19 6 9ApJ. . .158.1115S 1 classical workofLuyten andDartayet(1942,1945),Luyten,Jose, Foster (1944, velocity, andproper-motion dataexist.Theearlyonsubdwarfswereobtained inthe dwarfs isincreasedandifthediscoveryprocedures arechangedtoovercomecertaintypes ing negativeV?Theseandotherquestionscanbe answeredonlyifthesampleofsub- unique, oraretherelow-velocitystarswithvery weakmetallines?(2)Arethereap- 1945), LuytenandJose(1948), Luyten,Carpenter,andDeutsch(1952),Kuiper (1939, preciable numbersofsubdwarfswithhighangular momentum (thatis,starsoflowmetal of observationalbias. exist ontheELScollapsepicture?(3)Forthesehigh-/« stars,afewofwhichareknownto abundance whichmoveindirectgalacticorbitswith large+Vvelocity)whichshould exist, doesmetalweakeningbecomemorepronounced towardtheenergyboundary abundance andspacemotion(orequivalentlythe eccentricityoftheplaneorbit)truly meager enoughthatmanyofthequestionsraisedbyRoman(1965),Eggen,Lynden-Bell, increased rapidlyinrecentyears,theobservationaldataonfieldsubdwarfsarestill increasingly positiveVvelocity,butmoresubdwarfsofthistypeareneededtoestablishthecorrelation. (E =0)onthe+VsideofBottlingerdiagram, asitdoesforlow-^starswithincreas- answered. Forexample,wewouldliketoknow:(1)Isthecorrelationbetweenmetal and Sandage(1962;theseauthorsarehereinaftercalledELS),otherscannotyetbe directed awayfromthehigh-velocityantapex. rotational velocityseemstobeestablished.Theremayasystematicvariationofmetalabundancewith tained inthekinematicsofhigh-velocitystars.Althoughknowledgesuchstarshas dance butofdifferentcolorsfortheeffectguillotine. Candidates canbefoundinproper-motioncatalogsfromamongstarswhoseanglesare spectroscopic studies. gradient perpendiculartothegalacticplane. ultraviolet excessvaluesfrom8=0.00toô0.31magTheresultsareinterpretedintermsofachemical dispersions inUandWincreasesystematicallywithdecreasingmetalabundancefortheentirerangeof is generallybetterthan±2kmsec“.Ninepossiblevelocityvariableshavebeenfound,fourofwhichare sequence stars. subluminous companionswhicharebrighterthanwhitedwarfsbutconsiderablyfaintermain- almost certaincases.Twoparticularlyinterestingvariables(G9—16,G26—9)probablyhaveblue photometric catalogwhichcontains300newsubdwarfcandidatesTheaccuracyoftheradialvelocities (C) 1969.TheUniversityofChicago.AllrightsreservedPrintedinU.S.A The AstrophysicalJournal,Vol.158,December1969 © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem Many globular-clusterlikesubgiantsarepresentinthematerial.Candidateslistedtoaidfuture Fewer than250subdwarfsareknownforwhich allnecessaryphotometry,radial- A procedureisgiventocorrectobservedultravioletexcessvaluesforstarswiththesamemetalabun- The existenceofsubdwarfspossessinghighangularmomentumwhichleadtheSuninitsgalactic Clues totheearlychemicalanddynamicalhistoryofGalaxyareundoubtedlycon- Space motionsforallstarsareshowninaBottlingerdiagram.Theasymmetrical-driftvelocityandthe Radial velocitieshavebeenmeasuredfor112starsoflargepropermotionselectedfromanunpublished Mount WilsonandPalomarObservatories,CarnegieInstitutionofWashington,California NEW SUBDWARFS.II.RADIALVELOCITIES,PHOTOMETRY, Institute ofTechnology;andMountStromloSidingSpringObservatories, AND PRELIMINARYSPACEMOTIONSFOR112STARS Research SchoolofPhysicalSciences,AustralianNationalUniversity WITH LARGEPROPERMOTION Received 1969May12 I. INTRODUCTION Allan Sandage ABSTRACT 1115 19 6 9ApJ. . .158.1115S 1 1 1 1 lished byGreenstein(private communication),whichwillbediscussedbyhim inaforth- Paper I,standardwavelengths forthestellarlineswereadoptedfromsystem estab- a lineardispersionof18Ämm“.The8-inchaplanatic-sphere camera(Bowen1952)at color class2orbluer.Aphotometriccatalogisinpreparation,andadiscussionofthe about thirty-fivestellarlinesineachspectrumrelative totheiron-arccomparison.Asin stars G9—36,G44—30,G15—23,andG25—24,as notedinTable1. depending ontheseeingandcloudcover.Allbut fourofthestarswereobservedwith plates wereobtainedfortwentystars.Theexposure timesrangedbetween1and3hours, variables requiringfurtherstudy,and{d)toshowtheBottlingerdiagramforpresent field examplesofglobular-clustersubgiantsandgiants,{c)tolistpossibleradial-velocity inch orthePalomar20-inchreflector.Thecriteriaforselectionwerem^0^27year“, coming paperonhissearch forradial-velocityvariationsinknownsubdwarfs. the 200-inch,whichgivesadispersionof39Âmm“ inthethird-orderblue,wasusedfor and twenty-twowiththe100-inch.Mostwereobserved onlyonce,buttwoormore made byELS(1970)usingtheentireavailablesubdwarfdata. velocities, {b)toliststarsofspecialinterestforfurtherspectrographicwork,suchas with mbrighterthanLowellcatalogmagnitude14(laterreducedto13)and minutes) the200-inchmirrorsystemfromprimefocustocoudémodemade results willbegivenlater. c). ThesesurveysshowthatverymanysubdwarfsfainterthanF=8remaintobedis- last ofwhich[Evans1966]givesreferencestopreviouslists[SandageandLuyten1967, stars, segregatedaccordingtoultravioletexcess,inorderillustratepossiblesolutions judged byultraviolet-excessvalueslargerthan§{U—J5)=0.15.Asthephotometry either 18or39Âmm“.Thepurposesofthepresentpaperare(a)todiscussradial scheduled forotherproblems.Thepossibilityofrapidlychanging(usuallyin15-20 out onastandbybasisatthe200-inchreflectorpartiallycloudynightsoriginally were observed(principallybyKowal)inUBVcolorswitheithertheMountWilson60- standby programpossible. S{U —B)>0.15wereplacedonacoudéradial-velocityprogramwhichwascarried became available,allstarswith0.30<2?