (1984) comparedstellarsynthesismodelsagainsttheIUE Fabbiano, &Peres(1988).Ciani,D’Odorico,Benvenuti kert &Raflis1983).Aninterpretationofthenucleusasalow- a QSO. starburst galaxies.Mrk357appearsstellaronthePalomarSky old componentwithage~10yrsuperposed. spectrum ofthecenterandfoundabestfitwithmultigenera- nucleus isthebrightestX-raysourceinLocalGroup(Mar- in absorptionfeaturesfrommassivehotstars. nearby Scdgalaxyisbasicallyflat{FocX)acrosstheentire Survey plates,sothatitissometimesincorrectlyreferredtoas 1097 isabarredspiralwith ring ofstarformationsurround- 1023 isapparentlydominatedbyFandGstars.NGCa No. 1,1993 x Multiple IUEspectrawerecombinedbySnijders,Netzer, & M3 3hasbeenverythoroughlystudiedintheUV;butmost M3 3isabrightgalaxyintheX-rayband,andindeedits NGC 1097;SBbc,hotspot+LINER.—Thisgalaxyhasbeen NGC 1068(M77);Sb,Seyfert2.—Thisspectrumhasaflat NGC 1023;SBO.—Thelong-wavelengthspectrumof NGC 598(M33);Scd.—Thespectrumofthecenterthis © American Astronomical Society • Provided by theNASA Astrophysics Data System UV SPECTRAOFSTAR-FORMINGGALAXIES 12 6 the companiongalaxyNGC1097A. /¿m, andinHa(Phillipsetal.1984;Hummel,vanderHulst,& center (Wolstencroft,Tully,&Perley1984)andhastwopairs contains aweak,compact,flat-spectrumradiosourceatthe Keel 1987a;Gerin,Nakai,&Combes1988).NGC1097also emits inradiowavelengths,theCO(J=1-0)fine,at10 irregular galaxycontainingalargeblobofionizedgasinits suggests dynamicaldisturbance,perhapsbyinteractionwith Lorre 1978forspectacularimages).Itslarge-scalemorphology of opticaljetsextendingfromthenucleusoutto90kpc(see that thegalaxyhasexperiencedasingleburstofstarformation this galaxy,whichhasacontinuumslowlyrisingtoward center, wheretheIUEaperturehasbeenplaced.Lamb, the main-sequenceturnoffat ~2400Â,whichistypicalofan wavelengths anddoeshaveabsorptionfeaturesbetween1850 between theshort-andlong-wavelengthspectracouldbe above authorshavealsosynthesizedthespectrum,concluding tensity nonthermalemissionwithapeakcoincident the blue, narrowoneduetoyoungassociationsandHnregions, by Véron-Cetty&Véron(1986)becauseofthepresence a contributionfromsupergiantsand,possibly,Wolf-Rayet constituted ofmain-sequencestarswithmasses^50Af©, starting about3X10yragoandthatitspopulationismainly shorter wavelengthsthatisrichinabsorptionfeatures.The Hunter, &Gallagher(1986)havestudiedtheIUEspectrumof older intermediatepopulation presentinquiescentSOgalaxies spectra). and 2000ÁwhicharetypicalofAstars(seeFig.5for star component. TheUVspectrumrisesslowlytowardshorter Nieto (1984)callmetal-poorHnregionswithastrongA star complex centralstructuresofsize~10",whichEichendorf & companion galaxytothelargebarredspiralNGC1512and has types. NGC1433isanearlyface-on,barredspiralgalaxy,in- Gondoin (1983)mapsomeofthemanyHnregionsNGC due totypicalpointingerrorsofl"-2",orthedifficulty stars. optical nucleus. and abroad,redcomponent,composedofoldstars(Buta The nuclearandtheinnerringsconsistoftwocomponents:a cluding threeringsofenhancedbluecolorandactivestarfor- complex contributionfromapopulationwithrangeofstellar axy. AbsorptionfinesofCrv,Alm,Fei,n,Mgnreveala faint emissionfinesatopticalwavelengths,with[Nn]X6583 cluded intheRosa,Joubert,&Benvenuti(1984)catalogof range oftheIUEaperture.Althoughthisobjecthasbeenin- extracting fluxwithhighbackground(seeFig.17).Marcelin& mation (Buta1983)whichallfieoutsidetheIUEaperture. ous fromtheUVspectrum,whichisthatofanormalSbgal- stronger thanHa.Thesameclassificationdoesnotappearobvi- of Hnregions. H nregions,thespectrumdoesnothaveblueslopetypical ~ 1.5kpc,whichisbarelyoutsidetheIUEaperture.Thering 1986). Observationsintheradio(Harnett1987)showlow-in- 1313 intheopticalandshowthattheyextendwelloutside NGC 1140(Mrk1063);IrrAm,BCG.—NGCisablue NGC 1553;SOpec.—TheUV spectrumhasweakfluxbelow NGC 1313;SBdm,Hn.—Thesmallapparentdiscontinuity NGC 1510;Ampec,BCDG.—NGC1510isalow-mass NGC 1433;SBab.—ThisgalaxyisclassifiedasSeyfert-fike 25 1993ApJS ... 86 ....5K 7 A/o, althoughthisresultdoesnotexcludeacontributionfrom bles thatofitsneighbor,theLMC(Meureretal.1992). The that thisbluecompactdwarfgalaxyiseitherinamildstarburst radial gradientinsurfacebrightness.Itslowmetallicityresem- phase orinapostburstphase.Thisirregulargalaxyhassteep emission isduemainlytomassivebinaries.Inaddition, its gated andamorphousstructurecenteredonitsnucleus(Sersic the presenceoftwostellarpopulations coexistinginthegalaxy: are wellaccountedforbyB0andB1starsofapproximately 20 strong absorptionfeaturesintheUVspectrumofthisgalaxy X-ray emissionappearsextended(Fabbiano1989). mal spirals,NGC1672probablyhostsanX-raypointfike ray luminosityiscomparableinintensitytothatofmostnor- be undergoingactivestarformationandbyIsrael(1988) lanic irregulargalaxy,whichissaidbyHunteretal.(1989b)to though thespectrumisnoisyandotherabsorptionfeatures an innerhighsurfacebrightness component,extendingupto stars ofhighermassassuminganormalIMF(Lambet al. strong emissionfinesobservedintheopticalspectrumand the source initsnucleus,unlikemostnormalspiralswhoseX-ray X-ray source(Fabbiano&Trinchieri1987).AlthoughitsX- & Pastoriza1965).NGC1672isbotharadiosourceandan its stellarpopulation.Thislate-typebarredspiralhasanelon- with arichcollectionofbroadabsorptionfines,NGC1672is cannot beunambiguouslyexcluded.NGC1569isaMagel- plane oftheGalaxy{b=11?2)andshowsverystrongGalactic tic featureby11Â. starburst galaxycontainingawiderangeofagesrepresentedin pernova ratedecreasingintime(Israel&deBruyn1988). seen (CrvXI550,FenXX2585,2600,andMgX2800,al- spectrum, onlyabsorptionfeaturesfromourGalaxycanbe minous, youngstarcluster(Arp&Sandage1985).IntheUV The veryhot,brightnucleusofthisgalaxyresemblesasuperlu- dust extinctionwithadepressionat2200Áandbelow1475Á. intrinsic MgnabsorptionfeatureisseparatedfromtheGalac- gous behavioramongellipticalgalaxies,the“risingbranch”). wavelengths below1400Â(cf.Bursteinetal.1988foranalo- flat withnoindicationofa2200Ádustabsorptionfeature,and et al.1990,respectively).BasedontheUVspectrum,whichis starburst galaxy(Diaz1985,Mourietal.1989,Garcia-Vargas has beenclassifiedvariouslyasaLINER,Seyfert2,or continuum, whosenonthermalpartcanbeexplainedbyasu- deficient inveryearlyOstarsandbasedonanalysisoftheradio by 10yr.Hunteretal.considerNGC1569astarburstonthe This galaxyisatsufficientlyhighredshift(z=0.004)thatthe 500 pcfromthecenter,anda lowsurfacebrightnessone,upto on UVandopticalcolorswhichshowanOBstarpopulation is recoveringfromstarformation(poststarburstgalaxy),based reddening ofthisgalaxy[E(B-V)=0.56±0.10mag;Israel tained fromthestudyofopticalandIRproperties.Largeun- certainties areexpectedinthisanalysisbecauseofthehigh basis ofitspopulationcontent(extremePopulationI),asob- (Gregg 1989).Thereisanincreaseinfluxthespectrumat Israel &vanDriel(1990)tobepastitsburstofstarformation 1985). 1988]. Israeland&vanDrielconcludethatNGC1569 26 In amulti-wave-bandstudy, Meureretal.(1992)observe NGC 1705;IrrAm,BCDG.—Lambetal.(1985)suggest NGC 1569;Im,starburst.—NGC1569liesclosetothe NGC 1672;SAB(s)be,starburst+Seyfert.—Thisgalaxy © American Astronomical Society • Provided by theNASA Astrophysics Data System KINNEY ETAL. green 1981),basedonthedisjointnatureofitsindividual those inM33andtheLMC(Hodge1985).Themoreactive galaxies despitetheexceptionallyhighluminosityof blue magnitudeofM=-21.0andaneutralhydrogencontent arms. NGC2403containsalargenumberofHnregionsand constant throughtheultravioletregion.ThisnormalScgalaxy clumps. gest, itiseitherlackinginthe2200AfeatureseenMilky to thepresenceofdust.Ifdustispresentastheseauthors sug- L) ~11.1;Iyengar,Rengarajan,&Verma1985],probably cal disturbance(vanderBurg1985).Thisbluecompactgal- Mpc) north,butthisgalaxyshowsnoevidenceofmorphologi- compact group,withthreecompanionssituatedabout22'(0.5 (Beckman etal.1987),whichappearsquiescent. star formationregionsofNGC2403arenotinthenucleus OB associationsthataresimilarinsizeanddistributionto of theM81groupisprototypicalflocculentspiral(Elme- cal abundancesaretypicalofHnregionsinnormalspiral conditions suchastemperature,electrondensity,andchemi- gaard, Edwards,&Heidmann1982)showthatthephysical from OtoearlyB.Spectroscopicstudiesintheoptical(Boes- such galaxiesisfromasumofstarsranginginspectraltype with acompositepopulation of O,B,andAstars.Thespectral Way reddeningcurves,orelsethedustispossibly very owing tothepresenceofanintenseburststarformation and nebulosity (Gordon&Gottesmann1981).NGC2415has a axy isslightlyellipsoidal,withanirregularcoreand show thattheUVcontinuumemissionfromclumpsof population synthesis.TheUVspectrumisrichinabsorption cussed byFanelfietal.