text:
\section{Introduction\label{secI}}
The current state of accelerated expansion of the universe has been well established through a combination of the type-Ia supernova Hubble diagram \cite{Riess,Perlmutter}, primary and lensing-induced anisotropies in the cosmic microwave background (CMB) \cite{Sherwin,VanEngelen,PLANCK_PARAMS}, and measurements of baryon acoustic oscillations \cite{BAO}.
Such an expansion, believed to be driven by dark energy, leaves an imprint in the large-scale cosmic structure (at redshifts in a range of $z\lesssim 2$), as well as on the CMB temperature fluctuations.
Gravitational potentials evolve in time due to the accelerating expansion, giving a net change in energy to photons traversing an underdense or overdense region. This effect, known as the \emph{late-time Integrated Sachs-Wolfe effect} (late-ISW) \cite{SachsWolfe}, is described by the following integral along the line-of-sight:
	\begin{equation}
		\Theta(\mathbf{\hat{n}}) \equiv \frac{\Delta T}{T_{0}}=-2\int_0^{\chi^{\star}} d\chi g(\tau)\dot{\Phi}(\chi\hat{\mathbf{n}},\eta_0-\chi)
	\end{equation}
where $g(\tau)=e^{-\tau(\eta_0-\chi)}$ is the visibility function as a function of the optical depth $\tau$, the derivative of the Newtonian gravitational potential $\Phi$ is with respect to the conformal time, $\eta_{0}$ is the present value of the conformal time, $\chi^{\star}$ is the comoving distance to the surface of last scattering, and $T_0$ is the isotropic CMB blackbody temperature, corresponding to the multipole $\ell=0$. The late-ISW effect creates temperature anisotropies mostly on relatively large angular scales ($\theta > 3^{\circ}$).
A detection of this signal in a spatially flat universe represents an independent test for dark energy  \cite{Kamionkowski}, and in principle a useful tool to characterize its properties and dynamics \cite{Giannantonio08}.

In $\Lambda$CDM cosmological models, this secondary CMB anisotropy contributes only around $3\%$ of the total variance of the temperature sky, while having a Gaussian random distribution to a very good approximation, and hence it cannot be detected from temperature data alone. Nevertheless, it is strongly correlated with the large-scale galaxy distribution \cite{Crittenden}, and recently the angular cross-power spectrum $C_{\ell}^{Tg}$ between CMB temperature and galaxies has been exploited to detect the late-ISW signal \cite{Fosalba, Francis, Afshordi, Boughn, Nolta, Padmanabhan, Rassat, Sawangwit, Vielva, Cabre, Ho, Planck_ISW, Monteagudo13, Kovacs, Ferraro} (see Table 1 of \cite{Nishizawa} for a detailed list of related works).
A similar correlation was detected in pixel space, corresponding to the presence of hot and cold spots in the CMB sky preferentially centered on superstructures (\cite{Granett}, GNS08 hereafter). This strong detection exploited a novel technique involving photometric analysis of stacked CMB patches from the WMAP 5-year sky maps \cite{hinshaw09} centered on $100$ superstructures (50 biggest superclusters and 50 biggest supervoids) detected in the Sloan Digital Sky Survey (SDSS) Data Release 6 \cite{SDSS6}, covering a sky area of $7500$ square degrees in a redshift range $0.4<z<0.75$. In this redshift range, the expected cross-correlation spectrum peaks at $\ell \simeq 20$ ($\theta \simeq 4^{\circ}$) (\cite{Monteagudo}, HMS13 hereafter), which motivated the use of a compensated top-hat filter of $4^{\circ}$ radius to enhance the signal
\cite{GNS08Sup}. The mean temperature fluctuation reported by GNS08 of $\overline{T} = 9.6$ $\mu$K shows a departure from the null signal at a significance  of $4.4\sigma$.  Recently, the Planck satellite collaboration has confirmed the detection of the late-ISW effect with a statistical significance ranging from $2.5\sigma$ to $4.0\sigma$ (depending on the method involved) (\cite{Planck_ISW}, PLK13 hereafter). The strongest Planck detection is associated with the stacking analysis, using the GNS08 catalog,
giving an average peak amplitude of $\overline{T} = 8.7 \mu K$, which is consistent with the value found by GNS08 using the WMAP temperature map.

As pointed out by \cite{Ferraro}, the temperature-galaxy cross correlation requires prior knowledge of the galaxy bias, which may dominate the detection significance
and consistency tests of the underlying cosmological model. In contrast, the technique of stacking on the largest superstructures in a large-scale structure survey
does not rely on any knowledge regarding the galaxy bias, apart from the fact that visible matter traces dark matter. In addition, the GNS08 technique is based on an extreme-value statistic: in principle, it is sensitive to small departures from the $\Lambda$CDM model which may not significantly affect the cross-correlation $C^{Tg}_{\ell}$.
On the other hand, substantial control over systematic errors is required to carry out such an analysis.

It has been argued that the strong signal detected by GNS08 is in tension with the underlying $\Lambda$CDM model \cite{Nadathur,Flender}.
Analytical estimates of the stacked late-ISW signal in a comoving volume that corresponds to that probed by GNS08 predict an average signal of $\overline{T} = 2.27 \pm 0.14 \mu K$(\cite{Flender}, FHN13 hereafter), where the reported error is due to cosmic variance. The same work confirms this estimate using
late-ISW maps constructed from N-body simulations which include the second-order Rees-Sciama contribution \cite{ReesSciama}.The discrepancy with the GNS08 measurement has a significance greater than 3$\sigma$. Other cosmological models have been considered to explain the discrepancy, including primordial non-Gaussianities \cite{Monteagudo} and $f(R)$ gravity theories \cite{Cai}, but neither seems adequate to explain the strong detected signal.

A less interesting but more plausible possibility is that the strong detected signal is the result of correlations of the late ISW signal with other sources of temperature anisotropy, which may boost the mean temperature of the identified top-ranked peaks.
The current theoretical predictions of the stacked late-ISW signal do not include correlations between ISW temperature fluctuations formed at different redshifts. In HMS13, the primary temperature fluctuations, formed at redshift $z\simeq 1100$, were considered uncorrelated with the secondary anisotropies and simply added to gaussian random generated late-ISW maps. These high-redshift fluctuations are partially correlated with the secondary temperature anisotropies, at a level that depends on the underlying cosmological model. More importantly, we expect a non-negligible correlation between the late-ISW signal, traced by superstructures in GNS08 in the redshift range $0.4 < z < 0.75$, and the late-ISW effect due to structures at either higher or lower redshift.

In this work, we provide a complete description of these correlations through simulated skies based on simple linear perturbation theory. Temperature fluctuations on large scales
result from gravitational potential perturbations in the linear regime (see \cite{Chen} for alternative proposal). If the primordial perturbations are a Gaussian random field, which appears to be an excellent
approximation to the observed large-scale structure \cite{Papai10}, the statistical properties of the CMB sky on large angular scales are completely specified by the temperature power spectrum $C_{\ell}^{TT}$. We generate Gaussian random realizations of the CMB sky using the linear power spectra for its various physical components, including correlations between them. This is an easy computational process, in contrast to extracting large-angle late-ISW maps from large-box N-body cosmological simulations \cite{Watson14, Hotchkiss}.  The approach we adopt
in this paper allows full characterization of cosmic variance with a random sample of simulated skies, and it automatically accounts for the effects of the largest-scale perturbation modes beyond the reach of N-body simulations. We then reanalyze foreground-cleaned CMB temperature maps, processed to match the procedure adopted in our sky simulations. This last step guarantees that the discrepancy between theoretical estimates and the measured signal is not due to different analysis procedures.
Our simulated late-ISW mean peak temperature signal is consistent with previous estimates, but with a wider spread of values. Correlations between temperature signals increase the expected mean value as well as the spread slightly. The main reason for this larger spread, however, is the noise associated to the uncorrelated fluctuations at scales of our interest, and thus reduces the statistical significance of the discrepancy between theory and experiment to around $2.5\sigma$ when compared with our measured values from CMB maps.

We present our work as follows. In Section \hyperref[secII]{\ref*{secII}}, we describe an algorithm to generate realistic temperature maps, including spatial filtering and all correlations between temperature components. We then present the pipeline of our simulations in Section \hyperref[secIII]{\ref*{secIII}}, and the resulting distribution of late-ISW mean peak temperatures. In Section \hyperref[secIV]{\ref*{secIV}}, we apply the same procedure to the Planck CMB temperature maps. Finally, Section \hyperref[secV]{\ref*{secV}} concludes with a discussion of possible sources of systematic errors, a comparison with other late-ISW detection techniques, and future prospects for resolving the discrepancy between theory and measurements with wider and deeper large-scale structure surveys.

\section{Correlated Components of the Temperature Sky\label{secII}}

\begin{figure}[t!]
	\centering
		\includegraphics[scale=0.6]{cl.pdf}
		\caption{Top: Angular power spectra in $\Lambda$CDM, for the ISW effect due to structure in the redshift range $0.4 < z < 0.75$ (``ISW--in'', green), ISW effect outside of this redshift range (``ISW--out'', blue), and all temperature perturbation components except for ISW--in (yellow). Bottom: Correlation coefficients between ISW--in
	and ISW--out (blue), and between ISW--in and all other temperature perturbation components (yellow).}
	\label{fig:cls}
\end{figure}

The $\Lambda$CDM model is a compelling theory to describe the statistical properties of the CMB fluctuations, making precise predictions for the temperature power spectrum $C_{\ell}^{TT}$ \cite{WMAP9, PLANCK_PS}.
Different physical processes contribute to the temperature fluctuations over a wide range of angular scales; the CMB temperature sky is well approximated by the sum of correlated
gaussian random fields, one for each physical component, such that
\begin{equation}
	\begin{aligned}
		\langle a_{\ell m}^{i}, a_{\ell ' m'}^{i \star} \rangle &= \delta_{\ell \ell '} \delta_{mm'} C_{\ell}^{ii}\\
		\langle a_{\ell m}^{i}, a_{\ell ' m'}^{j \star} \rangle &= \delta_{\ell \ell '} \delta_{mm'} C_{\ell}^{ij}\\
	\end{aligned}
	\label{cov_mat}
\end{equation}
where $i$ and $j$ are the components making up the observed temperature field $\Theta(\mathbf{\hat{n}})=\sum_i \sum_{\ell m}a_{\ell m}^{i}Y_{\ell m}$ and the power spectra satisfy the condition $C_{\ell}^{i i} C_{\ell}^{j j} \ge \big(C_{\ell}^{i j}\big)^2$ \cite{KKS}. This set of power spectra specify the covariance matrix of the temperature given a cosmological model. For the purposes of this work, we consider a 2-component sky described by a symmetric 2x2 covariance matrix. The first component, $C_{\ell}^{1,1}$, is always the late-ISW component of the temperature field, corresponding to the GNS08 redshift range (ISW--in, hereafter). For the second component, $C_{\ell}^{2,2}$, we consider two distinct cases:
\begin{itemize}
\item \textbf{Case A}: \emph{only} late-ISW generated outside the probed redshift range, corresponding to $0<z<0.4$ and $0.75<z<10$ (ISW--out, hereafter);
\item \textbf{Case B}: primary and secondary anisotropies generated outside the probed redshift range. Specifically, we consider the sum of ISW--out, early ISW after
recombination, and Sachs-Wolfe, intrinsic and Doppler contributions at last scattering.
\end{itemize}

The off-diagonal terms $C_{\ell}^{1,2}$ are calculated according to the specific case we consider.
For a spatially flat, $\Lambda$CDM cosmological model with the best-fit Planck+WP+HighL parameters \cite{PLANCK_PARAMS}
we compute the covariance matrix in Eq.~(\ref{cov_mat}) with the numerical Boltzmann code \verb|CLASS v2.2|\footnote{\url{http://class-code.net/}} \cite{CLASS},
including the nonlinear effects calculated with \verb|Halofit| \cite{HALOFIT}.
The correlated harmonic coefficients are generated via Cholesky decomposition as
\begin{equation}
	\begin{aligned}
		a_{\ell m}^{i}&= \sum_{k=1}^2 A_{\ell, ik}\zeta_k\\
		a_{\ell m}^{T} &= a_{\ell m}^{1} + a_{\ell m}^{2}\\
	\end{aligned}
	\label{alms}
\end{equation}
where $\zeta_k$ is a column vector composed of $2$ complex gaussian random numbers with zero mean and unit variance, and $A_{\ell}$ is a lower-diagonal real matrix which satisfies $C_{\ell}=A_{\ell}^TA_{\ell}$.
The $a_{\ell m}^{1}$ are the harmonic coefficients corresponding to the ISW--in component alone.

