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 Issue A&A Volume 557, September 2013 A32 15 Cosmology (including clusters of galaxies) https://doi.org/10.1051/0004-6361/201219793 20 August 2013

## 1. Introduction

In recent years, cosmological observations (Larson et al. 2011; Percival et al. 2007; Schrabback et al. 2010) have lead to the establishment of a standard cosmological model. This model assumes an inflationary scenario leading to Gaussian features in the temperature anisotropies of the cosmic microwave background (CMB). Since the advent of the COsmic Background Explorer (COBE, Bennett et al. 1990) and Wilkinson Microwave Anisotropy Probe (WMAP, Spergel et al. 2003) several signatures of lack of statistical isotropy, or “anomalies”, have been reported on large scales.

On the largest scales, a low quadrupole was reported with COBE data (Hinshaw et al. 1996; Bond et al. 1998) and later confirmed with WMAP data (Spergel et al. 2003), suggesting that it was not due to Galactic emissions. The octopole presented an unusual planarity and a correlation with the quadrupole (Tegmark et al. 2003; de Oliveira-Costa et al. 2004; Slosar & Seljak 2004; Copi et al. 2010). Other anomalies include a north/south power asymmetry (Eriksen et al. 2004; Bernui et al. 2006), an anomalous “cold spot” in the CMB (Vielva et al. 2004; Cruz et al. 2005, 2006), alignments of other large-scale multipoles (Schwarz et al. 2004; Copi et al. 2006), the so-called Axis of Evil (Land & Magueijo 2005a), and other violations of statistical isotropy (Hajian & Souradeep 2003; Land & Magueijo 2005b).

If confirmed, these anomalies could provide a new window into exotic early-Universe physics. However, there is much debate about the possible causes of these claimed anomalies. The statistics used to detect them are often subtle, and given the large cosmic variance on the scales considered, the anomalies could be due to a simple statistical fluke or in fact not be anomalous (Bennett et al. 2011, 2012; Efstathiou et al. 2010; Gold et al. 2011), depending on how the significance is measured.

The anomalies could also have a low-redshift cosmological origin. Since statistical isotropy is predicted for the early Universe, analyses should focus on the primordial CMB, i.e. one from which secondary low-redshift cosmological signals have been removed. This should be done whether or not one believes the significance of the reported anomalies in the CMB.

Peiris & Smith (2010) investigated the kinetic Sunyaev-Zeldovich (kSZ) effect, a known secondary anisotropy, and found it was unlikely that the kSZ effect was the origin of these anomalies. On the largest scales, the only secondary anisotropy is the integrated Sachs-Wolfe (ISW) effect, which is correlated with foreground large-scale structure (SS). A first study by Rudnick et al. (2007) detected a cold spot in the NRAO VLA Sky Survey (NVSS), similar to that found in WMAP data, suggesting that the WMAP cold spot could be due to the late ISW effect. However, Smith & Huterer (2010) showed that the cold spot in the NVSS was no longer significant when systematics were taken into account, and Granett et al. (2009, 2010) rule out that the cold spot be due to a supervoid. Recently, Yershov et al. (2012) found a correlation between the spatial distribution of supernovae and the CMB, which they claim could be due to dust contribution, ionised gas, or the ISW effect.

Francis & Peacock (2010, hereafter FP10) investigated the impact of the ISW field due to 2 Micron All-Sky Survey (2MASS) galaxies on several CMB anomalies: the low quadrupole, the quadrupole/octopole alignment, the planarity of the octopole, the north/south asymmetry and the cold spot. They found that the first two of these anomalies were reduced in significance after the removal of the foreground signal, but that the octopole planarity was actually increased. The north/south asymmetry was somewhat reduced and the cold spot remained anomalous.

The study of these large-scale anomalies is extremely sensitive to the treatment of the Galactic mask to account for foreground removals (Bernui et al. 2006; Slosar & Seljak 2004; Bennett et al. 2012) in both the CMB and galaxy survey data used to reconstruct the ISW field, hence a statistically un-biased method for dealing with missing data should be used. Regarding the CMB, Bennett et al. (2012) found that the limiting factor in measuring the quadrupole/octopole alignment was foreground removal. Regarding the LSS side, FP10 reconstructed missing data by first filling the masked region with a random Poisson sampling of galaxies with the same average number density as outside the mask and then applying a Wiener filter, which is optimal for Gaussian data. Kim et al. (2012) investigated methods to reconstruct CMB data in masked regions using a Gaussian-constrained harmonic inpainting method. They found that the quadrupole/octopole alignment in CMB maps was increased after inpainting treatment. Both methods assume Gaussianity of the underlying maps, which is a limitation in the context of search for statistical anisotropy. The filling of the masked region with random galaxies may also cause an artificial quadrupole since the Galactic mask has the shape of a quadrupole.

In this paper, we investigate the use of sparse inpainting (see Abrial et al. 2008 and Starck et al. 2010, hereafter A08-SMF10) on CMB (WMAP) and LSS maps (2MASS and NVSS) in the context of probing large-scale anomalies in the CMB. The sparse inpainting does not assume that the true underlying map is Gaussian, or statistically isotropic. We reconstruct a full-sky tomographic ISW map due to 2MASS and NVSS galaxies. We test whether removing the ISW signal due to these LSS maps affects the observed large-scale anomalies in the CMB by focussing on the same three large-scale anomalies as FP10.

This paper updates the work presented in Francis & Peacock (2010) and Kim et al. (2012), with the following differences:

• 1.

Tomography: we reconstruct the ISW signal due to both2MASS (Jarrett et al. 2000) andNVSS (Condon et al. 1998) data.The data sets are described in Sect. 3.

• 2.

Trends: we look for trends by considering 11 different WMAP data sets, described in Sect. 3.

• 3.

Sparse inpainting: missing data in CMB and LSS maps are reconstructed using the sparse inpainting technique of A08-SMF10 and Starck et al. (2013), described in Sect. 4, which does not assume that the data is Gaussian or statistically isotropic.

• 4.

Tests for biases: we test that the sparse inpainting method neither introduce biases in statistical isotropy tests nor creates a spurious ISW signal in Sect. 4.1.

