By Strömberg G.
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Additional resources for A Determination of the Solar Motion and the Stream Motion Based on Radial Velocities and Absolute Ma
0. Auri`ere et al. also note that all of the newly discovered clusters have very small radii. Clearly it would be very useful to use the Hubble Space Telescope to place limits on the number of small faint globular clusters that could have been overlooked near the nucleus of M31. 5, the fact that the true nucleus (P2 ) of M31 exhibits a far-ultraviolet excess (King, Stanford & Crane 1995) suggests that some globular clusters containing blue horizontal branch stars might, indeed, have been sucked into the nucleus of M31 by tidal friction.
Moreover, these authors found that M31 globulars also have signiﬁcantly stronger Balmer lines than Galactic globulars. Van den Bergh’s tentative conclusion that the Ca II H - and K -lines in M31 are enhanced, relative to Galactic globulars of similar [Fe/H], was subsequently conﬁrmed by measurements of line-strength indices by Brodie & Huchra (1990, 1991). These authors also found the CN λ 4170 feature to be enhanced in the spectra of M31 globular clusters. Ponder et al. (1998) have used the Hubble Space Telescope to obtain spectra of the M31 globular clusters M II, M IV, K 58, and K 280.
In his paper Hubble appears so eager to establish the similarity between novae in M31, the LMC, and the Galaxy that he ignores the fact that objects such as nova Aquilae 1918, with M(max) = −9, appeared to be signiﬁcantly more luminous than any of the novae in the Andromeda galaxy. This, together with his (Hubble 1932) observation that Galactic globular clusters appeared to be less luminous than their counterparts in M31, should have alerted Hubble to the fact that there was a serious problem with the extragalactic distance scale.