In Fig.~\ref{fig:cls}, we plot the unfiltered covariance matrix components as function of the multipole $\ell$. The top panel shows the diagonal terms. Note that the signal of interest, ISW--in, has a lower amplitude compared than the other components at all multipoles. Thus, the statistics of temperature peaks for an unfiltered map are completely dominated by the anisotropies generated at last scattering. A wise choice for an $\ell$-space filter is required (see below, Sec. \hyperref[secIII]{\ref*{secIII}}).
The bottom panel shows the off-diagonal terms; we plot the normalized correlation coefficient
\begin{equation}
	r_{\ell} \equiv \frac{C^{i j}_{\ell}}{\sqrt{C^{i i}_{\ell} C^{j j}_{\ell}}}
\end{equation}
which satisfies the condition $|r_{\ell}| \leq 1$.
The correlation matrix cannot be considered diagonal, especially at low $\ell$ values.
In principle we expect a negative cross-correlation on large scales (i.e. $r_{\ell}<0$) due to the Sachs-Wolfe component: if we consider the entire late-ISW contribution (i.e., $0<z<10$), the cross-spectrum is dominated by the ISW-SW term, which gives an overall anti-correlation. In the case of interest (where we consider shells of late-ISW signal), the dominant part is the correlation between ISW--in and ISW--out.
Notice that $r^{\small{\rm CaseA}}_{\ell}/r^{\rm CaseB}_{\ell} \simeq \sqrt{C^{2,2 (\rm CaseB)}_{\ell}/C^{2,2 (\rm CaseA)}_{\ell}}$, which implies that the mean value of the stacked signal is mainly enhanced by the ISW--out component. This peculiar effect is attributed to the wide range of $k-$modes, which couples the fluctuations of neighboring redshift regions. On the other hand, the mildly correlated primary fluctuations dominate the statistical error in averaged peak values.  Analytical signal and error estimates are possible but not simple \cite{PEAK_AKW}, so we compute both numerically in the following Section.

\section{Methodology and Analysis\label{secIII}}

The multipole region of our interest is dominated by cosmic variance. This problem is difficult to characterize using N-body simulations, so we generate random temperature maps from the power spectra and correlations to construct the statistical distribution of ISW mean peak amplitudes. The procedure described in this section is based on the FHN13 analysis, adapted to multi-component correlated sky maps.

\subsection{Harmonic-Space Filtering\label{secIII.A}}

To isolate the late-ISW peak signal in $\ell$-space, we apply the  $4^\circ$ compensated top-hat filter adopted by GNS08:
\begin{equation}
	F(\theta) =
  	\begin{cases}
   	(2\pi(1-\cos{\theta_F}))^{-1}, & 0<\theta<\theta_F, \\
   	\\
   	-(2\pi(\cos{\theta_F}-\cos{\sqrt{2}\theta_F}))^{-1},  & \theta_F<\theta<\sqrt{2}\theta_F,
  	\end{cases}
	\label{tophat_filter}
\end{equation}
where $\theta_F=4^{\circ}$ is the characteristic filter radius. By performing a Legendre transform of the real-space filter $F(\theta) \rightarrow F_{\ell} = \int F(\theta)\mathcal{P}_{\ell}(\cos\theta) d\cos\theta$, we can compute a full-sky filtered map simply by rescaling the covariance matrix, $C_{\ell} \rightarrow C_{\ell}F^2_{\ell}B^2_{\ell}$, which also uses
an additional Gaussian beam smoothing $B_{\ell}$ with  \verb|FWHM|$=30'$ adopted by PLK13 to match the WMAP resolution.
The compensated top-hat filter does not give a sharp cutoff in multipole space. However, it drops off faster than $\ell^{-2}$, which ensures the suppression of the small-scale fluctuations.
At the scales enhanced by the filter $\ell \simeq 10-30$, the portion of the temperature fluctuations uncorrelated with the ISW--in signal  for Case B is approximately one order of magnitude larger than that for Case A, with a resulting increase in the scatter of the mean peak statistic.

\subsection{Simulation Pipeline\label{secIII.B}}

To identify the peaks of the late-ISW temperature fluctuations in the CMB sky map, GNS08 used the distribution of luminous red galaxies in \verb|SDSS DR6|
and looked for overdense and underdense regions.
The top-ranked $100$ superstructures identified in the sample have a median radial length calculated at $z=0.5$ of $R_v \simeq 85 Mpc$ and $R_c \simeq 25 Mpc$ for voids and clusters respectively.
The corresponding normalized fluctuations of the gravitational potential are of the order $\Phi \simeq 10^{-4}$ \cite{GNS08Sup}.
These gravitational potential fluctuations are still in the linear regime for standard structure growth.
\begin{figure}[t!]
	\centering
		\includegraphics[scale=0.34]{scatter.pdf}
		\caption{The mean value of the filtered CMB temperature at the locations of the top 50 cold spots $\overline{T_{\rm cold}}$ and top 50 hot spots $\overline{T_{\rm hot}}$ of the ISW--in map component, corresponding to the late-ISW signal from structures in the redshift range $0.4 < z < 0.75$, for a sky fraction $f_{sky}=0.2$.
	Plotted are $(\overline{T_{\rm hot}},\overline{T_{\rm cold}})$ for 5000 randomly generated skies with all contributions to the CMB signal (green points). The red cross is at the location of the mean values
	of $\overline{T_{\rm cold}}$ and $\overline{T_{\rm hot}}$ for the 5000 model skies. For comparison, we plot  5000 model skies generated
	using only the ISW--in signal (gray points), and 5000 skies generated using the full late late-ISW signal but no other temperature components (blue points).
	Also displayed are the measured values from GNS08 (purple diamond) and from the analysis in Sec.~IV using Planck data (black square).}
	\label{fig:scatter_plot}
\end{figure}

Assuming perfect efficiency in detecting and ranking superstructures from large-scale structure distribution data, the observed GNS08 signal should match the theoretical expectation from averaging the CMB temperature fluctuations traced by the $100$ biggest fluctuations in the filtered late-ISW map over the redshift range of the survey \cite{Flender}.
We generate correlated pairs of filtered random Gaussian maps, one for the ISW--in component and one for the other linear components of the temperature sky, using multipoles in both power spectrum $\ell \leq 800$; we use \verb|HEALPix|\footnote{\url{http://healpix.sf.net}} \cite{HEALPix} with \verb|NSIDE|=$256$. From the
filtered ISW--in map, we identify the $50$ hottest maxima and $50$ coldest minima in a sky region of area $f_{\rm sky}=0.2$, corresponding to the sky fraction of the \verb|SDSS DR6| survey. Maxima and minima are identified pixel-by-pixel, testing whether or not the temperature of the central pixels is the greatest or the smallest of the $8$ surrounding pixels. Finally, we take the pixels corresponding to these extrema and average their values in the full sky map consisting of the sum of the two correlated random maps. We find
the average of the 50 hottest ISW--in maxima $\overline{T_h}$ and 50 coldest ISW--in minima $\overline{T_c}$ separately, and we also compute the combined mean value as
$\overline{T_m} = (\overline{T_h} - \overline{T_c})/2$. For comparison, we also calculate the same quantities for the ISW--in map only, which we call \textbf{Case 0}. This procedure is performed on an ensemble of $5000$ random generated skies.

The procedure adopted here gives an upper bound on the theoretical signal from clusters and voids identified in any specific tracer of large-scale structure: we
simply assume that the 50 largest voids and 50 largest clusters in a sky region are correctly identified. Any error in identifying these features will lead to a smaller
mean signal. Since the measured signal is larger than the expected theoretical maximum signal, errors in cluster identification will increase the difference between
theory and measurement quantified in the next section.

\subsection{Results and Comparison with Previous Work}

\begin{table}[t!]
\caption{Results from Gaussian random skies, stacked on peaks of the ISW--in signal (the ISW generated for structure in the redshift range  $0.4<z<0.75$).
The simulated skies are constructed from the angular power spectra in the standard $\Lambda$CDM cosmology, smoothed with a Gaussian beam of FWHM 30' and a compensated
top hat filter of radius $4^{\circ}$, Eq.~(\ref{tophat_filter}).
We report the mean and the standard deviation of the stacks on the locations of the 50 hottest ISW--in spots $\overline{T_h}$, 50 coldest ISW--in spots $\overline{T_c}$, and
the mean magnitude for all 100 spots $\overline{T_m}$, calculated from $5000$ random realizations of the microwave sky, including correlations between the ISW--in signal and
other sky components. These values are presented for ISW--in skies only (Case 0), ISW--in plus ISW--out skies (Case A), and realistic skies including early ISW, intrinsic, and Doppler contributions to the sky temperature (Case B). The theoretical prediction from FHN13 and the measured value from GNS08 are reported for comparison.}
\centering
\begin{tabular}{c | c | c | c}
\hline\hline
&&&\\
Case & $\quad$ $\overline{T_h}$ $[\mu K]$ $\quad$ & $\quad$ $\overline{T_c}$ $[\mu K]$ $\quad$ & $\quad$ $\overline{T_m}$ $[\mu K]$\\ [0.5ex]
\hline\hline
\textbf{Case 0}& $1.97 \pm 0.09$ &$-1.97 \pm 0.09$& $1.97 \pm 0.07$\\
\textbf{Case A} & $2.23 \pm 0.25$ &$-2.23 \pm 0.25$& $2.23 \pm 0.20$\\
\textbf{Case B} & $2.30 \pm 3.1$ &$-2.30 \pm 3.1$& $2.30 \pm 2.32$\\
\hline\hline
\textbf{FHN13}& - &-& $2.27 \pm 0.14$\\
\textbf{GNS08} & $7.9 \pm 3.1$ & $-11.3 \pm 3.1$ & $9.6 \pm 2.22$\\
\hline\hline
\end{tabular}
\label{table:sims_res}
\end{table}
The results of our simulations are presented in Table~\ref{table:sims_res} and visually summarized in Fig.~\ref{fig:scatter_plot} and Fig.~\ref{fig:hist_plot}.
As expected for random realizations of a Gaussian field, $|\overline{T_h}|=|\overline{T_c}|$. The mean peak signal for the full simulated
sky maps (Case B) is $2.30\pm 2.32$ $\mu$K, compared to the GNS08 measurement of $9.6$ $\mu$K, a discrepancy at
a significance of $3.1\sigma$. Our discrepancy is about the same size as previous analyses, but the significance is somewhat lower.
This is due to our inclusion of all components in the microwave temperature map and their correlations, which increases the uncertainty
in our predicted values. The central value of our ISW--in peak signal, $1.97$ $\mu$K (Case 0), is lower by 0.30 $\mu$K than the signal
predicted in FHN13, which is expected due to a difference in the underlying cosmological models used. However, the difference is
small compared to the statistical uncertainty for the full sky signal (Case B). The central value of our full-sky peak signal is also higher
than the ISW--in peak signal by $0.33$ $\mu$K; this difference is due to the correlations between the ISW--in signal and the other components
which are included in the Case B peak signal.