In Sect. 2 we present how it is possible to estimate the primordial CMB on large scales with knowledge of foreground LSS maps by reconstructing the ISW field. In Sect. 5, we investigate the effect of subtracting the ISW field due to 2MASS and NVSS galaxies on three previously reported large-scale anomalies: the low quadrupole, the quadrupole/octopole alignment and the octopole planarity. In Sect. 6, we present a discussion of our results.

## 2. Estimating the large-scale primordial CMB

### 2.1. The large-scale primordial CMB after subtraction of the integrated Sachs-Wolfe effect

The observed temperature anisotropies in the CMB, δOBS, can be described as the sum of several components: (1)where \begin{lxirformule}$\delta_{\rm prim}$\end{lxirformule} are the primordial temperature anisotropies, are the total secondary temperature anisotropies due to the ISW effect, δother are other secondary anisotropies (e.g., Sunyaev-Zeldovich effect), and is noise. Here, we assume that the observed data are clean of any foregrounds and that any regions requiring masking due to contaminated data will be corrected for during the sparse inpainting phase. On large scales, the ISW signal is the only secondary anisotropy and the anisotropies are cosmic variance limited, so that the last two terms can be ignored: (2)The ISW effect arises in universes where the cosmic potential decays at late times, as is the case with dark energy, open curvature, or possibly some modified gravities. The temperature anisotropies due to the ISW effect are given by: (3)where η is the conformal time, defined by , and η0 and ηL represent the conformal times today and at the surface of last scattering respectively. The unit vector is along the line of sight and the gravitational potential Φ(x) depends on position and time. The integral depends on the rate of change of the potential Φ′ = dΦ/dη. The potential field can be related to the matter field, of which a galaxy map is assumed to be a tracer.

By subtracting the reconstructed ISW signal, , due to the matter field traced by a foreground galaxy survey, we can estimate the large-scale primordial CMB temperature anisotropy field by: (4)where this relation tends to equality (on large scales) when the entire mass distribution of the Universe is used to reconstruct the ISW field, i.e. when .

In this paper, we estimate by subtracting the ISW temperature anisotropy field as reconstructed in Sect. 4 using 2MASS and NVSS data (see Sect. 3): (5)where the extra last term corresponds to the removal of the kinetic Doppler quadrupole (ignoring the monopole and dipole). The kinetic Doppler quadrupole contribution is given by: (6)where θ is the angle between the position on the sky and the direction of motion creating the kinetic Doppler quadrupole (Copi et al. 2006). For our calculations, we take v = 370  km   s-1 towards (l,b) = (263.85°,48.25°), and c is the speed of light, similarly to what is done in Francis & Peacock (2010). We make the kinetic Doppler quadrupole map in Healpix format as well as code to generate it available for download1.

Table 1

List of the 11 temperature anisotropy maps we use to probe the anomalies in the primoridal CMB, including year of WMAP data they correspond to and a description of the mask treatment.

### 2.2. The ISW temperature field from LSS maps

The temperature ISW field can be reconstructed in spherical harmonics, , from the LSS field gℓm (Boughn et al. 1998; Cabré et al. 2007; Giannantonio et al. 2008): (7)where gℓm represent the spherical harmonic coefficients of a galaxy overdensity field g(θ,φ), given by (8)where Yℓm(θ,φ) are the spherical harmonics. The spectra Cgg and CgT are the galaxy (g) and CMB (T) auto- and cross-correlations measured from the data or their theoretical values given by: where where we use the same notation as in Rassat et al. (2007) and have assumed a linear bias b(k,z) ≡ bg and D(z) is the linear growth function.

From Eq. (7), we can check that: (15)and (16)Equations (7) and (16) show that the ISW temperature field is independent of the galaxy bias bg, which relates the galaxy and matter (m) fluctuations by gℓm = bgδm,ℓm, and that it is not necessary to estimate the value of the galaxy bias in order to estimate the ISW temperature field.

We note that the above method is suitable for photometric surveys where a projected spherical harmonic decomposition is satisfactory. For spectroscopic surveys, a full three-dimensional reconstruction can be done in spherical Fourier-Bessel decomposition, as in Shapiro et al. (2012) and Rassat & Refregier (2012) for the theoretical calculations, and using a code such as 3DEX (Leistedt et al. 2012) for the measurements.

 Fig. 1WMAP ILC 9th year CMB data (top in mK), 2MASS data (middle), and NVSS data (bottom) with mask (left) and after sparse inpainting (right). Data in the right column is presented up to ℓ = 10 for all maps. The original 2MASS data (middle left) is plotted with a maximum overdensity value of 3 to increase contrast in the map. Open with DEXTER

## 3. Data

We are interested in reconstructing the temperature ISW fields due to 2MASS and NVSS data. We describe the CMB and LSS data we use in the following section, while the reconstruction is described in Sect. 4.

### 3.1. Cosmic microwave background data

For the CMB, we investigate data from several years of WMAP, including independent treatments of masked data. We do this to identify trends in the observed large-scale anomalies. We use 11 maps in total: the Tegmark et al. (2003) reduced-foreground CMB map (TOH); the Internal Linear Combination Map (ILC) WMAP data from the 3rd year (Hinshaw et al. 2007)2, 5th year (Gold et al. 2009)3, 7th year (Gold et al. 2011)4, and 9th year (Bennett et al. 2012)5 as well as sparsely inpainted versions of the ILC and TOH maps (see Sect. 4). We also include the sparsely inpainted WMAP 5th year ILC map by Delabrouille et al. (2009), which was reconstructed using a wavelet technique. We summarise the CMB maps used in Table 1. The ILC 9th year temperature overdensity map is shown with its corresponding mask6 in the left-hand side of Fig. 1 (top).

### 3.2. The 2 Micron all sky survey (2MASS) data

As a tracer of the low-redshift matter distribution, we use the publicly available 2MASS full-sky extended source catalogue (XSC) selected in the near IR (Jarrett et al. 2000), which has median redshift . The near-IR selection means galaxies are relatively well observed, even in the region of the Galactic plane. As a result, the 2MASS survey has a large sky coverage, which is ideal for studying the ISW effect, with . For exact details of our selection criteria and the mask, see Rassat et al. (2007) and Sect. 6.2 of Dupe et al. (2011). The 2MASS overdensity map is shown with its corresponding mask on the left-hand side of Fig. 1 (middle).