(1988)andanalyzedusingspectral clumped. Theshort-wavelengthIUEspectrumhasbeen dis- of—6% ofthetotalmassgalaxy(Gordon&Gottesmann last episodearisingabout10 Myr ago. features andshowsthepresence ofOBsupergiantstogether crete episodesratherthanin continuousformation,withthe synthesis modelssuggestthat starformationtookplaceindis- gion oftheLWPcamera. due tothehighbackgroundandlowsensitivityofthisre- narrower thanthenormal2200Ádustfeatureandisprobably indicative ofthepresencesupergiants(Benvenuti,Casini,& which havethetypicalabsorptionfeaturesofOandBstars Heidmann 1982b).Afeatureispresentat2200Â,which age, 100timesbrighterintheopticalthan30Doradusand man 1981).UGC3838hasbrightclumpswhichare,onaver- compact galaxyisagiant,clumpyirregularwithnumberof to depletethegalaxyofalargeamountitsgassupply. starbursting knotsofexceptionalintensity(Gordon&Gottes- ( 1990)arguethattheISMcontributesSirvXI400andC imaging revealsthepresenceofabipolaroutflowgas,likely brightness populationbeingricherinhigh-massstars.Ha chotomy maystemfromadifferenceintheIMF,withhigh 1981). Itsfar-infrared(FIR)luminosityishigh[log(L^r/ B formation thataroseatdifferenttimes.Alternatively,thedi- 0 XI550 absorptionfinescomparabletothestellarcontribution. 1.5 kpc.Thedichotomymayoriginatefromtwoburstsofstar Synthetic spectra(Benvenuti,Casini,&Heidmann1982a) NGC 2415(Haro1);Irrpec,BCG.—NGCisina NGC 2403;Sc.—Thefluxofthisgalaxyisapproximately NGC 1705isagas-richBCG,andbecauseofthis,Yorketal. UGC 3838(VIIZw153,Mrk7);Im,BCG.—Thisblue Vol. 86 1993ApJS ... 86 ....5K jor burstsabout1-2Gyrago. intriguing galaxy. UV datawouldcontributesignificantlytounderstanding this core source(Hummeletal.1982).Highersignai-to-noiseratio rare examplesofaradio-emittingspiralgalaxywithVLBI higher resolution(VLBI),NGC2639isfoundtobeoneof the action withthecompanionA0843+49.Whenobserved galaxies andisintermediatebetweenthemetallicityof the UVspectrumbyBurstein etal.(1988)ledtotheconclu- cess isthermalandrelatedtostarformationtriggeredbyinter- extended natureoftheradioemissionthat pro- extended source.Condonetal.(1982)concludedfromthe and aSeyfertgalaxy.NGC2639isradio-loudgalaxywithan (1983b, 1984)toconcludethatitisacompositeofLINER galaxy (Sa)hasalargebulgecomponentwithbroadHaemis- ity ofHolmbergIIislowcomparedtothatnormalspiral berg II,sothatlittlehiddenstarformationcanbepresent this early-typespiralgalaxy(SO/a)showslittleevidence for indicate thepresenceofsomeweakabsorptionUnes. active starformation.DepressionsintheUVcontinuummay the absorptionfeaturestypicalofmassiveOandBstarsfrom LMC andthatoftheSMC(Hunter&Gallagher1985). can beconsideredapproximatelyconstantoveraHubbletime tion rateislowerthanthattypicalofnormalspiralgalaxiesand giant Hiiregion,whereintensestarformationistakingplace. the M81-NGC2403group.Withadistanceofabout3Mpc,it sion thatthegalaxyhassome residualstarformationwithma- sion andlow-ionizationemissionlines,whichleadKeel (Hunter etal.1989a).Likemostdwarfirregulars,themetallic- suggests thatonlyasmallamountofdustispresentinHolm- (Hunter &Gallagher1985).AnalysisofIRASobservations region (cf.Rosaetal.1984).Thespectrumshowspossible Holmberg IIdoesnotappeartobephysicallyinteracting (Sandage &Tammann1975).Despiteitslocationinagroup, is oneofthenearestcondensationsinlocalsupercluster with compactcoreandmanyknots.Itisaresolvedgalaxyin BCDG.—Holmberg IIisabluecompactdwarfgalaxyde- seen (vanderKruit1971;Condon 1987,Table2).Analysisof nuclear activityintheUVspectrum(Heckman1980). cates starformationactivity.However,thereisnoevidenceof Huchtmeier &Richter1988).Thehighshort-wavelengthUV up halfthetotalmassofgalaxy(Thuan&Seitzer1979; between themof^1?7(Thuan&Seitzer1979),correspond- possible companionofHolmbergIIwithanangularseparation nebular emissionofCm]XI909.Thegalaxy-widestarforma- Indeed, thecontinuumofUVspectrumistypicalanHn (Davis &Seaquist1983). flux ofthisgalaxyissimilartothatinHolmbergIIandindi- ing toabout0.1Mpc.Likemostdwarfgalaxies,theHicontent chentseva, Karachentsev,&Bomgen1985).UGC4483isa scribed byZwicky(1971)asalargeposteruptiveblueirregular of UGC4483isrelativelyhigh,withneutralhydrogenmaking high surfacebrightnessandbelongstotheM81group(Kara- No. 1,1993 Although detectedintheradio,nocompactsourcehasbeen The UVemissionofHolmbergIIisdominatedbyasingle NGC 2639;Sa,LINER+Seyfert.—Thisearly-typespiral NGC2782; SAB(rs)a,starburst.—This starburstgalaxyhas NGC 2681;Sa,LINER.—LikeotherLINERsintheatlas, Holmberg II(VIIZw223,Arp268,DDO50);Irr, UGC 4483;dimIV,Hn.—Thisdwarfgalaxyisofrelatively © American Astronomical Society • Provided by theNASA Astrophysics Data System UV SPECTRAOFSTAR-FORMINGGALAXIES 6 ing branch,withfluxincreasingfrom1800to1200Á. trum hasdeep,complexabsorption featuresofastarburstgal- axy, butwithaslopeincreasing towardlongwavelength.This entire nucleus(Bonatto,Bica,&Alloin1989).TheUVspec- early andlate-typestars,which isconsistentwiththeconclu- slope, aswellthecomplex absorptionfeaturesacrossthe formation withinitshotspotknotsandalsothroughout its the UVspectrum.However,NGC2841doesshowaclear ris- IUE aperture.)Noprominentemissionfeaturescanbeseen in the mechanismisphotoionization.Aringofenhanced star their paper.TheIUEslitwascenteredonthepeakof10¡xm entire IUEwaveband,indicates thepresenceofamixture tures, typicalofmassiveOandearlyBstars. ied byJosephetal.(1986),andmanydetailscanbefoundin galaxy ([O/H]-0.15[O/H];Kunth&Joubert1985). trum ofMrk19showsthetypicalfeaturesagiantHnregion tion (Sanders&Mirabel1985). by Keel(1984),whonotestheflatnessofradiospectrum. ble thoseinthespectrumofstarburstprototypeNGC7714 near-IR data(Prietoetal.1985).(Theringliesoutside the formation surroundingthenucleusissuggestedbyoptical and Phillips, &Terlevich(1981)concludethattheionizingmecha- of opticalemission-fineratiosandstrengths.WhileBaldwin, LINER byHeckman(1980)andKeel1983a,b)onthebasis emission. TheUVcontinuumisflat,asexpectedinastarburst short-wavelength IUEspectrumofNGC2798hasbeenstud- also inlinewiththeabovescenario(Josephetal.1986).The man, &Miley1990).Theextended10and20/unemissionis and forthepowerfulfar-inffaredluminosity(Annus,Heck- (Heckman etal.1983),forthenarrowopticalemissionlines, Prestwich 1986),fortheextendednuclearradioemission interaction mayberesponsibleforthestrongburstofstarfor- in agreementwiththepictureofanHnregion(seeRosaetal. The highfar-infraredluminosityandthestrengthofCO classification ofLINERplusstarburst.Thisideaissupported center. Thestarformationmaybetriggeredbytheanonymous nism isshockheating,Ferland&Netzer(1983)suggest that (cf. NGC7714),andthereareCrvSiabsorptionfea- mation presentinthenucleusofgalaxy(Joseph,Wright,& and theblendsforX>1800Â.Thepaucityofabsorption short bursts(Kunth&Joubert1985).TheUVcontinuumis stant starformationratesincethestartoflastburstabout (Neugebauer etal.1976)andisinterpretedasreflectingacon- emission supportthescenarioofanintenseburststarforma- radio spectrumiscontroversial:Heckmanetal.(1983)finda companion (Condonetal.1982).However,thesourceof nova remnantsfromtheactivestarformationingalaxy kpc) radiosource,whoseemissionisprobablyduetosuper- (Kinney etal.1984).Thenucleusisastrong,extended(~1 a UVcontinuumandstrongabsorptionlineswhichresem- forms aninteractingpairwithNGC2799.Thegravitational features maybeduetotherelativelylowmetallicityof “lazy” galaxyforitspropertyofformingstarsbyintermittent 6 X10yrago(Dottori1983).Thisgalaxyisalsodefinedasa nonthermal componentinaddition,leadingtothecomposite o 1984), buttheonlyvisibleabsoytionfeaturesareSirvXI400 NGC 2903;Sbc,hotspot.—NGC2903containsactivestar NGC 2841;Sb,LINER.—ThisSbgalaxyisclassifiedasa MCG 10-13-71(Mrk19),Irr,BCDG.—Theopticalspec- NGC 2798;SBa,starburst.—Thisbarredspiralgalaxy 27 1993ApJS ... 86 ....5K 7 by apower-lawspectrum.Thebroadpermittedfines,on the fine broadeningisduetothemotionofgasarounda very where gasisshock-heatedbyacentralsourceorphotoionized trum exhibitstheemissionfrom Wolf-Rayetstars)byKunth that hasalsobeencalledaW-R galaxy(awhosespec- belongs totheVirgoClusterand isastarburst(Balzano1983) is thatofanormalearly-type spiralgalaxy. Peimbert 1981;seealsothedetailedanalysisofFilippenko & compact centralobject(M—10M;Peimbert&Torres- den fines,ontheonehand,comefromanextendedregion difierent regions:Thenarrowpermittedfinesandtheforbid- Sargent 1988).Inspiteofthepresencetypicallybroad other hand,originateinasmall,compactcentralregion. The Ellis etal.