\section{The Stacked ISW Signal Using Planck Sky Maps\label{secIV}}
\begin{figure}[t!]
	\centering
		\includegraphics[scale=0.32]{hist_t_m.pdf}
		\caption{The combined mean value of the filtered CMB temperature at the locations of the top 50 cold spots and top 50 hot spots of the ISW--in map component, corresponding to the late-ISW signal from structures in the redshift range $0.4 < z < 0.75$, for a sky fraction $f_{sky}=0.2$. Plotted are the distributions (normalized to the maximum value) of the combined mean temperature $(\overline{T_{\rm hot}} - \overline{T_{\rm cold}})/2$ obtained from 5000 simulated skies, for the three difference cases considered in this work. Also displayed are the measured values from GNS08 (purple vertical line) and from the analysis in Sec.~IV using Planck data (black vertical line).}
		\label{fig:hist_plot}
\end{figure}

The original late-ISW peak analysis in GNS08 used WMAP sky maps, and PLK13 confirmed the measured value using Planck data.
Here we obtain the measured late-ISW signal from publicly available foreground-cleaned maps based on Planck and Planck+WMAP data,
using the same sky locations as GNS08.
The purpose of this re-analysis is testing the significance of the discrepancy by using the same analysis pipeline as the simulations in Sec.~\ref{secIII}, to
ensure that the difference between the model and the measured value is not due to any inconsistency in how the data and simulations are treated.

We use four different foreground-cleaned CMB temperature maps, based on different component separation approaches. Two are public CMB temperature maps from the \verb|Planck| collaboration\footnote{\url{http://www.sciops.esa.int/wikiSI/planckpla}}, namely \verb|SMICA| and \verb|NILC|\cite{PLANCK_CS}. The other two maps are based on the \verb|LGMCA| method\footnote{\url{http://www.cosmostat.org/CosmoStat.html}} from the recent work in Ref.~ \cite{Bobin}. The \verb|PR1| map uses only \verb|Planck DR1| data \cite{PLANCK_GEN}, and the \verb|WPR1| map uses both \verb|Planck DR1| and \verb|WMAP9| data \cite{WMAP9}.

\begin{figure}[t!]
	\centering
		\includegraphics[scale=0.6]{steps.pdf}
		\caption{Histograms of pixel temperatures centered on superstructures identified by GNS08, measured using 4 different foreground-cleaned filtered CMB maps. Top panel: measured temperatures at locations of voids in the GNS08 catalog; the dashed vertical line indicates the mean temperature. Bottom panel: the same
for locations of clusters.}
	\label{fig:steps}
\end{figure}

We process these four maps in the same fashion:
\begin{itemize}
\item we apply a gaussian beam smoothing in harmonic space to the map defined as $B_{\ell} = B_{\ell}(30^{\prime})/B_{\ell}(\rm map)$
where $B_{\ell}(\rm map)$ is the effective beam of the released map; this allows us to take into account for the finite resolution
of the instrument, and hence matching the overall smoothing applied to the simulated maps.
We also filter out the small-scale fluctuations by setting the harmonic coefficients of the map $a_{\ell m }=0$ for $\ell>800$;
\item the preprocessed map is then masked using the released \verb|Planck| mask \verb|U73|, avoiding contaminations from bright point sources;
\item the masked map is filtered in harmonic space using the compensated top-hat filter $F_{\ell}$ and repixelized to \verb|NSIDE|=$256$;
\item we read the temperature values of the pixels corresponding to the cluster/void positions used in GNS08 \footnote{\url{http://ifa.hawaii.edu/cosmowave/supervoids/publications-and-data/}}.
\end{itemize}

\begin{figure*}[t!]
	\centering
		\includegraphics[scale=0.5]{SMICA_filtered.png}
		\caption{The filtered SMICA-Planck CMB temperature map, in a Mollweide projection in ecliptic coordinates. The galactic region and point sources have been masked with the U73-Planck mask. The resolution of the HEALPIX maps is NSIDE$=256$. The locations of superclusters (red ``+'') and supervoids (blue ``x'') from the GNS08 catalog are also shown.}
	\label{fig:map}
\end{figure*}

Fig.~\ref{fig:map} shows the filtered \verb|SMICA| map in a Mollweide projection in ecliptic coordinates; superstructure locations from GNS08 are marked. In Fig.~\ref{fig:steps}, we plot the histogram of the temperature values for voids and clusters separately for the four analyzed maps. The measured values are used to calculate the quantities $\overline{T_c}$, $\overline{T_h}$ and $\overline{T_m}$ given in Table~\ref{table:maps_res}.
\begin{table}[t!]
	\caption{Mean temperature deviations for GNS08 cluster and void locations, for four temperature maps with different foreground cleaning procedures.
We estimate the mean and standard deviation $\sigma_{FG}$ from the four different maps.}
\centering
\begin{tabular}{c | c | c | c}
\hline\hline
&&&\\
Map & $\quad$ $\overline{T_h}$ $[\mu K]$ $\quad$ & $\quad$ $\overline{T_c}$ $[\mu K]$ $\quad$ & $\quad$ $\overline{T_m}$ $[\mu K]$\\
\hline\hline
NILC & $ 6.9 $ & $-9.4$ & $8.1$\\
SMICA & $ 7.0 $ & $-9.4$ & $8.2$\\
PR1 & $ 6.9 $ & $-9.3$ & $8.1$\\
WPR1 & $ 6.9 $ & $-9.2$ & $8.0$\\
\hline\hline
MEAN & $6.89$ & $-9.33$ & $8.11$\\
$\sigma_{FG}$& $0.01$ & $0.09$ & $0.04$\\
\hline\hline
\end{tabular}
\label{table:maps_res}
\end{table}
Different component separation methods quantify the effects of residual foreground contamination. We measure the fluctuations of the average temperature signal for different maps and use the variance of these fluctuations $\sigma_{\rm FG}$ as an estimate of the error due to foregrounds. The temperature values are extremely stable and fluctuations are always within
$1\%$ (see also Fig.~\ref{fig:steps}), suggesting that the temperature variations are predominantly cosmological. Our mean peak temperature values are smaller than those
reported by GNS08 and PLK13 by around 1.5 $\mu$K, which is within the 1$\sigma$ uncertainty. Such a difference is driven mainly by details of the filtering procedure.

The results of our simulations and our measured signals, shown in Fig.~\ref{fig:scatter_plot} and Fig.~\ref{fig:hist_plot}, can be summarized as
\begin{itemize}
\item The departure of the measurements from a null signal has decreased somewhat compared to previous analyses. It corresponds to a detection significance of $2.2\sigma$, $3.0\sigma$ and $3.5\sigma$ for clusters, voids and combined, respectively;
\item The measurements are higher than the expected maximum signal in $\Lambda$CDM cosmology at a level of $1.5\sigma$, $2.3\sigma$ and $2.5\sigma$ for clusters, voids and combined, respectively;
\newpage
\item The asymmetry between the measured signal for voids and clusters is not statistically significant, being smaller than $1\sigma$.
\end{itemize}
For these estimates, we consider foregrounds contamination and cosmic variance from simulations to be uncorrelated; hence we take $\sigma_{\rm tot} = \sqrt{\sigma^2_{\rm FG}+\sigma^2_{\rm sim}}$, but the residual foreground error is small compared to the cosmic variance uncertainty.

\section{Discussion\label{secV}}

Our analysis confirms both the size of the stacked late-ISW signal seen by GNS08 and PLK13,
and theoretical predictions for $\Lambda$CDM models by FHN13 and HMS13.
By using several maps with different foreground subtraction
methods, we demonstrate that foreground residuals contribute negligible uncertainty to the measured
signal. The theoretical modeling, using correlated Gaussian random fields, is far simpler than
previous analyses using N-body simulations, showing that the predicted signal has no
significant systematic error arising from insufficient box size or other subtleties of the simulations.
Our calculations also include the correlations between the late-ISW signal
and other sources of microwave temperature anisotropies, which mildly increases the theoretical mean signal
while also increasing the statistical uncertainty.
We find a stacked late-ISW signal which is different from null at $3.5\sigma$ significance,
and a discrepancy between the predicted and observed signal of $2.5\sigma$ in
Planck sky maps at the peak and void locations determined by
GNS08 from SDSS data in the redshift range $0.4<z<0.75$.

The statistic used in this work is the mean value at the sky locations of the 50 highest positive
and lowest negative peaks in the late-ISW signal, assumed to be traced by structures and voids in a large-scale structure
survey. In simulations, the late-ISW peaks can be identified directly, and the 50 highest peaks in a given
sky region are known precisely. When analyzing large-scale structure data, peak identification will
not be perfectly efficient: some of the actual 50 largest extrema in the late-ISW signal may be missed
in favor of others which have lower amplitude. Thus the observed signal will necessarily be
biased low. The observed discrepancy between observation and theory has the observed
signal high compared to the prediction, so any systematic error in cluster identification has
reduced this discrepancy. In other words, our observed discrepancy is a lower limit to the
actual discrepancy, which may be larger than $2.5\sigma$ due to the identified clusters and voids
being imperfect tracers of the late-ISW temperature distribution. In reality, the total late-ISW signal is the
superposition of signals from very large numbers of voids and clusters, and it is not clear the extent to which
the largest voids and clusters individually produce local peaks in the filtered late-ISW map.
Since our predicted maximum signal is consistent with that from N-body simulations,
it seems likely that large structures do actually produce local peaks in the filtered late-ISW map.
In the limit that the void and cluster locations from GNS08 do not
correlate at all with peaks in the late-ISW distribution, the model signal will be zero; but
then the mean signal at the GNS08 locations is $3.5\sigma$ away from the expected null signal.

