... 0:908 Ч 0:793 logЅL П8ч=L П24ч; П 1ч which we adopt in the following as our baseline ... Lk ( FUV )=Lk ( NUV ) ј ю0:1688 26 ю 0:0177; П 2ч where Lk(FUV ) and Lk( NUV ) are ...
[
Текст
]
Ссылки http://www.stsci.edu/~mutchler/documents/ApJ_2005_SINGS_M51a.pdf -- 1188.7 Кб -- 07.11.2005 Похожие документы
... Since in reality, the slack in the intervals of directly related exposures is of the order of ten degrees, this can only happen when there is a long ( 36) o Жo o o o o ( o Еo o o п o , o , o o o o ). ...
... Mref ПMcl ; Mref ч ј Rю1 Mcl ю1 х(M ) dM х(M ) dM ; П 2ч where Mref is the absolute magnitude limit to which we measure all ... scenarios based on the expression f јf юf Nzј0:5 а NE Ч ; Nzј1 Nzј1 П 3ч S0; zј1 EЧS0; zј1 E; zј0:5 736 POSTMAN ET AL ...
... Instead, we use the synthetic photometry to find a direct relation for the color term as a function of the J ю H color: (K 0 ю K ) MKO ј ю0:100 Ч 0:143(J ю H ) MKO ; П 1ч No. ...
... Mi < ю19:5) to dwarf galaxies (ю19:5 Mi < ю18:0) using the expression GDR ј N (Mi < ю19:5) : N (ю19:5 Mi < ю18:0) П 1ч The demarcation between dwarf and giant at Mi ј ю19:5 is chosen to correspond approximately to the start of the deviation between the ...
... the deconvolved images within a circular aperture of radius equal to Re or 3 pixels, whichever is ю z850 ј c0 Ч slope (z 850 ю 23): П 1ч The solid line in Figure 7 is the fit to the CMR for the elliptical galaxies, the black dotted line is the fit to the ...