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Revised Shapley Ames.Pdf A REVISED SHAPLEY-AMES CATALOG OF BRIGHT GALAXIES The Las Canspanas ridge iii Chile during the last stages of construction of the dome for the du Pont 2.5-meter reflector. The du Pout instrument is at the north end of'thr long escarpment. The Swope 1-meter reflector is in the left foreground. Photu courtesy oi'R, J. Bruuito ; 1*<7*J-. A Revised Shapley-Ames Catalog of Bright Galaxies Containing Data on Magnitudes, Types, and Redshifts for Galaxies in the Original Harvard Survey, Updated to Summer 1980. Also Contains a Selection of Photographs Illustrating the Luminosity Classification and a List of Additional Galaxies that Satisfy the Magnitude Limit of the Original Catalog. Allan Sandage and G. A. Tammann CARNEGIE INSTITUTION OF WASHINGTON PUBLICATION 635 WASHINGTON, D.C. • 198 1 ISBN:0-87U79-<i52-:i Libran oi'CongrrssCatalog Card No. 80-6H146 (JompoMtion. Printing, and Binding by Mmden-Stinehour. Inr. ('<»p\ritiht C ]'M\, (Jariit'^it* Institution nf Washington ACKNOWLEDGMENTS We are indebted to Miss B. Flach and Mrs. R. C. Kraan- Korteweg for their help in compiling part of the data. We also owe special thanks to Basil Katem for his large effort in de- termining revised coordinates by measurement of National Geo- graphic-Palomar Sky Survey prints and Uppsala Schmidt plates for most of the listed galaxies, and to John Bedke for his skill in reproducing the photographs. We are especially grateful to R. J. Brucato for his important help in obtaining the most recent plates at Las Campanas. We greatly appreciate the help of several observers for provid- ing prepublication redshift data. These individuals are listed in the key to the redshift sources (References A at the rear of the volume); we owe special thanks to Drs. H. G. Corwin, J. R. Fisher and R. B. Tully, W. K. Huchtmeier, U. Mebold, V. C. Rubin, R. M. West, and H. van Woerden. One of us (G.A.T.) thanks with pleasure the Swiss National Science Foundation for partial support. Finally, it is a pleasure to thank Ray Bowers and Patricia Parratt of the Carnegie Institution editorial office for their me- ticulous work in transforming a tedious manuscript into a book, Freeman Keith for the book design, and Meriden-Stinehour, Inc. for their care in its production. A.S. G.A.T. Contents Parti. DESCRIPTION OF THE CATALOG Purpose of the Catalog 3 Completeness of the Catalog 4 Details of the Column Entries 4 Part II. THE CATALOG 13 Part III. BINNING ACCORDING TO TYPE 71 PartlV. SOME STATISTICAL PROPERTIES OF THE CATALOG 89 Part V. THE ILLUSTRATIONS 95 Part VI. APPENDICES A. Table of Additional Bright Galaxies 131 B. DDO Dwarf Galaxies with mpg < 13^4 142 C. Finding List for Galaxies with Non-NGC Numbers 143 D. Cross-Reference Finding List When Two Names are Used 144 Part VII. REFERENCES A. The Sources of the Redshifts 147 B. General References 156 PART I Description of the Catalog INCE THE TIME OF THE HERSCHELS, Surveys been supplemented by the first and second editions of S of bright galaxies have provided the foundations the Reference Catalog of Bright Galaxies (de Vaucouleurs upon which much of observational cosmology rests. A and de Vaucouleurs, 1964, for RC1\ de Vaucouleurs, de history of the major surveys extends from William and Vaucouleurs, and Corwin, 1977, for RC2). John Herschel in the first half of the 19th century, through Following Hubble's initial work, the Mount Wilson William Parsons, the third Earl of Rosse, to Isaac Rob- photographic survey was continued through the 1930's, erts, Dreyer (1888), Keeler (1900), Perrine (1904), principally by Hubble, Baade, and Humason, with a Hardcastle (1914), Fath (1914), Pease (1917), Curtis primary aim of obtaining large-scale plates of all galaxies (1918), Hubble (1922, 1926), and into modern times. listed in the SA north of 3 = ~ 15°. The purpose was to The publication of the New General Catalog by Dreyer in classify the galaxies for morphological studies, a process 1888 and its two Index Catalog supplements in 1895 and which, as is now known, leads directly to the central 1908 marks the beginning of reference works that are problem of galaxy formation and evolution. The survey, still in regular use. stopped between 1940 and 1945 during World War II, Photographic studies of the brighter Herschel galax- resumed in 1946, and was transferred to Palomar when ies using large telescopes began with Keeler's survey, the Hale 5-meter telescope (P200) was put into opera- employing the Lick 36-inch Crossley reflector, which tion in 1949. culminated in the historic Lick Observatory Publications 13, Beginning in 1974, the project was extended to the 1918, by Curtis. Photographic surveys at Mount Wilson south using plates taken at the Las Campanas