text:
\section{Introduction} \label{sec:intro}
A number of theoretical models predict an anisotropy in the distribution of arrival directions of cosmic rays that results from the distribution of sources in the Galaxy and diffusive propagation of these particles~\citep{erlykin_2006, Blasi:2012jan, Ptuskin:2012dec, Pohl:2013mar,
sveshnikova_2013, Kumar:2014apr, Mertsch:2015jan}.
Although the observed distribution of cosmic rays is highly isotropic, several ground-based experiments located either in the northern or southern hemisphere have observed small but significant variations in the arrival direction distribution of TeV to PeV cosmic rays with high statistical accuracy, in both large and medium angular scales~\citep{nagashima_1998,hall_1999,amenomori_2005,Amenomori:2006bx,guillian_2007,Milagro:2008nov,abdo_2009,aglietta_2009,munakata_2010,IceCube:2010aug,Abbasi:2011ai,MINOS:2011icrc,IceCube:2012feb,IceCube:2013mar,ARGO-YBJ:2013gya,HAWC:2014dec,bartoli_2015,icecube2016,tibet2017,bartoli2018,hawclsa2017}.
The observed large-scale anisotropy has an amplitude of about
$10^{-3}$ and small-scale structures of amplitude of $10^{-4}$ with angular size of $10^\circ$ to $30^\circ$.

For previously reported measurements that rely on time-integrated methods~\citep{Alexandreas1993,Atkins:2003ep}, a difference between the instantaneous and integrated field of view of the experiments can lead to an attenuation of structures with angular size larger than the instantaneous field of view~\citep{0004-637X-823-1-10}. For this analysis, we apply an optimal reconstruction method that can recover the amplitude of the projected large-scale anisotropy.
The limited integrated field of view of the sky in all of these individual measurements also makes it difficult to
correctly characterize such an anisotropy in terms of its spherical harmonic components and
produce a quantitative measurement of the large scale characteristics, such as its dipole or quadrupole component, without a high degree of degeneracy~\citep{SOMMERS2001271}.
The resulting correlations between the multipole spherical harmonic terms $a_{\ell m}$ bias the interpretation of the cosmic ray distributions in the context of particle diffusion in the local interstellar medium (LISM).
In this joint analysis by the High-Altitude Water Cherenkov
(HAWC) and IceCube collaborations we have
combined data from both experiments at 10 TeV median primary particle energy
to study the full-sky anisotropy.
Important information can be obtained from the power spectrum of the spherical harmonic components at low $\ell$ (large scale),
which is most affected by partial sky coverage.
It should be noted that neither observatory is sensitive to variations across decl. bands since events recorded from a fixed direction in the local coordinate system can only probe the cosmic-ray flux in a fixed decl. band $\delta$.
As a result, the dipole anisotropy can only be observed as a projection onto the equatorial plane. However, some information about the vertical component can be inferred from medium- and small-scale structures.

\section{The HAWC Detector}\label{sec:HAWC}
The HAWC Gamma-Ray Observatory is an
extensive air-shower detector array located at 4100\,m a.s.l. on the slopes
of Volc\'{a}n Sierra Negra at $19^{\circ}$N in the state of Puebla, Mexico.
While HAWC is designed to study the sky in gamma rays between 500\,GeV and 100\,TeV,
it is also sensitive to showers from primary cosmic rays up to multi-PeV energies with an instantaneous field of view of about $2$\,sr.

The detector consists of a 22,000 m$^2$ array of 300 close-packed water Cherenkov detectors (WCDs),
each containing 200 metric tons of purified water and four upward-facing photomultiplier tubes (PMTs).
At the bottom of each WCD, three 8-inch Hamamatsu R5912
photomultiplier tubes (PMTs) are anchored in an equilateral
triangle of side length 3.2 meters, with one 10-inch high-quantum efficiency
Hamamatsu R7081 PMT anchored at the center.

As secondary air shower particles pass through the WCDs, the produced Cherenkov light is collected
by the PMTs, permitting the reconstruction of primary particle properties including the local arrival direction,
core location, and the energy.
Further details on the HAWC detector can be found in~\cite{Abeysekara:2017mjj,ABEYSEKARA2018138}.

The light-tight nature of the WCDs allows the detector to operate at nearly 100\% up-time efficiency,
with the data acquisition system recording air showers at a rate of $\sim$ 25 kHz.
With a resulting daily sky coverage of $8.4$\,sr and an angular resolution of $0^{\circ}.4$ for energies above 10 TeV, HAWC is an ideal instrument for measuring the cosmic-ray arrival direction distribution with unprecedented precision.

\section{The IceCube Detector}\label{sec:icecube}
The IceCube Neutrino Observatory, located at the
geographic South Pole, is composed of a neutrino detector in the deep ice and a surface air-shower array.
The in-ice IceCube detector consists of 86
vertical strings containing a total of 5,160 optical sensors, called digital
optical modules (DOMs), frozen in the ice at depths from
1,450 meters to 2,450 meters
below the surface of the ice.  A DOM consists of a pressure-protective glass
sphere that houses a 10-inch Hamamatsu photomultiplier tube together with
electronic boards used for detection, digitization, and readout.  The strings
are separated by an average distance of 125\,m, each one hosting 60 DOMs equally
spaced over the kilometer of instrumented length.  The DOMs detect Cherenkov
radiation produced by relativistic particles passing through the ice, including
muons and muon bundles produced by cosmic-ray air showers in the
atmosphere above IceCube.  These atmospheric muons form a large background for
neutrino analyses, but also provide an opportunity to use IceCube as a
large cosmic-ray detector. Further details on the IceCube detector can be found in~\cite{IceCube:detector}.

All events that trigger IceCube are reconstructed using a likelihood-based method that
accounts for light propagation in the
ice~\citep{Ahrens2004169}.  The fit provides a median angular resolution of $3^{\circ}$ according to simulation~\citep{Abbasi:2011ai}
but worsens past zenith
angles of approximately $70^{\circ}$~\cite{IceCube:detector}.
This is not to be confused with the $\sim 0^{\circ}.6$ angular resolution of IceCube for neutrino-induced tracks of where more sophisticated reconstruction algorithms and more stringent quality cuts are applied.
The energy threshold of cosmic-ray primaries producing atmospheric muons in IceCube is limited by the minimum muon energy required to penetrate the ice. As a result, the primary particle energy threshold increases with larger zenith angles as muons must travel increasingly longer distances through the ice. This is accounted for in the analysis as described in Sec. \ref{sec:dataset}.
Due to the limited data transfer rate available from the South Pole,
cosmic-ray induced muon data are stored in a compact data storage and transfer (DST) format~\citep{Abbasi:2011ai},
containing the results of the angular reconstructions described as well as
some limited information per event. However, detailed information such as PMT waveforms used for these reconstructions is not kept. The preliminary reconstructions encoded in the DST rely on faster, less accurate methods than those applied to the filtered dataset used in most neutrino analyses.

