1976ApJS...32..651K THE © line vey. used and Bidelman that the which but star and class1ficat10n narrow narrow." narrow; Star [of enhanced, is 8 4178 that Astronomy, plained Foundation. o (PO other * . (1967). F 16 . 1976. operated The D~lphi~ Cowley Del I~ giants, 8 a © AsTROPHYSICAL o Visiting the as stars IVp), the Catalog Cowley the of The by (Fe 8 Scuti Delphini The the metals American itself: having the o Delphini but a ities, most hydrogen main-sequence pariso~ are coexistence We ~?e but Four Subject hyp~thes1s (Cowley Cowley K-line American metallic r, 8 Delphini This as only (1968) late by Morgan defining (1965), are Fine whereas Y Inc., Student, difference Delphini variables stars coincidental. equal may argue stars the 8 (Cowley (Cowley of 1965) II, "The and s1nnlar noted a of description A Delphini classification. clarification abundance type Astronomical spectrum headings: Association under s~ndard Fe some states star] and ~oexist using and line metallic JOURNAL these on I. who H and perhaps that Astronomical and Kitt II) stars model paper ,\ reexamined of spectrum to INTRODUCTION and stars listed the is to Cowley 4417 resembles et spectrum contract 1973). between and Crawford stars that pulsation ionized Am have Peak designated slit pulsation Abt rather the stars, from al. We in basis were stars K "like Society. stars: SUPPLEMENT is line for for ,\ METALLICISM are of "the analyses (Ti by th~ir star 1969) spectra, other but evolved National lines. expanded of 4150 peculiar (1972) suggest Universities (1964), the University an with of _of the including Danziger star." are small." metallic-line defined II) calcium the the 8 and All is metallic that did abundances Bidelman's and bmary 1971) in Del." objective-prism 8 t~eir (Zr stars and metallic-line is Hydrogen rich rights presented. Received the 15 MKA Del metallic-line classification classify Ap the Society OF of and Am not that Observatory, weak, of diffusion spectra SERIES, who It II) of in metallic1sm National reserved. at;>u~dances, eight The and that related as They star an lines description of is for line mc1~e?ce. are shows THE elaborate and stars. the changed the 82 o Texas classified system further a 1976 F2 Research as similar 32:651-680, Del abundances, class especially 14 stars spectrum ,\,\ - Am anomalous-abundance Bright metallic­ o in class AND lines are (Cowley Dickens Five Printed DONALD • IV are are DELTA Delphini stars It to Science of rather February which stars: 4173- at which Provided itself type very is ABSTRACT sur­ star was was and the "in Austin, the are the the discussed. for of ex­ are on by in Some to of A position argued in PULSATION: is a U.S.A. the classical o stated 651 W. mutually 1976 23; Scuti DELPHINI stars and o and of KURTZ* Delphini It they th~ classify class main teria possible poses, Scuti and is MKA We the metrically mterpreted with ~redths spectroscopic sion element cannot ate in Smith Watson served dence, abundance data late revised which He that December by in the that and McDonald We Following 1s - and the a Am main Ca K-line II the use A the with these also of to exclusive classify spectra stars: o for V. sequence, classes photometric use similarities ionization 1976 supported, peculiar o (1971, it radiative abundance the one II and be Delphini (ft, some the stars. build of the (1970, o Delphini AN diffusion stars Malaroda was NASA confusion H sequence noted 8 STARS amplitudes Delphini the used abundances variable low-temperature a Mv) April and o as metallic-line early patterns and Observatory Cepheid Scuti o the which magnitude similar Scuti ANALYSIS have suggested classification; 1973a) a stars A are pulsational Delphini 8 among 8 1971) plane, with interchangeably. metal-line qualitative 12 Scuti that initial zone K preference Scuti zones. stars F Astrophysics to and stars, anomalies, shown variables could between lines star stars should as a classification stars subgiants (1973, the between periods instability used to all seen and inferred between generally luminosity classification the stars o calculations the are are relative Ba classification that (Baglin but that are This are of Delphini. - to account within Smith variables implications his classical spectral in be different II o 1975) model the for spectral have cutoff are, the stars: evolved weak with we between star element Scuti their of the clarified. model the and extensive rotation the the o two, believe to strip et less for (1971) 8 3 abundances abundances uses Scuti class Data and peculiar for for pulsation for temperature metallic of 8 al. four giants Del of H e agree We magnitudes pulsators. types. diffusion­ lying to Am classification from types metallic­ than as Delphini explains the 0.5 where Michaud to 1, diffusion the the 1973). the refer the veloc­ of itself-that that will 8 suggested variables brighter com­ He observational stars System refer Am and in with Am the MKA the A2 Delta Delphini a anomalous MKA spectra line 1, be the to there it few They that domain, 5 and and to the stars shown, crosses dispar­ (1970), photo­ depen­ and occurs hours, of exten­ stars. type. Scuti than hun­ stars pur­ that that is cri­ FO. ob­ the the are the is, to in a 8 a 1976ApJS...32..651K . 652 fusion The and dence the or or diffusion for overshoot do that, the that, As sinks 10- (ii) (i) Baglin known Am the the the that have rapidly pulsators. plausible with be (1976) eight four can the the rotation, what plausibility paper phini pendent subclassifications and class IV, nature to tions as on and 8 Breger In Some The Delphini convective our they related not. pulsation the © in not 5 metallic-line these driving Am 8 diffusion the physical coexist? pulsation H-R stars above V, pulsation. they major cm been in § Am-like within is of for o out comparison stars Delphini a American we indicating understanding II velocities o have nature exception of Delphini (1972) are from correlation known a star Latour pulsate, and Delphini s- of stars information stars. may pulsation, in we the and may will star (1970) of 8 diagram from labeled the to This 1 and used the mechanism radiative drawback of each , stars, Delphini in shown the the analyze If VI nature both disrupts mixing the 8 whereas to begin of in the not in and 8 spectra, have the Photometry, and which In about stars Delphini compare 8 so, the leads et stars. Delphini the the in He are and which stars present of to showed diffusion occur He whether of Delphini 8 stars pulsating be Appendix the and II. al. Astronomical standards. diffusion to this between what where He and that the Scuti these to evolved Vauclair the 8 proposed II of predicted on are able uvbyf3 II about of diffusion he us zone PHOTOMETRY the the Scuti stars In the and Am (1975) ionization of answer there II are exclusion for § ionization diffusion one the paper. that metallicism to metallic-line the other § also to it VIII stars effect ionization hypothesized cases. the pulsators. that, binary the to o extreme stars III stability pulsation one stars model a with pulsation produce stars, Am stars. photometry 8 are metallic-line sufficiently these ask, metallicism Scuti therefore, might from hypothesis velocity spectroscopically occur A is suggest the abundance large-amplitude Delphini et model coexistence these Section are is explanations to does 8 does in we There and stars, subgiants little and uvbyf3 incidence Is Scuti occurs, between al. In a zone, relationships however, stars be variables? Am for zone. discussed. general, there. stability define a against discussion and Society there zone § questions. their occur the an this scale and (1974) and on in is priori IX that theoretical but is A stars. star photometry provides which VII (Breger thus stars? as that their and of that 8 at Am phenomenon 8 Several the helium we have may stars, related the analyses a Kurtz of significance the metallicism is Scuti Scuti and the among convective present applied the relative appear Am necessary turbulent region are postulate speculate mentions plausible rotation. calculate damping diffusion order Some Sections implica­ What classical the star, element • may various defined disrupt 8 helium In among on 8 of giants either stars. 1972) stars. more Provided inde­ sinks Scuti et stars stars stars Del­ evi­ dif­ this the the the no al. be or of of to to to of of of is KURTZ from subgroups The and roda used by phini stars. stars second for Crawford class later implication slit tained two the system bright and of 7928 overlap and 2094 al. 2100 2557 2255 4760 man 8322 8787 8102 along 5017.. 6492 6561. 3185 3228 3265 3649 7859 7020 7984 1706 1971, 1974 University by 421. HR Table Observations * each 1969, Bidelman spectra. convenience Fraquelli Reference ...... subgroups, McDonald September first the the ...... (1965) (4) reclassified we to slit are stars. They .. (1975) with ; 8 by group from group. (2) Cowley help find in 4.27 4.53 6.44 6.44 2.83 2.88 4.72 4.30 4.71 5.08 5.03 5.37 5.98 5.28 5.06 5.68 5.88 3.54 6.34 6.30 6.38 6.67 1 source Delphini NASA spectra group astrophysically (1971), v the based lists Malaroda are They the about of and apparent They 1974. BRIGHT for it a) determine (1965) Lindemann Faint and we b-y 0.189 0.160 0.253 0.191 0.180 0.108 0.130 0.208 0.184 0.254 0.118 0.259 0.221 0.178 0.214 0.152 0.257 0.204 0.196 0.174 0.224 0.116 author stars convenient 1973, Texas classification the 8 so were we uvbyf3 the by of Observatory by of by on are Astrophysics Morgan will and have the stars. we which Cowley their 8 photometric Delta discussion will DELTA Cowley Cowley 1973, (5) originally their from Delphini stars 0.169 0.175 .4 0.644 0.242 0.231 .8 0.744 0.186 0.263 0.211 0.215 0.142 0.186 0.180 0.151 0.197 0.171 0.230 0.221 0.193 0.218 0.162 0.209 0.176 0.203 obtained visual refer physical TABLE reiterate Photometry for Volksphotometer on m1 Morgan mv whether refer Table spectral-type related. 1975, apparent Delphini and 1975 and classified DELPHINI the objective-prism to have > to and and et 0.913 0.764 0.913 0.656 0.996 0.744 0.998 0.674 0.830 0.630 0.831 0.937 0.952 0.853 0.897 0.685 0.890 0.731 0.786 1.023 magnitude of classification: break 6.4 to 76 1 C1 as classified Abt al. (3) nature faint only, and Hauck that 2 on February Cowley those Cowley indices as cm the mv the mag. lists Data Cowley In (1969), of Abt stars 1974 (1972), visual 2.766 2.746 2.780 2.724 2.830 2.741 2.768 2.799 2.726 2.749 2.733 2.775 2.753 2.789 2.733 2.768 2.840 2.715 2.706 2.790 2.753 2.739 STARS them the the o 8 < with faint the discussing members telescope. /3 of Delphini the stars 1972, (1973) Delphini There classifications. 6.7 subdivision bright (1965). as System the of September between (1965) and attached Cowley up (1) 15 magnitudes no indices 8 and plates o mag. Reference* the (6) by members Delphini Delphini Cowley into with Crawford is a 2, for Vol. 4, 2, 1, Cowley S of Mala­ Bidel­ or uvbyf3 priori 2 2 4 2 5, 3 3 3 5 2 2 5 1 1 1 1 1 1 1 using some these Each stars 6 5 5 Del­ The two and and ob­ 6 the the the the Fp 32 to is et 6 1976ApJS...32..651K No. served from efficients observation grations giving Thirty tions. to were (b (1970). and and Transformation in u system phini c is tion, using sequence is reddening excess-versus-distance of Crawford's Figure to dashed ± 1 11 b) 0.009, Color both For transformations not intrinsic - a = Mv © an 4, /3, 30 A preponderance y)o determined stars ±0.02, absolute the the American 1976 Mean a while for stars appropriate uvby the in The H/3. was error Comparison line 1 in excess, and total = were (ZAMS) is above each law the 1974 one standard standards by color, ing 223247 213634 213143 179641. 172743 2.943 mean in done (1970) as consisted 25515 47606 69682 30110 39390 72792 18460 81772 78388 a standards a u 3448 7119 McDonald ub-y in *Classification 8 applying assuming of applied color Figure to same filter plot close star magnitudes September Eb_ HD = 1 (2) (1) of calibrations, Bidelman distance ...... 80 ...... on ...... using - (b errors ..... Astronomical the as = ± and calibration 11 because of in is of f3 s term , - 0.011. of stars manner. as (Crawford 1974 can given ±0.006, 1 integration the relation - the of to program Indices ± y) (Crawford Eb-Y Crawford's linear represents these, that positive flMv (in 0.3 0.09oc 0 Observatory the sequence four was be f3 1965. , 7.43 7.53 8.20 8.46 8.64 8.40 8.96 6 6.47 7.80 7.81 7.63 7.56 7.59 7.29 8.18 8.07 modulus September for in in v and mag) and by can of mag, Eb-y calculated versus 1975 = and col. terms included relations Extinction a if consecutive of 1 O"m Crawford the all b September stars et 8oc mean be - color one 1 per (7) time - which the = we the f3nf3wybvuuvbyf3wf3n, and al. February = (1975) 0.2om patchiness Society 1 three b-y 0.195 0.199 0.219 0.238 0.184 .0 0.205 0.237 0.205 0.230 0.217 0.130 0.192 0.176 0.175 0.254 of 0.190 0.154 0.217 calculated . y distance 0.46 of according METALLICISM · (3) star to applies find 1966) ±0.008, The 6 expected zero-age Temperature extinction reddening the in in for excesses. Barnes for the about and corresponds 1 and mag determined the coefficients each • calibration nights FAINT 8 H/3 the that rms 10 y, were In standard observa­ 15 • a applied m derived to Barnes s b kpc- index: of o 0.221 0.183 0.210 0.231 0.195 0.202 0.228 0.168 0.223 0.208 0.237 0.200 0.233 0.192 O"c 1 filter. 1970) mean using 15%. addi­ color data. Provided there error main (4) inte­ m1 DELTA - Cowley Del­ The and 1 ob­ law co­ are the = y, TABLE 1 • AND DELPHINI and 0.787 0.817 0.701 0.778 0.735 0.712 0.729 0.754 0.714 0.726 0.730 0.758 0.791 0.751 0.821 1.000 indicating The in may A which negative reddening. some stars a can in interstellar more tially stars, by assuming represents o Crawford's 2 w (5) r·02. by C1 Cowley -.02 - plot Delphini PULSATION Two FIG. .08 .04 .06 . and which 04 the weak o~--/ account the r---r--r--.---.----r--r---r----..,-..,,...---r--, STARS o also '------'----'---'-----''-----'--_,__ distributions filled distant and both of of further 1.-Color . giants) F ___ stars, • 1965; a color • H/3 ro NASA f3 the the the account ...... giants mean metal for 2.753 2.709 2.738 2.813 2.757 2.803 2.723 2.697 2.799 2.755 2.761 2.760 (1970, 2.755 2.850 2.771 2.755 versus Some in • stars. . (~ computed medium. - indices objects, - expected for large ...... hydrogen ~ by classification HR • / :• a excesses. • supports or reddening . / __ excess, line group 1975) the // of selected Astrophysics b most line for ro 1974 of color these - blocking as radiation -'---~11------•---~'- may • Spectral color It from their F3V calibrations F3V F3 Fm FOIV FOY FOIV FO FOIV FOIV FOY 8 8 8 8 8 ye type* type* the y E blocking QI ~ might (7) of Del This Del Del Del Del 0 lines of the STANCE and (observed) law is -y, III III • stars in from be excesses, excess Am three the color uvby{J indicative, col. versus m with thesis due could HR of in (pc) be of have • • color stars (8) Cowley their (as the E ~ in versus expected a excesses. apply. groups 0 Data 2100, • photometry distance Spectral -u that _ cooler accord- possibly for Am part 8 8 8 8 8 8 8 8 8 8 8 especially 8 8 8 large • in primary (8) .. Del Del Del Del Del Del Del Del Del Del Del Del Del Del ~ spectrum, and = _._____. excesses • the the distance however, The ~ 0.46 reddening have to et System ...... are om companion. for ~ a ....-- in Figure interstellar _ o al. Am dashed mag be • group 1 Delphini . a the are __.__ assuming unusual indices, similar, for (1969). ~ caused relation binary in which kpc- stars) 8 I par­ that 653 2 the the line Del (as • .... ~ of is 1 . 1976ApJS...32..651K and The tion late (Breger " cators temperature severely mann 654 of of chosen HR 1952), 2.70 2.80 2.85 2.75 metallic FIG. FIG. Since The HR the © solid b a A 2100 and - for group American 2.-Comparison 3.-The description metallic H,8 but 1968). 1974. to y line as H,8 the Hauck = line discuss is index, + • • nothing x does of .10 2.943 represents indicator The Am o Bright A-Fm Faint a does metallicity spectrum Del Am line known (1973). 8 x error c) b 8 which - Del the Del of stars, stars - not Astronomical star" is Metallicity f3 o of y, without o bars known the calibrated the for Del The spectroscopic m, Delphini suffer the taken and index, .15 is should nor -makes .24 . .22 . .20 + .18 .16 26 28 are these rich itself f3 solid b-y for from and the from drawn 2.90 about m from and Index a 1 be stars (Cowley , lines om1 b stars group in one reddening, - (Crawford a Cowley similar .20 to the the •• Society or •• more line y represent • than binary further include suspect + • x temperature OC1 o of •• • 2.86 • • binary Faint Brighi Del Am et blocking A-F et terms. • • to b meaningful al. • • 1975) stars - 8 al. 75% 8 (Nadeau that we the in • that 1969)­ Del • • III • Del y. nature .25 • (1969). +• x terms • Provided have • mean compared of • stars indi­ rela­ of 2.82 the • as • the KURTZ a ••• •+ • • m1, sample x f3 •• • • • f3 with • m fied domain. g?F5 m m have to the with relations position but plot. stars 75'7 for from are and dices catalog imply is the mal metallicity value but phini Second, some stars, metal relation 2.78 by ~ 1 1 1 • I About Some Using • a from x • giant • indices a index indices 0 we a main-sequence southern Conti scatter the • metallicity. plot S the sample several do Two •• of • giants, and been of stars at the random we a Delphini abundance • give •• +. which ~· • of the high for other not caution the in the some stars • for Crawford's NASA of two-thirds • They have indicative m F6 1968). of index, of 2.74 d) Lindemann them the as and field drawn of + x sample of 1 m same m have x of the main-sequence the metallicity the ~ IV, the stars, index. 1 it Am 1 Position (Hauck one-third sample of (,8, the plotted decreases x them versus stars by are is mean have special field-star A must stars, mi. rest Astrophysics respectively abnormally x the ,8, stars m ma.y in few in + field-star Malaroda used value we 1 near of of so (Crawford ) First, 2.70 (1970) many lying might relations do S with be plane of been selected ,8 in 1971; HR of increased in the and that notice have have in Delphini to for do relative not the the these Am used Field at Stars the and those in S 7859 define some of error Hauck be a calibration appear relations and the that previously (,8, Delphini Baglin necessarily main-sequence not an cool high (Hofileit were from the here (1975), (,8, giant stars the 1970) Hyades in enhanced are Mv) stars, and S to their m metal Mv) inferring ,8. stars Data yet of Am the bars Am derived. plotted for Delphini m the border 1 the (1973). selected with and to et The 1 Plane index HR the have relation. observed their indices catalog may plane spectral but domain stars main main-sequence stars. 1964). very al. have encompassing line for of System imply classified in an metallic-line 8787, high in the of 1973). interesting metallicity The very Mv the not the very lie increased blocking, stars probably from the sequence Figure the Figure relation, of the As (Milton normal Vol. type. Hyades m in within a o classi­ for Linde­ them, apply mean large faint 1 near Del­ high nor­ they Am and For this the in­ as 32 A 3. 3 1976ApJS...32..651K No. classified stability mean Cowley Mv from stars the boundaries (1970), few quence A 8 so and and crosses sequence osity-class Figure 2100 1706 4760 3228 3265 3185 7020 1974 5017. 7984 7928 Faber ± 421. 3.0 2.0 1.0 Delphini FIG. 0.3 The subgiant • classified © 4, exceptions, (1) ...... •...... internal early HR Cowley relation ...... in ...... A2~/ Allen mag. ~ 1972, 4.-The American 1976 : I I I I faint I I I I (1965). I Baglin 5 I I while strip I (Baglin represent I Figure 2.86 ll show stars Del F III stars (5) ZAMS (1963). and The of is (Baglin 8 main-sequence (1965). by et the uncertainty The personal star. Delphini taken faint by the much and 5. et to al. giant in lines both The dashed the both dashed 2.82 al. be P Astronomical instability 0.087 Figure 0.060 1973, 0.135 0.097 0.141 Const. Var.? 0.153 0.194 Const. Const. Const. one, from et ll (day) x more The faint a 1973). stars, estimate. Del ZAMS al. Bidelman of Bidelman homogeneous . stars f3 (2) HR Allen lines lines 1973). luminosity 4 bright in stars. scatter. 8 Kukarkin, while and 2.78 The and in Delphini 2557, is strip the delineate (1963). represent • The Figure as (1965) Crosses the error AMPLITUDE 8 •/ (1965) subgiant FO • several xe, Mv given . Most is x near (mag) • Delphini Society luminosity 0.080 0.040 0.100 0.35 0.050 0.290 bright , VARIABILITY Efremov, METALLICISM a class group and the stars 2.74 4 calibration bars ~, bright, represent the the by seem, appear and ,'' are observed Cowley 8 x stars. are , Crawford that represent ,' of observed Delphini main F stars , • Cowley and class ,' lumin­ • with late main­ taken , Provided to AMONG ,' were 2.70 stars The and Kholopov , se­ in­ IV , be of in A TABLE 0.003 0.002 0.004 0.002 a mag AND DELTA CoNSTANCY lines have fore thousandths variability variability. variables five existence Others, outside Figure 8 of and 3 1958, by 3.0 2.0 1.0 PULSATION FIG. Some DELPHINI Delphini them, 8 are the stars been members A2~MS ~ (3) Set I 'Y + I • 5.-The I • I I I I I 5. the 2.86 Suspected Variable Constant the not however, of 2.6 4.0 3.0 1.3 Breger NASA hr of itself tested Table p all from I characteristic same STARS tested The Pup the the stars observed + have of bright (HR of variable for (private as 8 8 3 which (HR a 8 Astrophysics the Scuti is .2 2.78 2.82 Delphini which in are light relatively Delphini SOURCE* magnitude, 7020), e) ll a Fig. Del 8 listing 3185), 2 3 1 1 1 3 I I 3 3 1 I instability Variability communication), constant class. Eggen variability. Scuti 4. of stars, f3 have are stars pulsation, stars of large 8 + members class indicating (1956) been . Del while the FO--...._ to show Data ,( The strip v 41, which amplitudes. 'Y • / data sin of 33 25 80 32 93 70 itself 80 90 17 14 less ~ / tested 25 / dashed announced 2.74 still (4) and i variable / of periodic the System as / on than / Danziger are (HR the • / stars others are shown / . all ,• for and SOURCE* original 8 / a 7928), / • of there­ Three stars. 1, which Scuti 2.70 / light light 1 4 4 4 1 1 1 1 solid 1 655 few / 5 the the and lie in 1976ApJS...32..651K 656 as effects, computed line in stars classified and of of an due that range half because stars clude, mal magnitudes 1974b). for Conti classified of the range but be 8 v relation sin Delphini The The Assuming Half f3 Fm. normal some a f) uvbyf3 pulsational astrophysically © ({3, light many V A V to with m most blocking i of temperature are can stars in 1968; 1 American however, of m Summary 6.-The preceding Mv) increased or of between indices the 1 it luminosity cases, spectroscopically very stars, metal-rich as variability, normal-abundance photometry. index the be a 8 are stars. of color is plane stars Conti of Am normal combination Delphini normal the attributed labeled. relatively bright little and rotational the variables temperature these have even indicates that and excesses are stars faint metallicity, than sections parameter 1970), Astronomical 8 homogeneous because, dependence from by compared two 'lil 8 Delphini .=: normal a the Discussion ·;;; these Half masses, "'100 c E > and stars Delphini are have 8 much Cowley 160 140 120 We velocity 40 insensitive 60 80 20 parameters which of Delphini to class Hyades that of of in six have the as H023637 8 have the them reddening, is have HR8584 . • m • these. . for for ~ abundances, Delphini most more uncalibrated . • 8 • • stars. the •• of .02 some V bright 1 stars a • • versus is • • • HR114• with Delphini and on 8 stars of shown < m single-value to the also luminosity are these . • .. • main HR5017 Scuti group calculated 1 suggested HR3265 stars 0.230 . the indicates luminosity We of class .04 to compact indicate indices Society Cowley of • listed We the amplitude 8 8 have within the Photometry • stars reddening eHR7928 Delphini Delphini the have are that sequence, class. have line III. .06 field on stars cannot (Milton • • in since HRl287 8 been luminosity 8 that within known . Table with (1965). the the The that the chosen Delphini HRl706 group blocking Delphini class that function absolute been .08 Several, star • (Breger . are • of • low about tested range stars, Provided basis stars pulsation stars faint con­ they nor­ Amplitude 1 and and not but HR3185 the the or, re­ IV .10 as rotational • to in f3 KURTZ 8 Del .12 (mag) plot stars. photometry class, it the thousandths however, similarity strip. fore assume a light stars stars, stars stars same that stars. stars. (1973). pulsation, among pulsators, both are all v have mean by HR2107 velocity sin particular .14 is Because Before Figure • for of present metallic-lined. necessary the slow evolve III. i is are variability all relatively of the region the it Danziger the rotational and .16 The 53 that the is have is ROTATION, these 8 good NASA 6 discussing rotation slowly whereas to km are Scuti and conducive unsafe of slow is amplitude: into diagram observed star .18 late all of of of 8 a low to the s- quantities candidates small metallicism photometrically Del stars 8 a plot the for of the 3 and 1 discuss rotating A .20 rotators Astrophysics Delphini , magnitude, velocity v to Scuti inhomogeneity favors Abt Some although this PULSATION, sin and itself. stars all to listed shows rotation of H-R pulsational cool assume Faber .22 large (1975) class i, v of the pulsators, the early HR7020- sin of were while pulsation by A5-A9 comprising CC to diagram the boundary It are of stars a .24 in largest amplitude the And• relations Baglin (1972) there based i clear have is in physical has while versus general the 3 I listed F preferentially AND the Am certainly are the Scuti amplitudes. constant main-sequence shown Data subgiant correlation is done indicated and et only bright amplitude fastest as among have METALLICISM others 3 probably stars 3 al. amplitude of pulsation. by among Scuti the for stars the parameters Delphini the (1973). just the on System that Baglin shown incorrect must stars 3 rotators 8 3 the its 3 lie to and instability for pulsators. that. by Delphini Delphini Delphini rotation, Delphini virtually It between .3 spectral 3 a The outside The Vol. 3 a in of there­ which seems uvbyf3 selec- et stars, Scuti Scuti giant Scuti stars that, The few cor­ low the the for al. all 32 to 1976ApJS...32..651K No. anomalies that ti have In Am be stars. suggests difficult masses the strengthens evolutionary of and metallic-line {3, formed atmospheric classification abundance f3 abundances is Myron Figure program effective derived gravities Wells the with on and Table Effective b about Figure the spectra © worst intrinsically 4, stars effect giant - one-half been f3 The b American 1976 (1967) a) classical y, 6 and Smith IV. generally abundance - using to 4 that temperature were in when 250 and case, The 6 in stars. stars is y correlation identified, which of analyses ABUNDANCES the recognize BRIGHT the temperatures 44 6 28 20CVn 14 order y evolutionary 1970. p 8 1975, f favor did for a relation stars. most theoretical the parameters, K. Del. Ser Star Pup Mon Vir c prior Derived of checked information. • Tau Aur list And Breger's p 1 suspicion they may o Am Sources not indices. Good Pup, where ...... HR In ...... o slow (4) Scuti them Name preferred. characterize ...... of to of Astronomical ...... Delphini of DELTA to analyses We were agree, the Cowley on have slow stars difference test the exists. and 6561 at these publication. Atmospheric between by stars of rotators. (1974a, agreement are many cases In OF have Hy that higher stars ATMOSPHERIC the on tracks, rotators, the and DELPHINI fitting evolved a at rotational a the and were 2255 THE 1287 2557 5017 6561 3185 3265 7928 1706 4825 8272 8120 HR stars six classified f3 check weighted with These the profiles 114 Preliminary spectral along hypothesis classification these and on of of gravities performed for case these Crawford v o SHARP-LINED, b) rotational main Edmonds, they resemble the sin kindly the Delphini o which v Assuming the from b as pulsating calibration of Parameters was sin temperatures with Society STARS Del of types - i . for METALLICISM the DATA stars 7150 stars 7320 7500 7900 7400 8000 1500 7100 7450 7500 7840 7100 7600 mean velocities, two (K) Terr sequence. Table and as were stars i y were nonpulsating 1971, itself we obtained. < that provided many line the disagree, are: o parameters differential differential 40 FOR amplitude dispersion labeled stars velocities. are for Schlutter, was have probably Delphini subgiant 3 strength adopted (1) such (5) • initially normal km spectra and PROGRAM shows of of which logg (cgs) 3.25 3.9 3.6 3.8 3.4 3.4 4.3 3.25 3.7 3.75 3.5 2.5 3.35 Provided more used, Cowley That Hoffleit may per­ and and s - the the the an by 20 In in TABLE 1 AND et (km STARS 1964, al. 4.5 5.0 5.0 5.0 6.0 6.8 5.5 7.0 5.0 5.0 5.0 6.0 5.5 f1 justed we continuum variations manner within have than photometry, perature amplitude of of CVn, dex. in gravities. variations requiring sufficiently all abundances equivalent our lines. the with plate stants, systematic derived obtained of atmosphere the ther oscillator s- ±0.5 4 by 1969; (6) PULSATION Under Since The 1 AND 300 our a ) stars find line derived internal the values steady corroboration Cowley 8 the which (km km Values material, variable (2) K. temperatures CoMPARISON A v to and microturbulent 0.1 value. :5:10 many that sin blanketing, are will NASA mm 20 was photometric 30 36 33 27 22 20 25 Morgan the that s- 14 20 20 17 s-1) Baglin From strengths, with balance o of dex. scans, i the state. of widths small have effects derived 1 and Scuti microturbulent and error • in systematically and abundance the be - fl. assumption no of Smith correct, 1 While large fl.Terr all the log The Fraquelli effective this an plate treated· these Spectral et and been effective Astrophysics correlation the F2IV-V F3illp F3 F51Ip A7ill,F2V fitting FOIII POV A7 a a 8 8 8 excitation variables STANDARDS that in the Del Del Del Del contribute Del g range al. for derived contribute to we III estimated low for equivalent III (1973b) surface Abt the ~ equivalent ~ the analyzed these material stars surface parameter, (1973) be Fe the in estimate this 0.1 of 100 as Type 1974, 1972, microturbulence values use analyses 4.5 surface temperatures that temperatures ± these Balmer ionization have if are dex. surface K parameter. result + estimates 150 equilibria, exist numbers from gravities < and their indicate (3) of 0.08 about gravities. the by as o internal width and considerably of gt the K. effective These widths Malaroda Scuti abundance Data (7) the between gravity other compared Source• line (Smith g" < the higher atmospheres photometric of ± 6, internal gravity Conti 2 4 4 2 2 2 3 5 1 1 1 1 3-3.5 7.0 surface scale was 0.20 7 that Corliss-Warner derived equilibrium are that pulsators, profiles, late damping variations have He System investigators, derived for and We km accuracy temperature to the 1976) derived by dex the km typical associated dispersion the finds accuracy A s- the be was with estimate analyses a derived surface to gravity neglect model­ in s- 1 larger larger uvbyf3 range stars, from ± tem­ were were by con­ they Fe 1 657 fur­ this ad­ are the the 0.2 by to to of of a I 1976ApJS...32..651K abundances ture chan~e such estimate dances lin~s abundances and temperature, (1971,. analysis the program abundances We mately that with. radi~tion portion dampmg mumcatlon). presumed line-unblankete~ at_mospheres w1d.ths and pared la~or ured denved of CDC Observatories SPECTl Leonard KPNO two m.g widths. All and at densitometer turbulent by 658 matic ph~re gt= ~ qUit~ 32 Fourier . 0 Table Abundances For A the all © the "old" Aqr have of tabulated externally 1s plates 2.1 as of ~rrors 9 Ila-0 th~ mm treating strengths similar American 6600 internally changed the ~n1:1lysis km 1973a). 0.4 effects KPNO, author can on each m cancel _Fe eqwvalent each of About and m 5 which constants analysis stars the - damping intentionally spectrophotometric program b) and Kuhi, parameters. abundance is oscillator to the 1 s- a to 1, telescopes. plate were ~e , computer. to presented as due plates Smith's, a c) projected Data comparison Fe scale gravity, 1 ion with to Damping be 0.8 and internal by all curve close with to found with SPECT2, out be listing were relative Due half from by by Lick, The of yields II, used,. for Smith's, Deane material to traced Smith 10 mm measured, be lines of ±0.1 Acquisition width the ATLAS5 Astronomical constant. of converted t~e in and solar are of WIDTHS other the computed as strength Myron material Derived of incorrect of times to m the his of and present for Mount a log in the The were estimated possible slit reciprocal and Equivalent used gt systematic same the to growth McDonald error Ti dex as Appendix (1971) constants line the Petersen, scales on the this on variation published abundances we (Smith = Fe H and used, width microturbulence differential the II. rest triangles. the plates used for the 3 unblanketed log and Abundances the = No scale the if Smith f:om paper. consider star. This similarity profile Wilson to km and using (Kurucz in (Kurucz, soitd with associated comparison oscillator are program were to may 12.00 the were value reduction ions of its measured lines of error KPNO intensities the' University to 1971) our the s - used to dispersion and Reduction corresponds discussed widths diffe:ent B. of As ~nd for Observatory 20 effective the eqUivalent convective, Society source, be obtain 1 used. with ' generously keep rms in , A system abundance In Michel on of µm, and the analysis in the hence of derived our as applied derived all were 1970) Frank model-atmos­ between private complete the addition, the strengths star, the PDS 150 models conjunction scatter. many our We were number opposed same and McDonald lines standards. analysis equivalent computed equivalent programs, telescopes the using tempera­ and of of damping approxi­ Am obtained classical K, of • derived assume widths. Breger one widen­ of micro­ to metal- to micro­ model Smith abun­ Fekel'. meas­ Texas lines, these 2. taken syste­ Provided com­ oscil­ com­ with were with 8 and We our the 7 m the star the the list the of or or to to is KURTZ ternal for m standard systematic comparison and HR HR HR ~tars the will basis. and group HR the cussion in to in normalization given effective dance. metallic-line the sented widths systematic and differences HR the with scatter for good the Smith from abundances less lines Ila-0 rms were strong C growth,

