Abstract
We designate as star clusters those groupings of stars in which the members are known to be gravitationally associated or may be assumed from their apparent positions relative to each other to constitute distinct physical organizations. Such a category includes both the typical globular systems and the more numerous and less well defined open clusters which range, for instance, from the Hyades to the fairly compact system of Messier 11.
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References
Obs 48, p. 173 (1925).
Publ Obs Astr Univ Tartu (Dorpat) 26, No. 2 (1924).
Harv Circ 281 (1925).
Galileo, Sidereus Nuncius, 1610; Allen, Star Names and their Meanings, p. 113 (1899); see Shapley and Howarth, A Source Book in Astronomy, p. 49 (1929).
R. Wolf, Geschichte der Astronomie, p. 420 (1877).
Hist, de l’Acad. R. des Sci., Paris 1771, p. 423.
Phil Trans 154, p. 1 (1864). 5 A very full bibliography of the work done on clusters is to be found in Appendix C of Star Clusters, Harv Obs Monograph No. 2 (1930).
The term galactic cluster, suggested by Trumpler [Publ A S P 37, p. 307 (1925)] and others, is a natural name for the non-globular cluster, which is almost without exception near the galactic plane. It replaces the term “open cluster” which has caused some confusion because of the open type of globular cluster.
Harv Ann 76, No. 4 (1915).
A special study now in progress at Harvard, of the environs of the Large Magellanic Cloud adds several new globular clusters to the list; some of them may not be outlying members of the Cloud, and two or three are not N.G.C. or I.C. objects. In A N 246, p.171 (1932) Lampland and Tombaugh report that N.G.C. 5694 is a typical globular cluster.
Sawyer and Shapley, Harv Bull 848 (1927).
The approximate positions for 1900 in equatorial coordinates are conveniently contracted for tabulation into the form here given; the first four figures give the hours and minutes of right ascension, and the sign and subsequent figures indicate the declination in degrees (and may be extended to minutes, if desired).
Bailey, Harv Ann 76, p. 43 (1915); Hinks, M N 71, p. 693 (1911); Bohlin, Svenska Vet Akad Handl 43, No. 10 (1909); Clerke, Problems in Astrophysics (London) p. 428 (1903).
Mem R A S 61, p. 75 (1915).
See Footnote 3 on page 700.
Publ A S P 37, p. 307 (1925). A more recent study of galactic clusters is presented by Trumpler in Lick Bull 14, p. 154 (1930), where he gives a more complex, three-dimensional classification. The investigation also includes statistical material on distances, magnitudes, dimensions, and spectra.
Lick Bull 5, p. 74 (1908); Mt Wilson Contr 49 (1911).
Pop Astr 25, p. 36 (1917); 26, p. 8 (1918).
Harv Bull 868 (1929).
Shapley, Mt Wilson Comm 44 (1917).
Shapley, Mt Wilson Contr 116 (1917); see also Pease, Mt Wilson Ann Rep 9, p. 219 (1913); 10, p. 268 (1914); Sanford, Mt Wilson Ann Rep 14, p. 212 (1918); Pop Astr 27, p. 99 (1919).
Harv Obs Mon 2 (1930); Harv Bull 874 (1930). Ten Bruggencate has plotted the coordinates (my magnitudes and colors) for the individual stars used in making the color-magnitude summaries for Messier 13 and Messier 3. (Die Sternhaufen, Berlin, 1927). I think there is little gain and some danger in detailed subdividing of the observational material. Experience with the photometric measures in globular clusters leads to a belief that the group values presented in my color-magnitude arrays go as far as is justifiable in subdivision.
Seares, Mt Wilson Comm 16 (1915).
See Harv Bull 873 (1930).
Mt Wilson Contr 155, p. 8 (1918).
Internal Constitution of the Stars, Chapter VII (1926).
Babelsberg Veröff 5, p. 16 (1924).
