By Penrose R.

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Surprisingly it appears that this spiral-like feature is being viewed almost poleon. , the presence of a few dust patches need not imply the presence of a large mass of gas inside the nuclear bulge). Observations of the integrated light of the bulge of M31 (Morgan 1959, McClure & van den Bergh 1968) demonstrate that the dominant contribution to its light is produced by very metal-rich (µ Leonis-like) giant stars. 5 (M I = −5) and that (2) the population in the inner bulge at r < 40 does not differ substantially from that in an outer bulge field located ∼120 south of the nucleus.

At a given metallicity the G-band appeared to be weaker in P1: MRM CB240-03 November 20, 1999 34 12:55 Char Count= 0 The Andromeda galaxy (M31) the M31 spectra, while the H - and K -lines seemed to be slightly too strong in the spectra of the globulars associated with the Andromeda galaxy. Subsequently Burstein et al. (1984) found that CN is enhanced significantly in several M31 globulars with respect to the Milky Way. Moreover, these authors found that M31 globulars also have significantly stronger Balmer lines than Galactic globulars.

66 are open clusters. 94, is vdB0. 3 Spectroscopy of globular clusters The first spectroscopic observations of the globular clusters associated with the Andromeda galaxy (van den Bergh 1969) showed that these objects had approximately the same range in metallicities as their Galactic counterparts. 13. In that paper it was shown that the metallicity distribution of M31 clusters is skewed toward higher metallicities. This conclusion has been confirmed by more recent studies of the metallicities of globular clusters in M31 (Huchra, Brodie & Kent 1991) and in the Galaxy (Zinn 1985).

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A lecture on 5-fold symmetry and tilings of the plane by Penrose R.

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New PDF release: A lecture on 5-fold symmetry and tilings of the plane
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