\section{The Dataset}\label{sec:dataset}
The dataset selected for this analysis is composed of 5 years of data collected by the IceCube Neutrino Observatory between May 2011 and May 2016, as well as 2 years of data from the HAWC Gamma-Ray Observatory collected between May 2015 and May 2017.
In order to reduce bias from uneven exposure along R.A., only full sidereal days of continuous data-taking were chosen for this study. The residual contribution of the dipole anisotropy induced by the motion of the Earth around the Sun is estimated to be on the order of $10^{-5}$, which is smaller than the statistical error of this analysis (see section \ref{sec:systematics}).
Cuts are applied to each dataset in order to improve the angular resolution and energy resolution of reconstructed events.
In the case of HAWC these include a cut on the number of active optical sensors in order to increase the information available for the reconstruction of the shower. A cut on the reconstructed zenith angle excludes events with $\theta > 57^\circ$ where the quality of reconstructions decreases rapidly.  A cut is also applied on the variable CxPE40 which corresponds to the effective charge measured in the PMT with the largest effective charge at a distance of more than 40 m from the shower core with CxPE40 $> 40$. The effective charge $Q_\mathrm{eff}$ scales the charge of higher-efficiency central 10-inch PMTs by a factor of 0.46 relative to the 8-inch PMTs so that all optical sensors are treated equally. The value of CxPE40 is typically large for a hadronic events~\citep{Abeysekara:2017mjj}.
Finally, in order to identify and exclude gamma-ray candidates, a cut is applied on $\mathcal {P}$, that describes the ``clumpiness'' of the air shower \citep{Abeysekara:2017mjj} with $\mathcal {P}> 1.8$.
$\mathcal{P}$ is defined using
the lateral distribution function of the air shower.
$\mathcal{P}$ is computed using the logarithm of the effective charge
$\zeta_{i}={\rm{log}}_{10}(Q_{\rm{eff},i})$. For each PMT hit, $i$, an expectation
is assigned $\langle\zeta_i\rangle$
by averaging the $\zeta_i$ in all PMTs
contained in an annulus containing the hit, with a width of 5 meters,
centered at the core of the air shower.
$\mathcal{P}$ is then calculated using the $\chi^2$ formula:
\begin{equation}\label{eq:pinc}
\mathcal{P}= {1 \over N} {\sum_{i=0}^{N}  { {(\zeta_i - \langle\zeta_i\rangle)^2} \over{ {\sigma_{\zeta_i}}^2}   }}
\end{equation}
\noindent The errors $\sigma_{\zeta_i}$ are assigned from a study of a sample strong gamma-ray candidates in the vicinity of the Crab nebula.
The $\mathcal{P}$ variable essentially requires axial smoothness.

In the case of IceCube we apply a cut on the reduced likelihood of the directional reconstruction ($\mathrm{RlogL} < 15$), defined as the best-fit log-likelihood divided by the number of degrees of freedom in the fit~\citep{Ahrens2004169} which gives an estimate of the goodness of fit for the angular reconstruction. There is also a cut on the number of \emph{direct} photoelectrons and the corresponding length of the track  $N_\mathrm{dir} > 9 \cos(\theta)$ and $l_\mathrm{dir}> 200 \cos(\theta)$~meters. This cut depends on the reconstructed zenith angle $\theta$ in order to preserve sufficient statistics near the horizon.
Photons are considered direct when the time \emph{residual} (i.e., the delay in their arrival time due to scattering in the ice) falls within a time window of -15 ns to +75 ns with respect to the geometrically expected arrival time from the reconstructed track~\citep{Ahrens2004169}.

\begin{table*}[ht]
\centering
\scriptsize
\begin{tabular}{p{0.19\textwidth}|p{0.10\textwidth} | p{0.13\textwidth} | p{0.10\textwidth} | p{0.13\textwidth}}
 &\multicolumn{2}{|l}{\small \bf{IceCube}} & \multicolumn{2}{|l}{\small \bf {HAWC}} \\  \hline
Latitude& \multicolumn{2}{|l}{90$^\circ$ S} &  \multicolumn{2}{|l}{19$^\circ $ N}\\
Detection method &  \multicolumn{2}{|l}{muons produced by CR}  &  \multicolumn{2}{|l}{air showers produced by CR and $\gamma$}  \\
Field of view  &  \multicolumn{2}{|l}{-90$^\circ$/-16$^\circ$ ($\delta$), ${\sim}$4 sr (same sky over 24h)} &  \multicolumn{2}{|l}{-30$^\circ$/68$^\circ$ ($\delta$),  ${\sim}$2 sr (8 sr observed/24 h)}\\
Livetime & \multicolumn{2}{|l}{1742 days over a period of 1826 days}  &  \multicolumn{2}{|l}{519 days over a period of 653 days} \\
Detector trigger rate & \multicolumn{2}{|l}{2.5 kHz} &  \multicolumn{2}{|l}{25 kHz}   \\ \hline
 & Quality cuts & Energy and quality cuts &  Quality cuts & Energy and quality cuts \\ \hline
Median primary energy & $20$ TeV & $10$ TeV &  $2$ TeV & $10$ TeV \\
Approx. angular resolution &  $2^\circ - 3^\circ$ & $2^\circ - 6^\circ$ &  $0.4^\circ - 0^\circ.8$ & $0.4^\circ - 1^\circ.0$ \\
Events & $2.8 \times 10^{11}$ & $1.7 \times 10^{11}$ & $7.1  \times 10^{10}$  & $2.8 \times 10^{10}$
\end{tabular}
\caption{
\small Comparison of the IceCube and HAWC datasets. The median primary particle energy, angular resolution and number of remaining events is shown in the sub-columns after applying only quality cuts and after applying both energy and quality cuts. The angular resolution of IceCube corresponds to the DST dataset that relies on faster, less accurate reconstructions as well as less stringent quality cuts. The energy cuts applied are chosen to lower the median energy of IceCube data from 20 TeV down to 10 TeV. In the case of HAWC, the cuts are aimed to raise the median energy of HAWC data from 2 TeV up to 10 TeV.
} \label{tab:observatories}
\end{table*}

Table \ref{tab:observatories} shows the characteristics of both experiments next to each other.
The two detectors have different energy responses and this results in a difference in the median energy.
In order to select data that are consistent between the two detectors, we have applied additional cuts on the reconstructed energy of events:
in the case of HAWC we use an energy reconstruction based on the likelihood method described in~\cite{hamphel2017} to select
events with reconstructed energies at or above 10 TeV.
In the case of IceCube we apply a cut in the two dimensional plane of number of hit optical sensors (which act as a proxy for muon energy) and the cosine of the reconstructed zenith angle, as described in \cite{IceCube:2012feb}.
As a result of the overburden of ice described in Sec.~\ref{sec:icecube}, for a given number of hit optical sensors, events at larger zenith angles are produced by cosmic-ray particles with higher energy~\citep{IceCube:2012feb,icecube2016}.
The energy resolution is primarily limited by the relatively
large fluctuations in the fraction of the total shower energy
that is transferred to the muon bundle and is of the order of 0.5 in
$\log_{10}(E/\mathrm{GeV})$~\citep{icecube2016}.

