Common use of Physical Properties Clause in Contracts

Physical Properties. These UV-selected star-forming galaxies have stellar masses ⟨log10M∗/M⊙⟩ = −1 10.08 ± 0.51 (▇▇▇▇▇▇▇ et al. 2005). The typical star formation rates (SFRs) are ∼ 30 M⊙ yr , where the SFRs of individual objects vary from ≈ 7− to ≈ 200 M⊙ yr , and the mean SFR surface density is ⟨ΣSFR⟩ = 2.9 M⊙ yr−1 kpc−2 (▇▇▇ et al. 2006). These stellar mass and SFR estimates assume a Chabrier (2003) IMF. The galaxies show a correlation between their stellar mass and metallicity, but the relation is offset by 0.3 dex as compared to the local relation, with the same stellar mass galaxies having lower metallicity at z ≈ 2.4 (▇▇▇ et al. 2006c). Typical metallicities range from ≈ 0.3 Z⊙ for galaxies with ⟨M∗⟩ = 2.7 × 109M⊙ to ≈ Z⊙ for galaxies with ⟨M∗⟩ = 1 × 1011M⊙. As discussed in section 3.2.1.1, ISM absorption lines are almost always blue-shifted with respect to the galaxy systemic redshift, and the Lyα emis- sion line is always redshifted. These observed velocity offsets suggest that galaxy-scale outflows, with velocities of hundreds of km s−1, are the norm in these star-forming galaxies. ▇▇▇▇▇▇▇ et al. (2011, in preparation) use the Millennium simulation (Springel 2005), together with a clustering analysis, to connect galaxies from KBSS to dark matter halos. They find that this type of galaxy resides in halos with masses above 1011.75 h−1M⊙, with a median halo mass of ∼ 1012 h−1M⊙. The corresponding virial radii are ≈ 85 and ≈ 106 pkpc, respectively, with circular velocities ≈ 197 km s−1 and ≈ 244 km s−1.