### 3.3. The NRAO VLA Sky Survey (NVSS) data

As a tracer of the intermediate redshift matter distribution, we use the publicly available NRAO VLA Sky Survey (NVSS), which has a median redshift . The NVSS survey is a 1.4 GHz (radio) continuum survey covering the sky north of δ =  −37°, in which most sources away from the Galactic plane are of extragalactic origin (Smith et al. 2007). We select only sources with flux larger than 2.5 mJy. For the mask we exclude the Galactic region with | b |  < 10° and also mask out a 0.6° radius around bright sources with flux larger than 2.5 Jy, as in Ho et al. (2008). The resulting mask gives us an effective sky fraction of .

In order to account for the problem of declination-dependent density, which NVSS data suffers from, we apply the same method as in Schiavon et al. (2012) and Vielva et al. (2006): the NVSS overdensity is calculated separately for nine declination bins with Δsin(δ) = 0.1.

Alternatives to the declination problem have been proposed, e.g. by considering only objects above 5 mJy (Barreiro et al. 2013) or including templates to project out the declination-striping modes (Ho et al. 2008). However, none of these methods satisfactorily solves a problem of missing power on large scales for NVSS (Hernández-Monteagudo 2010). The NVSS overdensity map is shown with its corresponding mask on the left-hand side of Fig. 1 (bottom).

## 4. Reconstruction of full-sky maps

Large-scale modes in the CMB and LSS fields are very sensitive to large coherent regions of missing data, such as those which are due to a Galactic mask. Therefore it is crucial to use a reconstruction method which does not introduce biases in the reconstructed field. To account for regions of missing data in CMB and LSS maps, we use sparse inpainting (A08-SMF10) to reconstruct regions of missing data (see also Appendix A in Dupe et al. 2011). The sparse inpainting approach is powerful as the only assumption it makes on the underlying field is sparse representation. In this particular case, the assumption is therefore that the CMB and LSS signals are sparsely represented in spherical harmonic space, i.e. only a few aℓms (not C()s) are required to describe the data. This is easily verified directly from the data and is described in more detail in Starck et al. (2013) and Dupe et al. (2011).

Sparse inpainting does not assume statistical isotropy or Gaussianity of the underlying field, unlike other methods such as Wiener filtering (used by Francis & Peacock 2010) or constrained Gaussian realisations (as used by Kim et al. 2012).

In Sect. 4.1, we test whether the sparse inpainting reconstruction might produce biases in measurements of statistical isotropy or a spurious ISW signal. In Sect. 4.2, we describe the details of the sparse inpainting reconstruction for the LSS and CMB maps and in Sect. 4.3, we describe how we use these to reconstruct full-sky ISW maps.

### 4.1. Sparse inpainting as a bias-free reconstruction method

In order to use the reconstructed maps to test large-scale anomalies in the CMB, we must first be confident that there are no spurious large-scale anomalies due to our reconstruction technique. The full details of the tests are given in Appendix A, and we highlight the main conclusions here.

We first test whether sparse inpainting affects the three anomalies we are testing in the CMB data (see Sect. 5 for the anomaly descriptions). We test this by considering two sets of Gaussian random field simulations of CMB data. The first set of simulations has a low quadrupole as theoretical input, and the second set has a WMAP7 best-fit theoretical quadrupole (see Eq. (17)). We test for the three anomalies for both sets of simulations before and after inpainting (Tables A.2, A.1). We also apply the same tests to Gaussian random field simulations of 2MASS and NVSS galaxy fields, using theoretical values of their spectra (including the galaxy bias, Tables A.3 and A.4).

We find that the sparse inpainting method applied to statistically isotropic CMB and LSS simulated data does not introduce any significant biases for any of the three tests of statistical isotropy. After inpainting, the quadrupole is slightly lower but only by 3%, whether considering the simulations with low quadrupole or theoretical quadrupole on input. The test of quadrupole/octopole alignment can be somewhat altered due to sparse inpainting (see the standard deviation on the bias). We show here that if the CMB and LSS fields are statistically isotropic, then sparse inpainting does not alter this.

Finally, we want to test whether sparse inpainting will alter in any way the reconstructed ISW temperature signal, either by creating a spurious ISW signal or biasing the tests of statistical isotropy. To do this, we first consider simulated NVSS maps with uncorrelated CMB maps (1st line of Table A.5). We test for cross-correlations before and after inpainting of the individual NVSS and CMB maps (which have different masks). Since the maps are statistically uncorrelated, we expect a null cross-correlation on average, which we find is the case before and after applying sparse inpainting. This shows that sparse inpainting does not introduce a spurious ISW or cross-correlation signal, confirming what we had found in Dupe et al. (2011).

We also test the quadrupole/octopole alignment and octopole planarity of the reconstructed ISW signal from NVSS galaxies before and after inpainting (again where the NVSS and CMB maps are inpainting separately with different masks, see Table A.5) and find that the tests are unbiased after sparse inpainting.

We note that it would, of course, be interesting to know whether sparse inpainting is also unbiased in the case of statistically anisotropic fields, for example, the case where the CMB really does have anomalies before sparse inpainting is applied. However to do this, one would first have to decide on the models causing the anomalies (exotic physics, foregrounds, etc...) in order to test realistic statistical anisotropy. In this paper, we focus only on finding out if sparse inpainting creates spurious statistically anisotropic signatures in data where the true distribution is statistically isotropic.

### 4.2. Full-sky CMB and LSS maps

We describe here the details for the sparse inpainting reconstruction for the CMB, 2MASS and NVSS data. Our goal is to reconstruct the quadrupole and octopole only ( = 2,3), since we are only interested in anomalies on the largest scales. However, due to mode correlations induced by the masked data, we must consider multipoles larger than  > 3 for the reconstruction.

For the 11 CMB maps we reconstruct the harmonic coefficients up to  = 64 using nside = 64 using the sparsity prior as described in Starck et al. (2013), i.e. using the following command line in the open-source sparse inpainting package ISAP software7: > alm = cmb_lowl_alm_inpainting(map, Mask, lmax=lmax, niter=100, InpMap=result).

