 | noimgSummary of the main astrophysical components included in the current version of the model. See text for detailed description of each component. |
 | CMB dipole prediction as generated by the code (here for a $1^\circ$ `sky resolution', in Galactic coordinates). |
 | CMB intensity and polarisation power spectra used by default (for Gaussian CMB simulations) -- black: $C_\ell^{TT}$; red: $C_\ell^{TE}$ (dashed parts are negative); green: $C_\ell^{EE}$; blue: $C_\ell^{BB}$ (from scalar modes only). |
 | CMB temperature and polarisation anisotropy predictions as generated for a $1^\circ$ beam, $N_{\rm side}=256$, in Galactic coordinates. This prediction is based on the CMB extracted from \emph{WMAP} 5-year data using an ILC in needlet space. Note that the maps are not fully exempt from contamination by foregrounds and noise \citep[see][for a complete discussion of the component separation method used to obtain the CMB temperature map]{2009A&A...493..835D}. |
 | CMB temperature and polarisation anisotropy predictions as generated for a $1^\circ$ beam, $N_{\rm side}=256$, in Galactic coordinates. This prediction is based on the CMB extracted from \emph{WMAP} 5-year data using an ILC in needlet space. Note that the maps are not fully exempt from contamination by foregrounds and noise \citep[see][for a complete discussion of the component separation method used to obtain the CMB temperature map]{2009A&A...493..835D}. |
 | CMB temperature and polarisation anisotropy predictions as generated for a $1^\circ$ beam, $N_{\rm side}=256$, in Galactic coordinates. This prediction is based on the CMB extracted from \emph{WMAP} 5-year data using an ILC in needlet space. Note that the maps are not fully exempt from contamination by foregrounds and noise \citep[see][for a complete discussion of the component separation method used to obtain the CMB temperature map]{2009A&A...493..835D}. |
 | Linear part (top panel) and non--linear correction (bottom panel) for non-Gaussian CMB realisations used in the model. Note the different color scales, and that $f_{\rm NL} \sim 1$ (or a few) is a typical expected level. The cosmological parameters assumed for this simulation are from the fit of \emph{WMAP} 7-year + BAO + SN observations, as made available on the LAMBDA web site. |
 | Linear part (top panel) and non--linear correction (bottom panel) for non-Gaussian CMB realisations used in the model. Note the different color scales, and that $f_{\rm NL} \sim 1$ (or a few) is a typical expected level. The cosmological parameters assumed for this simulation are from the fit of \emph{WMAP} 7-year + BAO + SN observations, as made available on the LAMBDA web site. |
 | A simulated lensed CMB temperature anisotropy map (Top left), the amplitude of the difference of a simulated lensed and unlensed CMB temperature anisotropy map (Top right), the amplitude of the simulated deflection field map (bottom left) and the lensing potential map (bottom right) with {\sc HEALPix} pixelisation parameter $N_{\rm side}=1024$. These maps are obtained using the NFFT for the oversampling factor $\sigma =2$ and convolution length $K=4$. |
 | A simulated lensed CMB temperature anisotropy map (Top left), the amplitude of the difference of a simulated lensed and unlensed CMB temperature anisotropy map (Top right), the amplitude of the simulated deflection field ma |
 | A simulated lensed CMB temperature anisotropy map (Top left), the amplitude of the difference of a simulated lensed and unlensed CMB temperature anisotropy map (Top right), the amplitude of the simulated deflection field map (bottom left) and the lensing potential map (bottom right) with {\sc HEALPix} pixelisation parameter $N_{\rm side}=1024$. These maps are obtained using the NFFT for the oversampling factor $\sigma =2$ and convolution length $K=4$. |
 | A simulated lensed CMB temperature anisotropy map (Top left), the amplitude of the difference of a simulated lensed and unlensed CMB temperature anisotropy map (Top right), the amplitude of the simulated deflection field map (bottom left) and the lensing potential map (bottom right) with {\sc HEALPix} pixelisation parameter $N_{\rm side}=1024$. These maps are obtained using the NFFT for the oversampling factor $\sigma =2$ and convolution length $K=4$. |
