1994AJ 107.2184E 1 THE ASTRONOMICALJOURNALVOLUME107,NUMBER6JUNE1994 where C=-0.2(b—y), luminosity; young diskpopulationareextensivelydiscussedinEggen where Inc. undercooperativeagreementwith the NationalScienceFoundation. heavy elementabundance; (1993) onthebasisoffollowingcalibrations:reddening; 2184 Astron.J.107 (6),June1994 Operated bytheAssociationofUniversities forResearchinAstronomy, 1 A/V=4.86(C) —5.86(P—/)+0.95,(2) M=6.0 —13.00(P—/)—20.00A(45—48) © American Astronomical Society • Provided by the NASA Astrophysics Data System The normal(classIII)giantsoftypesGandKinthe P[Fe/H](DDO)=3.12ACN+0.031, (6) (¿>-y)o=0.826(P-/) +0.722M-0.5(by) A(45 —48)0=(45—48)—0.600(42—45)“0.605, (C)=(41—2.6[5 —58)0.45(42—45) 10 y0 1 0 m0 8 B lightcurvesofCepheids,F,andinterpretationthe(PLF)relationasa(PL[Fe/H])needs P>10 d). The reddening,luminosity,andheavyelementabundanceof250brightgiantssupergiantstypeGK greater than5X10yr,andoftypeGO/3withage2X10areveryscarceinthesolar further investigationinlightoftheapparentsensitivityMtoFe/HforFstars(thedomain previously notedcorrelationoftheheavyelementabundanceindex,AMj,withamplitudedefectin but maynotbereliableforthoseoftypeGO/3.Theavailablespectroscopicdeterminations[Fe/H]give photometry, whencorrectedforluminosity(gravity)effects,issensitivetoheavyelementabundanceinthe neighborhood. Themedianspacemotionvectorsofthebrightgiantsandsupergiantswithwelldetermined type stars.Thereislittleevidenceforanappreciablegalactic,radialgradientintheP[Fe/H]values.A F typestarsbutnotinthoseofGKtype.TheCNindexreflectstheheavyelementabundance space motionsare(£/,V,JV)=(+10.6,—13.2,-7.7)±(12.3,8.8,8.8)km/s.Theindexfor4color are discussedonthebasisof4color,DDO,RI,andGenevaphotometry.BrightgiantstypeGKwithage Cepheids withP<10d)andlackofthissensitivityfortheG0/3star(domain in thepeakfrequencyofphotometricallydeterminedvaluesP[Fe/H]forFtypeandGK mixed resultswiththetwolargestsamples[McWilliam,ApJS,74,1075(1990);Brownetö/.,71,293 (1989)] beinginternallyconsistentbutwithalargezero-pointdifference.Thereissimilarshift B — 3.12(CJ,(3) 1 0 PHOTOMETRY OFF-KTYPEBRIGHTGIANTSANDSUPERGIANTS.III.THELUMINOSITY, -0.792], (5) + 0.353,(1) 1 Cerro TololoInter-AmericanObservatory,NationalOpticalAstronomyObservatories,Casilla603,LaSerena,Chile 1. INTRODUCTION REDDENING, ANDHEAVYELEMENTABUNDANCEOFGKSTARS Received 1993December7;revised1994January31 0004-6256/94/107(6)/2184/27/$0.90 Olin J.Eggen ABSTRACT (4) where metric parametersintermsofluminosityandreddening.The pergiants (SG)requireadifferentcalibrationofthephoto- The (b—y),M,,C¡and(R,I)systemsaredefinedinEggen where adopted relationsare: (1982) andtheDDOsysteminMcClure(1976). P[Fe/H](M)=3.2A(M+010, (7) As notedinEggen(1993)thebrightgiants(BG)andsu- E(b—y) =1.085(1?—/)—0.603[(42—45) A(M)o=(M-2.15/?-/)o +0.240.(9) ACN=(C)-1.2(Ä/ +0.131,(8) My(4C) =2.75—10.50(1?—/) —7.65[« —6],(13) A/V(DDO) =1.75—9.50(1?—/) —20.05(45 Aiy(DDO) =3.43—14.00(1?—/)—20.05(45 10 5(45 —48)=(45—0.600(42—45)—0.695,(11) 1 m0 0 0 0 — 5(45—48)]+0.151,(10) — 48)for(l?-/)^0.375, (12) — 48)for(f?-/)=£0.375, 0 0 © 1994Am.Astron. Soc.2184 1994AJ 107.2184E 2185 O.J.EGGEN:GKGIANTSANDSUPERGIANTS © American Astronomical Society • 18.2032 65297 65228 64858 64572 64571 64320 63822 63700 63609 62236 61714 61561 58134 59890 54669 58526 58367 45416 44612 27385 59367 56695 47209 45629 43497 42456 41701 28085 26630 25049 23010 20902 57623 57118 54605 53003 49778 49105 48616 47667 47475 40805 39400 28794 24107 20176 55751 52497 51043 50372 49212 49102 49068 49050 38871 31910 31767 49091 49367 18145 17005 16901 15589 14985 13640 12409 HD 6446 8267 7927 3488 7.24 3.95 8.11 6.13 2.37 4.95 6.27 9.48 8.92 3.70 4.90 8.13 5.60 4.59 6.51 5.59 7.86 7.52 7.43 5.76 7.15 8.98 4.65 6.64 6.13 6.36 6.59 6.94 6.16 3.52 5.89 6.00 6.66 4.16 4.74 4.18 3.87 6.63 6.64 6.73 4.88 6.65 6.64 6.76 7.16 5.94 7.20 4.86 6.39 6.03 7.30 7.34 7.16 5.84 5.36 6.40 1.70 7.02 5.77 6.48 6.55 8.30 8.43 4.67 5.05 6.25 7.64 5?97 0.447 0.236 0.344 0.356 0.434 0.357 0.413 0.347 0.300 0.375 0.382 0.310 0.263 0.370 0.346 0.369 0.328 0.335 0.359 0.253 0.277 0.343 0.400 0.195 0.310 0.359 0.535 0.281 0.440 0.525 0.360 0.306 0.469 0.340 0.470 0.281 0.375 0.312 0.345 0.355 0.353 0.391 0.400 0.405 0.391 0.555 0.380 0.528 0.481 0.305 0.460 0.455 0.474 0.596 0.383 0.391 0.360 0.088 0.350 0.214 0.348 0.260 0.310 0.384 0.528 0.453 0.309 0.345 0.385 0®352 0.424 R-I 67243C 67243A 97189 96746 96544 95393 94584 93807 92449 91629 90772 90301 89925 89874 89805 89373 88756 89716 89175 88495 88092 87951 88069 86056 87323 87109 86453 85656 83609 85530 85205 84610 84533 84441 84341 63696 63657 83111 62415 82205 62150 82122 61949 61502 80126 80106 79739 79737 79696 78791 77020 73155 66111 67594 67523 66604 65699 77996 77615 75276 74160 72561 72125 71181 70555 66678 76006 75586 70385 70302 70046 HD Table 1.(R-I)photometry. , 10.46 Provided bythe NASA Astrophysics Data System 8.39 7.78 6.64 5.48 8.05 6.54 4.46 6.90 3.87 7.12 7.86 7.46 7.47 8.08 6.36 6.84 7.30 5.54 7.36 7.26 4.93 2.70 7.30 7.86 7.99 7.00 7.14 6.42 6.80 4.94 7.48 6.06 8.05 8.32 6.50 6.07 6.93 6.74 4.25 6.36 4.25 6.97 7.96 7.42 7.66 4.68 3.90 5.20 5.23 5.39 3.32 4.42 5.56 7.74 5.46 2.66 7.35 7.72 7.06 4.20 6.44 9.08 5.52 7.22 5.79 8.88 4?62 3.94 5.67 7.66 0.422 0.318 0.426 0.482 0.416 0.322 0.259 0.247 0.274 0.298 0.456 0.445 0.291 0.547 0.343 0.343 0.449 0.307 0.283 0.300 0.302 0.333 0 350 0.412 0.263 0.441 0.376 0.328 0.303 0.530 0.275 0.418 0.495 0.391 0.616 0 446 0.533 0.269 0.487 0.268 0.363 0.289 0.462 0.500 0.346 0.302 0.427 0.445 0.353 0.290 0.374 0.275 0.359 0.455 0.353 0.459 0.403 0.396 0.350 0.490 0.404 0.355 0.414 0.405 0.314 0.322 0.079 0.770 0.359 0.362 0*?345 R-I 15 2 0 6 2 0 2 2 2 2 0 0 2 3 5 4 5 4 4 0 6 2 1 0 2 2 2 2 2 4 4 2 1 5 0 4 3 6 3 4 0 2 2 1 1 5 4 3 7 7 3 4 4 2 1 5 5 4 5 0 7 2 0 1 0 7 5 5 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 3 2 3 2 2 2 2 2 2 4 2 2 2 2 1 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 3 2 3 4 3 2 2 2 2 2 2 2 2 2 2 2 2 3 2 2 2 2 1 3 2 1 103225A 145302 144338 142584 143084 142811 142277 141767 141120 136635 136537 136474 135551 143119 142822 137465 136636 136505 134704 134270 132594 135913 132242 131425 132223 131296 129330 110463 128713 127685 125609 120112 119605 116520 117740 117341 114756 114533 113778 112762 111790 126152 124602 124196 123349 122223 121976 121261 120537 111315 106262 106981 107265 106057 105340 105136 104096 103134 104215 102839 102305 101570 100276 101314 100137 99576 99313 99154 96782 98386 97534 HD 10.33 6.30 6.77 9.10 6.70 6.68 8.52 4.61 6.27 6.14 5.75 7.15 7.06 5.62 8.19 7.36 4.96 6.22 6.79 7.80 7.50 7.59 7.51 6.61 7.70 5.45 5.12 6.61 3.38 5.75 6.05 4.18 8.67 6.19 5.56 7.99 6.09 7.27 5.90 7.62 7.94 7.00 5.24 5.41 5.12 7.62 7.43 5.78 5.05 4.53 8.71 9.07 7.55 7.19 7.05 5.72 4.33 8.42 6.70 5.15 7.13 7.26 4.46 7.35 7.46 8.46 6.77 4®00 7.91 7.90 7.74 I 0.386 0.512 0.500 0.464 0.442 0.556 0.487 0.390 0.376 0.409 0.409 0.326 0.362 0.324 0.306: 0.366 0.211 0.391 0.356 0.436 0.396 0.396 0.485 0.661 0.404 0.499 0.362 0.436 0.456 0.265 0.391 0.341 0.506 0.356 0.336 0.447 0.204 0.364 0.512 0.393 0.493 0.356 0.369 0.344 0.369 0.440 0.300 0.466 0.409 0.485 0.469 0.441 0.457 0.356 0.475 0.371 0.400 0.374 0.268 0.380 0.359 0.462 0.395 0.334 0.457 0?347 R-I 219 416 391 374 338 2 0 2 2 2 3 3 2 0 2 0 2 1 0 0 0 4 2 1 5 2 6 2 5 4 2 0 2 4 4 1 5 5 1 5 1 2 5 3 4 0 1 1 1 2185 1994AJ 107.2184E where £[«—6]=[w—Z?]—3.80(Æ—/)—0.240.Thetem- bers ofthecluster.Thecluster members arerepresentedby wide binarysystemsarelistedinTable4.ThevaluesofM photometry isbasedonobservationswiththe0.6,1.0,and perature rangediscussedhereislimitedto(/?—/)=0.275 members (Eggen1981).Allthree starsareradialvelocity Table 1ofPaperIarecorrectedin3. mean deviationofasingleobservationfromthevalues ready intheliterature,arelistedTable2,whereAis lection ofmy(R,I)resultsisinTableI,wheremostthe mediate bandandH/3observations(Eggen1992,hereafter 0.425 mag. symbol forpeculiarAtypestars accompaniedby“p”.The closed circlesinthe[u—b],M planeofFig.1withthe cussed inthefollowing. from DDOand4color(4C)photometry,respectively,are of 45-48,42-45,and41-42,respectively.Afewerrorsin system, madewiththeCerroTololoreflectorsandnotal- intermediate bandobservationsareinEggen(1989ab).Acol- hereafter referredtoasPaperII).InadditionI,the heavy elementabundancesoftheFtypestars(Eggen1991, referred toasPaperI)andtheluminosities,reddenings, 2186 O.J.EGGEN:GKGIANTSANDSUPERGIANTS similar tothe9.35±0.20magderived from25BandAtype derived withEqs.(12)and(13).ThereddeningisfromEq. (Sowell 1987)andpropermotion (lannaetal.1987)mem- (10). Theindividualclustersandbinarysystemsaredis- 1.5 mreflectorsonCerroTololo.ObservationstheDDO 0 v v NGC 2287:Thethreegiantsgiveameanmodulusvery © American Astronomical Society • Provided by the NASA Astrophysics Data System The previoustwopapersofthisseriescontaintheinter- BG andSGmembersoffourgalacticclustersthree -53.7416 LSS3970 161471 161368 160706 160529 159633 159181 157549 157819 155072 156866 154853 153639 153573 151856 150675 150479 150416 150090 151834 150085 149900 148218 147266 147225 146525 146146 146143 145544 145336 HD LSI 4 2.82 7.34 2.36 5.71 7.36 5.62 5.47 7.64 9.06 6.19 5.41 8.55 9.60 6.40 6.56 7.64 4.44 5.99 6.28 7.30 7.22 7.50 6.96 7.86 5.41 5.70 5.36 4.60 3.33 9.63 8®66 7.81 0.216 0.558 0.666 0.355 0.654 0.650 0.420 0.332 0.358 0.988 0.432 0.726 0.450 0.382 0.474 0.999 0.415 0.564 0.452 0.403 0.456 0.259 0.541 0.300 0.436 0.377 0.413 0.494 0.310 0.370 0.535 0*400 R-I -0.3783 164591 183791 163418 162635 160540 179590 160262 179440 178937 176653 177433 173764 173368 176123 174947 174349 173568 172508 170866 172365 170457 170053 169660 166356 166245 165633 166263 165462 163413 161614 162565 HD Table 1.(continued) 6.94 6.66 4.46 7.52 4.36 6.58 7.36 7.34 6.96 5.90 6.49 3.69 6.51 6.64 6.26 7.78 5.19 6.00 6.26 5.99 6.64 6.66 6.99 5.15 7.64 7.14 6.67 7.22 6.11 7.15 5.93 5*41 0.312 0.394 0.412 0.346 0.262 0.321 0.432 0.350 0.305 0.536 0.350 0.390 0.357 0.429 0.584 0.391 0.754 0.726 0.546 0.299 0.566 0.532 0.353 0.403 0.466 0.443 0.516 0.491 0.397 0.335 0.499 0?600 8 8 R-I members ofthecluster.Thebrightestclusterstar,HR members arerepresentedinFig.1withclearcirclesand“p” members, 8.32±0.22mag(Eggen&Iben1991).Tliecluster uncertain althoughAmieux&Burnage(1981)havepub- of \u—b\isprobablyaffectedbythepeculiarity.Neverthe- Gieseking &Karimie1982)orpropermotion(King1978) stars. Theobjectsdiscussedhereareallradialvelocity(e.g., accompanies thesymbolforthoseknowntobeAporBp(si) 4X10 yr(Bertellietal.1992)withZ=0.02andconvective continuous curvesrepresentisochronesfor3X10and boundaries, hasamodulusof 10.5 mag,whichplacesitat found thatHD87283(F2II),which lieswithinthecluster of theclusterstarsarerepresented bycrossesinFig.1where lished radialvelocities.Threeknown Bp(si)stars(Fryeetal. for thethreeredgiantsinTable4.Clustermembershipis members forwhichStrömgrenphotometrywasobtainedby ter stars,whichareverysimilartothoseinHGC2287. less, thestarisapparentlymuchyoungerthanotherclus- 3147(V 374Car)isofspectraltypeBeIVpneandthevalue agrees wellwiththosefoundfrom35BandAtypecluster sidered here.Thisstargivesareddeningandmodulusthat one, HR3076(HD64320)isinthetemperaturerangecon- overshoot atthestellarcores. and reddening(Eggen1977)agreewellwiththoseobtained a modulusnear10.5mag,areomitted.Themean Schmidt (1982).Ahalfdozenobjects,whichappeartohave “p” accompaniesthesymbolfor Bpstars.InPaperIIitwas 1970) intheclusterareaddedat theendoftableandall NGC 3114:Table5containstheresultsforBtypecluster HGC 2516:Theclustercontainsfourredgiantsbutonly 2 2 2 2 2 2 2 2 2 2 2 2 1 2 2 2 2 2 2 2 2 1 2 2 2 2 2 2 1 2 2 1 167401A 223047 222820 222574 219135 217476 216206 211300 209750 205935 207089 204667 202109 201409 199997 198590 193721 193370 192676 192713 194093 190113 169337 187306 167299 186962 167203 185956 184624 185756 185016 HD 4.50 4.94 4.50 4.2V 2.56 2.59 7.20 5.66 5.70 2.82 4.65 5.92 6.66 6.53 2.00 5.21 4.90 4.72 7.36 3.76 6.00 7.05 6.35 6.06 7.47 7.02 4.00 4.13 6.60 7.20 9*24 0.375 0.545 0.620 0.279 0.405 0.400 0.370 0.310 0.473 0.374 0.270 0.216 0.301 0.274 0.262 0.222 0.465 0.272 0.365 0.334 0.565 0.325 0.370 0.346 0.565 0.330 0.342 0.342 0.246 0.296 0?446 R-I 2 2 3 2 2 2 2 1 2 1 1 1 3 2 2 2 2 2 3 2 2 1 1 2 1 1 2 1 3 1 1 2186 1994AJ 107.2184E 2187 O.J.EGGEN:GKGIANTSANDSUPERGIANTS -18.2032 67243A 61713A 88069 88056 87951 87323 85530 85205 87109 864 53 84610 84 533 84341 83609 83111 82415 81949 80128 83898 83657 82155 76340 65297 64571 63170 61561 79739 79737 76006 75586 70385 69444 68111 64558 63609 62236 72125 71181 66678 49778 © American Astronomical Society • 70046 59367 56695 56186 52220 49367 49334 58134 55612 51956 50372 49102 49091 47209 45829 44812 43497 42456 41701 35949 25749 24107 HD 18145 17005 15589 13640 12409 6446 db 8.54 8.67 9.12 8.12 7.88 8.76 8.18 9.37 7.48 8.36 9.22 9.38 8.31 8.31 8.73 9.68 7.44 9.47 8.05 9.31 7.26 7.76 8.66 8.82 8.13 9.70 7.63 8.06 9.32 8.62 6.57 8.30 8.92 6.96 8.68 8.48 8.99 8.04 9.72 8.22 9.44 8.62 7.28 9.60 8.25 8.74 7.40 8.54 7.49 7.28 7.35 8.30: 6.90 9.36 9.37 90.8 7.26 7.32 7.73 7.95 7.08 "48 781 1.151 1.172 1.150 1.224 1.312 1.104 1.236 1.196 1.325 1.235 1.119 1.159 1.229 1.331 1.258 1.200 1.401 1.283 1.263 1.130 1.334 1.132 0.126 1.059 1.222 1.258 1.155 1.072 1.263 1.206 1.260 1.286 1.254 1.298 1.126 1.274 1.153 1.180 1.242 1.178 1.084 1.184 1.211 1.078 1.134 1.104 1.003 1.261 1.124 1.208 1.267 1.270 1.234 1.404 1.186 1.481 1.237 0.955 1.407 1.199: 1.168 45-48 1.227 1.200 1.114 1.249 1.150 1.245 1.330 1?358 l 0.666 0.691 0.719 0.786 0.930 0.656 0.839 0.827 0.882 0.989 0.986 0.878 0.902 0.761 0.935 0.681 0.900 0.611 0.806 0.811 0.845 0.653 0.917 0.539 0.909 0.503 0.869 0.878 0.711 0.839 0.827 0.863 0.791 0.835 0.825 0.829 0.719 0.616 0.899 0.887 0.783 0.630 0.537 0.688 0.554 0.460 0.637 0.829 0.992 0.595 0.891 0.764 0.852 0.842 1.246 0.961: 0.824 1.023 1.078 0.439 1.115 0.953 0.887 0.676 0.769 0.996 42-45 1.004 1.055 l?023 0.122 0.139 0.135 0.172 0.352 0.102 0.263 0.276 0.358 0.316 0.348 0.298 0.288 0.120 0.302 0.104 0.162 0.237 0.329 0.182 0.180 0.105 0.083 0.236 0.296 0.254 0.269 0.103 0.104 0.087 0.212 0.225 0.295 0.196 0.235 0.264 0.182 0.118 0.220 0.118 0.113 0.148 0.229 0.074 0.120 0.336 0.333 0.127 0.108 0.320 0.205 0.220 0.168 0.326 0.269 0.262 0.440 0.390 0.273 0.067 0.315 0.290 0.089 0.237 0.212 0.375 0.130 0?149 41-42 Table 2.PreviouslyunpublishedDDOphotometry. 2.4.3 6.6.5 2.4.6 4.0.0 0.1.4 2.0.1 2.4.3 2.2. 6.4. 2.2. 0.1.0 2.1. 1.3.1 3.5.2 3.2.2 1.1.2 1.0.0 3.4.1 2.4.1 2.1.3 1.2.1 1.1.3 1.0.0 1.0. 2.3.3 2.0. 3 4.3.2 0.0.0 2.3.1 2.0.1 1.1.3 3.2.2 0.2.1 0.0.1 2.2.2 0.1.3 2.2.1 3.1.0 0.0.3 3.4.0 0.3.0 3.2.4 2.2.4 0.3.1 5.1.3 3.3.0 3.1.1 1.0. 3 1.2.3 1.0. 4 1.0.2 1.0. 2 3.4.5 3.0. 0 6.3.3 0.1.1 1.1.1 6.2.0 1.4.0 5.1.1 0.1.5 6.2.6 3.3.1 1.3.3 Provided bythe NASA Astrophysics Data System 2 2 2 2 2 2 2 3 2 2 2 2 2 2 2 2 3 4 3 2 2 2 3 2 2 2 2 2 2 2 1 3 2 2 2 3 2 2 2 2 2 2 2 2 2 1 2 2 2 2 2 2 2 2 3 2 2 1 2 2 2 2 2 1 2 2 1 2 3 146218 147225 146525 146148 145336 145302 144338 143119 143084 142822 142811 142644 142584 142277 141120 139915 137465 136636 136537 136505 136474 136456 135551 134704 132594 124196 114533 126713 125809 121936 120537 118520 117341 114756 120432 117000 112782 113190 111315 110483 106282 111790 107285 106961 104857 104096 101314 105136 104215 103225 100137 94313 99154 96782 97189 96746 95393 94584 93607 91629 90301 89925 89874 89805 89373 89175 88756 HD 88495 88092 10.22 6.68 6.40 8.72 9.63 7.97 9.88 7.95 7.98 9.16 9.46 7.14 6.06 6.93 7.90 7.76 6.06 6.52 9.07 8.36 7.24 8.56 8.26 7.14 6.44 6.77 6.69 8.92 8.38 9.27 6.50 6.24 8.56 8.61 6.66 7.23 9.41 6.61 8.90 8.30 8.24 9.82 8.39 7.65 5.98 8.14 6.75 8.50 6.34 6.38 8.66 8.68 9.12 7.58 8.65 8.79 9.16 7.66 7.61 8.42 7.70 7.59 6.96 6.56 8.09 6.39 6.60 7.94 "48 7*?92 1.417 1.257 1.244 1.276 1.222 1.373 1.418 1.201 1.284 1.243 1.276 1.178 1.247 1.337 1.295 1.214 1.264 1.236 1.264 1.275 1.278 1.219 1.263 V. 166 1.156 1.333 1.241 1.196 1.255 1.209 1.217 1.364 1.220 1.232 1.306 1.196 1.298 1.334 1.244 1.251 1.250 1.145 1.250 1.296 1.263 1.292 1.215 1.232 1.298 1.300 1.390 1.236 1.166 1.204 1.374 1.266 1.163 1.276 1.353 1.105 1.112 45-48 1.144 1.138 1.449 1.250 1.351 1.350 1.152 1.132 0.816 0.819 0.868 0.860 0.833 0.633 0.997 0.767 0.895 0.905 1.048 0.693 0.777 0.783 0.741 0.611 0.916 0.666 0.674 1.041 0.849 0.836 0.906 0.762 0.723 0.891 0.916 0.849 0.773 0.893 0.893 0.550 0.941 0.753 0.875 0.915 0.715 0.638 0.659 0.660 0.927 0.626 0.777 0.655 0.871 0.766 0.916 0.978 0.900 0.864 0.672 0.792 0.831 0.701 0.745 0.657 0.941 0.627 0.607 0.991 0.611 0.665 0.649 0.956 0.993 0.663 0^*632 42-45 1.176 1.064 0.334 0.215 0.280 0.264 0.264 0.205 0.193 0.389 0.376 0.215 0.282 0.275 0.276 0.227 0.171 0.151 0.228 0.323 0.244 0.262 0.284 0.239 0.392 0.156 0.079 0.294 0.332 0.264 0.172 0.267 0.142 0.319 0.067 0.337 0.164 0.357 0.359 0.234 0.240 0.269 0.364 0.099 0.159 0.250 0.255 0.307 0.367 0.310 0.264 0.170 0.260 0.196 0.166 0.220 0.249 0.134 0.308 0.206 0.375 0.104 0.119 0.122 0.111 0.377 0.366 0.291 0.373 0.207 O^ll? 41-42 3.7.7 4.2.2 2.5.0 5.3.5 0.2.5 0.0.3 6.5.3 1.1.1 3.2.2 0.4.6 1.0.1 6.3.0 5.1.1 3.7.4 1.1.4 1.0.6 0.2.0 8.4.7 4.3.2 7.4.2 6.7.7 3.3.0 2.4.7 5.5.6 5.5.3 4.0. 2 1.4.1 1.0. 1 7.7.1 4.3.3 0.2.5 2.3.1 5.1.5 3.7.4 0.0.1 2.1.2 1.4.3 1.2.4 1.0.2 1.0. 2 4.4.1 0 0.1 0.0.2 1.1.2 2.4.0 2.2.4 1.1.0 1.1.2 3.1.0 0.1.2 1.1.2 3.2.0 6.4.3 1.0. 5 1.1.3 1.0.1 1.1.1 2187 2 2 2 2 2 2 2 2 2 1 1 1 4 2 2 2 1 2 2 2 1 2 1 1 2 2 1 2 2 2 2 2 2 2 2 1 1 2 2 2 2 2 2 2 2 1 2 1 3 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 2 5 1994AJ 107.2184E component isoftypeA3Vandtheluminosityreddening velocity as170820andUSgrbutthemodulusreddening P=2323 d(Mermilliodetal.1987).Ifthecompanionisof are fromthe4colorandH/3photometry(Eggen1989a). and withacommonpropermotionradialvelocity.TheB indicate apositioninfrontofthecluster. from 4colorphotometry.HD170886hasthesameradial combined lightandexplaintheabnormallylowluminosity etry forHD170820.Thisstarisaspectroscopicbinary, The starmembersinTables4and5arefromLynga(1962). the distanceofhalfdozenBtypestarsmentionedabove. early typeitcouldvitiatetheultravioletcomponentof in theclustergiveamodulusof8.95±0.35mag(Eggen 1988) andthisagreeswiththatobtainedfromDDOphotom- 2188 O.J.EGGEN:GKGIANTSANDSUPERGIANTS -64.1193 ADS 6988:HR3475/4=iotaCnc,separatedby30arcsec M25: ThisclustercontainstheCepheidUSgr.TheBstars © American Astronomical Society • Provided by the NASA Astrophysics Data System 1553029 6724318 +55.2.5 192713 160529 153523 148586 131246 128428 LSS3970 14855 98386 93807 91269 66678 66604 166148 165633 165462 164774 163413 163020 162585 161388 160706 159633 158476 157919 156768 157549 154813 153892 153639 153573 153515 152501 151856 151824 150675 148586 HD Table 3.Correctionsto1,PaperI. 11.06 n 8.19 6.39 6.80 7.61 8.86 7.44 9.04 7.38 9.13 6.76 6.36 6.36 9.00 6.28 8.10 7.28 7.54 8.72 8.51 8.36 8.36 9.00 8?38 7.56 *8 1.166 1.289 1.194 1.426 1.196 1.454 1.382 1.439 1.535 1.314 1.124 1.231 1.411 1.217 1.322 1.546 1.253 1.344 1.267 1.261 1.268 1.302 1.553 1.259 1^093 45-48 b-y -0.628 b-y -0.963 M -0.391 C -0.339 M -0.224 Ci -0.015 b-y -0.29 C -0.290 Cj -0.672 x x x l V -6.88 -64.1993 V -65V - 0.267 1553029 6724318 +55.2.5 - 0.619 153523 14855 66678 66604 0.746 0.813 0.761 0.742 0.930 1.023 0.889 1.119 1.005 0.638 0.860 0.979 1.104 0.827 0.951 0.840 0.983 0.953 0.706 0.782 0.797 0.898 O^OS 1.013 1.076 42-45 0.181 0.165 0.136 0.399 0.172 0.386 0.307 0.231 0.438 0.284 0.114 0.286 0.373 0.268 0.304 0.124 0.262 0.363 0.179 0.151 0.198 0.514 0.364 0.292 0?100 41-42 LSS 3029 -64.1943 5.6.0 3.3.0 0.0.1 2.0. 0 2.0. 3 4.3.2 +55.215 4.1.2 2.0.2 1.2.0 153573 114855 67243A 0.353 0.286 0.637 0.274 0.315 0.841 0.290 0.267 0.363 0.614 0.463 66604 66678 6.08 6.65 Table 2.(continued) 2 2 1 2 2 2 2 2 1 2 1 2 1 1 1 1 1 1 1 1 1 1 1 1 1 Æ—/ atthesamephasearefrom Eggen(1985).Theredden- city anduncertaintyoftheDDO data,thisisreassuring 4 colorphotometry(Eggen1985) and,consideringthescar- ing valuesfromEq.(10)give a meandifferenceof-0.011 The availableDDOphotometryisphasedwith(UBVRÏ)pho- agreement. tometry (Eggen1983)andthevaluesof(45—48)(42 V340 Nor1.054 VY Car1.277 T Mon1.432 SV Mon1.180 RS Pup1.617 tometry fortheseLPC; range discussedhere.Dean(1987)haspublishedDDOpho- heids (LPC,P>10d)whichliejustoutsidethetemperature test ofthereddeningvaluesisavailableforlongperiodCep- cluster orbinarymembersisGKstars-BA=-0.04 the BGandSGinTable4thatofaccompanying tant andhasacommonpropermotionwiththeredgiant. though thecompanion,anA2Vstar,hasavelocityrangeof agree wellwiththosefortheearlytypestars.Anadditional at least40km/s. and showacommonpropermotionradialvelocity,al- ±0.016 magwhencomparedwith thevaluesobtainedfrom -45) readatquarterphase(0?25)arelisted.Thevaluesof ±0.14 mag.AlsothereddeningdeterminationsfromEq.(10) LPC igp 0 ADS 15764:Thefaintcompanion,A3V,is29arcsecdis- HR 3300AB:Thecomponentsareseparatedby86arcsec The agreementbetweenthemeanmodulusobtainedfor 201409 199997 196590 189337 187308 187203 184624 184591 183791 183416 178937 177483 174349 173568 173388 172508 172365 170886 170457 170053 169660 168356 168245 167506 HD 10.26 8.00 6.94 7.60 7.24 6.96 7.86 8.55 8.10 7.66 8.30 7.00 7.82 9.00 8.38 8.41 6.79 7.56 7.60 7.88 7.80 8.02 7.80 7.14 "48 p-1 45-48 0^565 1^440 0.450 1.262 0.385 1.280 0.425 1.340 0.420 1.350 1.160 1.126 1.162 1.235 1.202 1.233 1.031 1.107 1.234 1.164 1.201 1.202 1.391 1.427 1.562 1.551 1.100 1.380 1.344 1.387 1.352 1.190 1.210 1^253 45-48 0.800 0.675 0.821 0.639 0.900 0.678 0.957 0.731 0.757 0.609 0.693 0.885 42-45 0.604 1.251 1.008 0.908 1.069 1.192 0.967 0.932 0.700 0^925 0^190 0.685 0*903 1.091 42-45 0.716 0.107 0.760 0.129 0.830 0.147 0.850 0.145 Kb-y) ¿(45—48) DDO(4C) 0.214 0.141 0.260 0.236 0.179 0.142 0.177 0.162 0.163 0.062 0.126 0.174 0.297 0.349 0.362 0.410 0.098 0.229 0.363 0.334 0.306 0.150 0.171 0*221 41-42 0^321 0^349 0.242 0.254 0.188 0.196 0.200 0.219 0.182 0.171 2.6.1 1.3.3 4.2.2 1.0.2 7.7.3 2.4.4 2.0.3 1.4.0 4.5.2 7.6.2 3.3.2 8.6.2 0.6.0 1.3.2 0.3.0 3.2.1 1.1.5 2188 2 2 2 2 2 1 2 2 1 2 1 1 1 2 1 2 2 1 2 2 2 2 2 2 1994AJ 107.2184E 2189 O.J.EGGEN:GKGIANTSANDSUPERGIANTS ter starsarerepresentedbyisochronesfromalittleover three clustersisshowninFig.1wheretheisochronesrepre- shoot atthecores(Bertellietal1992).Thebulkofclus- sent stellarmodelsofsolarcompositionandconvectiveover- isochrones arebasedonstellarmodels, withovershootatthecore. Fig. 1.Color-luminosityarrayforthree clusterswithbrightgiants.The The color-luminosityarrayforthebrightstarsin © American Astronomical Society • Provided by the NASA Astrophysics Data System ADS 6988 M2 5 ADS 15764 NGC 3114 HR 7300AB NGC 2516 B stars NGC 2287 B stars BA stars BA stars0.018±0.015 HR 3076 211300B 0.033 211300A 0.033 49068 49212 49105 180243 0.035 180262 0.014 170820 170886 mean No. HD 74738 0.019 74739 0.024 mean 184 159 119 0.360 0.357 0.293 osai 0.074 0.084 0.090 0.024 0?035 0.060 0.075 0.072 Q^Q39 0.014 E(b-y) (R-I)(C)S(45-48)i[u-b] 0B ±0.024 ±0.006 ±0.020 0.320 0.296 0.326 0.327 0.313 0.1750.001 0.342 0.351 0.358 0?403 0.321 0.373 0.339 0.300-0.018 ß -2.882 ß -2.910 Table 4.Clustersandwidebinaries. 0.175 - 2.905 0.212 -0.010 0.078 0.022 0.164 0.202 0.346 0.244 0.246 0?266 0.107 0.044 0.086 0.212 0.036 0.055 0.047 0.021 0.1216.36 0®017 0.004 0.003 Eggen (1981) (Eggen 1988) (Table 5) (Eggen andIben1991) 8 M=-3.65 mag,inthecluster NGC2602(Eggen&Iben with theenhanceducausingadiminished[u-b],butthis blocking inthevisualregion.Thelatterisprobablycase, ultraviolet fluxbecauseofbackwarmingeffectstheline bers, orthedominatepeculiarity,Ap(si),iscreatingenhanced liar(si) objectsandarelabeled“p”inthefigure.Thesestars 4X10 yrtoalittlelessthan3X10yr,exceptforclumpof brightest starinNGC2516,thereisnoquestionthatitap- not knowntobeApstars.Forexample,Nos.13,14,and136 leaves unexplainedthefiftypercentofobjectsthatare are eitheryoungerthanthebulkofotherclustermem- tween 0and-1mag.Onehalfoftheselaterstarsarepecu- in NGC3114(Table4)areB9IVstarsandAaphotometry stars with[u-b]between0.75and0.95magMbe- binary withaperiodof1.8dand averycomplexspectrum pears youngerthantheotherclustermembersandthisis objects, doesnotisolatethelasttwostars.Incaseof members asHR3147inFig. 1. 6Carisaspectroscopic identical star,6Car,with [«-£>] =0.011magand matter exchangewithaveryclose companion.Analmost almost certainlybecauseofdelayedevolutioncausedby (Maitzen etal1988),whichisdesignedtodistinguishsuch 1988, Fig.8)bearsthesame relation totheothercluster v v 0.081 0.025 0.025 0.055 0.169 0.138 0.038 0.072 O^OSO 5.49 6.50 8.18 8.32 7.56 5.86 -3.19(-0.95)9.04 5.76 -2.43-1.97(7.96) 7.47 7.37 5.94 3.92 7.66 7.68 7?30 , -2.22 -1.85 -2.30 -0.94 -0.95 -0.97 -1.90 -1.86 -1.87 -1.64 -2?17 DDO +1.39 +1.30 +1.32 -0.87 -0.97 -0.94 -1.90 -1.29 -1.90 -1.46 -1.56 -1?96 4C MOD 4.88 6.26 6.40 6.90 8.95 6.93 5.18 9.70 9.60 9.53 9.75 9.47 8.32 8.24 9.35 9.32 9.32 9.28 9?36 2189 1994AJ 107.2184E 9 provide anorbitalsolution. with nitrogenenhancementandcarbondeficiency.Thespec- radial velocityhasnotbeenfollowedconsistentlyenoughto trum ofHR3147(V3741Car)intheclusterNGC2516(Fig. The propermotionsareontheFK5system.Usingstars 2190 O.J.EGGEN:GKGIANTSANDSUPERGIANTS motions amongstrecentlyformed stars,althoughsuchgroup, The valuesfortheBGandSG may beinfluencedbygroup plane. Perhapsthebestestimateof(U,V)velocity The consistentvalueof—7km/sforWprobablyrepresents GK(III) BG+SG served classificationsaremainlyfromKeenan&McNeil estimates arelistedinTable5asSp.T.(COMP).Theob- tral typesandluminosityclasstheresultingphotometric classified byKeenan&McNeil(1989)asstandards,the from Eq.(10)andtheluminositiesEqs.(12)(13). of theyoungdiskstarsingeneral. or superclustermotions,canalso influencethemeanvalues young diskstars,age1to2X10 yr,or(—17.5,+15)km/s. the +7km/svelocityofSunwithrespecttogalactic GK(III) (1989) andtheBrightStarCatalogue(Hoffleit1982).The apparent motionsarelistedinTable6.Thereddenings 1) isstrikinglysimilartothatof6Car,althoughthevariable Sun withrespecttothecenter of restisobtainedfromthe [w —b],{R—I)qgridinFig.2hasbeencalibratedforspec- 2. REDDENING,LUMINOSITY,ANDSPACEMOTIONOFTHE Ninety-nine BGandSGwithavailablephotometry © American Astronomical Society • Provided by the NASA Astrophysics Data System NEAREST BRIGHTGIANTSANDSUPERGIANTS Young disk Young disk Old disk mean No. 183 149 136 102 61 16 18 14 13 11 4 9 6 3 ±0.006 220 350 0.060 0.060 0,018 0.070 0.065 0.061 0.052 0.071 0.058 0.055 0.060 0.058 E(b-y) 93 N Table 5.PhotometryofearlytypestarsinNGC3114(Schmidt1982). 9 9 8 2- 10X yr 1- 2X10 yr ^5X10 yr 0.776 0.856 0.816 0.861 0.924 0.853 0.897 0.800 1.080 0®929 1.022 1.126 1.000 1.085 Age [u-b] 9.56 9.08 8.22 9.03 8.81 9.00 9.46 9.38 8.93 8.46 8.00 8.06 7.58 7?49 + 17.6±18.4 + 10.6±12.3 J +3.6 ±38.4 U a 8 8 9 vective overshootatthecores(Bertellietal1992).Themost The isochronesarefromsolarabundancemodelswithcon- nosity isusedtoconstructthecolor-luminosityarrayofFig. mean differenceinthecomputedluminositiesisM(DDO) values ofU,V,andWinTable5,comparedwiththosefor tion ofgalacticrotation,andtheenclosedregionisdo- to thatoftheHyades. to 5X10yrinstandardmodelsor,roughly,theageofMil 5X10 yrandtheupperluminositylimitofclassIIIstarsat notable featureofFig.3isthescarcitystarsbetween 3 wherethestarsofTable5arerepresentedbyclearcircles. the completesamplesofHRstarsinyoungdiskandold main oftheyoungdiskstars(e.g.,Eggen1989c).Themean respectively, awayfromthegalacticcenterandindirec- and SGinthe(U,V)plane,whereUVaredirected, disk populations(Eggen1993),are; tallicity index,M,issensitiveto luminosity(gravity)effects so thevaluesforBGandSG starsneednormalization. [Fe/H] valuesderivedfromhigh dispersionspectroscopy disk stars(luminosityclassIII) giveadispersionofabout 10 yr(Eggen1994).Thisagespanisequivalenttoabout2.5 (MeWilliam 1990).Modelatmospheres indicatethattheme- -My(4C) =-0.04±0.20(o-)mag.Theweighedmeanlumi- v ±0.10 dex(Eggen1993,1994) whencomparedwiththe 1 Figure 4(clearcircles)showsthedistributionofBG The valuesofP[Fe/H]derivedfromEq.(7)forsome100 (-0.14) (-0.24) (-0.32) -0.27 -1.52 -0.61 -0.96 -1.47 -0.60 -1.04 -1.59 -1.68 -1.90 -2?13 ±0.21 ±31 9.70 9.97 9.93 9.74 9.64 9.41 9.96 9.59 9.74 9.48 9?62 -20.2 ±27.5 -14.8 ±8.4 -13.2 ±8.8 MOD V a 3. METALLICITY B8(S1) B8(Si) B9 IV B9 IV B9 IV B9(S1) B9 V B9 III B3 V B9 IV B9 III B8 III Sp.T. -6.9 ±13.9 -7.7 ±8.8 -6.7 ±17.3 W a 2190 o oo r" 2191 © American Astronomical Society • Provided by the NASA Astrophysics Data System O. J.EGGEN:GKGIANTSANDSUPERGIANTS