Svenska Vet Akad Handl 61, No. 15, p. 126 (1921).
See bibliography in Harv Mon No. 2 (1930).
E. C. Pickering, Harv Ann 26 (1897); see also Table 6.
Publ A S P 37, p. 307 (1925). See note 1, p. 705, on his later work.
Doig, J B A A 35, p. 201 (1925); Raab, Lund Medd, Série II, No. 28 (1922).
Hertzsprung, M N 89, p. 660 (1929). See also Harv Bull 764 (1922).
M N 89, p. 660 (1929).
Publ A S P 38, p. 350 (1926).
The magnitudes determined for this cluster are apparently in error, probably by a constant amount, notwithstanding the consistency of the Mount Wilson photometric plates [Mt Wilson Contr 126 (1917)]. The color indices are systematically too great, as shown by my own spectrum plates (unpublished), and subsequently by the similar work of Lindblad and Trumpler. A correction of — 0,4 to the photographic magnitudes is indicated by an unpublished Harvard plate, but even then the colors and spectra are inconsistent. There is a probability of differential light absorption within the cluster.
Lick Bull 12, p. 10 (1924).
A N 236, p. 327 (1929).
See Table 6 above.
Previous to 1930.
Ludendorff, volume VI, chapter 2.
Harv Circ 173 (1912).
But see Guthnick and Prager, Sitzber Preuss Akad Wiss 1925, p. 508.
M N 50, p. 517 (1890); 51 p. 226 (1891).
A N 123, p. 207 (1889); Harv Circ 2 (1895).
Sid Mess 6, p. 381 (1890); 10, 170 (1890); Engl Mech 51, p. 378 (1890).
A N 147, p. 243 (1898).
Shapley, Mt Wilson Contr 116, p. 79 (1915).
Eberhard, Z f Phys 13, p. 288 (1912); Publ Astrophys Obs Potsdam No. 84, p. 1 (1926).
Bailey, Harv Ann 38, p. 2 (1902).
Bailey, Harv Bull 783 (1923).
Mt Wilson Observatory, unpublished.
Bailey, Harv Bull 802 (1924).
Miss Swope, unpublished.
Miss Woods, Harv Circ 216 (1919).
Bailey, Harv Circ p. 234 (1922).
Miss Davis, Publ A S P 29, p. 260 (1917).
Shapley, Mt Wilson Contr 175 (1920).
Shapley, Publ A S P 31, p. 226 (1919).
Baade, Hamburg Mitt 5, No. 16 (1922).
Baade, Hamburg Mitt 6, No. 27 (1928).
Baade, Hamburg Mitt 6, No. 29 (1928).
Innes, Union Circ 59, 201 (1923).
Shapley, Mt Wilson Contr 91 (1914).
Shapley, Mt Wilson Contr 176 (1920).
Guthnick and Prager, Sitzber Preuss Akad Wiss 1925, p. 508.
Larink, Bergedorf Abhandlungen 2, No. 6 (1921).
Barnard, A N 172, p. 345 (1906).
Bailey, Harv Bull 801 (1924).
Bailey, Harv Ann 78 (1917).
Miss Leavitt, Harv Circ 90 (1904).
R A J 1, p. 16 (1924).
Shapley, Mt Wilson Contr 116 (1917).
Shapley, Mt Wilson Contr 190 (1920).
Miss Woods, Harv Bull 773 (1922).
Miss Woods, Harv Circ 217 (1919).
Miss Woods, unpublished.
Hubble, letter.
Miss Woods, Harv Bull 764 (1922)
see also A N 215, p. 391 (1922).
Harv Bull 848 (1927).
Zô-Sé Annals 10 (1918).
Bailey, Pop Astr 28, p. 518 (1920).
Bailey, Harv Circ 266 (1924).
Miss Davis, Publ A S P 29, p. 210 (1917).
Mt Wilson Contr 195 (1920).
