Planck 2015 results. XXI. The integrated Sachs-Wolfe effect
Planck Collaboration, P. A. R. Ade, N. Aghanim, M. Arnaud, M. Ashdown, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, N. Bartolo, S. Basak, E. Battane… 展开作者
Planck Collaboration, P. A. R. Ade, N. Aghanim, M. Arnaud, M. Ashdown, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, N. Bartolo, S. Basak, E. Battaner, K. Benabed, A. Benot, A. Benoit-Lvy, J. -P. Bernard, M. Bersanelli, P. Bielewicz, J. J. Bock, A. Bonaldi, L. Bonavera, J. R. Bond, J. Borrill, F. R. Bouchet, M. Bucher, C. Burigana, R. C. Butler, E. Calabrese, J. -F. Cardoso, B. Casaponsa, A. Catalano, A. Challinor, A. Chamballu, H. C. Chiang, P. R. Christensen, S. Church, D. L. Clements, S. Colombi, L. P. L. Colombo, C. Combet, F. Couchot, A. Coulais, B. P. Crill, A. Curto, F. Cuttaia, L. Danese, R. D. Davies, R. J. Davis, P. de Bernardis, A. de Rosa, G. de Zotti, J. Delabrouille, F. -X. Dsert, J. M. Diego, H. Dole, S. Donzelli, O. Dor, M. Douspis, A. Ducout, X. Dupac, G. Efstathiou, F. Elsner, T. A. Enlin, H. K. Eriksen, J. Fergusson, R. Fernandez-Cobos, F. Finelli, O. Forni, M. Frailis, A. A. Fraisse, E. Franceschi, A. Frejsel, S. Galeotta, S. Galli, K. Ganga, R. T. Gnova-Santos, M. Giard, Y. Giraud-Hraud, E. Gjerlw, J. Gonzlez-Nuevo, K. M. Grski, S. Gratton, A. Gregorio, A. Gruppuso, J. E. Gudmundsson, F. K. Hansen, D. Hanson, D. L. Harrison, S. Henrot-Versill, C. Hernndez-Monteagudo, D. Herranz, S. R. Hildebrandt, E. Hivon, M. Hobson, W. A. Holmes, A. Hornstrup, W. Hovest, K. M. Huffenberger, G. Hurier, S. Ili_, A. H. Jaffe, T. R. Jaffe, W. C. Jones, M. Juvela, E. Keihnen, R. Keskitalo, T. S. Kisner, R. Kneissl, J. Knoche, M. Kunz, H. Kurki-Suonio, G. Lagache, A. Lhteenmki, J. -M. Lamarre, M. Langer, A. Lasenby, M. Lattanzi, C. R. Lawrence, R. Leonardi, J. Lesgourgues, F. Levrier, M. Liguori, P. B. Lilje, M. Linden-Vrnle, M. Lpez-Caniego, P. M. Lubin, Y. -Z. Ma, J. F. Macas-Prez, G. Maggio, D. Maino, N. Mandolesi, A. Mangilli, A. Marcos-Caballero, M. Maris, P. G. Martin, E. Martnez-Gonzlez, S. Masi, S. Matarrese, P. McGehee, P. R. Meinhold, A. Melchiorri, L. Mendes, A. Mennella, M. Migliaccio, S. Mitra, M. -A. Miville-Deschnes, A. Moneti, L. Montier, G. Morgante, D. Mortlock, A. Moss, D. Munshi, J. A. Murphy, P. Naselsky, F. Nati, P. Natoli, C. B. Netterfield, H. U. Nrgaard-Nielsen, F. Noviello, D. Novikov, I. Novikov, C. A. Oxborrow, F. Paci, L. Pagano, F. Pajot, D. Paoletti, F. Pasian, G. Patanchon, O. Perdereau, L. Perotto, F. Perrotta, V. Pettorino, F. Piacentini, M. Piat, E. Pierpaoli, D. Pietrobon, S. Plaszczynski, E. Pointecouteau, G. Polenta, L. Popa, G. W. Pratt, G. Przeau, S. Prunet, J. -L. Puget, J. P. Rachen, W. T. Reach, R. Rebolo, M. Reinecke, M. Remazeilles, C. Renault, A. Renzi, I. Ristorcelli, G. Rocha, C. Rosset, M. Rossetti, G. Roudier, J. A. Rubio-Martn, B. Rusholme, M. Sandri, D. Santos, M. Savelainen, G. Savini, B. M. Schaefer, D. Scott, M. D. Seiffert, E. P. S. Shellard, L. D. Spencer, V. Stolyarov, R. Stompor, R. Sudiwala, R. Sunyaev, D. Sutton, A. -S. Suur-Uski, J. -F. Sygnet, J. A. Tauber, L. Terenzi, L. Toffolatti, M. Tomasi, M. Tristram, M. Tucci, J. Tuovinen, L. Valenziano, J. Valiviita, F. Van Tent, P. Vielva, F. Villa, L. A. Wade, B. D. Wandelt, I. K. Wehus, D. Yvon, A. Zacchei, A. Zonca
备注：
34 pages, 24 figures, abstract abridged for arXiv. This paper is one of a set associated with the 2015 data release from Planck. Final version, accepted for publication in A&A
