Detection of the kinematic Sunyaev–Zel'dovich effect with DES Year 1 and SPT

Soergel, Bjoern; Flender, Samuel; Story, K. T.; Bleem, L. E.; Giannantonio, T.; Efstathiou, G.; Rykoff, E. S.; Benson, B. A.; Crawford, T. M.; Dodelson, Scott; Habib, Salman; Heitmann, Katrin; Holder, G. P.; Jain, Bhuvnesh; Rozo, Eduardo; Saro, A.; Weller, J.; Abdalla, F. B.; Allam, S.; Annis, J.; Armstrong, R.; Benoit-Lévy, A.; Bernstein, G. M.; Carlstrom, J. E.; Rosell, A. Carnero; Kind, M. Carrasco; Castander, F. J.; Chiu, I.; Chown, R.; Crocce, M.; Cunha, C. E.; D’Andrea, C. B.; Costa, L. N. da; Haan, T. de; Desai, S.; Diehl, H. T.; Dietrich, J. P.; Doel, P.; Estrada, J.; Evrard, A. E.; Flaugher, B.; Fosalba, P.; Frieman, Joshua A.; Gaztañaga, E.; Gruen, D.; Gruendl, R. A.; Holzapfel, W. L.; Honscheid, K.; James, D. J.; Keisler, R.; Kuêhn, K.; Kuropatkin, N.; Lahav, O.; Lima, M.; Marshall, J. L.; McDonald, Michael; Melchior, P.; Miller, C. J.; Miquel, R.; Nord, B.; Ogando, R. L. C.; Omori, Y.; Plazas, A. A.; Rapetti, David; Reichardt, C. L.; Romer, A. K.; Roodman, A.; Saliwanchik, B. R.; Sánchez, E.; Schubnell, M.; Sevilla-Noarbe, I.; Sheldon, E.; Smith, R. C.; Soares-Santos, M.; Sobreira, F.; Stark, A. A.; Suchyta, E.; Swanson, M. E. C.; Tarlè, G.; Thomas, Daniel; Vieira, J. D.; Walker, Andre; Whitehorn, N.

doi:10.1093/mnras/stw1455

Cited by 118 publications

(127 citation statements)

References 96 publications

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“…The first is based on SExtractor MAG_AUTO quantities from the Y1 coadd catalogs, as applied to REDMAPPER in [38]. The second is based on a simultaneous multiepoch, multiband, and multiobject fit (MOF) (see Sec.…”

Section: B Redmagic Samplementioning

confidence: 99%

Dark Energy Survey year 1 results: Galaxy clustering for combined probes

Elvin-Poole¹,

Crocce²,

Ross³

et al. 2018

Phys. Rev. D

Self Cite

159

235

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We measure the clustering of DES year 1 galaxies that are intended to be combined with weak lensing samples in order to produce precise cosmological constraints from the joint analysis of large-scale structure and lensing correlations. Two-point correlation functions are measured for a sample of 6.6 × 10 5 luminous red galaxies selected using the REDMAGIC algorithm over an area of 1321 square degrees, in the redshift range 0.15 < z < 0.9, split into five tomographic redshift bins. The sample has a mean redshift uncertainty of σ z =ð1 þ zÞ ¼ 0.017. We quantify and correct spurious correlations induced by spatially variable survey properties, testing their impact on the clustering measurements and covariance. We demonstrate the sample's robustness by testing for stellar contamination, for potential biases that could arise from the systematic correction, and for the consistency between the two-point auto-and cross-correlation functions. We show that the corrections we apply have a significant impact on the resultant measurement of cosmological parameters, but that the results are robust against arbitrary choices in the correction method. We find the linear galaxy bias in each redshift bin in a fiducial cosmology to be bðσ 8 =0.81Þj z¼0.24 ¼ 1.40 AE 0.07, bðσ 8 =0.81Þj z¼0.38 ¼ 1.60 AE 0.05, bðσ 8 =0.81Þj z¼0.53 ¼ 1.60 AE 0.04 for galaxies with luminosities L=L Ã > 0.5, bðσ 8 =0.81Þj z¼0.68 ¼ 1.93 AE 0.04 for L=L Ã > 1 and bðσ 8 =0.81Þj z¼0.83 ¼ 1.98 AE 0.07 for L=L Ã > 1.5, broadly consistent with expectations for the redshift and luminosity dependence of the bias of red galaxies. We show these measurements to be consistent with the linear bias obtained from tangential shear measurements.

