198 7ApJS. . .65. .45 9T 51 -1 line breadthsandfromthePCygni-typeprofilesintheir W-R atmospheres.Similarly,high-resolutionopticalwork can wavelength regimes,includingtherecentatlasofultraviolet reaches theW-Rstage,littlehydrogenisleft(seeAbbottand carbon, helium,andoxygen(WCWOstars),aswell be foundintheSmithandKuhi(1981)atlas,whichdiscusses high resolutionitisappropriateforstudiesoflinetransfer in from thelessercontributionsofotherions.Theseelementsare and excitationlevelsofnitrogenhelium(WNstars),or strong, broademissionlinesarisingfromvariousionization (UV) spectrapresentedbyWilhsetal.(1986).Becauseof its effective temperatures,bolometricluminosities,andmasses spectra. Thestellarwindterminalvelocitiesrangefrom~1000 stars aresomeofthestrongestknown,asevidencedfrom Conti 1987forarecentreview).ThestellarwindsofW-R all theproductsofnuclearburning;bytimeamassivestar and spectrophotometricstudieshavebeendoneinvarious 1987). Duringthelastfiveyearsanumberofspectroscopic are notoriouslyhardtodeterminedirectly(AbbottandConti 10“ Myr“(Abbottetal.1986). National OpticalAstronomyObservatories, whichisoperatedbyAsso- tion gleanedfromtheirspectralcharacteristics,since to 5000kms,andtheirmass-lossratesareoftheorder National ScienceFoundation. ciated UniversitiesforResearchin Astronomy,Inc.,undercontracttothe © 1987.TheAmericanAstronomicalSociety.Allrightsreserved.PrintedinU.S.A. The AstrophysicalJournalSupplementSeries,65:459-483,1987November q 2 The spectraofWolf-Rayet(W-R)starsareveryrichin Our knowledgeofW-Rstarsisbasedprimarilyoninforma- VisitingAstronomer,CerroTololo Inter-AmericanObservatory, National ResearchCouncilAssociate. identifications aregivenfortheopticallinesofWCandWOspectra,withmajorcontributionstabulated interstellar reddening.Amontageofprototypestarseachspectralclassisalsoshown.Comprehensiveline presented intheformofspectraltracings(inmagnitudeunits)arrangedbysubtype,withnocorrectionfor NASA/Goddard SpaceFlightCenter. resolution (~10À)ofalmostallWCandWOstarsintheGalaxy,LMC,SMC.Thedataare unidentified linesnoted.FluxesofindividualstarscanbeobtainedfromtheAstronomicalDataCenterat Subject headings:lineidentifications—spectrophotometrystars:Wolf-Rayet The atlascontamsahomogeneoussetofopticalspectrophotometricobservations(3300-7300A)atmoderate © American Astronomical Society • Provided by theNASA Astrophysics Data System AN ATLASOFOPTICALSPECTROPHOTOMETRYWOLF-RAYETCARBON I. INTRODUCTION NASA/Goddard SpaceFlightCenter,LaboratoryforAstronomyandSolarPhysics Kitt PeakNationalObservatory,OpticalAstronomyObservatories Received 1987February2;acceptedApril28 AND OXYGENSTARS 1 2 Ana V.Torres Philip Massey ABSTRACT AND problems: photometry ofseveralW-RstarsintheLargeMagellanic infrared spectraofsouthernGalacticW-Rstars.Inaddition, line profilesofthenitrogensequence(WN).Vreux,Denne- W-R stars.Thereforewehavedecidedtocompileahomoge- in intrinsiccolors(Massey1984)andterminalvelocities resolution (~10Á)ofWCstars,coveringallthesub- neous setofspectrophotometricobservationsatmoderate (more pronouncedinWNthanWCstars;seeConti1982), given subtype,orafewstarsofthesamesubtypes.However, optical spectroscopyofsouthernW-Rstars.Allthesestudies feld, andAndrillat(1983)havepublishedacatalogofnear- (Torres, Conti,andMassey1986),hasbeendemonstratedfor Cloud (LMÇ),andLundströmStenholm(1984)present types andalmostallknownWCWOstarsintheGalaxy the heterogeneityinlinestrengthswithinagivensubtype are complementedbytheSixthCatalogueofGalacticW-R Smith andWilhs(1983)havedoneUVvisiblespectro- and theLMC. Stars (vanderHuchtetal1981,hereaftertheCatalogue). pensable inordertoknowthechemicalcompositionand The purposeofthisatlasistohelpstudythefollowing photometry downto1100A takenwiththeInternational especially theonesinOBclustersorassociations.Spectro- observations inthisatlas(e.g., Garmany,Massey,and Conti 1984). subtype. therefore theevolutionarystatusofWCstars. Most oftheabovestudiesinvolveonlyprototypestarsa Ultraviolet Explorercanbe used asacomplementtothe 2. Heterogeneityofspectralpropertieswithinagiven 1. EvolutionofW-Rstars.Lineidentificationsareindis- 3. InterstellarextinctiontowardWCandWOstars, 198 7ApJS. . .65. .45 9T WC4. WO +Sk188 WC5. WC7. WC6. WC8. WC9. Type“ + BR28 + BR32 + BR31 +WR9 + BR22 + WR86 + WR42 + WR50 + WR30 + WR140 + WR137 + WR93 + WR27 + WR70 + WR113 b WR 102 WR 72 WR 142 BR 8 BR 7 BR 93 WR 114 WR 52 WR 33 WR 38 WR 19 BR 10 WR 143 WR 126 WR 111 WR 17 WR4 WR 144 BR 50 BR 43 © American Astronomical Society WR 23 WR 5 WR 150 BR 74 WR 15 WR 14 WR 13 WR 68 WR 57 WR 56 WR 154 WR 132 WR 39 WR 125 WR 135 WR 77 WR 60 WR 53 WR 69 WR 65 WR 81 WR 80 WR 73 WR 59 Star HD 32402 HD 32257 HD 32125 Sand 4 HD 36521 HD 36402 HD 36156 Sand 5,ST3 Sand 3,NS1 Sand 2,FD73 Sand 1,AB8 HD 115473 HD 63099 WS 16 HD 195177 HD 169010 HD 165763 HD 95435 HD 88500 HD 16523 MR 110 MS 8 LS 3 HD 37680 HD 37026 HD 17638 HDE 269888 HD 92809 HD 79573 HD 76536 ST 2 WRA 1581 NS 3 WRA 1297 BS 4 LS 8 HD 97152 HD 213049 MR 44 MS 9 MR 15 ST 5 HD 137603 HD 193793 HD 192641 MR 93 HD 157504 HD 156327 HD 119078 HD 190002 HD 94305 LS 4 MR 66 HD 136488 LSS 3164 HD 192103 HD 168206, HD 121194 HD 117297 MR 62 Other NameInstrument CV