Tomographic analyses of the CMB lensing and galaxy clustering to probe the linear structure growth. (arXiv:1908.04854v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Marques_G/0/1/0/all/0/1">Gabriela A. Marques</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bernui_A/0/1/0/all/0/1">Armando Bernui</a>
In a tomographic approach, we measure the cross-correlation between the CMB In a tomographic approach, we measure the cross-correlation between the CMB http://arxiv.org/icons/sfx.gif
lensing reconstructed from the Planck satellite and the galaxies of the
photometric redshift catalogue based on the combination of the South Galactic
Cap u-band Sky Survey (SCUSS), Sloan Digital Sky Survey (SDSS), and Wide-field
Infrared Survey Explorer (WISE) data. We perform the analyses considering six
redshift bins spanning the range of $0.1
lensing reconstructed from the Planck satellite and the galaxies of the
photometric redshift catalogue based on the combination of the South Galactic
Cap u-band Sky Survey (SCUSS), Sloan Digital Sky Survey (SDSS), and Wide-field
Infrared Survey Explorer (WISE) data. We perform the analyses considering six
redshift bins spanning the range of $0.1 <z<0.7$. From the estimates of the
galaxy auto-spectrum and the cross-spectrum, we derive with high significance
the galaxy bias and the amplitude of the cross-correlation at each redshift
bin. We have finally applied these tomographic measurements to estimate the
linear structure growth using the bias-independent $hat{D}_{G}$ estimator
introduced by Giannantonio et al. 2016. We find that the amplitude of the
structure growth with respect to the fiducial cosmology is $A_{D}=1.02pm0.14$,
in agreement with the predictions of $Lambda$CDM model. We perform tests for
consistency of our results, finding no significant evidence for systematic
effects.
