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I. Introduction
This is the fifth of a projected seven volumes in a program of systematic reclassification of the Henry Draper stars on the MK system and contains all HD stars between δ1900=–12○.0 and δ1900=+5○.0 . The previous volumes [VOL1-4] cover from δ1900=–90○.0 and δ1900=–12○.0 . It is recommended that users read the accompanying text before utilizing the catalogue in order to take full advantage of its contents and to learn the notation and practices followed.
The stars were classified visually on objective-prism plates taken with the Michigan Curtis Schmidt telescope at Cerro Tololo Inter-American Observatory. The 4○+ 6○ prisms yield a dispersion at Hγ of 108 Å/mm, and the average resolution is about 2 Å/mm, comparable to that of the original MK system [MKK]. The spectra were taken on IIaO plates and widened to 0.8 mm, with 20m, 4m, and 1m exposures being obtained. The high quality of the spectra is illustrated in our second Atlas [HN]. In order to maintain a uniform, consistent system, all the spectral classification was done by one person (Houk).
Over 170 standard stars were used. (See Tables 1-3 and section III). The HD stars were identified using computer-generated plots to the scale of the Schmidt plates [HC]. Of the 31,075 HD stars in the catalogue, 30,235 or over 97% were classifiable. Previously published types are listed for the 3% not classifiable on our plates. Over 96% of the stars in the catalogue have both temperature and luminosity types. Many of those that do not are peculiar stars. Internal classification errors were obtained using the 11% of the stars classified independently on more than one plate. Both the internal and external errors are similar to those usually obtained in classification of slit spectra. 16% of the stars have remarks in the back of the volume giving further information.
Sections below include II Acknowledgments, III. Spectral Classification, IV. Description of Catalogue, V. Description of Remarks, and References
A project of this scope, involving eventual reclassification of all the HD stars, necessarily involves the dedicated efforts of large numbers of people. These have contributed to the project in such substantial ways that it was decided the acknowledgments should hold the place of honor at the beginning, rather than appearing at the end as is customary.
First we acknowledge our enormous debt to Annie J. Cannon and the Harvard College Observatory for the Henry Draper Catalogue [CP], upon which our work is largely based. The present project scarcely would have been possible without the Henry Draper Catalogue as a foundation. Even with our present-day advantage of electronic computers and high-quality spectra the undertaking is proving a formidable one, and we appreciate and marvel more than ever at what Miss Cannon was able to do with the resources she had on hand.
We owe much to W. W. Morgan and P. C. Keenan for their encouragement and advice especially in the early stages of the project.
The role of William P. Bidelman in this undertaking is a large and critical one. For many years he had urged that such a project be carried out and he ultimately started it himself, while at the University of Michigan. He and Orren Mohler were instrumental in getting the Michigan Curtis Schmidt telescope moved to the Cerro Tololo Inter-American Observatory with the aid of a grant from the National Science Foundation. Bidelman also directed the southern observing program from 1967 through 1969. We thank him for much advice and help.
The reclassification itself might never have gotten under way if C. R. Cowley had not consented to become principal investigator and project director, obtaining the original grant from the National Science Foundation (with Anne Cowley as co-principal investigator). We thank them both very much for their support and input.
For day-to-day help on many phases of producing Volume 5 , including the training of assistants, but especially the computer programming and documentation, headed by graduate student and co-author Carrie Swift, we are deeply indebted to undergraduates Michael Allinger, James Barta, Clair Branch, Michelle Cornog, Aimee D'Onofrio, Aaron Evans, David Frankel, Carla Goodnoh, Robert Piontek, and Sarah Winfrey who all did fine work and went far beyond the call of duty, often under time pressure.
The sheer amount of data involved produced a plethora of tedious but vital clerical and proofreading tasks and a great deal of data entry. This work was mainly done by students in the University of Michigan Undergraduate Research Opportunities Program (UROP) and Work-Study Program. Almost everything was done or checked by two people to cut down on errors. We thank the following for their contributions: Richard Algra, Jena Baker, Jay Beeber, Charles Boulard, Luis Buitragn, Omar Cantu, Richard Carrera, Jean Chang, Scott Cramer, Raffy Davessia, Chaitanya Diwadkar, Michael Dojka, Adam R. Duncan, Dan Durda, Nicolas Fernandez, Rafael Francisco, Benjamin Graetz, Christopher Groesbeck, Margaret Grunow, Eric Hall, Jennifer Hippert, Angela Holt, Jason Hurley, Daniel Kocevski, Julie Lanyon (for last-minute herioc efforts), Madelene Means, Dina Mirijanian, Rafael Jose Mora, Megan Nesbitt, Thuyduong Nguyen, Jeremy J. Ortwine, Peter Rose, Erika Sandor, Elizabeth Sturgis-Doutre, Naomi Taylor, Joan Wang, A. White, Mark Wilson, Sherry Winkelman, and Joei Wroten. Names of others were lost in the mists of time, since neither UROP nor our project maintained complete records, but we are also grateful for the contributions of AB, SB, KJ, BL, SL, JHM, DN, Felipe F, SRP, CDR and JES, with apologies.
The earlier work of Wayne Fullerton, who produced the computer-generated plots of the HD stars to Schmidt scale for the whole sky, and of D. J. MacConnell, who did much early planning, observing, and training of observers, is still contributing to the success of the project.
Thanks also to the following observers, who took the high-quality plates so vital to good results: Klaus Czuia, Arturo Gomez, Gabriel Martin, Daniel Muturana, Mauricio Navarrete, and Mario Zemelman. We gratefully acknowledge the staff of the Cerro Tololo Inter-American Observatory for their help and cooperation during the 11 years that the southern survey was under way.
I am indebted to Robert F. Garrison for again kindly providing unpublished spectral types for most of the stars too overexposed to classify on Michigan plates.
The Goddard Space Flight Center has been very helpful, distributing both tape and CD-ROM versions of Volume 1, Volume 2, Volume 3, and Volume 4 of the Michigan Spectral Catalogue for us. Also Goddard's SkyView utility was very useful in identifing stars which were either on plates which had lost the matching Fullerton plots, or which were so closely spaced that identification from the plots was difficult.
We are also deeply grateful to Francois Ochsenbein and the Centre de Données Stellaires de Strasbourg for furnishing an extensive tape, which not only provided the more accurate values of right ascension and declination used in this catalogue, from the Proper Motion Catalogue, but also the CPD and SAO numbers and indication of the existence of the stars in several other catalogues, including an indication of all visual doubles. Also thanks to them for providing improved magnitudes for nearly all of the stars in this volume.
Many other people, too numerous to mention, have aided this project in various ways, and we thank everyone involved.
Finally we are especially grateful to the National Science Foundation for its continuing wholehearted support of this research, which has made the project possible. This material is based upon work supported by the National Science Foundation under Grant Numbers 8913683 and 9422318. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the National Science Foundation.
A. Standards
The similarity in resolution of our spectra to that of the original work by Morgan and Keenan [MKK] allowed us to classify on a system which is a good approximation to the MK system. We used MK standards when they were available and supplemented with others as necessary. (See Tables 1-3). Objective-prism classification differs from slit classification in that often the spectrum is not of optimum density. Almost all of our standards had from 4 to 8 widely varying exposures so a fairly good match could almost always be found with one of the 3 exposures we had of each program star. Because the appearance of the hydrogen wings varies strongly with exposure, Houk did not rely on memory but directly compared virtually all the B and A stars with one or more standards. Many stars of later type were similarly compared; it is estimated that nearly half of the classifications in the catalogue were made by direct comparison with standards. This procedure will also be followed in future volumes to avoid any drift in the system.
The primary standards are listed in Table 1 below. The MK standards were supplemented by types by Bidelman in order to get an adequate representation of supergiants. Table 2 lists 20 other stars used as standards for which plates already were available at Michigan or which were sought out in the course of the classification to fill gaps in the primary standard grid.
