Day 1111

Thursday.  Friday.  Monday.  Tuesday.

1606.07817
Constraints on assembly bias from galaxy clustering
Zentner, Hearing, van den Bosch, Lange, Villarreal

Constrain the newly-introduced decorated HOD model using SDSS DR7 measurements of projected galaxy clustering or r-band luminosity threshold samples.  The decorated HOD is a model for the galaxy-halo connection that augments the HOD by allowing for the possibility of galaxy assembly bias: galaxy luminosity may be correlated with DM halo properties besides mass, Mvir.  Demonstrate that it is not possible to rule out galaxy assembly bias using DR7 measurements of galaxy clustering alone.  Moreover, galaxy samples with Mr<-20 and Mr<-20.5 favor strong central galaxy assembly bias.  These samples prefer scenarios in which high-concentration are more likely to host a central galaxy relative to low-concentration halos of the same mass.  Exclude zero assembly bias with high significance for these samples.  Satellite galaxy assembly bias is significant for the faintest sample, Mr<-19.  Find no evidence for assembly bias in the Mr<-21 sample.  Assembly bias should be accounted for in galaxy clustering analysis or attempts to exploit galaxy clustering to constrain cosmology.  In addition to presenting the first constraints on HOD models that accommodate assembly bias, the analysis includes several improvements over previous analyses of these data.  Therefore, the inferences supersede previously-published results even in the case of a standard HOD analysis.


1606.07837
The systematic error test for PSF correction in weak gravitational lensing shear measurement bo the ERA Method by idealizing PSF
Okura, Futamase

Improve the ERA (Ellipticity of Re-smeared Artificial image) method of PSF correction in WL shear analysis in order to treat realistic shape of galaxies and PSF.  This is done by re-smearing PSF and the observed galaxy image smeared by a RSF (Re-Smearing Function), and allows use of a new PSF with a simple shape and to correct PSF effect without any approximations and assumptions.  Perform numerical test to show that the method applied for galaxies and PSF with some complicated shapes can correct PSF effect with systematic error less than 0.1%.  Also apply ERA method for real data of A1689 cluster to confirm that it is able to detect the systematic WL shear pattern.  The ERA method requires less than 0.1 or 1 second to correct PSF for each object in numerical test and real data analysis, respectively.