This paper presents a study of the ISW effect from the Planck 2015 temperature and polarization data release. The CMB is cross-correlated with different LSS tracers: the NVSS, SDSS and WISE catalogues, and the Planck 2015 lensing map. This cross-correlation yields a detection at $4\,σ$, where most of the signal-to-noise is due to the Planck lensing and NVSS. In fact, the ISW effect is detected only from the Planck data (through the ISW-lensing bispectrum) at $\approx 3\,σ$, which is similar to the detection level achieved by combining the cross-correlation signal coming from all the catalogues. The ISW signal allow us to detect $Ω_Λ$ at more than $3\,σ$. This cross-correlation analysis is performed only with the Planck temperature data, since the polarization scales available in the 2015 release do not permit significant improvement of the CMB-LSS cross-correlation detectability. Nevertheless, polarization data is used to study the anomalously large ISW signal previously reported through the stacking of CMB features at the locations of known superstructures. We find that the current Planck polarization data do not exclude that this signal could be caused by the ISW effect. In addition, the stacking of the Planck lensing map on the locations of superstructures exhibits a positive cross-correlation with these large-scale structures. Finally, we have improved our previous reconstruction of the ISW temperature fluctuations by combining the information encoded in all the previously mentioned LSS tracers. In particular, we construct a map of the ISW secondary anisotropies and the corresponding uncertainties map, obtained from simulations. We also explore the reconstruction of the ISW anisotropies caused by the LSS traced by the 2MPZ survey by directly inverting the density field into the gravitational potential field.
Integrated Sachs Wolfe Effect and Rees Sciama Effect
自R. K. Sachs和A. M. Wolfe预言了宇宙微波背景（CMB）中各向异性的存在，并且自10年前首次观测到积分萨克斯-沃尔夫效应（ISW）以来。ISW效应为我们提供了一个独特的宇宙加速膨胀的探测器。大尺度结构与CMB之间的互相关是从数据中提取ISW效应的最有前途的方法。在这篇文章中，我们回顾了ISW效应的物理学，并总结了最近的观测结果和解释。
We show in detail that the recently derived expression for evaluating the integrated Sachs-Wolfe (ISW) temperature shift in the cosmic microwave background (CMB) caused by individual embedded (compensated) lenses is equivalent to the conventional approach for flat background cosmologies. The conventional approach requires evaluating an integral of the time derivative of the lensing potential, whereas the new Fermat potential approach is simpler and only requires taking a derivative of the potential part of the time delay.
Impact of a causal primordial magnetic field on the Sachs Wolfe Effect
我们提出了一个分析推导的萨克斯沃尔夫效应的原始磁场，产生的因果过程，如一阶相变在早期宇宙。至于拓扑缺陷的情况下，我们应用广义相对论结的条件，以匹配的扰动变量之前和之后的相变，在这样的方式，总能量动量张量是保守的过渡。我们发现，相关的贡献，磁萨克斯-沃尔夫效应来自次领先的大尺度极限的度量扰动。由于自由流中微子的存在，导致序项被强烈抑制。我们导出了中微子补偿效应，并证实了由因果磁场产生的磁性SachsWolfe谱的性质与最近的数值分析结果一致，为l（l+1）C_l^B ~ l ^2。
Large-angle fluctuations in the cosmic microwave background temperature induced by the integrated Sachs-Wolfe effect and Compton-y distortions from the thermal Sunyaev-Zeldovich (tSZ) effect are both due to line-of-sight density perturbations. Here we calculate the cross-correlation between these two signals. Measurement of this cross-correlation can be used to test the redshift distribution of the tSZ distortion, which has implications for the redshift at which astrophysical processes in clusters begin to operate. We also evaluate the detectability of a yT cross-correlation from exotic early-…
Consistency relations of large-scale structures provide exact nonperturbative results for cross-correlations of cosmic fields in the squeezed limit. They only depend on the equivalence principle and the assumption of Gaussian initial conditions, and remain nonzero at equal times for cross-correlations of density fields with velocity or momentum fields, or with the time derivative of density fields. We show how to apply these relations to observational probes that involve the integrated Sachs-Wolfe effect or the kinematic Sunyaev-Zeldovich effect. In the squeezed limit, this allows us to expres…
The paper discusses ISW estimates through EMU-ASKAP survey. The main ideas this paper covers include: 1- Discussion on source distribution, confusion, position accuracy and shotnoise (with discussion focusing on SN ratios). 2- Selection of maximum redshift and maximum 'l' ranges in relation with SN ratios. Note: Complete abstract is available in the document.