—F1.0,brighterthan11.5,and vey ofproper-motionstarsinthefirst100fieldsLowellProperMotionSurvey covered andthatthesamplecanbeincreasedalmostatwill. other work(cf.theCapeObservatory’slistsoffundamentaldataforsouthernstars, are includedinEggen’s(1964a)high-velocitycatalog. to someofthequestionsraisedearlier.Amorecompletediscussionitem(d)willbe Adams etal,(1935).Thematerialavailableto1959hasbeensummarizedelsewhere to findnewsubdwarfs,SandageandKowalin1961beganasystematicphotoelectricsur- 100- or200-inchcoudé8-,16-,18-inchcameras,whichgivealineardispersionof the firstsubdwarfs(thencalledintermediatewhitedwarfs)byAdamsandJoy(1922) (Giclas, Burnham,andThomas1961-1967).Between19611964nearly2000stars 1969]) orbydesign[cf.Przybylski1961;Deeming1962;Sandage1964a;Eggen1968a,b> 1940a, ô,1942,1943),Roman(1954,1955a,6),andothers,promptedbythediscoveryof (Eggen andSandage1959;Eggen1959).Mostdataavailabletolate1962 1116 ALLANSANDAGE © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem The platesweremeasuredprincipallybyMaryWhiteoak andSylviaBurd,whoused Of the112starsobservedforradialvelocity,ninety wereobtainedwiththe200-inch To date,radialvelocitiesof112subdwarfcandidateshavebeenobservedwiththe To date,nearly300newsubdwarfcandidateshavebeenfoundinthissurveyas Since 1959,manynewsubdwarfshavebeenfound,eitherbyaccidentinthecourseof Encouraged bytheresultofapilotstudy(Sandage1964a,hereinaftercalledPaperI) a) RadialVelocities II. THEDATA 19 6 9ApJ. . .158.1115S 0.6 0.8 1.4 0.9 0.9 0.8 1.5 2.2 0.6 0.7 0.6 0.5 0.4 0.9 0.5 2.0 0.5 0.7 0.4 0,8 0.5 1.0 0.4 2.2 0.6 JG 0.8 0.4 0.8 0.7 0.5 0.6 0.4 0.4 0.6 0.6 0.8 0.6 0.7 0.6 0.8 0.5 1.3 0.9 0.6 0.4 0,6 0.3 0.4 0.3 0.6 0.7 1.9 0.6 0.3 0.5 0.6 0.4 (14) 1) A A 50 59* 58 57 56 55 54 53* 52* 51 50 49, 48 47* 46* 45* 44 43+ 42 41 40 39* 37 36 29* 28 27 26 24 22 21 38 35 34 33+ 32 31* 30* 19 18* 17 25* 23 20 12 13 10 16 15 14 11 5* 9 7* 6* 2* 1* 8 4* 3* © American Astronomical Society G14-32 G59-18 G13-1 G59-27 +5501362 -7°3509 G60-26 G5 8-23 Gll-36 G44-30 -21°3420 -I4O3322 G4 3-33 G9-16 +800245 G88-31 G88-2? +650737 G41-44 G90-25 G88-32 G90-3 G89-14 G114-26 G9-36 G112-36 G87-2Ö +590886 G1Q8-43 G101-33 G102-2Û G112-43 G88-40 G98-58 G1Ö2-47 G98-3 G96-20 “6°1598 G84-3? G84-29 G77-54 G37-34 G4-44 G8-51 G8-16 G5-17 G75-31 +680138 +72°94 G4-37 G76-21 G72-6Ö G71-40 G7Ö-35 G4-6 -170219 -110220 “9° 122 Name -20181 -80 128 (2) 13343 13597 13567 18140 13479 12737 12603 12503 12 848 12273 12084 12031 17969 12338 12040 12032 1182? 11665 11566 1212 8 17974 11819 11781 11645 11578 11966 11595 11473 11092 11486 11029 10934 10900 17399 10750 10615 10880 10720 10667 (3) 5030 4942 4459 4438 4228 2579 3319 2909 2698 16 39 1007 LTT 674 655 604 681 402 337 RADIAL VELOCITIESANDPHOTOMETRYFOR112STARSWITHLARGEPROPERMOTION 13 05.8 12 37.8 12 34.2 12 53.0 12 01.5 11 53.0 11 23.6 10 09.6 10 47.2 12 21.0 11 56.5 10 01.4 09 26.6 08 55.0 10 37.7 09 45.9 08 56.6 08 03.0 07 50.3 07 41.2 07 37.3 07 31.7 07 27.7 07 27.6 08 41.6 07 24.1 06 56*1 06 03*3 05 01.9 07 26*6 0? 19.8 06 59,7 06 12,6 05 37.3 05 28.6 04 38.3 06 30*2 06 15*5 05 22.2 05 07.3 04 58.6 03 25.9 03 16.5 03 07.2 02 49.3 02 35.7 04 11.6 02 41.9 02 38.5 02 11.0 02 05.6 01 43.0 01 54.7 01 50.6 01 10.9 01 07.7 01 01.9 00 41*4 01 11.7 00 36.0 a(1950} (4) +17 33 +54 35 +12 55 +27 45 + 338 +17 11 +11 27 +65 33 +24 59 - 703 -22 06 -15 26 +20 46 + 851 +24 40 +30 45 + 003 +17 01 +19 04 +38 13 - Ö24 +38 35 - 827 - 430 +80 01 +24 12 +32 58 +19 12 + 855 + 719 +12 09 +37 45 +59 07 + 3222 + 529 +40 11 + 402 +20 48 +22 14 +15 11 - 349 + 3325 +11 10 + 816 + 933 + 214 +11 43 + 3109 - 124 - 627 + 6847 + 7313 - 642 - 134 -16 42 -10 39 - 748 6 (1950) - 208 - 239 - 835 (5) Provided bytheNASA Astrophysics DataSystem 10.91 10.18 10.18: 10.45.* 11.30 11.15 11.95 10.43 10.07 10.40 10,22 10.27 10.82 10.74 10.22 10.18 10.53 10.31 10.28 11.43 10.20 10.60 10.06 9.25 9.66 9.81 9.96 8.35 9.00 7.90 9.70 9.69 8.98 9.32 9.23 9.05 8.95 9.89 9.76 9.66 9.81 8.30 9.45 9.72 9.26 9.68 8.51 8,92 9.07 8.62 8.01 9.31 8.26 9,21 8.38 7.43 9.40 9.27 9.18 8.95 (6) 0.94 0.40 0.72 0.65 0.72 0.58 0.64 0.60 0.58 0.52 0.60 0.70 0.67 0.38 0.54 0.48 0.31 0.62 0.50 0.44 0.82 0.51 0.48 0.44 0.65 0.57 0.36 0.51 0.57 0.36 0.47 0.56 0.74 0,64 0.64 0,60 0.52 0.42 0.85 0.59 0.75 1.08 0.62 0.83 0.54 0.44 0.46 0.41 0.47 0.56 0.56 0.53 0.64 0.38 0.69 0.57 0.80 0.59 0.45 0.72 ill B-V TABLE 1 -0.01 -0.14 -0.03 -0.24 -0.05 -0.11 -0.06 -0.22 -0.05 -0.20 -0.14 -0.12 -0.19 -0.19 -0.02 -0.13 -0.20 -0.16 -0.08 -0.05 -0.02 -0.22 -0.17 -0.15 -0.11 -0.02 -0.16 -0.18 -0.17 -0.12 -0.20 -0.20 -0.21 -0.07 -0.25 -0.16 -0.10 -0.10 -0.03 -0.02 -0.16 0.56 0.20 0.10 0.01 0.02 0.10 0.30 0.33 0.03 0.23 0.93 0.02 0.47 0.50 0.06 0.02 0.13 0.36 0.02 (8) m 0.16 0.18 0.20 0.24 0.21 0.16 0.19 0.16 0.23 0.09 0.18 0.22 0.17 0.12 0.22 0.23 0.22 0.30 0.11 0.20 0.17 0.17 0.15 0.19 0.11 0.17 0.15 0.09 0.21 0.15 0.17 0.23 0.24 0.16 0.19 0.19 0.16 0.24 0.23 0.05 0.20 0.07 0.01 0.13 0.25 0.18 0.00 0.14 0.22 0.18 0.08 0.23 0.16 0.27 0.12 0.11 0.11 0.07 0.10 0.16 (10) , + .218 + .107 + .130 + .260 + .060 + .150 -.256 + .300 + .180 -.194: -.175 + .711 + .104 + .031 + .352 + .259 -.212 -.162 + .186 +.124: + .059 +.174: +.304: + .038 + .145 + .250 + .309 + .360 -.100: -.002 -.030: -.102 + .008 + .166 + .441 + .430 -.280: -.114: + .045 + .348 + .178 -.415 -.019 +.310: + .220 + .355 + .267 -.124: -.054*. -.233 + .263 + ’.03 -.074 -.076 -.214 -.101 -.184 -.196 -.191 .000: (ID + .082 +.256: -.190 -.206 -.247 -.449 -.216: -.096: -.094 -.332: -.203 -.034 -.275: + .016 -.323 -.590 -.354 -.173: -.240 -.297 -.587 -.225 -.354 -.305 -.059 + .016 + .164 -.326 -.059: -.270 -.136 -1.830 -.306: -.250 -.270: -.262 -.602 -.306: -.073 -.290 -.439 -.268: -.193 -.254 -.369 -.285 -.190 -.571 -.206 -.032 -.027 -.029 -.086 -.031 -.352 -.117 -.180 -’.'560 -.116 .000: (12) +115.6 + 26.7 + 5.9(2) + 13.9 +112.6 + 73.8 + 11.4 + 60.3 +265.3 + 49.3V(3) + 32.8V? + 1.2 + 49.2 -123.1 + 92.0 + 31.6 -14.8 - 23.0 - 2.9(2) - 40.0 - 33.1 + 44.1 +144.0 +247.9 + 93.9 + 25.0 + 32.7 +109.7 +176.6 + 7.5 -15.6 + 63.4 + 6.1 + 57.6 - 46.9 -234.4 - 40.2 - 34.6 - 37.2 + 339.6 + 2.7 + 81.4(2) +127.6 + 43.8 - 83.2 - 40.2V?