Table 6. Reddening, luminosity, and space motion of BG and SG near the Sun. ï a •O «0 À J >1 D *1 s o < o < * (0 i > , > l , , ,>r cfl0 ^3oooooo©oo©ododoo©oooo©oooooooooooooo ^OOOOOOOO 000*0 0000000000000000000000 _tA K»fO ^>ooodddoodododddodddo©©do©oo 00000000 ^4 ©*-©•—©©«-■©•“»-©©aÍo^-aJaÍ^-w-^'-aÍajkÍ«“*”^©^'«“©»"»“©©*" ioo»->#»orw'OrsicONí'>»iAT->jrKS>#Or-r\ih*.^fOcg(NOrO'0&‘U^^K>^X¡^-rO^N. rsi*sf0‘0*-00'0*-^'000©00‘00'©0i>jfw^©000©>t^^0©0'00^ ©»XKÍ©©»nuíoÓsrrsí^fl¿Krgo<>©«0'«ííO>#©*-«©©c^KO»r>íMS.<>j>»-N.© 'OvA®>r'0©0'^*~N-0'0©U^^O‘>4N-00>fl0©©i/>'V©'0lAf^©CgK»O©O<>í0>'0«'-'* ©'^'*0‘©©'0©®OfM'0©0*»/>©ir*>0 »- i.r-*-•-I•“rsir-.-*-íO+ÍM«-^-4-»-'• '>#fl0»/>©Wi©»A'*C0©^'O«-©r-K»mO'«*©N*©©K«0«0tf>*#K>ÍM*-'*©'0'*'0CM r— rg^(TtmKKOOCgfOKI^O«0©©e-»-«-r-r-K» S>r K.0*>f'*K'0S}O'0’0*-rgN.KN.o>r^>t'#u-»K»to>r^Noflpoo>poo5> £ fA©- <>ian.okai*-aj brO‘^A4©fxKIAJ(APArA©*-(ArA©0>(A«>rxAJ»-N»Aí©j-© Ö = si§llisil2liiil$l^.i5ÍSs^S£Slliisll PO _AJ(A^V,.i^KifO«r-fO•^’O*"“ ♦-^0‘W^»X0‘»0©Kh.^i*/\^©iMS.-s#OO>iN.©©»-r>J»/>'00k©'0^K.^*-(M©»- «>iJ•- sssssaassssssíisssssssssswsssá^^s^ssss ^AJ0r-Ajrgp0Ar¡J^*-KjA.^ OOOOOOOOOOOOOOOOOOOOOOOOOOO© OOOOOOOO ^'AJAIAJíA*-»“PA*-fOA4AjAJ>^AJfOfO^AjrOAJAJAIvIfOfOAJpn < AJAJ*-AJAJ»-AIK> l^hs(AlA©s#*-©(A©©rA(AA4<>*-ÇA©0;©srA-^«îAs£©© o§Íl§§§§Í8S§83gSS©SS©§©SgSág8 S8© 9"(A©>íK«-fOíO^©«KtAi>»POO>o«©orx>>t«>*-05n S»A©r-0‘s**-U"»AJ©«(AA4*-»AQAJAJM"»'0srA4K©A4m*A*-í^©'i;:K>*Arx£-|A (A ©•AJo*'s*iI.rg^AIc-w«-K»Oiw»»t PAX.PAÄ'X •AJ*-AJ©«->^K>s#»-fO*-A.^-AJ*-X.iAX.V»X.>.kA©r-«OOii»-«-»As# ©OOOOOOOO©*— 0000000000000^-000000000000 ssssssssfcssssáássKssííRisssage^írgcíSSás äS?83K&?3338S3S$t:S::S£ä5ä3$ICS?;Q3!o£3:S8£ 0O«->»'0fxf00‘0'««-0>'— «AvTAJ'OO'OOOfA —•—flOOO——•OO-^OO'-'OO““ —0®0”“®0°00"" x. iX..KI'OAiPAX.O'xx.'^x.v.Ox.Ox.O•x.. ♦ ♦♦♦♦♦ ; ; « IlI•lllll••• ||||||||||||•|||»«••ll•|lll• •I« 00 ,l '0000000000000©00©0000000000000000000 K Kíirt«LA'0*-'ON*KSOQ»NÍ©PA^iA(APOlAA'0(A©©©AJ»í'(A©(A»A(AlAsí© PA0^4AsíAjKN.N»©(AA4(AIAA4>0«AO^K.©(A'^AI©r-AJ»-N.K>©lA©>K>Kí©«^ «2jQ.-!QQJc)*~*-OOAJO«— rAAir-*-c-c-AJAJ>r^-^-PAir-T-©0©©»-A4 r , • *-«-*-♦i*-ínj^POfOsÍNÍfOfAK>Ai^POPAPAAIK»rgpAA4AJK|A4AJAJ»A ©«rxfA«(A0^©5‘>t©KAJrAA4(A«-0‘K>(A«^&*©0^fg>fx^->©0'2£ © *-X» ; AJ «— (A©^ • AJIAAi©(AOOK>»^>T>»©Kl»-© r- T-Í-Í-^»-rsicgfNjrsifMfMrgrgr\j<\gfMrgrargpvj — -^~»-•>.>.»-'o.'s.O‘©K's.s v ♦ (M •-r-fAIK> r-^ rJfOrgrsj ♦ AJlAlA^O^g^r' iA>í^”>í©©(A©© j IA«0O>••AJ ♦ ♦ «f I «0 o 2191 oo 2192 O.J.EGGEN:GKGIANTSANDSUPERGIANTS © American Astronomical Society