The vast majority of the standard spectra fit very well into a
consistent scheme, but a few did not and these 5 are listed in Table 3.
We do not suggest that other classifiers use the types we have
assigned as these are based only on one plate. Others may well come to
different conclusions. If we are wrong about these stars, then the early
G dwarfs in the catalogue may be systematically slightly late since
several standards are involved.
B. Spectral Qualities and
At the time each spectrum was classified it was assigned a quality ranging from 1 to 4. Quality 1 spectra are of near-optimum exposure and unoverlapped by other spectra. Quality 2 spectra may be slightly under or overexposed or slightly overlapped. An error analysis shows that quality 2 types are very nearly as accurate as quality 1's. Quality 3 spectra are usually quite overlapped or underexposed and quality 4 are worse, though still probably better than the HD type. About three quarters of the spectra have qualities of 1 or 2, and it is recommended that statistical studies be restricted to these stars when practicable.
About 9% of the stars were classified independently on two or more plates. A total of 34,085 independent spectra were classified to yield the 30,235 spectral types by Houk in this catalogue. These multiple classifications for a single star were combined to produce a single spectral type, in most cases via a computer program. When a single classification was of quality 1 or 2, any quality 3 or 4 classifications were discarded and the quality 1 or 2 classification was used. These cases are not designated as averages in the catalogue. When more than one quality 1 or 2 classification was present, any quality 3 or 4 classifications were discarded and an average spectral type was formed from the quality 1 or 2 classifications. If only quality 3 or 4 classifications were available, they were averaged to form a single spectral type. To form the averages the temperature and luminosity types were converted to numerical codes. These codes were then combined in a weighted average and reconverted to normal spectral notation. Quality 1's were assigned weight 1.5 and quality 2's weight 1. Likewise, when no quality 1 or 2 classifications were available, quality 3's were assigned weight 1.5 and quality 4's weight 1. In the numerical codes the temperature types that are not used in the present classification system (Fl, F4, F9, G4, G7, G9, K6, K7, K8, and K9) were treated as non-existent. For example, the difference on the numerical scale between K5 and M0 is the same as that between M0 and Ml. The types O9.5, B0.5, and B9.5 were treated as half-temperature subtypes. Luminosity type Iab was also treated as a half type, but Ia and Ib were treated as full luminosity types. Cases in which one or more of the classifications to be averaged were peculiar could not be handled by the computer and were averaged by hand, sometimes after reexamining the spectra. Whenever the classification used in the catalogue is an average, the quality assigned it is the highest of the qualities used in forming the average and the quality is prefixed with an "A". The plate codes (see section IV) of all plates used to form the average are included in the catalogue.
C. Notation
A major deviation from normal notation in the catalogue is that hyphenated types (ex.,
The other major innovation has been in the notation for spectra of peculiar stars such as weak-line stars and strong or weak CN stars. These will be discussed in detail in part E below. The general idea is to indicate the degree of the peculianty by giving `normal' temperature or luminosity types determined from different lines, such as hydrogen line vs. metal line, or CN vs. Sr. With this scheme there is no need to introduce a verbal (strong, moderate, weak) or numerical scale which requires peculiar `standards' for its definition.
Uncertain types or uncertain parts of spectral types were enclosed in parentheses - ex.,
D. Classification Criteria
Nearly all the temperature and luminosity criteria outlined by
Morgan, Keenan, and Kellman [MKK] and Johnson and Morgan [JM] are
applicable to our spectra, so the criteria will not be outlined again
here. A few problem areas are discussed in part E. Almost all the
spectral lines labeled in our Atlas [HIR] and Second Atlas [HN] are
temperature and luminosity criteria. In addition to these and other MK
criteria, the general appearance of the spectrum was an important factor
in arriving at the final spectral type. Much of the classifier's previous
experience had been with low-dispersion spectra where the overall
appearance of the spectrum was of paramount interest. This approach was
carried over into the present work as much as possible, and the unknown
and standard spectra were considered as a whole in getting the best match.
E. Problems, Notation, and
O Stars
There are 22 O stars in the catalogue. Many O stars occur in tight
clusters where the overlap problems on objective prism plates are so bad
that they preclude discovery or at least lower the quality of the type
given. Because of such classification uncertainties Walborn's system
[W] of designating Of stars was not used for the few found. However,
since the lines in emission are listed in the remarks, such types may be
estimated.
B Stars
There are about 3000 B stars. The main classification problem was luminosity separation of giants and dwarfs for the mid-B stars. Even for good quality spectra, the differences are subtle on our plates. For example, compare π Ori and κ Hya on the B5 sheet of the Atlas. An area which may have been somewhat inadequately covered is the problem of moderately He-rich or He-poor stars. Only fairly strong cases would have been noticed. B stars are not designated as `e' unless the emission is above continuum level. When a line is totally, partially, or possibly filled in, a remark is made to that effect. Finally, a matter of notation: although most peculiar Si stars are really of type B, all such peculiar stars were designated Ap stars. Any exceptionally early cases have remarks.
A Stars
There are about 5800 A stars including ~300 Am and Ap stars. The notation used for the Am stars (ex., A2mA5-F0) gives three types. The first gives the type indicated by the Ca K line strength. The second, and least accurate, gives the type indicated by the hydrogen lines. The problem here is that in Am stars the hydrogen wings are suppressed. Hence comparing with ordinary dwarf standards gives too late a type. The third type is that indicated by the metal strength. Am stars have giant-like metals, and giant standards were used to get this type. For the Ap stars the elements (ex., ApCrEuSr) are listed in order of the strengths of the lines. Ap stars of the HgMn type are not usually detected at the resolution used here.
F Stars
There are nearly 7300 F stars. Note that peculiar stars are all called `Ap' even though a few are as late as FO or F2. There are a very few unusually late metallic-line stars called Fm which have G bands but also have line strengths (strong Sr λ4077 and λ4150, λ4416 << λ4481) similar to Am stars. There is a larger intermediate group which is called
`Fm δDel' since the characteristics are more similar to Am's than Ap's.
G Stars
There are about 6100 G stars. The following notation is used for weak-metal stars (ex., G5wFO): temperature type based on the H lines followed by a `w' and then the type based on the metal lines. Sometimes a luminosity type is also included. The difference between the two types indicates the degree of metal weakening. This notation breaks down in the case of extremely metal-weak or early stars where no metal type can be derived. For these the H-line type followed by a `w' is given in the catalogue accompanied by a remark in the back of the volume. Stars with no G-band or a very weak G-band are given no special designation but the type is followed by a `p' and a remark is included. A similar procedure is followed for stars with strong CH.
K Stars
There are about 7600 K stars including stars having noticeably weak or strong CN. In the catalogue the CN strength is indicated by a `pseudo-luminosity' as determined from the CN break and CN band strength (ex.,
M and C Stars
There are about 700 M stars and 20 C stars. C stars were not assigned subtypes.
Emission Stars and Other Miscellaneous Types
Stars which showed hydrogen lines in emission are designated with an `e'. A remark usually indicates what lines were seen in emission. Following the traditional practice, stars with Ca H + K but not hydrogen in emission are designated with a `p'. All of these stars have remarks indicating that Ca H + K are in emission.
Wolf-Rayet stars were classified `WN' or `WC'. No attempt was made to subdivide the Wolf-Rayet stars further.
The type `NEBULA' includes any spectrum, either emission or continuous, which looked extended rather than stellar. Thus it includes H II regions, planetary nebulae, and globular clusters. When the nebulae were identified on the tape provided by the Centre
de Données Stellaires de Strasbourg, these identifications were included in the remarks.
Column:
Further explanation of some columns in the catalogue:
Column 1. HD number. All stars in the Henry Draper Catalogue having δ1900 south of (and including) +5○.00 and north of –12○.00 are included, whether a new spectral type is available or not. It seemed unnecessary and unwise to introduce a consecutive running number since all the stars in these volumes will be HD stars. Note that due to an error in the HD Catalogue, HD numbers 91169 and 109005 represent the same star. It has been listed twice in the volume for the user's convenience.