(2j - 24.3 - 23.1 - 91.6 -106.0 - 68.3 -106.1 - 57.0 - 20.1 -265.7(2) -112.1 - 9.9 - 17.1 - 41.9 (13) 0.0(2) 19 6 9ApJ. . .158.1115S e (ra.e.)o. 0.5 0.4 1.0 2.9 0.7 0.5 0.9 0.5 1.4 0.5 0.7 0.7 0.7 0.4 0.4 1.0 0.5 0.5 0.6 0.6 2.5 0.8 0.7 0.3 0.3 0.8 0.6 0.7 0.4 1.2 0.7 0.9 0.6 0.7 0.7 0.7 0.6 0.7 0.6 0.3 0.9 0.5 0.6 0.7 3.3 0.6 0.4 1.3 0.5 0.7 1.4 (14) 1) & 12 08 06 05 01 00 99+ 90* 11 10* 09* 04* 97 95* 94* 92* 91 07 03 02* 93* 87 85* 7 3* 63* 61 98 96* 89 88 86* 78 75* 74 6 8* 67* 66 64 62* 84 79 76*+ 70 69 65 83* 82* 81* 80 77 © American Astronomical Society & Spectraobtainedwiththe8inchaplanaticspherecamera atthe200-inch. + Suspectedradialvelocityvariable(seeTable2) * RadialvelocityistabulatedinPaperI(Ap.J.139,442). +1603924 +71°1053 -9°5491 G24-3 G67-49 SAl15-147 G26-9 G25-24 G143-17 G22-6 + 3403239 G20-8 +2503252 G15-23 G66-30 +71°646 G29-33 G27-45 G18-28 G68-30 G190-34 +5902723 G28-17 G27-44 G18-39 G25-29 -3°4864 G23-1 G183-11 G17-30 G17-16 G24-13 -705235 G21-22 G141-19 G19-27 G17-25 +770521 Name G29-23 G126-19 31 Aql -9°4604 G15-24 G151-10 G66-22 G64-12 G63-44 HD114762 G16-13 -2°3811 G63-46 G14-45 (2) 16933 16 896 16892 16811 15821 16531 16463 16217 15686 15497 16851 16712 16327 15949 15880 15478 15475 15239 14602 16681 16268 15298 15157 14697 14388 14360 13819 16295 14607 13981 13980 13967 (3) 9662 9173 7498 5592 6649 6621 5932 5117 6968 6567 LTT 8434 8065 8021 7089 22 41.3 23 33.2 22 48.2 22 03.2 21 29.6 21 24.2 20 30.1 20 17.9 19 52.8 18 36.6 23 39.4 23 32.3 23 24.2 23 23.7 23 17.1 23 08.3 22 42.3 22 16.1 21 11.1 20 13.9 20 03.3 21 37.3 20 19,4 19 36.0 19 22.6 15 27.1 21 14.1 19 25.9 18 51.9 18 32.7 17 28.8 16 35.7 16 32.0 16 25.2 15 48.6 14 12.7 17 52.8 17 45.1 17 37.3 17 20.3 14 52.5 18 31.0 14 47.6 14 40.8 13 16.4 13 09.9 15 28.2 13 37.5 13 13.2 a (1950) 13 44.1 13 37.5 13 35.6 (4) + 1838 + 514 + 354 + 1036 + 3346 + 837 + 306 + 812 +12 08 +23 02 +16 35 +11 50 + 004 + 3423 +20 18 +60 20 + 136 + 337 +71 27 - 932 + 553 +13 54 +20 17 +70 33 - 000 - 322 - 736 + 2 + 7729 +12 51 - 016 - 236 - 131 + 103 + 602 + 013 +19 24 +17 47 +13 08 - 2 +24 56 - 440 - 935 - 313 - 248 Ô (1950) 6 19 0 58 8 34 8 53 8 34 (5) Provided bytheNASA Astrophysics DataSystem 10.12 10.20 10.72 10.54 10.38 10.20 10.44 10.01 10.47 11.50 11.6 3 10.57 10.96 11.07 10.47 11.49 10.86 10.13 11.43: (6) 9.08 9.55 9 .54 9.71 9.34 9.90 9.74 5.15 8.50 9.68 6.87 9.52 7.32 8.79 9.04 7.44 9.50 8.83 8.48 9.08 7.56 9.24 8.39 8.99 9.97 8.48 9.63 9.63 9.45 9.39 8.56 8.14 8.84 + .54 0.56 0.49 0.77 0.97 0.57 0.61 0.58 0.79 0.44 0.43 0.67 0.51 0.44 1.41 0.66 0.50 0.54 0.58 0.48 0.53 0.50 0.62 0.75 1.01 0.73 0.80 0.43 0.59 0.68 0.64 0.65 0.83: 1.85 0.59 0.71 0.40 0.71 0.57 0.66 0.38 0.46 0.79 0.64 0.66 0.59 0.57 0.72 0.75 0.71 0.68 0.58 B-V TABLE 1(continued) (7) -0.13 -0.03 -0.22 -0.16 -0.11 -0.11 -0.08 -0.19 -0.04 -0.06 -0.18 -0.26 -0.06 -0.10 -0.02 -0.05 -0,06 -0.23 -0.21 -0.20 -0.06 -0.05 -0.11 -0.17 -0.06 -0.08 0.27 0.09 0.03 0.21 0.39 0.00 1.18 0.49 0.00 0.10 0.16 0.10 0.03 0.05 0.43 0.26 0.40 0.05 0.14 0.04 0.08 0.06 0.67 -.08 0.17 U-B (8) (9) 0.17 0.01 0.12 0.20 0.22 0.18 0.03 0.07 0.16 0.15 0.28 0.23 0.06 0.14 0.20 0.17 0.04 0.26 0.16 0.08 0.19 0.16 0.26 0.19 0.26 0.15 0.24 0.13 0,17 0.17 0.07 0.14 0.22 0.13 0.12 0.15 0.21 0.15 0.26 0.10 0.23 0.13 0.17 0.12 0,19 0.20 0.21 0.16 0.25 0.17 (10) + .157 +.460: + .210 + .319 + .232 + .372 +.334: + .158 + .725 + .051 + .226 + .580: +.267: +.152: +.262: -.049 -.031 + .014 + .210 + .126 + .133 + .088 + .680 -.048 -.171 + .100 -.159 -.213 -.0 81 -.150 -.'ISO -.294 -.135 -.394 -.240 -.290; -.579 + .466 -.164: -.350 -.885 -.242; -.645 -.145 -.264: -.148 -.370 -.160 -.242 -.229 (11) .000: .000: + .248 + .188 + .272 + .640 + .080 +.246: + .343 +.260: -.226: -.465 + .201 -.110 -.242 + .031 -.283 -.043 + .048 -.383 -.360: -.240: -.029 -.135: -.335: -.377: -.183 -.226 -.093 -.434 -.319 -.048 -.060 -.004 -.179 -.138 -.425 -.274 -.199 -.102 -.699 -.120 -.295 -.107 -.303 -.165: -.238 -.135: -.112 -.110 -.108: -.322 (12) .000: .000 - 28.8 + 33.8 -200-6 (2) + 3.6 + 81.9 + 28.8 + 36.0 +101.5 (2) + 17.8 + 59.1 + 31.7 +125.2 + 46.0 -243.4 (2) +438.6(3) - 18.1 - 43.9 -150.4 - 82.2 -257.4 - 24,9 - 5.2 - 15.0 -207.4 -386.9 -100.6 - 37.0 + 2.1 - 38.6 -166 V(2) - 84.6 - 28.1(2) -103.2(3) - 44.8 -246 .4 -2 31.4(2) - 22.1 -395.9 (2) -167.2(2) -79.4 -110.6 - 46.2 - 97.6(2) -199.7 -109.8(2) -134.2 -145.4 -87.2 -106.7 - 51.1 - 64.3 - 22.4 (13) 19 6 9ApJ. . .158.1115S 1 1 1 1 B —F)-line,readatthe observed B—Vvalue,followingthedefinitiongiven elsewhere metric catalogmentionedin§I.Mostofthestars wereobservedmorethanonce, from PaperI,asamendedwithnewobservations,ortheunpublishedphoto- the velocitiesinTable1aregenerallycorrectto±2kmsec“.Nosystematiccorrections significant systematicdeviationfromtheWilsonsystemand,comparison(1),that differences betweentwomeasurementsofastar are AF~0.026,à{B—V)0.013, as shownincolumn(9).Comparisonoftheindividual valuesshowsthattheaverage 2.1 (a.d.).(3)Sixstarsincommonwithlower-dispersionvelocitiesduetoRoman Radial Velocities(Wilson1953;hereinafterGeneralCatalogue).Threestarsshowlarge present areAV=—0.004±0.024(a.d.),A(B — F)=—0.002±0.013(a.d.),and with Roman’s(1955<2)high-velocitycatalog.The differences inthesenseRomanminus and &{U—B)0.018mag,orhalfthesevalues fordeviationsfromthemean. have beenappliedtothedata. radial-velocity standardstakenspecially,arecommontotheGeneralCatalogueofStellar its mateisla=3.38kmsec“.(2)FifteenstarsinTable1,togetherwithtwoadditional plates areavailablefortwentystars.Thereisevidencevelocityvariationsfour A(U —B)+0.013±0.025(a.d.),whicharesatisfactorily small. Ps) =+1.1±2.9(a.d.).Thesixstarsofqualitiesaandbshow(pw—ps)+1.5 differences betweenourresultsandthoseoftheGeneralCataloguemaybevariable —4.8 ±3.6(a.d.).Weconcludefromcomparison(2)thatthepresentvelocitiesshowno (19556), butwhicharenotalsocommonwiththeGeneralCatalogue,give(pr—ps)= of these(§III).Fortheremainingsixteenstars,standarddeviationfrommeanis which havelargermeanerrorsare(1)thefourstarsobservedwith8-inchcamera, phase ofthepresentprogram.Suchstars(forty-oneinnumber)areindicatedbyan (Sandage andEggen1959, Fig.4). (running number99=G26—9),whichisalsoaradial-velocity variable(§III). (§ III).Thefourteenremainingstars(Wilsonqualityclassfromatod)show{pw— o- =1.69kmsec“;i.e.,thevarianceofdistributiondifferencesoneplatefrom ments wereindividuallymeasured. the plates,curvedunderpressure,brokeinplateholderandwhereseg- (2) starswherethelinesareextremelyweakandfewinnumber,(3)acases of thenumberlines.Themeanerrorsaregenerallylessthan1kmsec“.Thosecases determinations formanystars. ness