The uncertainty in the difference between the observed signal and the theoretical maximum signal
is dominated by the primary temperature anisotropies which are uncorrelated with the late-ISW signal.
When stacking at late-ISW peak locations, these primary fluctuations average to zero, with a Poisson error.
This uncertainty can be reduced only by including more peak locations in the average. The current
analysis uses late-ISW tracers from around 20\% of the sky, in a specific redshift range. Using the same
analysis with a half-sky survey at the same cluster and void threshold level
will increase the number of voids and cluster locations by a factor of 2, reducing the Poisson error
by a factor of $\sqrt{2}$ and potentially increasing the detection significance of an underlying
signal discrepancy from $2.5\sigma$ to $3.5\sigma$. Extending the redshift range to lower $z$,
where the late-ISW effect is stronger for a given structure in standard $\Lambda$CDM models, can further increase the census of
clusters and voids, potentially pushing the discrepancy to greater than $4\sigma$. However, complications
at lower redshifts arise due to differing angular sizes of voids on the sky. A stacking analysis
at locations of lower-redshift SDSS voids has seen no signal clearly different from null \cite{ilic2013},
suggesting that the discrepancy here and in GNS08 may be due to noise. Upcoming optical
surveys like Skymapper \cite{skymapper} and LSST \cite{lsst} promise a substantial expansion in the
census of voids and clusters suitable for late-ISW peak analysis.

If the discrepancy is confirmed with increased statistical significance by future data,
this would suggest that the late-ISW peak signal
is larger than in the standard $\Lambda$CDM model. Since the clusters and voids considered are on
very large scales, they are in the linear perturbation regime, and the physics determining
their late-ISW signal is simple, so it is unlikely that the theoretical signal in $\Lambda$CDM is being
computed incorrectly. While the association of voids or clusters with peaks in the late-ISW distribution
is challenging, any inefficiency in this process will only increase the discrepancy between theory
and measurement. The remaining possibility would be that the assumed expansion history in $\Lambda$CDM
is incorrect, and that the discrepancy indicates expansion dynamics different from that in models
with a cosmological constant. Any such modification must change the peak
statistics of the late-ISW temperature component while remaining within the bounds on the
total temperature power spectrum at large scales, and must be consistent with measurements
of the cross correlation between galaxies and microwave temperature. Given the
limited number of observational handles on the dark energy phenomenon, further work to understand
the mean peak late-ISW signal in current data, and its measurement with future larger galaxy surveys,
is of pressing interest.\\

\begin{acknowledgments}
The authors thank Ben Granett,  Seshadri Nadathur, Mark Neyrinck, and Uros Seljak for useful discussions. SA is grateful to Federico Bianchini
for introducing him to the CLASS code and Julien Lesgourgues for helpful suggestions on modifying it. SA and AK are supported in part by
the National Science Foundation under grant NSF-AST-1312380. AK thanks the International Center for Theoretical Physics, where this work was initiated during a stimulating conference.
We have used the \verb|HEALPix| package \cite{HEALPix} for map pixelization and the NASA Astrophysical Data System for bibliographic information.
\end{acknowledgments}

redpajama_set_name: RedPajamaArXiv


text:
Q: How can I dynamically switch the output destination of a script or command? I ran a shell command the other day which produced more output than expected.  It was writing to a file on a filesystem with very little available space and could have filled the filesystem.  The command took a long time to run so rather than rerunning it with a different output location, I would like to have been able to switch the output destination while it was running.  Is this possible?
I know that renaming the file wouldn't work because the system uses the inode number rather than the name, what options do I have?

A: Look at this one:
http://etbe.coker.com.au/2008/02/27/redirecting-output-from-a-running-process/

redpajama_set_name: RedPajamaStackExchange


text:
Tag: Demi Lovato
Demi Lovato premieres second single "SUBSTANCE" & reveals tracklisting of new album
A little over a month ago, Demi Lovato announced the release of her eighth studio album "HOLY FVCK", scheduled for August 19th, and also dropped
Demi Lovato releases new single "SKIN OF MY TEETH" & announces new album.
Demi Lovato has officially kicked off a new era in their music career by announcing the release of their eighth studio album, barely one and
Winnetka Bowling League and Demi Lovato collaborate on new single "fiimy (fuck it, i miss you)".
Alternative rock band Winnetka Bowling League joined forces with Demi Lovato on their new single "fiimy (fuck it, i miss you)". The new song was
G-Eazy and Demi Lovato collaborate on new single "Breakdown".
Rapper G-Eazy teamed up with Demi Lovato for the newest single from his upcoming fifth studio album "These Things Happen Too" scheduled for a September
27/03/2021 14/04/2021 by Nikos Vlamis
Demi Lovato had recently announced the release of her seventh studio album, 4 years after her last album "Tell Me You Love Me". After her
Demi Lovato's surprise release of new song "Still Have Me".
Demi Lovato surprised all of her fans yesterday by leaking her new song "Still Have Me" on her Twitter and Instagram account with the caption
Album Releases, New
JoJo released the Deluxe version of "good to know" – listen to all the new tracks!
JoJo fans cannot stop being excited as this year the talented singer has been the gift that keeps on giving. Not only has she released her

redpajama_set_name: RedPajamaCommonCrawl


text:
Alarmed Parents Share The Weirdest Thing They Found On Their Kids' Social Media
Shutterstock / astarot
What's posted on social media sites…stays on social media sites, where for the most part your parents can't see it (or are blocked). 'Cause God forbid they stumble across your account and found out what really goes on Friday nights on the town.
For more stories, you can find the original source thread at the end of the article.
"I was trying to figure out my niece's age, but it was too late to call my mom and ask. I remembered she had an Instagram account, and I thought that might help me figure out how old she was. I looked her up. She has the standard tween Instagram bio about what activities she likes and a list of like 15 of her BFF's, immediately followed by pondering (and I quote) "Mostly why do people hate me."
She's 12. She is definitely 12."
Text Source
"This was probably in the early 2000's. Me and my buddy were off school for the summer and he would hang out my house. Occasionally wed look at adult videos on the family computer.
Then one day my dad comes home from work, comes downstairs and says, 'Hey! You guys missed the bus!' Im like 'uuuhhh… its summer. Theres no school.' My dad responds 'the bang bus.'
Mother of God…we forgot to close the freaking browser."
"I found out my son is an urban explorer. He's 14 and I saw some video of him and his friends sneaking into an old air force base and climbing to the top of an air hangar."
"My younger brother thought that when you entered more searches, it would delete the ones before at some point. So I look on his iPad one day and see a search for lady lumps or intercourse, one of the two. The search after that was cheese. And then cheese cheese. And then cheese cheese cheese. And so on. So many cheeses."
"My 9-year-old son's Google history:
'Do girls in England poo blood for a month?'"
"I have a 6-year-old boy and a 5-year-old girl who are pretty obsessed with Youtube gamers. They narrate their play like they are performing for subscribers and my son actually figured out how to post videos to Youtube. But I did not find this out until they had posted a few already.
They had ridiculous titles where one of them had obviously just been using the next suggested word so it came out like, 'The ghost of the wealthy, but if they didn't then deserve.' and it would be a video of my foot while I was asleep on the couch and you'd hear one of them say, 'Foot.' and then giggle madly and then the video cuts out."
"Can I do the inverse? My dad recently opened an Instagram account, and within 10 minutes of having it, managed to accidentally upload a screenshot of our wifi password to it.
Like, I have no idea how he managed that. Even put a filter on it…for some reason."
"I checked my 11-year-old son's search history to find a number of interesting questions…
Do men grow lady bits?
Will my junk disappear when I'm 18?
Will I become a girl?
How do I save my private part?
I asked him about his search history a couple days later and he told me that some kids in his school told him that when boys turn 18 they turn into girls and lose their junk. Those jerks…"
"I went through my 13-year-old cousin's iPad.
He had searched 'cream pie', 'girls doing a cream pie' and 'cream pie videos.'
After, searches for 'apple pie', 'pizza pie', 'peach pie' and 'raspberry pie' came up, presumably to disguise his actual aims."
"I'm not a parent, but the other day my twelve year old little brother posted a topless photo on Instagram with the caption 'F-Boy'."
"My son has Autism, he is high functioning but still Autistic. He has been mainstream most of his schooling and in the 5th grade one of the boys told the others how to search lady bits on the computer. Well my son in all of his autistic glory was searching 'pagina' instead of the other thing and was only getting pictures of leaves. Poor kid."
"I'm not a parent, but one time my cousin got onto the computer when he was 11 or 12 or so and searched for 'naked girls.' I was there when his stepdad checked through the browser history, and needless to say he and my cousin had a chat about acceptable search terms."
"My kids are too young for twitter or snapchat, but they love to watch Youtube. I started getting notifications a few months ago from people replying to 'my' comments on conspiracy videos. I found out my son has a curiosity about flat earthers and doomsday preppers."
"I hopped on my nephew's tablet and proceeded to pull up the internet browser. Immediately I was staring at a screenshot of an overweight homeless looking Santa knocking the life out of a much younger Mrs. Clause.
I immediately asked my nephew what kind of research he was doing with his Santa video and his face turned fire engine red and he scurried back to his room."
"My 15-year old step bro-in-law used my wifes laptop while he was visiting the house and forgot to clear the history. His google searches included: bosom and girl pussing.
Hmmm, now that I type this out I am wondering if he was just misspelling pissing. That would make a little sense… albeit not comforting."
"When my twins were young and in elementary school, they were looking up the Simpsons and accidentally came across cartoon Simpson's adult films. The computer was in the living room so I heard them giggling and turned to see two guilty little faces. It was so hard not to laugh and so disturbing! What a conversation… the sight of Milhouse and Lisa is forever burned into my retinas."
"I'm not a parent, but when I was a kid I found an adult flash game website. I would go on it whenever I had the chance. Eventually my mom found out and she told my dad to talk to me about it. My dad and I got into the car and he started this serious talk about how 'the internet is a very powerful tool…' I felt really guilty.
Then he told me how to erase the browsing history."
"When I was like 12 my dad found Dragon Ball Z Hentai in my history searches and proceeded to look through all of the pages while I hid in the bathroom pretending to use it.
I remember him yelling my name and having to mentally prepare to deny everything. Im scared as heck to have kids and find their adult film searches."
"My step son is 7 and I found a bunch of searches for:
Dominicans with no hands and feet. Dominicans with no heads. Dominican chests. Dominican torsos. Dominican legs. Dominicans in stores. Dominicans for sale. Silver Dominicans. Black Dominicans. White Dominicans.
I was at a loss of how to bring it up to him. Thankfully, the next day we were in a clothing store and he asked me why Dominicans don't have hands or heads, then why there are so many different colored Dominicans. I remembered the internet searches and became a little upset. I told him to be quiet because what he was saying could be taken offensively by Dominican people. He then got frustrated and loudly said, 'Dominicans aren't people' as he pointed to a statue next to us.
I breathed a sigh of relief and said 'Mannequins.'"
"When he was little, my brother once wanted to help us find a cool new purse to order for my mom's birthday. He image searched 'fun bags', and my parents had to answer a LOT of questions."
"I'm not a parent but one time my mom made me really mad and my dad had to talk to me about how I searched, 'how to kill my mom' and why it's wrong to think killing someone will get me Play Station 2 games."
"A guy on Instagram sent my 12-year-old step-daughter and her friend's pictures of his junk. Not just once, but many times. The police are involved and he has been located in NYC but we have yet to hear anything back yet. Disgusting.
The man is at least 30."
"A dad here. My daughter is in elementary school and she's all about YouTube. (I'm assuming most kids are these days). She normally watches Minecraft or Little Pet Shop videos. I decided to search her history out of curiosity to my horror she was searching GUYS KISSING BEHINDS."
"I found my stepdaughters 'musical.ly' account. She had a bunch of poor attempts at sexy belly dancing to various Evanescence songs."
Points are edited for clarity.