TABLE 5 @ LoG OF THE DERIVED ABUNDANCES FOR COMPARISON AND PROGRAM STARS (log H = 12.00) > HR114 HR4825 HRB120 HRB272 HR1287 HR1706 HR2255 HR2557 HR3185 HR3265 HR5017 HR7928 9 8.18( 2).20 7.89( 2).09 7.91( 3).09 8.13( 3).24 C I 8.38( 2).01 8.05( 2).05 7.96( 2).12 8.31( 2).12 8.49( 2).15 8.14( 3).12 ("O CI 8.16( 3).24 '"I ..... Al I 5.08( 2).04 4.43( 2).00 4.66( 2).16 5.19( 2).07 4.80( 2).20 5.05( 2).29 Al I 5.45( 2).02 4.78( 2).36 5.06( 2).25 4.83( 2).37 5.49( 2).26 4.97( 2).15 ~ § Si II 7.05( 2).23 7.28( 2).37 7.06( 1) - 8.16( 1) - 7.59( 2).41 Si II 8.02( 2).28 7.14( 1) - 8.65( 2).39 7.80( 1) - 8.53( 2).17 7.58( 2).18 S I 6.56( 2).22 6.70( 2).05 6.45( 2).17 6.99( 3).13 6.89( 3).09 S I 7.00( 3).08 7.06( 3).13 6.45( 3).32 6.50( 3).07 7.03( 3).06 6.83( 3).18 >[IJ ..... '"I Ca I 5.95( 8).19 5.59( 7).24 5.50( 8).28 6.01( 8).28 6.07( 9).22 5.99( 8).26 Ca I 6.20( 8).28 5.91( 6).28 6.21( 8).25 5.94( 7).25 6.47( 7).29 5.69( 8).29 0 Sc II 2.84( 7).28 2.31( 6).12 2.68( 7).25 2.99(. 8).17 2.72( 8).24 3.11( 7).27 Sc II 3.32( 9).31 3.43( 8).48 2.92( 9).33 2.82( 6).27 3.64( 9).30 2.31( 9).21 =0 Ti II 4.19( 30).29 3.80( 35).25 4.05( 34).22 4.41( 34).22 4.39( 35).26 4.43( 38).29 Ti II 4.61( 37).31 4.45( 30).30 4.51( 33).30 4.20( 33).20 4.92( 38).28 3.95( 36).28 .....9 =~ V II 3.33( 6).25 3.34( 6).34 3.36( 5).18 3.65( 4).27 3.50( 6).14 3.96( 6).23 V II 4.01( 7).24 3.80( 5).34 3.78( 5).21 3.74( 4).20 4.26( 6).30 3.19( 7).18 Cr I 4.97( 13).16 4.62( 11).25 4.71( 8).13 5.15( 6).13 5.20( 7).20 5.12( 12).22 Cr I 5.30( 12).22 5.19( 5).22 5.36( 11).09 5.09( 8).30 5.62( 11).15 4.67( 11).16 rJJ- 0 Cr 5.11( 14).30 4.89( 12).23 4.99( 10).12 5.33( 12).13 5.38( 12).15 5.25( 13).18 ~..... II Cr II 5.50( 13).18 5.49( 9).25 5.59( 14).28 5.35( 13).30 5.83( 12).17 5.07( 13).20 ("O Ml I 4.40( 10).29 4.38( 11).38 4.40( 9).44 4.99( 10).25 4.82( 10).25 4.79( 11).37 Ml I 5.09( 11).29 4.77( 11) .30 5.16( 10).27 4.89( 11).31 5.34( 11).41 4.61( 11).38 ~ • Fe I 6.21(117).25 6.01(131).34 6.05( 85).32 6.42( 96).25 6.38(127).21 6.45(140).24 Fe I 6.69(151).25 6.46(119).37 6.72(126).26 6.49(117).26 6.98(154).26 6.13(146).24 "'ti Fe II 6.27( 21).20 5.94( 24).23 6.13( 23).18 6.39( 26).19 6.38( 22).21 6.37( 27).20 Fe II 6.69( 28).24 6.50( 21).38 6.72( 29).27 6.42( 25).26 6.97( 27).26 6.24( 26).16 '"I 0 C.OI 4.50( 3).50 4.38( 3).73 4.48( 2).59 4.85( 3).68 4.89( 3).74 4.94( 3).64 C.OI 5.19( 3).58 4.84( 3).70 5.14( 3).66 5.03( 3).45 5.49( 3).72 4.52( 3).57 ~ s: Ni I 5.27( 5).24 4.78( 7).25 4.84( 7).26 5.08( 6).13 5.06( 3).26 5.17( 6).30 Ni I 5.64( 8).38 5.10( 5).29 5.72( 7).34 5.38( 8).25 5.81( 7).27 4.98( 6).18 ("O Q. Ni II 5.05( 2).05 5.26( 4).35 4.76( 3).10 5.32( 3).18 5.07( 4).24 5.18( 4).23 Ni II 5.65( 4).28 5.36( 3).13 5.42( 3).17 5.69( 4).36 5.87( 4).21 5.10( 4).23