Table 6. (continued) u jO D E • '8 Ï — < >C A'C xj ms.fx.00 0000000000000000000000000000000000000 OÖO«— Ö000000000*-000000*-«—«—00*“00*— 00»—00«—o ^^^x^^K>egKíx»x»egxíegK»»-meg>íexfO'OfnN-©xíoop»*nom^ocoo«-ir» OCO'Ooegror-'O«—0.>i>0'ceg©c0w^vr\oegoooooeg'00000egr-'>roeg'0 KjfomegegKiKiegKixífnmmmmrofommegKiegfomKiKiegí irNOx»cûÇ^ego^r^o»-70»-egroooof«-^.>oao*—•-»-xi’O'r ' IT» ©,._^ 0000000000000000000000000000000000000 »- ©i 00000000000000000000000000000 megmegegegeg^-eg^egegegnjmegegegxiegmv-egr-egm^egm ••-eg 3?;§8SRS8P!gS53S^3S!5S8fít;S$ÍS$aí?¡ 83SÔSÎ o © d ^í}QK)ííí8SSlSSS©S-^8S^^ÍSaíQS&íe¡I^Sííí:í .2^ •»•£Nt'-K)'-op^'ONx*Kxrigo.tn«*©inoOinK*«-OKt'0'-Kx*o.iAO'0«- meg fO 00 ■O xt »-•-egeg»-r-o©»-rgo©o*“i-«-©*-egr-egr-egrgT-*-*-eg«- gfOfoeg«04njN|x£««-KO»K.g^i\j©peg^o»opKjNaooO‘tr-»Oxf oro©eg »-r-egeg*-»-*-©r-eg©©«»-*“*-r-*-©eg»-eg»^egeg*^*^*^e4*^*^T*^»^r^ !^ S^oOGO«~i/N'Oxtoo«~xj'^'flogrx-oO'Or~oOxfegxOC^^T-o^*'Oy>ro©xfr>>o K*- eg *>0N»rgK00'000xrrg©r->c0'OK>*-© mcg«-'0'0xtx#ir(0 o*^^KiOi>JO*»Ahxxr©*-rsim©'OflO»o©o© uegoO»O••©••©»xiON.h.rg© ír" K>U^0*rgK>fl0'0ir\KN.0‘0»N»K>KrMOO«0••00O‘'OxtN»00 w >*. « iNiirsjrg-f*-iM*-iiiMrjr-«-*-i»-r-*-psj •rj>ojieur-■♦ K.tx.^O>rO^OxfoOforgxTOoOiOxrxroooo>OOco ••*•o■•K»rgo»Ooo«O>»•n*xt OrorgO''ONxxfxí-oo»hxO‘vi'^Pv» ♦N>%rrsj>roo o*— »“»—»“fNírvifOKt>í>tU^U*»V/>^'O'O'0^'*«ílTk'OÍOCS»"'jFl/^4/>n-.0OQr-r- K<\iN*N.oO«NivrtON-oN*-N*vrNcdg»-N-0'r-flú cSro^-ooo^rsi^-st^f^arocoo «-^-«-1 .>*-♦i,rj• OíNj>oos.r-r-fMT-oroO‘'0'OeofvjcooO'^^^«o^”K»ooo^Kr»írg»oK>flO ♦ ♦♦♦44.4.4.4.4.+K>4>ill.••• ; — o0—oOoOflOoooOoOoOoOcO—oooooo—OO»-«•—o0oo*~*o0fl0—•■“•OO*—®flOflO « -O—ASi-I-,a • •iliti+ • ••«.o»*» • •••••••••••••«•••••4000* _.tco»no«-»-m>Kihx*->rmmmm'Oeg«-oN.^^Oxioo»m©r-N.egm< »AK*-»-io>»AM«o>«>K>0‘egN.r-ie\^K^oK.?Nj»nrviu>ir»Ä x»in«*-kíeg '0N-*-u^»-r-rx-egKt^‘0>©fO'0^»->^xrin^N.Ni-Kixrxregeg0>‘ •»0n.n-•-k> --- > ooooooooooooooooooooooooooo oo©ooooooo©ooooooooooooooo< 'Ominx^>OxrmxfKim'ömmxrir»'Omxr'Oxy%iknmxr0'0'Ommmx»fomx^uxi 3S2 88$íí&5|88$«St?iq2S5RJ55áS85!SSí5S5fí3!8 »OOOOOOOOOOOOOOOOOOOl ie.egr-©orvjegooo«>m«-©'>megmm4 e- eg•-©örg< 'pminewm©>f*-*-egx*m©‘Kx*Ki/>x*K4 -----©©< xto«»“*“ xiro*—ox^iA'O«ixtm«O<000eg•—»-o» • *i«O>0xteg>o*-exm^-xX1•- eg *-x#^«-xm/-x n ~ Provided bythe NASA Astrophysics Data System £> an&SiA > o¡r>•xt»o ‘ O'X^^N.oO’-.-_ xT vt•«í'>flT» i cos.eg*->*xf iloSáol ♦ rg»-•4-*-eg JQ -O.O~— xjegN.*- iN-'OX»eg»-s. jKifOKimegegegroegro >.eg>txt«>©0>.&>eg0»0 room©r-fx.egmo»^ j-x^egxO'Oxg-fo.-^ m «os.xj-o>oco «Û —«-X3 >0000 00 d o*do* r- eg m ©K 000000