I woke up this morning to the alarm going off. Why else would I wake up? I turned over and opened my eyes and read the numbers on the clock.
I pulled the covers back over my head and told myself that I could squeeze in nine more minutes of sleep if I just hit snooze. I thought about it for a minute and decided against it.
Today was the day. My magic number had finally come up.
I threw back the covers and sat up. Rubbing the sleep out of my eyes, I looked around my room and saw the neatly packed boxes in the corner. My entire life was packed into those boxes. Childhood momentos, clothes, extra food... it was all there.
I got out of bed and streched for what was the last time in this room. I had spent close to 20 years here and today I was leaving for good.
I could hear my parents going through their usual morning rituals - coffee pot being knocked against a cup, the newspaper rustling - and walked out of my room into the hallway.
"Oh, you're awake." My mother looked down the hall to see me walk out. She came towards me with a cup in her hand. "Come, sit down with your father and I."
I followed her to the kitchen and saw a fantastic spread on the table. She'd really gone all out this morning. It was likely the last time I'd ever see them and I guess she wanted me to fill up on her cooking before I left.
"Good morning, son." My dad set the newspaper down and seemed to want to talk to me. In all the years I sat at this table for this meal, he'd never set the paper down, never mind wanted to talk to me. Breakfast to him meant catching up on the scores from last night.
"Morning, Dad." I sat in my usual seat and poured myself a glass of orange juice. Mom handed me a plate of pancakes and I took a few. After drowning them in syrup, I began to eat.
"Darren? Can we talk to you?" Mom took her seat and reached for my hand. I put my fork down and let her take it.
"Son, we're very excited for you. This day doesn't happen every day, you know." Dad had taken off his reading glasses and was looking very intently at me. I wasn't sure if it was because he had something important to say or if it was because he couldn't see me.
"I know, Dad. I'm pretty psyched about it too."
"I'm sure you are. I, or rather, your mother and I want you to know that we're proud of you. And we want you to succeed."
"Thanks." I tried to get my hand away from my mother, but she squeezed it and held on to it for dear life.
"Son, if it's possible, we'd like to hear from you every once in a while."
"Um... I'm not sure if I'm allowed to do that. They've been pretty strict about no contact with the past from what I've heard."
"Yes, we understand that, dear." Another squeeze from my mother. The woman was just not going to let me eat my last breakfast in her house... dammit. "What I think your father wants to say is if you can find a way, somehow, we want to know you're okay."
"I can see what I can do. I don't want to get in trouble or anything..."
"Of course not. Darren, I know some people who might be able to help you. If you want their names, I can give them to you." I already knew that Dad had a list of names and addresses of people drawn up and in his pocket. If I didn't accept it, he'd be hurt. But if I took it and they found it, I could be in for some serious trouble.
"Sure, Dad, I'll take whatever you've got." My mother finally let go of my hand and I finished my meal. My parents sat in silence while I cleaned my plate and went to my room to get ready to leave.
I showered and dressed in the suit I had bought for the day. Looking in the mirror, I barely recognized myself. I was used to seeing myself in a t-shirt and jeans, not a three-piece business suit. I looked like a kid playing with his dad's clothes.
I went back to my room and phoned the contact number to be picked up. After confirming the meeting time - noon - I went back to the kitchen.
My mother burst into tears the minute she saw me. My father's eyes misted up. I felt like a dolt. Being an only child and having this happen to me, it was something they both hoped for and dreaded.
For the remainder of my time with them, we sat at the table and talked about old times and what they planned to do now that they had all this free time on their hands. Because of today, my parents could retire. They'd worked so long to do so much for me, it only seemed right that now that I was leaving, they could rest. Dad told me about the trip they planned on taking across the country. Mom told me about how she was going to join a couple of clubs and volunteer more. I felt good about the plans they'd made and didn't really seem concerned that their lives would go on without me - their only son, their only child. I wondered before today whether I'd feel cheated out of not 'knowing' them longer, but I came to the conclusion that they had their own lives to live. I was just an extension and they would cut me out, slowly, over time no matter what. Today just meant that the cutting would be faster and hurt more.
At quarter to twelve, the phone rang.
"Hello?" I knew who it was and what it was about.
"Darren, your pickup will be there in fifteen minutes. Are you ready?"
"Yep. As ready as I'll ever be."
I hung the phone back up and turned to my parents. I kissed my mother's cheek and shook my dad's hand. I took both of them into a hug and inhaled deeply. My dad's spicy cologne mixed with my mother's fruity perfume - a smell I wanted to hold with me forever.
A few minutes later, the doorbell rang. I opened the door and was met by a muscular man in a suit similar to mine.
"Come with me, please." He turned and started down the walk. Two other men, of roughly the same build, came up to the door. They passed by me and followed my dad into my old room.
I went to the large van parked on the street. Gabe, as his nametage proclaimed, opened the passenger door for me. I climbed in and buckled my seat belt. Gabe went to the other side and got in.
"Well, Darren, how does it feel?"
"Good, good. Nice weather, eh?"
"Yeah. Warm for this time of year."
"Yep. Yep. Good for the farmers, though."
"Yeah." I wanted to sit in silence and think about what was going to happen in a little while. I had no real idea what would happen, but for months now, I'd been imagining what the next few hours would hold.
The other large men loaded my belongings into the back of the van and slammed the doors shut. As they were getting into their seats in the back, I looked towards my old house and saw my parents standing on the front porch - my mother leaning against my father, both of them crying. I could feel my chest tighten and I resolved not to let myself show any emotion in front of these people. I had to be strong - I was a grown man and I needed to start acting like it.
Gabe put the van into gear and slowly pulled away. Vignettes of my life flashed through my mind - playing baseball with the neighbourhood kids in the park at the end of the street, riding bikes up and down the hill on the other side of town, fairs attended, cruising the main street for girls on Friday nights... these were all things that I would remember for the rest of my life. No one could take them away.
Gabe and the other men - Hank and Morty - carried on their own conversation while I was lost in my memories.
And this is where I've been stuck on this story for a year and a half. I've tried a few things, but it gets sappier and sappier every time. Help!
The following comments are for "The Day"


So you have your DIY Minnie Mouse Costume TuTu Skirt all ready to go and are just ready to top off the outfit with the DIY Minnie Mouse Bow Headband, right?! Well today's the day I show you how to make one for yourself. I love love love how this came – so simple and cute and awesome. This post may contain affiliate links.
You can't have a Minnie Mouse costume without mouse ears!
Looking for a DEAL for a Disneyland Trip?? Be sure to check out Getaway Today, they have amazing deals you won't want to miss!
They are mouse ear perfection! And I have the SECRET TRICK to get the ears to stand up….
OK, first up, let's make the ears – fold the felt in half and on the fold edge cut a circle with a little tab on the bottom. So when you open it up it looks kind of like a barbell 😉 Repeat for the other ear. The bar part will be the part that wraps around the headband. Hot glue the bar area and fold it over the headband.
Now – the SECRET TRICK to getting the ears to stand up – insert a small craft stick in the ear. Then hot glue the ear sandwich with the craft stick inside. Repeat for other ear. Voila!!
For the rest, make a bow out of the ribbon. Tie a knot in the thin red ribbon. Make a bundle out of the tulle. Layer it all together and tie the thin red ribbon (with knot in front) around the bundle. Use hot glue where necessary. Then hot glue the bow to the top of the headband, in between the ears. Fun, right?!?!


text:
namespace onnxruntime {

using DefaultIndexTypes = TypeList<int32_t, int64_t>;

namespace op_kernel_type_control {
ORT_SPECIFY_OP_KERNEL_ARG_DEFAULT_TYPE_LIST_ALL_OPSETS(
    kCpuExecutionProvider, kOnnxDomain, Gather, Input, 1, DefaultIndexTypes);

#if !defined(ORT_MINIMAL_BUILD) || defined(ORT_EXTENDED_MINIMAL_BUILD)
// enable all types for layout transformation
ORT_SPECIFY_OP_KERNEL_ARG_REQUIRED_TYPE_LIST_ALL_OPSETS(
    kCpuExecutionProvider, kOnnxDomain, Gather, Input, 1, DefaultIndexTypes);
#else
ORT_SPECIFY_OP_KERNEL_ARG_REQUIRED_TYPES_ALL_OPSETS(
    kCpuExecutionProvider, kOnnxDomain, Gather, Input, 1, int32_t, int64_t);
#endif
}  // namespace op_kernel_type_control

using EnabledIndexTypes = ORT_OP_KERNEL_ARG_ENABLED_TYPE_LIST_ALL_OPSETS(kCpuExecutionProvider, kOnnxDomain,
                                                                         Gather, Input, 1);
ONNX_CPU_OPERATOR_VERSIONED_KERNEL(
    Gather,
    1,
    10,
    KernelDefBuilder()
        .TypeConstraint("T", DataTypeImpl::AllTensorTypes())
        .TypeConstraint("Tind", BuildKernelDefConstraintsFromTypeList<EnabledIndexTypes>()),
    Gather);

ONNX_CPU_OPERATOR_VERSIONED_KERNEL(
    Gather,
    11,
    12,
    KernelDefBuilder()
        .TypeConstraint("T", DataTypeImpl::AllTensorTypes())
        .TypeConstraint("Tind", BuildKernelDefConstraintsFromTypeList<EnabledIndexTypes>()),
    Gather);

ONNX_CPU_OPERATOR_KERNEL(
    Gather,
    13,
    KernelDefBuilder()
        .TypeConstraint("T", DataTypeImpl::AllTensorTypes())
        .TypeConstraint("Tind", BuildKernelDefConstraintsFromTypeList<EnabledIndexTypes>()),
    Gather);

Status GatherBase::PrepareForCompute(OpKernelContext* context, Prepare& p) const {
  p.input_tensor = context->Input<Tensor>(0);
  const TensorShape& input_data_shape = p.input_tensor->Shape();
  p.indices_tensor = context->Input<Tensor>(1);
  const TensorShape& indices_shape = p.indices_tensor->Shape();

  const auto input_rank = input_data_shape.NumDimensions();
  p.axis = HandleNegativeAxis(axis_, narrow<int64_t>(input_rank));

  std::vector<int64_t> shape;
  shape.reserve(input_rank - 1 + indices_shape.NumDimensions());