O" Zn I 2.76( 2).22 2.75( 2).13 2.58( 2).22 3.28( 2).05 Zn '-< 3.04( 2) .38 I 3.63( 2).02 2.51( 1) - 3.61( 2).08 3.35( 2).06 3.58( 2).06 3.23( 2).05 ~ Sr II 2.87( 2).12 2.81( 2).12 3.12( 2) .15 3.29( 2) .02 3.64( 2) .16 Sr II 3.85( 2).08 3.68( 2).12 3.47( 2).20 3.98( 2).23 3.70( 2).13 3.51( 2).12 ("O z Y II 2.23( 6).18 2.32( 5).48 2.29( 4).14 2.40( 6).19 2.33( 7).37 2.82( 5).33 Y II 3.30( 7).30 2.80( 4).55 2.89( 7).55 3.69( 3).09 3.20( 7).38 2.73( 7).35 Zr II 2.61( 5).32 2.42( 5).25 2.47( 6).16 2.89( 5).15 2.79( 6).30 3.13( 6).25 Zr II 3.63( 6).29 2.98( 4).14 3.21( 5).31 3.33( 5).19 3.45( 5).26 2.93( 5).20 rJJ> > Ba II 1.69( 2).08 1.43( 2) .29 1. 71( 1) - 1.46( 1) - 2.01( 2) .29 Ba II 2.75( 2).30 1.14( 1) - 1.80( 2).10 1.96( 1) - 2.35( 1) - 2.27( 2).18 la II 1.55( 5).37 1.48( 5).23 1.70( 6).47 1.94( 4).58 1.55( 5).15 2.15( 7).33 la II 2.62( 8).25 2.33( 5).46 2.04( 7).21 2.36( 8).21 2.73( 8).22 1.82( 7).04 [IJ> ::;- Ce II 1.90( 6).15 1.85( 6).37 1.70( 6).43 2.24( 4).75 1.83( 6).28 2.38( 7).25 Ce II 2.69( 7).27 2.31( 7).35 2.36( 7).32 2.76( 7).25 2.87( 7).34 1.99( 7).23 0 "O Nd II 2.20( 2) .50 1.82( 2) .82 2.29( 2) .34 1.84( 2) .07 2.56( 2) .32 Nd II 2.58( 2) .17 2.97( 1) - 2.46( 2).22 2.84( 2).42 2.78( 2).15 2.25( 2).27 ::r '-< Sn II 1.52( 1) - 1.51( 2).11 1.43( 1) - 1.98( 1) - 1.69( 2).21 2.25( 2).01 Sn II 2.36( 2).05 2.03( 2).07 2.09( 2).10 2.32( 2).18 2.43( 2).14 1.74( 2).11 .....[IJ ~ Eu II 0.92( 2).16 0.73( 2).12 0.80( 1) - 0. 97 ( 2) .14 1. 36 ( 2) . 20 Eu II 2.24( 2).23 1.44( 2).67 2.05( 2).26 2.09( 2).40 2.42( 2).28 1.58( 2).17 [IJ 1.56( 1) - 2.09( 1) - ~ Gd II 1.12( 1) - 1.37( 1) - 1.81( 1) - Gd II 2.37( 1) - 2.14( 1) - 2.09( 1) - 2.14( 1) - 2.41( 1) - 1.70( 1) - =~ The fonnat of each entry in this table is the average of the log abundance rJJ derived for each ion, the rnnnber of lines measured for that ion in parentheses, '-< [IJ ..... and the rms scatter of the abundances . ("O 9 1976ApJS...32..651K is program dances 660 (Hartoog, of the have S from only derived high-excitation as quence Si dances average ment mean significant Delphini In also The the II the © iron-peak enhancement not Figure Eu of American unaccounted an Si range S is which Eu Fe accounted lines, + II S Delphini one unreliable. abnormal Cowley, stars. 0.5 abundance enhancement abundance abundance Delphini 8 from or the elements which dex we (x two anomalous is normal Teff(K) = Log ~t(km/sec) Astronomical CoMPARISON will from for in for and stars not (,\.\4128, Mn Al 9.8 acts Fe Fe v y [N/Fe] Ni Ni Si Sc s c Cr Cr Co Ti Ca Eu La Ba Sr Ce Gd Sm Zr Zn Nd *The All stars g(cgs) HR the was in is anomalies compare II II II II I I I I I the II II II II II II II II I I I I I II II II II II are eV) Adelman considered as is plotted of the probably in effect THIS average 2255 study determined a are + enhanced, HR the ratio). HR lines, pseudomicroturbulence .8 8.37 8.18 5.08 4.50 4.40 4.97 4.19 5.05 5.27 5.11 5.95 6.27 6.21 3.33 6.56 1. 1. 1. 2.76 2.84 4130) 0.92 2.61 2.23 2.87 1. metallic-line 2.20 abundances 3.5 7500 5.5 OF 0.3 STUDY 55 52 90 69 of of compared 4825 and abundances 7928 THE with in dex. difference 1974). hyperfine Smith. (by HR Society partially and too to Their DERIVED Figure FROM HR to 114 SMITH(l971a) be The the although for anomaly large, as an This 4.86 4.24 5.22 5.21 5.43 3.00 6.23 6.60 6.36 3.12 7.00 1. 1. 1. 1. 1. 2. 4.96 4.90 4.38 4.89 significant, 6.09 .4 2.32 2.34 2.84 1. 1. 2. 5.0 of 3.5 7700 star 6561. Tms Fe is each with enhance­ 73 83 a apparent 39 66 92 72 40 69 27 program blended, splitting ABUNDANCES 7 the defined beyond • conse­ as abun­ abun­ STUDY effect show Provided The star five the the we we THIS TABLE KURTZ as AND 4.43. 4.62 5.59 3.34 3.80 7.89 7.05 .1 2.29 2.31 1. 4. 4.89 4.38 5.26 5.94 6.01 6.70 2.81 2.75 1.12 1. 1. 0.73 .2 2.55 2.42 1. 4.3 5.0 7100 the STUDY 84 78 48 82 51 FOR THE value not earths case the the do respect note run S stars, a and cally abundances dances HR main [Sr/Fe] S 1971) 6 HR4825 by Delphini less Delphini THE STUDY the SMITH(l97la) Am deficient quite of 7653, the Sc, of from that deficient sequence HR and STANDARD are pronounced 4.85 8.25 5.81 4.54 4. main-sequence 5.14 5.01 5.99 5.32 6.06 3.17 6.61 3. 7.13 2.81 1. 1. 1.39 1. to 4. 0.84 2.57 1. 1.47 2.03 of 4.0 5.0 7100 abundances Ca and stars, OF are NASA 79 92 52 54 52 09 77 this enhanced the as Fe the with 1103, lying (Abt stars SMITH stars of [Y/Fe] in much elements normal study evolved with while evolved (Smith, AVERAGE the this STARS the from HR is 1965; is Astrophysics (1971) (-0.08) (-0.23) (+0.03) minus deficiency respect +0.07 +0.03 +0.11 +0.19 +0.09 +0.20 +0.08 +0.07 -0.10 in +0.40 similar -0.09 -0.04 -0.33 -0. -0.18 -0.07 -0.38 -0.09 -0.28 as -0.07 -0.27 -0.01 -0.26 -0.23 remarkably main-sequence group abundances abundances the for 1248, or HR these Am 21 Am in has 1 Am DIFFERENCE* Smith private [Zr/Fe] these the to only the 114 of to stars been stars. to HR S stars. 2 value Delphini S AND metallic-line Fe of the 1971, magnitudes slightly anomalous-abundance Delphini communication). similar 5752, have abundance noted are of these in This Data The evolved Am Am five 1973c). quite on stars, HR moderating elements elements deficient before to System stars, stars, stars evolved the stars. Am above similar the 6559, for although The average Vol. but (Smith C, in abun­ stars, these typi­ than with rare The The and Am the Ca, the we 32 to of 1976ApJS...32..651K No. standard are stars stars. elements, stars ratios ratio stars by but in hanced main-sequence tion). FIG. Smith FIG. the not more © 4, is (Smith are in This (Smith The in American 7.-The 1976 8.-A dependent Am high with stars. these the similar than (1971) diagram [Zr/Fe] 1971) these stars comparison increasing metallic-line compared Am The 6 "Q)' 1973c), stars LL. derived ' a and on to showed + + factor + the + + stars. -.2 standards anomalous-abundance -.8 -.6 shows -.4 1.0 +1.2----,_,,....-...---..- +1.0 + .2 + .8 +.2 .4 .6 -.6 ratio Astronomical -.4 luminosity. o~___...... ,~....+<---+'---'l+-++.-1+'-.,.+,-cT--r~+-++-+<>---++.---±--~~-+~~~~~~~~---1 2 - the ranges those .8 .4 0 element abundances and Note t • 0 - evolved of luminosity of with the appears in that stars -' + :Ii the M • over 2, have again, five especially anomalous-abundance 8 : + even the abundances abundances, Standard the evolved in Am been Del a normalized : •+ to factor general main-sequence as anomalous in though 91-:-•-4-•-1'-+ • Stars stars. become Society the separated ...... the in METALLICISM Am • Stars Ca of normalized the -1.• •• metallic-line stars do ~...--r-....,.....--..--.,,..-.,...-"'T'""-r"""'T~r--+T""""'T'""-r---r~r-~-r- 8 to 1, the [N/H], 5. more Sc Fe Delphini not deficient into That • lying [N/Fe] [Fe/H] n, in 8 Provided vary and Del two Am the en­ are from to is, + • anomalous-abundance Zr stars groups Fe AND 1 *_ 11 in to abundances. to .... ~ effect strongly for earlier, cussion than not show are Ca the •+·~· 2 by according _.t-+-+-..--=1=-•--. be mag The PULSATION • anomalous-abundance 1, all those very these the does less Sc is + • above abundances similar for present coupled similar II, here. + ••+ NASA scatter of to the 8 Ti .. statistical the surface the Delphini Fe 8 II, .... • • ~ to • The to main Delphini in when 1 main-sequence to Cr abundance Astrophysics X e •• • -l. the those the HR HR2255 gravity of the + I sequence e well-determined 1 I T 1, + • = : • ~ • evolved 1706 = - - reasons, normalized HR five HR8120 HR7928 Cr [Ca/Fe], Evolved 8 Am • [Fe/H] +.,•: .. stars "+ 8 stars of 114 Del Del II, to + 8 • * Stars • ii+• the and + • Delphini and itself. and Am show (Smith, Mn Stars Am stars ~ • is x • HR6561 HR3265 that abundance. evolved HR4825 HR8272 Am Stars [Sc/Fe], .. in • stars • x intrinsic 1, to Data that with the Y t • • the • .,....."'T"1 the private stars. rather stars abundances II, their four • those • + + Fe Am slow System and and We abundance and, communica­ abundances under This comparison than in stars rotation Zr [Zr/Fe] argued the to same as II 661 dis­ but Am the all of a 1976ApJS...32..651K 662 in consequence, thought were 7928 coupled HR Abundance that performed plotted classified giana Smith ticular, (1969), classified in 15 dances the the the pares stars. stars. larities Mn tween [Y/Fe], not hanced 8 abundance and large may mentioned -0.26, 1965) Delphini We FIG. the Vul the © Sr-Cr-Eu anomalous-abundance Ba be associated 1706, the and they on showing not the in They and They have American the 9.-Comparison (private Ba are to along Am between Smith with stars we significant. in and to the Eu the with their as anomalous-abundance A4 two be have van't stars are HR by stars effect indistinguishable Figure also be plotted point analyses do do Am main domain abundance respect striking they Ap 8 (Warner [Zr/Fe]. with significant. Ill groups finds positions Miczaika ,...... , ~ a probably the communication). not Delphini with if 2255, ' not marginal is compared the compared Veer-Menneret with the stars (Slettebak of sufficient (marginal - were out -.e -.6 -.4 -.2 sequence enhanced 1.0 similar 1.2 Astronomical 1.0 8, .e .4 .2 .6 The in have Ott---+-~--+--r-t--:-t-r1r--r--i;-,,--r<- present the [Ca/Fe] similarities appear to two the of ...__ U of several is (Abt HR 15 (Adelman While Figure that 1965), probably Fe T l Eu, the ...... one neglect in ~ in only et Hg-Mn stars --'l:l'-- the evolved Vul, Am classes. The overabundances 8 the rather 3265, abundances condition I ~ al. both and and 1949), it to Delphini Am?) because of = abundance from by other large this and element between characteristics. ... ~ 9 H-R .L--..L. Eu anomalous-abundance due has have (1956) the be -0.09 of we (1971), 0.15 8 1973). is Am Moyd These groups HR 8 ... stars, than The Delphini metallic-line hyperfine the --1.1:1--11:1-1=1.__ shows star and similar groups abundance overabundance feel evolved very in by diagram, to Society ~ dex, been slow stars normalized the stars. for 6561, and and abundances the the Fe for Cowley deficient Figure that ~ this has and as studies 1973). different two is analyses many metallicism which > of rotation abundance to of well when previously which previously past [Sc/Fe] by stars difference quite Am its been and splitting, Y groups. suggests peculiar ...... U [Sr/Fe], • In the 9 --1.l:l---1 Farra­ is abun­ is as et stars. to show Provided This, com­ simi­ as o stars been with they may par­ HR too un- en­ Ap the be­ Fe re­ al. by of of of in = KURTZ i ... is See ---1 in ~ .. - the -t-1--1.jf-J..f-;+-~~~~~~~~~r----'--t the S ... ._ is each certain anomalous-abundance the the the ing cessed is s-processing times. to during are overabundant other lack there material may stars enhancement as all and elements overabundances is mechanism to than necessary text of + by ..... Z Probably The We expected 1.1 the ---' coincidental. the the the be support 8 strength for normal 8 in ... Z the the be star. --' Delphini the abundance and dex of is Delphini iron-peak conclude heavier relatively C T arguments core similar This a [Y/Fe] ... as ~ a generated. '--l:l~:".1:1-:"1=1=-"1:1':-"':1:1:':-=1=1-=1:1':--!1:1':-"':1=1~=1=1 apparent to no NASA carbon-burning abundance. [Y for l in I stage an ~ shown the only a to the evolutionary /Fe] this material during of is known overabundance generating the ~ real of elements. s-process, in stars absorb abundance Ba abundance probably the stars, l surface, : T I one that The of of N I elements I that i ~ well thesis. anomalies 0.5 anomalies Astrophysics the difference in anomalous-abundance = similarity = stars Fe, ~ C hydrogen o which hydrogen 8 or a) dex Bo the mechanism the 2 difference Figure Del being ii Ba T understood I [C/Fe] whereas , most Del ~ and U CH, HR3265 two similarities The the and must T l] I stars not Stars Stars in mechanisms tracks, stars ~ evolutionary are core-to-surface is patterns anomaly theoretically in observed circulated of HR of between ~ lines not and between during 6 Ba possible the seems and of the burning be Warner by the burning, the is £ in apparent s-process stars 2255 the for CN C, Data the are Ba were different in significantly ~ a free C other for to which for factor Ba the 8 along coincidental. circulating stars, overabundances terms ~ bands the abundance, which as show and to Delphini stage. during inferred be 11 measured neutrons the cannot System HR Ba 14 and stars anomalous- two 8 the in seed circulation N(n, normal is significant HR in of measured of stars with that Delphini no Figure give thought 3265 Assum­ (Warner Vol. the surface groups 2 origin, do s-pro­ nuclei which larger p) 6561, from large stars to core it that and rise 14 for the the so, Fe 32 of in C is 9 5 1976ApJS...32..651K No. abundance cited parent usually HR the the reanalysis (1969), from (1973), Our Four © literature present 4, 3265 equivalent in two American 1976 in Breger large previous along Baglin and of a plates, abundances 8 Ishikawa's for enhancement visual Delphini has with b) et (1970), widths abundance 8 al. HR been previously been Astronomical a Del the (1973). inspection McDonald 7928, Reimers itself. for data with stars. abundances to HR Al 8 Mn v Si s c Ti Ca Sc Cr Cr COMPARISON y Ni Ni Co Sr La Ba Zr Zn Sm Nd Ce Gd Eu Teff(K) Log each Analysis numbers Stars Comparison rerun ~t(km/sec) relative [Fe/H] analyses those In Delphini be We * II II I I I I II II I II II I I I I II II II II II II II II II II (1969), g(cgs) 7928 Abundances of Table ion. on real. Observatory noted derived consider Society the to our in derived METALLICISM are are our It 7 parentheses THIS STUDY -.40 and -.24 -.17 -.08 -.04 -.02 -.02 -.20 -.01 OF HR8120 HR4825 HR114 3.25 HR8272 4.5 7320 fine system spectrum .15 .42 .12 .11 .06 .41 .60 .38 .14 .32 . .24 .00 .78 .12 .17 .06 we by available 72 is determined THE standards. by derived Ishikawa Smith even compare this • from BESSELL -.32 -.09 -.42 (1969) normal 3.6 4.2 11 7200 Bessell coarse and ABUNDANCES .11 .46 2.7 Provided Lep DELTA un­ ap­ represent compared as of in from m TABLE a BREGER -.35 -.08 -.26 -.23 (1970) - 11 3.2 .5 -.19 -.25 6950 a 4.3 fine AND .11 DELPHINI Lep CMi the [N/Fe] gfvalues telescope widths scope are 20% that the ment pendently offer in cantly dances Sun, absolute FROM by 7 with data REIMERS -.33 -.13 -.16 -.16 -.08 -.05 -.18 -.12 -.04 . - (1969) Sun 3.8 7.0 7100 fine PULSATION Reimers's oscillator .59 .22 .29 .03 .11 3 .56 .33 .09 .54 .45 number 03 basically the its using our no less DIFFERENT from with 8.9 from for normalized effect gfvalues, standard NASA ISHIKAWA -.04 explanation -.21 -.14 -.13 (1973) 1. 1. for 1. 3.6 -.19 7200 4.0 A Sun fine 8 than .49 .53 .04 .04 .44 .19 .29 by . .99 .50 .84 of Ishikawa's solar four 71 29 52 24 A each mm these strengths analysis others. in lines Bessell, mm- is STUDIES the - agreement gfvalues of stars. Astrophysics other. mostly 1 ISHIKAWA* -.13(1) -.40(5) -.14(23) . - -.40(1) -.14(11) -.14(2) HR8120 HR4825 HRll~ -.27(1) 3.25 7320 HR8272 4.5 two fine used to .03(9) and .09(6) .03(7) plate .28(5) .15(2) .25(1) . .27(3) . .55(1) .21 1 42 the 40 43 equivalent Our study plate Fe. (4) was for (2) (1) The Reimers, is plates for OF we five Nevertheless, which the canceled abundances for this suspect done and with ions reason. are some discrepancy, are widths and a each with systematically Data for KPNO that out in ions Ishikawa, In disagree excellent which other. respect the for this derived System addition, and 2.1 equivalent the difference but absolute he We m signifi­ to agree­ which about abun­ inde­ used note tele­ 663 can the the 1976ApJS...32..651K 664 used, partially discrepancies strong from growth. from abundances, the provide While ysis from dances resolve results numerical data able dances. internal with We 7928 dances derived dards, due reanalyzed dances is In Bessell's by scopically of of deficiency classified ible HR Zr, the the standards star of one The atmospheric HR [Ti/Fe], Ishikawa's There an As Three © abundances this particular, the implication, and metallicity, are Sun, and to low VI. 3265, analyzed, of abundance to 3185, derived F2 Breger's relative ours, listed the as his has American the lines are the of the this our beyond also seem It five group the The any the THE abundances Ishikawa's IV-V due [V/Fe], consistency v of those (1969) are spectroscopically using HR small list is been abundances basically atmospheric used sin HR lower normal is and we data, in general difference, rare standard-abundance difference the less lying understanding in and difference ABUNDANCES to o parameters some analysis for abundances suspect. to 7928 real, which i (1970) star Table HR which HR in agreement did 6561, Delphini abundances the previously [Fe/H], large-amplitude which by the a) HR the clear o number data. earths the and as anomalies our effective and Si on HR Delphini (Morgan Astronomical with not 3185, HR by 1287, Smith Reimers's different are and in large agreement most iron other 11, 5017, 7, in are of [Cr/Fe] and model-atmosphere the the why standards, has good was in Breger's Nevertheless, we we abundance are 7928 in are similar feel 1287, which parameters of those the Sr the adopted the AND in of the similarity fiat do stars the peak for temperature OF differences HR been (1971 Sc have the recent normalized as derived quite shown all stars also 11, of and that agreement stars ([N/Fe] and different abundances common are microturbulent data we not HR II marginal 8 equivalent may of 44 the portion line [Fe/H] enhanced the HR o and makes 7928, Delphini and and ), HR reanalyzed is lower of shown Delphini Breger the done Abt feel Tauri different. 8 deriving analyzed) derived using have stars five are gf analyzed, 1287, list discrepancies. is in in similar, also 5017 analysis. Scuti in the the Ni Ba of used Society F2 the values 1706, all ratios), Figure we 1972) given that common is ratio ions analyses all in of with HR the with readily I [Fe/H] and with he to and II trend deficiencies be to only present quite HR give stars. relative IV-V make only width variables reanalysis feel some the of in of from stars are abundances used. Fe abundances In in the real. be among is 7928 Ishikawa's in the Ishikawa's one believable. HR respect our ours. 2557, HR this the available. velocities disparate our HR 6, the common. curve of although different attribut­ order that HR Table at member spectro­ and • discern­ the ratio is o [Sc/Fe] of half would of scales. actual a Sr, abun­ abun­ of to abun­ abun­ Provided 2255, anal­ (and, 2557, Scuti least stan­ high. lines 1287 The 114, few HR this run the Fe. the the are the Y, of to to of of of KURTZ 8. is firms in amplitude line. The group tion there we heavier effective abundance cussed overabundance dance different lies this normal recently Crawford abundances classify detailed b trapolation 8c by Al Mn v Ti La Ba y Si Sc s Ni Ni c Cr Cr • Co Ca Te Gd Eu Zr Zn Nd Sr Sm Ce log [Fe/H] - 1 HR the ff (km/ .ABUNDANCES do II II II II II II II I I I I I I I I II II II II II II II II II I < the ATMOSPHERIC about y, Fe g(cgs) There (K) star and is that sec) 0.28 low {3, for 2557 not with anomalous-abundance elements no abundance in it analysis NASA from temperature discovered and using ionization of A9 HR was v (1971), is of consider mag apparent the spectroscopically a 3.4 of sin is v 0.07 a c HR1287 manner that the 1 -.24. -.12 -.19 2557, -.14 sin 5.0 -.29 -.32 -.29 -.01 -.23 3.4 -.10 -.02 -.12 -.44 - 7150 0.20 III. mag trend determined NORMALIZED classified HR .07 .81 .18 .18 .13 .07 .10 .13 .10 standard are i, of for PARAMETERS of Astrophysics Breger's for mag. standards. high-amplitude i calibration lies in while this Crawford = HR Si A 2557 the this b) above pattern in the TABLE and equilibrium good 20 similar 11 and within the HR Our 3185, variability HR2557 numbers -.31 -.28 -.07 -.16 -.36 3.4 5.5 -.63 -.20 -.01 . - - 7400 0.30 [N/Fe] km star o is .03 seem .08 .59 .19 . .11 .02 .08 .42 .12 .09 .36 .47 3 .72 .38 .35 stars. . surface Morgan calibration 04 71 08 from TO abundances IN agreement early Delphini the 2557 analysis not to AND s - normal 8 Fe THE indicates to has to the o 1 to these main one The AND ratio Data Delphini HR significant, F be STARS the to and HR3185 sector gravity range for is calibrated be -.09 -.18 -.33 -.32 .1 -.33 -.61 3.25 - 0.54 -.29 -.22 -.03 -.05 -.15 6.0 -.16 -.10 - . - 7100 stars, .04 .18 .96 . and 1 .26 .17 .07 .02 .22 .04 .07 .09 partially 77 THE 06 of in be 5017 variable, by deficiencies stars large previously with marginally to sequence. (1974a, Fe. a System HR that progress. of this meaningfully ADOPTED of Cowley of be Abt derived pulsational and Ni stars. the 1287, We can Fe Figure star apparent HR HR5017 low, blended -.44 5.0 -.06 -.03 -.05 -.04 -.09 -.15 3.7 0.80 -.09 7500 as and Vol. Mv . .58 .02 .00 .01 .05 .09 .14 .00 .14 .07 .83 .15 .16 .02 excita­ an (1972) and 01 abun­ b) exist 2557 have con­ The The The and and this dis­ but ab­ the ex­ for for 32 of 6. a 1976ApJS...32..651K Mn Si Al Sc s c Ti Ca v y Ni Ni Cr Co Ba La Sr Ce Cr Eu Zr Zn Nd from from Sm log Teff Gd the to ture ment while using predicted No. stars effects c deficiencies line derived gravity Comparison log that Analysis be Stars [Fe/H] ~t(km/sec) p [Fe/HJ 1 Pup HR II II II II In II II II II II I I I I II II II II II I I I I I II II question. the g(cgs) © yields COMPARISON (K) g normality blanketing, 4, indices the Table for a = the the American with with his 1976 3185, as [N/Fe] abundance single 3.9. 0.65 gravity. which Fe higher previously effective uvbyf3 Terr FOR calibration three 9 the of THIS We disagree. p ionization we dex line -.09 -.32 -.61 -. -.03 -.05 -.18 -.15 -.33 -.10 -.17 -.29 -.22 HR HR8120 HR4825 HR114 or -.06 -.16 0.54 7100 HR8272 fine 6.0 3.25 ratio OF = Pup, . .04 .07 .04 .02 .07 .22 .18 . . .c) [Zn/Fe] 77 96 reddening, 72 09 the Fe temperature, STUDY compare photometric other have abnormality THE 6850 3185 These each Astronomical HR lower temperatures may be may for excitation b discussed is ABUNDANCES TABLE - GREENSTEIN derived K, Breger's FROM studies 3185, one of (1948) and the and equilibrium y, discrepancies our {rare than log {3, -.36 -.22 -.96 -.32 -.43 -.24 . - - or -.30 -.21 0.17 2.5 sun coarse slightly rare of (b VARIOUS .21 . . .43 .11 .07 .03 .63 thus 38 26 03 p [Ba/Fe] which uncalibrated indices 9 of derived of g in c - the Puppis abundances equilibrium, earths 1 calibration ET earths. = and the this § this NORMALIZED y) are yields AL. II. worst 3.5 0 enhanced, Society STUDIES is , star. yields suspect. surface ~ star and photometrically METALLICISM BESSELL may are abundances in -.44 -.54 -.15 . - (1970) (1969) -.20 3.2 6,800 0.36 n 6.6 coarse for .14 .09 The between 08 Lep better Terr examples is The determined f3 luminosity be for of this a still and tempera­ apparent TO gravities = BREGER • We as surface -.08 -.05 -.19 -.32 -.25 due -.13 [Fe/H] n 6.0 3.3 7000 0.42 a fine b agree­ p Fe Provided 7100, Lep CMi open - star, may Pup find feel the for to of y, AND equivalent consider two scales splitting, for excellent from abundances abundance, conclude a as correct equivalent abundances lies. The 2.1 Dickens HR kawa's with which adopted a disappear. Ishikawa's KPNO but similar Ishikawa Ishikawa yses. results with [Fe/H] 1.9 elements determined. dance in when possible elements and analyses lines growth when Since some C overabundances, HR abundance 1974), by The HR similar PULSATION slightly 1, Eu in m m the in the VII lines The 3185, 3185 abundances Al respect respect and Even this normalized normalized the of telescope this mild ,\,\4130, we as the telescope were 5017, [Fe/H] to reanalyzed = of corrections Hyades, the 2.1 d) the 1, abundances it NASA et these exception are apparent agreement that we abnormal. indicates heavier reduce which 0.80 the study, the has (1975). and other [Fe/H] comparison We all necessarily larger widths this abundance Si m though widths abundances is HR al. [Fe/H] [Eu/Fe] deficiencies similar The lower of to small, measured to 20 still anomalous-abundance enhanced, II, telescope these other slightly 20 studies consider 4205 dex, abundance is (1971) the the abundance 5017, 4 and our stars CVn, are from Ca the Astrophysics and in we 8.6 to not to CVn = A than find equivalent We from scale data for overabundance are = the the which Sun other of to that (Hartoog, 1, analyses this rare Fe. mm- ratio 0.67 Fe with [Eu/Fe] Among all in standard A Ishikawa's cannot 0.44 20 S are anomalous accompanied Sc concluded, the enhanced analyzed Dickens is those of have agreement has [Eu/Fe] [Eu/Fe]. shows apparent mm the from 23% Fe to in appear of common 8.9 normalized two 1 by among but Canum study earths dex. II, the determined his 1 not rare effects each is abundances for dex, in be all the abundance been are A - Dickens is plates. the a 1 ratio reanalyzed the of McDonald the interpret data run are larger in HR width in of mm- Okayama no the determined higher effect McDonald The stars, Cowley, earths, that to plates are et = other, well-determined all the in do reanalyzed the basic agreement, Venaticorum the Using of [Fe/H] . Data [N/Fe] deficiencies analyzed lighter among the with listed abundance be from to 0.65. al., effect 5017 of This 1 hyperfine this normal, the derived equivalent not Hyades. to by et abundance o than about lighter scale. these slightly plate might metallicity from Si and agreement Delphini and ratios, which on so are al. the ours, star System and Fe the similar their Again, in study. show is and elements ratios is of Observatory the Observatory 11 plates. we our (1971) from Ishikawa's from which previously enhanced all anomalies look is typical Table Eu from +0.4 has We data hyperfine only from Adelman however. curve-of­ with elements be different deficient We possibly splitting of and data anoma­ derived [N/Fe], suspect do are system similar poorly of If abun­ width metal stars, as over­ these anal­ Ti have than Ishi­ only real. very dex. find Our give and and 665 two one not has the the the the the 10. we of in in of II, . 