♦19.9 -15.1 -3.1 643Ô G6/8 II G8 Ib-II 2192 oo 2193 © American Astronomical Society O. J.EGGEN:GKGIANTSANDSUPERGIANTS

Table 6. (continued) J À «0 2 o • o a < a. s « , ; N-OQ»-'í'Oote>TgDp0O' inin>ô'0>ô'ÔN-S-f^r^SoO' C0'ô'O'OK*O00N.0‘*-Klini T-mKi'Âvi'OoQ'ûvyrgvj--^ OhOinvfO'fO'O^f^mg^O' > ooooooooooooooooooooooooo fO oN*ineg o in org«- o r-m o oom pgr\joo<>S>»-oOflOrgf^mor^«- 'O'OKir-omON.rgoON* h*.coKmir»rgmo«-o>T'OflOoo^«“vn>o*rg>«K»flQ^- ooooooooooooooooooooooooo «- N*O* OOOOOOOOOOOO mroK>rgfOK»egrgK»egroK>roK»rOfOinK»fnKi>irgforgrg ooooooooooooooooooooooooo ooooooooooooooooooooooooo* k cgootfVN/os.N-ON.Qoorg ogmo^rooK.tnrM'OOj >o o«0>t1 tr> >0N*^r->r-u-k00'Or^*- ^»niO'0«0»-'0>0INIl/\ •-ooir\>^^0‘0'0»A*-Ko<\JO‘0oco«o oo >0< *-rgr-rgrg*-pg»-^-orvj«-pg»-*-fMr-*-fNipg^or-•-«— K> irv0*0'CN-»“ÍM>0>tO ^OO'O'O^rsik^OOOOOOOu^ *- IN-r-.<000fOK>Of\i«“rgIT\ p^N.fSlN.K>Q K)vf>^O'i'4'0Q0g>O*-«r-Kl«-ir»00vJrrsj| 00»“'ûr->OU^irk'ûinO'0^*'0*“r-0'Q'OOr-u*>'0«/»l r-oOOOONtOO»-K>mfO'0'0«“l isssss ßccßRRüfcissssäaasi OOlAflOr-r-aO '0»-'OcAOr-00'0öooOiOkr»«-4r>ooQocQ*-*“Of^wr>o«-N-ogNtK» — JD« w^wowooooowowowwwoouwooo« —. —Ü^3— irg>»rgrofM*-rgrg*-K>fMK>(\im>iOirorgK>>i*-cgrgÔ*-flÙ'ÔfvœS.rgt^\upK«O>C^00^^^íM'Or-rg>0O-oo ’»T'íkOOO>#K»*«rO‘^N- QfO(\J•-OJO*KI'O^iQ owovooawowowcjwwwoo^woooo i »n'v.'N.K»^s.'«s»rg*>*'N.•«>»^ Srvio>'í'írg^T-rn»-»“-^oroinKooo^'0 «-mm«-rgmK»»-r*“K>^o>rgN.rg^K>i'Org X) —« OOOOOOOOOOOOOOOO'-OOOO äfl0>Opr-fs»^rgK»»AONt0Q^^»-p»-O4p i»~kr»oor^o O*- Provided bythe NASA Astrophysics Data System >00000000«-»-00*-*“ »«-^rrgfnrg'ÇrgoOforgmr-o*- ‘>oe»'0'0in»-in»-o»-'»í'0foeg , )0‘»oe-rgoocQON.oOOrgo >inooinminoO'gom>í ‘«OflOOfO-sf>ö*mKK1'OK o 'OOOO'íM'OoOOO'OflOKí ■O00cgO'0S-'0O*-w\ ►- < ** +* O 8 o »-rg'Oór-e-oo >rm>Q r^rg*-«F->j'Ki«N.o«- K» O*-NÍ>tinN*« «-r-r-rgrgvtinm min^O O e->oinF~r* — U^C»Ofe* ^ ,--v,J.LT\F-íO QC»-a—a*- < U.Çcofe*CD ** *m'*r <- OlKO•«>0.1.11 Qb.C'DN VM«.u-^<0 J I 8 ? 8 01 (. « ■Sí 8 g“-S ^|¿ *>*>>> 2193 H1 oo^r 2194 O. J. EGGEN: GK GIANTS AND SUPERGIANTS 2194 h)

o>8 s 8 C

Fig. 2. Spectral type and luminosity class grid in the plane.

The mean correlations of (M^q and [u — b] with (R—I)0 lead to AíM^o^O.ÓTóAlw-fcl-O.OSO, giving for the luminosity corrected values of (M^q,

(M1)o = 0.676[w — h] — 0.50(i?—/)0 —0.427 (14)

and the values of (M1)0, observed and computed from Eq. (14), are listed in Table 7. Excluding the stars HD 42351, S 67249, 105138, and 223047, the mean difference is —0.004 3 ±0.014(cr) mag. Evidently the values of Mx are reflecting luminosity alone unless the BG and SG stars all have essen- tially the same metallicity, with a dispersion of only 0.04 dex. McWilliam (1990) and Luck & Bond (1989) have de- rived [Fe/H] values from high dispersion spectroscopy for the stars listed in Table 8 and they range from -0.38 to +0.38 dex.

V*a a. xu

»n«“ >0r- K>o. St>o > SK Or\i >0>i «-O 24-'O «O K «- K. «o ro «0ir» (\)— Ovi S-fO f>000 OK> O* *“•- ror- vr> K- o (\i