In this study, we are going to discuss the accelerated expansion of the universe and how this accelerated expansion affects the paths of photons from cosmic microwave background radiation (CMB). Then we will see how wide-field galaxy surveys along with cosmic CMB anisotropy maps can help us in studying dark energy. The cross-correlation of galaxy over/under-density maps with CMB anisotropy maps help us in measuring one of the most useful signatures of dark energy i.e. Integrated Sachs-Wolfe (ISW) effect. ISW effect explains the blue-shifting and red-shifting of CMB photons when they reach to u…
We present a new method for detection of the integrated Sachs-Wolfe (ISW) imprints of cosmic superstructures on the cosmic microwave background, based on a matched filtering approach. The expected signal-to-noise ratio for this method is comparable to that obtained from the full cross-correlation, and unlike other stacked filtering techniques it is not subject to an a posteriori bias. We apply this method to Planck CMB data using voids and superclusters identified in the CMASS galaxy data from the Sloan Digital Sky Survey Data Release 12, and measure the ISW amplitude to be $A_\mathrm{ISW}=1.6…
We present the first calculation of the cross-correlation between three-dimensional cosmic shear and the integrated Sachs-Wolfe (iSW) effect. Both signals are combined in a single formalism, which permits the computation of the full covariance matrix. In order to avoid the uncertainties presented by the non-linear evolution of the matter power spectrum and intrinsic alignments of galaxies, our analysis is restricted to large scales, i.e. multipoles below l=1000. We demonstrate in a Fisher analysis that this reduction compared to other studies of three-dimensional weak lensing extending to smal…
The evolution of the gravitational potentials on large scales due to the accelerated expansion of the Universe is an important and independent probe of dark energy, known as the integrated Sachs-Wolfe (ISW) effect. We measure this ISW effect through cross-correlating the cosmic microwave background maps from the Planck satellite with a radio continuum galaxy distribution map from the recent Rapid ASKAP Continuum Survey (RACS). We detect a positive cross-correlation at $\sim 2.8\,σ$ relative to the null hypothesis of no correlation. We parameterise the strength of the ISW effect through an ampl…
The recent AvERA cosmological simulation of Rácz et al. (2017) has a $Λ\mathrm{CDM}$-like 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 $Λ\mathrm{CDM}$. 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, a…
The Integrated Sachs-Wolfe Signal from BOSS Super-Structures
宇宙结构通过综合的萨克斯-沃尔夫效应在微波背景辐射上留下印记。我们使用SDSS-III重子声学振荡巡天在红移0.43 < z < 0.65处构造了线性信号的模板图。我们在97%的置信水平下验证了这张图在普朗克CMB温度图上的印记，并与密度-温度互相关测量结果一致。使用这个ISW重建作为模板，我们调查的存在下，ISW源，并进一步研究的Granett-Neyrinck-Szapudi超空和超星系团目录的属性。我们首次对这些结构的三维密度分布进行了研究，并证明它们是重要的结构。模型拟合表明，超空是沿着视线拉长，我们建议，这种特殊的取向可以挑选出来的光度红移空间中的空洞发现算法。我们从公开的空洞和星团星表中测量了普朗克图中的平均温度分布。在试图最大限度地堆叠ISW信号，我们构建了一个新的目录的超级结构的基础上，当地的高峰和低谷的引力势。然而，我们没有发现这些结构和CMB温度之间的显着相关性。
One of the physical features of a dark-energy-dominated universe is the integrated Sachs-Wolfe (ISW) effect on the cosmic microwave background (CMB) radiation, which gives us a direct observational window to detect and study dark energy. The AllWISE data release of the Wide-field Infrared Survey Explorer (WISE) has a large number of point sources, which span over a wide redshift range including where the ISW effect is maximized. AllWISE data is thus very well-suited for the ISW effect studies. In this study, we cross-correlate AllWISE galaxy and active galactic nucleus (AGN) overdensities with…