(1982).Theemissionprobablyoriginatesfrom two been analyzedbyPeimbert&Torres-Peimbert(1981)and by Seyfert emissionfines,suchasMgnX2800,theUVcontinuum Ellis, Gondhalekar,&Efstathion1982).TheUVspectrumhas centered onthegalaxy(cf.Peimbert&Torres-Peimbert1981; which showacommonHienvelope(Condonetal.1982). to beinteractingwiththeothercomponentsofM81group, companions increasetheactivityofnucleus.M81appears al. (1985)havefoundevidencethattidalinteractionswith them asgiantHnregions(Meabum&Terret1982).The galaxy hastwoparts,distinguishedbytheiropticalproperties: a centralredcore,consistingofolderstarsandinquiescent the blueandcontainsweaklow-ionizationabsorptionfeatures two separatestar-formingregionsinthisgalaxy,surroundedby to Galacticabsorptionalone(seeTable4). source (Condonetal.1982;Kellermann1976).Keel low-luminosity Seyfert1galaxy(Peimbert&Torres-Peimbert axy, whichhasthelow-ionizationemissionfinesofaLINER ing ofanumberknots,whoseemissionspectrumidentifies phase (noemission-fineactivity),andablueannulus,consist- (Dufour etal.1988). U Vspectrumofthissuper-metal-poorcompactgalaxyrisesto a 3kpcenvelopeofHaemission(Dufour&Hester1990).The first burstofstarformation(Searle&Sargent1970).Thereare extragalactic Hnregionthatismostprobablyundergoingits known ([O/H]^0.02[O/H];Dufour,Garnett,&Shields compact dwarfgalaxyisoneofthemostmetal-poorgalaxies extinction. TheMgnabsorptionfeatureistoostrongtobedue (Heckman 1980)butalsohasthebroademissionfinesofa H nregions. reddened B-andA-typestars(Walshetal.1986).Theredden- absorption fines.Frompopulationsynthesis,theknotsof and theonlyconvincingfeaturesareSirv,CMgn radius oftheringisabout4",andincludedinIUEslit ing isduetotheobscurationinducedbydumpinessof NGC 2997apparentlyconsistofreddenedOstarsandless (see Walshetal.1986).TheUVspectrumisweakandnoisy, central regionsintheFbandisduetoavariationofinternal mons etal.(1988)notethatthe“patchy”appearanceof sions ofOkaetal.(1974)basedonopticalobservations.Si- 0 1981). Thegalaxycontainsacompact,powerfulnuclearradio 1988). IZw18hasbeendescribedastheprototypicalisolated 28 o The spectraofM81includeonlythosewiththeaperture NGC 3049(Mrk710);SBbc, starburst.—Thisspiralgalaxy NGC 2997;Sc(s),hotspot.—Thenucleusofthis“hotspot” NGC 3031(M81);Sb,LINER.—MSIisanearbySbgal- / Zw18(UGCA166,Mrk116);Irr,BCDG.—Jhisblue © American Astronomical Society • Provided by theNASA Astrophysics Data System KINNEY ETAL. o 10 bright peculiargalaxyhasacomplexmorphology,with ring greater than350pc.Thelowmetalficityresemblesthatofthe broad absorptionfeaturesrevealthepresenceofyoung,hot trum (alsostudiedbyDurret&Bergeron1986)showsthe blue opticalcontinuum(Telesco&Gatley1984)andstrong than 20Myrold. lengths (Fanelfietal.1988).ThestellarsynthesisofFanelli et tion finesandacontinuumthatrisesslowlytowardshortwave- pact dwarfgalaxyhasgonethroughseveralburstsofstarfor- with verystrong,deepabsorptionfeatures.Whilethe Joseph &Wrightsignalamerger.Theshort-wavelengthUV by Joseph&Wright(1985)a“super-starburst.”NGC3256is a W-Rgalaxyintheoptical,itspopulationseemstobe ular amorphousgalaxyisadwarfundergoingstrongstarfor- luminosity (Phillips,Charles,&Baldwin1983).TheUVspec- galaxy hasthesamerelativeemission-fineintensitiesandemis- gether withapopulationsynthesismodel,canbefoundin the visible,UV,andfar-infraredpropertiesofMrk710,to- place NGC3310amongthemost luminousstar-forminggalax- cal emissionfines(Heckman & Bafick1980)andtheveryhigh lier burstsofstarformation,themostrecentbeingnotmore al. indicatesthatthegalaxyhasgonethroughatleasttwo ear- spectrum ofUGC5720exhibitswell-defined,strongabsorp- LMC (Meurer,Cacciari,&Freeman1990).Theultraviolet mation andpossessesalargestarformationregionofsize 0.13 mag]. stars, theoverallslopeisprobablyduetodust[E{B-V)= spectrum showsafluxdecreasingtowardshortwavelengths a PCygniprofileofCrvX1550,consistentwiththepicture of quiescence(Kunth&Sargent1981).TheUVspectrumhas result ofperiodicburstsstarformationfollowedbyperiods mation activity(Kunth&Sargent1983;GallagherHunter of aSeyfert2galaxy,aswelltheflatcontinuum(FceX). emission finesofhighexcitationandlowtypical present burstofstarformationisprobablyonlyabout5 IR luminosity(L^3X10 L;Telesco&Gatley1984), (Fabbiano, Feigelson,&Zamorani 1982;vanderKruit&de extended X-ray,UV,andradioemissionofthermalorigin Bertola &Sharp1984).Thegalaxyhasanextremelybright a radiusoffewkiloparsecs,andwith“bowarrow” ory 1990).Tidaltailsevidentintheopticalphotographsof also ultraluminousintheinfrared(Kawara,Nishida,&Greg- very brightstar-formingregionspanningover4kpcandcalled NGC 3125asaW-Rgalaxy. sion-fine profilesasaSeyfert2galaxy,butwithmuchlower Myr old. Mas-Hesse, Arnault,&Kunth(1989),whoconcludethatthe a thermalsource(Balzano&Weedman1981).Adiscussionof Cygni profilesorHenemission,aswouldbeexpectedifW-R Bruyn 1976).Alltheseaspects, inadditiontotheintenseopti- structure inthenorthwestregion(Walker&Chincarini1967; of Hnregionssurroundingthenucleus(anregionitself) at stars werepresent.Thenear-IRemissionhasbeenattributedto & Schild(1986).OurUVspectrumdoesnotshowclearP 1987; Kunth,Maurogordato,&Vigroux1988).Recognizedas x IR 0 NGC 3125(Tol3),IrrAm,BCDG.—Thismetal-poor,irreg- NGC 3310;SAB(r)be,starburst.—Thecentralpartofthis NGC 3256;Sb(s)pec,starburst.—Thisgalaxycontainsa NGC 3081;SBa,Seyfert2.—Thisearly-typebarredspiral UGC5720 (Haro2,Mrk33);Im,BCDG.—Thisbluecom- Vol. 86 1993ApJS ... 86 ....5K galaxy hasbeenrecognized as astarburstbecauseofmany properties; theradiobrightness ofthisamorphousgalaxy giants. tion absorptionfinesrevealsthattherearemanyearlysuper- comes mainlyfromthenucleus, thespectrumisdominatedby dally interactingbinarywith the dwarfspiralUGC6016.This the geocoronalemission,i.e.,LyaA1215andNvA1240. In tures. ThespectrumofthisBCGshowsarichandcomplex with strongabsorptionfeatures,suggestingthepresenceof forming activityofthegalaxy,andpresencehigh-ioniza- The relativelyflatcontinuumisamanifestationofthestar- clearly distinguishedfromthoseduetoGalacticabsorption. addition, theintrinsicFeuA2600andMgnA2800fines are tin (1981).Thecontinuumrisessteeplytoshortwavelengths system ofabsorptionfines,includingthoseusuallyhidden by massive, hotstars. it isablueemission-finegalaxyformingstarsbyintermittent as a“lazy”galaxybyKunth&Joubert(1985)—meaningthat emission finestypicalofSeyfert2nuclei.Adetailedanalysis tion episodes. giants; thelow-ionizationabsorptionfineshavestellarorigin; typical BCDGwithaUVcontinuumrisingtowardshortwave- tion istakingplace.Inparticular,theringlikestructureofM95 of thisgalaxyseparatesintrinsicfeaturesfromGalactic fea- short bursts—andasabluecompactgalaxybyThuan&Mar- can befoundinDiaz,Prieto,&Wamsteker(1988). ing continuumoftheSBagalaxyandwithverystrong,narrow low-level continuumfluxwithsomeevidenceoftheunderly- due tothehighstarformationrateandlimitedgassupply, that thestellarpopulationiscomposedofmain-sequencestars ties ofthisgalaxy,inadditiontoastudyspectralsynthesis, trum showsunusuallystrongCrvandMgnabsorptionUnes. produce anaccumulationofneutralgasontheinnerLindblad Nieto (1982)suggestthattheburstisrelatedtoexistenceof has anexternaldiameterofabout20",aroundareddernucleus galaxy: aquiescentnucleusissurroundedbyringofHn associations. negligible; thereisnosignificantpopulationofbluesuper- ranging from03tomid-A;thecontributioncoolstarsis can befoundinFanellietal.(1988).Themainconclusionsare lengths andaspectrumrichinbothlow-high-ionization resonance, providingfuelforthestarformation.TheUVspec- a radialinflowoftheringtowardnucleus,whichmight content ofOstarsgivesayoungagetotheburst.Alloin& There arethreemajorcomplexesofHnregions,whosehigh regions whichappearasbluerknotswhereintensestarforma- continuum andthedeepabsorptionlinesaretypicalofOB agreement withthepictureofastarburstinggalaxy:rising (Telesco &Gatley1984).TheIUEspectrumisinperfect ies. Themostintenseandyoungestburstistakingplaceinthe star formationhistoryischaracterizedbydiscreteforma- absorption features.AcompletediscussionoftheUVproper- of about2"(Alloin&Nieto1982andreferencestherein). “jumbo” Hnregion,situated15"southwestofthenucleus No. 1,1993 NGC 3448,IrrAm,starburst.—NGC 3448ispartofati- 1050+04 (Mrk1267);BCG.