andasareferencetoLuyten’sfundamentalcompilationspriorproper-motion which wereadoptedherebecauseoftheexistenceconvenientcharts,innowayindi- in thistablearevelocitiespreviouslylistedPaperIwhichwereobtainedanearly errors, definedastheaverageresidualvelocityofeachlinedividedbysquareroot catalogs ofLuyten(1957,1961).Column(3)liststheLTTnumbers,bothforcomplete- cates preference(astothebasicdata)forLowellcatalogorearlierall-skyLTT asterisk incolumn(1)andareincludedherebothforconveniencetomakethedis- cussion ofspacemotions(§V)morecomplete. © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem The photometricdataarelistedincolumns(6)-(10)ofTable1andtakeneither Column (10)givestheultraviolet excessrelativetotheHyadesfiducial (U—B, Evidence forpossiblelightvariabilityexistsinour presentmaterialforonlyonestar An externaltestofthephotometricaccuracyispossible fromtwelvestarsincommon The externalerrorsofthevelocitiescanbeestimatedinthreeways:(1)Twoormore Listed inTable1aretheheliocentricvelocitiestogetherwithinternalmean The decisiononnomenclatureinTable1wasdifficult.UseoftheLowellnumbers, The presentradialvelocitiesarelistedincolumns(13)and(14)ofTable1.Included NEW SUBDWARFS1119 b) Photometry 19 6 9ApJ. . .158.1115S -1 panion. Inviewoftheir unusual characteristics,G9—16andG26—9should obviously ordinary white-dwarfcompanion.ThestarBD+28°4211 doesnotvaryinlight,soastar of thistypewouldalsobeexcluded.UGemstars, starslikeMacRae+43°(Walker be followedfurther. somewhat fainterthan,BD+28°4211{My^+4, B~V=—0.34,U——1.26; white dwarfs(whoseMyvaluesareallfainterthan ~+10),becausetheywouldthenbe the integratedB—FandUvalues.Thecompanions cannot,however,benormal for thisnormalizationaregivenintheAppendix. with B—Fforstarsofthesamemetalabundance.Thepreceptsandacorrectiontable LTT catalogs(1957,1961)andtheblinkmotionsbyGiclasetal.(1961-1967)weregen- determined eitherbyJones(1966)orfromthetrigonometricparallax,bothofsec- interesting becausebothshowabnormalcolors,whichindependentlysuggeststhepres- dence comesfromthepresentprogramaregivenattop,whilestarswhereourvalue ^ ±0^04forstarsindicatedbycolons(seeGiclasetal.1961-1967andLuyten1967a principal proper-motionsourcesforotherstarsaretheGC,YaleZone,Greenwich, have beenreducedbyEggen,wherepossible,totheN30system(Morgan1952).The per yeartakenfromthefollowingsources.IfastarappearsinEggen’s(1964a)Catalogue Toulouse, McCormickparallax-serieslists,andinafewcasestheSmithsoniantabula- 1954), orevenstarsliketheX-raysourceScoX-l areremotepossibilitiesforthecom- G26—9 variesinlightbyÀliV—0.15mag,which, iftrue,wouldinitselfruleoutan Greenstein 1952;Eggen1959)wouldfitthenecessary conditions. too fainttocauseappreciablephotometriccontamination. Companionssimilarto,but ondary componentsmustberatherraretypesof subluminous bluestarssoastoaffect differs appreciablyfromotherpublishedvaluesarelistedonthebottom.Mostofstars in Table1.Forthese,themeanofmeasuredpropermotionsbyLuytentwo Yale ZonecatalogsthemselvesandthentotheN30.Eggenderivednewpropermotions of HighVelocityStars(thirty-eightcases),hisweightedmeanvalueisadopted.These in Table2showdifferencesgreaterthan3(20.16magwas within +0.15+0.11>(AMy)—0.360.09 magiftheWildeyetal.(1962)cor- relevant rangeof8byEggenandSandage(1962) wasfoundtogiveconsistentresults necessary fromreddening.Thecorrectionsare taken fromTable4ofWildeyetal. Blanketing corrections(Schwarzschild,Searle,and Howard1955;SandageandEggen age-zero mainsequencetoobtainMyandthenm —M. stein 19651). (1962) byusingtheobservedultravioletexcess.The staristhenfittedtotheHyades 1959; CodeMelbourne1960)areapplied toobservedB—Vcolors,freedif 36. .. companion. 99§. . 83f.. 45f.. 33.. . and byKowalsuggestsopticalvariabilityAV0.15mag.White-dwarfcompanion134"distant(EG145[EggenGreen- 90.. . 43*. . 1.. .. 76.. better than±0.4maginMyifthefollowingprocedureisadoptedforweak-linedwarfs. radial-velocity observationsofmanythesestarswouldbegreatinterest,because usual methodsforfindingphotometricparallaxesappeartogiveresultsaccurate only afewPopulationIIspectroscopicbinariesareknown. tances mustbedeterminedinsomeotherwayifspacemotionsaretofound.The No. 3,1969NEWSUBDWARFS1121 © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem It shouldbestressedthat theabovemethodneedbeconsideredinpresent context The methodhasbeentestedagainstavailabletrigonometric-parallax starsoverthe § Theabnormal5(0.6)suggestsbluecompanionfainterthanM-j-7butbrightercs¿-f9.PhotometrybyEggen * FourplatesbyRomangivep=+47.6±44;oneplateGreensteingives+55.5.BlueB—Vsuggestsblue f Greensteinsaysvariablevelocitywhichismoreconclusivethanthedatahere. Only fivestarsinTable1havetrigonometricparallaxesgreaterthan0íf040,anddis- t Greensteingivesp—+78.2;maythereforenotbevariable,because112ddependsononlyoneMcDonaldplate. v No. IV. PHOTOMETRICPARALLAXESANDPRELIMINARYSPACEMOTIONS G26-9 G141-19 G114-26 G143-17 G17-25 G88-31 G9-16 G89-14 9°122 Name 0.97 0.58 0.45 0.47 Suspected Radial-VelocityVariables B —V .64 .48 .75 .31 51 0.47! 0.22 0.19 0.22 0(0.6) .27 .25 .17 .28 .31 From ExternalEvidence TABLE 2 From InternalEvidence 1962 Nov1/2 1961 Feb17/18 1960 Oct23/24 1962 June1/2 1961 Aug22/23 1961 Oct7/8 1960 June21/22 1961 Feb17/18 1962 Apr12/13 1961 Aug16/17 1962 Apr12/13 1962 Feb6/7 1962 Apr16/17 1962 Feb5/6 Date + 92.0+0.4 + 81.91.2 + 32.8+0.5 -150.4 +1.0 -153.8 - 41.9+0.4 -178.4 +41.7 1.3 ± 41.61.4 -194.5 0.5 ± 61.20.6 -206.7 0.7 - 32.21.3 - 48.40.8 P± « 0.7 0.5 +112d(W) + 25c(W) - 78c(W) + 79.9+0.8(R) - 50.3+2.3(R) Other 19 6 9ApJ. . .158.1115S ~29 77 75" No. 21 20 18 16 14 19 30 28 27 23 26 22 (1) © American Astronomical Society +59°886 +68°138 + 7294 G90-3 G84-29 G77-54 G4-44 G8-51 -170219 G88-27 -11°220 G89-14 G87-20 G108-43 G101-33 G98-58 G102-20 G98-3 G8-16 G37 ~34 G5-17 G4-37 G76-21 G75-31 G71-40 G4-6 G72-60 -20181 G70-35 G102-47 G84-37 G96-20 -80128 -9°122 -601598 Name (2) .2^.4 JU5_ 5.71 5.19 2.3 5.40 6.47 6.10 5.22 5.32 4.90 4.62 3.3 5.22 6.00 5.78 2.5 5.85 5.68 6.68 5.48 5.02 4.90 3.0 1.5 2.35 5.91 5.02 4.40 4.00 4.51 4.4 4.92 2.9 5.57 6.10 3.2 4.78 6.50 5.81 5.02 5.19 3.4 3.magnitude diagramsforfourglobular = 0.45isgiveninparenthesesforeachclusterAbsoluteluminositieswerefoundbythemethodof within thestatedaccuracyoverexcessrangeof—0.05<5(0.6)+0.32. with theexternaltrigonometricevidence(EggenandSandage1962,Figs.2,4,5,6)to applied withtheadoptedblanketingcorrections,givesMforsubdwarfswhichagree and theextentofevolutionsubdwarfsfromtheirage-zeroconfiguration(e.g., in the(Mboi,logr)-planeisnotgermanetopresentproblem.Theanswerthis Strom and1967;Cayrel1968).Whatisgermaneherethattheprocedure,as question requiresanexaminationofthevalidityadoptedblanketingcorrections v e 1 © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem Thepresentargumentisunaffected iftheseparticularblanketingcorrectionsareinerror, becauseit Figure 1wasconstructedbydeterminingphotometric moduliforeachclusterbythe Fig. 1.