Day 748

Monday.

1409.5432
Formation of dark matter torii around supermassive black holes via the eccentric Kozai-Lidov Mechanism
Naoz, Silk

Suggest that if the BHs are spinning, the accreted DM particles may linger in the ergosphere and thereby may generate self-annihilations and produce an indirect signature of potential interest.

1409.5433
The Herschel view of the dominant mode of galaxy growth from z=4 to the present day
Schreiber et al

Present an analysis of the deepest Hershcel images in GOODS-N/S, UDS and COSMOS.  The picture provided by 10k individual FIR detentions is supplemented by the stacking analysis of a mass-complete sample of 62k SF galaxies from the CANDELS-HST H band-selected catalogs and from 2 deep ground-based Ks band-selected catalogs in the GOODS-N and COSMOS-w fields, in order to obtain one of the most accurate and unbiased understanding to date of the stellar mass growth over the cosmic history.  Show, for the first time, that stacking also provides a powerful tool to determine the dispersion of a physical correlation and describe the method called "scatter stacking" that may be easily generalized to other experiments.  Demonstrate that galaxies of all masses from z=4 to 0 follow a universal scaling law, the so-called MS of SF galaxies.  Find a universal close-to-linear slope of the logSFR-logM* relation with a non varying dispersion of 0.3 dex.  Also find evidence for a flattening of the MS at high masses (log(M*/Msun)>10.5) that becomes less prominent with increasing z and almost vanishes by z~2.  It is tempting to associate this ending with the parallel growth of quiescent bulges in SF galaxies.  The sSFR=SFR/M* of SF galaxies is found to continuously increase from z=0 to 4.  Finally, discuss the implications of the findings on the cosmic SFR history and show that more than 2/3 of present-day stars must have formed in a regime dominated by the MS mode.  As a consequence, conclude that although omnipresent in the distant Universe, galaxy mergers had little impact in triggering strong starbursts over the last 12.5 Gyr.

1409.5435
CoMaLit III. Literature catalogs of weak lensing clusters of galaxies (LC^2)
Sereno

Compiled, from the literature, a catalog of weak lensing clusters.  Cluster ID, coordinates, and z have been standardized.  WL masses were reported to over-densities of 2500, 500, 200, and to the virial one in the reference LCDM model.  Duplicate entries were carefully handled.  Produced 3 catalogs: LC^2-single, with 485 unique groups and cluster analyses with the single-halo model; LC^2-substructure, listing substructures in complex systems; LC^2-all, listing all the 822 WL masses found in literature.  The catalogs are publicly available.

1409.5601
Mass - concentration relation and weak lensing peak counts
Cardone et al

The statistics of peaks in WL convergence maps is a promising tool to investigate both the properties of DM haloes and constrain the cosmo parameters.  Study how the number of detectable peaks and its scaling with z depend upon the cluster DM halo profiles and use peak statistics to constrain the parameter of the m-c relation (MC).  Investigate which constraints the Euclid mission can set on the MC coefficient also taking into account degeneracies with the cosmological parameters.  To this end, first estimate the number of peaks and its z distribution for different MC relations.  Find that the steeper the mass dependence and the larger the normalization, the higher is the number of detectable clusters, with the total number of peaks changing up to 40% depending on the MC relation.  Then perform a Fisher matrix forecast of the errors on the MC relate parameters as well as cosmological parameters.  Find that peak number counts detected by Euclid can determine the normalization Anu, the mass Bnu and redshift Cnu slopes and intrinsic scatter sigmanu of the MC relation to an unprecedented accuracy of 1% (relative) if all cosmo parameters are assumed to be known.  Should this assumption be relaxed, constraints are degraded, but remarkably good results can be restored setting only some of the parameters of combining peak counts with Planck data.  This precision can give insight on competing scenarios of structure formation and evolution and on the role of baryons in cluster assembling.  Alternatively, for a fixed MC relation, future peaks counts can perform as well as current BAO and SNeIa when combined with Planck.