Observa- were begun by Ritchey in 1909 and by Pease when the tory, Chile, first with the Swope 1-meter reflector (G40), long-focal-length 60-inch reflector (hereafter W60) was and after 1977 with the du Pont 2.5-meter reflector completed. In two remarkable summary articles by (C100). Results from the southern survey to 1979 are Pease (1917, 1920), a number of features of famous near- given elsewhere (Sandage and Brucato, 1979, 1981). by galaxies were illustrated for the first time. In parallel with Hubble's work to obtain large-scale The Mount Wilson photographic survey was contin- plates of the bright SA galaxies, Humason at Mount ued by Hubble in the early 1920's using the Wr60 and the Wilson and Mayall at Lick began a program in the newly completed Hooker 100-inch (W100) reflector, 1930's to measure redshifts in the northern sector of the which had been put into routine operation in 1919. The SA. By 1956, they had obtained redshifts for all SA completion of this early work led Hubble (1922, 1926) to galaxies brighter than OT* = 1 lr?7 north of S — —30°, the formulation of the system of galaxy morphology that and for many fainter galaxies. The Humason-Mayall is the foundation of the modern standard method of redshift catalog (Humason, Mayall, and Sandage, 1956) classification. Hubble's 1926 paper contains the classi- is 63% complete for all listed SA galaxies north of S — fication of 400 of the brightest NGC galaxies taken from -30°. the Hardcastle (1914) listing, which until 1932 was the Since 1956, a number of radio and optical observers most homogeneous catalog in existence, based, as it was, have combined efforts to complete the redshift coverage on the Franklin-Adams plates taken in the early years of for nearly the entire Shapley-Ames catalog in both hemi- the century and covering the entire sky. spheres. Redshift values now exist for all but six SA The Harvard survey of 1246 bright galaxies was pub- galaxies; and many of the earlier optical values have lished by Shapley and Ames in 1932. This catalog (here- been improved through 21-cm observations. after called the SA) has a fair degree of homogeneity n within its magnitude limit at nip ^ V$ ?2. Furthermore, PURPOSE OF THE CATALOG the uniform way in which Shapley and Ames compiled the data from both hemispheres using new plate mate- In the early 1950\s. when the first stage of the Mount rial, produced for the first time an approximation to a Wilson and Palomar photographic survey north of S ™ magnitude-limited sample. The SA became the bask: — 15° was nearlv complete, a plan was set out to compile listing of bright galaxies and has played a major role in existing data on types, magnitudes, and recishilts, and to studies of galaxies in the local region. It has only recently obtain tw\% data where needed for all galaxies in the A Revised Shapley-Ames Catalog Shapley-Ames catalog. From the beginning, it was our COMPLETENESS OF THE CATALOG intention to restrict the revision of the original SA list- ings and to obtain comparable data for both hemispheres. It is known that the SA is not complete to its stated To this end, we began observations for redshifts, mor- magnitude limit of m^ = 13^2 but becomes progressively phological types, and photoelectric magnitudes at the more incomplete as this magnitude level is approached. Mount Stromlo and Siding Springs Observatories, Aus- A study of the incompleteness (Sandage, Tammann, tralia, in 1969 at the invitation of the director, O. J. and Yahil, 1979) suggests that the fraction/(m) of a Eggen. complete sample in fact contained in the SA is well The observations were made by Sandage for redshifts represented by with the Mount Stromlo 1.9-meter reflector, for types /(m) = [^-12.72)/0.19+1]-i5 with the Uppsala Schmidt, and for photoelectric magni- where m is the magnitude in the BT system. tudes with the Siding Springs 1-meter reflector. Obser- In this representation, the progressive incompleteness vations of the northern SA galaxies still lacking redshift of the SA is a rapid function of m, as shown in figure 6 of values were begun at Palomar in 1970. The detailed the above-stated reference, where the equation is com- data have been published in the archival literature pared with counts of E and SO galaxies contained in (Sandage, 1975b, 1978). In the time since the 1969- fainter catalogs. Note that at m = \2m,f{m) = 1, while at 1970 Australian expedition, galaxy types based on the m =* 12™7,/(m) is only 0.5. Uppsala Schmidt plates have been upgraded, in many As an aid toward the eventual revision of the SA to a cases using large-scale reflector plates from the later Las more complete magnitude-limited catalog, we list in Campanas survey already mentioned.
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