By P. Hodge (auth.)
ISBN-10: 9400720246
ISBN-13: 9789400720244
This booklet summarizes the collection of data on and the starting to be figuring out of M33 from the Twenties, while Hubble first decided its actual nature, to the twenty first century, while the Hubble Telescope probed deeply into its many secrets and techniques. With its average symmetrical spiral constitution, and its being no longer tilted an excessive amount of and close to adequate to permit special reports of its stars, M33 is well-suited for the research of a customary spiral galaxy.
In this paintings, Paul Hodge locations present examine on M33 (and comparable galaxies) in either old and worldwide views. The ebook 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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Example text
8 The spiral structure as deduced from the OB associations identified by Humphreys and Sandage (1980). Used by permission, copyright AAS 36 4 Structure To eke out the important physical characteristics of M33’s optical structure, Elmegreen et al. (2003) analyzed azimuthal scans of an image obtained with the wide-field camera of the CFHT, obtained by Cuillandre, Lequeuex and Loinard (1999). They then obtained Fourier transform power spectra and fitted them to fractal models of stars and continuum. 7, shallower than expected for a turbulent origin for the structure.
6. Radial velocities showed a large difference between the center and outer parts of M33 and, if interpreted as rotation, implied a very large mass. 7. The color-magnitude diagram of the brightest stars, if the Cepheid distance is assumed, was similar to what was known about the Milky Way’s brightest stars (actually, Hubble was learning more about M33’s brightest stars than was known then about our system’s most luminous stars). : Pub. Dom. Ap. Obs. : Proc. Nat. Acad. Sci. : Harvard Circular, No.
IRAS infrared data at 12 Pm was used by Deul (1989) and Bothun (1992) 32 4 Structure 80 M33 Mbol < 5 Nss Per arcminss2 60 40 20 0 0 2 4 6 8 R(arcmin) 10 12 14 Fig. 5 H-band distribution of K and M giants in the M33 bulge (Minniti et al. 1993). The dashed line is the disk profile from Kent (1987). 2 kpc. 15, but the shape of the profile was not fit well by a r1/4 law. An infrared image of the possible bulge was obtained by Minniti et al. (1993), who obtained an H-band mosaic of M33 which showed a bulge of red stars, identified as K and M giants, located in the inner 2 arcmin of the disk (Fig.
The Spiral Galaxy M33 by P. Hodge (auth.)
by Paul
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