—Therelativelylargeredshift MCG 9-18-32(Mrk153);Sep,BCDG.—Múl153isdefined NGC 3393;SBa,Seyfert2.—This2galaxyhasa NGC 3353(Haro3,Mrk35);Im,BCDG.—Rzro3isa NGC 3351(M95);SBb,hotspot.—Thisisatypicalringed © American Astronomical Society • Provided by theNASA Astrophysics Data System UV SPECTRAOFSTAR-FORMINGGALAXIES 1 5 galaxy isfaintandpointfikeintheUV.Mrk36probably type starburstgalaxyNGC7714. gest thatthegalaxyhasacompositenucleus,whichshowsboth tola etal.(1984)concludethattheshort-wavelengthUVflux these propertiesmaybeexplained withinastarburstmodel. looks likethatofanormalSBbcgalaxywithnononthermal between aSeyfert1andnarrowemissionfinegalaxy(NELG) with thestarformationscenario. low metalficity.OnlyCrvA1550andtheFeblendaroundA^ rich absorptionfeaturesresemblethespectrumofproto- population ofmassivesupergiants.Theflatcontinuumandthe The opticalspectrumisdominatedbytheregionsofactivestar radio sourceinaregionofabout1kpc(Condonetal.1982). The radioemissionisduetothepresenceofastrongnuclear is duetoearlyBstars. center ofthegalaxy(Noreau&Kronberg1985b,1987).Ber- can beidentifiedintheoptical, radio,andIRbands—regionA Carico etal.1988),andhasthemostluminousopticalemis- activity, presumablytriggeredbyaninteraction(Gehrz, Sra- acting” galaxies(deVaucouleurs,de&Corwin contains bothobjectsinthispairof“collidingorstronglyinter- This galaxyisclassified,onthebasisofopticalspectrum,as fine isalsodetected.Therisingbluecontinuumconsistent Pei, &MacMahon1989),purportedtobeproto-diskgalaxies tude aboveeventhatinferredfordampedLyasystems(Fall, ies. Indeed,thegas-to-dustratioofthisgalaxyisgreaterthan evolved enoughtohavebuiltupthedustseeninnormalgalax- young; althoughitisundergoingintensestarformation,its ence ofaPCygniprofileforCrv,indicativeanevolved (van Moorsel1983). companion NGC3512,50kpcdistantfromthemaingalaxy formation (Keel1984),whicharepossiblytriggeredbythe nonthermal activityandrecentstarformation(Keel1984). ence ofmassive,hotstars(Noreau&Kronberg1985a).The region C.Allofthemarestarbursting (Gehrzetal.1983).In (nucleus ofIC694),region B (nucleusofNGC3690),and The systemhasacomplexmorphology: threebrightestregions sion finesofanynon-Seyfertgalaxy(Weedman1972).All of et al.1982),hasahighinfraredluminosity(Z^r^5X10 L; mek, &Weedman1983).Itisastrongradiosource(Condon sentative exampleofintenseandwidespreadstarformation sion. activity. Thisgalaxy,withz=0.012,showsstrongLyaemis- (Kollatschny etal.1983).Nevertheless,theUVspectrum (Wolfe 1987). dust contentisexceptionallylow,basedonIRASfluxes supernova remnantsandarecoincidentwithadustlaneinthe sources similartothoseseeninM82,whicharemostprobably nuclear radiosourcehasbeenresolvedintoafamilyofpoint far-infrared emission,andtheUVfluxistypicalofpres- ( Gondhalekaretal.1986),suggestingthatthestarsmaynotbe 1976), thepartnerbeingIC694.Thissystemismostrepre- 1620 Àarerecognizable.TheCm]A1909nebularemission 10 (Gondhalekaretal.1986),whichistwoordersofmagni- 0 The UVspectrumisrichinabsorptionfines,withthepres- The UVabsorptionfinesareweak,probablybecauseofthe Mrk 36(Haro4),Irr,BCDG.—Thisbluecompactdwarf NGC 3690+IC694;Scpec,starburst.—TheIUEaperture NGC 3660(Mrk1291);SBbc,mini-Seyfert1,NELG.— NGC 3504;SABab,starburst.—Opticalandradiodatasug- 29 1993ApJS ... 86 ....5K 8 41 -1 tinuum emissionbetween1500 and1900Á. galaxy withhigh-excitationemissionfines,alargefraction dence ofemissionfines,while theshapeofcontinuumre- cannot besustainedformorethan10yr.TheUVspectrum in amultipleinteractingsystem isconsideredthemaincause sembles thatofanormalScgalaxy, withsomeadditionalcon- optical andradiowavebands,theUVspectrumshowsno evi- (Hummel etal.1987b).Inspiteofthesignsactivityin the has aweakbroadcomponentofHaandisradiosource in theringfikeouterarms(Keeletal.1985).NGC3994 also has acomplexstructure,withvigorousstarformationgoing on NGC 3991and3995.Onthebasisofcriteriagiven by with highsignal-to-noiseratioshowsabsorptionfinesaswell as emission dominatedbymassive,hotstars. resembles thoseofHnregions(cf.Rosaetal.1984)with sequence, thatthepresentstarformationrateofNGC3738 axies formstarsmoreefficientlythandospiralsand,asacon- However, Tacconi&Young(1985)suggestthatirregulargal- (following theprescriptionbyGallagher,Hunter,&Tutukov Phillips etal.(1983).Hunter&Gallagher(1986)conclude ately lowmetalficity.IthasbeencalledanormalHngalaxyby of itsmassintheformneutralhydrogen,andwithmoder- 0.012), theLyaabsorptionfineisdetected. UV spectrumconfirmstheintensethermalactivityofNGC may notbeexplainablewiththermalprocesses(Gehrzetal. Baldwin etal.(1981),NGC3994isclassifiedasaLINER. It emission inLyaandHen. emission totheintensestar-formingactivity.Thisspectrum where theemissioniscomparabletothatofaSeyfertgalaxy nuclear regionC(Joyetal.1989).Theabsorption-Une-rich nates fromacompactsourceinNGC3690,probablytheextra- (Seaquist &Bell1968),andintheX-ray(L=2.5X10ergs H nregion.Ahigherlevelofactivityisrevealedintheradio, in BCGsisalsotreated)andbythecharacteristicsofourUV Arnault etal.1988,wheretheproblemofnondetectionCO bles anHngalaxy,withaverybluenucleus(Keeletal.1985). the companionsmaytriggeractivityofgalaxy(Keelet region AthereisbotharadioandanIRunresolvedsource, s; Fabbianoetal.1982).TheauthorsattributetheX-ray spectrum, whichaccordingtoRosaetal.(1984)resemblesan The BCGnatureissupportedbyitslowmetalficity(see,e.g., al. 1985).TheopticalspectrumshowsthatNGC3991resem- NGC 3994and3995.Thegravitationalinteractionwith belongs toamultipleinteractingsystem,whichalsoincludes tures. 3690. Becauseoftherelativelyhighredshiftthisgalaxy(z= originates (Joyetal.1989).Thissourcemightbecompactand from which60%ofthefar-infraredluminositysystem in theoptical.TheUVcontinuumisdominatedbynormal presence ofhigh-excitationfinesandlowintrinsicluminosity fied asSeyfert2-fikebyPhillipsetal.(1983)basedonthe any prominentemissionfinesintheUV,despitebeingclassi- Sbc galaxyspectrumandshowsevidenceofabsorptionfea- 1984) thatthestarformationratehasbeenconstantintime. 1983) .Theremaining40%ofthefar-infraredemissionorigi- 30 x NGC 3738;IrrIKHn.—NGC3738isagiantirregular NGC3995; Sm,Hn.—Themembership ofthisspiralgalaxy NGC 3994;Sc,LINER.—Thisgalaxyinteractswithboth NGC 3991(Haro;Im,BCG.—ThisMagellanicirregular NGC 3982;Sbc,Seyfert2.—ThisSbcgalaxydoesnothave © American Astronomical Society • Provided by theNASA Astrophysics Data System KINNEY ETAL. their responsetotheinteractionmustvary,sincespectra broad absorptionfeatureofSirvindicatethepresence the abovepicture.AlthoughNGC3391,3394,and the lessthanoptimalsignal-to-noiseratio,ourUVspectrumis galaxy (Heckman1983),andaFIRG(Annus,Heckman, & with anoldstellarpopulation(cf.Gregg1989),showingMgn with someevidenceofamedium-agemain-sequenceturnoff. IUE aperture,theUVspectrumdoesnotresemblethatofa tion, andtheradiocoreissmallenoughtobeincludedin the radioemissionisattributedbyCondonetal.tosuper- presence ofopticallow-ionizationfines.NGC4102alsohasa which appearsasasupergiantHnregion(Annusetal.1990). powerful far-infraredgalaxy(FIRG)(Youngetal.1989), Ursa Majorgalaxygroup(Odenwald1986).ThisSbisa evolved, early-typemassivestars,withtemperatureshot ing ofinteraction-inducedstarformation. are allverydifferent.Thuswefarfromagoodunderstand- in thegalaxy.(TheUVspectrumcontainsemissionartifactsat in agreementwiththestrongHnregionsthoughttobepresent continuum inthevisible(Kennicutt&Keel1984).Despite burst ofstarformationthatisclaimedtobedrivenby the cal ofF-Gdwarfs.Theshort-wavelengthspectrumislackinga and Feabsorptionfeatureslongwardof2600Awhicharetypi- Keel (1983b)classifiedthisgalaxyasaLINERbecauseofthe enough toexcitetheforbiddennebularemissionfineCm] of itsenhancedHnregionemissionspectrumandveryblue Miley 1989).Theactivityisapparentlypoweredbyacentral 4194. and isprobablydueinparttointrinsicabsorptionNGC presence ofacoolercomponentAstars.Thedepth the profile ofCrv)showthepresenceahotpopulationmas- NGC 4111maybeontheboundarybetweenactiveandnor- little evidenceofnonthermalactivityfromtheUVspectrum. 4111 isclassifiedasaLINERbyHeckman(1980),butthere apparent effectonthegalaxyitself(vanderBurg1985).NGC 4111 hasatleasteightmuchfaintercompanions,theyhaveno hot starcomponent(Bursteinetal.1988).AlthoughNGC starburst galaxy.NGC4102appearstobeanormalSbgalaxy strong nuclearradiosource(Condonetal.1982).Although cient blueMagellanicirregular galaxy.IntheUVstudyby (Joseph &Wright1985). merging oftwogalaxies,asevidencedinpartbythetidal tail Mg nX2800featureisgreaterthanexpectedfromourGalaxy sive OandearlyBstars,theveryflatspectrumsuggests the absorption featuresofSirvandC(withapossiblePCygni shows anunusuallyflatcontinuum(seeTable5).Whilethe mal galaxies. nova remnantsassociatedwithastrongburstofstarforma- 3395 areallmembersofthesamegroup,andinteracting, Huchra etal.