  // replace the dimension for p.axis with the shape from the indices
  for (int64_t i = 0; i < p.axis; ++i)
    shape.push_back(input_data_shape[narrow<size_t>(i)]);

  for (const auto dim : indices_shape.GetDims())
    shape.push_back(dim);

  for (int64_t i = p.axis + 1; i < static_cast<int64_t>(input_rank); ++i)
    shape.push_back(input_data_shape[narrow<size_t>(i)]);

  p.output_tensor = context->Output(0, TensorShape(std::move(shape)));

  return Status::OK();
}

template <typename Tin>
Status GatherCopyData(const Tensor* indices_tensor, const uint8_t* src_base, uint8_t* dst_base, bool is_string_type,
                      const size_t element_bytes, const int64_t block_size, const int64_t M,
                      const int64_t N, const int64_t data_batch_bytes, const int64_t gathered_batch_bytes,
                      const TensorShape& input_data_shape, const int64_t axis, concurrency::ThreadPool* tp) {
  const Tin* indices_data = indices_tensor->Data<Tin>();

  // Check the indices first in case there's a out of bound index.
  auto axis_dim_limit = input_data_shape[narrow<size_t>(axis)];

  for (int64_t i = 0; i < N; ++i) {
    Tin idx = indices_data[i];
    if (idx < -axis_dim_limit || idx >= axis_dim_limit) {
      return ORT_MAKE_STATUS(ONNXRUNTIME, INVALID_ARGUMENT,
                             "indices element out of data bounds, idx=", idx,
                             " must be within the inclusive range [", -axis_dim_limit, ",", axis_dim_limit - 1, "]");
    }
  }

  auto lambda = [&](int64_t index) {
    int64_t batch = index / N;
    int64_t i = index % N;

    const int64_t src_offset_batch = batch * data_batch_bytes;
    const int64_t dst_offset_batch = batch * gathered_batch_bytes;
    Tin idx = indices_data[i];
    idx = idx < 0 ? idx + static_cast<Tin>(axis_dim_limit) : idx;
    const int64_t src_offset = src_offset_batch + idx * block_size;
    const int64_t dst_offset = dst_offset_batch + i * block_size;

    if (is_string_type) {
      reinterpret_cast<std::string*>(dst_base)[dst_offset / element_bytes] =
          reinterpret_cast<const std::string*>(src_base)[src_offset / element_bytes];
    } else {
      memcpy(dst_base + dst_offset, src_base + src_offset, narrow<size_t>(block_size));
    }
  };
  concurrency::ThreadPool::TryParallelFor(tp, SafeInt<ptrdiff_t>(M) * N, static_cast<double>(block_size),
                                          [&lambda](ptrdiff_t first, ptrdiff_t last) {
                                            for (int index = static_cast<int>(first), end = static_cast<int>(last); index < end; ++index) {
                                              lambda(index);
                                            }
                                          });

  return Status::OK();
}

Status Gather::Compute(OpKernelContext* context) const {
  Prepare p;
  ORT_RETURN_IF_ERROR(PrepareForCompute(context, p));

  const TensorShape& input_data_shape = p.input_tensor->Shape();

  bool is_string_type = p.input_tensor->IsDataTypeString();

  const size_t element_bytes = p.input_tensor->DataType()->Size();
  const int64_t block = input_data_shape.SizeFromDimension(SafeInt<size_t>(p.axis) + 1);
  const int64_t block_size = SafeInt<int64_t>(element_bytes) * block ;
  const int64_t M = input_data_shape.SizeToDimension(narrow<size_t>(p.axis));
  const int64_t N = p.indices_tensor->Shape().Size();
  const int64_t data_batch_bytes = input_data_shape.SizeFromDimension(narrow<size_t>(p.axis)) * element_bytes;
  const int64_t gathered_batch_bytes = N * block * SafeInt<int64_t>(element_bytes);

  const auto* src_base = static_cast<const uint8_t*>(p.input_tensor->DataRaw());
  auto* dst_base = static_cast<uint8_t*>(p.output_tensor->MutableDataRaw());

  concurrency::ThreadPool* tp = context->GetOperatorThreadPool();

  if (utils::HasType<EnabledIndexTypes, int32_t>() &&
      p.indices_tensor->IsDataType<int32_t>()) {
    return GatherCopyData<int32_t>(p.indices_tensor, src_base, dst_base, is_string_type, element_bytes,
                                   block_size, M, N, data_batch_bytes, gathered_batch_bytes, input_data_shape, p.axis, tp);
  }
  if (utils::HasType<EnabledIndexTypes, int64_t>() &&
      p.indices_tensor->IsDataType<int64_t>()) {
    return GatherCopyData<int64_t>(p.indices_tensor, src_base, dst_base, is_string_type, element_bytes,
                                   block_size, M, N, data_batch_bytes, gathered_batch_bytes, input_data_shape, p.axis, tp);
  }

  return ORT_MAKE_STATUS(ONNXRUNTIME, NOT_IMPLEMENTED, "Gather Tind type not supported in this build.");
}

}  // namespace onnxruntime

redpajama_set_name: RedPajamaGithub


There are very few people around the world who have never heard of the famous "Leaning Tower of Pisa".
Pisa's famous tower was completed in 1350 and has attracted tourists for centuries.
The tower can be found in the Field of Miracles near the cathedral (Duomo) and Baptistery (Battistero). It is certainly on of the top attractions in Tuscany Italy.


At www.airconditionerrepaircontractor.com find DIY resources on ac system repair, while you browse through tutorials for bad fan motor issues & profesional advice on air duct cleaning of electric forced air heater. Get estimate on replacing broken ductless air unit for your house or office buildings, as you contemplate home renovation resources by using our website for btu sizing and read mmanuals for help with how to fix problems related to 24 hour air conditioning service. Refer to instructive monthly blogs on cooling, heating and air systems by neighborhood local professionals in your town. Homeowners and building maitenance crew can find 10 best restoration companies in your area for home or business projects. Browse details and explore prices on roof, wall & eave caps, compressor relay, ignitors/reignitors, suction line filter driers, compressors, freon. At www.airconditionerrepaircontractor.com, we provide customers with the tool to connect with their local professionals from the comfort of their house. Below listing pages will help you find air coolers, equipment pads, dryer vents & hoods, diffusers, air quality products, ventilation fans, oils & chemicals, electrical, gas valves / controls sold by your local suppliers. If you have additional questions, use the seller listing page and contact the supplier. Do not forget to browse the weekly deals and offers posted by the contractors while you browse our website.
Browse citywide advertisement and local business directories of Air Conditioner Repair Contractor In Maryville TN for refrigerant leak repair. Search and browse through deals on home heat pump & air conditioner, replacing forced air heating, troubleshooting ductless air condition units for repairs, ac and heating unit maintenance and installation for a office, business, warehouse, home or commercial dwellings. Feel free to also glance over hvac blog site to find assistance, use our program for cost calculations and request job estimates from certified air conditioning specialists near you.
Eric H. did a fantastic job replacing our water heater and was very friendly. Very happy with our service!


Handmade** 100% Copper Water Bottle.
Smooth surface, coated in food lacquer on the outside to protect against scratches and oxidation, this lightweight bottle keeps your water temperate while also transferring the health benefits and taste associated with drinking and eating from copper vessels.
**Every bottle is handmade and so no 2 bottles look the same. Each bottle may have its own aesthetic and beautiful flaws, which gives it its character and individuality.
Copper utensils stain and darken over time. This is the natural process of Oxidation.
Slice a lemon and rub with salt. Apply to the outside of the bottle and squeeze the lemon. To clean the inside, squeeze half a lemon into the bottle and add 1 tbsp of salt. Shake thoroughly, then rinse. Rub the bottle completely dry with a cotton cloth.
Handmade 100% Copper Water Bottle.
Hammered for a honeycomb look and coated in food lacquer on the outside to protect against scratches and oxidation, this lightweight bottle keeps your water temperate while also transferring the health benefits and taste associated with drinking and eating from copper vessels.
Honeycombed hammered surface, coated in food lacquer on the outside to protect against scratches and oxidation, this lightweight bottle keeps your water temperate while also transferring the health benefits and taste associated with drinking and eating from copper vessels.


I wanted to do something drastic to my hair; my mom replied get a tattoo or piercing instead. I am definitely getting a tattoo. I have thought about for years. I have decided I am getting a Jesus fish on my left wrist. I never thought about getting another piercing though. Here are some piercings I like. Many I am too chicken to get but one can dream. Enjoy!
Posted in beauty, fashion, jewelry, Uncategorized and tagged daith piercing, dimple piercing, lip piercing, monroe piercing, nose bridge piercing, nose piercing, piercings. Bookmark the permalink.
I started graduate school this semester and was inspired to have a mini class of my own. Ladies and gentlemen, welcome to Fashion 101. LESSON 5!
Skirts are so fun and amazing! I have also found out there are SO many types of them!
Fitted at the hips then flares out.
A full skirt that reaches to mid-calf or just above ankles, often made up of multiple layers of fabric.
Skirts that bubble. They either look good or bad on people.
There can be mini, long and full circle skirts. A skirt that's cut in sections to make one or more circles with a hole for the waist.
These are really in right now.
Skirts that flare at the end, can be short or long.
Skirts that have room between one's legs and fabric.
Skirts that are high on thee waist.
I like to believe these are named hobble skirts because they make the girls literally hobble place to place. These are definitely vintage.
A skirt that is long, embroidered and pleated. They are worn in India.
The end of the skirt looks like a mermaid.
Skirts that are TOO short.
These are not too short but just right.
Short flounced skirt, popularized in the 80s, started with cheerleaders.
I am not going to lie I forgot these existed. I haven't heard or seen them since I was in 3rd grade. I am now 23.
These are different from pencil skirts, pencil skirts are tighter.
Great blog to help with really specific skirts and skirts in general.
Posted in fashion, Uncategorized and tagged a line skirts, bubble skirts, fit skirts, flared skirts, full skirts, maxi skirts, mini skirts, pencil skirt, peplum skirts, skirts. Bookmark the permalink.
I started graduate school this semester and was inspired to have a mini class of my own. Ladies and gentlemen, welcome to Fashion 101. LESSON 4!
Hope you enjoy some pretty pictures and a few details about special pieces.
Cameo is actually a method of carving into a gem or metalwork and having a raised positive image. The Romans are credited to have this look first. The most popular type of cameo worn is on the neck.
Pendant came from the Latin word "pendere" which means "to hang down". Pendants are a loose-hanging piece of jewelry. Most common in necklaces.
Blogger's favorite type of necklace.
A locket is actually a type of pendant but has a space that can hold a picture or a lock of hair.
Necklaces that are close and tight to the neck.
Pieces of jewelry that wrap around the upper arm.
Jewelry that wraps around your wrist.
Bracelets that are smaller and simple, easily layered.
These are bigger pieces that can wrap around but don't have to.
Jewelry that tells time. It's a beautiful thing!
They come in fish hooks, studs, snaps and pull throughs.
Perfect for girls who don't want to get their ears pierced. I didn't get mine pierced until I was 17. Also some connect to earrings.
I wore these all the time as a little girl.
I am not going to lie, I think these are weird. I have seen some people with gauges so big that a fist can fit through.
My favorite type of jewelry!
They get their own little category because they are cool!
Also if you are ever ordering necklaces online this picture helps me!
Posted in beauty, fashion, jewelry, Uncategorized and tagged bangles, bracelets, brooches, cuffs, earrings, Fashion, jewelry, necklaces, rings, watches. Bookmark the permalink.