We obtain the non-linear generalization of the Sachs-Wolfe + integrated Sachs-Wolfe (ISW) formula describing the CMB temperature anisotropies. Our formula is valid at all orders in perturbation theory, is also valid in all gauges and includes scalar, vector and tensor modes. A direct consequence of our results is that the maps of the logarithmic temperature anisotropies are much cleaner than the usual CMB maps, because they automatically remove many secondary anisotropies. This can for instance, facilitate the search for primordial non-Gaussianity in future works. It also disentangles the non-…
The integrated Sachs-Wolfe (ISW) effect is caused by the decay of cosmological gravitational potential, and is therefore a unique probe of dark energy. However, its robust detection is still problematic. Various tensions between different data sets, different large scale structure (LSS) tracers, and between data and the $Λ$CDM theory prediction, exist. We propose a novel method of ISW measurement by cross correlating CMB and the LSS traced by "low-density-position" (LDP, \citet{2019ApJ...874....7D}). It isolates the ISW effect generated by low-density regions of the universe, but insensitive t…
We re-analyse the cosmic microwave background (CMB) Cold Spot (CS) anomaly with particular focus on understanding the bias a mask (contaminated by Galactic and point sources) may introduce. We measure the coldest spot, found by applying the Spherical Mexican Hat Wavelet transform on 100 000 cut-sky (masked) and full-sky CMB simulated maps. The CS itself is barely affected by the mask; we estimate a 94 per cent probability that the CS is the full-sky temperature minimum. However, approximately 48 per cent (masked fraction of the mask) of full-sky minima are obscured by the mask. Since the obser…
In this paper, we estimate the cross-correlation power spectra between the Planck 2018 cosmic microwave background (CMB) temperature anisotropy map and the unresolved $γ$-ray background (UGRB) from the 9-years Fermi-Large Area Telescope (LAT) data. In this analysis, we use up to nine energy bins over a wide energy range of [0.631, 1000] GeV from the Fermi-LAT UGRB data. Firstly, we find that the Fermi data with the energy ranges [1.202, 2.290] GeV and [17.38, 36.31] GeV show the positive evidence for the Integrated Sachs-Wolfe (ISW) effect at $1.8σ$ confidence level, and the significance would…
The decay of gravitational potentials in the presence of dark energy leads to an additional, late-time contribution to anisotropies in the cosmic microwave background (CMB) at large angular scales. The imprint of this so-called integrated Sachs-Wolfe (ISW) effect to the CMB angular power spectrum has been detected and studied in detail, but reconstructing its spatial contributions to the CMB $\textit{map}$, which would offer the tantalizing possibility of separating the early- from the late-time contributions to CMB temperature fluctuations, is more challenging. Here we study the technique for…
We use the cross-correlation power spectrum of the integrated Sachs-Wolfe (ISW) effect in the cosmic microwave background (CMB) temperature anisotropy and galaxy fluctuations to probe the physics of late-time cosmic acceleration. For this purpose, we focus on three models of dark energy that belong to a sub-class of Horndeski theories with the speed of gravity equivalent to that of light: Galileon Ghost Condensate (GGC), Generalized Cubic Covariant Galileon (GCCG), and K-mouflage. In the GGC and GCCG models, the existence of cubic-order scalar self-interactions allows a possibility for realizi…
We present full-sky maps of the Integrated Sachs-Wolfe effect (ISW) for the MICE Grand Challenge lightcone simulation up to redshift 1.4. The maps are constructed in the linear regime using spherical Bessel transforms. We compare and contrast this procedure against analytical approximations found in the literature. By computing the ISW in the linear regime, we remove the substantial computing and storage resources required to calculate the non-linear Rees-Sciama effect. Since the linear ISW at low redshift $z\leq1$, at large angular scales, and after matter domination is $\sim 10^{2}\times$ la…