(1983),whohave carefullycenteredtheIUE XI909. aperture ontheopticalcenter ofthegalaxy,PCygniprofile 1987b) andintheX-ray(Fabbianoetal.1982)alsosupport 1280, 1290,and1663Â).Dataintheradio(Hummeletal. NGC 4194isaBCG(Thuan&Martin1981),radio-loud NGC 4111;SO,LINER.—NGC4111isanormalSOgalaxy NGC 4102;Sb,LINER+Hn.—NGC4102belongstothe ESO 572-34;Hn.—ThePCygniprofileofCrvandthe NGC 4194(Mrk201);Smpec,ÆCG.—ThisBCGgalaxy NGC 4214;lABm,starburst.—NGC 4214isametal-defi- Vol. 86 1993ApJS ... 86 ....5K -4 this normalgalaxyhasbeenstudied andsynthesizedbyRocca- biano, &Cañizares1986).The UVspectrumofthenucleus grated contributionoflow-mass binaries(Trinchieri,Fab- quiet galaxywithanX-ray/optical luminosityofabout1.3X disk asopposedtostarformationinthenucleus.Itisaradio- both ourGalaxyandNGC4321. comparison withtypicalSOgalaxies(Véron&Véron-Cetty UV spectrumconsistentwithitsHubbletype,asdescribed in the interstellarmediumpresentinhalosanddisks of gions, wherestrongstarformationispresent(Pierce1986;Ar- strongly interactingpairwithNGC4394(Cutri&McAlary surface brightness,belongstotheVirgoClusterandforms a § 1.NGC4350belongstotheVirgoCluster. They concludethattheabsorptionfeaturesaremostlydueto galaxy. of thegalaxy,andhavebeenstudiedbyPanagiaetal.(1980). of theseHnregionswhicharecontainedinthenuclearregion senault etal.1988).TheUVspectrapresentedhereareoftwo The ring,about13"inradius,containsfourdistinctHnre- Virgo Clusterandisanotherexampleofa“hotspot”galaxy. nonstellar emission.ThebluerisingbranchoftheUV, fied asaLINER,approachingtheSeyfertdomain(Heckman ratios oftheopticalemissionfines,thisgalaxyhasbeenclassi- Krause, Beck,&Klein(1984).Basedonthestrengthsand its innerregions,whichalsoemitintheradio.Theradioemis- tures insomelocationsNGC4214.Hartmann,Geller,& match up,mostlikelybecausethepositionanglesof10"X lution. Theshort-andthelong-wavelengthspectradonot broad, deepabsorptionfeatures,andthenebularemissionfine of matteroranexplosiveeventinthenucleus,accordingto sion isnonthermalinoriginandprobablyduetotheejection spiral galaxycontainstwoanomalousarmsofHaemissionin consideration isbasedonthedifierencesbetweenvelocity result ofamergerorstronginteractionwithcompanion.This 20" IUEaperturearenotthesame. several burstsofstarformationatdifferentstagestheirevo- (1984) suggestthattheUVcontinuumcanbeexplainedby contribution fromOstars.Barbon,Capacciofi,&Longo ( 1982)findthatNGC4258isdominatedbyBstars,withlittle fields ofthegasandolderstellarpopulation Huchra (1986)concludethattheburstofstarformationis UV wouldseemtoruleoutadecreasingorconstantstarfor- The lackofevolvedsupergiantsandWolf-Rayetstarsinthe can beopticallyresolvedintoHnregionsandassociations. while theabsorptionfeaturesatX<1400Âshowpresence typical ofOstars,whichproduce~50%theUVemission, of Cm]XI909areallcharacteristicHnregions.Ellisetal. note thatFilippenko&Sargent(1991)findWolf-Rayetfea- formation, superposeduponanolderpopulation.However, mation rate,suggestinginsteadarelativelyrecentburstofstar of Bstars.Thegalaxyhasacomplexphysicalstructure,which of CivX1550wasfoundtobeconsistentwiththestrongwinds 10 (Dressel&Wilson1985), easilyexplainedastheinte- 1985), interpretedasduetoenhancedstarformationin the 1985 ).Thisinteractionmightexplainitsbluervisiblecolor in 1980). TheUVcontinuumdoesnotmanifeststrongnuclear No. 1,1993 NGC 4382(M85);SOpec.—M85,agas-poorgalaxyofhigh NGC 4350;SO.—Thisnormalearly-type(SO)galaxyhas a NGC 4258(M106);SBc,LINER.—Thisbright,barred NGC 4321;Sbc,hotspot.—Thisisthelargestspiralin © American Astronomical Society • Provided by theNASA Astrophysics Data System UV SPECTRAOFSTAR-FORMINGGALAXIES tra wereanalyzedbyFerland&Osterbrock(1986)and tinuum. ThustheUVsourceinNGC4388appearstobeoc- fine ofsightbydustintheinterstellarmedium.TheIUEspec- thesis impliesthatthedominantcontributionisgivenbyWN7 culted fromdirectview. larger thanpredictedbasedonthestrengthofionizingcon- and suggestedthatthisemissionoriginatesfromanobscured Filippenko (1988)detectedbroadHaemissionoffthenucleus evidence thatitharborsanobscuredSeyfert1nucleus.Corbin, and WC8. UV, suggestthepresentofWolf-Rayetstars.Populationsyn- Á, aswellthepossiblePCygniprofilesinNvandCrv arms. ThepresenceoftheWolf-Rayetemissionfeatureat4650 ionized gasisconcentratedinacentralregionoffewkilopar- ties ofthisgalaxyaregiveninDurret&Tarrab(1988).To and foundthatthenumberofrecombinationphotonsismuch Kinney etal.(1991a).Theybothfoundasteepspectralslope Seyfert 1broad-fineregion(BLR)whichisreflectedintoour nucleus, andextendingabovebelowthedisk.Shields& high-ionization gasdistributedintwocones,withapicesatthe Baldwin, &Wilson(1988)andPoggehavereported secs andmanyHnregionsaredistributedalongthespiral and extendedHn.Itisatypicalnregiongalaxy,wherethe phy andanextensivediscussionoftheUVopticalproper- dominant contributionfromFandearlyGdwarfstars. tures exceptforstrongCm]XI909emission.Theweaknessof summarize, NGC4385isastarburstgalaxywithplentifulHi Volmerange &Guiderdoni(1987),whoconcludethatithasa blue luminosity,andthestrengthofHaemission(Gallagher et tra thatweretakenwiththeapertureplacedongalaxy with apeculiarsupernovaremnant(Blairetal.1984b). Be- absorption featuresinanobjectthoughttobeundergoingstar indicating thepresenceofhotstars,butlacksprominentfea- BCDG undergoingaburstofstarformation(Thuan&Martin is thoughttobeconstant,basedonananalysisofthemass, center. cause ofthis,wehavebeenespeciallycarefultoextractonly the lanic irregulargalaxy,containingalargeamountofgas,having Fanelfi etal.1988),whilethestrengthofstrongCm]emis- formation mayberelatedtoitslowmetalficity(Z~0.1Z; the long-wavelengthspectrais probablyduetotheplacement al. 1984)andalsobasedonthestrengthofinfraredemis- one short-wavelengthandthelong-wavelengthIUEspec- H nregions(see,e.g.,Rosaetal.1984;Lamb1986) and observations ofNGC4449areconcernedwiththeoff-nuclear star formation(Hunter1982;Bothun1986).ManyoftheUV a complexdistributionofHnregions,andundergoingactive fond &Thuan1983). sion mayberelatedtothehighnebulartemperature(Vialle- companion DDO125.Thepoor matchbetweentheshort-and formation rateisduetoamerger orinteractionwiththedwarf ations, Hartmannetal.(1986) concludethatthestrongstar sion (Thronsonetal.1987).Fromkinematicalconsider- of theaperture. 1981). TheUVspectrumrisestowardshorterwavelengths, 0 The timeevolutionofthestarformationrateinNGC4449 NGC 4388;Sab,Seyfert2.—This2galaxyshows NGC 4385(Mrk52);SBas,starburst.—Alargebibliogra- MCG 8-23-35(Mrk209);Smpec,BCDG.—Mrk209isa NGC 4449;IBm,Hn.—NGC4449isaveryblueMagel- 31 1993ApJS ... 86 ....5K 8 59 both narrowandbroademissionfines,unliketheotherLINER 4579 presentedinthisatlasincludeadditionalspectratothose that thegalaxyappearsstellarinUV.(ThespectraofNGC properties typicalofnormalgalaxies(Willneretal.1985). population ofgiantsfromanolderpopulation. analyzed byGoodrich&Keel.)TheUVspectrumcontains has beenanalyzedbyGoodrich&Keel(1986),whofound ing thepresenceofacentral,nonthermalsource(Halpem& et al.1987b).X-rayemissionhasalsobeendetected,indicat- This objecthasFenabsorptionandunusuallystrongMg sion intherange1-20pmisdominatedbydustandstarlight, a strongemitterat10/^m(Scovilleetal.1983),anditsemis- lines, isclassifiedasaLINER(Stauffer1982;Keel1983b).It Virgo Clusterand,frompropertiesoftheopticalemission are probablyduetoIUEartifacts. redshift. TheonlypossibleemissionlineisLya;otherfeatures vations showsthattheburstissuperposedonanunderlying Analysis ofthecombinationnear-IR,visible,andUVobser- tense far-infraredemissionfromthismetal-deficientbluecom- Seyfert 1(Stauffer1982;Keel1983b;Filippenko&Sargent Steiner 1983).IthasbeenclassifiedasaLINERanddwarf source withaflatspectrumandanunresolvedcore(Hummel absorption. sorption featureswhichareeasilyidentifiedduetothegalaxy’s Mrk 213hasanintenseUVluminosity(Gondhalekaretal. pact galaxy[logiLpm/L©)=10.40;Deutsch&Willner1987]. asymmetry similartothoseseen inNLRGs(Heckman,Miley, by Kormendy(1988)resultedinavelocitydispersionprofile & Green1984),whilenosuch asymmetryisseeninKß(Fair- has averyhighsurfacebrightness, sothatitresemblesNGC indicate thepredominanceofanoldstellarpopulation(Ellis et emission featuresinourUVspectmmindicatesthat the consistent withamassofM~10-10.Thelack of sesses astrongradiocoreembeddedindiffuseemission, and al. 1982). LINER activityisnotstrong,whiletheabsorptionfines(Mg n emission finesintheUV.Asearchforacentralmassiveobject common withtheotherLINERsinthisatlas,thereare no dio andX-rayemissionmayberelatedtothegalaxy’sactivity as aLINER(Heckman1980;Keel1983a,b).However, in and astrongX-raysource(Halpem&Steiner1983).Thera- radio source(Shaffer&Marscher1979;Condonetal.1982) has initsnucleusbothaverycompactandstrongnonthermal core. Goodrich&Keel(1986)proposethatitsUVcontinuum X2800 andFeiXX2868,3025)theshapeofcontinuum of aspiralgalaxy. spectra suggestinsteadthattheUVcontinuumissimply is similartothepowerlawseeninSeyfert2galaxies,butour double radiosourcewithanunresolved,flat-spectrum in theatlas;thismayberelatedtofactthatNGC4579hasa 1985) basedonthebroadHaemissionline.ItsUVspectrum 1984) ,suggestingarecentlytriggeredburstofstarformation. 