Wash Nat Ac Proc 7, p. 152 (1921).
Chèvremont, B S A F 12, pp. 16, 90 (1898).
Bailey, Harv Bull 798 (1924).
Baade, letter of June 8, 1932.
Grosse, A N 246, p. 27 (1932).
Baade, A N 230, p. 353 (1930).
See references in Harv Mon No. 2 (1930). See also the later papers by Heckmann and Siedentopf, Z f Phys 54, p. 183 (1929) and Z f Astrophys 1, p. 67 (1930).
Hertzsprung, A N 207, p. 89 (1918);\
Nabakov, R A J 1, p. 109 (1924); Hogg, Harv Bull 870 (1929)
Schilt, A J 38, p. 109 (1928); Pop Astr 36, p. 296 (1928). See also Hogg’s recent discussion of the luminosity distribution in six globular clusters. A J 42, p. 77 (1932).
Mt Wilson Contr 155 (1917); 175 (1919).
Hamburg Mitt 6, No. 29 (1928).
Harv Ann 76, No. 4 (1915).
Pease and Shapley, Mt Wilson Contr 129 (1917).
H. Shapley and Martha B. Shapley, Mt Wilson Contr 160 (1918).
Shapley and Sawyer, Harv Bull 852 (1928).
Shapley, Mt Wilson Comm 45 (1917).
That is, position angles without a colon in Harv Bull 852 (1927).
H. Shapley and Martha B. Shapley, Mt Wilson Contr 160 (1918).
Freundlich and Heiskanen, Z f Phys 14, p. 226 (1923).
See discussion by ten Bruggencate, Die Sternhaufen p. 72 (1927).
Pease and Shapley, Mt Wilson Contr 129 (1917).
Shapley and Davis, Publ A S P 30, p. 164 (1918).
Mt Wilson Contr 160, p. 7 (1918); Harv Bull 852, p. 25 (1927).
Shapley and Duncan, Pop Astr 27, p. 100 (1919).
Mt Wilson Comm 45 (1917).
Harv Mon 2, sec. 33 (1930); see also Collinder, Lund Circ No. 2 (1931).
Allegheny Publ 6, No. 4 (1922).
Mt Wilson Contr 190, p. 7 (1920).
See references in Appendix D of Harv Mon No. 2 (1930).
Mt.Wilson Contr 83 (1914).
See references in bibliography of Harv Mon No. 2 (1930).
Harv Circ 299 (1927).
Mt Wilson Contr 116 (1915).
See ciph. 12.
Shapley, Mt Wilson Comm 44 (1917).
Seares and Hubble, Mt Wilson Contr 187 (1920).
Shapley, Mt Wilson Contr 165, p. 5 (1918); see also Shapley and Mayberry, Mt Wilson Comm 74 (1921).
Ap J 50, p. 386 (1919). Through an error the value is printed ten times too small.
Shapley and Ames, Harv Circ 294 (1926).
Harv Ann 73, Part 2 (1917); Harv Bull 763 (1922); Harv Repr 5 (1923); Wash Nat Ac Proc 9, p. 386 (1923); see also ciph. 16 above.
Hemel en Dampkring, 22, p. 153 (1924).
Ludendorff, Volume VI, 2, chapter 2.
Shapley, Wash Nat Ac Proc 8, p. 69 (1922).
B A N 1, p. 37 (1922).
Harv Circ 237 (1922); R. E. Wilson, A J 35, p. 35 (1923).
A J 35, p. 35 (1923).
B A N 4, p. 91 (1927).
Schlesinger, Catalogue of Parallaxes, Yale Univ. Obs. 1924; Shapley, Harv Circ 237 (1922); Lindblad, Ap J 59, p. 37 (1924).
Publ A S P 32, p. 62 (1921).