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Section: B Redmagic Samplementioning

confidence: 99%

Dark Energy Survey year 1 results: Galaxy clustering for combined probes

Elvin-Poole¹,

Crocce²,

Ross³

et al. 2018

Phys. Rev. D

Self Cite

159

235

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“…In the following, we will take f free = 0.85 as our fiducial value (except where stated otherwise), and note that f free can be constrained with kSZ measurements [15,[29][30][31].…”

Section: Bias To Cross-correlation With Large-scale Structure Tramentioning

confidence: 99%

“…The kSZ signal can be used to measure the ionized gas abundance and distribution in galaxies and clusters, thus providing important information about the extent and nature of astrophysical feedback processes (e.g., energy injection from active galactic nucleus feedback). Taking advantage of this sensitivity to the gas distribution, recent detections of the kSZ signal have made progress towards resolving the long-standing "missing baryons" problem at low redshift [14,30,31,51,52]. In addition, through its dependence on the large-scale velocity field, the kSZ effect can also be used as a cosmological probe to measure the growth of structure [53][54][55].…”

Section: Introductionmentioning

confidence: 99%

Bias to CMB lensing reconstruction from temperature anisotropies due to large-scale galaxy motions

Ferraro

Hill

2018

Phys. Rev. D

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Gravitational lensing of the cosmic microwave background (CMB) is expected to be amongst the most powerful cosmological tools for ongoing and upcoming CMB experiments. In this work, we investigate a bias to CMB lensing reconstruction from temperature anisotropies due to the kinematic Sunyaev-Zel'dovich (kSZ) effect, that is, the Doppler shift of CMB photons induced by Compton-scattering off moving electrons. The kSZ signal yields biases due to both its own intrinsic non-Gaussianity and its non-zero cross-correlation with the CMB lensing field (and other fields that trace the large-scale structure). This kSZ-induced bias affects both the CMB lensing auto-power spectrum and its cross-correlation with low-redshift tracers. Furthermore, it cannot be removed by multifrequency foreground separation techniques because the kSZ effect preserves the blackbody spectrum of the CMB. While statistically negligible for current datasets, we show that it will be important for upcoming surveys, and failure to account for it can lead to large biases in constraints on neutrino masses or the properties of dark energy. For a Stage 4 CMB experiment, the bias can be as large as ≈ 15% or 12% in cross-correlation with LSST galaxy lensing convergence or galaxy overdensity maps, respectively, when the maximum temperature multipole used in the reconstruction is max = 4000, and about half of that when max = 3000. Similarly, we find that the CMB lensing auto-power spectrum can be biased by up to several percent. These biases are many times larger than the expected statistical errors. We validate our analytical predictions with cosmological simulations and present the first complete estimate of secondary-induced CMB lensing biases. The predicted bias is sensitive to the small-scale gas distribution, which is affected by pressure and feedback mechanisms, thus making removal via "bias-hardened" estimators challenging. Reducing max can significantly mitigate the bias at the cost of a decrease in the overall lensing reconstruction signal-tonoise. A bias 1% on large scales requires max 2000, which leads to a reduction in signal-to-noise by a factor of ≈ 3 − 5 for a Stage 4 CMB experiment. Polarization-only reconstruction may be the most robust mitigation strategy.

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“…The kSZ effect, on the other hand, while much more difficult to detect, is affected by all ionized gas regardless of its temperature, providing a more global and unbiased view of the universe during and after reionization. The next generation of ground based CMB surveys, such as the Simons Observatory (SO 1 ) and CMB-S4 2 (Abazajian et al 2016) will use the kSZ effect both as a probe of the intergalactic medium (Hernández-Monteagudo et al 2015;Schaan et al 2016;Hill et al 2016;Soergel et al 2016;De Bernardis et al 2017;: cosmology with large-scale velocity flows (Mueller et al 2015a;Sugiyama et al 2017;Mueller et al 2015b;) will soon become a reality. The kSZ effect can be detected in the cosmic microwave background alone or by cross-correlating it with tracers of large-scale structure such as galaxies and clusters.…”