32 1989). Thenarrow[Om]X5007 emissionfinehasablue 1068, theprototypeSeyfert 2galaxy(Ulvestad&Wilson 0 Our UVspectrumhasaflatcontinuumwithcomplexab- NGC 4569(M90);SABab,LINER.—M90belongstothe NGC 4579;Sab,LINER.—NGC4579isadoubleradio NGC 4500;SBa,BCG.—IRAShasrevealedrelativelyin- IC 3639;SBb,Seyfert2.—Thisnearby2galaxypos- NGC 4594(M104);Sa,LINER.—TheSombrerogalaxy © American Astronomical Society • Provided by theNASA Astrophysics Data System KINNEY ETAL. berg, Biermann,&Schwab1985;AntonucciUlvestad panding ringofHnregionssurroundingthenucleus.Studies tmm typicalofanHnregion(Huchraetal.1983).Itsspec- (Keel 1983b;Halpem&Steiner 1983).LikeotherLINERs, This galaxyisconsideredaLINER basedonopticalproperties and anirregularnuclearlow-ionization zone(Keel1983a). with asmallfine-of-sightvelocitydispersioninitsBLR. The galaxy. tmm showsaforbiddenemissionfine(Cm]X1909)andbroad the ringissiteofintensestarformationactivity.The synchrotron radiationfromsupernovaremnants,confirmthat found inM82andNGC253(Duric&Dittmar1988;Kron- ery ofmanydiscretecompactradiosourcessimilartothose al. 1983). carefully pointedtotheopticalcenterofgalaxy(Huchraet erations holdinthiscase,suggestingarelativelyrecentburstof tmm isverysimilartothatofNGC4214,andthesameconsid- lengths withaspuriousemissionfeatureat1820Á. action withitscompanionUGC7905N,andthisisthoughtto fines (andanemissionartifactat1663À). has acomplexemissionstmcture withnumerousHnregions C rvX1550)narrowerthanthoseofatypicalSeyfert1(Kinney UV spectmmdoesindeedshowemissionfines(mostnotably absorption features.ThecontinuumistypicalofanSab ( 1983a,b)toclassifythisgalaxyasaLINER.TheUVspec- low-excitation emissionfinesledHeckman(1980)andKeel hot bluehorizontalbranch(Pritchet1977).Thepresenceof bursting activity,althoughtheweakfinesandbluecolorsin tmm ofNGC4736,isconsistentwiththepicturepaststar- deduced bypopulationsynthesismodelsoftheopticalspec- and thusthegalaxydoesnotappearasastarburstinUV. of theHaemissionfromring(Buta1988)anddiscov- older population.AsinNGC4214,theIUEaperturehasbeen star formation,withtheyoungstarssuperposedonamuch short-wavelength UVspectmmissteeplyrisingtoshortwave- have triggeredtheactivityofgalaxy(Bushouse1986).The all 1985).TheUVspectmmisflat,withsomeweakemission et al.1991b). rich (1989).GoodrichconcludedthatNGC4748isaSeyfert 1 Osterbrock (1987),andasa“narrow-fine”Seyfert1byGood- has beenalternativelyclassifiedasaSeyfert1.5byDahari& De optical canbeevidencealsoforametal-poorpopulationwith The presenceofahighpercentagestarsasearlyA4-A7, man 1978).DeBmyn(1977)hasreportedanextended(5") and hasanextremelyhighsurfacebrightness(Keel&Weed- metal-deficient bluegalaxywhosecentralregionshaveaspec- Robertis (1988),onthebasisofschemebyVeilleux & Robertis (1985),deGrijpetal.andCarter1984). It Seyfert 1galaxyfromitsopticalspectmmbyOsterbrock& De ( 1988)astheresultofaverypowerfulbutnotrecentstarburst. of theCObandsisexplainedbyWalker,Lebofsky,&Rieke radio sourcecenteredonthenucleus.Theanomalousstrength 50" fromthenucleus,sothatitfallsoutsideIUEaperture, 1988), explainedasbremsstrahlungfromHnregionsand Studies ofthenucleusshowthatthisobjectisrelativelyblue NGC 4826(M64);Sb,LINER.—The “Black-Eye”galaxy NGC 4736(M94);SAab,LINER.—Thisgalaxyhasanex- NGC 4748;Seyfert1.—IRAS1249-131isclassifiedas a NGC 4670;Am,BCDG.—NGC4670isanamorphous, UGC 7905S;BCG.—CGC7905SisaBCGinstronginter- Vol. 86 1993ApJS ... 86 ....5K 8 this BCDG(Thuan&Martin1981;French1980)showsthe ings andrefertothembothasNGC4861.TheUVspectrumof pointings specificallytargetingthebrightknot(NGC4861) tion (Huchra1977).Ourtwospectraaretakenwithdifferent tion emission-finegalaxybelongingtoagroupofsevengalax- Rosa etal.(1984)donotdistinguishbetweenthetwopoint- and thecenterofgalaxy(IC3961)separately.Notethat part, theknotpossiblybeinganHnregionorOBassocia- with abrightknot(NGC4861)superposedonitssouthern still detectable. regions (contributing—25%of theemission;Thuan1984)are also present.Theluminosity oftheSeyfertnucleusissuffi- emission line. burst ofstarformation.Thespectrumisdominatedbyhot group with19memberswhichtracesthecentralComaregion IUE cameras. ciently lowthattheunderlying absorptionfeaturesoftheHn absorption featuresofSirvXX1397,1402andHenXI640 are are present,includingLya,CrvX1550,andHenXI640,while emission fines,thenucleusofNGC5135hasbeencalled a agree withtheageofburst(Bica1988).Thespectrumis stars. TheHnregionisrevealedbythestrongCm]nebular strong absorptionfeatureswhicharethesignatureofOandB stars, whichproduceaUVexcessinthecontinuumand (NGC 4861+IC3961)consistsofadwarfirregular(IC sion at1940ÂisSim]. C ivlineistheonlyidentifiableabsorptionfeature.Theemis- (Perea, 1986).TheUVcontinuumofthisBCDGisflat;the spectrum showsadualnature;severalnarrowemissionfines mini-Seyfert 2(Phillipsetal.1983;Thuan1984).The UV radio observationsandfromtheluminositiesofoptical ies whicharegravitationallyboundandfiewithin1Mpcof one stars. flat withstrongabsorptionfinestypicalofmid-tolate-B emission finesandasmallHnregioncontinuumcontribution yr ago.Adetailedanalysisofthevisiblespectrumsuggestsan tion synthesisofthevisiblespectrum(Bica&Alloin1987) C n]isevident,whilem]cannotbedetected,sinceitsred- this galaxyisastarburst(cf.Gondhalekaretal.1984).The fert 2activity(Kollatschny&Fricke1989).FromX-ray and another. TidalinteractionsmaybecausallyrelatedtotheSey- underlying metal-poorred(old)population;residualweak suggest aburstofstarformation,whichoccurredabout4X10 shifted wavelengthliesinthelowestsensitivityregionof relatively highredshift.Thenebularemissionline[Om]+ strong absorptionlineofLyacanbeobservedbecausethe uum andthecomplex,broadabsorptionfeaturessuggestthat possible emissionlineofCm]XI909). are typicalofnormalgalaxies(Fabbiano,Gioia,&Trinchieri the radio,X-ray,andfar-infraredluminositiesofNGC4826 dance (Bica&Alloin1987;Bica1988;GlassMoorwood axy isveryblueintheopticalandhassubsolarmetalabun- 1984 ).IRobservations(Glass&Moorwood1984)andpopula- 1988). TheUVspectrumistypicalofanSbgalaxybutwitha No. 1,1993 This galaxyhasananomalous ratioofLya/Hß(~5),sug- NGC 4861+IC3961(Mrk59);Im,BCDG.—Mrk59 NGC 5135;SABb,Seyfert2.—NGC5135isahigh-excita- NGC 4853;SO,BCDG.—Thisgalaxyisamemberof MCG 6-28-44(Mrk54),BCG.—ThestrongUVcontin- NGC 5102;SAOpec,starburst.—Thislow-luminositygal- © American Astronomical Society • Provided by theNASA Astrophysics Data System UV SPECTRAOFSTAR-FORMINGGALAXIES tems suchasX-raybinariesandoldstarbursts,ortogasout- wavelengths indicatesavalueforintrinsicE(B—V)^0.3 mag (Ellis etal.1982). there arenootherdetectedemissionfines.Thepresenceofa by Palumboetal.(1985)asbeingduetoevolvedstellarsys- tended overthegalaxydisk.TheX-rayemissionisexplained bles, probablyejectedfromthenucleus(Fordetal.1985). the starformationisstrongemissioninradio(Condonet continuum suggestthatthedominantpopulationisA-Gstars evidence ofnonthermalactivity;exceptforSimandCm], X-ray emissionisnotconcentratedinthenucleusbutex- However, thecompositenuclearactivityinradiodoesnot wings initsopticalemissionfines.Studiesoftheradio have classifiedNGC5194asatransitiongalaxybetween galaxies (Dodd,Andrews,&Macgilfivray1986).Thisgalaxy with brightknots,whichisamemberoftheIC4296group of (Richter &Rosa1984).AlthoughtheUVspectrumdoes not cleus isinagreementwiththegeneralscenarioofastarburst large numberofsupernovaehavebeenobservedinthisgalaxy tion ofsupergiants,whosesignatureisthePCygniprofiles companion NGC5253(Condonetal.1982).Associatedwith strong absorptionfeatureofAlmXI857andtheshape flowing fromthenucleus.TheUVspectrumdoesnotshow have acounterpartintheX-ray(Palumboetal.1985).The of NGC5194showacomplexstructureextranuclearbub- LINER andaSeyfertgalaxybecauseofthepresencebroad been studiedbyHartmannetal.