Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.iki.rssi.ru/galeev/astro2007/2012_Komberg.pdf Дата изменения: Tue Aug 28 17:45:37 2012 Дата индексирования: Tue Oct 2 14:16:12 2012 Кодировка: Поисковые слова: moon

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I.


Fig. 2.-- Hubble's (1936) "tuning fork" of galaxy morphologies is the basis for modern galaxy classification. (arXiv:1102.0550.v1)




Fig. 4.-- Examples of elliptical galaxies of different projected shapes. Type E galaxies are normal ellipticals with no structural details. Type E+ galaxies are "late" ellipticals, which may include faint extended envelopes typical of large cluster ellipticals, or simple transition types to S0-. (arXiv:1102.0550.v1)




Fig. 7-- Examples of barred and nonbarred S0 galaxies of different stages from "early" (S0-), to "intermediate" (S0o ), to "late" (S0+), including the transition stage to spirals,




Fig. 8.-- Stage classifications for spirals, divided according to bar classifications into parallel sequences(arXiv:1102.0550.v1)


Fig. 26.-- Examples of pseudobulges and classical bulges in spiral galaxies. (arXiv:1102.0550.v1)




Fig. 48.-- The Hubble tuning fork of ellipticals, using SDSS color images (arXiv:1102.0550.v1) .


(arXiv:1008.3386) , z>1 : , , . , EG, -- Irr. , EG , . EG. .


Fig. 2.-- Massive (M > 10^10M) galaxies orbiting within the group at z = 0.19 (arXiv:1008.3386v2).


, ( n < 2 B/T<0.2). , (MBH = 10^6M - 10^8M). .


arXiv:1107.4238v1


arXiv:1107.4238v1


z. z=0 z=0.8 (arXiv:1010.4442), : 1) EG ~40% z. 2) SG ~40% 15% . 3) S0 13% 40% . , z~0.4 S S0 .




(arXiv:1112.3990v1) 1000 S,S0 E (MB<-19) SDSS . 1) EG M*, Mhalo. EG M* Mhalo. EG M*, Mhalo EG. EG . 2) S0 M* Mhalo. S0 Mhalo<10^13M 70% .


Fig. 4.| Fractions of elliptical (red circles), lenticular (green triangles), and spiral (blue stars) galaxies as a function of B- and luminosity, with selection weights applied. Binomialerrors are computed using the Wilson (1927) method. (arXiv:1112.3990v1)


Fig. 5.| Fractions of each morphological type (elliptical, lenticular (S0), and spiral) for MB < -19 galaxies as a function of stellar mass, weighted using selection and V=Vmax weights. (arXiv: 1112.3990v1)


Fig. 6.Morphological group velocity disper (right); only galaxies lines indicate logistic

fractions as a function of halo mass (top), sion (bottom),and number of group members with M > 10^10.5M are considered. Dashed ts to the(unbinned) data. (arXiv:1112.3990v1


II.


Fig.3.-- Sample of z 0.7 Clumpy disks. Images are6в6 arcsec, from HST/ACS B, V and i bands. Spiral arms may be present but as not as contrasted as the main clumps (arXiv:1111.0987v1)


Fig. 4.-- Same as Fig. 3, for our sample of Stable disks. (arXiv:1111.0987v1).


(arXiv:1007.2422)


Figure 3. Ultraviolet luminosity functions at z 4, z 7 and constraints for z 10.arXiv:(:0912.4263v5)


, , , , . : , (, , ..), , (, , ..). : , , B/T, .


. , : , .


(M. Martig, F. Bournaud et al., 2012, arXiv:1201.1079v) , z~0 , n<2 ; 70% . , z=1 z=0. , «» z=0 z=1 . z=0.5 z=0.


arXiv:1207.1079


, z=2 , , . , z=2 .


Figure 4: Stellar mass of high-redshift galaxies. The colored symbols represent data for LBGs with characteristic luminosity (L). It is evident that stellar masses in typical LBGs decreases with redshift. The small grey circles denote LAEs for comparison, and the grey hatched region shows the interquartile range. The highest redshift LBGs seem to be more similar to the LAEs than to LBGs at lower redshift. Adopted from Finkelstein et al. (2010), where all references for the data shown here can be found.


Schaerer D., Pello R., astro-ph/0701195 , 8 jan 2007


. z>5, . , «downsizing», . (arXiv:1010.1381, L. Oser, J. P. Ostriker, T. Naab et al.) .


(in-situ), z>3, (<1kpc) c . (ex-situ), z<3, (dry minor mergers). M*^2, ex-situ M*, z.


(arXiv:1106.5490) M> 6.3*10^10M z=0 , c M > 10^11M z=2 1, z=0 R~(1+z)^-1.12. minor mergers 1:5. ~(1+z)^0.4.



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1) DM-, , , AGN. 2) , . 3) . 4) «archaeological downsizing», (logM*)^1.6


5) . ~(1+z)^n , n>1. 6) major mergers , . ( ) . , .