\begin{figure}[h]
\begin{center}
\includegraphics[width=0.98\columnwidth]{CRAI3HW2yr_Acceptance_sine-log.pdf}
    \caption{Distribution of events as a function of decl. for IceCube and HAWC. The figure shows the two datasets before and after applying energy and quality cuts. Restricting datasets to overlapping energy bins significantly reduces statistics for HAWC. The rates are dominated by events with energies near the threshold of each detector.
By imposing an artificial cut on low energies in the HAWC data, the detector response flattens since it becomes less dependent of zenith angle.
The statistics in HAWC with 300 tanks before cuts are comparable to one year of IceCube with 86 strings.}
        \label{fig:detector_acceptance}
        \end{center}
\end{figure}
\begin{figure}[h]
\begin{center}
\includegraphics[width=0.98\columnwidth]
{CRAI3HW2_energy_dist_noratio.pdf}
              \caption{
	Energy distribution of the final event selection for the two datasets based on Monte Carlo simulations.
              }
        \label{fig:energy_dist}
\end{center}
\end{figure}
\begin{figure}[h]
\begin{center}
\includegraphics[width=0.98\columnwidth]{energy_vs_dec.pdf}
\caption{Median energy as a function of decl. for Monte Carlo simulations before and after applying energy cuts.}
        \label{fig:energy_dec}
\end{center}
\end{figure}
Figure~\ref{fig:detector_acceptance} shows the distribution of data as a function of decl.
The resulting energy distribution of the two datasets is shown in Figure~\ref{fig:energy_dist}.
As a result of the applied energy cuts, both cosmic-ray data sets have a median primary particle energy of approximately 10 TeV with little dependence on zenith angle (Figure~\ref{fig:energy_dec}). The energy response of the observatories covers a 68\% range of approximately 3 TeV - 40 TeV, in the case of IceCube, and 2.5 TeV - 30 TeV for HAWC around the median energy.

The two experiments have different response to the cosmic ray mass composition. This is largely due to the detection method.
Particles entering Earth's atmosphere (15 to 20 km above sea level) interact with nuclei in air and produce a cascade of secondary particles. This particle cascade continues to grow until ionization becomes the dominant energy loss mechanism. The depth X$_\mathrm{max}$ at which this happens depends on both the energy of the primary particle, and its mass. Lighter nuclei penetrate deeper than heavier nuclei. As a result, the altitude of extended air shower arrays such as HAWC
can affect the response of the detector to different nuclei since they are sensitive to the electromagnetic component of the particle shower. In contrast, the IceCube in-ice detector observes cosmic rays through the detection of deep penetrating muons produced from the decay of charged pions and kaons generated in the early interactions.
As a a result, for the same composition, IceCube's response to different cosmic-ray nuclei differs from that of HAWC.

If the first interaction occurs at a lower air density (and higher elevation), mesons are more likely to decay to muons (and neutrinos) instead of re-interacting and producing lower energy pions and other secondary particles. As a result, the two experiments react differently to changes in atmospheric temperature and pressure.
\begin{table}[h]
\centering
\begin{tabular}{l|l|l}
 & IceCube (10 TeV) & HAWC (10 TeV)  \\ \hline
Proton & 0.756 $\pm$ 0.018 & 0.6160 $\pm$ 0.0054 \\
He & 0.195 $\pm$ 0.009 & 0.3110 $\pm$ 0.0014 \\
CNO & 0.028 $\pm$ 0.004 & 0.0467 $\pm$ 0.0004 \\
NeMgSi & 0.013 $\pm$ 0.002 & 0.0191 $\pm$ 0.0001  \\
Fe & 0.008 $\pm$ 0.002 & 0.0078 $\pm$ 0.0001 \\
\end{tabular}
\caption{
\small Relative mass composition for 10 TeV median energy cosmic-rays in the two samples as determined from {\tt CORSIKA} Monte Carlo simulations~\citep{corsika}
weighted to a Polygonato spectrum~\citep{horandel}.
Errors reflect statistical uncertainties in the simulation datasets.
} \label{tab:composition}
\end{table}
The data from both experiments are dominated by light nuclei (protons and alpha particles) as can be seen in Table \ref{tab:composition}.
All of the cuts applied were chosen based on {\tt CORSIKA} Monte Carlo simulations~\citep{corsika} weighted to a Polygonato spectrum~\citep{horandel} and detailed simulations of the detector response.

\section{Analysis}
We compute the relative intensity as a function of J2000 equatorial
coordinates ($\alpha$, $\delta$) by binning the sky into an
equal-area grid with a bin size of $0^\circ.9$ using the
{\tt HEALPix} library~\citep{Gorski:2005apr}.
The angular distribution can be expressed as $\phi(\alpha, \delta) = \phi^\mathrm{iso} I(\alpha, \delta)$, where $\phi^\mathrm{iso}$ corresponds to the isotropic flux (i.e., the flux averaged over the full celestial sphere), and $I(\alpha, \delta)$ is the {\it relative intensity} of the flux as a function of R.A. $\alpha$ and decl. $\delta$ in celestial coordinates.
Given that cosmic rays have been observed to be mainly isotropic, the flux is dominated by the isotropic term and therefore the {\it anisotropy} $\delta I = I-1$ is small.

The relative intensity gives the amplitude of deviations in the number of counts $N_\mathfrak{a}$ from the isotropic
expectation $\langle N_\mathfrak{a} \rangle$ in each angular bin $\mathfrak{a}$. The residual anisotropy $\delta I$ of the distribution of arrival directions of the cosmic rays is calculated by subtracting a reference map that describes the detector response to an isotropic flux
\begin{equation}
\delta I_\mathfrak{a} =  \frac{N_\mathfrak{a}- \langle N_\mathfrak{a}  \rangle}{\langle N_\mathfrak{a}  \rangle}~.
\label{eq:ri}
\end{equation}
In order to produce this reference map, we must have a description of the arrival direction distribution if the cosmic rays arrived isotropically at Earth.

Ground-based experiments observe cosmic rays indirectly by detecting the secondary air shower particles produced by collisions of the cosmic-ray primary in the atmosphere.
The observed large-scale anisotropy has an amplitude of about $10^{-3}$ but our simulations are not sufficiently accurate to describe the detector response at this level. We therefore calculate this expected flux from the data themselves in order to account for detector dependent rate variations in both time and viewing angle.
For Earth-based observatories, such a method requires averaging along each decl. band, thus washing out the vertical dependency (i.e. as a function of decl. $\delta$) in the relative intensity map $\delta I_\mathfrak{a}$.

A common approach is to estimate the relative intensity and detector exposure simultaneously using time-integration methods~\citep{Alexandreas1993,Atkins:2003ep}.
However, these methods can lead to an under- or overestimation of the isotropic reference level
for detectors located at mid latitudes,  since a fixed position on the celestial sphere is only observable over a relatively short period every day.
As a result, the total number of cosmic ray events from this fixed position can only be compared against reference data observed during the same period.
Therefore, time-integration methods can strongly attenuate large-scale structures exceeding the size of the instantaneous field of view~\citep{0004-637X-823-1-10}.

\subsection{Maximum Likelihood Method}
For this analysis, we have relied on the likelihood-based reconstruction described in~\cite{0004-637X-823-1-10} and recently applied in the study of the large-scale cosmic-ray anisotropy by HAWC~\citep{hawclsa2017}.
The method does not rely on detector simulations and provides an optimal anisotropy reconstruction and the recovery of the large-scale anisotropy projected on to the equatorial plane for ground-based cosmic ray observatories located in the middle latitudes as HAWC.
The generalization of the maximum likelihood method for combined data sets from multiple observatories that have exposure to overlapping regions of the sky is described in Appendix~\ref{sec:lh}.