Column 2. Spectral type. A dagger (+) in front of the type indicates it is taken from another source. For each such type there is a remark in the back of the volume.
For an explanation of spectral notation please read section III above.
Column 3. If the spectral type is the average from two or more plates (see plate code column 13), then an A indicates this (see section III ). See section III B for a description of the quality, and Section V below for a description of the remark codes.
Column 4. Unless otherwise noted, the magnitude given is photographic, and was supplied by the Centre de Données Stellaires de Strasbourg. Other magnitudes are noted by V (
Column 5-8. The coordinates given are based on the Epoch 2000 coordinates supplied by Strasbourg, from the proper motion catalogue. Following tradition and to maintain consistency with previous volumes, we list the Epoch 1900 coordinates and the precession to 2000.
Column 11. The declination zone of Volume 5
is
north of the dividing line between the CoD catalogue in the south and the
BD(SD) catalogue in the north. Therefore these numbers are from the BD catalogue. For stars with out a DM number, the CSI number is listed (
Column 13. Plate Code(s). Each plate has been assigned an identification code. By use of Table 4, knowing the plate code, the plate number and date the plate was taken can be obtained. These columns also serve to indicate the number of plates used in obtaining the average spectral type given. Plates whose codes start with 3 or 4 are the short-exposure plates of 3m + 1m or 4m + 1m exposure, respectively. Codes starting with 8 or 9 are 20m exposures at slightly different centers which are used only for stars not on the main plate.
Further information about 4906 stars is given at the back of the catalogue. To aid the user in deciding whether to consult the remarks of a particular star, the
following notation is used in Column 3 of the catalogue:
B indicates that the remark contains the HR (from The Bright Star Catalogue)
number and the Bayer or Flamsteed designations where applicable. (1164 stars)
L indicates that information from the astronomical literature is given. Remarks designated O (other) in previous Volumes are now included as L remarks. In most cases individual literature references are not given; references systematically searched are listed at the end of this section. Remarks were generally limited to those relevant to the spectral appearance, such as rotation, variablity, and duplicity, and generally have included only information about the star which might affect the spectral classification. However, for the first time proper motions of LHS stars are given. The entry `Emission Catalogue' refers to Wackerling's catalogue. (1121 stars)
R 846 of the stars in the remarks section have remarks of this type. All
`R' remarks were written by NH in the course of the spectral classification and all are related in some way to the spectrum. The other remark types (i.e. V,D etc.) were not available to NH during classification. The symbols and notation are self-explanatory. We discuss some of the more frequent types of `R' remarks.
283 stars in the catalogue have composite spectra or possibly composite spectra and each of these has a remark so that it can be easily differentiated from known double stars which also sometimes have two types listed in the catalogue.
In 290 cases the fact that the star was visually double was deduced from the appearance of the spectrum. Most of these clearly showed early and late components. The rest were suspected to be double because they were fuzzy, double-lined, or closely overlapped. The following data were listed (taken from [IDS], prior to 1996; from 1996 on [WDS] was used): position angle p, angular distance d, and magnitudes of components. Sometimes a rough spectral type for the secondary component is also listed in the remarks, but often only a single type is listed in the catalogue, and it may actually be an average of the two components in some cases.
Remarks are made for all stars (~ 75) showing emission or filled-in lines, and the lines in emission are identified in the remark. For nebulae the lines in emission are often not listed.
The great majority of Am stars do not have remarks, but ~ 50 do. Similarly some 40 of the Ap stars have `R'
remarks. For both Am and Ap stars these are mainly weak or questionable cases, and the spectral type listed in the catalogue may not indicate the possible metallic-line
or peculiar nature of the star. Unusual and extremely strong cases are also included among the remarks.
About 20 of the `R' remarks pertain to fuzzy or closely overlapped spectra some of which are probably new visual doubles.
About 40 of the weak-metal stars have `R' remarks. In many cases the spectral type indicated by the G band is given to supplement the H-line and metallic-line types given in the catalogue. Slight or questionable and extreme cases are also noted.
Other smaller categories of `R' remarks include:
substantial disagreements with the HD catalogue, mainly with respect to spectral types; possible Fm δ Del types; stars with strong CH - these are not indicated in the catalogue spectral types; star with weak CH, strong CN or weak CN.
D The Centre de Données Stellaires de Strasbourg provided a listing of visual double
stars from the Index Catalogue of Double Stars (commonly referred to as the Lick Catalogue). Remarks beginning `undetected visual double' were included for doubles
not discovered in the course of the spectral classification, the others having `R' remarks. `D' remarks were included for the 1904 doubles having a separation of < 30" and a Δ magnitude of < 4.0 mag, since for these the spectral appearance, and hence the assigned spectral type might be affected.
V All variables (337 stars) are indicated by a 'V' remark. Each has a remark in the back of the catalogue giving variable star designation, type of variablity, magnitude range and period, when these are known.
+ All spectral types in the catalogue taken from other sources are preceded by a dagger. Each such star has a remark giving the reason the star could not be classified on Michigan plates, and the source of the classification. Many are taken from the HD catalogue. Classifications of many bright stars were provided by R. F. Garrison, and are listed as `Garrison types'. W. Warren provided types for stars that were overlapped on our plates, where available. These are listed as `Warren types', and are followed by a number which indicates which references were used by Warren to obtain the type. Please see the references section. All stars that did not have a Garrison or Warren type were researched using the SIMBAD utility of the Centre
de Données Stellaires de Strasbourg. Those stars with MK types on SIMBAD are listed as `SIMBAD types'.