 | A portion of a simulated lensed CMB temperature anisotropy map (top left), the amplitude of the difference of a simulated lensed and unlensed CMB temperature anisotropy map (top right), the amplitude of the simulated deflection field map (bottom left) and the lensing potential map (bottom right) with {\sc HEALPix} pixelisation parameter $N_{\rm side}=1024$. These maps are obtained using the NFFT for the oversampling factor $\sigma =2$ and convolution length $K=4$. The size of the maps displayed here is about $16^\circ$ on a side. |
 | A portion of a simulated lensed CMB temperature anisotropy map (top left), the amplitude of the difference of a simulated lensed and unlensed CMB temperature anisotropy map (top right), the amplitude of the simulated deflection field map (bottom left) and the lensing potential map (bottom right) with {\sc HEALPix} pixelisation parameter $N_{\rm side}=1024$. These maps are obtained using the NFFT for the oversampling factor $\sigma =2$ and convolution length $K=4$. The size of the maps displayed here is about $16^\circ$ on a side. |
 | A portion of a simulated lensed CMB temperature anisotropy map (top left), the amplitude of the difference of a simulated lensed and unlensed CMB temperature anisotropy map (top right), the amplitude of the simulated deflection field map (bottom left) and the lensing potential map (bottom right) with {\sc HEALPix} pixelisation parameter $N_{\rm side}=1024$. These maps are obtained using the NFFT for the oversampling factor $\sigma =2$ and convolution length $K=4$. The size of the maps displa |
 | A portion of a simulated lensed CMB temperature anisotropy map (top left), the amplitude of the difference of a simulated lensed and unlensed CMB temperature anisotropy map (top right), the amplitude of the simulated deflection field map (bottom left) and the lensing potential map (bottom right) with {\sc HEALPix} pixelisation parameter $N_{\rm side}=1024$. These maps are obtained using the NFFT for the oversampling factor $\sigma =2$ and convolution length $K=4$. The size of the maps displayed here is about $16^\circ$ on a side. |
 | In all panels, the solid black line is the theoretical angular power spectrum of the lensed CMB, and red filled circles are the average angular power spectrum recovered from 1000 realisations of lensed CMB maps at {\sc HEALPix} $N_{\rm side}=1024$. Lensed CMB maps are obtained using the NFFT for the oversampling factor $\sigma =2$ and convolution length $K=4$. |
 | In all panels, the solid black line is the theoretical angular power spectrum of the lensed CMB, and red filled circles are the average angular power spectrum recovered from 1000 realisations of lensed CMB maps at {\sc HEALPix} $N_{\rm side}=1024$. Lensed CMB maps are obtained using the NFFT for the oversampling factor $\sigma =2$ and convolution length $K=4$. |
 | In all panels, the solid black line is the theoretical angular power spectrum of the lensed CMB, and red filled circles are the average angular power spectrum recovered from 1000 realisations of lensed CMB maps at {\sc HEALPix} $N_{\rm side}=1024$. Lensed CMB maps are obtained using the NFFT for the oversampling factor $\sigma =2$ and convolution length $K=4$. |
 | In all panels, the solid black line is the theoretical angular power spectrum of the lensed CMB, and red filled circles are the average angular power spectrum recovered from 1000 realisations of lensed CMB maps at {\sc HEALPix} $N_{\rm side}=1024$. Lensed CMB maps are obtained using the NFFT for the oversampling factor $\sigma =2$ and convolution length $K=4$. |
 | Template map at 408 MHz used to model the intensity of synchrotron emission in the PSM. The colour scale of the bottom panel is histogram--equalised |
 | Template map at 408 MHz used to model the intensity of synchrotron emission in the PSM. The colour scale of the bottom panel is histogram--equalised to increase the dynamic range. |
 | Synchrotron spectral index map used by default in the PSM. |
 | Emission law of the free-free, spinning dust, and main CO molecular line emission (in units of spectral brightness $I_\nu$, e.g., $\propto $ ${\rm MJy}\,{\rm sr}^{-1}$). The spinning dust emission law is here normalised to unity at $\nu=23\,$GHz and the free-free emission law to $I_\nu=2$ at the same reference frequency. The integrated amplitude of the first $^{12}$CO emission lines (transition (J=1--0)) is normalised to unity, and the other lines (transitions (J=2--1) and (J=3--2)) are displayed in proportion to their integrated intensity relative to the first one. |