\subsection{Statistical Significance}
In order to calculate the statistical significance of anisotropy features in the final reconstructed map, \cite{0004-637X-823-1-10} generalizes the method in \cite{Li:1983fv} to account for the optimization process of the time-dependent exposure.
The significance map (in units of Gaussian $\sigma$) is then calculated as
\begin{equation}\label{eq:significance}
  S_{ i } = \sqrt{2}\left(-\mu_{ i ,\rm on}+\mu_{ i ,\rm off} + n_ i \log\frac{\mu_{ i ,\rm on}}{\mu_{ i ,\rm off}}\right)^{1/2}\,.
\end{equation}
For each pixel $i$
in the celestial sky, we define expected {\it on-source} and {\it off-source} event counts from neighbor pixels in a disc of radius $r$ centered on that pixel. For this analysis we have chosen a radius of 5$^\circ$.  Given the set of pixels $\mathcal{D}_ i $, the observed and expected counts are
\begin{align}
  n_{ i } &= \sum_{ j \in\mathcal{D}_{ i }}\sum_{\tau}n_{\tau  j }\,,\\
  \mu_{ i ,\rm on} &=  \sum_{ j \in\mathcal{D}_{ i }}\sum_{\tau}\mathcal{A}_{\tau j }\mathcal{N}_\tau I_{ j }\,,\\
  \mu_{ i ,\rm off} &= \sum_{ j \in\mathcal{D}_{ i }}\sum_{\tau}\mathcal{A}_{\tau j }\mathcal{N}_\tau I^{\rm reference}_{ j }\,,
\end{align}
where $\mathcal{A}_{\tau j}$ is the relative acceptance of the detector in pixel $j$ and sidereal time bin $\tau$, $\mathcal{N}_\tau$ gives the expected number of isotropic events in sidereal time bin $\tau$, $I_{j}$ is the relative intensity, and where $I=I^{\rm reference}+I^{\rm residual}$ is divided into a contribution from the reference map and the residual relative intensity.
For small-scale features, $I^{\rm reference}$ corresponds to the first 3 spherical harmonic components ($\ell \leq 3$) of the relative intensity.
In order to distinguish excess and deficit, we multiply Eq.~\ref{eq:significance} by the sign of each smoothed pixel $\delta I_i$ in the anisotropy map.

\subsection{Harmonic Analysis and Dipole Fit}
The relative intensity can be decomposed as a sum over spherical harmonics $Y^{\ell m}$,
\begin{equation}
\label{eq:sphHarmonics}
  {\delta I(\mathbf{\mathbf{u}}_i)} =
    \sum_{\ell=1}^{\infty}
    \sum_{m=-\ell}^{\ell} a_{\ell m} Y_{\ell m}(\mathbf{u}_i)\,.
\end{equation}
The vector components of the dipole in terms of the spherical harmonic expansion $Y_{\ell m}$ in equatorial coordinates are related to the
$a_{\ell m}$ coefficients with
\begin{equation}\label{eq:ahlers1}
\boldsymbol{\delta}
\equiv  (\delta_{0h}, \delta_{6h},\delta_{N}) = \sqrt{\frac{3}{2\pi}}(-\Re(a_{11}), \Im(a_{11}),a_{10}) \,,
\end{equation}
where $\Re(a_{11})$ and $\Im(a_{11})$ are respectively, the real and imaginary components of $a_{11}$, and taking into account that $a_{1-1} = -a^*_{11}$ and $a_{10} = a^*_{10}$ (see~\cite{Ahlers:2016rox}).

From equation \ref{eq:ahlers1} and the $a_{\ell m}$ coefficients,
one can obtain the horizontal components of the dipole
$\delta_{0h}$ and $\delta_{6h}$ with respect to the $0$h and $6$h R.A. axes.
The phase and
amplitude of the projected dipole on the equatorial plane are given by
\begin{equation}\label{eq:ahlers2}
 (\delta_{0h}, \delta_{6h}) = (\tilde{A}_1 \cos \alpha_1, \tilde{A}_1 \sin \alpha_1) \,,
\end{equation}
where
$\alpha_1$ is the phase and $\tilde{A}_1$ is the amplitude of the projected  dipole on the equatorial plane and it is related to the true amplitude $A_1$ through the dipole inclination $\delta_0$ with $\tilde{A}_1 = A_1 \cos \delta_0$.
\begin{figure*}[ht]
\begin{center}
\includegraphics[width=0.65\textwidth]{Combined_LS.pdf}
              \caption{Mollweide projection sky maps of (A) relative intensity $\delta I_\mathfrak{a}$ (Eq.~\ref{eq:ri}) of cosmic-rays at 10 TeV median energy
and (B) corresponding
signed statistical significance $S_{i}$ (Eq. \ref{eq:significance}) of the deviation from the average intensity in J2000 equatorial coordinates.
The thick red and blue lines in the figures indicate correspondingly, the node and antinode of the phase in R.A. of the dipole component from the fit.}
        \label{fig:map:ls-comb}
        \end{center}
\end{figure*}

\subsection{Angular Power Spectrum}\label{sec:power_spectrum}
The angular power spectrum for the relative intensity field is defined as:
\begin{equation}
  \mathcal{C}_{\ell} = \frac{1}{2 \ell + 1} \sum_{m=-\ell}^{\ell} | a_{\ell m} |^{2}~~,
   \label{eq:cldef_true}
\end{equation}
for each value of $\ell$.
Since this analysis is not sensitive to the vertical component of the anisotropy, the largest recoverable dipole amplitude $\tilde{A}$ has the terms $m = 0$ missing and we can only measure a pseudo power spectrum $\tilde{\mathcal{C}}_{\ell}$:
\begin{equation}
  \mathcal{\tilde{C}}_{\ell} = \frac{1}{2 \ell} \sum_{m=-\ell, m\neq 0}^{\ell} | a_{\ell m} |^{2}~~,
   \label{eq:cldef}
\end{equation}
The angular power spectrum provides an estimate of the significance of structures at different angular scales of $\sim$ 180$^\circ/\ell$.
In the ideal case of a $4\pi$ sky coverage, the multipole moments ${a}_{\ell m}$ of the reconstructed anisotropy would carry all the information of the anisotropy (except for the $m=0$ vertical component terms). However, as will be discussed in Section \ref{sec:systematics}, partial sky coverage of individual experiments further limits the amount of information that can be obtained  from the reconstructed pseudo multipole moment spectrum.

