ebook img

Clusters of galaxies Virgo cluster Abell 1689 PDF

28 Pages·2013·5.22 MB·English
by  
Save to my drive
Quick download
Download
Most books are stored in the elastic cloud where traffic is expensive. For this reason, we have a limit on daily download.

Preview Clusters of galaxies Virgo cluster Abell 1689

Clusters of galaxies Virgo cluster Abell 1689 Perseo cluster Coma cluster Deep field SDSS H-R diagram Hertzsprung (1873-1967) Russell (1877-1957) the colour-magnitude relation Scaling relations: Showing two different properties of the galaxies as their lumonisity (or magnitudes) against their colours we obtain a distrution of points in the plane not uniform (Baldry 2006): SDSS, galaxias a z < 0.1 • “red sequence” • “blue cloud” Bimodalilty in colours is present up to z≈1 (Strateva et al. 2001; Blanton et al. 2003; Baldry et al. 2006) The Colour-Magnitud Relation (CMR): Fornax cluster Hilker et al. (2003) Hydra I cluster (Misgeld et al. 2008) Abell 1644, 1069 There is evidence of the break in Vaucoleurs et al. (1961), Tremonti et al. (2004), Baldry et al. (2004), Ferrarese et al. (2006), Boselli et al. (2008), Metcalfe, Godwin & Peach (1994) Virgo cluster (SDSS) Janz & Lisker 2009 Hydra I cluster (Misgeld et al. 2008) Motivation: The CMR constitutes an excelent tool to constrain galaxy formation models since galactic evoution is evidenced through the relation What are the physical processes involved in the development of the CMR of cluster galaxies? How can we explain the behavior of the bright end? Hybrid Model of Galaxy Formation N-body Semi-analytical Simualtions model of galaxy Formation (SAG) Semi-Analytic model of Galaxy Formation (SAG) Simulated clusters (Dolag et al. 2005):  Originally extracted from a DM-only simulation with a box size of 479 h−1 Mpc C15: 3 clusters  The Lagrangian regions surrounding M (z=0) ~ 1015 h-1 M the selected clusters have been  resimulated at higher mass and force resolution using the ’zoomed initial conditions’ technique (Tormen et al. 1997) C14: 5 clusters M (z=0) ~ 1014 h-1 M  9 −1 M = 1.13× 10 h M DM o Ω = 0.3, Ω = 0.7,Ω = 0.13 m Λ b GADGET- 2 Γ= 0.21, σ = 0.9 (Springel et al. 2005) 8 −1 −1 H = 100 km s Mpc , h= 0.7 0 M   M (M(i)  M(i)  M(i) ) hot b vir star cold BH i 3 kT (r) g t (r)  cool 2 m n2(r)(T,Z) p e dM dr cool  4r2 cool cool dt dt The model is calibrated to reproduce simultnaneously several galactic properties as the STARS n dM  V  M   vir  cold LF, the MBH, the CMR, morpholgy ratios, etc  4  E dt 220kms1 t M   SNCC SNCC M   reheat 3 V2  dyn vir Low mass stars SN CC SN Ia

Description:
Virgo cluster Coma cluster Abell 1689 Perseo cluster Deep field SDSS Clusters of galaxies
See more

The list of books you might like

Most books are stored in the elastic cloud where traffic is expensive. For this reason, we have a limit on daily download.