© American Astronomical Society Provided by the NASA Astrophysics Data System 1994AJ 107.2184E Fig. 4.TheGK(opencircles)andGO/3(closedstarsinthe{U,V) plane. Theoutlinedareaisthedomainofyoungdiskpopulation. 2195 O.J.EGGEN:GKGIANTSANDSUPERGIANTS 66190 67249 65699 64320 59669 58367 57478 55070 48329 47731 47475 45829 40808 54732 45416 42351 41380 41361 40733 52497 51043 50890 50877 76494 76219 50337 74739 73155 72561 69478 68752 67447 39775 39400 36597 14033 28100 71115 31767 27256 25877 21754 20894 12270 16307 16161 11763 9270 8267 5575 3712 © American Astronomical Society • Provided by the NASA Astrophysics Data System 0.561 0.635 0.478 0.528 0.542 0.400 0.362 0.428 0.411 0.361 0.443 0.505 0.812 0.415 0.341 0.715 0.468 0.499 0.727 0.439 0.464 0.534 0.422 0.576 0.641 0.455 0.673 0.691 0.533 0.401 0.408 0.623 0.460 0.373 0.420 0.689 0.419 0.384 0.359 0.434 0.509 0.435 0.326 0.444 0.316 0.362 0.511 0.399 0.429 0.450 0?544 0.500 0.617 0.467 0.530 0.530 0.386 0.363 0.405 0.434 0.372 0.820 0.448 0.490 0.310 0.711 0.468 0.504 0.739 0.584 0.684 0.421 0.443 0.550 0.450 0.428 0.409 0.692 0.701 0.556 0.414 0.420 0.633 0.714 0.394 0.465 0.376 0.424 0.418 0.382 0.444 0.514 0.448 0.336 0.457 0.314 0.365 0.528 0.398 0.428 0.443 0?568 COMP (Mi)o -J 1IL v -200 (+0.061) (-0.043) +0.018 +0.011 +0.012 +0.014 +0.023 +0.015 +0.004 +0.021 -0.002 +0.018 +0.005 +0.006 -0.001 -0.023 +0.001 -0.011 -0.005 -0.008 -0.019 -0.005 +0.002 +0.001 -0.012 -0.016 -0.019 -0.010 -0.023 -0.013 +0.001 +0.007 -0.006 •0.008 -0.025 -0.012 -0.010 -0.010 -0.023 -0.005 -0.003 -0.004 -0.013 -0.010 -0.005 -0.010 -0.013 -0.003 -0.017 -0?024 0.000 -0.086 -0.122 •0.042 -0.159 -0.099 -0.086 -0.188 -0.226 -0.173 -0.159 -0.233 -0.156 -0.134 -0.271 -0.170 -0.111 -0.011 -0.049 -0.152 -0.133 •0.184 -0.174 -0.184 -0.211 -0.190 -0.001 -0.140 -0.212 -0.185 -0.183 -0.210 -0.101 -0.189 -0.249 -0.169 -0.128 -0.273 -0.225 -0.197 -0.190-0.007 -0?069 -0T063-0?006 0.074 0.002 0.026 0.006 0.041 -0.038 -0.139 -0.162 -0.111 -0.180 -0.230 •0.186 -0.100 -0.162 -0.223 -0.154 -0.170 -0.244 -0.170 -0.124 -0.191 -0.070 -0.156 -0.051 -0.168 -0.189 -0.194 -0.196 -0.209 -0.179 -0.091 -0.192 -0.214 -0.015 -0.147 -0.193 -0.248 -0.131 -0.263 -0.240 -0.199 -0.163 0.125 0.012 0.008 0.025 0.004 0.050 (-0.051) +0.012 +0.017 +0.003 +0.014 +0.004 +0.013 +0.003 +0.014 +0.020 -0.004 +0.013 +0.002 +0.007 +0.014 +0.023 +0.001 +0.002 •0.008 +0.015 -0.010 +0.010 -0.027 -0.010 -0.016 +0.002 +0.014 +0.007 +0.002 +0.008 -0.019 +0.003 +0.016 +0.012 -0.009 -0.015 -0.001 -0.010 -0.010 -0.006 -0.001 -0.010 0.000 Table 7.Metallicityparametersforthestarsin5. +0.050 +0.086 +0.024 +0.040 +0.002 +0.018 +0.035 +0.008 +0.056 -0.003 -0.011 +0.061 +0.009 +0.003 -0.031 +0.014 +0.012 -0.028 -0.150 -0.010 -0.014 +0.024 -0.034 -0.038 -0.080 -0.020 -0.011 +0.011 +0?024 +0.008 -0.055 -0.018 +0.014 -0.004 -0.005 -0.010 -0.005 -0.050 -0.022 -0.053 -0.025 -0.049 -0.027 -0.002 -0.040 -0.010 -0.003 -0.004 0.000 0.000 P[Fe/H] (-0.87) +205 +0.31 +0.13 +0.14 +0.08 +0.06 +0.19 +0.16 -0.12 -0.17 -0.28 -0.11 -0.26 -0.03 -0.12 -0.17 -0.19 -0.05 •0.08 -0.07 -0.31 -0.52 -0.22 -0.29 -0.11 -0.18 -0.39 -0.21 -0.14 -0.06 -0.14 -0.17 -0.14 -0.37 -0.36 -0.25 -0.13 -0.17 -0.23 -0.39 -0.07 -0.14 -0.14 -0.25 -0.08 -0.32 -0.05 0.00 0.00 0.00 ACN +299 +122 +106 +134 +222 +178 +126 +896 +245 +193 +208 +562 +449 +170 +657 +230 +108 +161 +199 +110 +113 +166 +178 +212 +181 +140 +26 +69 +95 +93 +81 +36 +10 +44 +72 +50 -20 -82 +65 +66 +64 +73 +13 +38 +96 +92 +35 +91 -57 223047 216206 211053 port theresultsforMinthatthereislittleevidenceother 210807 210745 m inTable7giveO—C=+0.004±0.011(cr)mag,andsup- The observedandcomputed(luminositycorrected)valuesof 207089 which arenotinTable5butdiscussedthenextsection, Bond arecorrelatedwith(R—/), than aluminositysensitivityinm- 206854 206834 should notleadtoerrorsgreaterthanabout±0.2dexin the temperaturedifferencesarelessthanabout200°and and correlatingAm=m(obs)—m(comp)withADel tometry (Rufener1988),wheretheequivalentindicesto 199253 198700 [Fe/H]. exception ofthetwofainteststars,HD62236and151834, and thisisusedtocomputethevaluesinTable8.With 198308 ships ofmandDelwith(R-/)are and [u—b]aremDel,respectively.Themeanrelation- 185958 180809 180540 178345 173764 170866 174947 166063 164349 161664 =Del(obs)—Del (comp)gives 160635 159633 157819 150030 145544 141767 1 156768 150416 2 137465 131425 131246 128713 0 2 125809 118520 115004 111790 105138 2 102839 101570 20 2 93807 92449 85656 80126 79846 77912 77615 77020 The temperaturesadoptedbyMeWilliamandLuck log T=3.807-0.40(R-/)o(16) m= 1.95(jR—/)—0.770 Am =0.55ADelorm0.55Del-0.227(R-/) Del=3.95(R—/) —0.740, Most ofthestarsinTable7haveavailableGenevapho- e 20 20 0 0.474 0.442 0.428 0.333 0.647 0.638 0.524 0.495 0.514 0.613 0.516 0.457 0.413 0.485 0.512 0.438 0.363 0.424 0.594 0.511 0.583 0.519 0.469 0.442 0.475 0.426 0.495 0.436 0.429 0.555 0.460 0.536 0.437 0.488 0.470 0.491 0.579 0.424 0.627 0.410 0.617 0.406 0.404 0.426 0.513 0.477 -0.353. (15) 0.422 0.445 0.454 0.352 0.639 0.617 0.517 0.503 0.511 0.613 0.531 0.491 0.426 0.507 0.510 0.436 0.396 0.421 0.589 0.526 0.592 0.546 0.460 0.444 0.423 0.469 0.469 0.418 0.420 0.543 0.487 0.544 0.439 0.450 0.459 0.558 0.576 0.454 0.607 0.439 0.618 0.407 0.430 0.440 0.509 mean 0.463 COMP ͱÍ4) (-0.067) ±0.014 ♦0.008 +0.021 +0.005 +0.003 -0.004 -0.003 -0.026. -0.019 +0.002 +0.002 +0.003 -0.008 +0.005 +0.009 +0.003 -0.015 -0.033 +0.006 +0.026 -0.033 +0.018 +0.009 +0.012 -0.013 -0.022 -0.015 -0.009 -0.027 -0.002 +0.011 +0.003 -0.027 -0.008 +0.020 -0.002 +0.004 -0.002 -0.030 -0.029 -0.001 +0.014 -0.001 -0.026 -0.014 0.000 -0.210 -0.190 -0.157 -0.243 -0.042 -0.121 -0.108 -0.100 -0.021 -0.094 -0.135 -0.174 -0.086 -0.145 -0.229 -0.273 -0.158 -0.197 -0.039 -0.035 -0.127 -0.143 -0.154 -0.179 -0.200 -0.148 -0.223 -0.176 -0.106 -0.136 -0.195 -0.116 -0.148 -0.129 -0.099 -0.212 -0.033 -0.187 -0.023 -0.180 -0.175 0.041 -0.165 -0.120 -0.139 -0.215 -0.183 -0.158 -0.237 -0.044 -0.137 -0.118 -0.110 -0.034 -0.101 -0.129 -0.184 -0.106 -0.145 -0.205 -0.271 -0.177 -0.051 -0.170 -0.041 -0.133 -0.166 -0.209 -0.171 -0.180 -0.158 -0.231 -0.186 -0.116 -0.138 -0.197 -0.125 -0.162 -0.128 -0.099 -0.204 -0.046 -0.184 -0.190 0.064 -0.030 -0.173 -0.163 -0.136 -0.156 ±0.011 +0.004 +0.005 +0.001 +0.002 +0.016 +0.010 +0.010 +0.013 -0.007 •0.006 -0.023 +0.019 +0.007 +0.024 +0.012 +0.010 +0.020 +0.006 +0.023 +0.006 +0.026 +0.009 +0.010 +0.008 -0.006 -0.002 +0.010 +0.010 +0.002 -0.027 -0.008 +0.002 +0.009 +0.014 +0.013 +0.007 +0.010 -0.001 +0.016 +0.017 -0.008 -0.003 -0.002 -0.002 0.000 0.000 +0.027 +0.033 +0.049 -0.011 +0.050 -0.007 -0.035 -0.019 +0.025 -0.026 +0.011 +0.004 +0.044 +0.002 +0.012 -0.026 -0.060 +0.018 +0.050 +0.033 -0.011 -0.025 -0.064 +0.001 -0.012 -0.004 -0.064 +0.011 -0.030 +0.029 -0.015 -0.019 +0.023 +0.026 -0.028 +0.016 +0.004 +0.003 -0.007 -0.069 -0.005 -0.050 +0.014 -0.013 -0.018 0.000 ACN P[Fe/H) +0.02 +0.04 -0.18 -0.15 +0.12 +0.13 -0.22 -0.30 +0.01 -0.25 -0.25 +0.10 +0.01 -0.42 -0.18 -0.18 +0.13 +0.04 -0.06 -0.44 -0.10 -0.14 -0.27 -0.11 -0.44 -0.06 -0.03 -0.18 -0.12 +0.02 -0.21 •0.12 -0.06 +0.01 -0.26 -0.16 -0.46 -0.15 -0.32 -0.18 -0.21 -0.04 -0.10 -0.11 -0.05 ACN 0.00 -151 .-235 -114 -117 -145 -140 -133 -254 -381 -116 -149 -284 -106 -445 -243 -207 -132 -124 -229 -136 -152 -356 +57 +70 -226 +40 -138 -207 -116 +102 +63 -227 -70 -45 -90 -84 -73 -93 +11 -35 -90 -70 -31 -83 -33 -15 -41 2195 +6 1994AJ 107.2184E Luck &Bond(1989).PhotometryCatalogue(Rufener1988). Table 8.BGandSGobservedspectroscopicallybyMcWilliams(1990)9.FtypecommontoLuck&Bond(1989)theGeneva 2196 O.J.EGGEN:GKGIANTSANDSUPERGIANTS type objectsdiscussedinPaperII.Thereitwasfoundthat This relationwasbasedontenstarswith[Fe/H]between values of[Fe/H]fortenFtypeSGandBGderivedbyLuck presence ofthissensitivityintheFstars.Table9contains lower envelopeofthem,ßdiagramforallSGand Del arealsolisted.ThevaluesofSmderivedfromthe firm thelackofasensitivityintoheavyelementabun- fining starsshowadispersionof±0.09dex.Althoughthis stars, with[Fe/H]=-0.28dex(HD9973)and-0.64 indices oftheGenevaphotometrywereusedabovetocon- calibration cannotbeconsideredwellestablished,itappears 2.71 2.74 2™78 Catalogue (Rufener1988); BG starsinPaperIIthatarealsotheGenevaPhotometric & Bond(1989),andtheGenevaphotometricindicesm dance intheGstars,theycanalsobeusedtoconfirm difficult toquestionitsexistence.JustasthemandDel incorrectly printedas2.8A[M]+0.030 onpage1832ofPaperII. to, in the/3,Delplaneisgivenby Del=3.20)0-8.130,leading 2.72 2.76 (HD 172365)deviategrosslyfromthisrelation.Thetende- omitted. Thelowerenvelopefor thedistributionofstars Only twoorthreeobjectshave/3<2.650 andthesehavebeen —0.07 and+0.38dex(Luck&Bond1989).Twoadditional 2 2 2 2 1 223047 210745 206859 174947 151834 Luck andBond(1989) McWilliam (1990) 185958 199253 180809 47731 48329 45629 62236 45416 68752 74739 71115 58367 21754 16161 2 9270 5575 3712 ß P[Fe/H](F stars)=2.08AfMj+0.03 The apparentabsenceofasensitivitytometallicityinthe © American Astronomical Society • Provided by the NASA Astrophysics Data System index forGtypestarsleadstoareconsiderationoftheF +0.22 +0.10 +0.03 +0.38 +0.18 +0.19 -0.16 -0.09 -0.18 -0.03 -0.01 -0.14 -0.34 -0.22 -0.27 -0.15 -0.12 -0.38 -0.14 -0.13 -0.09 0.00 +0.627 +0.033 +0.011 +0.016 +0.035 +0.025 +0.001 +0?024 -0.035 -0.050 -0.010 -0.024 -0.022 -0.025 -0.Ö11 -0.026 -0.011 -0.040 -0.005 -0.049 -0.010 -0.004 -0.477 -0.490 -0.515 -0.535 -0^552 m 2 +0.02 +0.04 +0.06 +0.19 -0.30 -0.06 -0.37 -0.04 -0.17 -0.19 -0.17 -0.23 -0.25 -0.25 -0.32 -0.17 -0.14 -0.36 -0.17 -0.14 0.00 0.00 (+0.52) (+0.24) (+0.75) (+0.23) (+0.15) (+0.19) (+0.16) (-0.34) +0.01 +0.09 +0.07 +0.05 +0.02 +0.03 +0.01 -0.08 -0.07 -0.03 -0.09 -0.05 -0.02 -0.09 0.00±0.< 2^69 2.65 2.67 2.66 2.68 ß 4500 4825 4850 4625 4500 4850 4960 5000 5250 5000 4540 4690 4750 4820 5000 4890 4500 4700 4910 4610* 4770 5020 4400 4865 4770 4695 4745 4595 4885 5000 4515 4785 4710 4525 4805 4905 4900 4775 4635 4618 4995 4865 4710 4605* -0^445 -0.330 -0.400 -0.365 -0.425 -170 -155 -135 100 555 255 115 -40 165 155 115 -15 -80 m 2 80 30 65 45 85 25 0 whereas thevaluesobtainedfromA[M]andlistedin plane ofFig.5byclosedcirclesandthestraightlinerepre- penultimate columnofTable10arefromPaperII.Themean Table 10contains50,FtypeBGandSGfromPaperIIthat sents themeanrelation, The starsofTable9areshowninthe[Fe/H],¿m(Corr) corrected forgravityeffects, The correlationofômwith¿Delleadtovalues are alsointheGenevaPhotometricCatalogue.ApplyingEqs. difference betweenthevaluesofP[Fe/H]isonly+0.01 (17), (18),and(19)leadstothevaluesofP[Fe/H](m), supports thesensitivityoftoheavyelementabun- tometric system,correctedforgravity effects (Table9),withspectroscopic Fig. 5.Thecorrelationofôm(con),the valueofômintheGenevapho- determinations of[Fe/H]for10Ftype stars(Luck&Bond1989). ±0.04(2 0.046 0.142 0.146 0.118 0.139 0.088 0.091 0.048 0.134 0?178 +0.38 +0.10 +0.19 +0.15 +0.24 +0.23 -0.19 -0.10 -0.03 -0.07 F«/H DEX 2196 (17) 1994AJ 107.2184E 2197 O.J.EGGEN:GKGIANTSANDSUPERGIANTS © American Astronomical Society 1 i'S Z 4» I*! r Í at e | > ifs,>,,r,>ÖOe4 , *o dddddddddooooooooooooooo© oooooooooooooo 88S2 8íáSSSSíoS8SoS83S88o|o «. oooooooooooooooooooooooo O OOOOOOOOOOOOOOOOOOOOOOOOO íp rO'4’VO>^lO'^>^>»'>»K>VO'4'VOf^ r\jpgrMOjiMrp>f0^ooioK>0‘'iorQ oooooooo iE6g?SllliSIg| TMfMÍMPvjrvJÍMfMÍMrgrgíMfWfMOJÍMCvl *^^vog>£^[W2fl0voMvorg>j'0 SfeSCSSigSäSKtSt; o 38ooo®oootS88 dodooodddooooooooooooooooo K»0«-N>*-KvA0£0Kv/\^0©«-00*“ ^*jKi«pcg^*-OwtKi*-^*-O»C^50vno©52;5;r;f55£j ?o^>«o^fv'^!OC‘5P!lS^9Cifi£SSÄ!2iÄS — ^838383oo823o2ooo8282oS888 ©ooooooooooooooooooooooooo v»^<>K^ovn*-fl0K«voí000O'0wn¿rv£>N->rK5fvjO'0«srK «O «Vir- O o 2S2o8oñ35S828288~o2í;áSSo8o ooodooooodoooooooooooooooo I ♦♦.♦! Sic 8 O £ oK> 8R88Rf:::s:$í;SR5S3!S§S8g$S88g§ odd vnh^'Oto'Opu^pcOO^pf^íQ^C>¡ovA^»Q*J)jjOjO i ! o ¡8ÍÍS8S8S ;88SS^8S I o ■ o•- I fOCO . K>«OÍM i N-'OI ’ 'Otoi ‘ fONt( o < OJ fM•-< oooooooooooooooooooooo g: r- fMC-f fOOJ©>^OjCO«-fO^«-'00>0 ♦ ♦♦♦♦♦♦ dddddddddooooooooooooodoo O' ÍM r-oOO'(MKlvr»(ViO*-NÍlO-íP^»Q*“i£;'Ob;t;Pj©Í^50P fM O Sfcfc ooooooooooooo •o ^i ■o ç mO i K»ir»N* : =s-g ca >rg O gjO OOOOOOOOOO • Provided by theNASA Astrophysics Data System • >0 k oVOOJ > N-or- M w ddddddoooo *~fOOOrO fl0uvvrv^'O>r'Ovúfl0t/> «-flOflO^O'OOQKlN- *- IT»O“^ I OÍMr- ! 888 I ,S2SgS8 oooooooooooooooo■ asssfessgsssssssss'* tn ^pK 88^288 o d vnO-rovn^^O^ VO K*©'O vo ^'Oto • £§S! o ÍR2 d *0^0000000 ojo r i N-'O>t»ON-'0'0ir»fOiO OOOOOOOOOO Rg^8R8RSt:8 N-0*-0‘'OQ'i‘fM^ OOOOOOOOOO OOOOOOOOOO 8 0«"00^cg«00^ OOOOOOOOOO rgrsjojojojrgoirvi (MCO^-fOOCOflOtf «-rO'0>»oioh-K dddddddodd ^>»VOvOVOlOiO>» VOVOO>^>iMOJOJ’ SSCßRSÖSSS 00»“*”00j^“*“0 fMrsjfvirgrgpvjíNjíMrgrg dddddddooo 0000*-000'-’0 ÍRRSoSSS^á i/>KororCojo3>ooo *Oa0pKp'00«"0Q^^ dddddddooo t>tN>K.vnvrtvrt'^^vn > »— r-O^O*^*” K h- - “'O»O VO o ä o' o 2197 1994AJ 107.2184E 2198 O.J.EGGEN:GKGIANTSANDSUPERGIANTS resent starsobservedspectroscopicallybyBrownetal.(1989). for starsobservedspectroscopicallybyMcWilliam(1990).Thecrossesrep- Fig. 6.TheclosedcirclesrepresentthecorrelationbetweenÀCNand[Fe/H] The meanrelationbetweenC(I/II)and(R—I)qleadsto luminosity classIIIiscorrectedbyEq.(5),derivedMc- sensitivity intheGtypeSGandBG. dance intheFtypeBGandSGasmsupportlackofthis for theBGandSGstarsinTable6arenormalizedby The valuesofACNarelistedinTable8andcorrelatedwith Clure (1976).Usingthesameprocedure,(41—42)index the valuesof[Fe/H]fromMcWilliam(1990)inFig.6where, disk stars(luminosityclassIII) gave valuesofP[Fe/H]from In Eggen(1993,1994)itwas found thatalargesampleof except forHD45416,theyarerepresentedby divided betweenCNweakand CNstrongintheolddisk ACN andA(M)thatdifferedby morethan0.1dexforonly 10%, predominatelyCNweakin theyoungdiskandequally W0 2 10 © American Astronomical Society • Provided by the NASA Astrophysics Data System P[Fe/H](ACN)=5.0ACN—0.12. (22) The gravityeffectin(41—42)foryoungdiskstarsof C(I/II) =(41—42)—1.33[(45—48) ACN=C(I/II)o“ 1.90(Æ—/)o+0.355.(21) m m — 0.851(42—45)—0.506].(20) Fig. 7.TheclosedcirclesrepresentvaluesofACNand[Fe/H]fornormal scopically byMcWilliam(1990). straight lineisthemeanrelationfrom100normalgiantsobservedspectro- bottom ofTable8islesssatisfactory. by McWilliam.ThecomparisonwithLuckandBondatthe bly, HD180808aCNweakone.Thedispersionof[Fe/ (class III)giantsobservedspectroscopicallybyBrownetal(1989).The H]-P[Fe/H](CN) isonly±0.06dexfor11starsobserved population. HD45416maybeaCNstrongstarand,possi- by BrownetalandlistedinTable11,deviatesostrongly pected thatthe16SGandBGstarsofTable7alsodiscussed objects (luminosityclassIII)commonwithEggen(1994) large sampleofbrightstars,includingthe31youngdisk plicable totheBrownetal.data andapparentlycannotac- from theMcWilliamdatainFig.6wheretheyarerepre- data, withnearlyidenticaldispersion.Itisthereforeunex- mon withthespectroscopicinvestigationbyMcWilliam rived (Eggen1993,1994)fromover100diskstarsincom- Fig. 7.ThestraightlineinthefigurerepresentsEq.(6),de- and representedbyclosedcirclesintheACN,[Fe/H]planein velocity of1.7km/sforthesupergiants whereastheaverage ent slopethanEq.(22),fitstheBrownetaldata,buta sented bycrosses.Astraightline,indicatingaslightlydiffer- count forthisdisplacement.Brown etaladoptaturbulent sible. Thetemperaturescaleused byMcWilliamandLuck systematic displacementbyabout +0.25dexisequallypos- (1990), andequallywellrepresentedbytheBrownetal & Bond(1989),representedby Eq.(16),seemsequallyap- Brown etal.(1989)havedetermined[Fe/H]valuesfora 2198 1994AJ 107.2184E 4(Aßmax) 1 F =10°-~,iscorrelatedwiththeluminositydis- ues of[Fe/H].Theoverlapsamongstthethreespectroscopic value forsuchstarsintheMcWilliamanalysisisnear2.5 km/s. PL relationusingF(Sandage&Tammann1971)give placement fromtheridgelineofmeanPLrelation. 5575 surveys discussedhereare, values fromTable7isshownin Fig.8wherethebulkof Table 7. values ofACNandP[Fe/H]computedfromEqs.(21) 47731 3712 et al(1989)needsinvestigation. ThedistributionofP[Fe/H] the SGandBGanalyzedbyMcWilliam (1990)andBrown but byanalogywiththeBGandSGstarsdiscussedabove, Cepheids, where[M]=0.3(b-y)andA[M[M Eggen (1985)foundthatF=1.009-4.545AfMjfornormal Sandage &Tammann(1971)foundthattheamplitudedefect, lie justoutsidethetemperaturerangediscussedhere. to beofsomeconsequencefortheclassicalCepheids,which 21754 2199 O.J.EGGEN:GKGIANTSANDSUPERGIANTS the dependenceis,likethatF,directlyonluminosity luminosity on[MJwasinterpretedasanabundanceeffect, dependent anddonotmeasurethemetallicity.Thisappears displacement fromtheridgelineofPLrelation.The and A[MJareinterchanged.ThisdependenceofCepheid AA/V=0.00±0.09(o-) magforthenormalCepheidswhenF (22), respectively,forthestars inTable6arelisted 199253 185958 174947 —0.210 logP—0.160,andtheluminositiesobtainedfrom b B 1 ß B B Eq.(16). 216246 +0.11-0.010 210807 -0.20-0.019 206834 +0.40+0.049 185958 +0.24+0.025 164349 +0.39-0.004 150416 -0.02-0.015 115004 +0.08+0.029 199253 +0.01+0.026 174947 +0.39+0.011 HD 47731 -0.08-0.020 77912 +0.20+0.004 74739 +0.08-0.022 72571 +0.20+0.010 25877 -0.04+0.012 21754 +0.25-0.005 HD [Fe/H]ACNTe 5575 +0.10-0.004 3712 +0.33+0?024 Table 11.MetallicitiesofBGandSGstarsbyBrownetal(1989). © American Astronomical Society • Provided by the NASA Astrophysics Data System Certainly someofthedifficultyiswithspectroscopicval- This displacementofthezero-points for[Fe/H]between In summary,thevaluesof(M^areessentially,luminosity 1 McWilliam DEX Sp.COMPA -0.13 -0.09 -0.12 -0.03 -0.18 Brown etal. +0.10 +0.33 +0.01 +0.24 +0.39 -0.08 +0.25 4910 485060 4910 4920-10 4780 0 4580 4710-130 4880 4785105 4810 477040 4900: 487030 4800 4690110 4930 4805125 4780: 4795-15 4900 48855 4450 4515-65 4905 4910-5 4710 461895 4710 0 4470* 4605*135 5020 496555 Luck andBond -0.16 +0.18 Table 7,thevaluesof(M^oarealmostentirelyafunction zero-points ofthe[Fe/H]systems. Fig. 8.ThedistributionofP[Fe/H]valuesinTable6(clear)and12 H](ACN), for100pcstepsinX, areshownasclosedcircles the starsinTable7and12.The medianvaluesofP[Fe/ 7. Theradialdistancefromthe Sun, positiveinthedirection distribution isverysimilartothat ofthebrightstarsinTable represented bythecross-hatched areaofFig.8,wherethe computed valuesofminTable7.Forexample,thediffer- between thesedifferencesandthoseobserved puted valuesof(M^oissupportedbythelackcorrelation ues greaterthanabout0.02magbetweenobservedandcom- errors oftheindicesarelarger.Theaccidentalnatureval- noted inTable7,butthestarsarefainterandobservational and computedvaluesof(M^oforHD68111,85205,106981, luminosity [Eq.(14)].Thedifferencebetweentheobserved most identicaltothatfoundinTable6.Also,asnoted luminosity, M(DDO)-A/V(4C)=-0.04±0.19(cr)magisal- listed inTable12.Thevaluesofthereddeningandluminos- a peakat—0.1to—0.2dex,comparedwith+0.1 stars haveP[Fe/H](ACN)between+0.1and-0.3dexwith (crosshatched). away fromthegalacticcenterand designatedX,islistedfor 0.001 mag.Also,adifferenceAÍM^qof0.054magforHD ence is—0.067magforHD105138whereasinmitonly ity arefromEqs.(10),(12),and(13).Themeandifferencein for whichthe4colorphotometryisgiveninPaperI,are in theBrightStarCatalogue(Hoffleit1982).74fainterstars, accidental thatthisdisplacementisthesameasin 223047 iscontrastedwithonly0.005maginAm. 136474, 192277,143119,and161388areslightlylargerthan +0.2 dex(PaperIII,Fig.3)fortheFtypestars.Itmaynotbe 2 K 2 2 The valuesofP[Fe/H]derivedfromACNinTable12are With ahalfdozenexceptions,thestarsinTable6arealso P[F«/H] ACN 4. FAINTSTARS 2199 Table 12. Faint SG and BG of GK type. 2200 O.J.EGGEN:GKGIANTSANDSUPERGIANTS © American Astronomical Society e o- 3 ^ « 2 5 2 /■> o — o o o s , k ,>c,rK)>rí |á5lgsÍ?5li2sgiéÍ^l8ÍÍl!S5§ál^lI§^^i 0 ^>>AK>rgrororNiro<\jK|»orAK|rsirgroro»AK|K>K><^>A>AfArCK)AjAi(>jrAK>A)K>fAp>^iKt ^AJK|AJAJK|*^AJ«->A4rg»AA|r-v-fAK>AJIAAIAI^K>AJAJ iPvj•-r- iK)AJfO«-fA , >* >!> S a ^Aoc0K-oc5^0»rgcgrgNfíNjKS>o>tfl0>»>0^Í0Íc0ZriA>0kAÍANr^-5Sí^K.SS-5Í g ,>^»A's»>íl/>>4r»l|>/>r>#^tVA>tK>'^'jriA'0^>#'0'0»r>>í>írOfO>ÍU*k>y>í«»f^»¡AlA4A»A o ooooooooooooooooooooooddddddddddddddd oooooooooooooooooooooooooodddddddddddd ¿JÍ •“ÇOv»“rsjOOO^^FO00^4/>MO N» Of\JÍNJÄ oDí2nÍC2!^¡íÍ^?CDí®2S^PISm2E‘*"‘E^Pí '200>í'0>í«o ooooooooooooooddddddddddd *odd 'ddddddd o ooooooooooooooooooooooooodooooooooood 2 E9*0ÄPD;"í!0ü^ ia k»an.o o oooooooooooooooooooooooo•odd •ddddddd ¡o S2E®íü*0*59^r*°íik>»a ^oki>0^>«0O‘C0«--i0K>v#0 >|fl 'O'ON-KCOKCO'OKKKN.S.^^'OKcÔaÔeÔKK 'O^OKKcÔKf<<>K SS3SiOSSS!SSiQ5SS3ÊS5fî!(îî58D;t:!SSSSSlÇS23SRfe3 p*¡“*j’"0*-*-»-*-«-*-r-rg*-o»-»-*-rsjO»-PMfNjrgr- ■oo«-*•*-!«2rw«-?«Jr>¿ ssgs&sssfissftsasssssfc^jsßs; _&5Sásscssa (sîi;2ïPESiCÂSE29i;^àt*‘2i025E2*r^*“i'O‘''Ç^ooo«0'0 oooooooooooooooooooooooooooooooooooooo íCJC2EDí®2^tE29S?¡P2^i0229r'o^*'^‘^^«»»rs»^cp'0 "“"*“'“«*”f>i*-*“fvj»-o*-*-*-rgo*-rgrsjrj*-*“00*-rsi*^*2J«2jJ2 «í2E*^Dí29E9ÍTSiE^r29‘0E'$“^0>í>-í\íiA'OiA>íí\» OOOOOOOOOOOOOOOOOOOOOOOOO •ooo oáooooáoooooooooooooooáoo ooo 2 ^ES2'O°'O™K*K»***¥»£*•>*oco>0 OOOOOOOOOOOOOOOOOOOOOOOOOÍooo »-KíOO^-OrOOrOOÍM^-w-r-AjOr-OT-w-r-w-r-KíAJ AJAJIA Di E&S2fiE:^°®k^-ia «OCO-COflO-MCOMflOoO «OmoOâmmÇoOOOCOCO-CO«-«« i SSSSSSSSoSSSSSS^SSSSSïSSSSSSSïSSSoSSSSS rf>w MM "MTm2mT—Äi3XiX)J3 • •••••••••t••i, <>'0»r>u^N-Nr>tK>í\<*--q^Q(M'OmfOflOíOflO'0*-^r-QS-flO'00^0««r>QfO‘OK>ir>r- »ooooooooooo < eg rorg>^(rt>Okrk'OrNjrNj'0'OfV(^'0>0'Okn^'0<0'0<0'0'0<00'0'Ou^'0^'000 M ^m^mmmX).Û ösasasssissasssssssSQöässsssssssssä V ^-*k^._.^k.*•_••_•_•_• ♦♦ÍVJ. •iojrvj+«--rNirvirMrgr-rg<-rvjk/\r\j>?rvi>*'4’K»¿0>4' »OOOOOOOOOOOOOOOOOOOOOO • Provided by theNASA Astrophysics Data System w s sssols t Ö^"î•“ S íÍSS3S 2200 oo 2201 O.J.EGGEN:GKGIANTSANDSUPERGIANTS © American Astronomical Society