(1988),andfurthercom- which surroundsamorecompact nucleus.Thenumberof has adiffuse,extendedHnregion poweredbyOBassociations (Pastoriza 1975). show amarked2200Âdustabsorption,observationinoptical supernova withHnregionsinthespiralarmsand nu- (five since1923,amongwhichtheonedetectedinnucleus Si rvXX1397,1402andCX1550(Bohlinetal.1983).A sorption fines,whichhaveastrongsimilaritytothoseofNGC X-ray (Trinchieri,Fabbiano,&Palumbo1985).TheUVab- al. 1982),intheinfrared(Telesco&Houper1980and in thenucleusandspiralarms,possiblytriggeredbyits Pastoriza 1965).M83isundergoingaburstofstarformation a classofgalaxieswithan“amorphous”nucleus(Sersic& (Keel etal.1985).Heckman(1980)andBaldwin1981) forms aninteractingsystemwithitscompanionNGC5195 ments canbefoundintheirpaper. ing activestarformation.TheIUEspectrumofMrk66has 7714, suggestthatM83isastarburstwithanevolvedpopula- southern galaxywhichisalmostface-onandbelongsto is redshiftedenoughthatitsLyaemissiondistinguishable gesting thepresenceofdustoranextinctionlawforNGC5135 spectrum isnoisy,somefeatures arepresent,suchasabsorp- stars requiredcomparedwith theirlifetimesindicatesintense signatures ofmassivestars,indicatingthatMrk66isexperienc- short wavelengths,andtheCrvabsorptionfinearetypical from thegeocoronalfine.ThestrongUVcontinuum,risingto different fromthatofourGalaxy(Thuan1984). star formationactivity(Meabum 1983).AlthoughtheUV [ 1968L])isaTypeIIsupernova.Theassociationofthe II NGC 5236(M83);SBc,starburst.—M83isanearby,bright NGC 5194(M51);Sbc,LINER.—TheWhirlpoolNebula ESO 383-44;SAd,starburst.—ESO383-44isanSdspiral Mrk 66;BCG.—Thisbluecompact,low-metalficitygalaxy 33 1993ApJS ... 86 ....5K 1 8 7 Tarenghi 1980).Thesmallcontributionfromsupernovarem- fines intheUVwhicharetypicaloftheseregions(Perola& with thecompaniongalaxyNGC5236(Moorwood&Glass group (Sandage&Brucato1979).Thegalaxyisundergoing nants intheradioandX-ray,lowratioofredgiantsto the merging. tween theothertwo.Mazzarellaetal.(1988)hastentatively ment withthenonthermalactivityofnucleiandwide- Riestra, Rego,&Zamorano1987)andbyhotstarabsorption H nregions,asshownbyaverybluecontinuum(Gonzalez- violent starformation,whichmaybecausedbyinteraction classified asanamorphousgalaxybelongingtotheNGC5128 explained thisphenomenonassynchrotronemissiondueto two coincidewiththenuclei,whilethirdoneisbe- spread intensestarformationacrossthestructure. emission [log(Lfjr/Lq)11.37;Soiferetal.1987],inagree- wavelength spectrum.Theratiosbetweentheemissionfinesin been studiedbyKollatschny&Fricke(1984).Emissionfines axy hasalargeangularsize( —30')andisthemostluminous as aLINERandnucleusbSeyfert2galaxy. each ofthetwonucleihaveledtoclassificationnucleusa length spectrum,whileMgncanberecognizedinthelong- be theresultofamerger.BothnucleiareincludedinIUE member ofarichgroup.NGC 5457istidallyinteractingwith ( At;~50kms“;Hutchings & Neff1987).Thetwonucleiare galaxy [log(L^r/L©)=11.77;Sandersetal.1988].The na- of Lya,Civ,andm]canbeidentifiedintheshort-wave- aperture, andtheircontributionshavebeenaddedinthefinal tains twocompactnucleiseparatedbyabout4kpc,thoughtto tion, andSimemission.TheunredshiftedabsorptionUnes tion ofredshiftedCivX1550,thesignatureahotstarpopula- separated by3kpcandareboth includedintheIUEslit. small differenceintherecessionvelocityoftwonuclei ture ofMrk463Wisambiguous;itcouldbeeitheraSeyfert 2 is alsoconfirmedbythestrongfar-infraredluminosityof the that Mrk463Eisprobablyadust-obscuredSeyfert1nucleus. spectrum. Theshort-wavelengthspectrumofNGC5256has probably comefromourGalaxy. may beenhancedbythemergingprocess(Mazzarellaet al. nucleus orapowerfulstarburst. The presenceofalargeamountdustsurroundingMrk463E rich 1990),andstudiesofitsfeaturelesscontinuuminUV + ( Mazzarellaetal.1991)andinpolarizedfightMiller&Good- NGC 5253showscomplexabsorption,eveninLya,andemis- bursts mustbemucholderthan10yr(Moorwood&Glass optical andofitshydrogenfines(Kinneyetal.1991a),suggest of thisdoublenucleusgalaxyintheoptical,near-IR,andradio sion finesofWolf-Rayetstars(Nerv]X1486andHenX1640). of thepresentnuclearburst10yrandrequirethatprevious supergiants asrevealedintheIR,giveanupperlimittoage 1982). Thenucleusisdominatedbyemissionfromcomplex 1991 ),asmanifestedbythetidaltailsandexistence of a 1982). Theveryhighsignal-to-noiseratioUVspectrumof 34 Most oftheradioemissionisconcentratedinthreespots: The galaxyischaracterizedbyarelativelyhighfar-infrared The extendedradioemissionandthefar-infraredluminosity NGC 5253(Haro10);ImAm,starburst.—NGCis NGC 5457(M101);Sc,Hn.—This face-onnearbyScgal- NGC 5256;Seyfert2+LINER.—Thispeculiargalaxycon- UGC 8850(Mrk463);Seyfert2.—Extensiveobservations © American Astronomical Society • Provided by theNASA Astrophysics Data System KINNEY ETAL. which spreadfromitsnucleustothespiralarms,andof ject seemstohavesometraitsofaSeyfert1galaxy,suchas tion features,indicatingstarformationactivityandamixed trum showsaslowlyrisingbluecontinuumwithdeepabsorp- gions andOBassociations(Trinchieri,Fabbiano,&Romaine be individualmassivebinarysystemsassociatedwithHnre- tons agreeswellwiththenumberofphotonsavailabletoionize the continuum(DeRobertis1987;Kinneyetal.1991a).A tion opticalemissionfines.Thesecharacteristicsaresuggestive through B(Crv,SiandthefinesforX<1350Â)tomid-A in theformofOBcomplexes(Hill,Bohlin,&Stecher1984), Johnson 1980).ThemoststrikingX-rayfeaturesforthisgal- tending betweenthetwo.Thenumberofrecombinationpho- the ratiobetweenIR(80¿¿m)emissionand2?-bandflux Phillips etal.(1983).Itisalsoastrongnuclearradioemitter and thusithasbeenclassifiedasaSeyfert2-fikegalaxyby ever, itsluminosityislowerthanthatofa“classical”Seyfert2, face-on barredspiral(Morrisetal.1985)showshigh-excita- (features forX>1750Á). not particularlystrongemission.Thedisksourcesarelikelyto the Hidistributioninitsouterregions(Davies,Davidson,& companion objectlies50"fromMrk477,withtidaltailsex- example ofaSeyfert2galaxythathasdisplayedvariabilityin as Crv,in],[Nerv]X2424,and,marginally,Mgn. emission finestypicalofSeyfertactivityareclearlyvisible,such Olzewski 1985).TheUVspectrumisnoisywithverylowsig- and an“extremeinfrared”galaxy,thatis,agalaxyforwhich of thenonthermalnuclearactivityinSeyfert2galaxies.How- stellar populationfromtypeO(CrvandSiabsorptionfines) sources arefound,whilethenucleusshowsonlyextendedand axy areinthedisk,whereseveralbrightanddistinctpointfike NGC 5474,5477,andHoIV,resultinginadistortionof nal-to-noise ratiointheshort-wavelengthregion,butafew (per logarithmicfrequencyinterval)isupto250(Antonucci& tios indicateionizationbythehotstarscontainedin ring that theionizationmechanismmaybeacomposite,sincethere this barredspiralasaSeyfert2galaxy,butwithemission fine F[o m]xsooi/Fßratio.TheUVcontinuumisflatwithprominent is alow-ionizationgasringaroundthenucleuswhosefine ra- many Seyfert2galaxies,NGC5728containsacentralradio intensities lowerthanthoseofclassicalSeyfert2galaxies.Like the spectrumofatypicalSb galaxy. NGC 5728nearertoLINERs thantoSeyfert2galaxies,with absorption featuresdoesnot allow anyconclusionsaboutthe (Schommer etal.1988;Pogge1989). source (Wright1974).AsinNGC5135,thereisasuggestion emission finestypicalofaSeyfert2galaxy. fert 2galaxy,suchasalackofbroademissionfinesandhigh uum, whileatthesametimeshowingcharacteristicsofaSey- continuum variabilityandadirectviewtotheionizingcontin- the gas(Kinneyetal.1991a),indicatingthationizing star-forming component.The shapeofthecontinuumplaces source isnotblockedfromdirectview.Remarkably,thisob- 1264 havebeenidentified(Hodgeetal.1990).TheIUEspec- 1990 ).M101isdominatedintheUVbyextremePopulationI In thelowsignal-to-noiseratioIUEspectrum,lack of Mrk 477;Comp,Seyfert2.—Mrk477(IZw92)isarare NGC 5643;SBc,Seyfert2.—Thenucleusofthisalmost NGC 5728;SBb,Seyfert2.—Phillipsetal.(1983)classified UGC 9560(IIZw70,Mrk 829);IrrPec,BCDG.—The Vol. 86 1993ApJS ... 