References for the preface:
G = general reference for the Catalogue
Name HR No. HD No. Spectral Type Source Name HR No. HD No. Spectral Type Source
τ CMa 2782 57061 O9 Ib + MK (1973) 16 Sgr 6823 167263 O9 II J+M (1953) * ι Ori 1899 37043 O9 III + MK (1973) — — 52266 O9 V J+M (1953) — 6347 154368 O9.5 Iab B (1954) ζ Ori 1948 37742 O9.5 Ib J+M (1953) δ Ori 1852 36486 O9.5 II J+M (1953) σ Ori 1931 37468 O9.5 V + MK (1973) ** 15 Sgr 6822 167264 B0 Ia J+M (1953) ** — 6219 150898 B0 Iab B (1954) ** — 2479 48434 B0 III J+M (1953) δ Sco 5953 143275 B0.3 IV [B0.5 IV] + MK (1953) [H,G,S (1969)] τ Sco 6165 149438 B0 V + MK (1973) ** κ Ori 2004 38771 B0 .5 Ia + MK (1973) ** — 6142 148688 B1 Ia B (1954) * ρ Leo 4133 91316 B1 Ib J+M (1953) * σ Sco 6084 147165 B1 III J+M (1953) ** ω1 Sco 5993 144470 B1 V + MK (1973) ** χ2 Ori 2135 41117 B2 Ia + MK (1973) ε CMa 2618 52089 B2 II J+M (1953) ** π4 Ori 1552 30836 B2 III J+M (1953) γ Peg 39 886 B2 IV + MK (1973) 22 Sco 6141 148605 B2 V + MK (1973) 3 Gem 2173 42087 B2.5 Ib J+M (1953) σ Sgr 7121 175191 B2.5 V + MK (1973) o2 CMa 2653 53138 B3 Ia + MK (1973) ** — 3654 79186 B3 Ia B (1954) ** κ Cru — 111973 B3 Iab B (1954) ι Cma 2596 51309 B3 II J+M (1953) ν Ori 2159 41753 B3 V J+M (1953) — 6450 157038/9 B4 Ia B (1954) * η CMa 2827 58350 B5 Ia + MK (1973) ** — 3456 74371 B5 Iab B (1954) ** 67 Oph 6714 164353 B5 Ib J+M (1953) * τ Ori 1735 34503 B5 III J+M (1953) ι Aql 7447 184930 B5 III J+M (1953) ** κ Hya 3849 83754 B5 V J+M (1953) ψ2 Aqr 8858 219688 B5 V J+M (1953) — — 183143 B7 Ia J+M (1953) ** — 3708 80558 B7 Iab B (1954) ** β Ori 1713 34085 B8 Ia + MK (1973) ** γ CMa 2657 53244 B8 II J+M (1953) 18 Tau 1144 23324 B8 V + MK (1973) ** — 4338 96919 B9 Ia B (1954) — 1804 35600 B9 Ib J+M (1953) γ Lyr 7178 176437 B9 III J+M (1953) 134 Tau 2010 38899 B9 IV J+M (1953) ** — 4169 92207 A0 Ia B (1954) ** 13 Mon 2385 46300 A0 Ib J+M (1953) * γ Gem 2421 47105 A0 IV J+M (1953) γ UMa 4554 103287 A0 V + MK (1973) ** — 4876 111613 A1 Ia B (1954) ι Ser 5842 140159 A1 V J+M (1953) β Ser A 5867 141003 A2 IV J+M (1953) β Eri 1666 33111 A3 III J+M (1953) ** β Leo 4534 102647 A3 V J+M (1953) α PsA 8728 216956 A3 V + MK (1973) δ Leo 4357 97603 A4 V J+M (1953) ** — 825 17378 A5 Ia J+M (1953) ** — 2874 59612 A5 Ib J+M (1953) * o Sco 6081 147084 A5 II + MK (1973) ** — 3739 81471 A7 Iab B (1954) ** — 6144 148743 A7 Ib B (1951) θ2 Tau 1412 28319 A7 III J+M (1953) 21 LMi 3974 87696 A7 V J+M (1953) γ Her 6095 147547 A9 III J+M (1953) ** — 4110 90772 F0 Ia B (1954) α Lep 1865 36673 F0 Ib + MK (1973) ζ Leo 4031 89025 F0 III + MK (1973) µ Cet 813 17094 F0 IV J+M (1953) ρ Gem 2852 58946 F1A9 [F0 V] G, unpubl. [J+M (1953)] ** 89 Her 6685 163506 F2 Ia J+M (1953) — 3496 75276 F2 Iab B (1954) ** ν Agl 7387 182835 F2 Ib J+M (1953) ** ν Her 6707 164136 F2 II J+M (1953) * 14 Ari 623 13174 F2 III J+M (1953) * σ Boo 5447 128167 F2 V J+M (1953) 46 Tau 1309 26690 F3 IV/V [F3 V] M, unpubl. [J+M (1953)] ** — 2957 61715 F4 Iab B (1951) ** — — 172052 F5 Ib B (1951) * 41 Cyg 7834 195295 F5 II J+M (1953) * β Del 7882 196524 F5 III B (1951) 45 Boo 5634 134083 F5 V J+M (1953) — 7308 180583 F6 II B (1951) — 6577 160365 F6 III + MK (1973) α Tri 544 11443 F6 IV + MK (1973) ** γ Ser 5933 142860 F6 V J+M (1953) ι Psc 8969 222368 F7 V J+M (1953) ** δ CMa 2693 54605 F8 Ia J+M (1953) ** γ1 Nor 6058 146143 F8 Iab B (1954) ** 11 Pup 3102 65228 F8 II B (1951) υ Peg 8905 220657 F8 IV J+M (1953) β Vir 4540 102870 F9 V [F8 V] + MK (1973) [J+M (1953)] ** — 4511 101947 G0 Ia B (1954) — 8752 217476 G5 var 0 [G0 Ia] MK (1973) [J+M (1953)] β Aqr 8232 204867 G0 Ib + MK (1973) * 31 Com 4883 111812 G0 III + MK (1973) * η Boo 5235 121370 G0 IV J+M (1953) ε Leo 3873 84441 G1 II [G0 II] MK (1973) [J+M (1953)] — — 27836 G1 V + MK (1973) ** ζ Mon 3188 67594 G2 Ib + MK (1973) Sun (Uranus) — — G2 V + MK (1973) ξ Pup 3045 63700 G3 Ib B (1951) ** 9 Peg 8313 206859 G5 Ib + MK (1973) * 25 Gem 2453 47731 G5 Ib J+M (1953) * ω Gem 2630 52497 G5 II J+M (1953) — 1327 27022 G4 III [G5 III] MK (1973) [J+M (1953)] µ Her 6623 161797 G5 IV MK (1973) ** κ1 Cet 996 20630 G5 V J+M (1953) ** ε Gem 2473 48329 G8 Ib + MK (1973) ζ Cyg 8115 202109 G8 II CN 1 [G8 II] + MK (1973) [J+M (1953)] η Psc 437 9270 G8 III J+M (1953) κ Gem 2985 62345 G8 IIIa [G8 III] + MK (1973) [J+M (1953)] β Aql 7602 188512 G8 IV + MK (1973) ξ Boo (A) 5544 131156 G8 V J+M (1953) ** 12 Peg 8321 207089 K0 Ib MK (1973) θ1 Tau 1411 28307 K0 III J+M (1953) δ Eri 1136 23249 K0 IV J+M (1953) * 54 Psc 166 3651 K0 V J+M (1953) ζ Cep 8465 210745 K1.5 Ib + MK (1973) — 2334 45416 K1 II J+M (1953) 1 Peg 8173 203504 K1 III MK (1973) γ Cep 8974 222404 K1 IV MK (1973) 107 Psc 493 10476 K1 V J+M (1953) ε Peg 8308 206778 K2 Ib + MK (1973) 56 Ori 2037 39400 K1.5 IIb [K2 II] + MK (1973) [J+M (1953)] ** σ Oph 6498 157999 K2 II [K3 II] + MK (1973) [M,C,W (1955)] ** β Oph 6603 161096 K2 III + MK (1973) α Ari 617 12929 K2 IIIab + MK (1973) α Ser 5854 140573 K2 V + MK (1973) — 6806 166620 K2 III CN 1.5 J+M (1953) ** o1 CMa 2580 50877 K2.5 Iab [K3 Iab] + MK (1973) [J+M (1953)] η Per A 834 17506 K3-Ib-IIa [K3 Ib] + MK (1973) [J+M (1953)] θ Del 7892 196725 K3 Ib B (1951) * γ Aql 7525 186791 K2 II + MK (1973) π Her 6418 156283 K3 IIab + MK (1973) * δ And 165 3627 K3 III + MK (1973) ** β Cnc 3249 69267 K4 III + MK (1973) ξ Cyg 8079 200905 K4.5 Ib-II [K5 Ib] + MK (1973) [J+M (1953)] α Tau 1457 29139 K5 III + MK (1973) ** γ Dra 6705 164058 K5 III + MK (1973) — — 154363 K5 V J+M (1953) ν Gem 2905 60522 M0 III MK (1973) 6 Gem 2197 42543 M1-M2 Ia-Iab [M1 Ia] + MK (1973) [J+M (1953)] α Ori 2061 39801 M1-M2 Ia-Ib [M2 Iab] + MK (1973) [J+M (1953)] ** 119=CE Tau 1845 36389 M2 Iab-Ib [M2 Ib] + MK (1973) [J+M (1953)] * — — 95735 M2 V J+M (1953) µ Gem 2286 44478 M3 IIIab + MK (1973) η Gem 2216 42995 M3 III MKK (1943) 45=RZ Ari 867 18191 M6 III + MK (1973) ** — — 207076 M7 III MK (1973) * in First Atlas only ** in Second Atlas (A dagger(+) in front of this reference indicates that the spectral type has undergone re-examination by Morgan for self-consistency).