Ser WC andWOStarsIncludedintheAtlas 1RS, SIT 1RS SIT SIT SIT SIT SIT 1RS 1RS, SIT 1RS 1RS SIT SIT SIT 1RS SIT SIT 1RS SIT SIT SIT 1RS 1RS 1RS SIT SIT SIT SIT SIT SIT 1RS SIT SIT SIT 1RS 1RS 1RS SIT SIT SIT SIT SIT SIT SIT SIT SIT SIT 1RS 1RS SIT SIT SIT SIT SIT SIT SIT SIT SIT SIT SIT TABLEI Air massofredobservation-1.54 Nonphotometric Air massofredobservation=1.98 X4650 issaturatedintheblueobservation; Planetary nucleus Incorrect wavelengthscaleforredobservation X <4400Aisnonphotometric X <4400Aisnonphotometric Air massof1RSredobservation=1.56 Air mass=1.86 No blueobservation Incorrect wavelengthscaleforredobservation Blue continuumshapemaybewrong Other starinslit;blueincludesmeasurements No redobservation Incorrect wavelengthscaleforredobservation; Blue continuumshapemaybewrong No blueobservation;faintstarjustoffslit Other starinslit Red isnonphotometric Red isnonphotometric Blue isnonphotometric 1.51 1.5 Blue isnonphotometric Red isnonphotometric X4650 issaturatedintheredobservation incorrect wavelengthscaleforredobservation at airmasses=1.53 Provided bythe NASA Astrophysics Data System Comments 198 7ApJS. . .65. .45 9T -1 light losses.Theseparationbetween holecenterswas1'.Two were usuallymadeatairmasses<1.5,undertypicalseeings be 5orlowerfora14thmagnitudestar.Theobservations red regionsofthespectrum. Bothwere600linesmmand different gratingswereusedin thefirstorderforblueand magnitude star.Integrationtimesof16minuteswererequired integrations weredonewiththeprogramstarinonly one of l"-2". for fainterstars.Near3200Athesignal-to-noiseratiocould minutes andgavesignal-to-noiseratiosofabout25fora 12th be observedsimultaneously. aperture. Ifanotherstarappearedinthesameaperture(near package consistsofanITTproximity-focusedimagetube slightly offcenter.Totalintegrationtimesweretypically 8 areas usedforskymeasurements;inthesecasesthe four In someoccasionsanotherstarwaspresentinoneofthe two exposures aretakenwiththestarcenteredineastaper- ted intheeast-westdirectionsothatstarsandskycan spectrograph isreplacedbyapairofcircularaperturesorien- dual Reticonarrayof936pixelswithafiberopticwindow. with theintensifiedReticonscanner(1RS)onwhite the edge),observationsweredonewithprogram star first thestariscenteredinwestaperture,thentwo Only 820pixelsareusablebecauseofdistortionandvignet- followed byamicrochannelinverterimageintensifierand ture, andfinallythestariscenteredbackinwestaperture. ting attheedgeofimage-tubefield.Theslit spectrograph attheNo.10.9mtelescope.The1RSdetector Kitt PeakbyP.M.between1980Octoberand1983February The aperturesusedwere2"in diameter,soastoavoidany Each observationwiththe1RSconsistsoffourexposures: All WCstarsinthenorthernhemispherewereobservedat spheres. tions provideatestformodelsofextendedstellaratmo- 4. FluxdistributionofWCstars.Dereddenedobserva- © American Astronomical Society • Provided by theNASA Astrophysics Data System II. OBSERVATIONSANDREDUCTION a) NorthernHemisphereStars (Breysacher 1981).Sk188isintheSMC. by aplussign. WC9 (cont.) a b a Type WR numberfromtheCatalogue.BRcompilationofW-RstarsinLMC From Torres,Conti,andMassey1986.Starsthatshowabsorptionlinesintheirspectrumareindicated b WR 95 WR 92 WR 88 WR 119LS15 WR 104MR80 WR 103 WR 96 WR 121MR90 WR 106HDE313653, Star LSS 4265 HD 157451 MR 70 HD 164270 MR 74 Other NameInstrument MR 82 ATLAS OFWCANDWOSTARS TABLE 1—Continued 1RS 1RS 1RS, SIT SIT SIT SIT SIT SIT SIT -1 blue. WhentheapertureswereilluminatedwithaHe-Ne-Ar program stars.Thefluxesused forthesestarsarelistedby ing aHe-Ne-Arcomparisonsourceeverynight.Quartz con- lamp, theresolution(fullwidthathalf-maximum[FWHM] of in theredregiontoblockcontributionsfromsecond-order gave dispersionsof-125Ámm.Differentfilterswereused identical withtheAB79system ofOkeandGunn(1983).The each night,atairmasseschosentobracketthoseof the resolution. Thespectralcoveragefortheblueregion was Latham (1975)calibrationof Vega;thissystemisinessence Barnes andHayes(1982), arebasedontheHayesand to removelow-frequencyandpixel-to-pixelgainvariations. correction foratmospheric extinction wasdoneusingthe tinuum lampexposureswerealsotakeneverynightinorder 7200 À. approximately 3100-5900A,andfortheredregion4400- a line)wasroughly2.5pixels,whichcorrespondstoabout 9 A Spectrophotometric standardstarswereobservedthroughout 6735 ...245244 6579 161151 6562 ...142162 4650-4686 13013111701016 5875 64 5801-5812 7472116611T 5696 2622479199 5590 6.85562 5471 ...3741 5411 ...3136 5131 4649 Equivalent Widths(A)oftheStrongestLinesMeasuredfrom a X <3556Anonphotometric Air massofredobservation=1.63 No redobservation Air massofredobservation=1.59;blueand The wavelengthscalecalibrationwasdeterminedbyexpos- 1RS airmass=1.72;blueSITisnonphotometric Blue isnonphotometric Saturated. observations havedifferentfluxes (Â) 1RSSIT Comments 1RS andSITObservations WR 106114 TABLE 2 461 198 7ApJS. . .65. .45 9T especially intheultraviolet. classification purposes.Forallfigures intheatlastypicalsignal-to-noiseratioofspectrawas 25, butthefainteststarshadlowersignal-to-noise, ing to-1%. photometric conditions.Thenonphotometricdatawerein- blue andtheredspectralregions,atleastonceunder was betterthan4%duringanight,withrelativefluxesagree- percentage iswavelength-independent,althoughsomewhat vidual corrections.FormoredetailsseeMassey(1984). were usedtocomputethemagnitudecorrectionforeach defocused, theeffectonequivalentwidthsorlineintensi- observation. Alldatawerecombinedafterapplyingtheindi- For eachstar,theaverageX4515magnitudewascomputed cluded inthefollowingway.Magnitudeswerecomputedfor for allphotometricnights,andtheindividualX4515measures all observationsforaregion100Awidecenteredat4515A. standard KittPeaktable.Theagreementofthestars 462 the starchannelisscatteredintoskychannel.Sincethis The 1RSdatahaveascattered-lightproblem:roughly5%of Most ofthestarswereobservedseveraltimesinboth Fig. 1.