Measurement of the Integrated Sachs–wolfe Effect Using the Allwise Data Release

Shajib, Anowar J.; Wright, E. L.

doi:10.3847/0004-637x/827/2/116

Cited by 26 publications

(33 citation statements)

References 55 publications

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“…The crosscorrelation measurements we considered include Giannantonio et al Kovács et al (2017). Of these, the papers that reported two different results with a sufficiently different dataset or methodology are Granett, Neyrinck & Szapudi (2009); Fer-raro, Sherwin & Spergel (2015); Shajib & Wright (2016); Cai et al (2017); Kovács et al (2017).…”

Section: Comparison With Earlier Resultsmentioning

confidence: 99%

“…Most of the measurements quoted above are statistically consistent with expectations from the standard ΛCDM model, however, it cannot be stated that observational consensus has been reached in the field. Several experiments detected an ISW signal amplitude that exceeds the ΛCDM prediction by 1 sigma (Giannantonio et al 2008;Granett, Neyrinck & Szapudi 2009;Giannantonio et al 2012;Granett, Kovács & Hawken 2015;Nadathur & Crittenden 2016), 2 sigmas (Granett, Neyrinck & Szapudi 2008;Ho et al 2008;Pápai, Szapudi & Granett 2011;Goto, Szapudi & Granett 2012;Kovács et al 2017) or even 3 sigmas (Cai et al 2017), even though some of the detections were later revised to be of smaller magnitude as new data came available (Kovács et al 2013;Ferraro, Sherwin & Spergel 2015;Shajib & Wright 2016). The reported A amplitude factors (A = 1 matches ΛCDM) also vary wildly among papers, from just 0.64 up to even 20, depending on the dataset and methodology details.…”

Section: Introductionmentioning

confidence: 99%

“…);Ho et al (2008);Granett, Neyrinck & Szapudi (2009);Giannantonio et al (2012);Goto, Szapudi & Granett (2012);Kovács et al (2013);Ferraro, Sherwin & Spergel (2015);Granett, Kovács & Hawken (2015); PlanckCollaboration et al (2016);Shajib & Wright (2016), while the stacking measurements are comprised ofGranett, Neyrinck & Szapudi (2008);Pápai, Szapudi & Granett (2011);Granett, Kovács & Hawken (2015);Cai et al (2017);Kovács et al (2017). Of these, the papers that reported two different results with a sufficiently different dataset or methodology areGranett, Neyrinck & Szapudi (2009);Fer- raro, Sherwin & Spergel (2015);Shajib & Wright (2016);Cai et al (2017);Kovács et al (2017).…”

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confidence: 99%

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The integrated Sachs–Wolfe effect in the AvERA cosmology

Beck

Csabai

Rácz

et al. 2018

Monthly Notices of the Royal Astronomical Society

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The recent AvERA cosmological simulation of Rácz et al. (2017) has a ΛCDMlike expansion history and removes the tension between local and Planck (cosmic microwave background) Hubble constants. We contrast the AvERA prediction of the integrated Sachs-Wolfe (ISW) effect with that of ΛCDM. The linear ISW effect is proportional to the derivative of the growth function, thus it is sensitive to small differences in the expansion histories of the respective models. We create simulated ISW maps tracing the path of light-rays through the Millennium XXL cosmological simulation, and perform theoretical calculations of the ISW power spectrum. AvERA predicts a significantly higher ISW effect than ΛCDM, A = 1.93 − 5.29 times larger depending on the l index of the spherical power spectrum, which could be utilized to definitively differentiate the models. We also show that AvERA predicts an oppositesign ISW effect in the redshift range z ≈ 1.5 − 4.4, in clear contrast with ΛCDM. Finally, we compare our ISW predictions with previous observations. While at present these cannot distinguish between the two models due to large error bars, and lack of internal consistency suggesting systematics, ISW probes from future surveys will tightly constrain the models.

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Section: Comparison With Earlier Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

mentioning

confidence: 99%

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The integrated Sachs–Wolfe effect in the AvERA cosmology

Beck

Csabai

Rácz

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…In our investigation we use the data obtained by cross-correlating CMB temperature maps with the galaxies from the Wide-field Infrared Survey Explorer (WISE ) [38]; we shall refer to these data as the WISE ISW signal, for short. Our analysis will follow closely the steps described in [30,31] for ΛCDM, but applied to the Galileon model and for a large range of parameter values. In particular, before evaluating C Tg , we first make use of the cross-correlation of CMB lensing maps with the galaxy distribution to get an estimate for the galaxy bias which would otherwise be completely degenerate with the Galileon effects on the amplitude of C Tg .…”