For 2MASS data, we reconstruct the harmonic coefficients up to  = 64 using nside = 64 with the following command line in ISAP software7: > alm = cmb_lowl_alm_inpainting(t, Mask,lmax=lmax, niter=500, InpMap=result, /galaxy), where the keyword /galaxy was optimised for point source catalogues like galaxy surveys to take into account that the field does not have a zero mean.

For NVSS data, we reconstruct the harmonics up to  = 64 using nside = 128 and the same command line and options as for 2MASS. The WMAP 9th year ILC, 2MASS and NVSS maps are shown before (left) and after inpainting (right) in Fig. 1. The ten other CMB maps are also reconstructed in the same manner, but not plotted in Fig. 1.

 Fig. 2Quadrupole and octopole values (μK2) for the different CMB maps listed in Table 1. Points in black are with no extra treatment than that given in the literature, and points in red are after application of sparse inpainting. Open with DEXTER

In Fig. 2, we plot the measured quadrupole and octopole from all CMB maps listed in Table 1 before (black) and after (red) sparse inpainting. Apart from the TOH W1 map, the values of the quadrupole and octopole are similar across different WMAP years. After inpainting, both the quadrupole and octopole are lowered for all maps, with the TOH W1 map again having slightly different values than the other maps for the quadrupole.

The simulations in Appendix A show that inpainting on W7-like maps (i.e. with low quadrupole, C = 2 = 250.6    ±    161.0  μK2) introduces only a slight bias (7.2, i.e. about a 3% drop) on the quadrupole, so that we do not expect the drop in quadrupole value shown in Fig. 1 to be an artifact of inpainting.

 Fig. 3Redshift distributions for 2MASS (see Afshordi et al. 2004; Rassat et al. 2007; Dupe et al. 2011) and NVSS (from Ho et al. 2008). Open with DEXTER

Regarding the LSS data, we find that after reconstruction of the NVSS map the theoretical power spectrum as predicted from the redshift distribution of radio sources given by Ho et al. (2008) does not correspond well to the measured power spectrum, especially at higher multipoles (using their value of the galaxy bias bNVSS = 1.98), as already noted by Hernández-Monteagudo (2010). However, since we are focussing on very large angles only ( = 2,3), it is difficult to assess whether the theoretical spectrum needs to be revisited. For this work, we use the N(z) provided from Ho et al. (2008), which is only used in the NVSS simulations for testing sparse inpainting (Appendix A) and for the prediction of the value of quadrupole and octopole of the ISW due to NVSS data (Table 2 in Sect. 4.3). The actual reconstructed ISW map uses the measured auto- and cross-spectra (see the following Sect. 4.3) and is therefore independent of theory.

### 4.3. Full-sky ISW temperature maps

We reconstruct the full-sky ISW maps due to 2MASS and NVSS data from their inpainted maps (Fig. 1), using Eq. (7). Since the redshift distribution of 2MASS and NVSS has little overlap (see Fig. 3), we calculate the total ISW signal simply by summing the ISW maps reconstructed from each survey individually.

Table 2

Amplitude of the ISW temperature quadrupole and octopole due to the 2MASS galaxy survey (left: as measured from data using inpainted WMAP 9 data for the CMB, and right: from theoretical calculations) and a Euclid-type survey (using theoretical spectra).

 Fig. 4Quadrupole and octopole values (μK2) for the different reconstructed ISW maps. The ISW maps are reconstructed from sparsely inpainted CMB and LSS maps using Eq. (7), where the auto- and cross-correlations are measured directly from the data. Small variations in the phases of different renditions of CMB maps can lead to negligible differences in the auto-correlation (see Fig. 2) and to larger differences in a cross-correlation with a second map. This in turn can result in larger variations in the amplitude of the ISW signal, explaining why the reconstructed ISW maps vary slightly more between CMB maps than the observed temperature power does. Open with DEXTER

We estimate the cross- and auto-correlations in Eq. (7) using data only with inpainted maps for both the LSS and CMB data. This has the advantage of assuming only the form of the ISW signal, but not its presence, i.e. in the absence of a correlation between the CMB and the LSS maps, the reconstructed ISW map would be zero. As mentioned in Sect. 2.2, no numerical knowledge of the linear bias is necessary in this case. This method also means there is an ISW map for each CMB map considered.

Quadrupole and octopole values for the reconstructed maps using WMAP 9 ILC inpainted map are reported in Table 2 and plotted for each CMB map in Fig. 4.

The theoretical values in Table 2 are calculated employing the N(z) used in Afshordi et al. (2004) and Rassat et al. (2007) for 2MASS data and Ho et al. (2008) for NVSS data. They also require the assumption of a fiducial cosmological model, for which we assume a “vanilla” model, not a specific best-fit value, given that we are considering several CMB maps. The vanilla model we chose has the following cosmological parameters: Ωm = 0.25,Ωb = 0.045, ΩDE = 0.75, w0 =  −1,wa = 0,ns = 1,h = 0.7,σ8 = 0.80, i.e. a flat universe without massive neutrinos.

The theoretical values in Table 2 are calculated using the exact formulae (not the Limber approximation). The error bars due to cosmic variance are calculated using , and .

For comparison, we also indicate the expected value of the ISW map from Euclid data (Laureijs et al. 2011; Refregier et al. 2010). We predict this by considering a galaxy survey with median redshift and a Smail-type redshift distribution with α = 2 = 1.5 (see for e.g. Eq. (19) in Kirk et al. 2012) and fsky = 0.48. We calculate the expected ISW signal assuming a single large redshift bin.

Figure 4 shows the quadrupole and octopole power for the six reconstructed ISW maps (we only consider inpainted maps for the ISW reconstruction). The ISW quadrupole varies from 37.8 − 41.9  μK2 (except for TOH, which returns a significantly smaller quadrupole of 23.2  μK2, as shown in Fig. 4), while the octopole varies from 13.4 − 20.6  μK2, depending on the WMAP inpainted data used. Since each map is estimated from the cross-correlation of the reconstructed LSS maps with the corresponding reconstructed CMB map, this may explain the larger variation in Fig. 4 than in Fig. 2. This is because a small phase change may not change the auto-correlation (as in Fig. 2), but can lead to larger variations in cross-correlations with another map. This in turn can lead to larger variations in the amplitude of the ISW signal.