—Thespectrumofastar representative ofeachWCsubtypeisshowntoillustratetherange ofintensityandbreadththelinesusedfor 3000 3500400045005000 55006000650070007500 © American Astronomical Society • Provided by theNASA Astrophysics Data System TORRES ANDMASSEY WAVELENGTH (A) setting thecontinuumlevel. ties isnegligiblecomparedwithotheruncertaintiessuchas giving resolutionsof10-15À(FWHMaspectrallinein have verystrongemissionlines,twoexposureswereingeneral Vidicon systemhasapoordynamicrange,andsinceWCstars necessary: onetogetgoodsignal-to-noiseratiosonthecon- saturated, andonetogetthestronglinesunsaturated. intensified target(SIT)-Vidicondetectorwasusedonthe observed byP.M.atCerroTololoInter-AmericanObserva- tinuum andweaklines,withthestrongestlinesusually Cassegrain spectrographofthe1.5mtelescope.TheSIT- tory between1981Novemberand1985February.Thesilicon Several combinationsofgratingsandfilterswereused, The majorityofthesouthernhemisphereWCstarswere b) SouthernHemisphereStars Vol. 65 198 7ApJS. . .65. .45 9T photometric observations.Whencorrectingforatmospheric metric observationsbyasmuch as12%at\<3600A.When effect istochangetheshapeofcontinuum,with the clouds aregray.Thisassumptionintroducesanerrorwhose conditions, althoughinalmostallcasesthereareatleastthree slope ofthecontinuummay bedifferentfromthatofphoto- extinction inthepresenceofclouds,itisassumedthat the gions. Notallobservationsweredoneunderphotometric (3360-4780 Á)andyellow-red(3900-7350À)spectral re- each night(StoneandBaldwin1983),thewavelength calibrations weredonebyobservingseveralstandardstars shortest wavelengthsbeingaffectedthemost.Sometimes the calibration bytakingexposuresofaHe-ArandHglamp. absolute fluxestobemeasured.Thespectrophotometric the comparisonarc).Theslitwasopenedto6"-10"allow WR 80indicateamonochromaticvmagnitude~1magfainterthanthatgivenintheCatalogue,{b)Ourobservationsof121are0.65 magfainterin the slopevariedmorethan8%, theobservationwasdiscarded. v thanpublishedintheCatalogue(seeMassey1984). No. 3,1987 Most starswereobservedfivetimesormoreintheblue Fig. 2.—SpectralenergydistributionofeachWC9starobserved.Areferencemagnitudeisgivenforstar,(a)Ourobservations WR59and © American Astronomical Society • Provided by theNASA Astrophysics Data System ATLAS OFWCANDWOSTARS have anerrorofatleast0.08magX<3600À,and 0.06 precision wasdoubtlessduetotheuseofasmalleraperture mag atX>3600À. con. Thefewstarsthatdonothavephotometricobservations that showabsorptionlines in theirspectrumareindicated the relativefluxeswas-3%.Someofpoorerphotometric of thephotometricobservations,andallobservationsthat The nonphotometricobservationswerescaledtothefluxlevel with aplussign.Wemakeno distinctionifthestarisknown than withthe1RS,butsomeisattributabletoSIT-Vidi- of agivenstar(especiallythestandardstars),wefound that gave thebestsignal-to-noiseratiowereaveraged.The un- and withinonlyabout6%forX<3600Á.Theagreement of the absolutefluxesagreewitheachothertowithinabout 5%, saturated lineswereinsertedinthefinalreduction. Table 1listsallthestarsthat areincludedintheatlas.Stars When comparingthevariousSITphotometricobservations 463 198 7ApJS. . .65. .45 9T both 1RSandSITobservations,butunfortunatelynone of WR 102donothavealargewavelengthregionincommon to We madethreecomparisons ofthefluxesWR106:B in doubt,andthe1RSdatawere takenatairmassesof-1.7. blue observationwasdoneunder nonphotometricconditions, yellow-red (YR)regionswithbothinstruments.(Remember good agreement. line canbecompared.Itsequivalentwidthis384Ameasured make ameaningfulcomparisonofthefluxes;only4650 A from the1RSdata,and360AmeasuredSIT in these weretakenundergoodconditions.Theobservations of 1RS-5 SIT(3421-4737À), B IRS-7RSIT(4046-5593À), that eachSITobservationconsistsoftwoexposures.)The SIT observations andwithmeasurementsatairmasses>1.5have the photometricaccuracyof the redobservationissomewhat a noteinthetable. to beaspectroscopicbinary.Thestarswithnonphotometric 464 Only threeWCstars(WR102,WR106,and114)have WR 106wasobservedonceintheblue(B)and c) Comparisonof1RSandSITObservations © American Astronomical Society • Provided by theNASA Astrophysics Data System TORRES ANDMASSEY WAVELENGTH (A) Fig. 2b by 10%,12%,and13%respectively,whiletherelativefluxes within 15%,whichisstillvery goodgiventhattheequivalent was stillsaturatedintheSIT data.Theequivalentwidthsof whose photometricaccuracyisindoubt.Thewavelength could havenotknownthatthe strongestlineofthespectrum coverage