1976ApJS...32..651K Al Si Mn s c v Sc The Cr Ca Ti y Ni Ni La Cr Co this Eu Ba Zn rerun Nd (cf. Sr dances larger Teff(K) Gd Ce tion. the Zr which used between star 666 scales. Sm due differing Mount this Stars estimated dard decrease dispersion, line Comparison log HR ratio st [Fe/H] (km/ The •Abundances II I I II II II I I I II II I I I II II II II II II I II II II II g(cgs) COMPARISON © analysis to numbers for Smith blanketing difference 5017, star sec) on stars. abundances according is American the than This difference in each Wilson our not dispersions in spectral is internal this difference FOR [Fe/H] we The l system ion. typical difference this in THIS and those in 973b -.33 -.05 -.04 -.09 -.44 -.15 HR -.06 -.03 HR4825 HR114 HR8272 HR8120 5.0 3.7 0.80 7500 OF consider analysis derived .07 .01 .14 .58 .14 .00 .01 .05 .09 .00 .02 parentheses .83 .02 .09 .15 .26 .16 excellent in between metallicity 2.5 STUDY Ishikawa's ratio ). THE to in 5017 dispersions = and Astronomical error of equivalent derived and Our m in the 0.80 the ABUNDANCES of TABLE from Dickens compared DICKENS is FROM is the respective telescope for are that -.12 -.12 -.02 (1971) 8.6 -.26 - 0.44 7520 2.0 4.1 sun of HR probably equivalent agreement calibration expected .11 .09 .23 .23 . .01 .16 [Fe/H] .03 .31 .31 .28 .12 dex, 18 represent the which index, reanalyzed with VARIOUS A from ± the ET 5017 10 data 0.2 mm used. is its usually widths et AL. with derived NORMALIZED respect correct abundance 6.8 we dex, from al. Sm - and attributable due plates the ISHIKAWA Society STUDIES 1 our with widths have Since A equivalent 1 -.04 -.30 (1975) sun 3.5 3.8 0.33 7875 of measured and .24 .13 .13 .38 .37 . .37 .07 .09 .21 .55 .23 .70 .49 .19 .57 .35 .87 although number data Ishikawa's 07 - = mm the to standard metallicity to to [Fe/H] no our of differential 4 the four - 0.035, is within ISHIKAWA* standard­ are A TO 1 explana­ between -.13(7) . - -.03(1) -.12(7) -.40(2) . - . - • -.30(1) -.44(1) -.04(2) HR8272 HR8120 HR4825 HR114 3.7 0.67 7500 4.0 entirely of similar . [Fe/H] .11 . .30(1) .14(1) . plates, mm found 53 46 to 09 49 08 05 Fe abun­ width Provided some from study stars. stan­ 43 with (1) (19) (2) lines (5) (1) (1) (2) the for an % - of KURTZ 1 interpretation incidence. line to three the stars stars, metallic-line Am respect and and anomalous-abundance duplicity, about dance gram lies HR two known bright Subdividing S stars; are conditions; Most may mechanism star 1974). of then be possibilities S 2100 4760 7928 1706 6561. 8322 by Delphini We In What If Delphini be the HR the in stars, stars ...... several Barker have (/3, the HR and 6561, the .... Table be short-period there on HR to of (ii) correct these have the of S S BINARIES to metallic-line to Mv) Delphini is able NASA S determine 7928, the may the a Delphini VII. each not 40.58 the f3 Three most so binary be 1706, 2.74050 Perhaps 3.789 2.292285 1.022768 stars P Delphini the and S must 1973). 11 suggested than S and possi~ilities: below. or stars, the stars binary plane, (days) it explanation binary five Delphini basis been to Scuti DUPLICITY be others that we of (iv) explanation AMONG are of is m of may HR HR incorrect, coexist the class, Astrophysics incidence the be stars. S 1 anomalous list We and binaries. which not VIII. these tested HR stars also the for of these star; DELPHINI the rotational stars. and stars abundance two 6561, be pulsating 7928, TABLE have that five THE are .L2/.L1 stars their possible S Am S we DISCUSSION diffusion binary five a 1706, ~1 S in AMONG Scuti are one (iii) which for for Delphini (i) stars mechanisms DELTA presently binary are S Scuti i.e., the We and note for This stars a for may are not stars, Delphini abundances, the binary pulsation. the STARS which 11 diffusion single abundance not anomalous pulsators the anomalous-abundance HR the discuss frequency are to the velocity, HR THE evolved abundance anomalies is DELPIIlNI seem pulsators. f(.L) 0.004 arise 0.037 0.060 been from (Rydgren consisting hypothesis Data suggestion HR abundance consistent evolved make group stars engaged evolved anomalous-abun­ (Abt 2255, is 7828, BRIGHT star from stars 1 thought tested to Table for 706, and Nadeau each Batten Preston Harper Young Frost System both? metallic-line STARS under are a 1961 communica- ti and as position be S among are abundance on) HR and in The producing a Am which anomalies Source statement of HR pulsation in Delphini metallic­ a et may that different with of the evolved evolved anoma­ yet 11 1961 1911 ; Vol. 1934 an known whole. (private al. 1952 binary a to Smith There Conti 3265, other stars, 3265, some these pro­ that 1929 Am Am not are the the for the be 32 in . 1976ApJS...32..651K ·overabundance dance communication) reports communication) Am secondary, for fer continuance clusters for constraint phini dance observed component dwarf, day The lous-abundance line larger tion the the to the Ap very rejected Am phini binary scopic face for for abundance accretion are as dance dance and transferred was bombardment, produce Such source stars. such stars. stars of dance can, mechanism No. Sc 1972a), 8 Delphini Havnes Brancazio the is Si the hypothesis © the the present pure the stars, abundance basis 4, presence spectroscopic later period) stars, nuclear Y first stars to similar deficient however, and reactions stars. and Van reactions stars It American relations 8 pattern. 8 enhancement 1976 binaries of of because predictions observed source observed being systems because be Am (Conti the Delphini Delphini an does, proton abundance the objection argued model in Si of but were and on enhance and which den unlikely in None deficiencies stars could are in odd-even s-process with nuclear spallation of abundance and stars the anomalous and the enhanced in of the them for Adelman this of however, such because in Brancazio or should rule should are Heuvel 1967; the Am in anomalies of require 8 Conti originally in abundance for bombardment. 8 metallic-line anomalies by on Cameron a of then observed nearly be stars cool Delphini 8 stars. which the the binary Del because Astronomical clusters, Sr, observed system are which Del cannot Cr third for main-sequence in a the anomalous-abundance the stars Adelman the out of patterns the at effect processed mechanism process Conti anomalous iron-peak itself, became Ap that reactions has probably (1971) Y, best and (1968a, of the the itself the We qualitatively more Sr-Cr-Eu abundances anomalies large that the basis identical (1973) predict surface exist (for deplete close, and stars. C, the secondary in and seems they not stars (1967) be anomalies in abundances in Am rare manner. only 8 so consider Mn secondary we and in and in 8 stars. should 4 the Ca, Delphini (1973), the the than of magnetic in Am. proposed applied Cameron primary Del been the we b) the Zr, has reject None days stars The as are could earths. relative undetected, a partially enhance spallation material double-line elements, Fe, Strom the also thought unlikely, Sr-Cr-Eu suggested components. abundances Ap run Ba suggested or similar can in 8 a binary Society itself anomalous-abun­ This We Zr, with argued in investigated. found Preston magnetic Delphini group. not Co, magnetic out METALLICISM observed is Sc form components in similar the for the II stars of of be the is to place stars untenable and have in evolved These the fields 1968; stars was predict is to observed produce these a not abundances and of the mass perhaps responsible responsible to the Sc 8 frequency. 8 overabun­ onto and a those which, a a in Ap magnetic reactions magnetic Fe that Delphini that Delphini its that an produce spectro­ rejected because (private • evolved double­ anoma­ a relative already natural no Ni greater to stars. 8 nature as young in 8 which Smith accre­ abun­ trans­ abun­ abun­ white 40.58 Provided Since stars. for since even Del­ Del­ that sur­ and and this age We the the the the the the Ap on Sr as in in a AND fore, evolved, effect tive vide to there the three most hypothesis, between both using plates primary star, from and abundance, and a dance explaining case deficiency could it line, is line Delphini would this mentioned, Am- the normal-abundance whereas thought A hypothesis the the not high both present pulsate. because 8-10 (i) abundances of of of diffusion mechanism 1976). by system out The Where We PULSATION the Zeeman explain the a the if metallic-line metallic anomalous-abundance 8 tenable model, of normal the HR rotational stars. to A was a as components has components the Delphini much of 8 and any Am be the by luminous, the are 8 in A star slowest the mm dominate postulate very magnetic Scuti in Delphini of none is of NASA Unfortunately, them similar the and is should do interpreted measuring 5017, stars metal-line is 13 been left the the phenomenon. KPNO in indication 8 last how for 32 the the the the the - analysis The and, as operating a lines for stars, 8 the which 8 not stronger 1 Delphini anomalous-abundance 8 strong 8 Vir, presence star can of with stable Del K the the rotators. phase are Delphini is spectra stars velocities, 8 success fit 8 shown case observed Del Delphini a the high-metallicity, stars explanation be finally, the second Astrophysics Delphini and the that and not stars Delphini line and star Ap are a into Am lack Grant the would binary exist binary itself the different are radial velocities 8 8 reportedly velocity. of itself to 8 as test for which of Am the correct of possible these in Delphini phenomenon 8 HR stars Delphini can velocity Scuti therefore stars. is stars of choice to of metallic-line the be of the of not having the Such one We Scuti in this stars, the is line is 32 very Ca but properties stars measuring magnetic of contribute is the hypothesis and star magnetic be stars. significantly 8 these 3185 be have stars, spectra above three an transition observed; a tantamount prefer radial Delphini for of are Vir. n K n difficult Ap are pulsator the We hypothesis could doubling. theoretical an a attractive diffusion metallic-lined that pulsators. pulsating due pulsating it transition the SB2 and HR significantly stars. on stars the and binary It no but stars Data spectrum analysis probably stars 8 magnetic, eliminates line, We magnetic therefore producing scheme? the velocity is either properties fields to of 24 Delphini measurable be anomalous-abun­ from fields the 2557, system HR 8 non-anomalous­ than of machine. tempting, spectrum to is to as In stars. of first tested should their as are most Delphini and done (Kurtz different 8-10 System known hypothesis in the As since explain the secondary a classical none 2557 metallic-line star, The to the would is (i) those abundances explanation would representa­ would alternative HR model which previously curves the variables, (ii) reject HR has relatively accretion in probably then the A on diffusion and metallic­ of the different Ca Am Ap-type for stars at of also [Sc/Fe] are or of mm In et to which there­ plates fields. many a the while 3185, show most from need been stars 2557 least II such with pro­ also rule null 667 Am star few this our the the the the for for be. (ii) no al. be - in K is a 8 1 1976ApJS...32..651K cism amplitude abundances abundance a the true pulsation. pretable similarity stars, suggest ence are origin. in HR to model tatively the helium Smith stars scatter (1972), our He the tion the 668 and observed zone lower zone sufficient helium during arise occurring provides required [Sc/Fe] types by should or Roman, Hyades-type We Following The In Classical IX. explain the the more © evolved II pulsating metallicity convective Am objections 7928 zone the for for coexist. into this into quickly and for other ionization have (1971, radiative American SUGGESTIONS for classical of Roman, the radiative note, is depletion BETWEEN and that deficiencies. retaining predicts HR 8 Morgan, and a as by subclasses. these metallicity appendix of to the to in exclusion sufficiently in Scuti and the then normal the convective 8 main-sequence in Am investigators Am HR inhibit We for Vauclair their eliminate having 2557 all the however, 1973a), Delphini the this, overlying anomalous-abundance Fm from the Am is in metallicity relationship stars overshoot of Am zones Morgan, propose pulsators. stars of stars remain these 3185 too the zones METALLICISM observations zone the in suggestion their and Eggen zone. rotational and previous Latour stars, Astronomical stars, we these stars. CONCERNING pulsation, (or diffusion between for range Following high the diffusion we abundances The run depleted in and are so et barrier that stars clarify three HR convection between radiative position in Fm) normal propose We which the essentially He and (Dickens al. that especially and stars to of hydrogen They stars HR from for lifetime the from This et misclassification 3185. section between following HR be II abundances further velocity stars (1974), stars, (1948). of the the we hypothesis AND between al. Eggen thus in the this from ionization 5017 (Smith Am in pulsation may Breger which stars. also A4 in the the are, zone, THE 1706, that Watson the While have meaning the (1975) within classical Am are in PULSATION of accounting et star. the stated coupled stars. to Society through time-independent the line the have This He suggest H RELATIONSHIP criteria we serves 8 metallicism range and however, diffusion This that upper al. diffusion the therefore thus are the 1972a, HR suggested anomalies the Delphini (1972), (j3, 1, for He The [Ca/Fe] types n suggest as and 1971) to observed usually zone the Am This (1971) pulsational our a anomalous Mv) is zone. classified He of upper mitigating ionization a 3265, of Am may to HR II common radiative with diffusion Fl, certainly (hence working that the unusual metalli­ • normal 1973a). ioniza­ cosmic for prefer­ star reduce which I, occurs Baglin model plane, found is quali­ metallic-line inter­ Provided APPENDIX stars occur, and 5017 stars This various that that means and and and and and and can not the the the as in KURTZ we Am are are as would that consistent according subcla~sifications intermediate in factor diffusion increasing Am not presently border pulsational shown sufficient (iii) anomalous-abundance as do equally esized coexist of or of occurs lightening HR marginal vided the the velocity that ok for work, radiative sen, some stars evolved densitometer, as of available. Smith, I Michel Enough to metric 8 by also the stars the Delphini In Pulsation I metallicism these in acknowledge not, Texas it A call degree not yet evidence pulsation would 4594 the stars and pulsational summary, the evolves case K-line of evolve thank unpublished or that with that reduction among they below eliminated Michel regions it grateful Breger, evolved with pulsate, the helium Am to reduction NASA anomalous-abundance no (Am:) in in to Mr. and zone factors classical This of for of discussions density, stars his like the pulsation while pronounced between partial the spectra determine are Dr. type amplitude and longer 15 the presented into into stars. Doctor and Grant HR in pulsation, Frank the the work continued is Breger, we of Vul of MK to process KPNO metallic-line insufficient remains Am instabilities Robert represent who a to derived and Astrophysics (ii) are metallicism programs, a rotation, metallicism given the the the 8210, Am), 8 propose express He the subgiant abundances fulfillment program, Thanks which used occurs or Dr. slow measuring stars classification the was of involved, Scuti Fekel metallicism the may suggested apparent metallic-line giant and if 8 n Am (ii) Leonard for in Kurucz becomes of Philosophy. metallic-line which Myron line-strength but in and temperatures. in Delphini K-line a metal-line submitted ionization enough in evolved Slettebak guidance this testing my but the be star mixing that temperature, for the this pulsators. to for domain. and are region can which which stars. SPECTl have and may of may determine one do use sincere for and paper engine, of He very surface will for generously work. 8 (i) types Smith due and giant grow Kuhi, the Data Delphini small and all pulsate. criteria process stars Am HR of and the coexist found classical which either II has making of across type as we to (1949) coexist be and star. zone generously requirements Abt of to anomalies. the ionization supervised that It and in them. A The is thanks the and pulsation stars related 6561 for spectrophoto­ anomalies. been KPNO metallic-lined have Deane System are the differ Drs. is due and the PDS required and an help. (i) Some two mixing (1975) defined among University called where that the a metal-line some WIDTHS stars, many providing SPECT2. Am pulsating examples marginal in diffusion in Am reclassi· and pleasure strength hypoth­ We age F Vol. to Myron by so to micro­ stars. which Peter­ upper radial I other other these stars stars zone pro­ One Am and Am five star this far, can five has Dr. has are are en­ the the the am by by 32 of 1976ApJS...32..651K in tion emulsion in treating types the complete and computer. itself curve-of-growth that No. same abundance early as only. is marginal magnetic 1975) sequence. fied a ginal latter indicators star. F less There Marginal Table Early Delta Delta their this evidenced © KPNO IVp-F 4, A4 the potentials for FO A We and Am as uses than classification. American 1976 paper. See definition III stars, all or classification IVp. metal is Scuti Delphini the 12 peculiar discussion 20 28 44 6 y Am 14 have with p 8 The metal-line stars of Ilp Photographic a hot Baglin the anomalies. Del. Pup Vir spectrophotometric (marginal lines Mon the is or Tau And CVn Aur. Name classical selection by Star the Care The a the stars stars classifications...... S mild Am ...... line MKA projected shown and five ...... listing are Scuti the ...... as analyses .... uvbyf1 EQUNALENT stars of et stars H plates stars Astronomical should triangles. strengths Am subclasses are oscillator are systematically Sc of the In al. PLATE spectra lines Am Am?) classification criteria effect purposes in of this II are early such stars Population (1973) photometric addition, are MKA 7928 2557 2255 4825 5017 3265 3185 8120 8272 1706 1287 HR this density-to-intensity were ,\4246/Sr slit which 114 the stars, are be MATERIAL stars classification stars in by similar as F are The widths are taken paper stars A strengths to at necessary for traced the system subgiant Cowley reduction y these but are photometric with Am classify their earlier weakening Eql equivalent there a stars WIDTH II hotter and Plate implies not I to that USED not Society complete are D2843a EC6249 EC6245 B8774 B8503 B8507 D2847 B8930 B8929 B8924 B8925 D2011 N613 N597 N621 N610 Ce20609a "4215 system. of stars short-period using or MKA METALLICISM spectra because broad the PRESENTED et plate to used classified Number 20 are than classified not and for 49 physically stars will FOR programs al. than confuse in Am pulsational variability; µm line Cam the Am classification classified DATA F giant due THE width which There which material maximum, (1969). A4 calibrations be analysis similar discussion. • as the K-line the stars. IVp-F and the KPNO ratio. treated Provided ABUNDANCE which stars which to as S as stars the pulsating APPENDIX Dispersion (Amm- TABLE data many classical Delphini, the is are SPECTl widening marginal increased The classical FOR The 10 10 10 to So used as therefore Ilp 8.9 8.0 8.0 8.6 8.0 8.6 8.6 8.0 8.9 8.6 8.6 8.6 8.9 8.6 MKA of IN with AND difference PDS which Conti from are in derived the S classical abundance far type the S as of were stars THIS 1 Del; a THE 12 for Delphini ) classified ANALYSES pronounced by a Am the K A future as microdensitometer and Fp Am the marginal PULSATION (1965) and Am of are is classical ionization, the and line used is are probably that the S earlier stars are B ABUNDANCE 0.4-0.8 STUDY stars lists Observatory SPECT2 Lick KPNO KPNO KPNO Lick between McDonald McDonald McDonald McDonald McDonald McDonald McDonald McDonald McDonald McDonald Mt. McDonald stars, classified Am known, it Delphini (Am:) Anne differential publication. is F S does presented analyses pointed NASA classification is, at PRESENTED FOp Wilson with Delphini of on stars because, according Am Am than namely stars 4100 Cowley mm. Corliss by abundance the not a (Cowley these making the K-line the the on as star. within large stars stars Cowley the out Astrophysics flat with referenced imply and peculiar the Equivalent fine very in IN stars. at the stars and metal-line and have Telescope (private are portion Table THls overlap to is University is ANALYSES 4630 the the subgiant three abundance et probably early (m) anything 2.7 2.7 2.7 2.7 2.1 2.1 2.1 2.1 2.1 2.1 2.1 2.1 2.1 2.1 3.1 3.1 2.5 presently a et the converted anomalies probably type Warner are Morgan al. pronounced STUDY spectroscopic surface MK by al. A. 13 in 1969). b magnitudes Am phenomenologically communication) of in Morgan and widths (1969) - type. All along this criteria and the the physically of spectroscopic Data y stars. (1964), and temperature in analyses the Kurtz Kurtz Breger Kurtz Kurtz Breger Kurtz Kurtz Kurtz Smith Smith Smith Observer Petersen Kuhi Kurtz Kuhl Fekel evolved plates paper to or Texas determined curve Malaroda hot giant in progress, with were intensity metal-line and Abt Am f1 insensitive that System classification Am temperature of Corliss support were CDC the luminosity Abt of anomalies Am call presented measured unrelated the. main the growth, and excita­ agrees (1972) (1973, of and about Ila-0 S using stars. 6600 from mar­ type and 669 Del the the the the to a 1976ApJS...32..651K

