Measurement of the pairwise kinematic Sunyaev-Zeldovich effect with Planck and BOSS data

Li, Yi Chao; Ma, Yin‐Zhe; Remazeilles, M.; Moodley, Kavilan

doi:10.1103/physrevd.97.023514

Cited by 34 publications

(32 citation statements)

References 42 publications

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“…We set σ to be the angular projection of the halo virial radius θ 200c . DGD3 can be thought of as a dipolar generalization of the aperture photometry filter used for kSZ detection (Li et al 2018;Soergel et al 2016;De Bernardis et al 2017;Schaan et al 2016). Evaluating Eq.…”

Section: Differential Gaussian Derivative Filtermentioning

confidence: 99%

Pairwise Transverse Velocity Measurement with the Rees–Sciama Effect

Yasini

Mirzatuny

Pierpaoli

2019

ApJL

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We introduce a new estimator for the mean pairwise velocities of galaxy clusters, which is based on the measurement of the clusters' transverse velocity components. The Rees-Sciama (RS) effect offers an opportunity to measure transverse peculiar velocities through its distinct dipolar signature around the halo centers in the Cosmic Microwave Background (CMB) temperature map. We exploit this dipolar structure to extract the magnitude and direction of the transverse velocity vectors from CMB maps simulated with the expected characteristics of future surveys like CMB-S4. Although in the presence of lensed CMB and instrumental noise individual velocities are not reliably reconstructed, we demonstrate that the mean pairwise velocity measurement obtained using the estimator yields a signal-to-noise ratio of 5.2 for ∼ 21, 000 halos with M > 7 × 10 13 M in a 40 × 40 [deg 2 ] patch at z = 0.5. While the proposed estimator carries promising prospects for measuring pairwise velocities through the RS effect in CMB stage IV experiments, its applications extend to any other potential probe of transverse velocities.

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Section: Differential Gaussian Derivative Filtermentioning

confidence: 99%

Pairwise Transverse Velocity Measurement with the Rees–Sciama Effect

Yasini

Mirzatuny

Pierpaoli

2019

ApJL

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“…(C.3). (b) The differences between Sugiyama et al (2018) and Li et al (2018) are that the former used a Fourier-space analysis and a density-weighted pairwise estimator, while the latter used a real-space analysis and a uniform-weighting pairwise momentum estimator. (c) Galaxy peculiar velocities form SDSS/DR7 in Planck Collaboration Int.…”

Section: Maps From the Planck Legacy Archivementioning

confidence: 99%

“…By using the same estimator to the South Pole Telescope (SPT) data and Dark Energy Survey (DES) data, Soergel et al (2016) achieved the detection of kSZ signal 4.2 σ C.L. More recently Li et al (2018) detected the pairwise kSZ signal for BOSS DR13 low mass group (M h 10 12 h −1 M ) by using the 2D-ILC map (see Sect. 2.1.2).…”

Section: Introductionmentioning

confidence: 99%

Planck intermediate results

Aghanim¹,

Akrami²,

Ashdown³

et al. 2018

A&A

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Using the Planck full-mission data, we present a detection of the temperature (and therefore velocity) dispersion due to the kinetic Sunyaev-Zeldovich (kSZ) effect from clusters of galaxies. To suppress the primary CMB and instrumental noise we derive a matched filter and then convolve it with the Planck foreground-cleaned “2D-ILC” maps. By using the Meta Catalogue of X-ray detected Clusters of galaxies (MCXC), we determine the normalized rms dispersion of the temperature fluctuations at the positions of clusters, finding that this shows excess variance compared with the noise expectation. We then build an unbiased statistical estimator of the signal, determining that the normalized mean temperature dispersion of 1526 clusters is 〈(ΔT/T)2 〉 = (1.64 ± 0.48) × 10−11. However, comparison with analytic calculations and simulations suggest that around 0.7 σ of this result is due to cluster lensing rather than the kSZ effect. By correcting this, the temperature dispersion is measured to be 〈(ΔT/T)2〉 = (1.35 ± 0.48) × 10−11, which gives a detection at the 2.8 σ level. We further convert uniform-weight temperature dispersion into a measurement of the line-of-sight velocity dispersion, by using estimates of the optical depth of each cluster (which introduces additional uncertainty into the estimate). We find that the velocity dispersion is 〈υ2〉 = (123 000 ± 71 000) (km s−1)2, which is consistent with findings from other large-scale structure studies, and provides direct evidence of statistical homogeneity on scales of 600 h−1 Mpc. Our study shows the promise of using cross-correlations of the kSZ effect with large-scale structure in order to constrain the growth of structure.

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“…The kinematic Sunyaev-Zeldovich (kSZ) effect (Sunyaev & Zeldovich 1972, 1980Vishniac 1987) offers a unique opportunity to measure peculiar velocities at cosmological distances (e.g. Ho et al 2009;Shao et al 2011;Hand et al 2012;Hernández-Monteagudo et al 2015;Planck Collaboration et al 2016;Schaan et al 2016;Hill et al 2016;Ferraro et al 2016;De Bernardis et al 2017;Lim et al 2017;Li et al 2018, for recent investigations). By combining future optical surveys (such as DESI DESI Collaboration et al 2016, Euclid Amendola et al 2018and LSST LSST Science Collaboration et al 2009) and Cosmic Microwave Background (CMB) experiments (such as the future Simons Observatory Ade et al 2019 andCMB-S4 Abazajian et al 2016) the radial peculiar velocities can be measured with high precision from the kSZ effect imprinted on the CMB for millions of galaxies and can be used to constrain cosmological parameters (e.g.…”

Section: Introductionmentioning

confidence: 99%

Reconstruction with velocities

Zhu

White

Ferraro

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Reconstruction is becoming a crucial procedure of galaxy clustering analysis for future spectroscopic redshift surveys to obtain subpercent level measurement of the baryon acoustic oscillation scale. Most reconstruction algorithms rely on an estimation of the displacement field from the observed galaxy distribution. However, the displacement reconstruction degrades near the survey boundary due to incomplete data and the boundary effects extend to ∼ 100 Mpc/h within the interior of the survey volume. We study the possibility of using radial velocities measured from the cosmic microwave background observation through the kinematic Sunyaev-Zel'dovich effect to improve performance near the boundary. We find that the boundary effect can be reduced to ∼ 30 − 40 Mpc/h with the velocity information from Simons Observatory. This is especially helpful for dense low redshift surveys where the volume is relatively small and a large fraction of total volume is affected by the boundary.

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Measurement of the pairwise kinematic Sunyaev-Zeldovich effect with Planck and BOSS data

Cited by 34 publications

References 42 publications

Pairwise Transverse Velocity Measurement with the Rees–Sciama Effect

Pairwise Transverse Velocity Measurement with the Rees–Sciama Effect

Planck intermediate results

Reconstruction with velocities

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