commontobothsetsofdatais4057-7237A. The agree by3%-4%.Thedifferenceintheabsolutefluxesisworse and R1RS-YRSIT(5541-7237Á).Theabsolutefluxesagree mass =1.56),andoneSITobservationintheYRregion observations areaccurate. The 6579Alineshowsthelargestdisagreement,anditisonly was observedathighairmassesandundernonphotometric than expected,butthisisnotafairtestgiventhatWR106 are comparedinTable2. Our measurementscoincideto 5801-5802 Álineunsaturated.Withoutthe1RSdata we absolute fluxesagreeto9%andtherelative4%. The at the7%level.Weconcludethatrelativefluxesofboth strongest linesmeasuredfromthe1RSandSITdata. skies. InTable2wecomparetheequivalentwidthsof the strongestlinesmeasured fromthe1RSandSITdata two SITexposureswerenotshortenoughtogettheC iv WR 114hasoneblueandred1RSobservation(air Vol. 65 198 7ApJS. . .65. .45 9T (1985). Wehavealsochosentogiveobservedfluxes(corrected continuum level.AllthesequantitiescanbefoundinTorres line widths,orintensitiesabovethecontinuuminorderto not tonormalizetheplots,orgiveanyequivalentwidths, avoid anyerrorsthatcanbeintroducedbypickingthe instead offluxunits,therelativestrengthsUnescanbe to outsidetheEarth’satmosphere)ratherthandereddened any givenwavelengthcanbereaddirectly.Wehavechosen readily comparedfromtheplots,andapproximatecolorsat fluxes becausetheinterstellarextinctionisnotuniformacross m, =-2.5logf-48.59.Byplottingthedatainmagnitudes the averageextinctionlawcouldgivemisleadingfluxes.Fur- calibration ofVegabyHayesandLatham(1975),thatis, No. 3,1987 the sky(e.g.,Massa,Savage,andFitzpatrick1983);thususing widths ofW-Rstarsareingeneralaccuratetoonly30% (Torres, Conti,andMassey1986). fv The fluxeswereconvertedtomagnitudeunitsusingthe 3000 35004000 4500500055006000 6500 70007500 © American Astronomical Society • Provided by theNASA Astrophysics Data System Fig. 3.—Spectralenergydistributions ofWC8stars.Indicatedarethereferencemagnitudeseachstar. III. THEATLAS ATLAS OFWCANDWOSTARS WAVELENGTH (A) belonging toagivenWCclass(Figs.2-7).Wehavenot A5696 andCivAA5801-5812inFigure1.Notealsothat WC8. The latterpointisevidencedbytherelativestrengthsofCm higher ionizationsthanlatesubtypes(WCL=WC7-WC10). A5696) and(CmA5696/0m-OvA5590).TheFWHMof C inA5696changestoaflat-toppedprofilestartingatsubtype Early subtypes(WCE=WC4-WC6)showbroaderlinesand (1968) andontheCatalogue,hasbeenrecentlymade which maymaketheirreddeningdeviateevenmorefromthe the 4650Alineisacomplementaryclassificationcriterion. quantitative byTorres,Conti,andMassey(1986).Briefly,it criterion forclassificationisbasedontheworkbySmith taking ratiosoflinestrengths:(CivAX5801-5812/Cm follows anionization/excitationsequenceanditconsistsin Galactic average. the linesthatareusedtoclassifyWCstarsindicated.The thermore, manyW-RstarsareassociatedwithHnregions, The nextpartoftheatlasconsistsmontagesstars Figure 1isaplotofonestareachsubtype.Forreference, 465 198 7ApJS. . .65. .45 9T in Figurç8.Thisisthought tobeoneofthedistinguishing characteristics betweenPopulation IandPopulationII (planetary nuclei)WCstars, as discussedbySmithandAller having muchnarrowerandweaker linesthantheotherstars here forcomparison.Itshowsclearlyinourmontage as known tobeacentralstarofplanetarynebula(Barlow and here. belonging totheWC10subclass(WR118=CRL2179)was (e.g., Doom,DeGrève,anddeLoore1986).WR72is now greatly enhancedwithrespecttotheoxygenlinesinWCstars. (for peculiar)untilBarlowandHummer(1982)proposed to classified byMasseyandConti(1983)isnotincluded binary systems.Ingeneral,thesecanbeeasilydistinguishedin It isbelievedthattheyaremoreevolvedthanWCstars Galaxy wereoriginallyclassifiedintheCatalogueasWCpec Hummer 1982;vanderHuchtetal1985),butitisincluded treat themasaseparatetypebecausetheiroxygenlines are separated thosestarswith“+abs”classification,orin the figuresbecausetheyshowweakerlines.Theonlystar The WOstarsareshowninFigure8.onesthe 3000 35004000450050005500600065007000 7500 © American Astronomical Society • Provided by theNASA Astrophysics Data System Fig. 4.—SpectralenergydistributionofeachWC7star,withitsreferencemagnitudeindicated WAVELENGTH (A) high enoughtoseparateall the blends,sowehavelookedat lines thatbelongtothesameatomicseriesor be resolved;theycanonlyinferredbylookingatall the multiplet. Theresolutionof thespectrainthisatlasisnot many instancesthecontributionsfromindividualionscannot tions of1and2Aintheblue andredregions,respectively. tracings ofspectrogramstaken byDr.P.S.Contiatresolu- planetary nucleusandaW-Rstar. (1971), whogiveathoroughcomparisonofthespectra Breysacher 1979),sevenofwhichareWNsandtheotherone we feltitwasimportanttoincludeintheatlas. incorrect, butsinceitistheonlystarofitstypeinSMC, 1985) showninFigure8.Thewavelengthscalecalibration of the redobservationsofthisstar(Sk188=Sand1AB 8) is the W04+04Vstar(Moffat,Breysacher,andSeggewiss Most ofthelinesinWCstarsarebroadandblended.In The SMCcontainsonlyeightW-Rstars(Azzopardiand IV. LINEIDENTIFICATIONS 198 7ApJS. . .65. .45 9T well asseveralionsthatarenotpresent(orseen) in (1971), whoidentifiedalltheopticallinesinWC9 star (1945, 1965,1970)andonthepaperbySmithAller narrowest linesandthelargestrangeofionizationstages, as Massey (1986). for