 | Template map at 23\GHz\ used to model the intensity of free-free emission in the PSM. As seen in the top panel, free-free emission is strongly concentrated in compact regions of the Galactic plane. The colour scale of the bottom panel is histogram--equalised to increase the dynamic range, and to show more extended, diffuse structures. |
 | Template map at 23\GHz\ used to model the intensity of free-free emission in the PSM. As seen in the top panel, free-free emission is strongly concentrated in compact regions of the Galactic plane. The colour scale of the bottom panel is histogram--equalised to increase the dynamic range, and to show more extended, diffuse structures. |
 | Map of the ratio of 100$\,\mu$m to 240$\,\mu$m emission, as obtained by \citet{1999ApJ...524..867F} and used in the present model. |
 | Map of thermal dust emission 100$\,$\micron. Colours are saturated at 100$\,{\rm MJy}\,{\rm sr}^{-1}$, and the colour scale is hist |
 | Top: a small patch of free-free emission before and after adding random small scale fluctuations. Middle and bottom: power spectrum of free-free emission before and after adding small scales. |
 | Top: a small patch of free-free emission before and after adding random small scale fluctuations. Middle and bottom: power spectrum of free-free emission before and after adding small scales. |
 | Top: a small patch of spinning dust emission before and after adding random small scale fluctuations. Middle and bottom: power spectrum of spinning dust emission before and after adding small scales. |
 | Top: a small patch of spinning dust emission before and after adding random small scale fluctuations. Middle and bottom: power spectrum of spinning dust emission before and after adding small scales. |
 | $E$ and $B$ power spectra of diffuse Galactic emission simulated with the model at \wmap\ central frequencies (solid and dashed thick lines respectively). The P06 Galactic mask is used. The \wmap\ derived foreground levels from Gold et al. (2011) are also shown (thin lines). |
 | Synchrotron $Q$ and $U$ maps at 23\GHz\ for a sky resolution of $3^\circ$. At this frequency the synchrotron $Q$ and $U$ maps of the sky model are exactly the \wmap\ 7-year data. The two bottom panels show the polarisation fraction and the polarisation angle as implemented in our model. The average polarisation fraction is about 18\%. |
 | Maps of the large-scale geometrical depolarisation $g^\prime$ and polarisation angle $\gamma^\prime$ for the synchrotron and dust, based on a model of the Galactic magnetic field and density distributions of the energetic electrons and dust grains. These maps are used to correct the dust depolarisation and polarisation angle maps deduced from the 23\GHz\ polarisation data for the |
 | Model of the dust polarisation at 200~GHz and at 3$^\circ$ resolution. The polarisation fraction and polarisation angle maps are slightly modified versions of the same maps obtained for synchrotron at 23~GHz using the \wmap\ and 408~MHz data. |
 | Density of MaxBCG clusters. The clusters are mainly concentrated in the northern Galactic hemisphere. |
 | Top panel: Cluster number counts for different mass functions. Bottom panel: Cluster number counts for different values of $\sigma_8$, using the Tinker mass function. |
 | Top panel: Cluster number counts for different mass functions. Bottom panel: Cluster number counts for different values of $\sigma_8$, using the Tinker mass function. |
 | Maps of thermal and kinetic SZ effect from the Hubble volume simulation (left column), from the local universe (middle column), and total thermal and kinetic SZ effects from both simulations together, smoothed here to a sky resolution of 5 arc-minutes (right column). All the displayed maps are small $5^\circ \times 5^\circ$ patches centred on the North Galactic Pole. The original full sky maps are at {\sc HEALPix} $N_{\rm side} = 2048$ for the Hubble volume, and at $N_{\rm side} = 1024$ for the local hydrodynamical simulations. The contribution from the local universe comprises a large cluster at sky coordinates close to those of the Coma cluster, which dominates the total SZ emission in the maps displayed here. |