Name HR No. HD No. Spectral Type Source — — 93619 B1 Iab H+C (1975) — 2360 45796 B6 V H,G,S (1969) — 3898 85355 B7 III H,G,S (1969) — — 149019 B9/A0 Iab H+C (1975) — 4218 93526 A0 III CCJJ (1969) — 3981 87887 A0 III CCJJ (1969) o Peg 8641 214994 A1 IV CCJJ (1969) — — 2692/3 A3 Ia H+C (1975) τ Peg 8880 220061 A5 IV H+C (1975) σ2 Tau 1479 29488 A5 V CCJJ (1969) — — 96746 G2 Iab H+C (1975) δ CrB 5889 141714 G5 III/IV R (1952) θ Psc 8916 220954 K1 III R (1952) — — 184467 K1 V R (1955) — 753 16160 K3 V R (1955) — 6005 144889 K4 III R (1955) — 7633 189276 K5 II/III R (1952) — — 79210/1 M0 V + M0 V R (1952) — 4278 5129 M2 III R (1955) — 4333 96813 M4 III H+C (1975)
Spectral Standard Name HR No. HD No. Type Used Spec. Type Source * β Com 4983 114710 G2 V G0 V +MK (1973) ζ Her 6212 150680 G3 IV G1 IV +MK (1973) ξ Pup 3045 63700 G3 Iab/Ib G3 Ib J-M (1953) 85 Peg 9088 224930 G3/5 V G2 V M,H,J (1953) G3 V R(1955) π Leo 3950 86663 M1 III M2 IIIab[M2 III] +MK (1973) Sources B(1951) Bidelman, W. P. 1951, Ap. J.,113,304. B(1954) Bidelman, W. P. 1954, Pub. A.S.P.,75,226. CCJJ (1969) Cowley, A. P.,Cowley, C. R., Jaschek, M., and Jaschek, C. 1969, A. J.,74,375. H+C (1975) Houk, N., and Cowley, A. P. 1975, University of Michigan Catalogue of Two-Dimensional Spectral Types, for the HD Stars (Astronomy Dept.,Univ. of Mich.,Ann Arbor, Michigan). H,G,S(1969) Hiltner, W. A., Garrison, R. F., and Schild, R. E. 1969, Ap. J.,157,313. J+M(1953) Johnson, H. L., and Morgan, W. W. 1953, Ap. J.,117,313. M,C,W(1955) Morgan, W. W., Code, A. D., Whitford, A. E. 1955, Ap. J. Suppl.,2,41. M,H,J (1953) Morgan, W. W., Harris, D. L., and Johnson, H. L., 1953, Ap. J.,118,92. MK(1973) Morgan, W. W., and Keenan, P. C. 1973,Ann Rev Astr and Ap.,11,29. MKK (1943) Morgan, W. W., Keenan, P. C. and Kellman, E. 1943, An Atlas of Stellar Spectra (University of Chicago Press) R (1952) Roman, N. G. 1952, Ap. J.,116,122. R (1955) Roman, N. G. 1955, Ap. J. Suppl.,2,195.
Averaging
Miscellaneous Comments
Quality: 1 (best) to 4 (worst)
Remarks code: V,B,L,R,D
Plate Plate Plate Plate Plate Plate Code Number Date Code Number Date Code Number Date Plate Plate Plate Plate Plate Plate Code Number Date Code Number Date
Code Number Date
YE 1334 Dec. 2/3 '67
ZH 1323 Dec. 1/2 '67
ZL 1355 Dec. 3/4 '67 ZN 1325 Dec. 1/2 '67
ZO 1326 Dec. 1/2 '67
ZP 17304 Dec. 12/13 '74 ZQ 1327 Dec. 1/2 '67
ZR 1344 Dec. 2/3 '67
ZS 1328 Dec. 1/2 '67 ZT 1345 Dec. 2/3 '67
ZU 1346 Dec. 2/3 '67
ZV 1331 Dec. 1/2 '67 ZW 1347 Dec. 2/3 '67
ZX 1332 Dec. 1/2 '67
ZZ 1348 Dec. 2/3 '67 AAA 3563 Jan. 16/17 '69
AAB 15546 Jan. 24/25 '74
AAD 15547 Jan. 24/25 '74 AAE 17291 Dec. 11/12 '74
ABF 3565 Jan. 16/17 '69
ABG 3600 Jan. 21/22 '69 ABH 3615 Jan. 22/23 '69
ABI 20232 Dec. 27/28 '76
ABJ 21732 June 1/2 '78 ABM 7915 Jan. 30/31 '71
ABN 4759 July 7/8 '69
ABQ 4819 July 15/16 '69 ABR 7880 Jan. 27/28 '71
ABS 7881 Jan. 27/28 '71
ABT 4582 June 15/16 '69 ABU 8454 Mar. 29/30 '71
ABX 8455 Mar. 29/30 '71
ABY 6117 Mar. 10/11 '70 ACA 8456 Mar. 29/30 '71
ACB 8457 Mar. 29/30 '71
ACC 8458 Mar. 29/30 '71 ACH 4594 June 16/17 '69
ACI 4739 July 5/6 '69
ACN 16551 Aug. 11/12 '74 ACR 4740 July 5/6 '69
ACS 4596 June 16/17 '69
ACT 4597 June 16/17 '69 ACU 4574 June 15/16 '69
ACV 4595 June 16/17 '69
ADE 8428 Mar. 26/27 '71 ADL 6114 Mar. 10/11 '70
ADR 2505 June 23/24 '68
ADY 13522 May 31/June 1 '73 ADZ 2503 June 23/24 '68
AEC 2504 June 23/24 '68
AEE 16550 Aug. 11/12 '74 AEF 4579 June 15/16 '69
AEH 4580 June 15/16 '69
AEJ 4760 July 7/8 '69 AEK 4761 July 7/8 '69
AEN 4577 June 15/16 '69
AFD 4817 July 15/16 '69 AFH 4818 July 15/16 '69
AFI 4820 July 15/16 '69
AFJ 4821 July 15/16 '69 AFM 4762 July 7/8 '69
AFN 13567 June 2/3 '73
AFV 1329 Dec 1/2 '67 AFW 7253 Aug. 28 '70
AFX 7254 Aug. 28 '70
AFY 7276 Aug. 30 '70 AFZ 7256 Aug. 28 '70
AGA 7257 Aug. 28 '70
AGB 7258 Aug. 28 '70 AGC 1208 Nov. 19/20 '67
AGD 1209 Nov. 19/20 '67
AGE 1210 Nov. 19/20 '67 AGF 1315 Nov. 30/Dec. 1 '67
AGG 1309 Nov. 30/Dec. 1 '67
AGH 1308 Nov. 30/Dec. 1 '67 AGI 13569 June 2/3 '73
AGJ 17307 Dec. 12/13 '74
AGK 7255 Aug. 28 '70 AGL 1330 Dec. 1/2 '67
AGM 1300 Nov. 30/Dec. 1 '67
AGN 1304 Nov. 30/Dec. 1 '67 AGO 1305 Nov. 30/Dec. 1 '67
AGP 1306 Nov. 30/Dec. 1 '67
AGQ 1307 Nov. 30/Dec. 1 '67 AGR 1317 Dec. 1/2 '67
AGS 17309 Dec. 12/13 '74
AGT 1312 Nov. 30/Dec. 1 '67 AGU 1311 Nov. 30/Dec. 1 '67