adescriptionofthoseobservationsseeTorres,Conti,and is thepaperbyEdlén(1956),whowasfirsttorecognize early types. HD 164270(WR103).TheWC9andWC8subtypesshow the Spectrograms areavailableforalmostallstarsinthisatlas; (Vreux, Dennefeld,andAndrillat1983)ultravioletfines quantum levelsinCiv.Wehavealsolookedattheinfrared successfully thehydrogenictransitionsarisingfrom high fines areshowninFigures9-14 fortheprototypestarofeach (Willis etal1986)tomakesurethatourfineidentifications It shouldbenoticedthatseveral finesstillremainuniden- are compatiblewiththefines presentinotherspectralregions. tified, themostprominentone beingnear5910A. No. 3,1987 The lineidentificationsarebasedonthetablesbyMoore Another importantsourceforidentifyinglinesinWCstars The positionsofthelaboratory wavelengthsofcontributing © American Astronomical Society • Provided by theNASA Astrophysics Data System Fig. 5.—SpectralenergydistributionofeachWC6star.BR22isanLMC ATLAS OFWCANDWOSTARS WAVELENGTH (A) All finesgiveninthelattertableareseenonlyspectra Table 3coversthecarbonfines,4isforhelium,5 which givetheidentificationsoffinesgroupedbyelement: intensity ofthestrongestfine inthemultipletisgivenhere. lengths weightedbytheirintensity).Ifvariouswavelengths of of WC9andWC8stars.CnHeiareseenonlyin the (1945, 1965,1970),exceptwhen otherwisespecified.Onlythe effective wavelengthisgiven(i.e.,theaverageofwave- The wavelengthsarisingfromhighlevelsofCivare spectrum ofWCLstars,whileOvisnotseeninWC9’s.This for oxygen(excludingOn),andTable6siliconn. subtype. ThefiguresmustbeusedinparallelwithTables3-6, Intensities areinparentheses iftheyarefromonlyonesource Usually, ifthemultipletconsistsoftwoormorefines, the Edlén (1956);allothersarefromMoore(1945,1965,1970). should bekeptinmindbecauseitisnotspecificallystated in the samemultipletaregiven,theyconnectedbyabrace. the tables. A generaldescriptionofTables3-6isgivenbelow. 2. 7istheestimatedlaboratory intensityfromMoore 1. Columnsheaded\givethelaboratorywavelength. lab lab 467 198 7ApJS. . .65. .45 9T weak; ifvwisfollowedbya subtype,itisgenerallyabsentin line, whichisseenasPCygnithroughWC5stars;vw= very WC8 andWC9stars,mostlyinWC9’sexceptforthe4650 Â line isabsentinasubtype,italsoallearlier h =hazy;HveryLshadedtolongerwavelength; in thespectrum.Symbols(Moore1945)denotefollowing: (i.e., majorcontributor);m=masked;npnotpresent; if a consisting ofablendnlinesspanningwavelengthrange m =masked;ndiffuse(withoutstructure)orhazy;ppart or iftheyareonaverydifferentscalefromthemajorityused all earliersubtypes;w=weak; x=weakertransitionsofthe subtypes; PCygni=typeofprofile,seenonly in of band;s=shadedtoshorterwavelength;wwide(fine- structure type),broad,orcomplex;W=verywide(fine-struc- 1970). ture type)orverybroad. > 8A;thewavelengthrangeisalsogiven;d=dominant line 468 4. KeytotheNotescolumn:b=blended;bntransition 3. Misthemultipletnumber,fromMoore(1945,1965, 3000 35004000450050005500600065007000 7500 © American Astronomical Society • Provided by theNASA Astrophysics Data System Fig. 6.—SpectralenergydistributionsofWC5stars TORRES ANDMASSEY WAVELENGTH (A) properties ofWolf-Rayetstars,wehavecompiledanalmost complete sampleofWCand WOstarsintheGalaxyand LMC. well asafistingoftheunidentifiedfinesthatweseein WO outside theregionstudiedbyaforementionedauthors, as not seenorpresentinthestellarspectrum. stars. (1980) intheregion3860-6100À.Theseidentifications are shown inFigure8andlistedTable7.Alsoincluded the § III)havebeenidentifiedbyBarlow,Blades,andHummer same multipletarenotincludedinourtablesbecausethey table andthefigureareothertransitionsseeninourspectra 72 (previouslybelievedtobeaPopulationIW-Rstar;see With theaimofimprovingourunderstandingbasic The spectrallinesintheplanetarynebulacentralstarWR V. SUMMARY 198 7ApJS. . .65. .45 9T 16 15 14 15 15 11 12 13 14 12 16 14 3000 35004000450050005500 © American Astronomical Society • Provided by theNASA Astrophysics Data System Fig. 7.—SpectralenergydistributionofWC4stars.Referencemagnitudesaregiven.StarswithBRnumbersintheLMC. _L WAVELENGTH (A) J. 6000 6500 _L 7000 7500 198 7ApJS. . .65. .45 9T planetary nebulaandisshownhereforcomparison.NoticethatitslinestrengthsbreadthsaremuchsmallerthanthoseofPopulation IWOstars. spectra areshown.ThesubtypesfromBarlowandHummer(1982)Moffat,Breysacher,Seggewiss(1985).WR72isthe centralstarofa Fig. 8.—SpectralenergydistributionofWOstarsintheGalaxy,LMC,andSMC(Sk188).Thecontributinglinesobserved theiroptical © American Astronomical Society • Provided by theNASA Astrophysics Data System WAVELENGTH (A) 470 198 7ApJS. . .65. .45 9T E 3000 35004000450050005500600065007000 I i © American Astronomical Society • Provided by theNASA Astrophysics Data System Fig. 9.—ContributinglinesintheopticalspectrumofWC9stars.ShownhereisWR103. i 1r WAVELENGTH (A) 471 7500 198 7ApJS. . .65. .45 9T Fig. 10.—LinesseenintheopticalspectrumofWC8stars.ShownhereisWR53,although135consideredasprototype star. 10 11 12 9 _ 3000 35004000450050005500600065007000 7500 - on Silll—IV © American Astronomical Society • Provided by theNASA Astrophysics Data System CIV cu cm out WAVELENGTH (A) 472 Il II 198 7ApJS. . .65. .45 9T E 10 11 7 8 9 3000 35004000450050005500600065007000 7500 © American Astronomical Society • Provided by theNASA Astrophysics Data System Fig. 11.