Table 12. (continued) : h «C flO j: X D o O > , , , , >, , >S, S® eg. r- eg ddddddddddddddddddddddododddddoodddd > ©'OlA egego«-o«-oor-r-o*-r-^-f-rg«-»-r-Ovf©*-«-egpo>í*-«-*-«-eginegego K>íOrOporofvjroegiOK»rofoejpOíorgroegegKiro>ífOfOPOK>ejK>KiegK>foegfOpOPO egpo>íwr»oegK.ir>ege^<>u-keg*-^»-'0'0'4ir»Ní>í®®N»0-*“«->TOe-ví®e>»^'0 Kl K-4AN. oooooooooo K>f®KKr^eg»r»KN.oK©©>trgK»0‘K©*-KK>Ki®0>©u>®>î/''0®©«0>t PO oooo ©•-oO©eg«©Kr-ooo®*-*-«00'00>»egegpo>^oejN-'0»rk^*-»-oOK>©© o ©' eg rg o oocgK o ©eooo ©0.00 O o» *-cg>t •-eg©»-rg*-©©©pgr-rg3,-i-org*-i\i^K»*-K\rgrgrg^rrg^-*- ro©rgS.T-ro©o^*-«o©®vA^O‘^-»r»»“©fO®©cg®®N.®©ooN-r^©^M># N.'ON.®'0>O^XO'^'0'0^'0®'0'0'0^'0«ON.'0'ON-'0'0'00'0'ö«rt>»^N.'0 mrsiNf00>t*-^>f«-*-®©K-«^>trOi/>©©f^trpN.K»>ÎK.>»‘QN«©N.>TQ«-»n'O o ^ç.ooO'Oir»'0'0«rg*-rvjfv»'0'0'Of^'OfM«po«^^'iiOir»pfcn^.>fN.f»nsr©»r> oooooooooooooooooo fM^^®KS»-^tlVJ©'Oh»^rgh*K>®PO^KI©r-*-K.N.'ON»©»r»K» »-'0®*-'0©K>UN^O‘*-©'0'0 —©'O©0»r^®>orsi«ptooor<>-tf^®©^x. oooooooooooooooooooooooooooooooooooo ©ir»N-'0>í»-ooorsíN.(M>oro©^'0©'Oirtrg©ofMooLr>'Oi^^>f'í^f>-o>í^»r> fl0«0—QOOO —«0oooooocooooooo—0000oo—-eoooco00«0 *- ra•r-f\j r^rjc^r-^rg«-’ OOOrgr-’r\jor-^^-rg*-*“«-KÍr4rviÍNJf\JKífMÍNJ<\ífOrvJr-r- ^©®fMra^»/>®*-h»©®’Org'OíNi»A*->r<>*-Kioo^'0^>í^4»n'0»OíOoo»nm '*íiAu^Ni-wr>N»K»Ki>i'4'>í4ro«4'>»rO'0>íNí>í-«o®iAkrku^'Oro»A'Ostirpu*»irk®>»>r S''0t'OiA'Ol/'»u^K3U"»«Q©'Q'0©flQ'Q'0«-K>tf\m 'N. « £^~7Z'kzñZZZ*?Z*7xijq7• f\IKI'íO'0/>OOLnrOO>ífM'0'0^'0^mir>ON-KO-NÍfMl/?NfVi/>u^00S.^NiNw k> »-•-oorvjtr>KrgN-rgK-vrii/>íO'egOino«“N.*“'r-^>OK>egeg©N.foejeg«-N.vrks»>^m»^K>K»oegir»eg — X).ÛJD---01>££«^^£0£«—C«£«£jO >ow • m , 1all egejK»»OK>Kíioro^^>f>r>t>»>»jn»n»n»njnir»®'0>0'0'0'óN.KKF-< u-»0-eg^>0'0'0'OegegegpoNí'0'00*-«-f0^íe^<5«-eg>jN.Optop^O‘( flOKifNjN»>i'fi/\tstegutoo«-ror-t/p^Kttn^f ^ 3egrgoegeg®f-«-mir>'OOu^kne-KiOOO'ON-e^Oi/>ir»«-u^OO , pi/>e^ororgoO*^*-POvtejXpe(i/>fO^:>j'pooopxo^iriOO>oviPO OK)-^'O^tg>N>N>^tr>0'©©irkVrk'^’O(>KtO''O®tn'<^'0QN>flQ0QOS. > , ©©©©©©©OOOOOOr-OOOO«- —ooooo»-ooo ©©g>^*/N©'í*-»r«KP-í^«-^©tAK^flprg«-®oíN»^>r>g>M K’0'0>i©T-cgco*©<\irOKP»/>s*^u">*-w»©«~'0'0>ri/>©(M>í 00000©0000©0©0©©00©©©0000©©00 Kt <0OO ©00©©©00©0©0000000©0000000000 >r eg O rvj á*“(M*-^'00-V/>»“'0«-->íO*-**-rsí ® ©O >í’ÍVJO'0>0P0©^‘0« ooooooooooooooo©ooooooooooooo eg OOOOOOOOOOOOO-r-OOOOOOOOOOOOOO SegfO©®rojAM'^g>©>fO‘W^^K>iK)©®«oo®Kr^K egegegegeg*->íegegpoeg^rOfOrOfO©egKi*-egpoegegrgeg o* o N- OOvT» «'í©' : oegirooeg<\(KTf^*-íOQpoo©^©>g>eg>ro«-©’0'r- r-* o^r-‘o¿r-’*-po<\JrgcJr\¿rocg<\¡kÍK?r-'•-* 1 oooooooooo©oooooooooooo SK»u^s>'ON.Q®N'rgrg'Oin'ON.'Oro>K. Provided bythe NASA Astrophysics Data System w >oooooooo©oooo©o©o :ss: 2201 2202 O. J. EGGEN: GK GIANTS AND SUPERGIANTS 2202 h) S 8