AGV 1301 Nov. 30/Dec. 1 '67
AGW 1219 Nov. 20/21 '67 AGX 1220 Nov. 20/21 '67
AGY 1227 Nov. 20/21 '67
AGZ 1302 Nov. 30/Dec. 1 '67 AHA 1229 Nov. 21/22 '67
AHB 1303 Nov. 30/Dec. 1 '67
AHC 9713 Oct. 14/15 '71 AHD 16790 Aug. 17/18 '74
AHE 16789 Aug. 17/18 '74
AHF 16792 Aug. 17/18 '74 AHG 17294 Dec. 12/13 '74
AHH 7914 Jan. 30/31 '71
AHI 7911 Jan. 30/31 '71 AHJ 17178 Dec. 5/6 '74
AHK 16793 Aug. 17/18 '74
AHL 16795 Aug. 17/18 '74 AHM 16796 Aug. 17/18 '74
AHN 9526 Sept. 21/22 '71
AHO 1310 Nov. 30/Dec. 1 '67 AHP 7272 Aug. 29 '70
AHQ 7273 Aug. 29 '70
AHR 1316 Nov. 30/Dec. 1 '67 AHS 3469 Jan. 8/9 '69
AHT 3493 Jan. 11/12 '69
AHU 3474 Jan. 9/10 '69 AHV 3470 Jan. 8/9 '69
AHW 9714 Oct. 14/15 '71
AHX 3475 Jan. 9/10 '69 AHY 3494 Jan. 11/12 '69
AHZ 3477 Jan. 9/10 '69
AIA 3476 Jan. 9/10 '69 AIB 3512 Jan. 13/14 '69
AIC 17265 Dec. 11/12 '74
AID 17292 Dec. 11/12 '74 AIE 17176 Dec. 5/6 '74
AIF 3478 Jan. 9/10 '69
AIG 17175 Dec. 5/6 '74 AIH 5867 Feb. 4/5 '70
AII 3616 Jan. 22/23 '69
AIJ 3561 Jan. 16/17 '69 AIK 5866 Feb. 4/5 '70
AIL 7910 Jan. 30/31 '71
AIM 7912 Jan. 30/31 '71 AIN 7894 Jan. 28/29 '71
AIO 6131 Mar. 12/13 '70
AIP 6132 Mar. 12/13 '70 AIQ 8314 Mar. 20/21 '71
AIR 8315 Mar. 20/21 '71
AIS 8316 Mar. 20/21 '71 AIT 8328 Mar. 21/22 '71
AIU 8329 Mar. 21/22 '71
AIV 8327 Mar. 21/22 '71 AIW 9715 Oct. 14/15 '71
AIX 9716 Oct. 14/15 '71
AIY 9527 Sept. 21/22 '71 AIZ 9566 Sept. 23/24 '71
AJA 6145 Mar. 13/14 '70
AJB 7284 Aug. 30 '70 AJC 7285 Aug. 30 '70
AJD 16852 Aug. 25/26 '70
AJE 7286 Aug. 30 '70 AJF 21734 June 1/2 '70
AJG 18239 May 5/6 '75
AJH 18240 May 5/6 '75 AJI 17180 Dec. 5/6 '74
AJJ 20224 Dec. 22/23 '76
AJK 15585 Jan. 28/29 '74 AJL 7916 Jan. 30/31 '71
AJM 6135 Mar. 12/13 '70
AJN 3545 Jan. 15/16 '69 AJO 3490 Jan. 11/12 '69
AJP 3508 Jan. 13/14 '69
AJQ 3509 Jan. 13/14 '69 AJR 3523 Jan. 14/15 '69
AJS 3510 Jan. 13/14 '69
AJT 6133 Mar. 12/13 '70 AJU 3511 Jan. 13/14 '69
AJV 3544 Jan. 15/16 '69
AJW 7895 Jan. 28/29 '71 AJX 6134 Mar. 12/13 '70
AJY 7897 Jan. 28/29 '71
AJZ 6124 Mar. 11/12 '70 AKA 3633 Jan. 24/25 '69
AKB 3489 Jan. 11/12 '69
AKC 3481 Jan. 10/11 '69 AKD 3612 Jan. 22/23 '69
AKE 3488 Jan. 1/2 '69
AKF 3482 Jan. 10/11 '69 AKG 8320 Mar. 20/21 '71
AKH 3471 Jan. 8/9 '69
AKI 3495 Jan. 12/13 '69 AKJ 6136 Mar. 12/13 '70
AKK 8170 Mar. 1/2 '71
AKL 8313 Mar. 20/21 '71 AKM 8152 Feb. 28/Mar. 1 '71
AKN 8149 Feb. 28/Mar. 1 '71
AKO 8148 Feb. 28/Mar. 1 '71 AKP 8169 Mar. 1/2 '71
AKQ 7920 Jan. 30/31 '71
AKR 8104 Feb. 25/26 '71 AKS 8171 Mar. 1/2 '71
AKT 8153 Feb. 28/Mar. 1 '71
AKU 18199 May 4/5 '75 AKV 3562 Jan. 16/17 '69
AKW 8154 Feb. 28/Mar. 1 '71
AKX 3487 Jan. 11/12 '69 AKY 6146 Mar. 13/14 '70
AKZ 4602 June 16/17 '69
ALA 6147 Mar. 13/14 '70 ALB 8150 Feb. 28/Mar. 1 '71
ALC 8151 Feb. 28/Mar. 1 '71
ALD 6137 Mar. 12/13 '70 ALE 6138 Mar. 12/13 '70
ALF 8337 Mar. 21/22 '71
ALG 18241 May 5/6 '75 ALH 20710 June 14 '77
ALI 13158 April 25/26 '73
ALJ 8136 Feb. 27/28 '71 ALK 4783 July 14/15 '69
ALL 6125 Mar. 11/12 '70
ALM 6126 Mar. 11/12 '70 ALN 4641 June 18/19 '69
ALO 16613 Aug. 13/14 '74
ALP 4752 July 7/8 '69 ALQ 4643 June 18/19 '69
ALR 4642 June 18/19 '69
ALS 4621 June 17/18 '69 ALT 16612 Aug. 13/14 '74
ALU 4622 June 17/18 '69
ALV 4598 June 16/17 '69 ALW 16771 Aug. 17/18 '74
ALX 4784 July 14/15 '69
ALY 4806 July 15/16 '69 ALZ 20685 June 13/14 '77
AMA 4807 July 15/16 '69
AMB 4808 July 15/16 '69 AMC 4785 July 14/15 '69
AMD 4809 July 15/16 '69
AME 4810 July 15/16 '69 AMF 4788 July 14/15 '69
AMG 16773 Aug. 17/18 '74
AMH 13571 June 2/3 '73 AMI 4794 July 14/15 '69
AMJ 4793 July 14/15 '69
AMK 20724 July 14 '77 AML 9737 Oct. 15/16 '71
AMM 9669 Oct. 12/13 '71
AMN 9668 Oct. 12/13 '71 AMO 9667 Oct. 12/13 '71
AMP 9738 Oct. 15/16 '71
AMQ 9717 Oct. 14/15 '71 AMR 9661 Oct. 11/12 '71
AMS 9567 Sept. 23/24 '71
AMT 17266 Dec. 11/12 '74 AMU 3520 Jan. 14/15 '69
AMV 17268 Dec. 11/12 '74
AMW 3517 Jan. 14/15 '69 AMX 8173 Mar. 1/2 '71
AMY 3543 Jan. 15/16 '69
AMZ 8317 Mar. 20/21 '71 ANA 13151 April 25/26 '73
ANB 3522 Jan. 14/15 '69
ANC 20231 Dec. 27/28 '76 AND 8331 Mar. 21/22 '71
ANE 17270 Dec. 11/12 '74
ANF 10889 April 9/10 '72 ANG 8330 Mar. 21/22 '71
ANH 8353 Mar. 22/23 '71
ANI 3521 Jan. 14/15 '69 ANJ 20211 Dec. 20/21 '76
ANK 3611 Jan. 22/23 '69
ANL 17345 Dec. 14/15 '74 ANM 8350 Mar. 22/23 '71
ANN 8351 Mar. 22/23 '71