—ContributinglinesinthespectrumofWC7stars.ThestarfigureisWR57. WAVELENGTH (A) 473 198 7ApJS. . .65. .45 9T © American Astronomical Society • Provided by theNASA Astrophysics Data System Fig. 12.—ContributinglinesinthespectrumofWC6stars.ShownhereisWR13. WAVELENGTH (A) 474 198 7ApJS. . .65. .45 9T 3000 35004000450050005500600065007000 7500 © American Astronomical Society • Provided by theNASA Astrophysics Data System Fig. 13.—OpticallinesseeninWC5stars.ShownhereisWR111. WAVELENGTH (A) 475 198 7ApJS. . .65. .45 9T © American Astronomical Society • Provided by theNASA Astrophysics Data System Fig. 14.—LinescontributingtothespectrumofWC4stars.ThestarinfigureisBR8. WAVELENGTH (A) 476 198 7ApJS. . .65. .45 9T 4 4, 2,4 2 ,4,4 ,44 ,2 4017.3 5 4075.4 12L364f'F-3d'D° 4021.2 3 4009.9 7 4409.7 5 4319.9 4289.0 3h 4267.1 20 3975.4 8374f'D-3d° 3972.6 7h384f'D-3d° 3919.0 18 4619.4 8h504f'G-3d'F° 4411.5 7 4373.0 9 4370.5 6 4293.7 4h 3947.9 9324fF-3d° 3877.5 12334fG-3d'F° 3833.9 8hL133pD-4pP° 3588.3 9 3361.3 8 ^lab (A) © American Astronomical Society • Provided by theNASA Astrophysics Data System ,22 ,4 ,42 ,4 42 4 ,24 ,4 2 2 2 2 42 4fD-3d'° 23 4sP°-3pD 41 4fD-3d'° 27 4sP°-3pS 40 4f'F-3d'D° 45 4/'D-3d'P° 46 4fD-3d'P° 28 4sP°-3p C ii M 39 4f'F-3d'D° 4 4sS-3pP° 6 4fF°-3dD 7 5pP°-3dD Transition ,33 3;,, l 3 s/ ,3 3 l1 4739.7 2 4661.8 8 4730.2 1 JS ÏT)“ 4247.3 4069.1 4724.3 Ip 4358.9 2WH495gH°-4f'G 4315.4 3wh485/'/-4¿/D° 4256.9 4186.9 9h 4173.1 2 4158.5 4121.8 5L 4056.1 4649.6 14 4383.4 4 4325.6 8 3887.0 6 3703.7 4hs123p'P-3d'° 3609.3 6105dD-4pP° 4593.7 1WH/• 4587.6 0WH|5gF°-4f'D 4516.1 6L95sS-4pP° 4443.1 2?23.014dD-3d'P° 51 (A) Carbon LinesObservedintheOpticalSpectrumofWCStars 3, 3 l 3 l l 3 f3 C in 3 20.01 3pP°-3pD 21 24 15.01 5dD-4fF° 18.01 4dD-4fF° 16 15 5fF°-4dD 11 5pP°-3p' 18 5gG-4fF° 17 M Transition 14 5pP°-4dD 5 3pP-3s'° 1 3pP°-3sS l 3 l 3 3P'D-3s'P° 5fF°-3p'D 5dD-4pP° 5gG-4fF° TABLE 3 477 4685.4 1W 4680.8 ... 4688.9 ... 4658.3 9W8 4646.8 mCin6 4229.2 3934.5 3929.4 3689.6 4441.0 3L 4429.5 4338.3 3720.1 3566.9 3450.5 4541.3 3359.7 ^•lab (A) 2W Civ 8.02 8.03 M 2 2 2 2 2 2 6pP°-5sS 13-7 Transition 6fF°-5dD Iallcontributions 9/ T-6hH° 6h H°-5gGIdominateover 14-7 15-7 16-7 8/ I-6hH° 17-7 11-7 17-8 6dD-5pP° 20-8 12-7 18-8 19-8 / CinWCE \ PCygni; \ fromCiv np inWC9,WC8 m byCiv b intothe4650 w; npinWC7 vw ornpinWC9 vw ornpinWC9 b7 4313-4326À vw ornpinWC9 vw ornpinWC9 b6 4153-4164A; vw inWC8; b8 3582-3591Á vw ornpinWC8 np orminWC8 np inWC8 b withCin w inWC8;vw b8 4368-4377Â np inWC7 Resolved only vw inWC8; w inWC8;vw b6 4379-4388Á np orminWC8 w; blO3944 blO 3970-3980Á w inWCE in WC9 b6 4651-4674Á A line np inWC7; and earlier np inWC7 or npinWC7 or npinWC7 -3953 Á Notes He ii,Oii.Siii m by He I,ii m byHei\3888 m byHen On He ii,Ovi O in.HeI m byHen He ii O ii,Heii He i O iv He i,Oin He I On Si in On m byHen On On On He iw O ii He i He iw On m byHeii On Si iv,HeI, Blends with Other Ions O n;v 198 7ApJS. . .65. .45 9T 2 2 2 4, 2 4 6738.1 8 6580.2 18 6258.8 4h10.035dD-4pP° 6251.8 438.034p'P-3d'D° 6151.4 4hL16.046fF°-4dD 6789.4 10 6098.2 5910.0 6444p'S-3dP° 5890.3 1554/7P°-3dD 4741.9 5836.6 5223d'P°-3p'D 4959.9 5662.5 8 5648.1 10 5140.9 15 5123.1 5117.4 5113.3 5045.4 5640.6 12 5536.2 5 5485.9 5478.6 5256.2 5034.7 (A) 4h 4h 5 7hL 17 42 2 © American Astronomical Society • Provided by theNASA Astrophysics Data System 50.03 4/'D-3d'P° 51 12 3p'P—4pp° 16 30 C ii 25 21 14 35 34 24 15 10 M 2 / 2 4 4, 4 4 4 4 20 2 2 23 2 4 2 4/D-3d' P° 4p'D-3d' F° 3p'P-3s° 4p'P-3d'D° 3d'D°-3p'*D 6731.0 3p'S-3s'P° 4p'D-3d' ° 3/7 P-2p 3d' D°-3p'P 5/7 P°-4sS 3p'D-2pP° 3d' P°-3p' 3p'D-3s'P° 38/7 P°-3sS Transition l 3 3/ 1l l1 P 3 6205.6 6773.4 6744.4 6742.2 6727.4 6460.3 Ow386dD-5pP° 6155.5 5249.1 5244.7 6872.1 6Z62.1 6857.3 6762.2 5894.1 3203d'P°-p'D 5871.1 2203d'P°-3pD 5826.4 7223d'F°-4dD 5771.7 2hL376gG-3d'F° 5695.9 12 5272.5 5253.6 7037.3 7h 8ÏÏ S} 5305.1 2HL46lgG-5fF° 5133 (A) Carbon LinesObservedintheOpticalSpectrumofWCStars 4L 3 5 C in l 3 1 3 3 3 3 l 1l 23 5pP°-4dD ... lh-5g 32 19 3d'D°-3p' 16.02 5s^^pP° 13 3d'D°-4d M 4 3p'S-3s'P° 4 3p'S-3s'P° 4 3p'S-3s'P° 2 3dD-3pP° 6.01 4dD-3s'P° 3 3p'D-s'P° Transition TABLE 3—Continued 478 6150 6747 5946 6408 4859.0 4785.9 6559.6 5092.9 5812.0 9i 5865.5 5801.3 101 5470.8 5411.1 5017.8 5783 (A) Civ M 2 2 2 15- 20-9 6/7 P°-5dD 14-8 6s S-5pP° 18-9 19-9 13-8 10-7 16-9 12-8 17-9 3/7 P°-3sS 16-8 Transition w inWC9; b7 5133-5151À vw ornpinWC8 vw ornpinWC8 Edlén 1956 np inWC7 b8 5818-5856À; b9 5244-5260A w; CIIId;np vw inWC8; vw inWC9 b7 6148-6164À vw vw inWC9; vw ornpinWC9 vw; npinWC7; b4 4954-4965A; b8 6781-6812A vw ornpinWC9 x6851-6881 À np inWC4 np inWC7 vw inWC9;x P Cygni blO 6725-6755A w; npinWCE m byA.X5801, Flat-topped profile np inWC8;x b4 4735-4745Á 5812 in WC7 b5 5042-5049Á b3 5907- np inWC7 np inWC7 np inWC7; 5920 À in WC8 and earlier Notes Blends with Other Ions O iv m byHen O vdinWCE weak OIV He ilÀ6560 C in O v,Cii m byHen He i He i m byHen He ii He i O iv 198 7ApJS. . .65. .45 9T 7234.5 20 7120.3 12 7046.3 4 7063.7 8 7053.1 6 (A) 7 lab 3 3 3 3 4e> 4>, 7065.3 6678.1 4921.9 4713.2 (3)124S-2P° 