Section: Contentsmentioning

confidence: 99%

Galileon gravity in light of ISW, CMB, BAO andH₀data

Renk

Zumalacárregui

Montanari

et al. 2017

J. Cosmol. Astropart. Phys.

216

215

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Cosmological models with Galileon gravity are an alternative to the standard ΛCDM paradigm with testable predictions at the level of its self-accelerating solutions for the expansion history, as well as large-scale structure formation. Here, we place constraints on the full parameter space of these models using data from the cosmic microwave background (CMB) (including lensing), baryonic acoustic oscillations (BAO) and the Integrated Sachs-Wolfe (ISW) effect. We pay special attention to the ISW effect for which we use the crossspectra, C Tg , of CMB temperature maps and foreground galaxies from the WISE survey. The sign of C Tg is set by the time evolution of the lensing potential in the redshift range of the galaxy sample: it is positive if the potential decays (like in ΛCDM), negative if it deepens. We constrain three subsets of Galileon gravity separately known as the Cubic, Quartic and Quintic Galileons. The cubic Galileon model predicts a negative C Tg and exhibits a 7.8σ tension with the data, which effectively rules it out. For the quartic and quintic models the ISW data also rule out a significant portion of the parameter space but permit regions where the goodness-of-fit is comparable to ΛCDM. The data prefers a non zero sum of the neutrino masses ( m ν ≈ 0.5eV) with ∼ 5σ significance in these models. The best-fitting models have values of H 0 consistent with local determinations, thereby avoiding the tension that exists in ΛCDM. We also identify and discuss a ∼ 2σ tension that Galileon gravity exhibits with recent BAO measurements. Our analysis shows overall that Galileon cosmologies cannot be ruled out by current data but future lensing, BAO and ISW data hold strong potential to do so.

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“…The linear part is due to the decay of the gravitational potential on large scales because of the late-time cosmic acceleration. This is a very large-scale effect and detectable at < 100 (for a measurement of ISW with WISE galaxies, see [54,63]). For this reason any analysis of the kSZ 2 signal should explicitly filter out scales with less than a few hundred.…”

Section: B Gravitational Secondary Anisotropiesmentioning

confidence: 99%

Kinematic Sunyaev-Zel’dovich effect with projected fields. II. Prospects, challenges, and comparison with simulations

et al. 2016

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The kinematic Sunyaev-Zel'dovich (kSZ) signal is a powerful probe of the cosmic baryon distribution. The kSZ signal is proportional to the integrated free electron momentum rather than the electron pressure (which sources the thermal SZ signal). Since velocities should be unbiased on large scales, the kSZ signal is an unbiased tracer of the large-scale electron distribution, and thus can be used to detect the "missing baryons" that evade most observational techniques.While most current methods for kSZ extraction rely on the availability of very accurate redshifts, we revisit a method that allows measurements even in the absence of redshift information for individual objects. It involves cross-correlating the square of an appropriately filtered cosmic microwave background (CMB) temperature map with a projected density map constructed from a sample of large-scale structure tracers. We show that this method will achieve high signal-to-noise when applied to the next generation of high-resolution CMB experiments, provided that component separation is sufficiently effective at removing foreground contamination. Considering statistical errors only, we forecast that this estimator can yield S/N ≈ 3, 120 and over 150 for Planck, Advanced ACTPol, and a hypothetical Stage-IV CMB experiment, respectively, in combination with a galaxy catalog from WISE, and about 20% larger S/N for a galaxy catalog from the proposed SPHEREx experiment. We show that the basic estimator receives a contribution due to leakage from CMB lensing, but that this term can be effectively removed by either direct measurement or marginalization, with little effect on the kSZ significance. We discuss possible sources of systematic contamination and propose mitigation strategies for future surveys. We compare the theoretical predictions to numerical simulations and validate the approximations in our analytic approach.This work serves as a companion paper to the first kSZ measurement with this method, where we used CMB temperature maps constructed from Planck and WMAP data, together with galaxies from the WISE survey, to obtain a 3.8 -4.5σ detection of the kSZ 2 amplitude. PACS numbers: 98.80.-k, 98.70.Vc

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Measurement of the Integrated Sachs–wolfe Effect Using the Allwise Data Release

Cited by 26 publications

References 55 publications

The integrated Sachs–Wolfe effect in the AvERA cosmology

The integrated Sachs–Wolfe effect in the AvERA cosmology

Galileon gravity in light of ISW, CMB, BAO andH₀data

Kinematic Sunyaev-Zel’dovich effect with projected fields. II. Prospects, challenges, and comparison with simulations

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Measurement of the Integrated Sachs–wolfe Effect Using the Allwise Data Release

Cited by 26 publications

References 55 publications

The integrated Sachs–Wolfe effect in the AvERA cosmology

The integrated Sachs–Wolfe effect in the AvERA cosmology

Galileon gravity in light of ISW, CMB, BAO andH0data

Kinematic Sunyaev-Zel’dovich effect with projected fields. II. Prospects, challenges, and comparison with simulations

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Galileon gravity in light of ISW, CMB, BAO andH₀data