Day 423

Tuesday.

1304.7273
The M87 Black hole mass from gas-dynamical models of space telescope imaging spectrograph observations
Walsh et al

As the title says.  Map out the complete kinematic structure of the emission-line disk within about 40 pc from the nucleus.  The gas-dynmical BH mass continues to differ from the most recent stellar-dynamical mass by a factor of two.

1304.7276
High velocity outflows from young star-formin galaxies in the UKIDSS ultra-deep survey
Bradshaw et al

Galactic scale outflows for 0.71<z<1.63 using 413 K-band selected galaxies observed in spectro follow-up.  Average M* of 1e9.5 Msun and span a wide range in rest-frame colors, representing typical SF galaxies at this epoch.  Stack the spectra by various galaxy properties, including stellar mass, [OII] EW, SFR, sSFR and rest-frame spectral indicies.  Find that out flows are present in virtually all spectral stacks, with velocities ranging from 100-1000 km/s, indicating that large-scale outflowing winds are a common property at these redshifts.  [are there any red galaxies or non-SF galaxies in the sample?]  The highest outflows (>500 km/s) are found in galaxies with the highest stellar masses and the youngest stellar populations.  Findings suggest that high velocity galactic outflows are mostly driven by SF processes rather than AGN, with implied mass outflow rates comparable to the rates of SF.  Such behaviour is consistent with models required to reproduce the high-z mass-metallicity relation.

1304.7317
Cosmic opacity: cosmological-model-independent tests and their impacts on cosmic acceleration
Li, et al

Assume distance-duality relation entirely arises from non-conservation of the photon number, and absorption is frequency independent in the observed frequency range; perform cosmological-model-independent tests for the cosmic opacity.  ... analysis suggests that an accelerated cosmic expansion is still needed to account for the dimming of SNe.

1304.7681
Reconstructing the projected gravitational potential of galaxy clusters from galaxy kinematics
Sarli, ... Meneghetti, ... Bartelmann

Develop a method for reconstructing the 2d, projected gravitational potential of galaxy clusters from observed line-of-sight velocity dispersions of cluster galaxies.  It is the third of an intended series of papers aiming at a unique reconstruction method for cluster potentials combining lensing, X-ray, SZ and kinematic data.  The observed galaxy velocity dispersions are deprojected.  The obtained radial velocity dispersions are then related to the gravitational potential by using the tested assumption of a polytropic relation between the effective galaxy pressure [?] and the density.  Once the gravitational potential is obtained in 3d, projection along the LoS yields the 2d potential.  For simplicity, adopt spherical symmetry and a known profile for the anisotropy parameter of the galaxy velocity dispersions.  Test the method with a numerically simulated galaxy cluster and galaxies identified therein.  Extract a projected velocity-dispersion profile from the simulated cluster and pass it through the algorithm, showing that the deviation between the true and the reconstructed potential is <10% within approximately 1.2 Mpc/h from the cluster center.

1304.7689
Accurate weak lensing of standard candles, Part 1: flexible cosmological fits
Amendola, Marra, Quartin

Magnitude scatter of SNIa will become a major issue, affecting parameter estimation.  Current N-body simulations are too time consuming to be integrated in the likelihood analysis used for estimating the cosmo parameters.  In this paper, show that in the WL regime a statistical numerical approximation produces accurate results orders of magnitude faster.  Fits to lensing magnification probability distribution as a function of redshift, of the PS normalization and of the present-day matter density.  Also improve upon existing models of lensing variance and show that a shifted lognormal distribution fits well the numerical one.  These fits can be easily employed in cosmo likelihood analysis.  Theoretical predictions make it possible to invert the problem and begin using SNe lensing to constrain the cosmo parameters.