4471.5 4437.5 4387.9 5047.7 4143.8 4120.9 5875.6 (10)113D-2P° 5015.7 4026.2 (5)185D-2P° 3888.6 3819.6 (4)226D-2P° 3732.9 3613.6 3447.6 3354.6 3705.1 3964.7 C II © American Astronomical Society • Provided by theNASA Astrophysics Data System 2 20 3d'F-3p'D 26 3¿/'/"-3/7S M 3 3dD-pP° ^lab (A) Transition (5) 10 (6) 46 (2) (6) (4) 48 (6) 14 (10) 2 (3) (3) (2) (1) 24 (2) (1) 50 (3) 51 (2) (3) (4) 5 He i 47 25 53 16 4 6 7 8 3 l1 3 l 1l l 3 l l l l 3 3 l l li 3 3 S-2P° 4 S-2P° 4 D-2P° 6 P°-2S 4 Z)-2P° 4 P°-2S 1S-2 P° 5 P°-2S 7 P°-2S 3 D-2P° 6 D-2P° 3P°-2S 1D-2 P° 3 P°-2S 5 ^-2P° 5 D-2P° 5 S-2P° 3 Transition 7211.1 2WH396dD-5pP° (A) Helium LinesObservedintheOpticalSpectrumofWCStars Carbon LinesObservedintheOpticalSpectrumofWCStars ^lah 6890.9 6683.2 6560.1 6527.1 6310.8 6233.8 6074.1 A 4859.3 4541.6 4338.7 4199.8 7177.5 6406.3 6170.6 6118.2 6036.7 4685.7 4100.0 4025.6 3858.1 3833.8 3813.5 3781.7 3203.1 5411.5 3968.4 3923.5 3887.4 3796.3 lab C in (A) M 21 2 2 Transition M 2 8G-4F 4 15(7-4F° 3 12G-4F° He ii 2 2 TABLE 3—Continued 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 UH°-5G UH°-5G 13 G-4F° 14 (7-4F° 21 (7-4F° 20 <7-4F° 16 (7-4F° 17 (7-4F° 18 G-4F° 4 F°-3D 10 (7-4F° 11 G-4F° 19 (7-4F° 9 G-4F° 21H°-5G 11H°-5G 13 H°-5G 16 H°-5G 19 H°-5G 20 H°-5G 1 G-4F° 14 H°-5C 15 H°-5G 17 H°-5G 5 F°-3D 6 G-4F° Transition TABLE 4 479 2 T70 7062.4 7207 ^•lab (A) vw ornpinWC7andWCE vw inWC7 vw ornpinWC5;WO vw ornpinWC7andWCE vw ornpinWC7andWCE np inWC7 b ormincdlsubtypes vw inallsubtypes b orminallsubtypes b orminallsubtypes b orminallsubtypes vw ornpinWC8;WC7 vw ornpinWC8;WC7 np inWC7 np inWC7 vw ornpinWC7andWCE b intoÄ.4650forWCE d vw ornpinWC8;WC7 vw ornpinWC8;WC7 vw ornpinWC7 b orminallsubtypes vw ornpinWC7 d; PCygni b orminallsubtypes np inWC7 b orminallsubtypes P Cygni P Cygni np inWC7 np inWC7 w ornpinWC7 P Cygni;vwinWC7 P Cygni Civ A/ Transition Notes 9-7 15-9 Blends with b9 7113-7114A Other Ions weak Civlines C in,Oii,Siiv C ii,On; O in,Siiv O II,IV O inX3609d C II C ii,iv He I He ii C ii C in;ivA4441d On C ii,Oii;iv C hi C in C ii,Ovi O in,Siin O in,Cin O HI C ilX6580 C in Civ Civ C iv C in He ii He i Civ Si in O hi Si hi,OVI Civ inWCE Notes Held Blends with Other Ions in WCL 198 7ApJS. . .65. .45 9T 1 l 4569.5 In363dF-3pD° 5592.4 3261.0 3695.4 3455.1 3444.1 3430.6 3312.3 3299.4 3284.6 3281.9 3267.3 3265.5 3702.8 3698.7 3450.9 3340.7 3961.6 8173dF°-3pD 3791.3 3774.0 3759.9 3757.2 3754.7 3715.1 3707.2 3703.4 7 Mab lab © American Astronomical Society • Provided by theNASA Astrophysics Data System 5 5 3 3 O in 1 3 3 3 21 3pD°-3sP 25 3dF~3pD° 14 3dD°-3pP 15 3dP°-3p M Transition 5 3pP-3sP° 3 3pS-3sP° 8 3tdF°-3pD 2 3pD-3sP° Oxygen LinesObservedintheOpticalSpectrumofWCStars 5305.3 5362.4 4813.1 4798.3 4794.2 4783.4 4779.1 4772.6 3995.2 3977.1 3413.7 3411.8 3736.8 3563.4 3560.4 3425.6 3409.8 3381.3 3729.0 3725.8 3403.6 3396.8 3385.6 10 4 2 (!) §} (2) (6) (4) (5) (4) (3) (2) (2) }33pD-sP° (2), (4) 1 (2) (2) x 2) 123dF°-3pD 2 ] 113dD°-3p O iv ¿2 M Transition 2 3D-P° 4 4 3dP°-3pP 3d F°-3pD TABLE 5 480 3 4123.9 243pD-3sP°x;Cin 5608 4925 6500.2 4940 6466.0 6460.0 5604.2 (0) 5597.8 (4) 5583.2 (1) 5580.0 (3) 5571.8 (1) 5114 3239 3222 3834.2 3811.4 3275.7 3144.7 7 'lab lab 3 " ^)103dD°-3pS O vandVI )! 1 2 M Transition 2 3D-P° 1 3P°-S l 3 3 3 3 3 P°-3SCin 3 D-P°Edlén1956 3 D-P°Edlén1956,exceptX5608 3d' F-3p'DEdlén1956;Cin 3p S-3sP° x; Civ vw; CIIIX5305d; vw P CygniinWCL x; HeH He I Sole Oviline P CygniinWCL Si hi,HeII Si iv,HeII x; On,He1 x; Civ.He1 x; HeI O v x; Cm,He1 Civ O in X5362 npinWCE Notes andBlends very stronginWOstars 198 7ApJS. . .65. .45 9T 0 4574.8 4567.8 4552.6 4829.0 4819.7 4813.3 4716.7 3796.1 3590.5 3486.9 5739.7 3924.5 208.14Sg'G^f'f 3806.5 3791.4 20 25 20 30 15 l © American Astronomical Society • Provided by theNASA Astrophysics Data System l 3 3 l Si in 4 4pP°-sS 1 4dD-4pP° 8.06 5/F°-4dD 3 9 5gG-4fF° 8.09 5fF°-4dD M Transition 5 4dD-4pP° 3 4pP°-4sS Silicon andOiiLinesObservedintheOpticalSpectrumofWC9WC8Stars 4654.3 lOhs 4631.2 9hL 4088.9 10 6701.2 4116.1 4212.4 7hL 3149.6 3773.1 3762.4 3165.7 2 I} 3.025dD-5pP° 2 Si iv M Transition 2 4dD-4pP° 2 2 2 2 6hH°-5gG 4pP°-4sS 4p P°-4sS 6fF°-5dD TABLE 6 481 4696.4 4676.2 4673.8 4661.6 4650.8 4649.1 4641.8 4638.9 4596.2 4591.0 4110.8 4105.0 4104.7 4103.0 4097.3 4075.9 4072.2 4069.9 4452.4 4417.0 4349.4 4336.9 4319.6 4317.1 4120.4 4119.2 4414.9 4366.9 4349.5 4345.6 4325.8 3982.7 3954.4 3945.0 3919.3 3973.3 3912.0 3749.5 3727.3 3712.8 10 /lab A/Transition 5 4 20 4 2 4 4 10 j 10 \ 4 ,2 4 I 6 \13pD°-3sP 6 163p'D-3s' 2 9 5 }203dD-3pP° 8 8 j53pD°-3sP 1 23pP°-3s 8j 33pS°-3sP j} 203dD-3pP° !} 153pF°-3s’DCm 4 20 10 3dF-3pD° On 6 3pP-3s° Notes andBlends O in,Heii C ii,Siin,Heii x, Cind m byHeI He i C ii He i,Cin He ii C ii C iv,Heil,Oii O in,Heii O iv,Hei C ii C ii C ii,in C ii,in He ii m byX4650 m byXÀ4650, 4686 absorption 198 7ApJS. . .65. .45 9T 2 4859.0. . 4785.9.. 4688.9.. 4685.4.. 4680.8.. 4658.3.. 4646.8.. 4441.0. . 4229.2.. 4944.7 7-6 4520.0 9-7X 7062.4.. 6747 ... 6559.6.. 6408 ... 6150 ... 6560.1. 4859.3. 4645.7. 4541.6. 4338.7. 4199.8. 4100.0. 3409.0 3D-P°Xffective(seeTable5) 7207 ... 5946 ... 5865.5.. 5812.0/ 5801.3 \ 5470.8.. 