在本文中，我们依靠的类星体（QSO）的斯隆数字巡天数据发布六（SDSS DR 6）的约100万光度选择类星体的目录计算积分萨克斯-沃尔夫（ISW）效应在高红移，旨在约束的行为的膨胀率，从而在这些时期的暗能量的行为。这个独特的样本显着扩展了以前的目录，以更高的红移，同时保持高效率的选择算法。我们计算了类星体数密度的自关联函数（ACF），从中提取了偏差和恒星污染。然后我们计算了不同子样本中类星体数密度和宇宙微波背景（CMB）温度涨落之间的互相关联函数（CCF）：在高z>1.5和低z<1.5的红移下，对两种不同的类星体选择进行了保守和更投机的分析。我们发现了在2.7σ水平上不为零的互相关性的总体证据，而该证据在z>1.5时下降到1.5σ。我们专注于ISW的能力，以约束在高红移的暗能量分量的行为在\LambdaCDM和早期的暗能量宇宙学，当暗能量基本上不受观测。目前，包括ISW数据的结果在一个穷人的改善相比，从其他宇宙学数据集获得的约束。我们研究了未来高红移类星体巡天的能力，发现ISW信号可以改善普朗克CMB数据中最重要的宇宙学参数的约束，包括高红移暗能量丰度，改善因子为\sim 1.5。
The late integrated Sachs-Wolfe (ISW) effect correlates the Cosmic Microwave Background (CMB) temperature anisotropies with foreground cosmic large-scale structures. As the correlation depends crucially on the growth history in the era of dark energy, it is a key observational probe for constraining the cosmological model. Here we present a detailed study based on full-sky and deep light cones generated from very large volume numerical N-body simulations, which allow us to avoid the use of standard replica techniques, while capturing the entirety of the late ISW effect on the large scales. We …
CMB temperature anisotropy at large scales induced by a causal primordial magnetic field
我们提出了一个由原始磁场的萨克斯沃尔夫效应的解析推导。为了一致地指定初始条件，我们假设磁场是由因果过程产生的，即在早期宇宙中的一阶相变。对于拓扑缺陷的情况，我们应用广义相对论结条件来匹配产生磁场的相变之前和之后的微扰变量，以这样的方式，总能量动量张量在整个过渡中守恒，并且满足爱因斯坦方程。我们进一步解析地求解了包含中微子的大尺度下的度规和流体扰动的演化方程，并导出了磁性Sachs Wolfe效应。我们发现，相关的贡献，磁萨克斯-沃尔夫效应来自次领先的大尺度极限的度量扰动。事实上，由于自由流中微子的存在，首阶项被强烈抑制。我们动态地导出了中微子补偿效应，证实了由因果磁场产生的磁性SachsWolfe谱的性质为l（l+1）C_l^B \propto l ^2，这与最近的数值分析结果一致。
The cosmic microwave background (CMB) is sensitive to the recent phase of accelerated cosmic expansion through the late-time integrated Sachs-Wolfe (ISW) effect, which manifests as secondary temperature fluctuations on large angular scales. However, the large cosmic variance from primary CMB fluctuations limits the usefulness of this effect in constraining dark energy or modified gravity. In this paper, we propose a novel method to separate the ISW signal from the primary signal using gravitational lensing, based on the fact that the ISW signal is, to a good approximation, not gravitationally …
The largest structures in the cosmic web probe the dynamical nature of dark energy through their integrated Sachs-Wolfe imprints. In the strength of the signal, typical cosmic voids have shown good consistency with expectation $A_{\rm ISW}=ΔT^{\rm data} / ΔT^{\rm theory}=1$, given the substantial cosmic variance. Discordantly, large-scale hills in the gravitational potential, or supervoids, have shown excess signals. In this study, we mapped out 87 new supervoids in the total 5000 deg$^2$ footprint of the Dark Energy Survey at $0.2<z<0.9$ to probe these anomalous claims. We found an excess imp…
We derive updated constraints on the Integrated Sachs-Wolfe (ISW) effect through cross-correlation of the cosmic microwave background with galaxy surveys. We improve with respect to similar previous analyses in several ways. First, we use the most recent versions of extragalactic object catalogs: SDSS DR12 photometric redshift (photo-$z$) and 2MASS Photo-$z$ datasets, as well as employed earlier for ISW, SDSS QSO photo-$z$ and NVSS samples. Second, we use for the first time the WISE~$\times$~SuperCOSMOS catalog, which allows us to perform an all-sky analysis of the ISW up to $z\sim0.4$. Third,…
Probing dark energy evolution with Quaia quasars through the integrated Sachs-Wolfe effect
MTA–CSFK Lendület “Momentum” Large-Scale Structure (LSS) Research Group（MTA-CSFK 伦杜莱特“动量”大尺度结构研究组）；Konkoly Observatory, HUN-REN Research Centre for Astronomy and Earth Sciences（孔科利天文台，匈牙利研究与教育网络天文学与地球科学研究中心）；Institute of Physics and Astronomy, ELTE Eötvös Loránd University（罗兰大学物理与天文学研究所）；Institute for Astronomy, University of Hawaii（夏威夷大学天文学研究所）