 | Maps of thermal and kinetic SZ effect from the Hubble volume simulation (left column), from the local universe (middle column), and total thermal and kinetic SZ effects from both simulations together, smoothed here to a sky resolution of 5 arc-minutes (right column). All the displayed maps are small $5^\circ \times 5^\circ$ patches centred on the North Galactic Pole. The original full sky maps are at {\sc HEALPix} $N_{\rm side} = 2048$ for the Hubble volume, and at $N_{\rm side} = 1024$ for the local hydrodynamical simulations. The contribution from the local universe comprises a large cluster at sky coordinates close to those of the Coma cluster, which dominates the total SZ emission in |
 | Maps of thermal and kinetic SZ effect from the Hubble volume simulation (left column), from the local universe (middle column), and total thermal and kinetic SZ effects from both simulations together, smoothed here to a sky resolution of 5 arc-minutes (right column). All the displayed maps are small $5^\circ \times 5^\circ$ patches centred on the North Galactic Pole. The original full sky maps are at {\sc HEALPix} $N_{\rm side} = 2048$ for the Hubble volume, and at $N_{\rm side} = 1024$ for the local hydrodynamical simulations. The contribution from the local universe comprises a large cluster at sky coordinates close to those of the Coma cluster, which dominates the total SZ emission in the maps displayed here. |
 | Maps of thermal and kinetic SZ effect from the Hubble volume simulation (left column), from the local universe (middle column), and total thermal and kinetic SZ effects from both simulations together, smoothed here to a sky resolution of 5 arc-minutes (right column). All the displayed maps are small $5^\circ \times 5^\circ$ patches centred on the North Galactic Pole. The original full sky maps are at {\sc HEALPix} $N_{\rm side} = 2048$ for the Hubble volume, and at $N_{\rm side} = 1024$ for the local hydrodynamical simulations. The contribution from the local universe comprises a large cluster at sky coordinates close to those of the Coma cluster, which dominates the total SZ emission in the maps displayed here. |
 | Maps of thermal and kinetic SZ effect from the Hubble volume simulation (left column), from the local universe (middle column), and total thermal and kinetic SZ effects from both simulations together, smoothed here to a sky resolution of 5 arc-minutes (right column). All the displayed maps are small $5^\circ \times 5^\circ$ patches centred on the North Galactic Pole. The original full sky maps are at {\sc HEALPix} $N_{\rm side} = 2048$ for the Hubble volume, and at $N_{\rm side} = 1024$ for the local hydrodynamical simulations. The contribution from the local universe comprises a large cluster at sky coordinates close to those of the Coma cluster, which dominates the total SZ emission in the maps displayed here. |
 | Maps of thermal and kinetic SZ effect from the Hubble volume simulation (left column), from the local universe (middle column), and total thermal and kinetic SZ effects from both simulations together, smoothed here to a sky resolution of 5 arc-minutes (right column). All the displayed maps are small $5^\circ \times 5^\circ$ patches centred on the North Galactic Pole. The original full sky maps are at {\sc HEALPix} $N_{\rm side} = 2048$ for the Hubble volume, and at $N_{\rm side} = 1024$ for the local hydrodynamical simulations. The contribution from the local universe comprises a large clust |
 | Power spectra $D_\ell = \ell(\ell\! +\!1)C_\ell/2\pi$ of thermal and kinetic SZ effect, as modelled by the PSM for various options. Black (resp. green) curves give the spectrum of the tSZ (resp. kSZ) maps as modelled on the basis of a population of clusters as described in~\ref{sub:sz_mf}. Upper curves are obtained using the mass function of \citet{2008ApJ...688..709T} with WMAP 7-year cosmological parameters and the $Y$--$M$ scaling law of \citet{2010A&A...517A..92A}. Lower curves are obtained when the value of $\sigma_8$ is set to 0.75 instead of 0.809, and assuming an hydrostatic bias of 15\% in the $Y$--$M$ scaling law, i.e., the $Y$ parameter is 15\% lower than in \citet{2010A&A...517A..92A} for a given cluster mass. Red (resp. blue) curves are tSZ (resp. kSZ) power spectra for the model described in~\ref{sub:sz_lss-massfunction}, where the high redshift part is generated with the same two modeling alternatives (upper curves for $\sigma_8=0.809$ and no hydrostatic bias, lower curves for $\sigma_8=0.75$ and 15\% hydrostatic bias). As the low-redshift part of the SZ maps uses maps at {\sc HEALPix} $N_{\rm side}=1024$, power spectra for this case are computed only up to $\ell=2000$. The red diamond at $\ell=3000$ is the tSZ measurement of $D_{3000}^{tSZ}=3.65\pm 0.69$\uKsquare\ obtained recently by SPT \citep{2011arXiv1111.0932R}, improving on previous measurements from \citet{2010ApJ...719.1045L}, \citet{2011ApJ...739...52D}, and \citet{2011ApJ...736...61S}. The blue arrow is the corresponding upper limit for kSZ. |