5411.1.. 5092.9.. 5017.8.. 3934.5.. 3929.4.. 5411.5. hydrogenic e previous ones;6311inWR72;thisfinecannotarisefromHenbecause othern-5transitionsofHenarenotobserved. WR 142;6207in102(?),verynoisy,probablysamefineas6197; 6223inBR93,noisy,probablysamefineasthetwo Â): 3560inWR72andBR93;364872;39263945 in BR93;4043WR72(?)and6197 signal-to-noise ratioofthespectra,followingwavelengths[inA]may beinaccurateto~10A;forWR72theaccuracyis3 Note.—Approximate wavelengths(inA)ofunidentifiedfinesinWO stars(owingtothebreadthoffinesandlow Line (A) Transition 2 2 2 2 2 2 2 6sS-5pP° 6pP°-5dD 6pP°-5sS 6dD-5pP° 6hH°-5gG © American Astronomical Society • Provided by theNASA Astrophysics Data System 3p P°-3sS 6/ F°-5dD 2 8/ T-6hH° 11-7 15-9 16-9 12-8 17-9 18-9 19-9 13-8 10-7 14- 8 15-8 16-8 17-8 12-7 13- 7 10-4 11-4 12-4 4-3 9-7 6-4 7-4 9-4 8-4 He ii O iv Civ C v Lines ObservedintheOpticalSpectrumofWOStars Notes TABLET 4555.7. 4340.5. 6084.9. 6068.2. 6064.2. 5669.7. 3887.1. 5298 .... 3936.6... 3834.2/’ 3509 .... 3435 .... 3426 .... 3487.9. 3486.5. 5289 .... 5279 .... 3811.4 \ Line (A) 3 3 32 1 3 3d'F-3p'D 1 32 3d D°-3pP 3d D°-3pS 3d D°-3pP 3rf D°-ip 2 2 2 2 1l 3d F°-3pD O vinHydrogenicWavelengths O vuHydrogenicWavelengths 2 3p D-3sP° 3 2 7 P°-6D 7 F°-6D 3 P°-S 8 F°-1D 3 P°-S %D-1F° 3 D-P° 8 G-1F° Transition 13-9 10-9 11-9 12- 1 0 11- 9 13-11 13-10 7-6 9- 8 9-8 8- 7 O vi O v see x Wavelength fromEdlén1956 ^effective (Table5) ^effective (seeTable5) hydrogenic Notes 198 7ApJS. . .65. .45 9T chemical compositionofsuchstars,and,asaconsequence,in spectral subclassesshouldbehelpfulintheanalysisof the studyoftheirevolutionarystatus. preparation byContiandMassey. dard SpaceFlightCenter.AnatlasofW-Rstarsthe (f) andmagnitudes(mjasafunctionofwavelengthis nitrogen type(WN)similartotheonepresentedhereisin available fromtheAstronomicalDataCenteratNASA/God- stars, aswelltheirfluxdistributions. the linewidths,strengths,andintrinsiccolorsofWC Azzopardi, M.,andBreysacher,J.1979,Astr.Ap.,75,120. Abbott, D.C,andConti,P.S.1987,Ann.Rev.Astr.Ap.,25,inpress. Abbott, D.C,Bieging,J.H.,Churchwell,E.,andTorres,A.V.1986,Ap. Edlén, B.1956,VistasAstr.,2,1456. Conti, P.S.1982,inIAUSymposium99,Wolf-RayetStars:Observations, Barlow, M.J.,andHummer,D.G.1982,inIAUSymposium99, Garmany, C.D.,Massey,P.,andConti,P.S.1984,Ap.J.,278,233. Barnes, J.V.,andHayes,D.S.1982,ÏRSStandardStarManual Barlow, M.J.,Blades,J.C,andHummer,D.G.1980,Ap.(Letters), Doom, C,DeGrève,J.P.,anddeLoore,C.1986,Ap.J.,303,136. Breysacher, J.1981,Astr.Ap.Suppl.,43,203. Massey, P.1984,Ap.J.,281,789. Lundström, L,andStenholm,B.1984,Astr.Ap.Suppl.,56,43. Hayes, D.S.,andLatham,W.1975,Ap.J.,197,593. Ana V.Torres:NASA/GoddardSpaceFlightCenter,MailCode680,Greenbelt,MD20771 Massey, P.,andConti,P.S.1983,Pub.A.S.P.,95,440. Massa, D.,Savage,B.andFitzpatrick,E.L.1983,Ap.J.,266,662. Mofl'at, A.F.J.,Breysacher,andSeggewiss,W.1985,Ap.292,511. Philip Massey:KittPeakNationalObservatory,P.O.Box26732,Tucson,AZ85726 Moore, C.E.1945,AMultipletTableofAstrophysicalInterest(NBSTech. x (Dordrecht: Reidel),p.3. (Tucson: KittPeakNationalObservatory). 241, L27. Loore andA.J.Willis(Dordrecht:Reidel),p.387. Physics andEvolution,ed.C.W.H.deLooreA.J.Willis The lineidentificationsthatweregivenforallWCandWO Note 36;Washington,DC:GPO). Wolf-Rayet Stars'.Observations,PhysicsandEvolution,ed.C.W.H.de The atlascanalsobeusedtoexaminetheheterogeneityof A magnetictapecontainingtheaveragedobservedfluxes 303, 239. © American Astronomical Society • Provided by theNASA Astrophysics Data System ATLAS OFWCANDWOSTARS REFERENCES generous allocationsofobservingtimeduringtheyears.P.M. with theexpertassistanceofR.VegnasandE.Hardy,we was aPostdoctoralFellowattheDominionAstrophysical .1970,SelectedTablesofAtomicSpectra,EnergyLevels couragement andsupport.TheCTIOobservationsweremade grateful toitsdirector,SidneyvandenBergh,forhisen- were madeaspartofalargercollaborativeprojectwithPeter reducing SIT-Vidicondata.SomeoftheCTIOobservations Observatory whenmuchoftheobservingtookplaceandis Moore, C.E.1965,SelectedTablesofAtomicSpectra,Energy also thankDonHayes. the adviceandencouragementofJeannetteBarnes,we thank DrewPhillipsforexcellentadviceanddiscussionof Torres, A.V.,Conti,P.S.,andMassey,1986,Ap.J.,300,379. Torres, A.V.1985,Ph.D.thesis,UniversityofColorado. Oke, J.B.,andGunn,E.1983,Ap.J.,266,713. S. Conti.The1RSobservationsatKittPeakweremadewith Smith, L.F.,andKuhi,V.1981,AnAtlasofWRLineProfiles,JILA Smith, L.F.1968,M.N.R.A.S.,138,109. van derHucht,K.A.,Conti,P.S.,Lundström,I.,andStenholm,B.1981, Stone, R.P.S.,andBaldwin,J.A.1983,M.N.R.A.S.,204,347. Smith, L.J.,andWilhs,A.J.1983,Astr.Ap.Suppl.,54,229. Smith, L.F.,andAller,H.1971,Ap.J.,164,275. Vreux, J.M.,Dennefeld,andAndrillat,Y.1983,Astr.Ap.Suppl., van derHucht,K.A.,Jurriens,T.Olnon,F.M.,Thé,P.S.,Wessehus, Willis, A.J.,vanderHucht,K.A.,Conti,P.S.,andGarmany,C.D. and MultipletTables:CI-CVI(NSRDS-NBS3,Sec.3;Washington, DC: GPO). Washington, DC:GPO). Rept. 117. Levels andMultipletTables:SiII-SiIV(NSRDS-NBS3,Sec.1; Space Sei.Rev.,28,227(Catalogue), 54, 437. P. R.,andWilliams,M.1985,Astr.Ap.,145,L13. 1986, Astr.Ap.Suppl.,63,417. We aregratefultotheKPNOandCTIOdirectorsfor 483