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H-ATLAS/GAMA: Magnification Bias Tomography. Astrophysical constraints above $sim1$ arcmin | | J. González-Nuevo
; A. Lapi
; L. Bonavera
; L. Danese
; G. de Zotti
; M. Negrello
; N. Bourne
; A. Cooray
; L. Dunne
; S. Dye
; S. Eales
; C. Furlanetto
; R. J. Ivison
; J. Loveday
; S. Maddox
; M. W. L. Smith
; E. Valiante
; | | Date: |
12 Jul 2017 | | Abstract: | In this work we measure and study the cross-correlation signal between a
foreground sample of GAMA galaxies with spectroscopic redshifts in the range
$0.2<z<0.8$, and a background sample of H-ATLAS galaxies with photometric
redshifts $gtrsim1.2$. It constitutes a substantial improvement over the
cross-correlation measurements made by Gonzalez-Nuevo et al. (2014) with
updated catalogues and wider area (with $S/Ngtrsim 5$ below 10 arcmins and
reaching $S/Nsim 20$ below 30 arcsecs). The better statistics allow us to
split the sample in different redshift bins and perform a tomographic analysis
(with $S/Ngtrsim 3$ below 10 arcmins and reaching $S/Nsim 15$ below 30
arcsecs). Moreover, we implement a halo model to extract astrophysical
information about the background galaxies and the deflectors that are producing
the lensing link between the foreground (lenses) and background (sources)
samples. In the case of the sources, we find typical masses values in agreement
with previous studies: a minimum halo mass to host a central galaxy,
$M_{min}sim 10^{12.23} M_odot$, and a pivot halo mass to have at least one
sub-halo satellite, $M_1sim 10^{12.85} M_odot$. However, the lenses are
massive galaxies or even galaxy groups/clusters, with minimum mass of
$M_{min}sim 10^{13.06} M_odot$. Above a mass of $M_1sim 10^{14.57} M_odot$
they contain at least one additional satellite galaxy which contributes to the
lensing effect. The tomographic analysis shows that, while $M_1$ is almost
redshift independent, there is a clear evolution of an increasing $M_{min}$
value with redshift in agreement with theoretical estimations. Finally, the
halo modeling allow us to identify a strong lensing contribution to the
cross-correlation for angular scales below 30 arcsecs. This interpretation is
supported by the results of basic but effective simulations. | | Source: | arXiv, 1707.3709 | | Services: | Forum | Review | PDF | Favorites | |
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