 | Sky coverage of the surveys listed in Table~\protect\ref{tb:summary}, in Galactic coordinates. Green points: sources present in both $\simeq 1\,$GHz (NVSS or SUMSS) and 4.85\GHz\ (GB6 or PMN) catalogues; blue points: sources in the NVSS catalogue only; yellow points: sources in the SUMSS catalogue only; red points: sources in the PMN catalogue only; white regions: not covered by any survey. |
 | Modelled source number counts at 5 and 20\GHz\ for one sky realisation, normalised to $\Delta N_0 = S({\rm Jy})^{-2.5}$, compared with models and observational data. Data at 5\GHz\ are from \citet{1986HiA.....7..367K}, \citet{1991AJ....102.1258F}, and \citet{2000ApJ...544..641H}. Data in the 20\GHz\ panel are from the 9C survey \citep{2003MNRAS.342..915W} at 15\GHz\ and from the ATCA survey at 18\GHz\ \citep{2004MNRAS.354..305R}; no correction for the difference in frequency was applied. |
 | Comparison of modelled radio source counts (red points) and the \planck\ radio counts \citep[blue points,][]{2011A&A...536A..13P}. Also shown are: the counts estimated at 31GHz from DASI \citep[grey dashed box,][]{2002Natur.420..772K} and PACO \citep[grey diamonds,][]{2011MNRAS.416..559B}, at 33 |
 | Emission law for a selected sample of typical radio sources produced in a realisation of the sky emission with our model. |
 | Similar to \ref{fig:30_143}, but with additional green points showing the counts of \emph{WMAP} radio sources as represented in our model. The solid black curve shows the total number counts of extragalactic radio sources as predicted by the updated model of de Zotti et al. (2005). |
 | Cosmic infrared background power spectrum. Solid lines are obtained from a simulation. Data points are from \planck\ observations \citep{2011A&A...536A..18P}. Dashed lines at high multipoles for 143 and 217\GHz\ are from the \citet{2011ApJ...739...52D} best-fit model for IR sources (at 148 and 218\GHz, extracted from Fig.~2 of their paper). The CMB power spectrum (in black) is a theoretical model fitting \emph{WMAP} observations. |
 | Temperature r.m.s. fluctuations at {\it WMAP} frequencies for $|b|>20^{\circ}$ at a resolution of $10^{\circ}$. The symbols represent the fluctuations in the various diffuse components of the sky model, the total simulated fluctuations, and \wmap\ 7-year maps. The total signal is a good match to the \wmap\ data. |
 | Comparison of sky emission as observed by WMAP (7-year data) and as predicted by the PSM in the same frequency bands, at a resolution of $1^\circ$. For each frequency channel, the color scale is the same for WMAP (left column) and PSM prediction (middle column). An histogram equalised color scale is used for the K, Ka, and Q channels, and a linear scale for the V and W channels. Maps are saturated to highlight common features away from the galactic plane. Maps of difference between PSM prediction and WMAP observation are displayed in the right column (note that the color scale is different from that used to display the K, Ka and Q maps), highlighting discrepancies in the galactic plane specifically and at the location of a few regions of compact emission. The agreement is excellent over most of the sky away from the galactic ridge and a few compact regions. |
 | Comparison of sky emission as observed by WMAP (7-year data) and as predicted by the PSM in the same |
 | Comparison of sky emission as observed by WMAP (7-year data) and as predicted by the PSM in the same frequency bands, at a resolution of $1^\circ$. For each frequency channel, the color scale is the same for WMAP (left column) and PSM prediction (middle column). An histogram equalised color scale is used for the K, Ka, and Q channels, and a linear scale for the V and W channels. Maps are saturated to highlight common features away from the galactic plane. Maps of difference between PSM prediction and WMAP observation are displayed in the right column (note that the color scale is different from that used to display the K, Ka and Q maps), highlighting discrepancies in the galactic plane specifically and at the location of a few regions of compact emission. The agreement is excellent over most of the sky away from the galactic ridge and a few compact regions. |