ANO 8352 Mar. 22/23 '71 ANP 10988 April 15/16 '72
ANQ 10990 April 15/16 '72
ANR 3519 Jan. 14/16 '69 ANS 3498 Jan. 12/13 '69
ANT 3497 Jan. 12/13 '69
ANU 3518 Jan. 14/15 '69 ANV 3537 Jan. 15/16 '69
ANW 3496 Jan. 12/13 '69
ANX 4792 July 14/15 '69 ANY 8332 Mar. 21/22 '71
ANZ 4790 July 14/15 '69
AOA 4813 July 15/16 '69 AOB 17436 Dec. 19/20 '74
AOC 20210 Dec. 20/21 '76
AOD 10868 April 8/9 '72 AOE 4644 June 18/19 '69
AOF 18169 May 3/4 '75
AOG 4645 June 18/19 '69 AOH 4646 June 18/19 '69
AOI 4755 July 7/8 '69
AOJ 4647 June 18/19 '69 AOK 20688 June 13 '77
AOL 4603 June 16/17 '69
AOM 7252 Aug. 28 '70 AON 7275 Aug. 30 '70
AOO 8239 Mar. 5/6 '71
AOP 16718 Aug. 16/17 '74 AOQ 7279 Aug. 30 '70
AOR 4624 June 17/18 '69
AOS 16712 Aug. 16/17 '74 AOT 16727 Aug. 16/17 '74
AOU 7291 Aug. 31 '70
AOV 16767 Aug. 17/18 '74 AOW 7278 Aug. 30 '70
AOX 9653 Oct. 11/12 '71
AOY 9666 Oct. 12/13 '71 AOZ 9733 Oct. 12/13 '71
APA 4757 July 7/8 '69
APB 13591 June 3/4 '73 APC 7243 Aug. 24 '70
APD 13570 June 2/3 '73
APE 7290 Aug. 31 '70 APF 7292 Aug. 31 '70
APG 7293 Aug. 31 '70
APH 7277 Aug. 30 '70 API 9648 Oct. 11/12 '71
APJ 7280 Aug. 30 '70
APK 9664 Oct. 12/13 '71 APL 9665 Oct. 12/13 '71
APM 4625 June 17/18 '69
APN 4626 June 17/18 '69 APO 13547 June 1/2 '73
APP 16686 Aug. 15/16 '74
APQ 16688 Aug. 15/16 '74 APR 16690 Aug. 15/16 '74
APS 5015 Aug. 12/13 '69
APT 5016 Aug. 12/13 '69 APU 4811 July 15/16 '69
APV 4789 July 14/15 '69
APW 4812 July 15/16 '69 APX 13551 June 1/2 '73
APY 13552 June 1/2 '73
APZ 13572 June 2/3 '73 AQA 9776 Oct. 20/21 '71
AQB 9777 Oct. 20/21 '71
AQC 9778 Oct. 20/21 '71 AQD 9729 Oct. 15/16 '71
AQE 9730 Oct. 15/16 '71
AQF 9649 Oct. 11/12 '71 AQG 9650 Oct. 11/12 '71
AQH 9651 Oct. 11/12 '71
AQI 9652 Oct. 11/12 '71 AQJ 10893 April 9/10 '72
AQK 10895 April 9/10 '72
AQL 8251 Mar. 6/7 '71 AQM 8252 Mar. 6/7 '71
AQN 8253 Mar. 6/7 '71
AQO 13274 May 5/6 '73 AQP 13559 June 2/3 '73
AQQ 13560 June 2/3 '73
AQR 13561 June 2/3 '73 AQS 20690 June 13 '77
AQT 13562 June 2/3 '73
AQU 13563 June 2/3 '73 AQV 20742 June 16 '77
AQW 7251 Aug. 28 '70
AQX 20728 June 14 '77 AQY 18377 May 15/16 '75
AQZ 20747 June 18 '77
ARA 9800 Oct. 21/22 '71 ARB 9799 June 13 '77
ARC 13574 June 2/3 '73
ARD 13553 June 1/2 '73 ARE 20705 June 13 '77
ARF 13573 June 2/3 '73
ARG 13607 June 3/4 '73 ARH 20707 June 13 '77
ARI 10891 April 9/10 '72
ARJ 18242 May 5/6 '75 ARK 18243 May 5/6 '75
ARL 20694 June 13 '77
ARM 11038 April 22/23 '72 ARN 16715 Aug. 16/17 '74
ARO 20741 June 16 '77
ARP 7250 Aug. 28 '70 ARQ 9801 Oct. 21/22 '71
ARR 13608 June 3/4 '73
ARS 19958 Aug. 27/28 '76 ART 9731 Oct. 15/16 '71
ARU 9732 Oct. 15/16 '71
ARV 18200 May 4/5 '75 ARW 6148 Mar. 13/14 '70
ARX 20862 Aug. 15 '77
ARY 4623 June 17/18 '69 ARZ 7249 Aug. 28 '70
ASA 8155 Feb. 28/Mar. 1 '71
ASB 13550 June 1/2 '73 ASC 7244 Aug. 24 '70
ASE 9789 Oct. 20/21 '71
3AJH 10688 Mar. 19/20 '72 3ALB 10687 Mar. 19/20 '72
3ALG 10691 Mar. 19/20 '72
3ALI 10694 Mar. 19/20 '72 3ANF 10890 April 9/10 '72
3AOD 10869 April 8/9 '72
4ZS 17157 Dec. 4/5 '74 4ZT 17158 Dec. 4/5 '74
4ZU 17159 Dec. 4/5 '74
4ZV 17161 Dec. 4/5 '74 4ZX 17162 Dec. 4/5 '74
4ZZ 17163 Dec. 4/5 '74
4AAB 12310 Jan. 3/4 '73 4AAD 12312 Jan. 3/4 '73
4ABG 15536 Jan. 23/24 '74
4ABH 13167 April 26/27 '73 4ABR 13174 April 27/28 '73
4ABX 13177 April 27/28 '73
4ABY 13171 April 26/27 '73 4ACS 15741 Feb. 15/16 '74
4ACU 15844 Feb. 22/23 '74
4ADL 13168 April 26/27 '73 4AFX 16653 Aug. 14/15 '74
4AGE 16783 Aug. 17/18 '74
4AGF 17192 Dec. 5/6 '74 4AGH 17188 Dec. 5/6 '74
4AGL 12306 Jan. 3/4 '73
4AGP 13966 Oct. 3/4 '73 4AGS 12308 Jan. 3/4 '73
4AGT 17191 Dec. 5/6 '74
4AGU 17165 Dec. 4/5 '74 4AGW 16787 Aug. 17/18 '74
4AGY 16755 Aug. 16/17 '74
4AHA 13962 Oct. 3/4 '73 4AHC 16781 Aug. 17/18 '74
4AHD 16782 Aug. 17/18 '74
4AHE 16788 Aug. 17/18 '74 4AHF 16791 Aug. 17/18 '74
4AHG 16847 Aug. 25/26 '74
4AHH 15537 Jan. 23/24 '74 4AHI 17195 Dec. 5/6 '74
4AHJ 17179 Dec. 5/6 '74
4AHK 16794 Aug. 17/18 '74 4AHL 16797 Aug. 17/18 '74
4AHM 13975 Oct. 4/5 '73
4AHN 13976 Oct. 4/5 '73 4AHP 13977 Oct. 4/5 '73
4AHQ 17169 Dec. 5/6 '74
4AHR 15721 Feb. 15/16 '74 4AHS 13987 Oct. 6/7 '73
4AHT 17193 Dec. 5/6 '74
4AHU 13988 Oct. 6/7 '73 4AHV 13989 Oct. 6/7 '73
4AHW 16849 Aug. 25/26 '74
4AHX 13991 Oct. 6/7 '73 4AHY 17194 Dec. 5/6 '74
4AHZ 17172 Dec. 5/6 '74
4AIA 17171 Dec. 5/6 '74 4AIB 17183 Dec. 5/6 '74
4AIC 16848 Aug. 25/26 '74
