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Toward a tomographic analysis of the cross-correlation between Planck CMB lensing and H-ATLAS galaxies | | Federico Bianchini
; Andrea Lapi
; Matteo Calabrese
; Pawel Bielewicz
; Joaquin Gonzalez-Nuevo
; Carlo Baccigalupi
; Luigi Danese
; Gianfranco de Zotti
; Nathan Bourne
; Asantha Cooray
; Loretta Dunne
; Stephen Eales
; | | Date: |
Mon, 16 Nov 2015 20:32:37 GMT (1888kb,D) | | Abstract: | We present an improved and extended analysis of the cross-correlation between
the map of the Cosmic Microwave Background (CMB) lensing potential derived from
the Planck mission data and the high-redshift galaxies detected by the Herschel
Astrophysical Terahertz Large Area Survey (H-ATLAS) in the photometric redshift
range $z_{
m ph} ge 1.5$. We compare the results based on the 2013 and 2015
Planck datasets, and investigate the impact of different selections of the
H-ATLAS galaxy samples. Significant improvements over our previous analysis
have been achieved thanks to the higher signal-to-noise ratio of the new CMB
lensing map recently released by the Planck collaboration. The effective galaxy
bias parameter, $b$, for the full galaxy sample, derived from a joint analysis
of the cross-power spectrum and of the galaxy auto-power spectrum is found to
be $b = 3.54^{+0.15}_{-0.14}$. Furthermore, a first tomographic analysis of the
cross-correlation signal is implemented, by splitting the galaxy sample into
two redshift intervals: $1.5 le z_{
m ph} < 2.1$ and $z_{
m ph}ge 2.1$. A
statistically significant signal was found for both bins, indicating a
substantial increase with redshift of the bias parameter: $b=2.89pm0.23$ for
the lower and $b=4.75^{+0.24}_{-0.25}$ for the higher redshift bin.
Consistently with our previous analysis we find that the amplitude of the cross
correlation signal is a factor of $1.45^{+0.14}_{-0.13}$ higher than expected
from the standard $Lambda$CDM model. The robustness of our results against
possible systematic effects has been extensively discussed although the tension
is mitigated by passing from 4 to 3$sigma$. | | Source: | arXiv, 1511.5116 | | Services: | Forum | Review | PDF | Favorites | |
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