 | Comparison of sky emission as observed by WMAP (7-year data) and as predicted by the PSM in the same frequency bands, at a resolution of $1^\circ$. For each frequency channel, the color scale is the same for WMAP (left column) and PSM prediction (middle column). An histogram equalised color scale is used for the K, Ka, and Q channels, and a linear scale for the V and W channels. Maps are saturated to highlight common features away from the galactic plane. Maps of difference between PSM prediction and WMAP observation are displayed in the right column (note that the color scale is different from that used to display the K, Ka and Q maps), highlighting discrepancies in the galactic plane specifically and at the location of a few regions of compact emission. The agreement is excellent over most of the sky away from the galactic ridge and a few compact regions. |
 | Comparison of sky emission as observed by WMAP (7-year data) and as predicted by the PSM in the same frequency bands, at a resolution of $1^\circ$. For each frequency channel, the color scale is the same for WMAP (left column) and PSM prediction (middle column). An histogram equalised color scale is used for the K, Ka, and Q channels, and a linear scale for the V and W channels. Maps are saturated to highlight common features away from the galactic plane. Maps of difference between PSM prediction and WMAP observation are displayed in the right column (note that the color scale is different from that used to display the K, Ka and Q maps), highlighting discrepancies in the galactic plane specifically and at the location of a few regions of compact emission. The agreement is excellent over most of the sky away from the galactic ridge and a few compact regions. |
 | Comparison of sky emission as observed by WMAP (7-year data) and as predicted by the PSM in the same frequency bands, at a resolution of $1^\circ$. For each frequency channel, the color scale is the same |
 | Comparison of sky emission as observed by WMAP (7-year data) and as predicted by the PSM in the same frequency bands, at a resolution of $1^\circ$. For each frequency channel, the color scale is the same for WMAP (left column) and PSM prediction (middle column). An histogram equalised color scale is used for the K, Ka, and Q channels, and a linear scale for the V and W channels. Maps are saturated to highlight common features away from the galactic plane. Maps of difference between PSM prediction and WMAP observation are displayed in the right column (note that the color scale is different from that used to display the K, Ka and Q maps), highlighting discrepancies in the galactic plane specifically and at the location of a few regions of compact emission. The agreement is excellent over most of the sky away from the galactic ridge and a few compact regions. |
 | Comparison of sky emission as observed by WMAP (7-year data) and as predicted by the PSM in the same frequency bands, at a resolution of $1^\circ$. For each frequency channel, the color scale is the same for WMAP (left column) and PSM prediction (middle column). An histogram equalised color scale is used for the K, Ka, and Q channels, and a linear scale for the V and W channels. Maps are saturated to highlight common features away from the galactic plane. Maps of difference between PSM prediction and WMAP observation are displayed in the right column (note that the color scale is different from that used to display the K, Ka and Q maps), highlighting discrepancies in the galactic plane specifically and at the location of a few regions of compact emission. The agreement is excellent over most of the sky away from the galactic ridge and a few compact regions. |