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© American Astronomical Society Provided by the NASA Astrophysics Data System 1994AJ 107.2184E 8 boxes intheradialdistancefromSun,positiveawaygalactic 2203 O.J.EGGEN:GKGIANTSANDSUPERGIANTS Fig. 9.TheclosedcirclesrepresentmeanvaluesofP[Fe/H]for100pc pc. center. ThecrossesrepresentindividualstarswithZ<-500pcand>300 The dispersionofP[Fe/H]withineachstepisalsorepre- in Fig.9forstepsof100pcthatcontainatleasttenstars. than about1kpcfromtheSunindirectionofgalactic ranging from[Fe/H]=+0.18±0.45(cr)dexfor25starsmore individual starsarerepresentedbycrossesinthefigure.Luck sented. ForXgreaterthan300pcorless-500the kpc fromtheSuninanti-centerdirection.The14stars center to+0.07±0.06((j)dexfor13starsmorethanabout1 Fig. 9morethan500pcfromtheSunindirectionof & Bond(1989)foundametallicitygradientinsupergiants galactic center(—X)giveameanP[Fe/H]=—0.05±0.18(cr) direction awayfromthegalacticcenter(+X)give—0.18 dex whereas8starsmorethan300pcfromtheSunin indication ofthisgradientisfromthestarswithX<500pc, agrees withtheLuckandBondconclusion,althoughonly inconsistency ofmanypublishedvalues[Fe/H],nocon- and consideringtheobserveddispersionofP[Fe/H], of threeneighboring,earlytypeobjectsintheclusterNGC of fourKIstarsnear(a,<5)=(7^5,-15*0).The4colorand Way (Stephenson&Sanduleak1971,LSS),revealedagroup clusion concerningametallicitygradientcanbedrawn. listed atthebottomofTable13,isconsistentwithearlier 2414 (Vogt&Moffat1972).ThereddeningoftheKIstars, (P,J) observationsarelistedinTable13,togetherwiththose the region.ThethreestarsinNGC2414showthatavery ±0.14(cr) dex.IfthisrepresentsagradientinP[Fe/H],it large increaseintheabsorptionoccursbetween1.5and4 After theobservationswereobtained,itwasnoticedthat mag, agreeswiththevalueof13.2magderivedbyVogt& kpc. ThemodulusofthethreemembersNGC2414,12.92 (e.g., Eggen1981)resultsindicatingverylowreddeningin four KIstarsareradialvelocitymembers(Mermilliodetal Moffat (1972),whoalsofoundnearlythesamereddening. Nandy (1962)findamodulusof11.11magandE(£—y) lar totheresultsinTable13.The clusterappearstobenear giants fromthephotometricindices. Thesestarsarelistedin early typestarswouldbeofinterest. 2X10 yrold(Fig.3)and4color andH/3observationsofthe SG inPaperIhavebeenfound tobeluminosityclassIII 1989) ofalittlestudiedcluster,NGC2437(M46).Smyth& =0.105 magforthiscluster,whichareextraordinarilysimi- © American Astronomical Society • Provided by the NASA Astrophysics Data System A surveyoftheLuminousstarsSouthernMilky 21 oftheGKstarswithspectral classificationasBGor -800 -400y0.0400800p« Table 14.Thereddening,luminosity,andmetallicityarede- rived fromEqs.(1)through(9). pected ofvariationandshouldbefurtherinvestigated. tected companion.Oneobject,HD74000,istheonlystar these objectsarepossibleCH-t-(Ban)starsorhaveanunde- the basisofboth<5(45-48)and<5[w-b].Aboutonethird are listedinTable15,wheretheytreatedasSGorBGon be accidental.Thedifferencebetweentheobservedandcom- puted valuesof(M^qis0.515—0.695=—0.180mag,which inconsistent withthegalacticlatitudeof40°,soexcellent disk spacemotion.Theradialvelocityofthisstarissus- discussed herethathasayoungdiskluminosityandanold agreement betweenthetwoluminositydeterminationsmay is inconsistentwiththefactthatotherBGandSGoftype H]= -1.42dex.Thepossibilitythatthespectrumiscompos- observed valueof(C)leadstoACN=—0.261orP[Fe/ GK indicateasensitivityofMtoluminosityalone.The ite (Houk&Cowley1975)needsfurtherinvestigation. values of(45—48)areshown inFig.10.Thecontinuous range. Some50starsinthisrange arediscussedhereandthe sensitivity ofthephotometric indices inthistemperature 0.27 mag)needspecialattention becauseofthechanging line representsthedefinitionof (45—48)usedforthelater 0 m0 1 0 0 -15.1864 LSS460,G5I(StephensonandSanduleak1971),Sp.B.,P-248.3d. -15.1864 -15.1864 HD59609 HD60308 HD59698 HD59589 LSS 516 LSS 515 HD60308 LSS 516 LSS 515 HD59698 HD59609 HD59589 Problem starsamongstboththebrightandfaintobjects HD 6446maybeahalogiant.Thederivedreddeningis The starsinthespectralrange GO toG3(P—7=0.15 59698 LSS463,KOI(StephensonandSanduleak1971),HDtypeG5. 59609 LSS456,KOI(StephensonandSanduleak1971),(Houk 59589 LSS455,K2I(StephensonandSanduleak1971),KlV(Houk Table 13.RtypeSGnearNGC2414and2437. E(b-y) (R-I)A[u-b]V 10.77 12.11 0 companion maybeanearlytypestar. 0.102 0.100 0.110 0?100 0.427 0.428 0.424 0.430 0.100 Smith-Moore 1988). Smith-Moore 1988). 8.17 9.77 (Mermilliod etal1989).Theumagnitudeisvariableandthe 9.94 9.60 0.147 0.053 0.193 0.347 0.296 0.280 0?426 0.389 0.309 0.325 0.753 0.697 0.673 0?920 b-y 5. PROBLEMSTARS -0.056 0.104 -0.039 0.008 -0.026 0.115 0.095 0.187 0.108 0-132 0.433 0.409 0.378 0?656 Notes toTABLE13. 6. G0/3STARS 10.27 6.33 8.93 9.51 9.30 9.17 8?45 0.487 0.455 0.387 0“311 -1.62 9.31 0.440 9.24 0.398 9.12 0.373 8?20 0?519 -6.40 12.73 -4.04 12.97 -2.79 13.06 -1.78 -1.70 - 3?73 ± 0.17 t 0.16 12.92 11.11 11.13 11.18 10.87 11?18 2.540 1.4.0.0 2.590 3.7.8.3 2.623 6.0.5.1. R-1 iß) KO II G6/8 Ib-II G5 II KI Ib-II 38.8.2 5.5.9.3 COMP Sp.T. 0B+ 0B+ B2 la KO I KO I KO I K2 I 2203 oo 2204 O.J.EGGEN:GKGIANTSANDSUPERGIANTS © American Astronomical Society

Table 14. Stars classified as SG or BG but with photometric indices of normal giants. .o , 0000000^.0000000000000000 liiSsig SiS£igigiig§igSS oddddd o ooooooooooooooo*-^-o*-oöoo JT«— O«—ÇOK>ÎO»OFOt£*“^^-Aj*—^OlO'íOÍÑ3c5*“r- Soaoojrnio>o^K>'od?irtdN»-o«-OQflOQr-o ooooooo oooddddddddddddd ooooooo ooooooodddododdd ooooooo dddddddddddddddd ® S;jmNroioKj—nXj 0|N»OrsiK*-<>r-*-OflO>4rOK>rOfNJO'0»-fO>r*-«OfNi ooooooo*-*-do «-ddddddr^dd^dd •r*-0'*K»«/\0'*0'*'0»nooK<*io£*-KfMO*op imssi ii^SSlSSSiSiiSi »-•-oooo*- ddddd!dodo*-* siiRSRsg-^gss, sssi^s^iq^e ooodddd ddddd!dddddddddd ooooooo ooooooooodooddod SR1QSS8S o ??????? ???????????????? íR2oSo~ áSSÍ5SÍ5Ríí3S2s:§g5S sassssssisssassssissssesis O curgí>í*-*fNji>4K)04«-ror>j(MvfMoj?>rg«-Xifg rj N.*rs.‘dn»’n>*>rn.*n!n-* RR5RSá$3Sí5í S3S5:3 ooooo•oooo ♦ ♦♦♦•♦♦♦♦ X < J S (/> û.a.O 3 SSI ë =«.ü M ** « 2 ° —i*-, r- U^ ÍM *- l • 5I Ï ■ ‘.-I *Í O *•*9 O «0w . «»sigáis • i-^M aa!^!ak: o a X w ~ H ♦ •« R'V O_ao<> ♦* %• • wXU 01 K^fl t ♦O’O• • ^çc J ! I • *-i» ^ >» Í 3 u I « t 2204 oo 2205 O.J.EGGEN:GKGIANTSANDSUPERGIANTS © American Astronomical Society

Table 15. Problem stars. j "1 X ‘I J3 o b 8 #s-r^s»inN-00inininN.K» j”>rrgr-inrgr-6grgfnfOíOíO>íxiin*-mr-pg *2 OK»fx*-00rslK3pooo©corto>íp>r ÍÍ»-rxrxpininin«-inrgvfpinorg'OiON.o jo roo ^»-—■*^-“-^»->fK.inPrg s§iás ^sn'O^in^oor-moo m'Qrsjn-oPjn fvi rsjdK»rsi’•-«-k>nj»- Ömmorgt-pop^in^ ini. >0 'O oOr^K»oO'*-«0«K>pogp«-in*-inrg'r-in ooooooooooo •“rgoíMO-^O«-*-«-*- *oo<«-«-rgoo fOKfnoO'Oin«-om«cgp>org>t>0'00't «o ö*>oinao'Oorgk><>^ÎÎ*“, Q^m>#^POin*-inp pfOr-s.N-»-rsiKi rJ xirsj«r-*indrvj!n¡ rsj '0>rOoON->ri)inroKiro rgooKKr-^N. s 5 <> •-«-xi^i-oinpopp •x^^pu^po JQ -iï«i>«0Ü!!-Û«-O — «.0~.ûx.—ÂÆ- XXwOXwOX^XX MM MM'S.MMflQOO« 0 IOOOOOOOOOOOOOOOOOOO dddddddddo N* O-sf^ooo#0ûk*KO'0«0»- orsir->f'0inrg XXXXo V. Provided bythe NASA Astrophysics Data System ooooooooo o in m K»inrg o K oro>op O N-K» »-* o’ro m o> "X "s. x o • o o m ►- 3 2 « *? c 8 ® O a x rgOw --o'* s-s <33 1*^: Ï » » _*®ca ill;! I - ? • 3? itjilf 5.75 > c-♦X JM! s S I I ! s SS s » • (C ■ X o«M It 1$ •- o ^ o "|êl I o £ax^. 1:5« «i - 8iE» X© ro<=> ÍÍ 7* «i s"I“ ü o M s d u at* 1 a wxz . -■,— a ? ? s ? 4i u. jz•a CO OKl i I§ M 4-« 2 S „ H-O u -C^ s ? 8 ? I & s 5 5^ Ï s ? I 1 i 4-* «-» X a u a o a i 9 a 8 i HO 74006 Beta Pyx. The only problem with this object it that the V-mot ion is unique for a young disk star. The problem may be with the proper motion, which needs strengthening. The radial velocity is possibly variable. 2205 H1 oo^r 2206 O. J. EGGEN: GK GIANTS AND SUPERGIANTS 2206 h) > ? i ni ï « M r ? - k 3 2 r.-s « O «O O ! I ? C? • S Ultr Wg* s & I -I ïlï N-» O «I ôii“ jj Q. t-Ï *0 ! :4 Fig. 10. The GO/3 I stars (closed circles) and GO/3 II stars (open circles) in f ! «Íi2 8 the 45-48, 42-45 plane. The straight line is the extrapolation of the upper CMO envelope for the normal (class HI) giants of type GK. 1 >r i. - " » t0 , s¡ »• 3 ¿ M 4-»(A iO « -+j « *- .t. ? rated into what are spectroscopically defined as luminosity- *8 i « =ï im«4- class II and I objects, and those of class I are represented by S*« - I I " 3 closed circles. The class I stars are listed in Table 16 where "^5 *■* ï .£ I 5 s fl W the values of E(b—y) are obtained from Eq. (10), (C ) O m 0 1 c >* ? ? from Eq. (20), and á(45-48)0 from Eq. (11). The quantity I?M C:âfï Z i I 5 [u-b], Eq. (13), has been redefined for the GO/3 stars « M £ « 5 « h4« ¿ s ¡ió'Z ^ U>* 2-s¿l ¿ ¡S S[u — b] — [u — b] —1.200. (23) 'S fl ^ «o S3 - ° s s g 1 • S S O ii Ç *5 •; c % 2 The luminosities are derived from £ S > >* 9 v * «i 51* 5 ¿ 8 IL

My(DDO) = 2.5(Ä-/)0-20.0^(45-48)0-3.40, P:5fl I il? 1--1 i ï- (24) U ‘‘S ^

ihii'Â s X OA *-v s=-^ o °-•- A/y(4C) = 2.5(/?—/)o —5.9 <5[M — b] —2.75. (25) « $ f.r JÜS *® ? r?:« Ils! u The following checks on the luminosity calibrations are M cl ?û - 5 j." > • a 5-5 available. ^- fl S fl« • >.>n 3°- I" îï*A C O fl*“ 4rf44 w—» .¡î| HD 204867I209750(a and ß Aqr): These stars are sepa- * U S 5 'o^ -fi •5 gc «0 «D9 O Q. a u fl fl fl rated by some 10° but have nearly identical apparent mo- aS >••“Q.ât w _S U8w 4-*^o£ •O- X4- —C £I- 5J?1 tions. This motion is shared with the early type star HD 209409(/c Aqr), a variable shell star, and at least three fainter objects; HD 208349(A2), -D4247(F) and HD 209905(B9) (see Eggen 1985, Tables XXI and XXII). The mean modulus Kl U-> i «0 Kltn 9<0 S « Í 209750 in Table 16. S SS Long Period Cepheids: The LPC fall in the temperature domain is discussed here. The five variables for which DDO photometry is available and discussed in Sec. 1 are