See various papers by ten Bruggencate, Curtis, Doig, Kienle, Malmquist, and Strömberg. Since this chapter was written in 1930 there have been further discussions of the zero point by Gerasimovič [A J 41, p. 17 (1931)], Nordström [Lund Obs Circ 2 (1931)], and others.
From Harv Bull 869 (1929).
Harv Bull 869 (1929).
The long period variables in 47 Tucanae (Harv Bull 783) could not be safely used in. measuring the distance.
The mean magnitude of the 25 brightest stars was determined at Mount Wilson to be 14,81, with a range of 14,38 to 15,04.
The magnitudes, of N.G.C. 3201 and N.G.C. 6541 may be considerably in error due to unsatisfactory comparison sequences. They are not included in the determination of the reduction curves for apparent integrated magnitudes and diameters, though they are appropriately used in constructing Table 22.
For N.G.C. 6121 the zero point of the magnitude scale depends, on both Harvard and Mount Wilson measures of Mount Wilson plates.
The mean magnitude of the 25 brightest stars was determined at Harvard to be 13,76 with a range of 13,4 to 14,1.
Baade has recently studied this difficult system [A N 239, p. 353 (1930)] and his better results give a modulus 16m,52 ± 0m,05. He correctly reassigns the cluster to a much earlier class (on the basis of new long exposure plates).
Harv Bull 852 (1927).
Harv Circ 234 (1922).
Harv Bull 848 (1927).
Lyon Bull 11, p. 59 (1929).
Mt Wilson Contr 152 (1918).
Pickering, Harv Ann 56, p. 1 (1912).
J B A A 35, p. 201 (1925).
Lund Medd Série II, No. 28 (1922).
Mt Wilson Comm. 62 (1919).
Preliminary publication in Lick Bull 14, p. 154 (1930), after the completion of this manuscript.
Publ A S P 37, p. 307 (1925).
Lund Obs Ann 2 (1931).
Harv Circ p. 348 (1929). Miss Anger has extended the method and applied it to various galactic clusters. [Harv Circ 352 (1930); Harv Bull 882 and 883 (1931)].
Mt Wilson Contr 284 (1925).
Mt Wilson Contr 338 (1927).
See, for example, Pop Astr 27, p. 101 (1919).
See Figure 15.
Later revised to 1340 parsecs. Lick Bull 14, p. 154 (1930).
Lick Bull 12, p. 10 (1925).
Harv Circ 275, 276 (1925).
Harv Bull 775 (1922); Harv Circ 271 (1925).
It was included in Harv Bull 848, 849, and 852 as a doubtful object.
In 1932 (two years after the completion of the manuscript) a dozen new globular clusters were found in the vicinity of the Large Cloud (Harv Bull 889).
Harv Bull 868 (1929).
Shapley, Yamamoto, and Wilson, Harv Circ 280 (1925); see also Shapley, Harv Circ 255 (1924).
See ciph. 30.
Shapley, Harv Circ 268 (1924).
Leavitt, Harv Ann 60, No. 4 (1908). Approximately 600 new variables have been found on Harvard plates of the Large Cloud since 1930 (as yet unpublished).
Harv Repr 61 (1929).
Shapley, Harv Repr 61 (1929).
Harv Bull 776 (1922).
Shapley, Harv Repr 51 (1928).
Nort, Recherches Ast Obs Utrecht 8, p. 113 (1917); Seares, Mt Wilson Contr 347 (1927).
Shapley, Harv Repr 52 (1928).
Shapley and Mayberry, Mt Wilson Comm 74 (1921).
Mt Wilson Contr 157, Sect. 7 (1918).
Harv Circ 350 (1930).
Harv Circ 350 (1930).
See Addendum on p. 773.
Cf. footnote on N.G.C. 4147 on page 741.
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Shapley, H. (1933). Stellar Clusters. In: Curtis, H.D., Lindblad, B., Lundmark, K., Shapley, H. (eds) Das Sternsystem. Handbuch der Astrophysik, vol 5/2. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-90704-3_2
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