\section{Results}\label{sec:results}

The measured relative intensity map is shown in Figure~\ref{fig:map:ls-comb}.
A  smoothing procedure was applied to all maps using a top-hat function in which a single pixel's value is the average of all pixels within a 5$^\circ$ radius.
The map shows an anisotropy in the distribution of arrival directions of
cosmic rays with 10 TeV median primary particle energy that extends across both hemispheres.
The significance (smoothed by summing over pixels) of the IceCube region reflects the much larger statistics in the IceCube dataset compared to that from HAWC at energies of $\sim$10 TeV.
\begin{figure*}[ht]
\begin{center}
\includegraphics[width=0.65\textwidth]{Combined_SS.pdf}
\caption{(A) Relative intensity $\delta I_\mathfrak{a}$ (Eq.~\ref{eq:ri})
after subtracting the multipole fit from the large-scale map and (B) corresponding
signed statistical significance $S_{i}$ (Eq. \ref{eq:significance})  of the deviation from the average intensity in J2000 equatorial coordinates.}
        \label{fig:small:relint}
\end{center}
\end{figure*}

Figure~\ref{fig:small:relint} is the residual small-scale anisotropy after subtracting the fitted multipole from the spherical harmonic expansion
with $\ell \leq 3$
from the large-scale map in Figure~\ref{fig:map:ls-comb} in order to reveal structures smaller than $60^\circ$.
The large-scale structure and significant small-scale structures in Figures~\ref{fig:map:ls-comb} and~\ref{fig:small:relint} are largely consistent with previous individual measurements, as shown in Figure~\ref{fig:phase}.
Observed features extend across the horizon of both datasets. The one referred to as ``region A'' by the Milagro Collaboration~\citep{Milagro:2008nov} roughly extends from $(54^\circ,  -16^\circ)$, to $(78^\circ, 18^\circ)$, in equatorial coordinates ($\delta$, $\alpha$). The so called ``region B''~\citep{Milagro:2008nov} corresponds to the boundary between the excess and deficit regions (see Figure \ref{fig:map:ls-comb}) in the northern sky that appears as a small scale feature (see Figure \ref{fig:small:relint}) for short integration times.

\begin{table*}[ht]
\caption{Spherical Harmonic Coefficients [$10^{-4}$]}
\begin{center}
\footnotesize{
\begin{tabular}{l|lllllllll}
\hline
$\ell$ &$m=$1&2&3&4&5&6&7\\
\hline \\
1 & -13.26 +10.49$i$\\
2 & -0.21 -3.6$i$& -7.20 +2.05$i$\\
3 & { }1.75 -1.7$i$& -2.03 +0.13$i$& { }0.20 +0.17$i$\\
4 & { }1.70 -0.52$i$& { }0.07 +1.69$i$& -0.86 -0.8$i$& -1.19 +0.04$i$\\
5 & { }0.58 +0.27$i$& -0.07 -1.1$i$& -1.64 -0.051$i$& { }0.18 -0.15$i$& -0.11 -1.5$i$\\
6 & { }0.80 -0.88$i$& -0.24 -0.38$i$& -0.10 +0.63$i$& { }0.13 -1.2$i$& { }0.27 +0.47$i$& { }1.65 -0.53$i$\\
7 & { }0.44 -0.67$i$& { }0.37 +0.15$i$& -0.21 -0.14$i$& -0.70 +0.04$i$& { }0.84 -0.27$i$& { }0.13 -0.54$i$& { }0.07 +0.91$i$\\
8 & { }0.26 +0.06$i$& { }0.14 -0.47$i$& -0.39 -0.22$i$& -0.42 +0.72$i$& -0.15 -0.15$i$& -0.72 -0.61$i$& { }0.42 +0.36$i$\\
9 & { }0.11 -0.88$i$& -0.29 -1.3$i$& { }0.22 -0.17$i$& { }0.12 -0.56$i$& -0.01 -0.34$i$& { }0.60 +0.47$i$& -0.06 -0.48$i$\\
10 & { }0.21 -0.97$i$& { }0.25 -0.5$i$& { }0.21 -0.65$i$& { }0.09 -0.088$i$& -0.10 +0.12$i$& { }0.11 -0.017$i$& { }0.02 +0.19$i$\\
11 & { }0.56 -0.39$i$& { }0.06 -0.42$i$& -0.15 -0.68$i$& -0.04 +0.05$i$& -0.26 +0.04$i$& -0.07 -0.26$i$& -0.16 +0.25$i$\\
12 & { }0.40 +0.07$i$& { }0.19 -0.56$i$& -0.27 -0.48$i$& -0.17 -0.1$i$& -0.13 -0.18$i$& -0.03 -0.23$i$& { }0.33 +0.13$i$\\
13 & { }0.45 -0.33$i$& -0.04 -0.69$i$& { }0.17 -0.92$i$& -0.26 -0.6$i$& { }0.13 +0.24$i$& -0.08 +0.02$i$& { }0.04 +0.04$i$\\
14 & { }0.57 -0.16$i$& { }0.13 -0.53$i$& { }0.17 -1.1$i$& -0.31 -0.089$i$& { }0.08 -0.09$i$& -0.25 -0.12$i$& -0.05 +0.22$i$\\
\hline \\
$\ell$ &$m=$8&9&10&11&12&13&14\\
\hline \\
8 & -0.54 +0.19$i$\\
9 & { }0.15 +0.64$i$& -0.04 +0.45$i$\\
10 & { }0.22 +0.12$i$& -0.66 -0.57$i$& -0.26 +0.38$i$\\
11 & { }0.25 +0.02$i$& -0.21 -0.4$i$& { }0.15 -0.25$i$& -0.06 -0.18$i$\\
12 & { }0.37 +0.09$i$& -0.46 +0.25$i$& -0.13 +0.20$i$& -0.08 +0.21$i$& { }0.04 -0.18$i$\\
13 & { }0.11 +0.13$i$& { }0.13 -0.13$i$& -0.35 -0.098$i$& { }0.39 +0.45$i$& -0.01 -0.3$i$& { }0.41 -0.17$i$\\
14 & -0.13 +0.34$i$& { }0.36 -0.11$i$& -0.04 -0.072$i$& -0.11 -0.17$i$& -0.19 +0.32$i$& { }0.13 +0.21$i$& { }0.18 +0.35$i$\\
\hline \\
\end{tabular}
}
\end{center}
\label{tab:alms}
\end{table*}
\begin{figure*}[ht]
\centering
\includegraphics[width=.7\textwidth]{CRAI3HW2yr_faseyamplitud.pdf}
\caption{Reconstructed dipole component amplitude and phase from this measurement along previously published TeV-PeV results from other experiments (adopted from~\cite{Ahlers:2016rox}). The  results shown are from~\cite{hawclsa2017,kgrande2015,baksan2009,aglietta_2009,macro2003,guillian_2007,abdo_2009,bartoli_2015,amenomori_2005,IceCube:2013mar,icecube2016}}
\label{fig:phase}
\end{figure*}
We obtain the $ a_{\ell m}$ through a transformation of spherical harmonics using the {\tt HEALPix} function \emph{map2alm}. The results are presented in  Table~\ref{tab:alms}.
The horizontal components of the dipole obtained from equation
(\ref{eq:ahlers1}) using the $a_{\ell m}$ values in Table \ref{tab:alms} are
$\delta_{0h} =  9.16 \times 10^{-4}$ and
$\delta_{6h} = 7.25 \times 10^{-4}~(\pm0.04 \times 10^{-4})$, respectively, with respect to the $0$h and $6$h R.A. axes.
The dipole amplitude and phase
$\tilde{A}_1=(1.17\pm.01) \times 10^{-3}$,
$\alpha_1=38.4\pm0^\circ.3$ measured in this combined study are shown in Figure~\ref{fig:phase} along with
previously published results from other experiments in the TeV-PeV primary particle energy range. The combined systematic uncertainty in the amplitude and phase of the dipole are expected to be $\delta \tilde{A}_1\sim 0.06 \times 10^{-3}$, and $\delta \alpha_1 \sim 2^\circ.6$ respectively (see section~\ref{sec:syst}).

