Day 573

Saturday.  Monday.

1312.5490
Large scale structure observations
Percival

[Lecture notes]  Looks at some of the physical processes that underpin measurements by ground-based multi-object spectrographs, the evolution of measurement themselves, and looks ahead to the next 15 years and the advent of surveys such as eBOSS, DESI and Euclid.

1312.5514
Accurate shear measurement with faint sources
Zhang, Luo, Foucaud

Previous work of this series have demonstrated that cosmic shears can be measured accurately in Fourier space in the presence of background noise and finite pixel size, without assumptions on the morphologies of galaxy and PSF.  The remaining major source of error is source Poisson noise, important for faint galaxies in space-based WL measurements.  Propose a simple and rigorous way of removing the shear bias from the source Poisson noise [how?].  Noise treatment can be generalized for images made of multiple exposures through MultiDrizzle, demonstrate with COSMOS/ACS data.  With a large ensemble of mock galaxy images of unrestricted morphologies, show that shear measurement method can achieve sub-percent accuracy even for images of S/N < 5.

1312.5610
Accounting for selection effects in the BH-bulge relations: no evidence for cosmological evolution
Schulze, Wisotzki

As the title says: Presently no statistical evidence for cosmological evolution in the relation between z~1.5 and z~6.

1312.5618
Probing the accelerating universe with radio weak lensing in the JVLA sky survey
Brown, Abdalla, Amara, … et al

Highlight the potential advantages and unique aspects of performing WL in the radio band: the inclusion of continuum polarization information can greatly reduce noise in WL reconstructions and can also remove the effects of intrinsic galaxy alignments, the key astrophysical systematic effect that limits WL at all wavelengths.  …

1312.5643
The bright end of the galaxy luminosity function at z~7: before the onset of mass quenching?
Bowler, et al

Photo-z analysis to ID high-z galaxies: sample of 34 luminous galaxies with 6.5<z<7.5 (M_UV = -22.7 to -21.2), M*~1e10 Msun, majority resolved.  Provide strong evidence that the bright end of the z=7 LF does not decline as steeply as predicted by Schechter function fitted to fainter data.  Exclude GL or AGN contamination.  Results favor double power-law for high-z LF, which simply follows the form of the DM halo mass function at bright magnitudes.  This suggests that the physical mechanism which inhibits SF activity in massive galaxies (i.e., AGN feedback or some other form of 'mass quenching') has yet to impact the observable galaxy LF at z~7, a conclusion supported by the estimated masses of brightest galaxies which have only reached a mass comparable to the critical 'quenching mass' of m*=1e10.2 Msun derived from studies of the MF of SF galaxies at lower z.