In our analysis, we chose to use all six reconstructed ISW maps, because each reconstructed ISW map is self-consistently produced, i.e. without any assumption about the theoretical amplitude of the ISW signal. In addition, we are interested in identifying possible trends in the way subtraction of the ISW signal affects the CMB anomalies, which will provide a stronger case for any conclusions.

Finally, Fig. 5 shows the reconstructed ISW temperature maps due to 2MASS galaxies (top) and NVSS galaxies (middle) where the CMB map is the W7 inpainted data. Only the quadrupole (left) and octopole (right) are shown, since we are interested in probing large-scale anomalies at  = 2 and  = 3.

The quadrupole and octopole of the ISW map due to 2MASS galaxies can be compared with those obtained by Francis & Peacock (2010, top of their Fig. 3). The main difference is that our reconstructed quadrupole is much less planar. This may be due to the difference in reconstruction of missing data. Francis & Peacock (2010) reconstructed missing data by first filling the masked region with a random Poisson sampling of galaxies with the same average number density as outside the mask. However, this can cause an artificial quadrupole, since the Galactic mask has the shape of a quadrupole.

 Fig. 5Quadrupole (left) and octopole (right) of the reconstructed ISW map for 2MASS (top) and NVSS (middle) and both NVSS and 2MASS together (bottom). The quadrupole and octopole of the ISW map due to 2MASS galaxies can be compared with that obtained by Francis & Peacock (2010, top of their Fig. 3). Maps are shown in units of μK. Open with DEXTER

## 5. Probing anomalies in the observed and primordial CMB

The main goal of this paper is to test whether reported large-scale anomalies in the observed CMB are still present in the primordial CMB, which we estimate by subtracting the ISW signal. Since the estimation of the ISW signal requires sparse inpainting of all CMB and LSS maps to account for regions of missing data, we can also test whether reported large-scale anomalies persist in the observed CMB after inpainting.

We investigate three large-scale anomalies in the CMB, which are the same as those investigated in Francis & Peacock (2010). In Sect. 5.1, we consider the impact on the low quadupole power, in Sect. 5.2 the alignment of the quadrupole and octopole, and in Sect. 5.3 the planarity of the octopole.

Table 3

Quadrupole ( = 2) power and corresponding probability of the quadrupole power being so low.

The low power of the quadrupole was first reported for COBE data (Bennett et al. 1992; Bond et al. 1998; Hinshaw et al. 1996) and subsequently observed in WMAP data (Spergel et al. 2003). Depending on how the significance of the low quadrupole is measured, recent WMAP papers now argue that there is no anomaly in the amplitude of the quadrupole (Bennett et al. 2011, 2012). However, we are still interested in studying how the amplitude of the quadrupole behaves after sparse inpainting and after subtraction of the reconstructed ISW field.

The values of the quadrupole before subtraction of the ISW field are reported in the top part of Table 3 [labelled “1)” and “2)”] before and after sparse inpainting. The third column of Table 3 gives the probability8 for a χ2 random variable with 5 degrees of freedom to take a value less than or equal to the WMAP9 (Bennett et al. 2012) expected theoretical (TH) value: (17)The inpainted maps, which were shown not to introduce a bias in the quadrupole reconstruction (see Sect. 4 and Appendix A), have lower quadrupole values than the input maps. This means that the application of inpainting for the CMB reconstruction actually increases the significance of the low quadrupole anomaly for all considered CMB maps.

The third part of Table 3 [labelled “3)”] shows the measured quadrupole power and probability after subtraction of the ISW reconstructed map due to 2MASS and NVSS galaxies. The last column shows the new expected theoretical value of the CMB quadrupole, given by: (18)the values for and are given by the values in Table 2 for the combined NVSS + 2MASS case. These values are compared with those calculated in FP10 [labelled “4)”] of Table 3.

After ISW subtraction, the quadrupole power decreases for all CMB maps (from 102.1 − 124.7  μK2 to 60.7 − 81.7  μK2, omitting TOH, which has a much larger quadrupole value than all the other maps after inpainting), but since the expected theoretical value also decreases there is nearly no change in the significance of the anomalies before or after ISW subtraction.

We note that the WMAP9 team uses a different approach to measuring the significance of the low quadrupole (Bennett et al. 2012). In any case, our study shows that there is no change in the signifiance of the low quadrupole value after ISW subtraction.

 Fig. 6Quadrupole (left) and octopole (right) of WMAP 9 data before inpainting (top), after sparse inpainting (middle), and after subtraction of the reconstructed ISW signal due to 2MASS and NVSS galaxies (bottom). Open with DEXTER

Table 4

Scalar product of the preferred axes of the quadrupole and octopole (), its corresponding separation (°), and the probability (%) of having such a low separation.

It was first noted by de Oliveira-Costa et al. (2004) that not only did the CMB quadrupole and octopole both appear planar (i.e. the dominant mode was m = ), they also seemed aligned along a similar axis. For a Gaussian random field there is no reason for the preferred axes of two different multipoles to be correlated. For each multipole, this preferred axis can be quantified by maximising the quantity (19)where corresponds to the aℓm coefficients of the rotated CMB temperature anisotropy map, where corresponds to the new z-axis, and is best calculated with at least nside = 512. The axes and correspond to the preferred axes (i.e. where is largest) for  = 2 and  = 3 respectively. We note that this way of measuring the quadrupole/octopole alignment differs from that used by Bennett et al. (2011, 2012), who maximize the quantity: (20)Bennett et al. (2012) found that the limiting factor in measuring the quadrupole/octopole alignment was foreground removal and treatment of the Galactic mask. This motivated us to investigate how the measured quadrupole/octopole behaves after sparse inpainting.

In the top part of Table 4, we present the dot product of the preferred axes for  = 2,3 for each CMB map before and after sparse inpainting and before and after ISW subtraction, as well as their corresponding separation (note the maximum separation is 90° since the axes are not vectors). We also note the probability of having such a separation in a Gaussian random field, which we estimate using the fact that the dot product of the two vectors has a uniform distribution (de Oliveira-Costa et al. 2004). Finally, we compare this with the effect found by FP10 using their 2MASS-ISW reconstruction subtracted from the ILC W3 map (last line of Table 4).