 | Comparison of sky emission as observed by WMAP (7-year data) and as predicted by the PSM in the same frequency bands, at a resolution of $1^\circ$. For each frequency channel, the color scale is the same for WMAP (left column) and PSM prediction (middle column). An histogram equalised color scale is used for the K, Ka, and Q channels, and a linear scale for the V and W channels. Maps are saturated to highlight common features away from the galactic plane. Maps of difference between PSM prediction and WMAP observation are displayed in the right column (note that the color scale is different from that used to display the K, Ka and Q maps), highlighting discrepancies in the galactic plane specifically and at the location of a few regions of compact emission. The agreement is excellent over most of the sky away from the galactic ridge and a few compact regions. |
 | Comparison of sky emission as observed by WMAP (7-year data) and as predicted by the PSM in the same frequency bands, at a resolution of $1^\circ$. For each frequency channel, the color scale is the same |
 | Comparison of sky emission as observed by WMAP (7-year data) and as predicted by the PSM in the same frequency bands, at a resolution of $1^\circ$. For each frequency channel, the color scale is the same for WMAP (left column) and PSM prediction (middle column). An histogram equalised color scale is used for the K, Ka, and Q channels, and a linear scale for the V and W channels. Maps are saturated to highlight common features away from the galactic plane. Maps of difference between PSM prediction and WMAP observation are displayed in the right column (note that the color scale is different from that used to display the K, Ka and Q maps), highlighting discrepancies in the galactic plane specifically and at the location of a few regions of compact emission. The agreement is excellent over most of the sky away from the galactic ridge and a few compact regions. |
 | Comparison of sky emission as observed by WMAP (7-year data) and as predicted by the PSM in the same frequency bands, at a resolution of $1^\circ$. For each frequency channel, the color scale is the same for WMAP (left column) and PSM prediction (middle column). An histogram equalised color scale is used for the K, Ka, and Q channels, and a linear scale for the V and W channels. Maps are saturated to highlight common features away from the galactic plane. Maps of difference between PSM prediction and WMAP observation are displayed in the right column (note that the color scale is different from that used to display the K, Ka and Q maps), highlighting discrepancies in the galactic plane specifically and at the location of a few regions of compact emission. The agreement is excellent over most of the sky away from the galactic ridge and a few compact regions. |
 | Comparison of sky emission as observed by WMAP (7-year data) and as predicted by the PSM in the same frequency bands, at a resolution of $1^\circ$. For each frequency channel, the color scale is the same for WMAP (left column) and PSM prediction (middle column). An histogram equalised color scale is used for the K, Ka, and Q channels, and a linear scale for the V and W channels. Maps are saturated to highlight common features away from the galactic plane. Maps of difference between PSM prediction and WMAP observation are displayed in the right column (note that the color scale is different from that used to display the K, Ka and Q maps), highlighting discrepancies in the galactic plane specifically and at the location of a few regions of compact emission. The agreement is excellent over most of the sky away from the galactic ridge and a few compact regions. |
 | Comparison of sky emission as observed by WMAP (7-year data) and as predicted by the PSM in the same frequency bands, at a resolution of $1^\circ$. For each frequency channel, the color scale is the same f |
 | Comparison of sky emission as observed by WMAP (7-year data) and as predicted by the PSM in the same frequency bands, at a resolution of $1^\circ$. For each frequency channel, the color scale is the same for WMAP (left column) and PSM prediction (middle column). An histogram equalised color scale is used for the K, Ka, and Q channels, and a linear scale for the V and W channels. Maps are saturated to highlight common features away from the galactic plane. Maps of difference between PSM prediction and WMAP observation are displayed in the right column (note that the color scale is different from that used to display the K, Ka and Q maps), highlighting discrepancies in the galactic plane specifically and at the location of a few regions of compact emission. The agreement is excellent over most of the sky away from the galactic ridge and a few compact regions. |