Section: Introductionmentioning

confidence: 99%

“…The kSZ effect can be detected in the cosmic microwave background alone or by cross-correlating it with tracers of large-scale structure such as galaxies and clusters. Cross correlation is done by combining CMB temperature maps with line intensity maps in the EOR (Cooray 2004;Salvaterra et al 2005;Alvarez et al 2006), with projected fields of large scale structure (e.g., Doré et al 2004;Ferraro et al 2015;Hill et al 2016), or by stacking on groups and clusters (Schaan et al 2016;Soergel et al 2016). These techniques use the fact that the peculiar velocities responsible for the effect are correlated with large scale density fluctuations, while the electron density fluctuations required to avoid line of sight cancellation occur on small scales.…”

Section: Introductionmentioning

confidence: 99%

The Impact of Baryonic Physics on the Kinetic Sunyaev–Zel’dovich Effect

Park

Alvarez

Bond

2018

ApJ

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Poorly understood "baryonic physics" impacts our ability to predict the power spectrum of the kinetic Sunyaev-Zel'dovich (kSZ) effect. We study this in one sample high resolution simulation of galaxy formation and feedback, Illustris. The high resolution of Illustris allows us to probe the kSZ power spectrum on multipoles = 10 3 − 3 × 10 4 . Strong AGN feedback in Illustris nearly wipes out gas fluctuations at k 1 h Mpc −1 and at late times, likely somewhat under predicting the kSZ power generated at z 1. The post-reionization kSZ power spectrum for Illustris is well-fit by D z<6 = 1.38[ /3000] 0.21 µK 2 over 3000 10000, somewhat lower than most other reported values but consistent with the analysis of Shaw et al. Our analysis of the bias of free electrons reveals subtle effects associated with the multi-phase gas physics and stellar fractions that affect even linear scales. In particular there are fewer electrons in biased galaxies, due to gas cooling and star formation, and this leads to an electron bias less than one even at low wavenumbers. The combination of bias and electron fraction that determines the overall suppression is relatively constant, f 2 e b 2 e0 ∼ 0.7, but more simulations are needed to see if this is Illustris-specific. By separating the kSZ power into different terms, we find at least 6 (10)% of the signal at = 3000 (10000) comes from non-Gaussian connected four-point density and velocity correlations, δvδv c , even without correcting for the Illustris simulation box size. A challenge going forward will be to accurately model long-wave velocity modes simultaneously with Illustris-like high resolution to capture the complexities of galaxy formation and its correlations with large scale flows. Subject headings:1. INTRODUCTION The cosmic microwave background (CMB) is a powerful probe of cosmic history through secondary anisotropies generated by free electrons in the intergalactic medium, resulting in a spectral distortion and cluster-concentrated anisotropies from inverse Compton scattering off of hot gas in galaxy clusters, the thermal Sunyaev-Zel'dovich (tSZ) effect (e.g., Sunyaev and Zeldovich 1972), and spectrally undistorted temperature anisotropies from Thompson scattering from moving electrons participating in the bulk flow of the medium, the kinetic Sunyeav-Zel'dovich (kSZ) (e.g., Sunyaev and Zeldovich 1980) effect.Of these two, the tSZ effect is much easier to detect because it is determined by electron pressure, which is much higher in clusters. The distinct spectral signature allows it to be separated from other sky signals if observations are made in multiple frequency bands. Because the tSZ effect is dominated by massive clusters, however, it gives a rather biased view of the intergalactic medium, concentrated towards the rarest peaks at relatively late times, z 1.5 (e.g., Komatsu and Seljak 2002). The kSZ effect, on the other hand, while much more difficult to detect, is affected by all ionized gas regardless of its temperature, providing a more global and unbiased view o...

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Detection of the kinematic Sunyaev–Zel'dovich effect with DES Year 1 and SPT

Cited by 118 publications

References 96 publications

Dark Energy Survey year 1 results: Galaxy clustering for combined probes

Dark Energy Survey year 1 results: Galaxy clustering for combined probes

Bias to CMB lensing reconstruction from temperature anisotropies due to large-scale galaxy motions

The Impact of Baryonic Physics on the Kinetic Sunyaev–Zel’dovich Effect

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