text:
Miejscowości w Polsce:
 Turośń Dolna
 Turośń Kościelna

redpajama_set_name: RedPajamaWikipedia


TORRECID MEXICO / In July 1992, Torrecid Group opened a subsidiary in Mexico, the first one in America, following its strategy of developing competitive advantages for the ceramic industry, with a global mentality but with local service.
In October 1994, Torrecid started its production in Mexico through a totally automatized plant in the State of Nuevo Leon.
Service: we take advantage of the proximity to our customers and the technical knowledge we obtain globally from the major ceramic markets in world.
Innovation: through the development of personalized products, that generate Trends in the market.
Process: through efficient quality procedures, and the automatized operation of our plant.
In Mexico we have three offices, they are located in the cities of Monterrey, Tlaxcala and San Luis Potosi.
Since 2005, at our headquarters in Monterrey, we have a showroom where our Clients could find different options and new product developments.
In 2010, Torrecid Mexico successfully completed its first project in relation with digital printing technology at a ceramic producer plant in Mexico.
In order to strengthen the ceramics market in Mexico, through placing ceramic tiles in spaces where traditionally were not used; we offer the technology and the engineering for installing Ventilated Façades.
As part of a global leader organization, we guarantee our Clients the maximum added value as well as the best innovations and future trends through STYLE-CID.


text:
Friday Photo
Go/No Go
I Can't Believe I Did That
Weather Geek
What I Know About…
Young Pilots
What is Air Facts?
Air Facts History
Sarah Fritts
Sarah is dedicated to helping aviators get better at their craft. Sarah is a West Point graduate and Army combat aviator. She flew the OH-58D during the invasion of Iraq in '03. She also flew C-12s in Afghanistan in 2013. She currently flies the King Air 350 full time out of the Portland International Airport. In her spare time she flies the LUH-72 for the National Guard. She recently wrote a book called The Instrument Pilot's Survival Guide. You can find more of her work on her website: ThinkAviation.net
Technique December 26, 2017 December 26, 2017
How to nail taxi instructions every time
Have you ever botched taxi instructions? I cannot count how many times I have made this mistake. The most prominent one I can remember was at Seattle (KSEA) in a King Air many years back. I called ground, proceeded to butcher the response call, and, because it's a Class B airport, I advertised to the world I was an amateur.
Technique June 8, 2017 June 12, 2017
Should I touch that circuit breaker?
Checklists are great, but consider this: can you locate all of the circuit breakers mentioned in the procedures in less than five seconds? Why not? It's a bad idea to hunt for circuit breakers during an abnormal situation.
Technique May 19, 2016 May 23, 2016
What every VFR pilot needs to know about arriving IFR traffic
VFR pilots operate in the same airspace as commercial IFR jet aircraft without having to ever hit the push-to-talk button. Most of the time things go just fine and the two operate without running into each other. Not having a requirement to talk to anyone doesn't alleviate your responsibility as a small airplane driver to understand the airspace around you, though.
Did you know that most of the articles at Air Facts are written by readers like you? You do not have to be Richard Collins or Ernest Gann--simply a GA pilot with a story you'd share with friends sitting in the hangar. Share your experience on any aspect of GA transportation flying, whether for business or pleasure. Photos are an added bonus.
Send your story to: editor@AirFactsJournal.com
About Air Facts
Air Facts was first published in 1938 by Leighton Collins and relaunched in 2011 as an online journal by Richard Collins and Sporty's Pilot Shop. Air Facts still champions, educates, informs and entertains pilots worldwide with real-world flying experiences.
Join thousands of other pilots - sign up for our informative email newsletter. It's completely free, and we will not share your information with anyone.
Copyright 2011-2020, Sportsman's Market, Inc.


The World's End and Zero Dark Thirty actors join Tom Hardy and Noomi Rapace.
Paddy Considine and Fares Fares have been cast in Child 44.
They will join Tom Hardy, Noomi Rapace, Joel Kinnaman and Gary Oldman in the adaptation of Tom Rob Smith's best-selling novel, reports The Wrap.
Hardy will play a Soviet policeman who becomes the target of his own government's suspicions as he investigates a series of child murders.
Fares will play one of Hardy's trusted associates, while Considine's role is yet to be revealed.
Considine made his directorial debut in 2011's Tyrannosaur. He will shortly star in The World's End.
Swedish actor Fares featured in Zero Dark Thirty.
Child 44 is expected to arrive in 2014.
Jason Clarke to join Hardy's 'Child 44'?


text:
Civil war forced the family out of the country when Hassan was just 3, and they ended up in neighboring Kenya with thousands of other refugees.
The Hassans wandered from village to village, sharing tents with other refugees, rarely knowing where they might get their next meal. They eventually ended up in Nairobi, living off the generosity of Somalis who got there first.
The family registered for an immigration lottery, and that's how their mother made it to the U.S., ending up in a Somali community just outside Atlanta and working at a Marshall's clothing store. She would send back $100 a month, which her family used for food, clothes and rent.
Five years later, Hassan found himself on one of those plane flights to Atlanta, where more than 50 immigrants from Africa, including his weeping mother, greeted him and his siblings at the airport.
They learned English at school and other places.
"I remember getting up every day and watching 'Saved by the Bell,' " Hassan said, smiling.
Hassan said he studied hard and spent extra time learning English: "I wanted to express myself and also be valuable."
Some uncles attracted the family to Nashville after hearing of job openings with the Dell computer company.
Hassan ended up working at the West End Avenue Pizza Hut and a security company. Part of Hassan's turf at his security job included the offices of the Tennessee Immigrant and Refugee Rights Coalition.
That's where Hassan fell in love with the idea of helping other new Americans, and he went to Tennessee State University to get a degree in political science. His entire college tuition was paid for with a few grants and two part-time jobs.
Since graduating, Hassan has started a consulting company to help other new Americans, and he has purchased a coffee shop where fellow Africans gather. Hassan spends many hours outside work helping those who have recently immigrated to Nashville.
"My favorite part of coming to America — leaving a place where there were no options in life, coming to a place that is increasingly challenging and rewarding at the same time," he said.
"Here, despite challenges, you are the driver of your destiny."
Reach Brad Schmitt at 615-259-8384 or on Twitter @bradschmitt.
Hassan helps
Mohamed-Shukri Hassan's community activities in Nashville include:
• Mayor's New American Advisory Council
• Nashville International Center for Empowerment
• American Muslim Advisory Council
•A new business incubator for immigrants through Lipscomb University's Andrews Institute for Civic Leadership.
•Som Cafe and Deli, 1040 Murfreesboro Pike, a hangout for people from East Africa.


[100% Working Unlock Methods] Step by step method Bypass Google APK 2019 FRP zte t36 device 2019. Best tools for remove Google account verification by Factory Reset Protection on your device .
Download APK 2019 Bypass Google FRP for models: zte x4212, zte a4860, zte c2841, zte j4713, zte u4499, .


text:
Major fire threat on way to California while fire danger and winter storm expected in Colorado Saturday
Sat, October 24, 2020 by ABC News
HomeNationalMajor fire threat on way to California while fire danger and winter storm expected in Colorado Saturday
BY: DANIEL MANZO, ABC NEWS
(NEW YORK) — The fire danger in parts of the West, especially in parts of California is looking quite significant.
A major offshore wind event is coming to California and extreme southern Oregon. Red flag warnings and fire weather alerts have been posted for large parts of the state including, San Francisco and Los Angeles.
The event will begin on Sunday and last into Tuesday. Wind gusts could top out at 75 mph, and relative humidity could be as low as 4%.
This could be a very significant fire weather set up, especially for the Bay Area, and into parts of Northern California.
The most damaging wind gusts will arrive late Sunday into Monday in the Bay Area and northern California. The National Weather Service is comparing this event setup to the 2017 Wine County Fires and the 2019 Kincade Fire.
All of this comes just weeks after the August Complex burned over 1 million acres of northern California.
In Colorado, the East Troublesome Fire is now at least 188,000 acres and is still only 5% contained. The fire grew by over 17,000 acres on Friday. Although this is less than previous days, that is still quite considerable.
Winds were a little calmer on Friday and relative humidity has been higher, which has helped firefighters battling the blazes. Unfortunately, the winds will strengthen Saturday, and it will be another challenging day for fire containment efforts in Colorado.
Red flag warnings have been issued for parts of Colorado and Utah, where wind gusts to 60 mph can be expected Saturday, and relative humidity as low as 10%. These conditions could produce more fires and rapid fire spread.
The relatively good news is that a winter storm is on the way to Colorado, and a widespread snow event is expected to arrive in Colorado Saturday night, which will greatly help the firefighting efforts.
Winter weather alerts stretch from Washington to Iowa Saturday morning. This includes a winter storm watch for Denver, and the Colorado Rockies, where the fires are burning.
Some snow may even make it into the Twin Cities metro region, which has now seen its snowiest October on record with 8.9 inches.
Spokane, Washington, got 6.8 inches of snow on Friday, which made it their snowiest October day on record. Around a foot of snow has also been reported in the mountains of western Montana. Snow totals in parts of the highest peaks of Montana could top out at 18 inches. The heavy snow and cold will expand south and east through the weekend.
Through Monday, over 12 inches of snow in parts of the Colorado Rockies and 3 to 6 inches through parts of the central and northern Plains are expected.
By Monday some of the snow will likely make it into parts of Kansas, Oklahoma and Texas. Some of the snow is likely to fall as mixed precipitation and could create icy conditions close to the I-34 corridor, especially near Oklahoma City and northern Texas.
Behind this storm, winter air will race down into the central and northern U.S. Wind chills on Sunday morning will be into the negatives from Idaho to North Dakota. Island Park, Idaho, is expected to have a -17 wind chill.
You Might Also Like These...
California massacres suggest phenomenon of 'mass shooting contagion': Experts
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Illinois man charged with setting fire to Planned Parenthood clinic
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7 killed in mass shooting in San Mateo County, California: Report
Apple AirTags causing major security concerns over reports of stalking


Fortunately, basic insulation and air-sealing upgrades can be done very affordably, enabling homeowners to cut monthly utility expenses, improve interior comfort and also improve home value. But to make these improvements, it's important to hire a full-service insulation contractor. "Full-service" means that the contractor has the training, experience and capability to install a wide range of insulation types. In contrast, some insulation companies can only install one or two types of insulation.
There are many different types of insulation. Factors like location, moisture conditions, installation requirements and local building codes determine which types of insulation should be used in various parts of your house. Since Energy Plus is a full-service insulation contractor, we can help you select the insulation that will provide the best value and energy savings for your home.
Why put up with rooms that are too cold or too hot, and a monthly utility bill that's too high? During a free home insulation inspection by Energy Plus, you'll learn how comfort and energy problems can be solved by installing the right insulation in the right way. An insulation upgrade is a "once-and-done" improvement that requires no maintenance and never wears out. Your home will be more comfortable and you'll pay less to keep it that way for as long as you live there.


