SPTpol: an instrument for CMB polarization measurements with the South Pole Telescope

Austermann, J. E.; Aird, K. A.; Beall, James A.; Becker, Daniel; Bender, A. N.; Benson, B. A.; Bleem, L. E.; Britton, J.; Carlstrom, J. E.; Chang, C. L.; Chiang, H. C.; Cho, H. M.; Crawford, T. M.; Crites, A. T.; Datesman, A.; Haan, T. de; Dobbs, M.; George, E. M.; Halverson, N. W.; Harrington, N. L.; Henning, J. W.; Hilton, G. C.; Holder, G. P.; Holzapfel, W. L.; Hoover, S.; Huang, N.; Hubmayr, J.; Irwin, K. D.; Keisler, R.; Kennedy, James E.; Knox, L.; Lee, A. T.; Leitch, E. M.; Li, D.; Lueker, M.; Marrone, Daniel P.; McMahon, Jeff; Mehl, J.; Meyer, S. S.; Montroy, T. E.; Natoli, T.; Nibarger, J. P.; Niemack, Michael D.; Novosad, V.; Padin, S.; Pryke, C.; Reichardt, Christian; Ruhl, J. E.; Saliwanchik, B. R.; Sayre, J. T.; Schaffer, K. K.; Shirokoff, E.; Stark, A. A.; Story, K. T.; Vanderlinde, K.; Vieira, J. D.; Wang, G.; Williamson, A. R.; Yefremenko, V.; Yoon, K. W.; Zahn, O.

doi:10.1117/12.927286

Cited by 130 publications

(61 citation statements)

References 41 publications

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“…[141] obtained by combining data from SPTpol [142] and Herschel [143] [more specifically, we illustrate the ðÊ 150φCIB Þ ×B 150 cross correlation]. models with massive neutrinos (active or sterile).…”

Section: Discussionmentioning

confidence: 99%

Constraints on large-scale dark acoustic oscillations from cosmology

et al. 2014

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If all or a fraction of the dark matter (DM) were coupled to a bath of dark radiation (DR) in the early Universe, we expect the combined DM-DR system to give rise to acoustic oscillations of the dark matter until it decouples from the DR. Much like the standard baryon acoustic oscillations, these dark acoustic oscillations (DAO) imprint a characteristic scale, the sound horizon of dark matter, on the matter power spectrum. We compute in detail how the microphysics of the DM-DR interaction affects the clustering of matter in the Universe and show that the DAO physics also gives rise to unique signatures in the temperature and polarization spectra of the cosmic microwave background (CMB). We use cosmological data from the CMB, baryon acoustic oscillations, and large-scale structure to constrain the possible fraction of interacting DM as well as the strength of its interaction with DR. Like nearly all knowledge we have gleaned about DM since inferring its existence this constraint rests on the betrayal by gravity of the location of otherwise invisible DM. Although our results can be straightforwardly applied to a broad class of models that couple dark matter particles to various light relativistic species, in order to make quantitative predictions, we model the interacting component as dark atoms coupled to a bath of dark photons. We find that linear cosmological data and CMB lensing put strong constraints on the existence of DAO features in the CMB and the large-scale structure of the Universe. Interestingly, we find that at most ∼5% of all DM can be very strongly interacting with DR. We show that our results are surprisingly constraining for the recently proposed double-disk DM model, a novel example of how large-scale precision cosmological data can be used to constrain galactic physics and subgalactic structure.

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Section: Discussionmentioning

confidence: 99%

Constraints on large-scale dark acoustic oscillations from cosmology

et al. 2014

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“…and is one of scientific goals of current and forthcoming surveys, e.g. the Hyper Suprime-Cam survey (HSC; Aihara et al 2017 Carlstrom et al 2011;Austermann et al 2012) for tSZ.…”

Section: Introductionmentioning

confidence: 99%

Investigating cluster astrophysics and cosmology with cross-correlation of the thermal Sunyaev–Zel'dovich effect and weak lensing

Osato

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Nagai

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Recent detections of the cross-correlation of the thermal Sunyaev-Zel'dovich (tSZ) effect and weak gravitational lensing (WL) enable unique studies of cluster astrophysics and cosmology. In this work, we present constraints on the amplitude of the nonthermal pressure fraction in galaxy clusters, α 0 , and the amplitude of the matter power spectrum, σ 8 , using measurements of the tSZ power spectrum from Planck, and the tSZ-WL cross-correlation from Planck and the Red Cluster Sequence Lensing Survey. We fit the data to a semi-analytic model with the covariance matrix using N-body simulations. We find that the tSZ power spectrum alone prefers σ 8 ∼ 0.85 and a large fraction of non-thermal pressure (α 0 ∼ 0.2-0.3). The tSZ-WL cross-correlation on the other hand prefers a significantly lower σ 8 ∼ 0.6, and low α 0 ∼ 0.05. We show that this tension can be mitigated by allowing for a steep slope in the stellar-mass-halo-mass relation, which would cause a reduction of the gas in low-mass halos. In such a model, the combined data prefer σ 8 ∼ 0.7 and α 0 ∼ 0.2, consistent with predictions from hydrodynamical simulations.

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“…There are many experiments looking for B-modes on degree scales, including KeckArray [139], EBEX [140], SPIDER [141], ABS [142], and CLASS [143]); and on arcminute scales, including POLARBEAR [144], SPTpol [145], and ACTpol [146]). Finally, given the size of the signal seen by the BICEP2 collaboration, the Planck satellite has a chance to see the reionization peak in the B-mode spectrum at low .…”

Section: Inflation After Bicep2mentioning

confidence: 99%