For non-inpainted maps, the separation varies from 2.3−9.7°, i.e. probabilities ranging from 0.08% to 1.4%. The same CMB maps, when inpainted, are less anomalous with separations ranging from 10.6−17.9°, corresponding to probabilities of 1.7−4.9%.

When the ISW field due to 2MASS and NVSS galaxies is removed, FP10 noted that the alignment was significantly reduced (see the last line in Table 4 or their Table 2 for more details). Using our reconstruction, we also find the alignment is reduced, though the change in significance is not as large as in FP10. We note that we are removing the ISW from both 2MASS and NVSS galaxies, whereas FP10 only removed the ISW field due to 2MASS galaxies. Therefore, the general trend is that removing the ISW field reduces the anomalous alignment of the quadrupole and octopole.

Figure 6 shows the quadrupole (left) and octopole (right) for the specific case of WMAP9 data, before inpainting (top), after inpainting (middle) and after ISW subtraction (bottom). Inpainting reduces the power in both the WMAP9 quadrupole and octopole, as we had seen in Fig. 2. Before inpainting, the preferred axes are in the direction of (l,b) = ( − 124.1,58.1) and (− 122.3,62.9) for  = 2,3 respectively. After inpainting, these become (l,b) = ( − 134.5,54.8) and (− 110.8,57.7). After inpainting and subtraction of the ISW signal due to 2MASS and NVSS galaxies, the preferred axes become (l,b) = ( − 90.1,40.8) and (− 97.2,65.1) for  = 2,3 respectively. In other words, the quadrupole axis is the one which changes the most and which causes the anomaly to decrease since this anomaly measures the correlation between the preferred direction of both the quadrupole and the octopole. We find this trend is true for all maps considered, i.e. that it is the change to the quadrupole shape which is the main cause of the anomaly decrease, whether after sparse inpainting only or after ISW subtraction.

### 5.3. Planarity of the octopole

The third anomaly we investigate is the reported planarity of the CMB octopole, i.e. the fact that the phase m =  is preferred, which was first noted by de Oliveira-Costa et al. (2004). To quantify if the octopole is planar, de Oliveira-Costa et al. (2004) suggested measuring the quantity: (21)This quantity represents the ratio of the octopole power which is contained in the mode m =  = 3, i.e. it is a test of planarity. For a Gaussian random field, the distribution of power amongst modes should be random, and so there is no reason that the value of t should be close to 1.

In Table 5, we report values of the “t” statistic for CMB maps, before and after inpainting, and before and after ISW subtraction. The “t” value is calculated using nside = 128, and its corresponding probability is estimated using 1000 simulated Gaussian random fields with the same power as the map considered.

Before inpainting, the probability of having such planar octopoles ranges from 9.60−14.3%. de Oliveira-Costa et al. (2004) reported t = 0.94 and a probability around 7% using the TOH map, so we first note that later WMAP data are less anomalous than the first year. After inpainting, octopole planarity is reduced even further, with probabilities ranging from 13.6−26.1%. After ISW subtraction, FP10 had found that the octopole became even more planar. We find the opposite, i.e. that after ISW subtraction, there is no evidence for any octopole planarity. However, we keep in mind that even before ISW subtraction the significance of the octopole planarity was not particularly high.

Table 5

The “t” value for the octopole as defined in de Oliveira-Costa et al. (2004) using nside = 128, calculated from the observed CMB maps (top) and after subtraction of the ISW field due to 2MASS and NVSS galaxies (middle).

Table 6

Summary of results in this paper.

Table 7

List of products made available in this paper in the spirit of reproducible research.

## 6. Discussion

Although there is currently a debate over the significance of the claimed large-scale anomalies in the CMB (see e.g., Bennett et al. 2011), their existence is not totally dismissed. In parallel to the debate on the statistical significance of the anomalies, recent work has also focussed on the impact of the reconstruction method to account for masked regions of the sky (e.g., Bernui et al. 2006; Slosar & Seljak 2004; Kim et al. 2012). Moreover, in some cases the Galactic mask is a limiting factor in the study of anomalies (Bennett et al. 2012). Studies have also focussed on low-redshift cosmology and astrophysics as potential sources of contamination (Rudnick et al. 2007; Peiris & Smith 2010; Francis & Peacock 2010; Yershov et al. 2012). Since statistical isotropy is predicted for the early Universe, analyses should focus on the primordial CMB, i.e. one from which secondary low-redshift cosmological signals have been removed. This should be done whether or not one believes the significance of the reported anomalies in the CMB.

In this paper, we focus simultaneously on both the reconstruction method and the ISW effect as a means to estimate the primoridal CMB and test it for anomalies. We focus on three previously reported large-scale anomalies, namely: the low quadrupole power, the quadrupole/octopole alignment, and the octopole planarity.

This work updates that of Francis & Peacock (2010) and Kim et al. (2012) in the following ways:

• 1.

Tomography: we reconstruct the ISW signal due to both2MASS (Jarrett et al. 2000) andNVSS (Condon et al. 1998) data(see Sect. 3).

• 2.

Trends: we look for trends by considering 11 different WMAP data sets (see Sect. 3), including 6 data sets for which we reconstructed missing data using the sparse inpainting technique mentioned below.

• 3.

Sparse inpainting: missing data in CMB and LSS maps are reconstructed using sparse inpainting (see Sect. 4, A08-SMF10), which does not assume the data are Gaussian or statistically isotropic.

• 4.

Tests for biases: we show in Sect. 4 and Appendix A that the sparse inpainting method used is a bias-free reconstruction, which does not introduce a spurious statistical anisotropies nor a spurious ISW signal.

In this work we first investigate the impact of our bias-free sparse inpainting on various CMB maps and on the claimed CMB anomalies. We then subtract the ISW signal reconstructed in Sect. 4 and test again for impact on the three studied anomalies. Our main conclusions are made by identifying trends amongst the 11 CMB maps considered.