© American Astronomical Society Provided by the NASA Astrophysics Data System 1994AJ 107.2184E V340 Nor VY Car T Mon The luminositieslabeled“PL”arefromtheperiod- RS Pup 2207 O.J.EGGEN:GKGIANTSANDSUPERGIANTS SV Mon tion (Eggen1988)whichhave,respectively,moduliof10.5 tion ofNGC6067andthebackgroundNormaOBIassocia- luminosity relation(Eggen1985).V340Norisinthedirec- member oftheclusterand—4.2magifa for allthesestarsagreeswellwiththeavailablespectro- reliable apparentmotionsarealsorepresentedbyclosed early typestarsgiveamodulusof11.55mag(Eggen1980). association. VYCarisamemberofclusterforwhichthe and 11.6mag,orM=—3.1magfortheCepheidifitisa circles inFig.4.The“computed”spectraltypeofG0/3lb in thecolor-luminosityarrayofFig.3.Thefewobjectswith scopic resultsnotedinTable16. luminosity. Thiscanbedemonstratedwiththeobjectsthat in Table16havevaluesof(M^othataresensitiveonlytothe have GenevaPhotometry(Rufener1988)andlistedinTable 17, so v either thevaluesofm(likeMj)areindicatingthatall leaves ameanvalueof0-C=+0.001±0.009(o-)magand Removing theluminosityeffectfrommwithEq.(26), the latertypestarsdiscussedinSec.3,arelistedTable16. indices aresensitivetotheluminosity(gravity)alone. stars haveessentiallytheheavyelementabundance,or The valuesofACNareallvery smallandexceptforabout four stars,indicateametallicity spreadoflessthanP[Fe/H ]=0.1 dex.Therearenotenough reliabledeterminationsof [Fe/H] toattemptacorrelation; 2 2 LPG © American Astronomical Society • Provided by the NASA Astrophysics Data System The starsofTable16arerepresentedwithclosedcircles Like thelatertypestarsdiscussedinSec.3,G0/3 m =[Bl-B2]0.457[B2—VI], Del=[U—B2]—0.832[B2—G], m =0.958(P—/)+0.620Del—0.722.(26) Am =m—1.95(P—/)o+0.695, Aw= +0.002+0.620ADel, ADel=Del-1.60(P-/)o+0.695, The valuesofACN,whicharecorrelatedwith[Fe/H]for ACN(G0/3 I)=(C)—0.130(P—/) +0.220.(27) 2 20 2 2 m0 0 (*-/)o 0^267 0.224 0.210 0.239 0.251 <5(45—48), 0^139 0.099 0.069 0.116 0.115 'o ¿[u —b] 0^894 0.792 0.847 0.814 0.860 9 89 8 9 8 r 209750 +0.008+0.10LuckandBond with <5(45—48)<0.04magwhereasthevalues It appearspossiblethat,likeMthevaluesofCfor evidence, theslopeofAM/<5(45—48)increasesforstars known abouttheluminosityoftheseobjects.Frominternal luminosity classIIandarelistedinTable18.Verylittleis abundance. GO/3 Istarshavelittleornosensitivitytoheavyelement perature range(P—7=0.15to0.27mag).Consequently,Eq. 159181 —0.019+0.14LuckandBond AM/S[u —b]appeartobecontinuousoverthewholetem- indices, parent motionsare The luminositiesofstarsinTable18thathaveaccurateap- (25) hasbeenusedforM(4C)inTable18and,theDDO My—+0.4 mag(i—10yr),arerareexceptions.Thissparse- These, togetherwiththespacemotionsinTable16,arerep- 222754 14/-1 resented withfilledcirclesinFig.4. between 5X10and10yrago. TheratioofGO/3starsbe- was littleornostarformation inthesolarneighborhood populated inthecolor-luminosityarray.Twogiants,31 0 tween theisochronesfor2and5X10 yrinFig.3mayreflect star formationbursts.Asnoted inSec.2,thereapparently ness istheresultofbothevolutionary ratesandthetimingof 72779 (GOIII,P-7=0.24mag)inPraesepe,bothwith Com(G0III, P-7=0.23mag)inComaBerenicesandHD r~5000° to5600°)extendingfromtheclassIIgiants 1?m y0 (My—+3.0 mag,í—5X10yr)isoneofthemostsparsely (M 2.5mag,Í—2X10yr)totheclassIVsubgiants a changeintheevolutionaryrate inthisregion. 119605 13/—4 V V e v 57146 +0.023+0.03McWilliam 31910 +0.006-0.25McWilliam 26630 -0.002-0.32McWilliam(1990) 26630 —0.002+0.15LuckandBond 16901 +0.007—0.08LuckandBond 84441 -46/11 24395 -9/1 4362 -0.028-0.12Luck&Bond(1989) HD CN[Fe/H]Source The starsshownasclearcirclesinFig.10areequatedto Afy(DDO) =2.5(P—/)—37.0<5(4548)—2.70. The regionoftheG0/3stars(P—7=0.15to0.27mag, 0 —5^51 -5.10 -5.09 -4.22 -4.86 DDO 0"001 + 17.8+17.8-9.0 +20.2 -9.4 +31.4 +26.3-21.5 -20.0 -20.1+6.0 km/s U P V —5^25 -4.56 -4.82 -4.98 -5.16 M v 4C -4.35 -4.71 -4.72 -5.16 -5^71 PL -13.4 7.25 -10.9 7.65 -9.5 7.85 + 1.97^25 W Modulus log P 1.054 1.183 1.277 1.432 1.617 2207 (28) h) 2208 O.J.EGGEN:GKGIANTSANDSUPERGIANTS © American Astronomical Society • Provided by the NASA Astrophysics Data System

1 ECb-y) (R-I)0 5(45-4B)0 ACu-b] V0 Ny ACM m./M4 p N V W Sp.T. S Note DDO 4C OTOOI lue/sec km/sec , i>ÎV,>K0,1-fl , 1 , s ^0>Kl'OKIOOOir>KlOfSi*-00'N»*-00^'ÖCOOKICOrsjNr'OKN.*-rsl <»d oddddddddddddddddddddddddddd pSSooäoSSoSooooSSSSooooäoooSoo o d d 0‘rgoooKrg^N.r>-'06‘0>'0‘^or-oooKir-*->4oof^^.Oinin'00‘ 5p>«-KrsitoKoQ>tOKi^rvi«-»»r>jK.wKi o d d S§ál2^2igS^S^íá8SSá2&Sl85g2gálfe O d d «QSt^KirNifOKIKIKIKiœ^F^^Kl^irirOKlinKl^lA^N^^lA^I/l K» >fKlKIkÍkÍ^’kÍ'VkIkÍkikÍki^K»^>^K>KI>^*- f^r-rgrMjr«jo»jrsi*-«-rgrgrsjrg*-fMrsirgfMr«j<\ifMT-rg 2'û'Pmroi/><**-inN-iACOjn©^C**-Ki<\j»“'00^'00*“OJKyiKi .I9''0Ç*SP'0vc0''*ûKiK‘^"^<>?‘eptf$Q P o dO O l£Ot>*KOO«-’OtOO'in'£'OK>KOtOO>«-0'U%0»&<->rN>OlS!0'i'* o o*dddddd f'J Klrvj•r-rgf\jKirjKifMKir-rgrviKirgKiKi*--rgKi*-»ro^rfiir-nj i^rgyio 'sroO'OKiN-KirgooO^'iw-k>0'0«^o^rrgcmk>^ in>ííOrOlA00ir»U^>f>íO00N'N>N-N*N»fl0O'ON-N.'OOí'J'OO'O»r»^“ Kl^rKIK>KIKIKIKIKIK>>ÍKIKI» Si&SSR3SS833SS83»C83Ä8iSfiSSaSS8^8 SfeSKRSe8fcS2ï8^S32S; «or^oj^OKi —Kiir»o>ooooivi*-ioor^*-Ki'0«mfMO‘^>oi\iOK> O* IAKf\JKi*-**>0fVJ (M •-r-infVIKl K) N-*“Oj«O>*>0 K ^K)K«~co it•»«'g*•£ rMtn^ooK •>oívi*-oi OOOflQrg'OfV»OKirsifN4f\iiMOQOOfVI(NifNiOfOfOKir\/0»OnOrj ‘0”U"‘*-Kl«“"Î>*inN* in rvi^>r *“Ki0^rgi'04r>f-^' •'^ ooouoooooooooooooooooooooooooo ; I KK 00O•-O; O >lS>'0'?'*m 00 O - —^ i3-OaoI5i3J3i5^-Ûi3i'8i3‘8i3^^"-oio^)‘8^ — IKIKIKIKIKIKIKIKIKI>#KI W N» • V OÍ O «0 0 J S % t i ¿ S^8O(Q : 1=^1 eu w ? ►- w KlW^ *-* C POU.Ir-• 10 8" Í3^"i a *o—uïv ^ •>XS «- cda « •OC- r.^ir.S C0 (NJwo «B o CO «> «I . O~>s (NJ I gl * • O 2: »• T9 (> w ö« C0 UC ¡L s eu Kik> U « *-• S s j? A 2 I O S S % (NJ S ß 2208 1994AJ 107.2184E 8 8 8 very largedeviationsfromthiscorrelation. with M>—2.5mag(i~2Xl0yr)arealsoextremelyrare. between theagesofMilandHyades,areveryscarcein near 2X10yrforNGC2437,3X102516and types GandK. However, afewstarsanalyzedbyLuck&Bond(1989)show H]=5.0 CN—0.12(Fig.6)andadispersionof0.06dex. the solarneighborhood.TheG0/3stars(HertzsprungGap) shoot atthecores,agesofBGandSGinclustersare dances arederivedfrom250brightgiantsandsupergiantsof spectroscopically byMeWilliam(1990),givingP[Fe/ heavy elementabundancewithadozenstars,alsoanalyzed the Fstars. 3114, and4X10yrforNGC2287. in contrasttoitssensitivityheavyelementabundance (f/,U,1T) =(+10.6,-13.2,-7.7)±(12.3,8.8,8.8)km/s. Kl, (Æ—/)=0.275to0.425mag,havemedianvaluesof 2209 O.J.EGGEN:GKGIANTSANDSUPERGIANTS v 204867 -0.284 209750 -0.214 159181 -0.281 192876 -0.217 108282 -0.394 107285 -0.234 101314 -0.234 89 96746 -0.293 88092 -0.318 87323 -0.229 88069 -0.297 67594 -0.230 59890 -0.236 58526 -0.249 57146 -0.244 31910 -0.297 16901 -0.290 4362 -0?288 © American Astronomical Society • Provided by the NASA Astrophysics Data System (2) Onthebasisofstellarmodelswithconvectiveover- (1) Theluminosity,reddening,andheavyelementabun- (7) Thecorrelationof[Fe/H]withACNfor100normal (3) BGwithanagebetween5X10and10yr,orroughly (6) TheCNindexoftheDDOsystemdoesreflect (5) TheMjindexreflectsonlytheluminosityofGKstars, (4) ThespacemotionsoftheBGandSGtypesG5to 1 HD mDel(R-I)¿“2ADel 20 222574 S 199997 132594 119605 63609 87951 84441 83609 74395 70046 79698 HD Table 17.Starsin16withGenevaphotometry. OBS COMP0-C I E(b-y) Referenc« tospectraltype(see notestoTable12). 0.077 0.078 0?127 0.057 0.128 0.093 0.053 0.069 0.048 0.077 0.191 0.422 0.245 0.392 0.200 0.401 0.256 0.307 0.259 0.211 0.166 0.377 0.241 0.402 0.252 0.340 0.223 0.371 0.179 0.360 0.199 0.393 0.265 0.403 0.257 0.419 0.235 0.375 0.241 0.384- 0.249 0.345 0.215 0?336 0?230 0.430 0.186 7. SUMMARY I 0.208 0.221 0.248 0.213 0.746 0.226 0.224 0.244 0.212 0.236 0?228 (R-Do +0.003 -0.015 +0.021 +0.027 +0.028 +0.040 +0.010 -0.003 +0.001 -0.002 -0.021 -0.054 +0.042 +0.094 -0.091 -0.152 -0.049 -0.054 -0.023 -0.100 -0.030 -0.046 -0.033 -0.062 -0.051 -0.076 -0.036 -0.053 -0.024 -0.056 -0.035 -0.031 -0.021 -0.044 -0?042 -0?077 0.050 0.085 0.045 0.052 0.106 o'Poss 0.074 0.067 0.121 0.069 0.065 10 galactic centergiveameanvalueabout0.1dexsmaller, away fromthegalacticcenteragreewithmeanvaluenear stars between300and900pcfromtheSunindirection an accidentthatthisdisplacementisthesameasin SG starsanalyzedbyMcWilliam(Fig.6).InFig.6,the are wellrepresentedbytheluminositycalibrationsadopted d) lieinthisrange,andtheluminositiesfromPLrelation, tivity ofthephotometricindicestoluminosityissubject SG, arephotometricallyidentifiedasnormal(classIII)gi- although withadispersionof±0.18dex. SG andBGincommonwithTable6thesedepartdra- common withaspectroscopicanalysesbyBrownetal. ants. almost preciselymirroredby31luminosityclassIIIstarsm (1989). However,thesamestudybyBrownetal.contains17 (class III)giantsanalyzedbyMcWilliamiswelldefinedand =0.15 to0.27mag(T~5600°5000°),wherethesensi- e 2 e (9) ThemeanvaluesofP[Fe/H],groupedin100pcsteps (8) TheBGandSGshowadistributionofP[Fe/H],from (12) TheGO/3stars,liketheGKobjects,haveM(and (10) Some20stars,spectroscopicallyclassifiedasBGor (11) TheGO/3starsareinthetemperaturerange,R—I 2.67 4.51 8.36 4.31 8.12 5.28 7.45 7.53 7.74 5.33 7^75 x -3.10 -2.78 -2.80 -2.35 -2.54 -2.23 -2.24 -2.98 -2.18 -2*31 -2.30 DDO My I -3.19 -2.76 -2.26 -2.44 -2.65 -2.55 -2.94 -2?44 -2.65 -2.75 -2.27 4C (-0.056) -0.005 -0.004 -0.022 0.000 0.018 0.006 0.000 0.024 0.013 O'POO 7 ACN G2 Ib/II G1 lb G3 lb G2 II Gl II G5 II GO Ib-II G3/5 II Gl II GO lb G6 II Sp.T. 2209 1994AJ 107.2184E Houk, N.1978,MichiganSpectralCatalogueVol.2(Universityof Hoffleit, D.1984,SupplementtoTheBrightStarCatalogue(YaleUniversity Hoffleit, D.1982,TheBrightStarCatalogue(4thEd.)(YaleUniversity Frye, R.,MacConnell,D.,&Humphreys,R.1970,PASP,82,1360 Fehrenbach, C,&Rebeitrot,C.1961,Pub.HauteProv.Obs.No.54 Eggen, O.J.,&Iben,Jr.,I.1991,AJ,101,1377 Eggen, O.J.,&Iben,Jr.,I.1988,AJ,96,635 Eggen, O.J.1994,AJ(inpress) Eggen, O.J.1993,AJ,106,80 Eggen, O.J.1992,AJ,103,138(PaperI) Eggen, O.J.1991,AJ,102,1826(PaperII) Eggen, O.J.1989c,PASP,101,366 Gieseking, R,&Karimie,F.1982,A&AS,49,497 Eggen, O.J.1989b,PASP,101,54 Eggen, O.J.1989a,PASP,101,45 Eggen, O.J.1988,ASPConf.1,editedbyV.M.BlancoandPhillips Eggen, O.J.1985,AJ,90,1260 Eggen, O.J.1983,AJ,80,998 Amieux, G.,&Burnage,R.1981,A&AS,44,101 Eggen, O.J.1982,ApJS,50,221 Eggen, O.J.1981,ApJ,247,507 Eggen, O.J.1980,ApJ,238,919 Eggen, O.J.1977,PASP,89,187 Drilling, J.1986,AJ,73,590 Dean, J.1987,SouthAfricanAstron.Obs.Ciro.No.6 Brown, A.,Sneden,C,Lambert,D.,&Dutchover,E.1989,ApJS,71,293 Bertelli, G.,Betto,R.,Bressan,A.,Chiosi,C,Nair,E.,&Vallenari,A.1992 tion. 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