TABLE 13 © MEASURED EQUIVALENT WIDTHS FOR THE PR.OGRAM STARS (mA) ). (.8.) x(eV) log gf HR114 HR482S HR8120 HR8272 > \(A) x(eV) log gf HR114 HR4825 HR8120 HR8272 9 ..,~ C I 4301.93 1.16 -1.11 136 89 156 ..... 4771. 72 7 .46 -1. 70 59 32 51 119 4312.86 1.18 -1.06 159 111 149 192 n 4775.85 7 .46 -2.20 - 17 18 25 4367.66 2.69 - 0. 39 121 114 131 ~ 4932.00 7.65 -1. 92 62 37 22 4386.86 2.60 -0.46 77 48 78 4390.98 1. 23 - 2. 03 82 76 = Al I 4394.06 1. 2 2 -1. 4 7 100 47 98 116 3944.01 0.00 -0.62 195 143 131 202 4395.03 1. 08 -a.so 235 179 198 241 >[IJ 3961.52 0.01 -0.32 193 160 115 192 4395.8S 1. 24 -1. S3 67 4S 78 85 ..,...... 4399.76 1. 24 -1. 06 16 s 82 140 164 0 Si II 4411.08 3. 0.9 -0.07 S7 31 8S 74 4128.05 9.79 0.22 144 35 127 4411.94 1. 22 -2 .11 28 19 46 =0 4130.88 9.80 0. 77 57 42 106 108 4417.72 1.16 -1. 18 181 92 1 S4 179 4418.34 1. 24 -1. 6 7 106 61 82 116 .....9 S I 4421. 9S 2.06 -1.14 19 60 77 n 4694.13 6.50 -1. 39 10.6 19 8.8 23 4443.80 1. 08 -0.74 111 118 191 87 ~ 4695.45 6.50 -1. 54 13.4 30 44S0.49 1. 08 -1. 41 92 111 129 1 70 4696. 25 6.50 -1. 76 12.4 10.5 19 4464.46 1.17 -1. 66 10 2 68 118 169 -r.r.i 4468.49 1. 73 -0.6S 218 10 s 17S 240 0 Ca I 4488.32 3.12 0.01 76 56 92 99 n 4226. 72 0.00 -0.55 295 161 316 4493.S3 1. 08 -1. 9 2 24 12.6 ..... 4283.01 1. 88 -0.39 147 69 37 114 4501.27 1.12 232 1S2 201 240 ~ -0.79 ...... 4302.53 1. 89 0.30 172 162 95 4S29.46 1. S7 -1. s 2 78 108 99 '-< 4318.65 1. 89 -0.15 60 4533.97 1. 24 -0.64 207 261 277 4425.43 1. 87 -0.33 103 74 34 84 4S44.0l 1. 24 - 2. 0 8 26 31 47 • 4435.69 1. 88 -0.69 65 53 31 79 4S4S.14 1.13 -1. 61 46 22 64 67 4455.89 1. 88 -0. 72 95 82 33 83 4S63.76 1. 2 2 -0.86 10 7 20 7 234 ..,~ 4578.56 2.51 -0.82 26 48 21 23 4568.31 1. 2 2 -1. 9 3 29 27 4585.87 2.52 -0.31 67 62 32 54 4S71.97 1. s 7 -0.34 260 162 212 249 0 4S89.96 1. 24 -1. 61 129 113 129 128 ~ 0\ ..... -...) Sc II 4779.99 2.04 -1. 12 20 114 102 ~ 0 4246.83 0.31 0.09 232 255 480S.ll 2. 0 s - 0. 7 4 168 1S3 ~ 4294.77 0.60 -1. 27 39 25 38 38 ~ 4305.70 0.59 -1.33 164 V II 4314.08 0.62 -0.10 191 117 231 207 4002.94 1. 43 -1. 2 8 38 11. 9 O' 4320.76 0.60 -0.22 232 138 239 231 400S.71 1. 82 -0. 2 2 '-< 4325.01 0.59 -0.37 147 97 134 4008.17 1. 79 -1. 61 17 8.7 17 22 ...... 4374.45 0.62 -0.45 100 - 171 4023.39 1. 80 -0.3S 61 37 80 62 4400.36 0.60 -0.80 156 82 142 135 4036.78 1. 48 -1. 42 12.7 17 32 22 =-~ 4415.56 0.59 -0.94 4039.S7 1. 82 -1. 60 9.8 22 14 z 4431. 3 7 0.60 -.2. 02 25 21 17 4183.43 2. OS -0.77 16 34 31 SS > Ti II Cr I r.r.i 3913. 46 1.12 -0.24 271 179 192 238 3919.16 1. 03 0.14 94 Sl 45 4012.37 0.57 -1.58 178 100 178 186 42S4.3S 0.00 -0. 27 149 108 190 > 4028.33 1. 89 -0.65 123 70 111 140 4274.80 0.00 -0.39 127 118 9S 149 4056. 2.1 0.61 -2.46 24 30 so 4371.28 1. 00 - 0. 90 33 so >[IJ 4163.63 2.58 0.45 98 181 4Sll.90 3. 0 7 0.37 20 9 .1 2S ..,...... 4294.10 1.08 -0.90 196 131 188 196 4S9l.39 0.96 -1.18 15 10.6 0 4300.05 1. 18 -0.46 269 209 253 4616.13 0.98 -0.9S S7 24 48 "O 4646.17 1.03 - 0. 49 73 64 23 4651. 28 0.98 -0.97 33 22 9.9 17 '-<=- 46S2.16 1. 00 -0.78 34 44 28 [IJ 11. s ..... 4664.20 3.11 0.37 n 4718.4S 3.18 0.82 3S 8. 1 9.9 36 [IJ 0 ~ ...... ~ r.r.i '-< [IJ ...... ~ 9 1976ApJS...32..651K

