By P. Hodge (auth.)
This ebook summarizes the collection of knowledge on and the becoming knowing of M33 from the Nineteen Twenties, while Hubble first decided its precise nature, to the twenty first century, whilst the Hubble Telescope probed deeply into its many secrets and techniques. With its typical symmetrical spiral constitution, and its being now not tilted an excessive amount of and close to sufficient to permit distinctive experiences of its stars, M33 is well-suited for the research of a standard spiral galaxy.
In this paintings, Paul Hodge locations present study on M33 (and related galaxies) in either old and international views. The e-book is written in a language obtainable for experts and non-specialists, for pro and novice astronomers, for scientists and the curious public and, most significantly, for students.
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Extra resources for The Spiral Galaxy M33
1999) achieved resolution at wavelengths ranging from uv (1,491 Å) to the near-infrared (10,190 Å). P. V. 2012 49 50 5 The Nucleus Fig. 1 The B-ﬁlter proﬁle of the nucleus of M33 obtained at the Canada-France-Hawaii Telescope on Mauna Kea (From Kormendy and McClure 1993). Used by permission, copyright AAS Fig. 2 The luminosity proﬁle of the nucleus in the ultraviolet (dots), compared to the proﬁle of a nearby star (triangles) (From Dubus et al. 1999). 2 shows the proﬁle of the nucleus in the UV.
Subsequently Maucherat et al. (1984) re-examined the problem using isophotometry, HII region distributions, spiral arm patterns and HI data, concluding that there is no signiﬁcant warp of the plane and that the “classical” value of the inclination, i = 55°, is correct (Fig. 3). The reasons for the disagreements appear to be related to the methods used to derive them and the range of radii considered. The spiral structure considerably inﬂuences the measured ellipticities of isophotes and their inﬂuence is difﬁcult to separate from geometrical effects.
Used by permission, copyright AAS Although red-sensitive plates required much longer exposures at that time, Hubble was able to determine that the Cepheids had intermediate colors (like the sun’s) and this further conﬁrmed their identity as normal Cepheids. Having established that his stars were Cepheids, Hubble then plotted their maximum magnitudes against the logarithm of their periods and obtained a periodmagnitude relation similar to that of the Cepheids in the Small Magellanic Cloud. Using Harlow Shapley’s latest version of that (Shapley 1925) and using a simple process of superimposing the diagrams and ﬁtting them by eye, he concluded that the Cepheids in the two galaxies were similar and that the relative distances could be derived by the comparison.
The Spiral Galaxy M33 by P. Hodge (auth.)