By P. Hodge (auth.)
This e-book summarizes the collection of data on and the starting to be realizing of M33 from the Twenties, while Hubble first made up our minds its actual nature, to the twenty first century, while the Hubble Telescope probed deeply into its many secrets and techniques. With its usual symmetrical spiral constitution, and its being no longer tilted an excessive amount of and close to sufficient to permit distinctive reviews of its stars, M33 is well-suited for the research of a regular spiral galaxy.
In this paintings, Paul Hodge locations present learn on M33 (and related galaxies) in either historic and international views. The e-book is written in a language obtainable for experts and non-specialists, for pro and beginner astronomers, for scientists and the curious public and, most significantly, for students.
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Additional resources for The Spiral Galaxy M33
Ann. Obs. Lund. : Lund Medd. Astro. Obs. Ser. II. : Realm of the Nebulae. Yale U Press, New Haven (1936) Huchtmeier, W. : Structure and properties of nearby Galaxies. In: Proceedings of the Symposium, Bad Muenstereifel, West Germany, 22–26 August 1977 (A79-13481 03–90), pp. 197. Dordrecht, D. : Harvard Obs. Bull. 914, 9 (1940) Pritchet, C. : RR Lyrae Stars in Nearby Galaxies. In: Proceedings of the ASP 100th Anniversary Symposium, Victoria, Canada, June 29–July 1 1988 (A90-14129 03–90), pp. 59–67.
S (1984) plot of the distribution with radius, r, of associations and HI peaks (points) compared to a logarithmic spiral (line). 6 The Inner Disk and Bulge 31 Fig. 4 The major axis luminosity proﬁle of M33 in B (Kent 1987). 5 Optical Luminosity and Color Proﬁles At optical wavelengths the most conspicuous feature of M33 is an exponential stellar disk. Following early photographic studies by Patterson, Shapley, Holmberg and others (loc. 9 kpc. 3 kpc (Fig. 4). The diameter of the disk in the optical is a matter of debate.
Variable 2 became so bright in 1924 that it was the brightest star that Hubble felt could be assigned to M33. He obtained a spectrum of it with the 100-in. and characterized it as having a blue continuum with superimposed emission lines of hydrogen. The nature of these stars was barely discussed by Hubble, who limited himself to stating that “variation of this type is not sufﬁciently known among galactic stars for analogies to be traced”. [Analogies were traced later, however, by Hubble, working with his young disciple, Allan Sandage, who gathered data on these stars in a variety of galaxies and discussed their properties in terms of possibly using them as distance indicators.