By Livio M.
Number of evaluation articles on all facets of darkish topic and theories of gravity.
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Extra resources for Dark Universe: Matter, Energy and Gravity (2004)(en)(204s)
No. Dark Halo No. 5 4 >1 2 2 3 ? 0? † Oppenheimer et al. 2001a, Science Online, March 22 ‡ Monet et al. 2000, AJ 120, 1541 ¶ Ibata et al. 2000, ApJ 532, L41 Harris et al. 2001, ApJ 549, L109 †† de Jong et al. 2000 astro-ph/0009058 ‡‡ Stetson et al. in progress ¶¶ Ibata et al. 1999, ApJ 524, L95 Table 1. Predicted and observed numbers of faint white dwarfs cooled to very low luminosities by a Hubble Time and would be basically unobservable. The seventh column lists the number of old white dwarfs actually found out to the limiting distance only in each survey.
Of course, at the moment, it is also true that the surveys do not rule out such a dark matter halo either. 4. Temperature and age distribution of dark halo white dwarf candidates We can examine the totality of objects in the surveys of Table 1 from a diﬀerent perspective. If they are, in fact, local examples of the MACHOs, and thus important Galactic dark matter contributors, they should be quite old, likely as old as the globular clusters. This would place them in the 12–14 Gyr range if we take the current spread quoted for globular cluster ages.
2000 AJ 120, 1541. Oppenheimer, B. , Hambly, N. , Digby, A. , & Saumon, D. 2001a Science 292, 698. Oppenheimer, B. , Hodgkin, S. , Jameson, R. , Hambly, N. , Filippenko, A. , Coil, A. , & Brown, M. E. 2001b ApJ 550, 448. Reid, I. , Sahu, K. , & Hawley, S. L. 2001 ApJ, 559, 942; astro-ph/0104110. Richer, H. , et al. 2002, in preparation. Richer, H. , Fahlman, G. , Ibata, R. , Bell, R. , Bond, H. , Harris, W. , Hesser, J. , Stetson, P. , & Wood, M. A. 1997 ApJ 484, 741. Richer, H. , Fahlman, G. , Ibata, R.