TABLE 13-Continued

© >.(Al x(eV) log gf HR114 HR4825 HR81ZO HRS27 Z •cP.i X(eV) log gf HR114 HR4825 HR81ZO HRSZ 72 Fe I > Cr II 9 4209.35 3.83 -1. 75 18 23 4047'.32 2.28 -1. 84 7.8 13.0 ..,~ 4252.16 3.86 -1. 85 31 17 57 54 4049.33 2.59 -1. 35 21 22 ..... 4261. 92 3.86 -1. 21 . 43 47 106 109 4059.72 3.54 - 0. 52 7.1 11. 9 39 n 4269.30 3.85 -2.06 36 4062.44 Z.84 0.05 56 44 ~ 4275.58 3.86 -1. 33 34 25 80 94 4063.54 1. 56 0.43 27 245 175 313 4284.21 3.86 -1. 85 38 21 57 59 4065.39 3.43 -0. 70 18 = 4555.02 4.07 -1. 44 58 35 70 85 4067.98 3.21 0.29 74 80 36 96 4558.66 4.07 -0.45 156 90 196 182 4070.76 3.24 0. 01 64 49 >[IJ 4588.ZZ 4.07 -0.65 144 80 157 4071. 74 1. 61 0.40 237 217 217 ...... , 4592.09 4.07 -1. 3 7 74 BO 91 99 4072.52 3.43 -0.43 28 26 0 4616.64 4.07 -1. 51 57 24 48 81 4073.76 3.14 -0.14 64 33 ZS 51 4618.82 4.07 - 0. 9 8 144 96 108 133 4074.79 3.05 -0.14 43 47 69 =0 4634.11 4.07 -1.19 111 105 112 4076.73 3.21 0.24 149 170 150 4848.24 3.85 -1.13 74 59 115 4079.84 Z.86 - 0. 5 2 40 11. 0 .....9 4876.41 3.86 -1. 9 4 76 42 4084.49 3.33 0 .13 49 81 n 4091.56 Z.83 -1. 28 ~ Mn I 4107.49 2.83 0.06 70 34 23 60 4030.77 0.00 -0.48 138 240 4112.97 4.18 - 0. 0 2 37 52 r.ri- 4033.07 0.00 -0.64 182 206 129 175 4114.44 2.83 -0.47 37 21 0 4034.49 0.00 -9.88 125 90 61 119 4120.21 2.99 - 0. 43 26 31 24 n 4035.73 2.11 0.37 108 106 99 121 4123.74 2.61 -1.13 18 ..... 4041.36 2.11 0.93 65 108 113 4126.19 3.33 -0.35 29 64 42 ~ ...... 4048.76 2.13 0.25 69 95 133 4132.06 1. 61 -0.16 166 172 140 186 '-< ....i,_. 4055.54 Z.13 0.47 31 so 25 4132.90 2.84 -0.02 63 80 °' 4082.94 2.17 0.25 17 65 4133.86 3.37 -0.48 42 21 35 • 4083.62 2.13 0.24 25 83 28 99 4134.68 2.83 0.18 10 5 98 65 97 4502.22 2.91 0.18 18 22 19 4136.51 3.37 - 0. 82 8.8 12.6 8.0 ..,~ 4754.04 2. 27 0 .13 34 79 4137.00 3.14 0.12 87 70 68 4783.42 2. 29 0 .11 56 82 4139.93 0.99 - 2. 86 14.7 12.6 19 0 4140.44 3. 4 2 -1.11 14.7 8.5 .....~ Fe I 4141.86 3. 0 2 -1. 04 18 27 ~ 3815.84 1. 48 0.60 279 302 4147.67 1. 48 -1. 4 7 89 100 22 25 ~ 3865.82 1. 01 -0.56 225 129 161 4153.90 3.40 0.33 127 151 117 ~ 3871. 80 2.95 - 0 .15 95 70 41 4156.80 Z.83 0.13 108 172 3872.50 0.99 -0.54 199 4157.78 3.42 0.17 76 69 72 O' 3895.65 0.11 -1. 4 7 147 183 4174.92 0.91 -2.34 26 70 11. 0 20 '-< 3902.94 1. 56 0.12 273 157 244 4175.64 2.84 0.10 61 33 ...... 3920.26 0.12 -1. 49 177 124 117 190 4176.57 3.37 0.04 45 79 37 64 3922.91 0.05 -1. 41 194 112 125 181 4181. 75 2.83 0.46 184 180 181 =-~ 3927.92 0 .11 -1. 29 240 152 160 198 4182.38 3.02 -0.37 18 73 3955.35 3.28 -0.41 50 37 4184.89 2.83 -0.05 66 45 z 3983. 96 2.73 0.06 99 102 69 4187.04 2.45 0.17 119 128 70 139 3998.05 2.69 -0.04 123 96 43 4187.80 2.42 0.13 14 2 14 7 113 153 r.ri> 4005.24 1. 56 -0.07 251 4191.43 2.47 0.06 182 14 7 145 4007.27 2.76 - 0. 45 37 47 24 4202.03 1. 48 -0.25 218 175 158 228 > 4017.15 3.05 -0.17 90 94 79 4203.98 2.84 -0.21 101 89 51 75 4021.87 2.76 0.12 114 69 85 4207.13 2.83 -0.69 44 59 >[IJ 4029.64 3.26 -0.42 39 44 34 48 4210.35 2.48 -0.19 106 71 ..,...... 4040.65 3.30 - 0. 30 41 49 28 4213.65 2.84 -0.55 33 31 17 51 4043.90 2. 73 -0. 56 84 70 29 94 4216.29 0.00 - 2. 9 8 64 48 47 0 94 "O 4044.61 2.83 -0.17 51 68 19 4217.55 3. 43 0.12 76 78 47 4045.81 1. 48 0.68 377 249 333 4219.36 3.57 0.79 125 101 63 120 4222.21 2.45 -0.35 85 65 65 112 '-<=- [IJ 3.42 0.13 100 79 ..... 4225.46 n [IJ 0 ~ ...... ~ r.ri '-< [IJ ...... ~ 9 1976ApJS...32..651K TABLE 13-Continued--- @ 'cJti x(eV) log gf HR114 HR4825 HR8120 HR8272 ). ( J() x(eV) log gf HR114 HR4825 HR8120 HR8272

> Fe I Fe I 4227.43 3.33 0.90 164- 140 206 ("O 4228.72 3.37 -1. 6 5 4494.57 2.20 -0. 35 131 89 106 .....='"I 4235.94 2.42 0.31 192 129 181 4495.97 3.65 - 0. 99 18 12. 7 ~ 4238.81 3. 40 0.47 55 80 114 4517.53 3.07 -1.11 25 9.9 4240.37 3.55 -0. 59 26 18 4525.14 3.61 0.03 77 = 4245.35 2.86 -0.44 54 47 34 89 4531. 63 3.21 -1. 20 11. 9 26 4246.09 3.64 -0.42 26 22 17 4547.85 3.55 -0.10 26 53 = 4247.43 3.37 0.45 90 82 4587.13 3.57 -0.91 24 26 11. 2 21 >[IJ 4248.22 3.07 -0.53 23 29 12.3 39 4602.00 1. 61 - 2. so 13. 4 28 7. 4 '"I 4250.12 2.47 0. 25 10 2 89 160 4602.94 1. 48 -1. 46 0 4250.79 1. 56 -0.28 186 125 114 19 5 4607.67 3.26 -0.66 22 12.0 - 4260.47 2.40 0.63 255 247 257 4611. 28 3.65 - 0 .13 60 69 0 4264.21 3.37 -0.78 20 13. 4 26 4625.05 3.24 -0.63 32 42 18 42 = 4266.96 2.73 -0.87 25 9.6 39 4630.11 2.28 -1. 83 ..... 4267.98 3.11 - 0. 34 42 33 18 32 4632.92 1. 61 -2.31 25 12.0 ~ 4268.74 3.30 -0.63 16 40 11. 9 4635.84 2.84 -1. 46 9.8 = 4271.15 2.45 0. 25 132 98 4637.51 3.28 -0.60 49 23 = 4271. 76 1. 48 0.20 20 7 219 186 242 4638.01 3.60 -0.35 64 42 51 rJJ- 4276.68 3.88 -0.75 12.7 4643.46 3.65 -0.59 32 19 30 0 4282.41 2.18 -0.16 98 124 4647.43 2.69 -0.47 60 24 32 ~ 4285.44 3.24 -0.42 34 42 42 4668.14 3.26 -0.30 57 ..... -.:i ("O °' 4291. 46 1. 56 -1.99 21 22 78 4673.17 3.65 -0.53 38 16 N 4298.04 3.05 -0.56 24 43 32 4678.86 3.60 0.05 58 65 ~ 4325.76 1. 61 0. 36 147 214 178 19 5 4690.17 3.69 - 0. 79 10.9 18 - 4327.92 3.30 - 0. 90 4691. 42 2.99 -0.54 48 42 21 • 4352.74 2.21 -0.56 77 42 4705.46 3.55 -1. 2 7 12.6 4375.93 0. 00 - 2. 59 91 49 92 4707.28 3.24 -0.23 58 71 "'ti 4376.78 3.02 -1. 27 11. 9 8.7 9.3 11. 7 4710.28 3. 0 2 -0.74 35 35 32 '"I 4382.78 3.57 -0.16 14.7 4733.60 1. 48 -2.38 37 0 4383.56 1. 48 0.51 299 4735.85 4.08 -0.37 21 .....~ 4387.87 3.07 -0.62 22 50 4736.78 3.21 -0. 0 2 95 81 ~ 4388.41 3.60 0.02 68 74 4745.81 3. 6 5 -0. 55 14.7 ("O 4392.58 3.88 -0.96 9.2 4772.82 3. 0 2 -1. 0 5 25 23 ~ 4404.75 1. 56 0.25 199 156 223 70 Fe II O" 4408.41 2.20 -0.95 58 91 38 4415.12 1. 61 -Q.13 4122.63 2. 58 -2.73 89 73 112 104 ~ 4422.57 2.84 -0.22 56 97 4128.73 2.58 -2.76 57 48 72 68 4427.31 0.05 -2.51 120 111 4178.85 2.58 -2.00 145 137 178 210 2 2 02 56 83 90 4233.16 2. 58 -1. 43 201 ("O=- 4430.61 2. -1. - 4432.57 3.57 -0.82 21 8.8 4273.31 2.70 -2.27 70 106 125 4433.22 3.65 -0.14 55 36 4296.56 2.70 -2.36 132 82 133 139 z 4438.35 3. 69 -0.99 17 8.4 4303.16 2.70 - 2. 00 177 109 149 176 . > 4442.34 2.20 -0.50 138 65 4351. 76 2.70 -1. 76 218 rJJ 4443.19 2.86 -0. 22 111 87 4385.38 2.78 - 2. 0 2 155 106 190 161 4447. 72 2. 2 2 -0.58 90 66 67 88 4416.81 2. 7 8 -2.09 115 135 156 > 4466.58 2.83 0.18 132 78 103 4472.92 2.84 -2.80 66 35 75 87 4469.38 3.65 0.19 115 78 88 4489.18 2.83 -2.23 132 93 156 124 [IJ> 4476.02 2.84 0.14 127 10 2 77 137 4491. 40 2.85 -2. 09 87 156 140 '"I 4479.61 3.69 -0.70 34 17 4508.28 2.85 -1. 76 82 178 191 0 4480.14 3. 0 5 -1. 01 14.8 4515.33 2.84 -1. 91 178 96 168 191 "O- 4484.23 3.60 0.08 53 59 37 46 4520.24 2.81 -1. 8 7 166 149 174 4485.67 3.68 -0.40 30 28 43 4522.63 2.84 -1. 51 211 109 20 7 2 33 ~=- 4490.08 3.02 -0.74 28 32 .....[IJ ~ [IJ =~ = -rJJ ~ [IJ -("O = 1976ApJS...32..651K TABLE 13-Continued