—CompositeC-MdiagramforfourglobularclustersandtheoldgalacticclusterNGC188, But evenifthemethodwereperfect,photometric parallaxes forPopulationIIandold NEW SUBDWARFS1125 19 6 9ApJ. . .158.1115S 1 1 1 1 procedure justdescribedandapplyingtheresultingm—Mvaluestoreddening-free motion limit,thesubgiants,whicharemoredistantatagivenF,willbediscriminated velocities. Thefactorisquitedifficulttoestimatebecausetheselectioncriteriaforstars not shown)hasbeenforced.ThevalueofMy^+0.4forthecluster-variablegapsin normal [Fo,{B—F)o]-pointsforeachclustertogetMyvalues.Theclusterswerethen with theobservatoryand probableerrorindicatedwhereonlyonedetermination isavail- distance expressedaskm sec“pc“;column(14),thetrigonometricparallax inO'fOOl, against relativetothedwarfs,becauseofsmallerpropermotionsforsamespace surveyed islargerforsubgiants{(My)—3)thandwarfs{{My)=5)byafactorof with b>0.16issimilartothatforM3(Sandage1957,Table9),theratioofsubgiants ber canbeestimatedasfollows.IftheluminosityfunctionforPopulationIIfieldstars a sampleofweak-linestarsthatiscompletetogivenapparentmagnitude,andthenum- whose valuesof{B—F)oandbareknown.Alargenumbersubgiantsisexpectedin Deutsch quotedbyKinman1959a)andisshownheretheobservedultraviolet plotted togetherinFigure1byusing{B—F)colorsastheabscissa(noblanketingcor- M15, or47TuefromFigure1;columns(11)-(13) list thegradientinZ7,F,andIF,with occasionally moreexplicitstatementsastothetype ofsubgiantsuchasthoseinM13, sequence, sgforsubgiant,Jtheabsolutemagnitude obtainedbyJones(1966),and B —V=0.6bythemethodinAppendix;columns (7)-(9)aretheUVWvelocity from similarmaterialGreenstein’splatesofknownsubdwarfs. subgiant contaminationmustoccurinbothTable1andEggen’s(1964a)high-velocity in Table1areheterogeneous,butitmaybeoftheorder3.Allthesefactorsmultiply about 15.However,acompensatingfactoristhat,inlistschosentogivenproper- of space.However,incatalogscompletetoagivenapparentmagnitude,thevolume in therange20.4 Space motionswerecalculatedforallstarsinTable1byusingdistanceseitherfound 0 19 6 9ApJ. . .158.1115S 1 1 -1 9 1 motion forM67isalsosimilartothegroupswithvaluesclose7/=+40,V—40, factor <10lowerthantheHyades),haveonlymoderate \Z\distances(Kinman1959a, stein (1955,1965)wasamong thefirsttopointoutthatvelocitydispersion amongthe AS >5,weak-lineglobularclustersofMorganclasses I-IIIorDeutschclassC,and Tables 7and8;Oort1965,§4.2).Objectsinthispopulation appeartoformanextension itself mayhavea3near0.03(EggenandSandage1969,butseeSpinradTaylor subdwarfs withthelowestmetalabundance,show thelargestdriftvelocities(F^ increasing (3)beyondtheaPupgroup. shortest period(0450>P0420)(Kinman19593) orwithAS<5(Preston1959, of theolddiskgroups,continuingtrendincreasing (|7/|),(V),and(|IF|)with Fig. 6)andarelativelysmallasymmetricalmean driftvelocityofF~—80kmsec“ of 3,thetotalspacemotionand3-valuesappeartobelooselycorrelated.GalaxyM67 and IF=—20(Murray1966).Evenamongthissample,whichspansonlyasmallrange type withMorgan(1959)classesV-VIH(whosemetal abundancesappeartobeonlya Eggen aspossiblemembersofseveralmovinggroups,summarizedfollows: ranging from^0.00to0.10.Thebestlocalexamplesofsuchstarshavebeenisolatedby Mv areinconsistentwithFigure1inthesensethat,forexample,high-ôstarscannotlie the plane(Fricke1950;Kinman 1959a,3;Preston1959;Roman1965,Fig. 4).Green- order ofZ7~±60kmsec“,—1000),(2)eitherJones(1966) by Jones(1966).ThepresentdataforstarsincommonwithEggenarethoseused (Kinman 19593).Thesepropertiesaresharedby the BaileytypeabRRLyraestarsof 1967), indicatingslightmetalweakening. within afactorof^0.5-2theHyadesvalue)moveinnearlycircularorbitscloseto Eggen astheywereavailablein1963. to M67andNGC188(-~5-10X10years)haveintermediateUVvelocitiesofthe the galacticplane.The77,F,andIFvectorsareconfinedtosmallvalues,usuallyof abundance. YoungdiskstarswithmetalabundancessimilartotheHyades(Fe/H or thetrigonometricparallaxdoesnotpermitassumedMf,(3)valuesofband of thestarincatalogseitherRoman(1955ö)orEggen(1964^),Mvassigned along theNGC188sequence.Theseimpossiblealternativesolutionsareindicatedbyan asterisk incolumn(10). — 200kmsec“),thelargest dispersioninUandIF,thelargestmeandistance from No. 3,1969NEWSUBDWARFS1127 9 © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem The extremePopulationIIobjectsinthehalo, such asRRLyraevariableswith The intermediatePopulationIIobjects,suchastheglobularclustersoflatespectral The C-MdiagramsforeachofthesegroupsaregenerallysimilartoM67.space Old diskstarsintheagerangedefinedbyNGC762and7789(^2X10years) It hasbeenknownforsometimethatstarsofthevarioussubsystemsGalaxy Some ofthealternativespacemotionsforvariousMvvaluesareclearlyimpossible, 7} Cep Wolf 630. a Pup.. 61 Cyg.. y Leo.. f Her. V. CORRELATIONOFSPACEMOTIONSWITHUVEXCESS Group 0.10 0.03 (0 .06 .03 .07 .04 +40 +91 +70 +54 -23 -75 u •80 ■97 •53 - 4 •45 -33 Small Small Small - 8 -26 -18 w Eggen 1965a Eggen 1959 Eggen 1958 Eggen 19643 Eggen 1964a Eggen 1964a Reference 19 6 9ApJ. . .158.1115S subdwarfs themselvesincreaseswithincreasinglineweakening,asestimateddirectlyfrom metal abundanceisamorerecentresult,nowapparentlywellestablishedbytheworkof spectrograms. the GalaxyhavebeenknowninageneralwaysinceearlyworkofStromberg(1924, velocities andthedispersionsinUWchangewithbforsubdwarfsalone.We subdwarfs givesarapidandpowerfulmethodoftestinghowtheasymmetrical-drift Fricke, Roman,Greenstein,Morgan,Kinman,Preston,Eggen,Lynden-Bell,Sandage, and othersinthereferencescited. 