\begin{figure*}[ht]
\begin{center}
\includegraphics[width=0.7\textwidth]{CRAI3HW2yr_ang_power_spectrum3.pdf}
\caption{Angular power spectrum of the cosmic ray anisotropy at 10 TeV.
The gray band represents the 90\% confidence level around the level of statistical fluctuations for isotropic sky maps.
The noise level is dominated by limited statistics for the portion of the sky observed by HAWC. The IceCube dataset alone has a lower noise level and is sensitive to higher $\ell$ components.
The dark and light gray bands represent the power spectra for isotropic sky maps at the 68\% and 95\% confidence levels respectively.
The errors do not include systematic uncertainties from partial sky coverage.
}
\label{fig:power-spectrum}
\end{center}
\end{figure*}
The angular power spectrum for the combined dataset in Figure~\ref{fig:power-spectrum} provides an estimate of the significance of structures at different angular scales of $\sim$ 180$^\circ/\ell$. Biases are substantially reduced with the likelihood method and by eliminating degeneracy between multipole moments with a nearly full sky coverage. The angular power spectrum can therefore be considered to be the physics fingerprint of the observed 10 TeV anisotropy, providing information about the propagation of cosmic rays and the turbulent nature of the Local Interstellar Magnetic Field (LIMF)~\citep{Giacinti:2011mz,Ahlers:2016rox}. The large discrepancy between the combined and individual datasets is the result of the limited sky coverage by each experiment. This systematic effect will be discussed in Section \ref{sec:systematics}.
A residual limitation in this analysis is the fact that ground-based experiments are generally not sensitive to the vertical component of the anisotropy as discussed by~\cite{hawclsa2017} and~\cite{0004-637X-823-1-10}, as mentioned earlier.

The measured quadrupole component has an amplitude of $6.8 \times 10^{-4}$ and is inclined at $20.7~\pm0^\circ.3$ above (and below) equatorial plane.
As with the dipole, the fitted quadrupole component from the spherical harmonic expansion is also missing the $m = 0$ terms. However, the combination of $a_{21}$ and $a_{22}$ non-vertical quadrupole components can still provide valuable information.
The experimental determination of the vertical components of the anisotropy would require accuracies better than the amplitude of the anisotropy ($\sim 10^{-3}$).
This becomes easier at ultra-high energies where a dipole of much larger amplitude has been observed~\citep{auger1266}.
The full-sky coverage also provides better constraints for fitting the $\ell = 2$ and $\ell = 3$ multipole components and reduces correlations  between spherical harmonic expansion coefficients $a_{\ell m}$.

\section{Systematics Studies}
\label{sec:syst}
\subsection{Overlapping Region}
\begin{figure}[h]
\begin{center}
\includegraphics*[width=0.99\columnwidth]
{CRAI3HW2_1d_projection_overlap_bands.pdf} \end{center}
\vskip -0.7cm
\caption{\small
One-dimensional R.A. projection of the relative intensity of cosmic rays
for adjacent $\delta$ bins in the overlap region at -20$^\circ$
for HAWC and IceCube data.
There is general agreement for large scale structures.
The two curves correspond to different $\delta$ bands. The shaded bands correspond to systematic uncertainties due to mis-reconstructed events,
derived from the relative intensity distributions in adjacent decl. bands between $-25^{\circ}$ and $-15^{\circ}$.
} \label{fig:overlap}
\end{figure}
We have studied two adjacent $\delta$ bands at -20$^\circ$ for HAWC and IceCube data near the horizon of each detector (see Figure~\ref{fig:overlap}). The HAWC band extends from -21$^\circ$ to -19$^\circ$ while the IceCube band extends from -22$^\circ$ to -20$^\circ$.
The large structure between the two datasets is consistent though small structures differ.
It is worth noting that the overlap region is where we expect to find the largest difference in median energy between the two datasets (see Figure~\ref{fig:energy_dec}).
The angular resolution of both detectors also decreases toward the horizon. While HAWC data has a smaller point spread function at this decl. and is sensitive to structures on smaller scales, IceCube has better statistics so the structures are more significant.
One particular feature that stands out is the excess in HAWC around $\alpha=50^\circ$ that coincides with the so called ``region A''.
There appears to be a corresponding small excess in the IceCube data.
It is also worth noting that statistics in this region are quickly decreasing with increasing zenith angle as is the quality of angular reconstructions. As a result, $\delta$ bins closer to the horizon contain a high level of contamination from bins in higher zenith angles.

\subsection{Partial Sky Coverage}\label{sec:systematics}
\begin{figure}[ht]
\begin{center}
\includegraphics[width=0.99\columnwidth]{horiz_toy_dipole_ps.pdf}

              \caption{
 Angular power spectrum as a function of sky coverage for $\ell = \{1, 2, 3, 4\}$. The horizontal axis indicates the maximum decl. $\delta_\mathrm{max}$, keeping $\delta_\mathrm{min} = -90^\circ$ for a dipole injected horizontally in direction $\delta_{6h}$. The partial coverage of sky produces an artificial quadrupole and octupole that decrease in power with greater celestial coverage.
              }
        \label{fig:toy:horiz}
\end{center}
\end{figure}
Incomplete coverage of the sky leads to an underestimation of the angular power of the dipole perpendicular to the axis of rotation of the Earth.
The pseudo-moments of the projected dipole, $a_{11}$ and $a_{1-1}$, are corrected by a geometric factor introduced by~\cite{0004-637X-823-1-10}
in order to estimate the true moments $\hat{a}_{11}$ and $ \hat{a}_{1-1}$.
Furthermore, there is a degeneracy between different $\ell$ pseudo-modes under partial sky coverage that primarily affects the multipolar components $\ell = 2$, $\ell = 3$, and to a lesser degree, $\ell = 4$ as has been previously studied by~\cite{SOMMERS2001271}.
This effect is evident in Figure~\ref{fig:toy:horiz} which corresponds to a dipole injected horizontally in the direction $\delta_\mathrm{6h}$. The partial coverage of the sky produces an artificial quadrupole, octupole and hexadecapole that, in the case of a horizontal dipole, decrease in power with greater celestial coverage. The horizontal axis indicates the maximum observable decl. $\delta_\mathrm{max}$, keeping $\delta_\mathrm{min} = - 90^\circ$.
\begin{figure*}[ht]
\begin{center}
\includegraphics[width=0.65\textwidth]{correlation_matrix_bw.pdf}
        \caption{Correlation matrix for $C_\ell$ modes with partial sky coverage from individual experiments (A, B) and for the combined field of view (C).}
        \label{fig:correlation_matrix}
\end{center}
\end{figure*}
From Figure~\ref{fig:toy:horiz} it is possible to see that the spurious quadrupole and octupole components (which are significant for partial integrated sky coverage) are reduced to an amplitude to order $10^{-5}$ in this analysis.
Figure~\ref{fig:correlation_matrix} shows the correlation matrix~\citep{efstahiou2004} of the different $\ell$-modes up to $\ell=30$ calculated using the {\tt PolSpice}\footnote{
PolSpice website: http://www2.iap.fr/users/hivon/software/PolSpice/.} software package. The correlation between $\ell$-modes due to partial sky coverage is appreciable for larger $\ell$, though to a lesser degree.