In all honesty, there are a lot of things that you shouldn't be throwing down the drain (or your garbage disposal, or even your toilet).
2019 Food & Beverage Trends We Can't Wait to Sink Our Teeth Into - Netplus Marketing, Inc.
To stay relevant in 2019 on the search network, you can't just sit back and watch 2018 campaigns sink.
My inspector didn't find it as funny as I did!
AFL 2019: The six teams an AFL legend simply can't trust.
Consequently, your sink is dripping, or if you hear your toilet running frequently, get replacement parts and give it a try.
... 3 days since I found out I am pregnant and it hasn't sink in yet. I need to stop waiting for my period and get with the pregnancy plan.
To all these elements, don't forget to add an accent of color and a touch of copper. Bleu and olive green will be trendy!
This class will work on refining skills through repetition and teacher feedback. Can't make that tall, even cylinder? Do your bowls all sink or look uneven?


Hi, I am Jessica! I am dedicated to the marine underwater life. The past six years I have been studying to become a marine biologist and communicator. In 2018 I have spent six months working with fisheries and fish ecology for the organisation 'Marine Conservation Philippines'. This year (2019) I will move to Norway to start my PhD on sustainable harvesting of marine fish working for the University of Bergen. I enjoy scuba diving and have dived at several locations around the world. This year my goal is to learn to read waves and get into surfing.
Marine protected areas (MPAs) are well-known and used globally to protect and maintain biodiversity. It can also serve the purpose of protecting natural and cultural resources. Generally, it is an area in the ocean where human activities are more strictly regulated. The concept can be great for both people and the marine ecosystem. However, considering both people and marine life in a balance is difficult. Failing to find this balance is where marine protected areas might suffer and even lose their purpose. Yet, marine protected areas can maintain food sources, provide income and jobs whilst protecting biodiversity.
Conservationists usually consider both marine life and humans, however at times the human aspect does become forgotten. This is where MPAs may suffer due to a lack of support for the MPA by the people, which can lead to poor management or no management at all. If humans are forgotten in the process of implementing an MPA, it can lead to no one honouring the rules set up.
Especially in small communities dependent on fisheries as a source of food and income it is important to consider how a protected area can be organised to also benefit people. Since these communities are highly dependent on the ocean for food and income, forgetting humans in local communities could put them at risk. That is why governments and other organisations need to consider the human aspect and encourage people before implementing a protected area. Without the support of the people the MPA stands no chance of being effective.
Tubbataha Reef in the Philippines, which celebrates its 30 years of being a marine protected area this year. Credit: Jessica Tengvall.
Marine protected areas have the potential of having such a great impact in these communities that we cannot afford to implement what is often referred to as paper-MPAs. When a protected area is called a paper-MPA, sometimes it stems from the fact that they have only been implemented to "look good". These types of MPAs do not consider people or marine life. In this case, paper-MPAs are merely designated areas usually of no significance for anything or anyone. Thus, enforcement becomes lost and MPAs actually lose the effect that they can have.
There can often be a tendency to not uphold the interest of marine protected areas due to a lack of support from the community, especially when MPAs come across as not being beneficial or relevant for people. However, the lack of relevance can be overcome by including people in the process.
In local communities the enforcement of an MPA needs to be supported by the community in which the area exists. When MPAs are implemented without passion and encouragement from governments and organisations it can lead to non-supportive people. Encouragement should occur before the process of implementation begins. The MPA should be brought to local communities in a suggestive format to give people a chance to consider the restrictions and give suggestions. People should feel that the MPA is theirs and that they are in control of it. This does not mean that governments or organisations should not be involved in implementing and enforcing the MPA. They should merely act as providing guidance, suggestions and continuously monitor the MPA.
By encouraging people and letting everyone feel that MPAs are publicly owned might lead to more effective MPAs. Paper-MPAs would be avoided since people would have a say about where and what restrictions should apply. Marine protected areas are for everyone to benefit from – both humans and marine life alike. This can provide a sustainable sea where humans and marine life simpler can live in harmony with each other.
Older PostHey! Beach managers! Leave that seaweed alone!


...that Jacob Keyes' pipe can be found sticking out of his Flood body?
This article is about the installation. For the weapon-mounted telescopic sight, see A2 Scope.
The A2 Hydroelectric Facility is a hydroelectric dam in Tanzania in the East African Protectorate. Located along an unidentified river, it is a part of the Global Water Campaign installations in the jungle south of Mount Kilimanjaro supplying water to the GWC Trans-African Pipelines. By the 26th century, while the main facility of the GWC had fallen into disrepair, it seems that the dam was at least partially active by 2552 as evidenced by newer equipment present in the facility.
During the Battle of Earth on November 17, 2552, after John-117 was recovered from the jungle, Sergeant Major Avery Johnson was captured by Covenant forces and freed by John-117 and Thel 'Vadam. The three of them and all surviving Marines were then extracted by Kilo 023.
Concept art of the facility.


Fully self contained spacious Studio Apartment, with good heating, 32 inch LCD TV with Sky, Queen sized bed, Free Wifi and full kitchen facilities.
Fully self contained spacious One Bedroom Apartment, with good heating, Queen sized bed, 32 inch LCD TV with Sky, Free Wifi and cooking facilities.
Fully self contained spacious One Bedroom Apartment, good heating, 32 inch LCD TV with Sky, Free Wifi and kitchen facilities. Non Refundable INSTANT PAYMENT REQUIRED.
Fully self contained spacious Two Bedroom Apartment, good heating, 32 inch LCD TV with Sky, Free Wifi and kitchen facilities.
Fully self contained spacious Two Bedroom Apartment, good heating, 32 inch LCD TV with Sky, Free Wifi and kitchen facilities. Non Refundable INSTANT PAYMENT REQUIRED.


text:
package org.apache.apex.examples.enricher;

import java.util.Random;

import com.datatorrent.api.Context.OperatorContext;
import com.datatorrent.api.DefaultOutputPort;
import com.datatorrent.api.InputOperator;
import com.datatorrent.common.util.BaseOperator;

/**
 * Generates Subscriber Data:
 *    A Party Phone
 *    A Party IMEI
 *    A Party IMSI
 *    Circle Id
 *
 * @since 3.7.0
 */
public class DataGenerator extends BaseOperator implements InputOperator
{
  public static int NUM_CIRCLES = 10;

  private Random r;
  private int count = 0;
  private int limit = 1000;

  public final transient DefaultOutputPort<byte[]> output = new DefaultOutputPort<>();

  @Override
  public void setup(OperatorContext context)
  {
    r = new Random(System.currentTimeMillis());
  }

  @Override
  public void beginWindow(long windowId)
  {
    super.beginWindow(windowId);
    count = 0;
  }

  @Override
  public void emitTuples()
  {
    if (count++ < limit) {
      output.emit(getRecord());
    }
  }

  private byte[] getRecord()
  {
    String phone = getRandomNumber(10);
    String imsi = getHashInRange(phone, 15);
    String imei = getHashInRange(imsi, 15);
    String circleId = Math.abs(phone.hashCode()) % NUM_CIRCLES + "";
//    String record = MessageFormat.format(baseDataTemplate, phone, imsi, imei, circleId);
    String record = "{" + "\"phone\":\"" + phone + "\","
        + "\"imei\":\"" + imei + "\","
        + "\"imsi\":\"" + imsi + "\","
        + "\"circleId\":" + circleId + "}";
    return record.getBytes();
  }

  private String getRandomNumber(int numDigits)
  {
    String retVal = (r.nextInt((9 - 1) + 1) + 1) + "";

    for (int i = 0; i < numDigits - 1; i++) {
      retVal += (r.nextInt((9 - 0) + 1) + 0);
    }
    return retVal;
  }

  private String getHashInRange(String s, int n)
  {
    StringBuilder retVal = new StringBuilder();
    for (int i = 0, j = 0; i < n && j < s.length(); i++, j++) {
      retVal.append(Math.abs(s.charAt(j) + "".hashCode()) % 10);
      if (j == s.length() - 1) {
        j = -1;
      }
    }
    return retVal.toString();
  }

  public int getLimit()
  {
    return limit;
  }

  public void setLimit(int limit)
  {
    this.limit = limit;
  }
}


text:
Danwon-gu es un barrio de la ciudad de Ansan en Gyeonggi, Corea del Sur.

Administrative divisions

Referencias

Véase también
 Geografía de Corea del Sur
 Organización territorial de Corea del Sur

Ansan


text:
Transfer round-up: Man United want to sign 30-year-old, Arsenal linked with Perisic
Read today's top transfer news and rumours on The Grapevine - The Sport Review's football transfer gossip column
Wednesday 10 April 2019, 08:45 UK
The Grapevine is published every day on The Sport Review
Welcome to the latest football transfer gossip column from The Sport Review, featuring all of the latest Premier League transfer news and rumours.
Here, we look at some of the top football transfer stories from the British and world media in The Sport Review's Grapevine, published every day in the build-up to the 2019 summer transfer window.
It was a busy January transfer window in the Premier League as most of the top teams brought in some reinforcements for the second half of the season.
Attentions will now inevitably turn towards the summer transfer window, as Premier League clubs begin considering bringing in some potential reinforcements ahead of next season.
We'll keep you up to date with the very latest transfer news concerning your club in our daily football gossip and rumours column.
So, with the summer transfer window drawing gradually closer, The Grapevine has the very latest football transfer news from the Premier League's top clubs in the round-up below.
Football transfer news:
Manchester United striker Marcus Rashford, 21, is close to signing a new contract at Old Trafford worth £78m.
Full story: The Daily Mirror
Manchester United are planning to trigger 30-year-old defender Toby Alderweireld's £25m release clause at Tottenham Hotspur. However, they are yet to contact Spurs.
Full story: The Sun
Liverpool FC could lose 18-year-old Portuguese midfielder Rafael Camacho this summer after contract talks stalled.
Full story: Sky Sports
Gareth Bale's agent says the 29-year-old international is happy at Real Madrid and the winger has no plans to return to the Premier League after reports linking him with Manchester United.
Ander Herrera, 29, will listen to offers from other clubs and has not yet signed a new contract at Manchester United because he and the club "do not think the same".
Full story: ABC
North London rivals Arsenal and Tottenham are both interested in signing Inter Milan and Croatia midfielder Ivan Perisic, 30, this summer.
Full story: Corriere dello Sport via Sport Witness
Eden Hazard, 28, will refuse to sign a new contract at Chelsea FC, even if the club decide to play hardball with Real Madrid.
Full story: The Daily Telegraph
Duncan Castles: Man United could rival Man City for 19-year-old defender
Rio Ferdinand hails Scott McTominay after Man United's 1-0 loss to FC Barcelona