4AID 15604 Feb. 1/2 '74 4AIE 12303 Jan. 3/4 '73
4AIF 17173 Dec. 5/6 '74
4AIG 17174 Dec. 5/6 '74 4AIH 17182 Dec. 5/6 '74
4AII 15705 Feb. 14/15 '74
4AIJ 15719 Feb. 15/16 '74 4AIK 17234 Dec. 8/9 '74
4AIL 15846 Feb. 23/24 '77
4AIM 15704 Feb. 14/15 '74 4AIN 15515 Jan. 21/22 '74
4AIO 13360 May 21/22 '73
4AIP 13361 May 21/22 '73 4AIQ 15852 Feb. 23/24 '74
4AIR 15853 Feb. 23/24 '74
4AIS 15711 Feb. 14/15 '74 4AIU 15851 Feb. 23/24 '74
4AIV 15849 Feb. 23/24 '74
4AIW 16850 Aug. 25/26 '74 4AIX 16851 Aug. 25/26 '74
4AIZ 17220 Dec. 8/9 '74
4AJA 13264 May 5/6 '73 4AJB 17225 Dec. 8/9 '74
4AJC 17226 Dec. 8/9 '74
4AJD 16853 Aug. 25/26 '74 4AJE 17227 Dec. 8/9 '74
4AJF 26559 Feb. 29/Mar. 1 '84
4AJG 15518 Jan. 21/22 '74 4AJI 17181 Dec. 5/6 '74
4AJJ 17285 Dec. 11/12 '74
4AJK 15519 Jan. 21/22 '74 4AJL 15775 Feb. 18/19 '74
4AJN 15720 Feb. 15/16 '74
4AJO 17235 Dec. 8/9 '74 4AJP 17236 Dec. 8/9 '74
4AJQ 17237 Dec. 8/9 '74
4AJR 17240 Dec. 8/9 '74 4AJS 17238 Dec. 8/9 '74
4AJT 13362 May 21/22 '73
4AJU 17239 Dec. 8/9 '74 4AJV 17241 Dec. 8/9 '74
4AJW 15516 Jan. 21/22 '74
4AJX 15517 Jan. 21/22 '74 4AJY 13211 May 2/3 '73
4AJZ 13212 May 2/3 '73
4AKA 15848 Feb. 23/24 '74 4AKB 17233 Dec. 8/9 '74
4AKC 17231 Dec. 8/9 '74
4AKD 15847 Feb. 23/24 '74 4AKE 17230 Dec. 8/9 '74
4AKF 17232 Dec. 8/9 '74
4AKG 13263 May 5/6 '73 4AKH 17170 Dec. 5/6 '74
4AKI 17228 Dec. 8/9 '74
4AKJ 13210 May 2/3 '73 4AKK 15708 Feb. 14/15 '74
4AKL 15706 Feb. 14/15 '74
4AKM 15714 Feb. 14/15 '74 4AKN 15710 Feb. 14/15 '74
4AKO 15709 Feb. 14/15 '74
4AKP 15707 Feb. 14/15 '74 4AKQ 10689 Mar. 19/20 '72
4AKR 26560 Feb. 29/Mar. 1 '74
4AKT 13399 May 24/25 '73 4AKU 10690 Mar. 19/20 '72
4AKV 17186 Dec. 5/6 '74
4AKW 13262 May 5/6 '73 4AKX 17229 Dec. 8/9 '74
4AKY 13265 May 5/6 '73
4AKZ 16713 Aug. 16/17 '74 4ALA 13266 May 5/6 '73
4ALB 15540 Jan. 23/24 '74
4ALC 15713 Feb. 14/15 '74 4ALD 13213 May 2/3 '73
4ALE 13214 May 2/3 '73
4ALF 13215 May 2/3 '73 4ALJ 13455 May 27/28 '73
4ALK 13456 May 27/28 '73
4ALL 13216 May 2/3 '73 4ALN 20776 June 21 '77
4ALO 18326 May 11/12 '75
4ALP 15808 Feb. 20/21 '74 4ALQ 15809 Feb. 20/21 '74
4ALS 15785 Feb. 18/19 '74
4ALT 21778 June 7/8 '78 4ALU 15810 Feb. 20/21 '74
4ALW 16772 Aug. 17/18 '74
4ALY 13270 May 5/6 '73 4ALZ 13458 May 27/28 '73
4AMA 13271 May 5/6 '73
4AMC 13273 May 5/6 '73 4AMF 20717 June 14 '77
4AMG 16774 Aug. 17/18 '74
4AMH 20752 June 19 '77 4AMI 20703 June 13 '77
4AML 17216 Dec. 8/9 '74
4AMN 17214 Dec. 8/9 '74 4AMO 17213 Dec. 8/9 '74
4AMP 17217 Dec. 8/9 '74
4AMQ 17218 Dec. 8/9 '74 4AMS 17222 Dec. 8/9 '74
4AMU 17287 Dec. 11/12 '74
4AMV 17269 Dec. 11/12 '74 4AMW 17272 Dec. 11/12 '74
4AMX 13401 May 24/25 '73
4AMY 17290 Dec. 11/12 '74 4AMZ 15731 Feb. 15/16 '74
4ANB 17289 Dec. 11/12 '74
4ANC 17325 Dec. 13/14 '74 4AND 17374 Dec. 16/17 '74
4ANE 17271 Dec. 11/12 '74
4ANH 17372 Dec. 16/17 '74 4ANI 17288 Dec. 11/12 '74
4ANL 17368 Dec. 16/17 '74
4ANM 17369 Dec. 16/17 '74 4ANN 17370 Dec. 16/17 '74
4ANO 17371 Dec. 16/17 '74
4ANS 17277 Dec. 11/12 '74 4ANT 17276 Dec. 11/12 '74
4ANV 17273 Dec. 11/12 '74
4ANY 17375 Dec. 16/17 '74 4ANZ 20750 June 19 '77
4AOA 20751 June 19 '77
4AOB 13400 May 24/25 '73 4AOC 17327 Dec. 13/14 '74
4AOE 20714 June 14 '77
4AOG 16759 Aug. 17/18 '74 4AOL 16714 Aug. 16/17 '74
4AOP 18323 May 11/12 '75
4AOQ 16733 Aug. 16/17 '74 4AOS 20693 June 13 '77
4AOT 16768 Aug. 17/18 '74
4AOY 17263 Dec. 11/12 '74 4APB 16765 Aug. 17/18 '74
4APC 16766 Aug. 17/18 '74
4APD 20699 June 13 '77 4APF 18704 Aug. 31 '70
4APJ 16777 Aug. 17/18 '74
4APK 16778 Aug. 17/18 '74 4APN 16710 Aug. 16/17 '74
4APO 18174 Aug. 15/16 '74
4APS 16654 Aug. 14/15 '74 4APT 16655 Aug. 14/15 '74
4APU 20718 June 14 '77
4APV 20748 June 17 '77 4APY 18343 May 11/12 '75
4APZ 18344 May 11/12 '75
4AQA 20754 June 19 '77 4AQB 20755 June 19 '77
4AQD 18348 May 11/12 '75
4AQG 18710 Aug. 10/11 '75 4AQI 17262 Dec. 11/12 '74
4AQQ 20782 June 21 '77
4AQS 20691 June 13 '77 4AQT 20784 June 21 '77
4AQU 18229 May 4/5 '95
4AQW 18322 May 11/12 '75 4AQX 18376 May 15/16 '75
4AQY 20729 June 14 '77
4ARB 20032 Oct. 22/23 '76 4ARC 13554 June 1/2 '73
4ARD 20880 Aug. 17 '77
4ARM 20865 Aug. 17 '77 4ARN 18173 May 3/4 '75
4ARV 13269 May 5/6 '73
4ARW 13268 May 5/6 '73 4ASA 13267 May 5/6 '73
4ASB 20698 June 13 '77
4ASC 18335 May 11/12 '75 9ALV 4575 June 15/16 '69
9ALZ 4751 July 7/8 '69
9ARC 20726 June 14 '77