© A(A) xCeVJ log gf HR114 HR4825 HR8120 HR8272 >-CAJ xCeV) log gf HR114 HR4825 HR8120 HR8272 > Fe II Zr II 3 4 541. 52 2.85 -2.29 51 132 4149.22 0. 80 -0.13 118 127 98 133 ~ 4555.89 2.83 -1. 79 246 215 238 4150.97 a.so -1. 02 10.l 18 38 .,.... 4S76.33 2.84 -2.22 50 127 12S 41S6.24 0.71 - 0. 8S 79 so 49 79 !°') 4582.83 2.84 -2.44 97 72 102 4208.99 0.71 -0.S4 41 Sl 64 ~ 4S83.82 2. 81 -1. 2 s 242 168 245 244 4211. 88 O.S2 -1. 21 12.7 10.5 43 27 4620.Sl 2.83 -2.63 78 S2 93 S6 4317.32 0.71 -1. 48 24 6.9 8.9 4629.33 2. 81 -1. 7 8 166 70 158 187 = 4635.35 S.9S -1. 43 38 Ba II [IJ> 45S4.03 0.17 135 .... 46S6.97 2.89 -2.53 135 66 149 0.00 220 204 ., 4666.75 2.83 -2.64 83 70 102 • 4934.10 0.00 -0.14 173 183 124 0 4670.17 2.58 -2.87 41 110 89 4731.44 2.89 - 2. 29 142 79 92 La II 0 4923.92 2.88 -0.93 2 53 3988.Sl 0.40 -0.26 11. 5 16 11 = 4086.72 0.00 -0.60 16 26 24 ....3 Co I 4123.23 0.32 -0. 40 22 25 24 20 !°') 4020.90 0. 43 -1. S8 7.1 11.1 7.1 4263.59 1. 9S 0.03 (4.8) 10. 2 17 ~ 4058.60 2.00 -0.67 26 S4 13. 8 Sl 4322.Sl 0.17 -1. 62 4121. 32 0.92 -0.03 39 32 24 33 4333.76 0.17 -0.60 52 14.1 4662.Sl 0.00 'JJ.- - 2. 04 ( 4. 5) 14.l 0 Ni I 4748.73 0.92 -1. 20 5.4 9.7 13.l !°') 38S8.30 0.42 -0.62 166 132 87 .... 4401.55 3.18 0.83 98 39 87 Ce II ~ -...) .... °'\.>.) 4606.99 3.47 0.77 55 30 39 3882.45 0.32 -0.06 56 133 '-< 4606.23 3.58 0.30 16 23 9.9 4120.83 0.32 -0.74 (4.2) 4648.65 3.47 0.78 66 41 13 .1 42 4137.60 0.04 0.09 27 29 14.8 8. 2 • 4686.22 3.58 -0.39 21 12. 2 4142.40 0.22 -0.14 31 45 13. 8 4714.42 3.37 0.84 88 4S 47 76 4193.09 0.74 -0.10 (4.0) 4.5 ~ 4715.78 3.S3 0.76 34 13. 9 20 4202.94 O.S6 -0.34 7. 4 s. 7 10.5 ., 4418.7B 0.38 0.03 25 13.6 17 0 Ni II 4486.91 0.29 -0.62 10.9 6.4 s.o S.8 ....~ 4015.SO 4.03 -1. 2 5 63 57 34 54 Q. 4067.05 4.03 -0.59 132 157 125 176 Nd II ~ 4244.80 4.03 -2.03 34 29 4061. 09 0.47 0. 03 17.8 (S.O) 18 Q. 4362.10 4.03 -1. 43 14.7 37 4462.98 0.56 -0.84 22 25 llO O" Zn I Sm II '-< 4722.22 4.01 0.69 29 35 5. 4 31 4424.34 0.48 -0.42 14.0 9.2 16 .... 4810.S3 4.06 0.86 14.9 27 19 so 4467.34 0.66 -0. 39 7.4 6.7 ~=- Sr II Eu II 4077. 71 0.00 -0.78 283 276 216 309 4129.73 0.00 -0.31 20 16.8 12.0 13 z 4215.S2 0.00 -0.99 248 241 214 268 420S.05 0.00 -0.08 61 46

'JJ.> y II Gd II 3950. 35 0.10 -0. 71 111 80 42Sl. 73 0.38 -0.39 (4. 7) 10. 2 12. 5 > 3982.59 0.13 -0.79 6S 45 82 87 4177.54 0.41 -0.24 186 196 196 210 [IJ> 4309.62 0.18 -0.98 106 163 96 ....., 43S8.73 0.10 -1. 61 24 54 37 23 4374.94 0.41 -0.14 171 0 4398.02 0.13 -1. 25 49 53 "O '-<=- [IJ.... !°') [IJ 0 ....~ ~ 'JJ. '-< ....[IJ ~ 3 1976ApJS...32..651K TABLE 13-Continued---·- •cft.1 HR1287 HR1706 HR2255 HR2557 HR3185 HR3265 HR5017 HR7928 © >.(A) HR1287 HR1706 llR2255 llR2557 HR3185 HR3265 HR5017 HR7928 > CI Ti II 9 4771. 72 31 106 64 122 143 76 4301. 93 192 190 240 2SS 276 236 2S3 121 ..,~ 4775.85 23 49 29 37 34 44 41 4312. 86 210 147 210 197 2S6 159 234 120 ..... 4932.00 79 -- 24 - - 30 4367.66 184 llS 184 194 260 162 202 98 n 4386.86 113 70 129 111 168 111 171 60 ~ Al I 4390. 98 146 74 153 131 216 146 198 70 3944.01 204 184 221 212 "266 247 247 191 4394.06 144 96 136 123 17S 99 178 S7 = 3961.52 178 131 220 148 224 162 199 171 439S.03 266 219 260 274 326 240 302 186 4395. 85 124 54 130 100 143 196 17S 43 >[IJ 4399. 76 217 2S2 64 232 117 ..... Si II 193 140 204 .., 4128.05 135 120 162 196 279 204 89 4411. 08 107 57 94 73 143 149 41 0 4130.88 75 95 164 98 259 206 230 107 4411. 94 82 29 S6 48 101 26 llO 13.4 4417. 72 192 lSO 180 167 2SO 175 216 ll8 =0 SI 4418.34 131 49 99 1S3 99 1S8 46 4694.13 21 49 4S 65 18 37 43 4421. 95 100 53 84 138 53 142 20 .....9 4695.45 16.6 26 29 23 10.1 37 14. 9 4443. 80 227 187 216 292 248 173 4696. 25 lS.3 17 3S 11.0 S.2 18 20 44SO. 49 183 140 212 169 222 249 113 n 4464. 46 266 166 212 80 ~ 168 106 161 160 Ca I 4468. 49 227 179 240 299 222 24S 163 so -r.r.i 4226. 72 363 289 319 338 396 369 364 268 4488. 32 139 63 ll6 lOS 180 88 166 0 4283. 01 148 97 128 -167 126 158 93 4493. S3 62 22 46 61 81 22 84 93 n 4302.S3 195 166 162 210 240 19S 123 4501. 27 228 176 260 190 296 234 269 164 ..... 4318.65 lSl ll6 120 4529 .46 16S SS 149 ll9 196 103 19S S3 ~ ..... 0\ 442S.43 146 78 120 99 162 8S 1S8 79 4S33. 97 290 2S2 310 297 3S2 298 329 '--< -:i 443S.69 139 68 151 91 210 173 9S 4S44. 01 65 26 72 107 82 31 96 23 ..i;:.. 445S. 89 132 Sl 120 168 122 146 79 4545 .14 84 34 93 96 53 127 37 • 4578. 56 57 25 S2 65 39 81 40 4S63. 76 239 156 233 217 260 20S 261 lSS 458S. 87 124 37 98 87 ll8 6S 146 43 4S68. 31 18 37 47 10. l 83 ..,~ 4S71. 97 260 196 298 260 325 302 319 198 Sc II 4S89. 96 142 9S 161 192 92 187 77 0 4246. 83 197 222 249 280 249 274 lSS 4779. 99 7S 88 120 154 74 .....~ 4294. 77 84 45 74 62 95 44 128 lS 4805.11 102 162 220 180 ll2 Q. 430S. 70 220 ~ 4314.08 212 196 280 2S4 32S 278 303 163 VII Q. 4320. 76 219 281 290 333 261 316 141 4002. 94 72 141 S4 134 15S 29 432S. 01 180 ll2 192 197 233 232 94 4005. 71 ll6 162 197 80 O' 4374.45 178 201 302 205 219 91 4008 .17 21 42 40 98 12. 3 '--< 4400. 36 155 106 196 1S3 177 179 237 81 4023. 39 110 81 131 96 lSO ll8 16S SS ..... 441S. S6 153 154 169 188 70 4036. 78 38 36 57 33 66 36 97 11. 5 4431. 37 26 14.8 41 62 50 10 .1 79 8.6 4039. 57 18 27 26 55 52 13.8 47 8.4 =-~ 4183. 43 71 39 77 104 111 128 18 Ti II z 3913.46 266 238 278 319 362 325 314 217 Cr I 4012. 37 221 188 278 212 290 298 307 170 3919.16 158 64 138 186 130 170 74 r.r.i> 4028.33 146 149 172 185 179 156 196 89 4254.35 207 164 216 277 196 248 140 4056. 21 62 52 66 30 142 12.8 4274.80 204 130 192 276 203 221 137 > 4163.63 188 145 199 2S7 176 232 111 4371. 28 115 49 92 99 121 104 44 4294.10 231 198 234 203 299 196 244 175 4511. 90 31 13.2 24 47 15 36 17 >[IJ 4300 .OS 264 22S 285 2SO 372 298 311 181 4S91. 39 48 14.2 46 so 26 66 7. 7 ..,..... 4616.13 64 S4 52 97 92 92 19 4646.17 36 101 92 170 129 44 0 4651. 28 14. 7 40 52 70 18 59 24 "O 4652.16 26 47 41 94 34 77 32 =- 4664. 20 14. Ii 12.8 '--< 4718.45 18 28 46 69 64 20 .....[IJ n [IJ 0 ~ ..... ~ r.r.i '--< [IJ ..... ~ 9 1976ApJS...32..651K

TABLE 13-Continued

© A(A) HR1287 HR1706 HR2255 HR2557 HR3185 HR3265 HR5017 HR7928 A(A) HR1287 HR1706 HR2255 HR2557 HR3185 HR3265 HR5017 HR7928

> Cr II Fe I 4209. 35 14.9 23 44 4047. 32 10.l 22 31 42 7 .6 29 15 9 4252 .16 43 165 85 140 36 ..,~ 63 69 4049. 33 21 49 82 47 73 23 ..... 4261.92 126 95 149 124 211 142 193 73 4059. 72 48 26 S8 27 110 47 86 29 4269.30 68 33 108 92 134 no 157 35 4062.44 113 92 167 86 18S 162 184 89 n 4275. 58 123 60 116 103 176 99 161 S6 ~ 4063. 54 27S 2S3 339 368 405 368 286 267 4284. 21 99 51 81 98 1S3 99 143 34 406S.39 55 24 80 66 34 79 21 = 4555. 02 109 56 88 125 146 85 141 74 4067. 98 136 97 124 186 123 173 85 4558.66 194 143 210 240 204 239 119 4070. 76 no 73 n8 150 114 151 62 >[IJ 4588. 22 156 124 176 149 205 137 199 67 4071. 74 272 210 263 244 262 267 276 192 ...... , 4592.09 114 78 112 141 141 1S7 19 4072. 52 67 28 S9 72 8S 111 19 4616.64 101 35 99 101 136 78 133 51 0 4073. 76 101 59 125 129 129 65 4618. 82 156 78 144 176 220 126 192 93 4074. 79 115 48 113 71 148 110 147 61 4634.11 134 77 122 144 185 92 161 83 =0 4076. 73 152 188 214 240 257 139 4848. 24 110 1S9 138 77 4079. 84 84 28 67 90 105 SS 4876. 41 167 165 173 .....9 4084.49 120 49 96 126 66 123 SS 4091. S6 29 19 lS 29 6.1 29 n Mn I ~ 4107 .49 97 38 114 80 141 85 108 70 4030. 77 299 218 4112.97 3S 74 77 llS 43 107 31 4033.07 230 177 219 262 290 289 270 177 r.ri- 4114.44 72 29 72 37 76 49 96 36 4034. 49 176 133 140 231 0 173 187 204 124 4120. 21 80 23 67 80 103 62 103 35 n 403S. 73 171 14S 178 137 237 170 228 94 4123.74 96 32 106 89 121 72 147 S4 ..... 4041. 36 158 113 155 141 232 162 203 104 4126.19 102 34 95 141 70 119 38 ~ 4048. 76 134 118 179 137 227 205 227 115 4132.06 256 160 263 27S 314 319 294 188 .... 0\ 4055.54 98 75 96 91 168 83 130 51 '-< -...I 4132. 90 117 77 101 188 148 149 80 VI 4082. 94 87 13.1 73 60 96 53 97 4133.86 84 59 120 163 107 142 54 • 4083.62 147 48 120 109 177 114 176 51 4134.68 166 126 162 279 162 209 113 4502. 22 36 8.9 33 39 63 16 38 89 4136. Sl 34 37 S2 56 19 ..,~ 4754. 04 27 87 171 75 102 51 4137. 00 112 59 109 79 197 1S6 73 4783.42 43 101 73 107 107 60 4139. 93 10. 5 23 22 70 20 57 0 4140.44 33 12.0 3S 23 65 22 59 14.6 ~ Fe I 4141. 86 43 13. 5 61 86 19 ..... 381S. 84 313 303 4147 .67 128 62 114 129 169 122 lSl 71 ~ 3865.82 254 240 ~ 4153. 90 164 110 133 249 217 99 ~ 3871.80 122 212 188 214 208 4156.80 169 97 143 224 220 124 3872. 50 41S7. 78 130 80 94 93 186 117 154 82 O' 3895. 65 202 268 293 245 232 175 4174.92 95 147 9S 78 162 62 112 44 '-< 3902 .94 232 221 340 296 331 2S6 208 4175.64 139 80 116 75 20S 141 159 91 .... 3920. 26 190 165 225 188 228 231 217 162 4176.57 130 61 108 107 192 116 151 74 3922. 91 224 167 263 228 283 278 265 189 4181. 7 s 1S8 198 193 328 249 254 16S =-~ 3927. 92 220 177 275 225 264 312 245 216 4182. 38 85 43 86 33 162 90 127 49 3955. 35 108 37 105 52 132 73 153 S4 4184.89 111 73 105 71 187 114 143 93 z 3983. 96 148 86 167 228 179 222 103 4187 .04 178 149 176 281 267 219 138 > 3998.0S 158 88 163 138 264 187 208 99 4187. 80 230 141 221 181 314 249 251 147 r.ri 4005. 24 116 261 275 210 4191. 43 206 140 229 258 262 141 4007. 27 83 45 123 124 125 34 4202.03 240 217 279 250 379 285 310 192 > 4017 .15 122 87 128 182 159 146 171 4203.98 1S7 74 127 91 224 137 201 89 4021. 87 148 95 155 143 239 - 196 215 121 4207 .13 78 39 72 66 174 114 149 41 >[IJ 4029.64 101 93 115 137 142 140 77 4210.35 163 100 168 225 170 185 112 ...... , 4040.65 98 Sl 126 112 205 174 4213.65 64 44 76 51 146 82 110 54 4043. 90 127 62 123 196 117 170 74 4216.29 110 29 118 48 205 157 80 0 4044.61 108 59 96 151 99 147 58 192 130 148 80 "O 4217. 55 110 59 139 41 404S.81 431 314 420 436 537 428 462 360 4219. 36 164 98 143 107 234 161 196 99 =- 4222. 21 143 104 161 153 249 201 179 104 '-< 4225.46 113 129 1S6 160 214 225 103 .....[IJ n [IJ 0 ....~ ~ r.ri '-< [IJ .... ~ 9 1976ApJS...32..651K

TABLE 13-Continued

HR2557 HR3185 HR3265 HR5017 HR7928 © •CAJ HR1287 HR1706 HR2255 HR2557 HR3185 HR3265 HR5017 HR7928 •c.Ai HR1287 HR1706 HR2255