Our conclusions are summarised in Table 6, namely:

• The low quadrupole becomes more anomalous after sparseinpainting of CMB maps, and remains so after additionalsubtraction of the ISW signal, contrarily to what Francis &Peacock (2010) (who used a differentreconstruction method) found.

• The quadrupole/octopole alignment becomes less anomalous after sparse inpainting of the CMB maps, contrary to what was reported by Kim et al. (2012), who used a Gaussian constrained inpainting method.

• The quadrupole/octopole alignment anomalies are reduced in significance after subtraction of the ISW signal, similarly to what was reported by Francis & Peacock (2010).

• We note that the reduced significance of the quadrupole/ octopole alignment (both after sparse inpainting and ISW subtraction) is mainly due to changes in the quadrupole shape, not the octopole, suggesting that the main source of both anomalies could be the quadrupole.

• We find that after inpainting and ISW subtraction, the octopole planarity becomes less anomalous, contrary to the report of Francis & Peacock (2010) who found the octopole planarity had become more anomalous after ISW subtraction. We also note that the octopole planarity did not seem significant in any CMB map subsequent to the first year WMAP data.

We therefore conclude that after application of sparse inpainting and subtraction of the ISW signal due to the low-redshift Universe out to z ~ 1, as estimated from the 2MASS and NVSS surveys, that the quadrupole/octopole alignment and the octopole planarity appear less significant. In addition, it seems that both of these previously reported anomalies could be in fact due to the quadrupole only. Other hypotheses remain possible (e.g. exotic physics).

In the spirit of participating in reproducible research, we make public all codes and resulting products which constitute the main results of this paper public. In Table 7 we list the products which are made freely available as a result of this paper9.

6

We use the 7th year temperature analysis mask for nside = 512 (http://0-lambda.gsfc.nasa.gov.iii-server.ualr.edu/product/map/dr4/masks_get.cfm)

8

This is done using the idl routine chisqr_pdf(quad*df/theory, df), where quad is the observed value of the quadrupole, theory the theoretical value given by Eq. (17), and df the number of degrees of freedom for a quadrupole, i.e. 5.

## Acknowledgments

The authors are grateful to John Peacock, Caroline Francis, Shirley Ho, Olivier Doré, Arnaud Woiselle, the Euclid CMB cross-correlations working group and the anonymous referee for useful discussions. A.R. thanks François Lanusse, Florent Sureau, and Yves Revaz for computational help. We also thank Jacques Delabrouille for providing the wavelets ILC 5yr map from the WMAP 5yr data. We used iCosmo10 software (Refregier et al. 2011), Healpix software (Górski et al. 2002; Gorski et al. 2005), ISAP7 software, the 2 Micron All-Sky Survey catalogue (2MASS)11, WMAP data12, the NRAO VLA Sky Survey (NVSS, Condon et al. 1998)13, and the Galaxy extinction maps of Schlegel et al. (1998). This work was supported by the European Research Council grant SparseAstro (ERC-228261)

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## Appendix A: Testing statistical isotropy biases for sparse inpainting

To justify that sparse inpainting is indeed an appropriate reconstruction method in the context of probing anomalies in the primordial CMB, we test whether we can indeed consider sparse inpainting as a bias-free reconstruction. To do this we test whether the three statistics studied in Sect. 5 are unchanged after the application of sparse inpainting to CMB, LSS, and ISW simulated maps.

Our aim here is to test whether statistically isotropic maps conserve this quality after sparse inpainting. It would also be interesting to test whether maps which are intrinsically anomalous are still anomalous after sparse inpainting. However, testing the latter requires a knowledge of the model creating the anomalies (exotic physics, foregrounds, etc...) in order to test these realistically. In this appendix, we focus only on testing whether sparse inpainting creates spurious statistically anisotropic signatures in data where the true distribution is known to be statistically isotropic.

We sparsely inpaint all CMB and LSS simulations using the public ISAP software7 of A08-SMF10 as described in Sect. 4.

### Appendix A.1: Impact of sparse inpainting on CMB data

We start by considering the impact of sparse inpainting on CMB maps. We consider 1000 Gaussian random field realisations of a CMB map with an input power spectrum corresponding to the “vanilla” cosmology considered in Sect. 5. We sparsely inpaint each simulation after applying the WMAP 7th year temperature analysis mask, as described in Sects. 3 and 4.

We test the mean values for each statistic (low quadrupole, quadrupole/octopole alignment, and octopole planarity) before and after sparse inpainting. The results are reported in Table A.1 and show that the sparse inpainting method introduces negligible biases in all three tests, compared to the intrinsic cosmic variance. The test of quadrupole/octopole alignment can be somewhat altered due to sparse inpainting (see the standard deviation on the bias).

Since with current data we observe a low quadrupole, we test whether sparse inpainting is also robust in cases where the quadrupole is low. We perform a new set of 400 Gaussian random field simulations, where the input power spectrum is WMAP 7 data. Table A.2 shows the results for the three statistical isotropy tests performed on this set of simulations before and after application of sparse inpainting. Again, we see that biases are very small compared to cosmic variance.

### Appendix A.2: Impact of sparse inpainting on LSS data

For the reconstruction of the ISW signal, we must first reconstruct full-sky LSS maps (Sect. 4). Thus we also want to test whether the statistics of the LSS maps are altered by sparse inpainting. To do this, we specifically test how Gaussian random field simulations of 2MASS and NVSS-like surveys are affected by sparse inpainting using the same masks as used in Sect. 3. The simulated maps are for the galaxy overdensity (i.e. including the galaxy bias). Results are shown in Tables A.3 (2MASS) and A.4 (NVSS). Again, biases are negligible compared to cosmic variance for all three statistics considered.

Table A.1

Testing whether sparse inpainting (A08-SMF10) affects the tests of statistical isotropy used in Sect. 5 for 1000 simulated Gaussian random fields with input power spectrum taken as the best-fit theoretical power spectrum for WMAP7 (i.e. with no low quadrupole).

Table A.2

Testing whether sparse inpainting (A08-SMF10) affects the three tests of statistical isotropy used in Sect. 5 for 400 simulated Gaussian random fields with input power spectrum taken as WMAP7-like data (i.e. with low quadrupole).