\subsection{Seasonal Variations and Local Variations in Solar Time}
The relative motion of the Earth around the Sun can introduce a systematic solar dipole, a dipole anisotropy analogous to the Compton-Getting effect~\citep{Compton:1935} produced by the motion of Earth around the Sun, that points in the direction of Earth's orbital velocity vector.
The influence of diurnal variations (such as the solar dipole) on the sidereal anisotropy can be estimated from the influence it has on the anti-sidereal distribution in a frame with 364.24 cycles per year (see, e.g.~\cite{guillian_2007}). Any significant variations in this frame result from a modulation of the solar frame and represents a systematic effect of the solar frame on the sidereal anisotropy~\citep{icecube2016}. The anti-sidereal distribution of the HAWC dataset has a maximum amplitude of $5 \times 10^{-5}$. Both contamination from the solar dipole and atmospheric pressure variations are included in this systematic.
For IceCube, the same systematic uncertainty is at the level of $\sim 3\times 10^{-5}$. The worst-case uncertainty on the reconstructed phase of the dipole is $\delta \alpha = 2^\circ.6$ and a combined systematic uncertainty of $\delta \tilde{A} = 6 \times 10^{-5}$ for the dipole amplitude.

The solar dipole anisotropy produced by the motion of Earth around the Sun is given by the equation
\begin{equation}\label{eq:solardipole}
\frac {\Delta I} {I} = (\gamma + 2) \frac {v} {c} \cos(\theta_v) \,,
\end{equation}
where $I$ is the cosmic-ray intensity, $\gamma$ is the index of the differential energy spectrum of cosmic rays, $v$ is the velocity of the Earth, $c$ is the speed of light
and  $\theta_v $ is the angle between the direction of the reconstructed cosmic rays and the direction of the velocity vector~\citep{Compton:1935}.
This vector rotates by $360^\circ$ such that, after one year, the effect is ideally completely cancelled for 100\% duty cycle of observation. However, a residual dipole can be introduced if the data does not cover an integer number of years with uniform coverage.
In other words, any gaps in data taking can result in a slight bias to the measured dipole. A solar dipole anisotropy at the level of $10^{-4}$ has been previously observed at
several TeVs~\citep{Amenomori:2004bf,Amenomori:2006bx,abdo_2009,Abbasi:2011ai,IceCube:2012feb,bartoli_2015}. Based on Monte Carlo studies, the residual contribution solar dipole that results from gaps in data taking is estimated to be of order $\sim 10^{-5}$ for the HAWC dataset, which is smaller than the statistical error of this analysis. In the case of IceCube, the detector has an uptime of 99\% (see ~\cite{IceCube:detector})  reduced to an uptime of 95.4\% after selecting full sidereal days. As a result, the systematic effect of data gaps is smaller~\citep{IceCube:2012feb}.

In addition to variations caused by the anisotropy and the solar dipole, there may also be local variations in the detection of cosmic rays caused by changes in atmospheric conditions, such as pressure and temperature, and also by changes in the detector.
For 10 TeV energies, HAWC is located below the shower maximum X$_\mathrm{max}$ for all primary masses. As a result, an increase in pressure leads to an increase of the atmospheric overburden which results in an attenuation of shower sizes. Atmospheric overburden is related to ground pressure $p$ as $X_0 = p/g$, where $g =$ 9.87~m~s$^{-2}$ is the local gravitational acceleration~\citep{ABBASI201340}.
In first order approximation, the simple correlation
between the change in the logarithm of the rate $\Delta\{\ln R \}$ and the surface
pressure change $\Delta P$ is
\begin{equation}\label{eq:pressurecorr}
\Delta\{\ln R\} = \beta \cdot \Delta P
\end{equation}
where $\beta$ is the barometric coefficient~\citep{Tilav:2010jan}.
The variations in atmospheric pressure at the HAWC site are primarily due to \emph{atmospheric tides} driven by temperature and a small contribution from \emph{gravitational tides}~\citep{JGRA:JGRA20326}.
We have studied the effect of atmospheric pressure variations by applying a correction to the data rate to account for measured changes in pressure at the HAWC site. The procedure involves determining the correlation coefficient between the surface pressure data and the detector rate from Eq.~\ref{eq:pressurecorr} in order to weight individual events. This yields a barometric coefficient of $\beta = -0.0071$ hPa$^{-1}$ The residual contamination from atmospheric variations is estimated to be on the order of $\sim 10^{-6}$. Temperature variations in the stratosphere can introduce a similar effect with a 24h cycle and a 365 day cycle. However, this effect is small for latitudes near the equator and in the case of the daily variations, it is a smaller effect than that of pressure variations.

In contrast with HAWC, where the event rate is anti-correlated with atmospheric pressure and with the effective temperature of the stratosphere, the muon rate in IceCube is directly correlated with the effective temperature~\citep{Tilav:2010jan}.
Event rate variations in IceCube have an annual period since one day at the South Pole lasts 365 days instead of 24 hours. In the case of IceCube there are also faster atmospheric variations of lower amplitude but these approximately affect the event rate globally in all azimuth directions (with a maximum Kolmogorov-Smirnov distance below $9.6 \times 10^{-4}$ for daily variations at a 90\% confidence level). Due to the geometry of the detector and its location at the South Pole, this also means that such variations equally affect every angle in R.A.

Seasonal variations in the effective temperature can introduce modulations in the intensity of the Solar dipole. As a result, the Solar dipole would not average to zero over a full year and thus would produce a residual bias. However, the amplitude of the anti-sidereal distribution indicates that this is not a significant effect.

\section{Discussion}

The combined sky map of arrival direction distribution of the 10 TeV cosmic rays collected by HAWC and IceCube and the corresponding power spectrum of its spherical harmonics components, may provide important hints on the origin of the observation. In particular, the angular power spectrum can reveal information about how cosmic rays propagate through the interstellar medium while the large-scale arrival direction distribution provides hints about the structure of the nearby LIMF and the heliosphere.