1948, 1950),Kukarkin(1954),andothers.Butthecorrelationofthesepropertieswith 1128 ALLANBANDAGEVol.158 1925), Oort(1926),andLindblad(1927),and"laterfromthestudiesbyParenago(1946, which areradial-velocityvariableswhosecolorsmaybeaffectedbythecompanions. Lynden-Bell byusingequations(2),(10),(14),(15), and(30)ofELS(1962).Theparts were examined.Figure3istheBottlingerdiagram showinglinesofequalapogalactica radial-velocity variablesG9—16andG26—9are shown asopencircles. fiducial lineformsthelowerboundary,whileupper envelopeistakentobethelimit while thelineshowingmaximumabundanceeffectformsupper.OpenCircles,G9—16andG26—9, poulos andStrömgren(1965).Figure3issimilar toadiagrampublishedbySchwarzs- for starswhichhavethemaximummetalunderabundance (seeAppendix).Thetwo would liketoknowifthechangesaregradualordiscreteandcorrelationsholdfor the rangeofultravioletexcessamongstars in thepresentprogram.TheHyades all valuesof5(0.6).Figure2isthetwo-colordiagram forallstarsinTable1andshows of thediagramwithlowvaluesUandVagree wellwiththecalculationsofConto- child (1952).. {closed ovals)andperigalactica{nearhyperbolae)as calculatedfromthemodelgalaxyof circles for0.10<5(0.6) < 0.15,half-closedcirclesfor0.165(0.6)0.20, andclosed circles for5(0.6)>0.21. © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem The easewithwhichlineweakeningcanbedeterminedfromtheultravioletexcessfor These progressivechangesinthekinematicpropertiesofdifferentsubsystems Fig. 2.—Two-colordiagramforallstarsinTable1.TheHyadesfiduciallineformsthelowerboundary, The starsinTable3weredividedintofourexcess groups,andthespacemotions The starsinTable3are plottedasverticalcrossesfor0.00<5(0.6) 0.09, open 19 6 9ApJ. . .158.1115S f abundance. Thisgradient appearstobeanaturalconsequenceofthecollapse ofthehalo sion attheHerstmonceux conferenceonevolution). dates removed.Ineithercase,thetrendofkinematical propertieswithincreasing toward theplane,withmetal enrichmenttakingplaceasthecollapseproceeds (ELS exists inthegalactichalosuchthatstarswith largest(\Z\)havethekwestmetal All starsinTable3areincludedthefirstpartof this Tableasiftheyweredwarfs(with ing bisconfirmedbythecalculatedmeanvelocities andtheirrangesaslistedinTable4. b isclearandinthesenseexpectedfromearlier work(ELS1962,Figs.4and5). 1962), althoughotherexplanations maybepossible(Schwarzschild[1964] in thediscus- the exceptionoftwocertainglobular-clusterlike giants,No.62[G3IIIp]and89 [K3 IIIp]).ThesecondhalfofTable4showsthe correlationswiththesubgiantcandi- hyperbolae) aremarkedinkiloparsecs.Velocitiesrelativetothelocalstandardofrest,obtainedfrom the UandVvectors(relativetoSun)byZ7'=—10, V'—V-f-15. stars intofourultraviolet-excessgroups.Linesofconstantapogalactica(ovals)andperigalactica(near These starsarenotplottedinFigure3,becausemanyofthemfactsubgiantsfrom are listedassuspectedsubgiantsinTable5ofthenextsection,anassignmentwhich,if correct, willremovethediscrepancy,becausespacemotionsthenbelarger. existed whichhadsmallvaluesofUandV;thisclearlyviolatedthegeneraltrend.These external evidenceasdiscussedin§VI. a progressivechangeof(V)and(|I/|}withbwaspresent,butfewstarslarge that usedallstarsinTable3withthemain-sequencechoiceofMy,itwasveryclear Sun’s peculiarmotionhyU—10andVF+15.InatrialplottingofFigure3 No. 3,1969NEWSUBDWARFS1129 © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem The increaseof|IFwithbisparticularlystriking andshowsthatachemicalgradient The visualimpressionofFigure3that|Vand{|£71 )graduallyincreasewithincreas- Fig. 3.—BottlingerdiagramforstarsinTable3,excludingthoselisted5.Codingseparates The spacemotionsarefromTable3ascorrectedtothelocalstandardofrestfor 19 6 9ApJ. . .158.1115S r 1 -1 21/ violates thecorrelationsofTable4.Forconvenience infuturespectroscopicinvestiga- That ageneraltrendofthistypemaybepresent issuggestedbyEggen’sdata(19656) prediction isthateverysubdwarffainterthanthis magnitudeshouldhave5(0.6)>0,21. and Fvelocities(referred tothelocalstandardofrest)calculatedonassumption that for subdwarfsinthedistancerange00.16whose“eccentricity oftheplaneorbit”(asdefinedin particular timesbuthigherWvaluesatothertimes,duetothe“exchange”of plane, formedfromthatpartoftheoriginalhalomaterialwhichwasitselfcloseto to progressivelylargerZdistances.Wewouldexpectfindonlytheextrememetal- abundance existintheplane,metalisexpectedtodecreaseaswesample values fordifferentorbitnumbers),althoughtheeffectissmallparticularcases sional boxorbits(Ollongren1962,cf.hisFigs.24and31,whichshowdifferent|Z[x plane intheearliestphasesofcollapse,or(b)mightpossiblyhavelowWvelocitiesat at anygiventimeinthesolarneighborhood(but,ofcourse,withhighjW|velocities). orbits ofstarsformedhighinthehalopassthroughplane,andsomewillbeobserved to theplanewhichhavelow|Wvelocities.Theseeither(a)alwaysbeennear Many starsofthistypeexistinTable3.(2)Thereare,however,extremesubdwarfsclose computed byOllongren. than theformaldispersionsbyafactorof(2/tt)^=Í25ifdistributionsareGaussian. W =Í00kmsectakesastarto2200pc. (U +F)andtheWvelocitiesthatappearspossibleincertaintypesofthree-dimen- 1130 ALLANSANDAGE ma Mean VelocitiesandTheirDispersionasFunctionsofô(06)forStarsinTable3* -1 © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem Many starsinTable3havelarge6(0.6)valuesbut low£/,F,andWvelocities,which The chemicalgradientthenonlymeansthat,whereasstarsofbothhighandlowmetal Although ageneralgradientappearstoexist,itisnottruethatstarswiththelowest * Thespreadofthedistributionsisindicatedbyaveragedeviations{j£/f),(F—(F)},and(jIF|).Thesearesmaller t AIFvelocityof50kmsecforastarnowintheplanewilltaketoheight800pcattopitsorbit 5(0 6) <0(0 6)} 0.254 0.236 0.180 0.127 0.054 0.184 0.127 0.054 VI. POSSIBLESUBGIANTSINTABLE3 37 33 42 23 23 14 19 14 +48 +11 +14 +53 + 15 + 6 +14 +15 00 TABLE 4 Excluding SubdvvarfCandidates Including SubgiantCandidates 158 117 145 61 62 85 61 62 -204 -192 - 62 -105 - 62 -149 - 45 - 45 () (W)(¡TFf)t F 27 28 74 27 28 79 82 78 +4 +4 -9 -9 -2 -9 -2 -9 31 31 93 49 93 51 17 17 19 6 9ApJ. . .158.1115S •4(12) 39* >0* 38* 36* 34* 79* >6 54 >3* 50* 36 34 33 31 18 38 30* >6 23 L> 6* 100 © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem 6 3Trigitvelocitiesaretabulated.Photometricttremovesthemildanomaly. 