Day 306

Thursday.

1209.5745
Numerical simulations of the dark universe: state of the art and the next decade
Kuhlen, Vogelsberger, Angulo

Review of the current state of the art of cosmological dark matter simulations, with particular emphasis on the implications for dark matter detection efforts and studies of dark energy.  Cosmo simulations are massive, requires supercomputing centers.  Limitations of cold and collisionless DM-only approach; some efforts to include different particle physics as well as baryonic physics in galaxy formation simulations, including a discussion of recent results highlighting how the distribution of DM in haloes may be altered.  

1209.5752
The cosmology of atomic dark matter
Cyr-Racine, Sigurdson

DM kinematically decouples from standard model plasma early on; it can remain coupled to a bath of "dark radiation" until a relatively late epoch.  Atomic Dark Matter model, form neutral atom-like bound states and form gravitationally-bound structures.  Necessarily includes an extra dark radiation component.

1209.5753
Gaia and the dynamics of the galaxy
Famaey

Gaia mission will answer: rotation curve of the outer Galaxy, departure from axisymmetry and equilibrium of the Galaxy, hierarchical formation and secular evolution in shaping the Galaxy and its various components, properties of the Galaxy in accordance with expectations from the standard model of cosmology.  Dynamics of the MW, gravitational potential and mass distribution, including DM component.

1209.5842
Escape of Lyman-alpha and continuum photons from star-formng galaxies
Yajima, Li, Zhu, Abel, Gronwall, Ciardullo

Ionizing photos from LAEs alone are not sufficient to ionize IGM at z>6, but they can maintain the ionization of IGM at 0<z<5.

1209.5930
The distribution of faint satellites around central galaxies in the CFHT legacy survey
Jiang, Jing, Li

Radial number density profile and abundance distribution of faint satellites around central galaxies in the low-z universe.  3 magnitude bins of centrals; projected radial number density of satellites obeys a power law form with the slope of -1.05, independent of central galaxy luminosity and satellite luminosity.  Projected cross correlation function between central and satellite galaxies exhibits a non-monotonic trend with satellite luminosity.  Decreasing trend of clustering amplitude with satellite luminosity is reversed when satellites are fainter than central galaxies by more than 2 magnitudes.  Comparison with the satellite luminosity function is MW and M31: MW and M31 have 2x as many satellites as around a typical central galaxy of similar luminosity.

1209.5938
Richness-mass relation self-calibration for galaxy clusters
Anderon, Berge

(1) Derive richness-mass scaling in local universe from 53 clusters (slope and scatter).  (2) Show in photo-z in 250 clusters of 0.06<z<0.9 (mostly z<0.3) with red-sequence photo-z of delta-z < 0.02.  (3) Compute predicted prior of the richness-mass scaling to forecast the capabilities of future wide-field-area surveys of galaxy clusters to constrain cosmological parameters.  Better knowledge of scaling parameter likely has a strong impact on the relative importance of the different probes used to constrain cosmological parameters.  

1209.6021
Constraints on primordial black holes as dark matter candidates from star formation
Capela, Pshirkov, Tinyakov

Estimate amount of DM trapped in stars, considering adiabatic contraction of the DM during star formation.  If DM consists partly of primordial BHs (PBHs), they will be trapped together with the rest of the DM and will be finally inherited by a star compact remnant (WD or NS), which they will destroy in a short time.  Observations of WDs and NSs thus impose constraints on the abundance of PBH.  Best constraints: Omega_PBH/Omega_DM < 1e-5.