86 ....5K 1 burst ofstarformationcoupledwithasmallextinctioncannot be distinguishedfromweakstarformationwithhighextinc- (Belfort, Mochkovitch,&Dennefeld1987).However,alarge present whichcanbeattributedtothegalaxybecauseoftheir ing contributionsfromOtomid-Astars),isevidenceofstrong gest acurrenthighlevelofstar-formingactivityinNGC6217. tion onthebasisofL/alone.Otherdiagnostictoolssug- has strongandextendedIRemission,withlog(L^/Lß)^1.4 redshift. the maincontributorstoemittedfight,arecomposedof than observed,thegalaxyislikely tobesurroundedbyasub- Lya absorptionequivalentwidths shouldbemuchsmaller ing strongLyaabsorptionaswellPCygnifinesofC rv. trum ofMrk499showscomplexabsorptionfeatures,includ- emission andthepresenceofdeepabsorptionfeatures(show- concentrated inafew“condensations”andprobablyisther- unresolved nuclearsourceandextendedemission(Vilaet al. stars ofspectraltypefromOtoAO.Absorptionfeaturesare The UVslope(FocX“),indicatesthattheclumps,whichare Casini, &Heidmann1979;seealsoBenvenutietal.1982a). two strongestclumps,”andafewminorknots(Benvenuti, stantial cloudofneutralhydrogen. Hartmann etal.(1988)surmise that,sincetheexpectedstellar nearly stellarcorewithlittlevisiblenebulosity.TheUVspec- star formationactivity. of itsUVspectrumtothatNGC7714,withastrong UV mal (Hummel,vanderHulst,&Dickey1984).Thesimilarity VLA radioobservationshaveshownthepresenceofbothan aperture includes“thecentralclump,abouthalfofthenext in thecenterofgalaxy(Alloin&Duflot1979).TheIUE have producedtheobservedburstsofstarformationinclumps probable resultofthecollisiontwogalaxies,whichmight interaction withthecompanionNGC5994(Bushouse1987). Willner 1987).Thisactivityispossiblytriggeredbythestrong NGC 7714.HerealsoSirvandCshowPCygniprofiles,a confirms thepresenceofvigorousstarformation(Deutsch& signature ofWolf-Rayetstars.Ahighfar-infraredluminosity basis ofopticaldata)issimilartotheoneprototype toward shorterwavelengths,absorptionlinesfromhigh-ioni- to thoseseeninM82(Skillman&Klein1988).Thehighsig- of thisstarburst(classifiedassuchbyBalzano1983onthe Rosa etal.1984). zation species,andthenebularemissionlineCm]XI909(cf. characteristics ofHnregionemission,withafluxthatisrising probably duetoasuperpositionofsupernovaremnantssimilar is thecombinationofathermalandnonthermalcomponent, in theradio(Altschuler&Pantoja1984).Theemission both intheIR(Cutri&McAlary1985;Youngetal.1989)and the existenceofarelationbetweengravitationalinteraction nal-to-noise ratioUVspectruminouratlasshowstheusual and abnormalactivity,thisgalaxyshowsenhancedemission 1990). Theextendedradioemissionhasacomplexstructure (Cutri &McAlary1985).Inagreementwiththehypothesisof cause ofthedistortioninspiralstructuretwogalaxies interaction betweenUGC9560and9562isprobablythe mB x No. 1,1993 Mrk 499;BCG.—Thisfaint,bluecompactgalaxyshows a NGC 6217;SBbc,starburst.—Thisopticallynormalgalaxy Tol 1924-416;BCG.—Thecentral regionofthisBCDGis NGC 6052(Mrk297);Clhr,starburst.—NGCisthe NGC 5996(Mrk691);SBb,starburst.—TheUVspectrum © American Astronomical Society • Provided by theNASA Astrophysics Data System UV SPECTRAOFSTAR-FORMINGGALAXIES 4 1 7 6 the dualnatureofnucleusinopticalandIRstudies.NGC both broadabsorptionfinesandbluecontinuumshowingthe emission fine.Shields&Fifippenko(1990)haveconfirmed presence ofmassivestarsandstarformation,theLya tion, butthiscannotexplainthediscrepancybetweenvalue gas-to-dust ratiosimplyreflectsthelackofanevolvedpopula- and avigorousstar-formingHnregion. 7130 issimilartoNGC5135inhavingbothSeyfert2activity they obtainandthatofthedampedLyasystems. the effectivespectraltypeofOBassociationionizinggas nucleus ofthisgalaxyasseenintheIUEUVspectrum,with core (Norrisetal.1990).Bothcharacteristicsarerelatedtothe extremely luminousfar-infraredsourcewithacompactradio (Fall etal.1989).Gondhalekarsuggestthatthehigh tional considerationscanbefoundintheirpaper,suchasthat low Galacticlatitude.TheinternalreddeningisindeedE{B- Seyfert activity.Thuan(1984)discussesthedualnatureof magnitude largerthaninhigh-redshiftdampedLyasystems magnitude higherthaninlargegalaxiesandaboutoneorderof ( 1986)tobeoforder6X10,whichistwothreeorders ratio ofTol1924-416isestimatedbyGondhalekaretal. is 04.Thisgalaxyhasalowheliumcontent.Thegas-to-dust zero redshiftislikelyduetoourGalaxy,consistentwiththe is unusualforastarburstinggalaxy.TheMgnabsorptionat emission ofCm]X1909.ThepresenceMgnX2800 galaxy withthecontinuumrisingtowardshortwavelengths.It (1980) havestudiedtheIUEspectraofgalaxy,andaddi- an absorptionfeaturearound1305Â(Sin+Oi)andnebular is alsorichinfeatures:duetotherelativelyhighredshift,Lya burst regionplusextendedsystemsofphotoionizedgas(Berg- irregular andknotty,unusuallyluminousforitstype.Tol vall 1985).TheUVspectrumisthatofatypicalstarburst type stars)andSeyfert2activity(Véronetal.1981).Itis also bright nucleuswithanintenseUVcontinuumandfairly both anHnregion(thebluecolorisalsoduepartlytoearly- X1216 isvisible;CrvX1550hasaPCygniprofile;andthere continuum anddeepabsorptionfines,thesignatureof hot Lq ),withacompactradiocore(Norrisetal.1990).Inthe UV an extremelyluminousfar-infraredgalaxy(L^r^7.8X 10 longs totheGrusCluster(Aaronsonetal.1981).Ithasavery features ofearly-typestars,presumably fromaburstofrecent ponents oftheGrusquartet. The centershowstheabsorption spectrum theHnregioncomponentdominates,witharising strong opticalemissionfines.Thenucleusofthegalaxyhosts younger than5X10yrand withsolarmetalficity.TheUV stars. NoemissionfinesarepresentintheUV. here. Milky Way.Inaddition,theIUEcameraartifactsareevident absorption featuresduetothegalaxyitselffromthoseof has activestarformation.However,itisdifficulttodistinguish acting doublesystem(Markaryanetal.1985).Thepresenceof synthesis byBica(1988)indicates apopulationcomponent star formation(Alloin&Kunth 1979).Spectralpopulation absorption finestypicalofhotstarssuggeststhatNGC7250 V) <0.04mag(lye,Ulrich,&Peimbert1987).Carswelletal. 1924-416 harborsanextremelyblue~7X10yroldstar- NGC 7130;Sapec,Seyfert2+starburst.—NGC7130isan NGC 7552;SBbc,starburst.—NGC7552isoneofthecom- NGC 7496;SBc,Seyfert2+Hn.—Thisbarredspiralbe- NGC 7250;S/I,starburst.—Thisgalaxyappearsasainter- 35 1993ApJS ... 86 ....5K +a3 -1 three orfourcyclesofstarformation(Dottori&Pastoriza dest” ofthestarbursts,withFocX.Thecomplexoptical galaxy hasarichabsorptionspectrum,therelativelyhighred- which fallintheIUEaperture(Benvenutietal.1982a).This tion. than B8.Also,thespectrumincreasesslowlytowardshorter the clumps.Thefeatureat1670-1690AmaybeablendofAln irregular galaxywithmanyregionsofstarformation,four spectrum ofNGC7552hasbeenattributedtothepresence star population.TheUVslopeofthisgalaxyisonethe“red- Fe n,andm—thelattertwoarebothsignsofadominantA absorption featuresbetween1850and2000ÂofAln,A1m, young stars,isrisingtowardlongerwavelengthsandalsohas quence stars(Leitherer&Lamers1991).Theburstofstar presence ofanevolvedpopulationmassivepost-main-se- blueshifted by1000and500kms,respectively,manifestthe the prototypestarburstgalaxy(Weedmanetal.1981).TheP later thanB,althoughtheOBstarsdominate.Benvenutietal. wavelengths, showinganonnegligiblecontributionfromstars and Fen,indicatingthepresenceofastellarpopulationlater intrinsic, showingthepresenceofanearly(OB)populationin rest wavelengthisduetoourGalaxy,butallotherfeaturesare shift allowingeasyidentification.TheCrvXI550absorptionat spectrum, inadditiontohavingmanyabsorptionlinesfrom formation isthoughttobecausedbyinteractionwiththecom- Cygni profilesofSirvandCrv,whoseabsorptionwingsare of 30Doradus,indicatinganenormousburststarforma- find thattheUVluminosityofeachclumpis~100times .1982b,AdvancesinUltraviolet Astronomy:FourYearsofIUE .1982a,MNRAS,198,825 Arsenault, R.,Boulesteix,J.,Geoigelin,Y.,&Roy,J.-R.1988,A&A, 200, Arp, H.,&Sandage,A.1985,AJ,90,1163 .1990,ApJ,364,471 Bergvall, N.1985,A&A,146,269 Benvenuti, P.,Casini,C,&Heidmann, J.1979,Nature,282,272 Belfort, P.,Mochkovitch,R.,&Dennefeld,M.1987,A&A,176,1 Beckman, J.,Ceper,Pueto,M.,&MunozTanon,C.1987,Rev.Mexi- Barbon, R.,Capaccioli,M.,&Longo,G.1984,Mem.Soc.Astron. 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ApJ, 248,105 Zwicky) Galaxies andofPost-eruptiveGalaxies,ed.L.Speich(Guemügen:F. IUE UltravioletSpectralAtlas(NASANewsletterNo.43) Univ. Press) ApJ, 299,443 220, 453 D. C.,&Wamsteker,W.1990,ApJ,351,412 Blades, D.A.Tumshek,&C.Norman(Cambridge:Cambridge Schiffer, F.H.,Burstein,D.,Fanelli,M.N.,&O’Connell,R.W.1991, 1993ApJS ... 86 ....5K -2-1 background FN,1

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