Table A.3

Testing whether sparse inpainting (A08-SMF10) affects the tests of statistical isotropy used in Sect. 5 for 1000 simulated Gaussian random fields with input power spectrum taken as the theoretical galaxy power spectrum for 2MASS galaxies.

Table A.4

Testing whether sparse inpainting (A08-SMF10) affects the tests of statistical isotropy used in Sect. 5 for 1000 simulated Gaussian random fields with input power spectrum taken as the theoretical galaxy power spectrum for NVSS galaxies.

Table A.5

Expected values of all anomaly tests presented in this paper for 1000 ISW maps due to NVSS galaxies. The ISW maps are calculated from both CMB and NVSS Gaussian random field simulations using Eq. (7). The first column shows results for full sky simulations, while the second column shows results for inpainting CMB and NVSS simulations with respective masks as described in Sect. 4.

### Appendix A.3: Impact of sparse inpainting on the ISW signal

Finally, we want to test whether sparse inpainting can alter the reconstructed ISW signal, either by modifying tests of statistical isotropy or by introducing a spurious ISW signal. We consider 1000 Gaussian random realisations of NVSS galaxies and 1000 uncorrelated WMAP 7 realisations. The goal is to see if inpainting of each map with its respective masks can introduce a spurious ISW signal, when none should be measured. The results are shown in the first line of Table A.5, which gives the value of the cross-correlation quadrupole (CgT,ℓ = 2). Since the maps are uncorrelated by construction, we expect a median cross-correlation equal to zero, which is what we find both before and after sparse inpainting. This indicates that our method does not introduce a spurious cross-correlation signal.

We also test the quadrupole/octopole alignment and octopole planarity of the reconstructed ISW signal from NVSS galaxies (where the ISW map is constructed from NVSS and CMB simulations with different masks). We find that the tests are unbiased after sparse inpainting.

## All Tables

Table 1

List of the 11 temperature anisotropy maps we use to probe the anomalies in the primoridal CMB, including year of WMAP data they correspond to and a description of the mask treatment.

Table 2

Amplitude of the ISW temperature quadrupole and octopole due to the 2MASS galaxy survey (left: as measured from data using inpainted WMAP 9 data for the CMB, and right: from theoretical calculations) and a Euclid-type survey (using theoretical spectra).

Table 3

Quadrupole ( = 2) power and corresponding probability of the quadrupole power being so low.

Table 4

Scalar product of the preferred axes of the quadrupole and octopole (), its corresponding separation (°), and the probability (%) of having such a low separation.

Table 5

The “t” value for the octopole as defined in de Oliveira-Costa et al. (2004) using nside = 128, calculated from the observed CMB maps (top) and after subtraction of the ISW field due to 2MASS and NVSS galaxies (middle).

Table 6

Summary of results in this paper.

Table 7

List of products made available in this paper in the spirit of reproducible research.

Table A.1

Testing whether sparse inpainting (A08-SMF10) affects the tests of statistical isotropy used in Sect. 5 for 1000 simulated Gaussian random fields with input power spectrum taken as the best-fit theoretical power spectrum for WMAP7 (i.e. with no low quadrupole).

Table A.2

Testing whether sparse inpainting (A08-SMF10) affects the three tests of statistical isotropy used in Sect. 5 for 400 simulated Gaussian random fields with input power spectrum taken as WMAP7-like data (i.e. with low quadrupole).

Table A.3

Testing whether sparse inpainting (A08-SMF10) affects the tests of statistical isotropy used in Sect. 5 for 1000 simulated Gaussian random fields with input power spectrum taken as the theoretical galaxy power spectrum for 2MASS galaxies.

Table A.4

Testing whether sparse inpainting (A08-SMF10) affects the tests of statistical isotropy used in Sect. 5 for 1000 simulated Gaussian random fields with input power spectrum taken as the theoretical galaxy power spectrum for NVSS galaxies.

Table A.5

Expected values of all anomaly tests presented in this paper for 1000 ISW maps due to NVSS galaxies. The ISW maps are calculated from both CMB and NVSS Gaussian random field simulations using Eq. (7). The first column shows results for full sky simulations, while the second column shows results for inpainting CMB and NVSS simulations with respective masks as described in Sect. 4.

## All Figures

 Fig. 1WMAP ILC 9th year CMB data (top in mK), 2MASS data (middle), and NVSS data (bottom) with mask (left) and after sparse inpainting (right). Data in the right column is presented up to ℓ = 10 for all maps. The original 2MASS data (middle left) is plotted with a maximum overdensity value of 3 to increase contrast in the map. Open with DEXTER In the text
 Fig. 2Quadrupole and octopole values (μK2) for the different CMB maps listed in Table 1. Points in black are with no extra treatment than that given in the literature, and points in red are after application of sparse inpainting. Open with DEXTER In the text
 Fig. 3Redshift distributions for 2MASS (see Afshordi et al. 2004; Rassat et al. 2007; Dupe et al. 2011) and NVSS (from Ho et al. 2008). Open with DEXTER In the text
 Fig. 4Quadrupole and octopole values (μK2) for the different reconstructed ISW maps. The ISW maps are reconstructed from sparsely inpainted CMB and LSS maps using Eq. (7), where the auto- and cross-correlations are measured directly from the data. Small variations in the phases of different renditions of CMB maps can lead to negligible differences in the auto-correlation (see Fig. 2) and to larger differences in a cross-correlation with a second map. This in turn can result in larger variations in the amplitude of the ISW signal, explaining why the reconstructed ISW maps vary slightly more between CMB maps than the observed temperature power does. Open with DEXTER In the text
 Fig. 5Quadrupole (left) and octopole (right) of the reconstructed ISW map for 2MASS (top) and NVSS (middle) and both NVSS and 2MASS together (bottom). The quadrupole and octopole of the ISW map due to 2MASS galaxies can be compared with that obtained by Francis & Peacock (2010, top of their Fig. 3). Maps are shown in units of μK. Open with DEXTER In the text
 Fig. 6Quadrupole (left) and octopole (right) of WMAP 9 data before inpainting (top), after sparse inpainting (middle), and after subtraction of the reconstructed ISW signal due to 2MASS and NVSS galaxies (bottom). Open with DEXTER In the text

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