... Burenin,6 B. T. Jannuzi,7 M. Kim,2 M. G. Smith,8 R. C. Smith,8 H. Tananbaum,2 and B ... parameters such as m (the matter-density parameter) and 8 (the rms density ... of mass and redshift strongly depends on m and 8 (see Rosati et al. 2002 and ...
... 1 {T (y ) c (j ) 0 Tc ( yobs ) } 1+M , (1 8 ) recommended in Davison & Hinkley (1997 ... 2 2 ) 8 ^ Under the null hypothesis, Pr (pnaive = i M ) = 1 (M + 1), for i = 0, 1 ... M. (Technically, this requires the posterior variance of for any given y0 to ...
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Ссылки http://hea-www.harvard.edu/AstroStat/etc/SvDKS2015_ApJ813_66_LIRA_pval.pdf -- 964.8 Кб -- 30.10.2015 Похожие документы
... GCs in more distant galaxies, such as those in the Virgo and Fornax clusters can be individually detected and spectroscopically studied with 8-m class telescopes. ...
... This gives 1.8 в 1010 M for the whole disk, which is roughly consistent with the ... 1 0.5 - 2.8 в 1026 ergs s-1 M in 2 - 8 keV for the luminosity 32 34 range of 5 в 10 ...
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Ссылки http://hea-www.harvard.edu/ChaMPlane/papers/0902-draft-jaesub-xray_dist.pdf -- 750.9 Кб -- 09.03.2009 Похожие документы
... 1 M p c ( NGC 4 2 7 8 ) , a n d 1 1 . 8M p c ( NGC 4 6 9 7 ) are adopted. ... 1 M p c ( NGC 4 2 7 8 ) , a n d 1 1 . 8M p c ( NGC 4 6 9 7 ) are adopted. ... of a heavy (2-3 M ; Kalogera & Baym 1996) NS, or a 1.4M NS with a 8 It is also noted ...
... that dwarf A and F stars that lie in the d Scuti pulsational instability strip might have massloss rates between 10 9 and 10 8M, yr 1, but Brown et al. (1990) argued that Ver y Large Array measurements placed much lower limits on the ionized mass-loss ...
... 8.0M Statistical Computation At least 3N + 3 parameters for cluster with N stars Local modes based on choices of cluster ... 4 6 8 Sun 2 4 6 8 Sun 2 4 6 8 Sun True Initial Mass (M ) True Initial Mass (M ) True Initial Mass (M ) 95% Posterior Intervals ...
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Ссылки http://hea-www.harvard.edu/AstroStat/Stat310_1213/nms_20120904.pdf -- 1424.4 Кб -- 04.09.2012 Похожие документы