> Fe I Fe I 9 4227. 43 209 165 215 217 273 279 279 155 4494. 57 174 93 177 165 243 175 183 118 ..,~ 4228. 72 21 19 25 34 4495.97 10.0 42 40 14.2 48 10.9 ..... 4235.94 228 169 244 186 325 305 256 187 4517.53 43 16 39 56 72 22 57 14.9 n 4238. 81 159 100 156 109 257 201 101 4525.14 128 65 138 113 242 150 175 99 ~ 4240.37 69 29 49 41 31 110 25 4531.63 29 20 34 4245. 35 127 49 103 200 114 162 61 4547.85 69 23 61 97 107 53 97 42 = 4246.09 67 24 72 131 92 114 36 4587 .13 45 11.4 25 27 42 52 10.9 13.8 46 17 >[IJ 4247.43 171 96 151 101 184 154 189 111 4602.00 14.1 33 ..... 4248. 22 74 31 71 79 106 43 4602.94 122 43 89 51 153 75 130 63 .., 4250 .12 179 126 183 268 209 124 4607 .67 16.2 71 50 84 75 92 45 0 4250. 79 202 167 212 269 239 160 4611.28 118 34 85 73 160 72 143 69 4260.47 256 214 266 367 279 268 196 4625.05 87 22 77 66 116 59 102 43 =0 4264.21 44 21 34 32 92 74 23 4630.11 18 38 15 54 18 56 35 4266. 96 so 30 51 59 115 42 73 23 4632.92 64 21 53 26 88 32 .....9 4267. 98 94 33 68 55 130 56 96 37 4635.84 35 24 30 55 26 27 38 n 4268.74 71 26 58 99 36 4637. 51 71 37 46 71 115 94 ~ 4271.15 199 150 202 250 225 143 4638.01 68 29 72 60 118 94 62 4271. 76 268 202 285 354 277 208 4643.46 44 40 57 34 74 36 r.ri- 4276.68 31 16 34 46 13.6 57 20 4647 .4'.l 91 85 180 78 136 64 0 4282. 41 165 117 198 145 253 214 222 130 4668.14 84 105 167 106 63 .....n 4285. 44 87 28 80 143 88 114 45 4673.17 29 72 83 94 36 85 ~ 0\ 4291.46 53 17 43 67 103 21 70 4678.86 40 78 116 85 113 80 ..... -.l 4298.04 81 27 65 81 86 32 4690.17 21 20 43 46 47 19 "'< 0\ 4325. 76 292 206 315 280 359 308 228 4691. 42 76 75 167 137 54 4327 .92 25 30 30 16 59 10.9 4705.46 24 35 21 15 • 4352. 74 137 47 112 72 164 67 147 73 4707.28 54 83 80 184 115 65 4375. 93 123 54 128 116 185 82 146 86 4710.28 31 60 51 100 84 37 ..,~ '4376. 78 22 23 23 31 53 11.6 38 5.6 4733.60 42 71 68 0 4382. 78 39 44 48 82 53 80 32 4735.85 11.3 35 80 53 28 140 80 -< 4383. 56 282 220 292 288 357 283 247 4736. 78 108 77 ..... 4387. 87 64 43 59 55 122 107 110 28 4745.81 12.1 60 50 58 62 ~ 4388.41 103 40 92 82 159 68 146 52 4772.82 30 so 61 45 ~ 4392. 58 16 14. 7 41 47 57 5.6 ~ 4404. 75 255 189 262 257 335 280 218 Pe II O' 4408. 41 59 105 204 141 169 68 4122.63 163 99 168 160 197 141 208 95 4415.12 225 230 335 261 201 4128. 73 135 57 89 111 123 89 149 "'< 273 263 256 152 ..... 4422. 57 131 58 145 201 146 167 96 4178.85 185 160 216 225 4427. 31 160 89 150 217 156 196 107 4233.16 266 260 259 358 372 304 225 209 164 183 82 =-~ 4430.61 129 60 89 105 192 130 164 68 4273.31 123 96 169 140 4432. 57 19 17 16.8 47 52 13.0 4296. 56 184 128 220 189 266 222 243 140 z 4433.22 78 34 75 83 121 82 111 46 4303.16 186 147 189 202 268 236 217 145 4438.35 17 11.1 25 33 52 10.l 54 9.5 4351. 76 298 309 > 4442.34 147 75 81 127 193 163 93 4385.38 188 134 214 294 170 240 141 r.ri 4443.19 112 89 135 199 164 115 4416.81 179 130 182 231 168 204 127 4447.72 137 60 111 97 184 127 152 .98 4472.92 157 47 133 216 147 172 60 > 4466. 58 148 104 155 117 207 162 186 119 4489.18 172 102 170 145 251 146 218 106 4469.38 84 141 232 145 202 88 4491. 40 170 127 166 142 233 149 190 119 >[IJ 160 ..... 4476.02 177 85 145 . 121 236 154 186 123 4508. 28 190 117 215 167 278 190 233 .., 4479.61 37 18 49 48 83 27 4515.33 192 115 197 151 264 179 220 150 0 4480.14 13.6 45 80 17 4520.24 182 128 182 176 248 170 215 143 "O 4484.23 33 87 131 114 115 63 4522.63 228 166 254 210 305 303 301 196 4485.67 64 14.4 71 45 48 76 28 "'<=- 4490.08 69 28 54 62 82 33 .....[IJ n [IJ 0 ~ ..... ~ r.ri "'< [IJ ..... ~ 9 1976ApJS...32..651K

TABLE 13-Continued - i-(AJ HR1287 HR1706 HR2255 HR2557 HR3185 HR3265 HR5017 HR7928 © A(A) HR1287 HR1706 HR2255 HR2557 HR3185 HR3265 HRS017 HR7928

> Fe II Zr II 149 88 167 148 190 148 177 111 ('ti 4541. 52 4149. 22 184 1S7 237 176 27S 274 238 166 = 4555.89 154 2SO 215 299 281 281 180 4150.97 86 33 100 52 76 103 84 42 "'"i ..... 4576.33 134 85 147 181 137 174 97 4156.24 142 103 201 232 218 112 ~ 4582.83 125 76 124 80 171 122 157 81 4208. 99 62 56 141 196 133 90 4583.82 240 187 272 316 267 277 204 4211. 88 67 47 135 47 120 114 128 6S = 4620. 51 108 S6 105 92 163 72 144 88 4317.32 23 10.5 68 40 47 24 41 19 = 4629. 33 182 116 216 202 255 201 213 187 .,.,> 4635.35 74 26 Ba II ..... 4656.97 84 131 243 92 192 76 4554.03 215 168 273 169 310 302 264 230 "'"i 4666.75 70 132 162 243 141 186 89 4934.10 196 256 232 0 4670.17 70 166 141 202 122 199 4731.44 64 143 225 174 99 La II =0 4923.92 330 243 3988.51 36 22 138 69 91 101 141 56 4086. 72 40 26 94 82 107 106 58 ..... Co I 4123. 23 62 26 108 115 92 131 54 =~ 4020.90 21 10. 7 23 19 50 34 53 18 4263. 59 20 35 28 37 39 48 11.9 4058.60 128 52 98 89 146 53 150 40 4322. 51 7.4 10.2 35 34 23 18 31 6.8 = 4121. 32 100 37 105 60 127 96 106 45 4333. 76 38 25 91 38 95 56 109 so rJ".J- 4662. Sl 6.3 40 43 22 so 8. s 0 Ni I 4748. 73 33 24 13.8 33 ~..... 0\ 3858. 30 173 272 303 218 ('ti -J 4401. 55 163 79 165 2SS 187 199 117 Ce II ..... -J 4606.99 60 28 61 54 120 53 lOS 46 3882.45 194 162 '-< 4606. 23 49 69 40 36 S6 16 4120.83 6. 2 9.4 31 38 24 44 37 6.0 4648.65 37 100 92 176 85 124 70 4137. 65 30 38 96 S2 135 99 llS 49 • 4686.22 14.6 46 77 26 S9 4142.40 68 S7 119 97 177 146 169 SS 4714.42 S9 117 S4 208 lSO 167 103 4193.09 9. 7 11. 5 53 21 30 33 44 10.2 ""C 3S "'"i 471S. 78 2S S6 28 S9 83 4202.94 11. 7 15.6 72 42 92 78 93 27 0 4418. 76 13.3 48 37 59 S9 22 ~ Ni II 4486.91 23 8. 7 28 9.4 32 34 so 13.0 ..... 401S.SO 94 Sl 122 80 143 145 182 70 i:i. 4067.05 174 1S9 238 28S 232 159 Nd II ('ti 4244.80 8.9 8.0 31 35 S5 82 Sl 10.3 4061.09 38 26 64 99 72 89 43 i:i. 4362 .10 32 18. 2 63 62 74 41 84 26 4462. 98 7. 7 lS.3 23 4S 45 67 32 21 O" '-< Zn I fon II ..... 4722.22 12.l 83 13 108 68 8S S7 4424. 34 38 21 45 28 75 34 68 16 4810.53 47 104 3S 1S3 68 85 78 4467.34 12.6 18 44 30 42 56 34 20 =-('ti Sr II Eu II z 4077. 71 36S 320 437 386 531 618 401 382 4129. 73 40 21 136 23 180 109 148 79 > 421S. S2 328 268 362 406 394 445 333 296 4205.05 96 73 210 196 275 276 233 142 rJ".J y II Gd II > 39SO. 35 94 107 179 107 154 152 125 4251. 73 20 17 SS 43 67 36 S6 20 3982. S9 86 7S 185 168 162 1S3 111 .,.,> 4177.54 228 224 314 303 364 394 310 249 ..... 4309.62 143 120 221 191 327 287 213 73 "'"i 43S8. 73 110 37 141 50 169 222 146 158 0 4374.94 200 245 288 247 201 "O 4398.02 156 188 139 105 =- '-<.,., ...... ,.,~ 0 .....=

=rJ".J '-<.,., ..... ('ti = 1976ApJS...32..651K plate equivalent Fm. Fm. © and American 10.-Comparison 11.-Comparison a widths K.PNO for 2.1 HR Astronomical m o<{ of telescope of 114 - ·5 .r: w ~~ - -o ~u E 0 ~~ C" c: the ! our 0 of c: equivalent Smith equivalent 100 100 8.9 10 10 5"-1.....u 5 A (1972b) I . mm- Society . . widths / .. widths ..... • 10 1 from ~~.....1...~"--..._ 10 plate. measured . . . . for ··:: • a •/.. • Equivalent K.PNO / Provided .· • .. /: HR • ... ·/:: Equivalent ...... /." • . by . / • 114 /. I : KPNO the • .. 2.1 . I . / I from KPNO Width . . '* . ·~ ·""': author . m ., .. .. ·'./·· ...... '° • •f. et. ···~.~ by .. .. telescope .. •• :=· .. . _._ . Width{mA) a %" -~ (mAl : r·~ •.z:. ·.~..... 9\r:'i• ...... • for • the McDonald ...... • 0 . -~·-,· • 100 . .. ·!.""'' • 100 .5 ~~-'-~....._ . • . ~..v· :~~·. .. • . Del ·~ NASA - 8.9 z. . . • . :S • ;/.".,• 0 ... I A from ·.:~· : .... :~~ .. mm- ,.. 2.7 • . "}~·· =·· :-..,>:· ... / .. a Astrophysics .. . .. m /. . McDonald 1 telescope plate...... 500 500 2. 8.0 7 m A Data telescope mm- 1 System plate 8.0 A with mm the - 1 1976ApJS...32..651K --. --. Allen, Abt, Adelman, Abt, mind be equivalent as tion ternally equivalent-width equivalent of There Figure the ured plates pared of agree widths for our Bozman to the stars abundances. line Athlone). We Fm. We first 20%. taken other Smith © the K.PNO most H. H. data list of with by is C. of in with is American have have 12.-Comparison 1975, 1965, A., A. 12 for approximation. given same this /l and in W. a Bessell any S. (1962), investigators, Although especially from each (1971). Del recent 1961, are and systematic widths widths others J. order 8 1963, compared the compared used 2.1 Ap. Ap. shift with interpretation Because 1973, Del are stars by also other, Moyd, Ap. different m J., J. (1969) Lambert but Astrophysical in Ishikawa a Both scales to is is from the is Suppl., of telescope 195, Ap. J. compared and Astronomical good in heterogeneous such whereas offered. ± facilitate ± K. rather Suppl., 3 shift puqlished the J., 0.09 all 0.09 of 405. Del regardless of at find A I. a derived internal telescopes 11, 183, a our abundances plate case 1973, and 6.8 these critical equivalent-width (1973, of dex. shift dex. our from 6, 429. were of on at equivalent Bessell Quantities 95. with our A 37. intercomparison 100 Warner of equivalent Ap. the 8.9 agreement, In the taken figures In mm from equivalent 10 in a chosen 1975). equivalent stars discussion of Figures another group J., some A data McDonald the and average Society - and the mm 182, 1 plates METALLICISM with were widths (2d (1968a, for at equivalent-width are with presented cases widths equipment Reimers's to of - 809. as ed.; 10 Mount I which 1 plate widths typical the 0, data • derived no be shown plates widths of for of the Figure London: 11, • our b, 2.1 are of systematic the comparable McDonald more /l Provided of used data only REFERENCES and Del c, Stromlo the Equivalent smaller equivalent in m of herein of from same 3 data compared d), differentially, used Fig. 11 telescope with other Del recent most 12 in 3 of one AND and compares Delphini we different this 10. scale than are other as in those to that shift. plate and 2. Baglin, Batten, Baglin, investigators. Bessell, Bidelman, Width(mAl of dispersion have oscillator Warner by Figure those obtain 7 m in analysis widths J. 23, theirs. PULSATION with is of 8.6 the such investigators. Reimers good M., the The was 221. plotted Bessell exceptional telescope star telescopes A. A., A. errors M. our A 0 equivalent-width 100 used theirs Note, 10, Sareyan, the x • differ a NASA (1967). W. 1972, mean mm- measured. H. S. Breger, Mt. Mt. with agreement strengths abundances shift equivalent are with (1969) 1961, 1969, P. plates. Strom Wilson (1969) by some however, in Figure of Astr. from 1 1965, usually other scatter at plate a be may The Smith oscillator J. good about lo M., and Pub. Astrophysics Ap. in and Figµre 8 representative P., Ap., The at those useful Vistas A this Chevalier, J. 12 oscillator published equivalent-width published but that observatories, Reimers D.A.O., are and widths agreement 10 of mm in and Suppl., 20% (1971, 19, represents rms 500 x present. comparisons analysis, 10 A the our compared our in in good Valtier, 45. strength in - Smith's mm Astronomy, 1 compares the or scatter equivalent 11, (1969). the author's 18, for equivalent and 1973a) C., strengths 0.08 agreement - literature 395. 167. examples analysis 1 Data there, Special Hauck, HR J. it a a at values Bessell Am dex. C. with but worst in plate must for Mount 114 8, made our data widths 1973, the also. System find and B., used 53. widths No most those care of by as and taken comparing with be case. with cancel equivalent compared Le shown Astr. A explana­ both from Fm that Wilson. kept are Reimers should Contel, and of meas­ much those those com­ In with data 679 star Ap., not out two the the in­ it, in in F 1976ApJS...32..651K --. --. --. --. --. --. --. --. Brancazio, Breger, 680 Conti, Corliss, Corliss, Cowley, Conti, Conti, Eggen, Danziger, Danziger, Dickens, Crawford, Crawford, Cowley, Edmonds, Faraggiana, Frost, Cowley, Cowley, Cowley, Havnes, Hauck, Hoffieit, Harper, Hartoog, DONALD Phys., 1969, 119. 53. Cameron and 12, Powell, Mem. Obs., Ap. Haven: © 258. J., E. P. P. P. Perry, 0. American M. B. C. C. 1970, 1974b, 1974a, 1972, 1970, 1965, 1973, 7, A.J., W. A. A. A. A. 0., 1967, 45, R.A.S., A. D. R. S., B., S., S. 187, M. I. I. J. W. A. D. Yale D. 1971, F. 1. H., H., P. 1968, P., P. P., P., E. 1965, J., (Baltimore: and J., J., R., 3297. P., and and 1956, 1964, Barrett, 74, C. L. Pub. Pub. Pub. N., Ap. Ap. L., R., J., L., 1968, and 551. 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Q., 1929, 1967, 152, 1. Suppl., Penny, A.S.P., Pub. D. 186, J., and Ap., 14, 1971, A.S.P., 6, 75, Golson, (3d Stars, C., 149, 483. 207. Pub. Monog. 1. Canadian 185. Jaschek, A.S.P., 18, S. 978. A. 8, ed.; Astr. III. 86, • 55. J. 428. 83, 395. ed. J., Yerkes 70. J. Provided 1974, 1967, New San Ap., 296. No. and 76, C., R. C. J. KURTZ Diego --.1968b, --. --. --. --. --. --. --. --. --. --. --. --. --. Ishikawa, Lambert, Latour, Rydgren, Lindemann, Kukarkin, Kurtz, Kurucz, Warner, van Vauclair, Smith, Slettebak, Malaroda, Reimers, Roman, Watson, Young, Nadeau, Miczaika, Michaud, Milton, Morgan, by State 31, Bull. stein, Ap. 183. 19, W. General of den Comm. the 63. 309. H. J., M. D. A.A.S. 1968c, 1975, J., R. 1972a, 1975, 1968d, 1976, 1972b, R. 1913b, 1913a, 1967, 1968b, 1971, 1973c, J. University, R. Heuvel, B. W. P.H. N. W. D. G., 1976, 108, A. D. M. G. A. E. B. A. NASA Catalog L. s. K. L., W., Spiegel, 1965, L. E., D. 1969, E., W., E., Vauclair, R., 29 1970, 1949, V., 1973, 1956, 1973, Pub. L., A.J., 1971, Ap. Mem. Astr. 107. 1911, 1970, and M.N.R.A.S., 1952, (abstract), Bull. M.N.R.A.S., M.N.R.A.S., Astr. Ap. Ap. Ap. Ap. invited and 1970, Breger, and and Efremov, E. Franklin, and Morgan, M.N.R.A.S., and J., Astr. of Astr. J., J., J. Conti, 80, J., Ap. Pub. Ap. Pub. Ap., Ap. E. Astr. P. Hauck, Astrophysics Lick Astr. R.A.S., S.A.O. Ap. Pub. Smith, 36 203, Abt, San Ap. Suppl., Variable 175, 182, 207, A., S., Warner, 637. J. paper J., J., J., of Ap., 13, M., A.S.P., Soc. Astr. Suppl., Ap., Obs. 1968a, 7, J. and Inst. 603. P. David 160, Toomre, 109, the Diego, 124, H. Yu. W. F. 765. 159. 181. B. Spec. 263. M. 138, (Letters), 140, 138, 526. 70 3, S. Evans, 25, Japan, presented A. A., 11, Pamjatnikh, Soc. IAU, Bull., Stars 1973, 129, . Netherlands, I., W., 641. 94. 547. 165. 134. 1968, A. B. 85, 5, Bull. Dunlap 277. 229. 213. 197. 1972, 325. Deutsch, Rept., and 81. 1974, Japan, CA 1968a, 263. 328. J., and 27, Sydney, (Moscow: 6, Astr. S. Ap. 162, Astr. Kholopov, Data A.J., and 160. for W., 1. Obs., No. Ap. Eggen, J., 92182 Ap. 25, L45. A. M.N.R.A.S., A. Inst. Zahn, the 19, 77, 154, and J., Australia. 309. 1974, 111. Suppl., 1, System J., IAU). 326. Joint 193, 35. 537. Netherlands, 0. and 1147. Sandmann, P. J.-P. Astr. N. J. 125. 11, Session Green- 1958, 1975, 1948, 138, 119. Ap.,