60 Mustbesgiftrig,ttiscorrect.Dwarfofphotometric^=0.067which 39 MustbesgnearMv=+1.7ifJonesiscorrect.ThisgivesU=-264,V=-375, 88 86 79 30 MainsequenceaccordingtoJones.LowUVandWraisesthepossibility 84 G22-6 G14-32 +3403239 G88-40 G102-20 G19-27 G63-46 G63-44 G58-23 +55°1362 6 MustbesgifJonesiscorrect. G126-19 G23-1 G13-1 -601598 G84-37 -17°219 G112-36 G14-45 G59-18 -2103420 Name (2) consistent withFigure Trig itnotconclusive. Trig 7Tnotconclusive. Trig tínotconclusive, impossible onbasisoftttrig. W= +69.Trigonometricttisveryuncertain. of acontaminatingcompanionaffecting5(0.6). a possiblesolution. If asglike47Tueat a possiblesolution. If asglike47Tueat 07 07 06 05 21 17 05 01 13 13 13 12 19 18 18 11 10 13 11 10 «(1950) (3) 28.8 05.8 56.5 01.4 25.9 51.9 21.0 53.0 35.6 16.4 37.3 37.5 47.2 37.3 31.7 37.3 11.7 32.7 30.2 Assigned MainSequenceorTrigonometricLuminosities 7.3 Stars with6(0*6)>0.16ButWithe<^0.40If 0.67 0.58 B-V 0.77 0.68 0.94 0.72 0.58 0.60 0.70 0,82 0.51 0.56 0.65 0.52 0.79 0.59 0.50 0.52 0.72 1.01 (4) M= +1.3,thenE>0andV=+144.Mildsgat^+3 is Mv= +1.5,thenE>0andV=+113.MildsgatM-+3 is 1. v v Jones givesM=4.0butsuchasgwith6=0.18isnot Notes If asgatM.=3.2,the5isnotconsistentwithFigure v y 6(0.6) 0.19 0.18 0.31 0.22 0.16 0.24 0.19 0.16 0.16 0.21 0.18 0.31 0.17 0.16 0.18 0.17 0.16 0.20 0.16 0.20 (5) Candidates ForSubgiants (6) +56 + 10 + 17 + 47 +40 -22 -51 -68 -12 + 6 -16 -77 - 4 +46 -5 4 +24 U' V'w - 5 -22 -50 -77 Table 5 km sec"-*- (7) -15 -14 -59 -61 -25 +32 -26 -21 -54 + 4 -52 -51 -11 -62 -70 -80 + 6 + 7 -41 -80 +109 (8) +73 +26 +51 + 72 -81 -31 -49 -57 +65 -39 -30 +12 -82 -45 +71 -16 -50 -16 +15 kpc k 10 (9) 6 5 9 6.2 6 6 9 5.8 5.8 2 5.8 9 7 7 4.3 4.5 8 8 8.8 8 kpc 10.8 10.2 10 10 13 10.2 10.2 10.5 15 R 12 12 11 10.5 13 10.1 10 11 11 10 10.2 (10) i 0.19 0.27 0.19 0.25 0.30 0.06 0.27 0.29 0.20 0.26 0.16 0.40 0.11 0.27 0.18 0.38 0.27 0.12 0.37 0.14 (ID sg(R) sd(T) sg{T) ms (J) sg(J) sg(J) ms (J) sg(J) (12) (13) 24(7) -5(8) 43(8) 16(7) 11(7) 37(13), 1. "t 19 6 9ApJ. . .158.1115S ; ; -1 -1 -1 here. TheU,F,andWvectors listedinTable6havebeencalculatedasif the starswere proper motions(theirspace motionsrelativetotheSunaresmall)have beenchosen which is7Pav,whoseparametersarelistedatthe endofTable3underrunningnumber tion andradialvelocityarewelldetermined,giving F=+59at5(0.6)0.18. 0.21 andF'=+78.Severalbrightnearbystars haveF'>0,themostinterestingof stars arerelativelybright and,therefore,nearby,astheymustbetohave largeenough 113. ThetrigonometricparallaxforyPavislarge (0M11+0T006),andthepropermo- have 5(0.6)>0.16.Othersbeenfoundby Eggen (1968í;),suchasBruceProper few, acircumstancewhichfurtherreducestheproper motion. volume ofspaceduetoreasons(1)and(2),alarge volumemustbesurveyedtofinda have aparticularlyhighvelocityrelativetotheSun.Theywill,therefore,bebiased Motion numbers46420,with5(0.6)=0.20and V —+64,and46491,with5(0.6)= against incatalogslistedaccordingtopropermotion. Andbecausetheyaresorareper such starsinthesolarneighborhoodwillbenearperigalacticonandmoving galactica forsuchstarsareallgreaterthani£—5andmorelikelytobe proper motion,isexpectedtobesmallforatleastthreereasons:(1)Becausetheperi- of lowdensity,farfromthecenter,andtherewillpresumablybefewthem.(2)All than7 (for|<200kmsecaccordingtoFig.3),theywereallformedinregions Sun willbeaminimum.(3)InmostregionsofFigure3withF'>0,thestarsdonot lead theSuninitsrotationbyamountsuptoF'=+160kmsec,whichisescape velocity ontheLynden-Bellmodel. through thesolarneighborhoodneartheirmaximumvelocity.Thetimespent matter nowintheGalaxyknowntohaveh>25,albeitpresentlymovingnearly formed andwasfallingtowardthecenter.Thatsuchmatterdidexistisprovedby on thispointwasmade. of thistype(h>25,ö0.16)wereknowntoELS(1962,Fig.6,e.g.),andadiscussion collapse willstillhaveh>25,butmoveineccentricorbits(i.e.,\U\>0).Nostars circular orbitsatoroutsidetheSun’sorbit.Starsformedfromsuchmatterduring now available.ButthetrendofcorrelationsinTable4isnotaffectedbythesebiasing mated fromFigure3.Column(11)showstheresultingvalueofe.(12)listsinde- was atlargedistances{R>10kpc)fromthecenterbeforeequilibriumgalaxy should exist.Thisfollowsbecause,iftheGalaxydidindeedcollapse,matterwithh>25 momentum ofthehalopopulationcanbemadefromanysamplehigh-velocitystars pendent estimatesoftheluminosityclass,eitherfromJones(7)or,whereavailable, selected onthebasisofU-F-,orfF-values. 2 angular momentaequaltoorgreaterthantheSun(h=25inunitsof100kpckmsec) effects, becausestarswithallvaluesof<5existinthesample,whichitselfwasnotpre- from thetrigonometricparallaxes{T)givenincolumn(13). stars werealldwarfs.Becauseoftheseselectioneffects,novalidestimatetheangular side ofthediagramthanareshown,duetofactthatfigureisplottedasif complete pervolumeofspacebutalsobecausemorestarsundoubtedlyexistontheleft of starsinFigure3ishighlybiased,notonlybecausethesampleTables1and other starsinTable3.Inthisconnection,itshouldbeemphasizedthatthedistribution doubtedly exist,asindicatedbytheestimatesmadein§IVandJones’sresultsfor (9) and(10)ofTable5aretheperigalacticonapogalacticondistancesasesti- 1132 ALLANSANDAGEVol158 y f © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem The starswithF'>0inthepresentprogramare listedinTable6.Mostofthese Such starsdoexist,however.Therearethirteenin thepresentsample,sevenofwhich The numberofsuchstarsnowinthesolarneighborhood,andlistedcatalogshigh Such stars,iftheyexist,willoccurinFigure3totherightoflineV=0.They On theELSgalactic-collapsepicture,starswithhighlyeccentricorbitsand Table 5doesnotexhaustthepossibilitiesforsubgiantsin3.Manymoreun- VII. HIGH-ANGULAR-MOMENTUMSTARSWITHLARGE5(0.6) 19 6 9ApJ. . .158.1115S IInohm -1 rf /2/21 /21 ing awayfromthehigh-velocityantapexat/~270°,5c^0(ora~9105~ away fromthehigh-velocityantapex.Fewsuchstars exist,ascanbeseenbyinspection