Wide-area tomography of CMB lensing and the growth of cosmological density fluctuations

Peacock, J. A.; Bilicki, Maciej

doi:10.1093/mnras/sty2314

Cited by 45 publications

(46 citation statements)

References 63 publications

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“…[24][25][26] and, more recently, in Refs. [27][28][29], while the most advanced and comprehensive studies in the field have been recently published by the DES and SPT collaborations [30,31]; for future galaxy surveys, such as Euclid and LSST, this approach is destined to become the standard baseline analysis to obtain cosmological constraints [15,32,33].…”

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confidence: 99%

CMB lensing reconstruction biases in cross-correlation with large-scale structure probes

Fabbian

Lewis

Beck

2019

J. Cosmol. Astropart. Phys.

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confidence: 99%

CMB lensing reconstruction biases in cross-correlation with large-scale structure probes

Fabbian

Lewis

Beck

2019

J. Cosmol. Astropart. Phys.

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“…This work adds to previous WSC analyses that have investigated its observational and cosmological properties, such as hemispherical anisotropies [36], Minkowski functionals [37], cross-correlation with CMB lensing [38,39] and temperature [40]. It also contributes with a new strategy for mitigating systematics to those previously proposed [41][42][43][44][45][46].…”

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confidence: 74%

“…[34,35]). Finally, we also verified the impact of different assumptions about photo-z properties on the measured parameters.This work adds to previous WSC analyses that have investigated its observational and cosmological properties, such as hemispherical anisotropies [36], Minkowski functionals [37], cross-correlation with CMB lensing [38,39] and temperature [40]. It also contributes with a new strategy for mitigating systematics to those previously proposed [41][42][43][44][45][46].The basic technique we employ here -the measurement of angular power spectra in tomographic redshift shells -has been applied before to other photometric galaxy catalogs such as the MegaZ [47] and the 2MASS Photometric Redshift datasets (2MPZ) [34], to photometric quasar samples [42] and spectroscopic galaxy data [35].The outline of this paper is as follows: in Sec.…”

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confidence: 87%

All-sky angular power spectra from cleaned WISE×SuperCOSMOS galaxy number counts

Xavier

Costa-Duarte

Balaguera-Antolínez

et al. 2019

J. Cosmol. Astropart. Phys.

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Aiming to extract cosmological information from linear scales of the WISE×SuperCOSMOS photometric redshift catalog, we perform a characterization of the systematic effects associated with stellar content, evidencing the presence of contamination and obscuration. We create an integrated model for these effects (which together we call "usurper contamination"), devise a method to remove both of them simultaneously and show its functionality by applying it to a set of mock catalogs. When administered to WISE×SuperCOSMOS data, our method shows to improve the measurements of angular power spectra on scales 15 and the extraction of cosmological parameters therefrom, even though a significant excess of power remains at these scales. When ignoring scales < 15, we still find strong indications of systematics, albeit these can be localized in the southern equatorial hemisphere. An independent analysis of the northern hemisphere at ≥ 15 agrees with the ΛCDM model with parameters from the Planck satellite and gives Ω c = 0.254 ± 0.020 and Ω b < 0.065 at 95% confidence limit when combined with priors on H 0 , A s and n s . lensing of the cosmic microwave background (CMB) -which serves as a consistency check for our cosmological model, besides helping improve constraints on halo bias and on the amplitude of matter perturbationspeaks at large angular scales [25]. This is also the case for the integrated Sachs-Wolfe effect [26], probed by the cross-correlation of CMB temperature maps with galaxy distribution, whose signal comes from the evolution of gravitational potential along the CMB photon path. Another topic that requires almost full-sky galaxy surveys is the measurement of our own peculiar velocity with respect to all other galaxies [27][28][29]. Large galaxy surveys can also help us improve our understanding of galaxy bias, that could be enhanced at the largest scales if we assume that galaxies form at density peaks (see e.g. [30]).This type of studies are among the main aims of the largest forthcoming surveys. The Large Synoptic Survey Telescope 1 (LSST) [31] will cover 18, 000 deg 2 up to redshifts z 3, while the Euclid space telescope 2 will observe 15,000 deg 2 and detect galaxies up to z 2 [32]. The huge volume probed by these surveys will lead to such a high number of observed galaxies and quasars that spectroscopic measurements will be performed only for a small fraction of them, while for most sources we will have to rely on photometric redshifts (photo-zs hereafter) and photometric classification. These techniques are, however, plagued with high contamination levels, large systematic effects and uncertainties, which must be controlled and understood in order to fully mine the relevant datasets.An existing testbed for such surveys is the WISE×SuperCOSMOS catalog [33] (WSC hereafter), a fullsky photometric galaxy dataset reaching z 0.4. Our goal in this paper is to estimate cosmological parameters from this sample under the standard cosmological model ΛCDM. In this process, we characterize the systematic effects ass...

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“…These cross-correlations of galaxy clustering and CMB lensing have been measured by a number of recent experiments (see [16] for a recent list). In particular, [15] crosscorrelated CMB lensing maps from both the South Pole Tele-scope (SPT) [17] and the Planck Satellite [13] with Dark Energy Survey galaxies from z = 0.2 − 1.2.…”

Section: Introductionmentioning

confidence: 93%

Effects of redshift uncertainty on cross-correlations of CMB lensing and galaxy surveys

Cawthon

2020

Phys. Rev. D

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We explore the effects of incorporating redshift uncertainty into measurements of galaxy clustering and crosscorrelations of galaxy positions and CMB lensing maps. We use a simple Gaussian model for a redshift distribution in a redshift bin with two parameters, the mean, z0, and the width, σz. We vary these parameters, as well as the galaxy bias, bg(z), and cosmological parameters σ8(z) and Ωm in a Fisher analysis across 12 redshift bins from z = 0 − 7. We find that incorporating redshift uncertainties degrades constraints on cosmological parameters in the LSST/CMB-S4 era by about a factor of 10 compared to the case of perfect redshift knowledge. In our fiducial analysis of LSST/CMB-S4 including redshift uncertainties, we project constraints on σ8(z) for z < 3 of less than 5%. Galaxy imaging surveys are expected to have priors on redshift parameters from photometric redshift algorithms and other methods. When adding priors with the expected precision for LSST redshift algorithms, the constraints on σ8(z) can be improved by a factor of 2-3 compared to the case of no priors. We also find that 'self-calibrated' constraints on the redshift parameters from just the auto-correlation and cross-correlation measurements (with no priors) are competitive with photometric redshift techniques. In the LSST/CMB-S4 era, we find uncertainty on the redshift parameters (z0, σz) to be below 0.004(1+z) at z < 1. For all parameters, constraints improve significantly if smaller scales can be used. We also project constraints for nearer term survey combinations: DES/SPT-SZ, DES/SPT-3G and LSST/SPT-3G. arXiv:1809.09251v1 [astro-ph.CO]

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Wide-area tomography of CMB lensing and the growth of cosmological density fluctuations

Cited by 45 publications

References 63 publications

CMB lensing reconstruction biases in cross-correlation with large-scale structure probes

CMB lensing reconstruction biases in cross-correlation with large-scale structure probes

All-sky angular power spectra from cleaned WISE×SuperCOSMOS galaxy number counts

Effects of redshift uncertainty on cross-correlations of CMB lensing and galaxy surveys

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