year. Theresultstobeexpectedfromsufficient materialofthistypeare(1)afirmer But, dependingontheradialvelocity,remainder aregoodcandidatesforstarswith catalogs byselectingthosewhichhavepropermotions inthe“forbidden”quadrant determination oftheescape velocityoftheGalaxyand(2)atestwhether 5(0.6)in- proper motionfortheirpositionsinthesky. of theBruceProperMotionSurvey(Luyten1963), theLowellfields,or,forexample, and specialobservations. creases towardtheleading boundaryofFigure3.Asearchforsuchstars hasbeen especially ifproper-motioncataloguesareusedwhose limitsaresmallerthan/x~0'i20 The RadcliffeCatalogueofProperMotionsintheSelected Areas(Knox-ShawandBarrett 1934), andmanyofthosewhichdoexistwillbenearby whitedwarfswithsmallmotion. U' =£7'0have5(0.6)<0.16.Butthesamplemustobviouslybeincreasedbynew 103 started. F' >0.MostofthestarsinTable6do,fact,have unusualvaluesofthedirection —48° [1950]),andarethereforeunusual.Manyofthemcanbelocatedinproper-motion 113 y most elementaryprediction,5(0.6)mustcorrelatewithincreaseddistancefromthe0,0 close tothelineR\=20kpcallhave5(0.6)>0.16,whereasmostotherstarscloser origin forF'>0intheBottlingerdiagram. and mustthereforehaveincreasinglyeccentricorbits.Ifthecollapsepictureisrightinits such asnumbers3,5,52,84,88,and103yPav.Ifanyofthesearesubgiants,F'be- have V>0iftheyaresubgiants,becausetheincreaseddistancewillcausetobecome negative. TheonlycertaincasesforF'>0arethosewhosedV/drvaluespositive, creases systematicallywithincreasingpositivevaluesof(F+U).Thestars dwarfs, thereforegivingminimumdistancesandspacemotions.Someofthestarswiilnot comes evenmorepositive,andthestarmovesfarthertorightinFigure3. No. 3,1969 F' >0haveapogalacticawhichbecomeprogressivelylargeras(F+£/')increases 93. 48 84 68 88. 54. 78 52 20 10 No ; 3. 5 © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem Candidates forstarsofthistypecanbefoundasfollows.IfF>0,thearemov- It seemsprobablethatmanystarswhichleadthe Suncanbelocatedinthisway, Figure 3suggeststhatthismaybethecase.ThefourstarswithF'>0whichlie The presentmaterialisnotsufficienttotestadequatelyifthemetalweakeningin- 7 Pav G27- G24-13 0.61 +34°3239 0.50 -j-25°3252 0.51 G23-1 0.79 G13-1 —14°3322 —2°3831 0.57 -f-55° 1362 G8-51 G72-60 —2°181 G70-35 Name B—V Stars withF+15>0ifAssignedtheMain-SequenceLuminosity -44 0.49 0.49 0.58 0.58 0.56 0.70 0.69 0.80 1.08 5(0 6) 0 18+0.088 0.08 .19 .000: .16 +.232 .16 +.107 .21 -.114: .13 +.157 .17 +.210 .11 +.051 .07 -f.100 .06 -.233 .18 +.220 24 -f.130 11 0.191 Ma NEW SUBDWARFS .196 TABLE 6 +0.800 + .343 + .031 + .201 + .256: - .335: - .183 - .190 - .112 -0.116 - .034 - .086 - .254 - .027 MÔ + 28.8-67 - 30.2+4 - 28.8+44 +101.5 -138 + 3.66 + 31.7-47 + 11.486 +127.6 - 370+40 - 23.054 - 9.9 - 40.0 - 17.1 0.0 +147 - 33 - 37 - 51 - 18 t U +29 +10 +59 +32 + 3-7 + 6 +52 +22 + 7-30 +27 +5 + 4 + 10 +14 +13 +65 + 6 +37 -39 + 4 -87 -31 - 2 -16 -28 -42 W* +3.454 +0.408 +0.729 +0.493 +0.230 +0.948 -0.317 -0.082 -0.408 -1.069 +0.094 -0.062 -0.261 -0.737 possible sg possible sg possible sg dV/dr 1133 19 6 9ApJ. . .158.1115S proper motions,andK.C.FreemanM.E.Dixonfortheircarefulreadingofthe of thespectrograms.ItisalsoapleasuretothankOlinEggenforhisadvicewith manuscript. parallel totheintrinsicHyadesline.Correctionsobserveddareneededifmetalabun- who useddifferentmethods. dances aretobecomparedamongstarsofdifferentcolors. different B—Vvalueswiththesamemetalabundancewillshowultraviolet-excess maximum abundanceeffect.Althoughtakenfromadifferentsource(thephotometriccatalog values. Forredstars,d(U—B)ispartiallyguillotinedbecausetheblanketinglinenearly 0.45. . 1134 ALLANSANDAGEVol.158 0.70. . 0.60 .. 0.50 . 0.40 .. 0 35.. discussed in§I),theguillotineagreeswellwithanindependentdeterminationbyEggen(1968a) for 0.75,0.50,and0.25ofthemaximumblanketing are listedincolumns(5),(6),and(7)of 0.65 . 0.55. 0.80 ... 0.75 ... columns (9),(10),and(11). Table 1A,Thecorresponding correctionfactorsfromwhichö(0.6)canbefound aregivenin the coordinatesofmaximumabundanceline,column (4)istheexcessofthislinefrom 0.95.... distances alongthesevectorsforallZ7—B(cf.Arp1962). Theôfromthe(U—BV)lines Hyades, andcolumn(8)istheratioofexcessat(B —F)=0.60(where5isamaximum)to 0.90 ... 0.85. blanketing vectorsfromWildeyetal.(1962,eq.[9])in Figure2andmarkingoffproportional ô atanyother(B—F). 1.10. 1.05.. 5(0.6) foranystarwhosevalues of{B—F)and5areknown. 1.00.. y 0 0 0 (B-Vh © American Astronomical Society •Provided bytheNASA Astrophysics DataSystem Table 1Acanbeusedwith interpolationincolumns(1)and(4)-(7),respectively toobtain It isapleasuretothankSylviaBurdandMaryWhiteoakformeasuringthemajority The shapesoftheblanketingvectorsin{U—V)diagramaresuchthatstarswith The guillotinecanbeseeninFigure2.upperlineisconsideredtotheenvelopefor Table 1Agivestherelevantdata.Column(2)showsHyadesfiducialline,column(3) For underabundancelessthanthemaximum,similar ratios canbeobtainedbydrawingthe (1) NORMALIZATION OFOBSERVEDULTRAVIOLETEXCESSES (U—B) Hyades h 0.03 0.99 (2) .34 .25 .13 .08 .00 .01 .19 .03 .74 .64 .43 .94 .84 .54 (U~B) + .19 - .18 - .22 -0.22 +0.87 + .67 T .55 + .44 + .08 + .79 + .32 - .03 - .11 - .25 - .27 - .25 m Limit TO CORRECTFORTHEGUILLOTINE (3) 5 =/(£-V)forVarious5(0.6)Values 0.25 0.12 (4) .31 .30 .19 .24 .30 .27 .26 .17 .20 .22 .26 .28 .28 .15 TABLE 1A APPENDIX So 75AÍ 0.09 0.17 (5) .20 .21 .21 Observed 5 .20 .19 .18 .17 .12 .14 .15 .18 .19 .20 .16 0.11 0.06 5o.6Af (6) .13 .13 .12 .11 .09 .10 .11 .12 .12 .12 .12 .11 .12 .12 0.04 0.055 §0 MM .055 (7) .055 .06 .06 .06 .055 .06 .06 .055 .06 .055 .055 .06 .06 5(0 6)/8m 2.58 2.06 1.15 1.19 1.11 1.24 1.82 1.63 1.03 1.00 1.03 1.41 1.29 1.19 1.10 1 55 (8) S CorrectionFactor 5(0.6)/ 5o 75M 2.33 1.17 1.23 1 23 1.75 1.10 1.08 1.10 1.50 1.40 1.31 1.17 1.00 1.00 1.05 1.00 (9) 5(0.6)/ 2.2: 1.08 1.08 1.18 1.18 1.44 1.30 1.08 1.08 1.00 1.18 1.18 1.12 1.04 1.00 1.04 (10) (11) 5o 5MMM 1.1 1.0 1.1 1.1 1.1 1.5: 1.1 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 1.0 No. 3, 1969 NEW SUBDWARFS 1135 REFERENCES Adams, W. 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