\begin{figure*}[ht]
\begin{center}
\includegraphics[width=0.65\textwidth]{Combined_w_Labels.pdf}
 \caption{(A) Relative intensity of cosmic-rays at 10 TeV median energy (Figure~\ref{fig:map:ls-comb}(A)) and (B) corresponding small-scale anisotropy (Figure~\ref{fig:small:relint}(A)) in J2000 equatorial coordinates with color scale adjusted to emphasize features. The fit to the boundary between large scale excess and deficit regions is shown as a black crossed curve. The magnetic equator from~\cite{2041-8205-818-1-L18} is shown as a black curve as is the plane containing the local interstellar medium magnetic field and velocity ($B-V$ plane). The Galactic plane is shown as a red curve and two nearby supernova remnants, Geminga and Vela are shown for reference as is Cygnus X-1, a black hole X-ray binary known to produce high energy
$\gamma$ rays~\citep{1538-4357-665-1-L51}.}
        \label{fig:map:comb_feat}
        \end{center}
\end{figure*}
\subsection{Cosmic Ray Propagation in the Interstellar Medium}
The angular power spectrum in Figure~\ref{fig:power-spectrum} shows two different regimes: a steeply falling slope at large scales $\ell =1, 2, 3$ and a softer slope at small scales $\ell > 3$. This suggests that two different mechanisms are responsible for the structures observed in the sky map.
The steep portion of the angular power spectrum may be associated with large scale diffusive processes (over many mean free paths) across the interstellar medium, as suggested by~\cite{erlykin_2006,Blasi:2012jan,Ptuskin:2012dec,pohl_2013,sveshnikova_2013,savchenko_2015,ahlers_2016,0004-637X-835-2-258}.
On the other hand, the softer slope portion appears to be consistent with non-diffusive pitch angle scattering effects on magnetic turbulence within the mean free path~\citep{Giacinti:2011mz} and with that obtained from numerical calculations of sub-PeV protons propagating through incompressible magnetohydrodynamic turbulence~\citep{barquero2016}.
In~\cite{Ahlers2014} it is shown that under certain conditions, those small-scale structures arise as natural consequence of hierarchical evolution of angular scales under Liouville's theorem.

The dipole component of the anisotropy may provide a hint into the direction of the large scale cosmic ray density gradient on the equatorial plane, thus linking the observed anisotropy with possible contributions of the closest sources, such as the Vela supernova remnant at a distance of about 0.3 kpc and with an age of about
11 kyr~\citep{Ahlers:2016rox}. The fact that Vela is located within the large-scale excess region of the sky is consistent with it being a potential source contributing to the large-scale anisotropy.
However, predictions of the anisotropy amplitude depend on many unknown factors such as the actual contributing source (or sources), the diffusion coefficient, and the unknown component of the anisotropy perpendicular to the equatorial plane that complicate such calculations.

The measured amplitude and phase in this study is consistent with
observations from multiple experiments that show a turning point in the energy dependency of the dipole component amplitude at an energy scale of 10~TeV (see Figure~\ref{fig:phase}). After initially increasing with energy, the dipole amplitude begins to decrease above 10~TeV, while the phase has an abrupt change at the 100~TeV energy scale where the amplitude begins to increase again. Cosmic rays with rigidity of 10~TV have a gyro-radius of about 700~AU in a 3 $\mu$G magnetic field, which is comparable to the transversal size of the heliosphere (i. e. perpendicular to the long axis)~\citep{Pogorelov:2009may,Pogorelov:2013jul,1742-6596-719-1-012013}. It is reasonable to assume that at lower energies the heliospheric influence is important, while above 10~TV the interstellar influence is progressively more important~\citep{desilaza2013}.
An understanding of how interstellar propagation of 10~TV-scale cosmic rays influences the arrival direction distribution must, therefore, also take into account heliospheric effects~\citep{Schwadron2014,0004-637X-842-1-54, 2016JPhCS.767a2027Z}. An alternative approach is to study cosmic ray anisotropy above 100 TV rigidity~\citep{IceCube:2013mar, icecube2016}, where the heliospheric influence is expected to be negligible. In this case, the arrival direction distribution can be used to probe the global properties of interstellar turbulence by fitting theoretical models to observations~\citep{0004-637X-835-2-258}. However, at high energies a full-sky study is currently not possible with the dataset used in this analysis due to limited statistics.

\subsection{Large-scale Anisotropy and the Local Interstellar Magnetic Field}
\begin{figure}[ht]
\begin{center}
\includegraphics[width=8.5cm]{chi2fit.pdf}
\caption{$\chi^2$ distribution map for circular fit to boundary between large-scale excess and deficit regions shown in J2000 equatorial coordinates. The black point corresponds to the minimum $\chi^2$ for the center of the circle and the black curve is the fitted circle. The grey points are the selected pixels for the fit. The best fit has a value of $\chi^2$/ndof $=585/579$.
}
\label{fig:chi2fit}
\end{center}
\end{figure}
\begin{figure}[h]
\begin{center}
\includegraphics[width=0.5\textwidth]{limf_circlefit.pdf}
\caption{Circular fit to boundary between large-scale excess and deficit regions shown in J2000 equatorial coordinates along with published magnetic field measurements by~\cite{0004-637X-776-1-30}
inferred from the emission of energetic neutral atoms (ENA) originating from the outer heliosphere by the Interstellar Boundary Explorer (IBEX)~\citep{2041-8205-818-1-L18}, and
~\cite{0004-637X-814-2-112} obtained from the polarization of stars within 40 pc.
}
\label{fig:circlefit}
\end{center}
\end{figure}
Figure~\ref{fig:map:comb_feat} shows the direction of the LIMF from~\cite{2041-8205-818-1-L18} and the corresponding equator (the continuous black line), the so-called $B-V$ plane defined by the LIMF and the direction of the Sun's velocity through the interstellar medium $v_{ISM}$, as well as the direction of the velocity relative to the local standard of rest $v_{LSR}$. The figure also shows the location of the Geminga and Vela supernova remnants as possible contributing sources, and those of the Cygnus X-1 X-ray binary and Galactic center GC for reference. The location of the Galactic plane is shown as a red line.
A fit to the plane defined by the small-scale feature that marks the boundary between the excess and deficit regions ($\sim 115^\circ$ R.A.) is shown in Figure~\ref{fig:chi2fit}. The fit yields a vector pointed towards
$(\alpha_\mathrm{fit},\delta_\mathrm{fit}) = (229.2\pm 3^\circ.5,  11.4\pm 3^\circ.0)$
in J2000 equatorial coordinates, as shown in Figure~\ref{fig:map:comb_feat}, along with the corresponding equator (the crossed black curve).
The direction is located $9^\circ$ from the LIMF inferred by the Interstellar Boundary Explorer (IBEX) from the emission of energetic neutral atoms (ENA) originating from the outer heliosphere (see ~\cite{0004-637X-776-1-30}. This point is also located $6^\circ.5$ from the LIMF direction
reported by~\cite{2041-8205-818-1-L18}
and consistent with the average LIMF direction
obtained from the polarization of stars within 40 pc by~\cite{0004-637X-814-2-112}.
This is shown in Figure~\ref{fig:circlefit} and summarized in Table \ref{tab:bismfits} along with the value of $\alpha$ obtained from the dipole fit and the value of $\delta$ obtained from the quadrupole fit. The errors on the fit are derived from the $\chi^2$ distribution shown in Figure~\ref{fig:chi2fit} and don't include possible systematics uncertainties from the missing $m=0$ dipole component.

\begin{table*}[ht]
\centering
\begin{tabular}{l|l|l|l|l}
Source & R.A. [$^\circ$] & decl. [$^\circ$] & $\Delta \psi$ [$^\circ$] & $\delta_N$ [$10^{-4}$] \\ \hline
\cite{0004-637X-776-1-30} & $229.7\pm 1.9$ & $23.3 \pm 2.5$ & 9.0 & -5.03 \\
\cite{0004-637X-814-2-112} & $237.9\pm16$ & $22.2\pm16$ & 12.2 & -4.77 \\
\cite{2041-8205-818-1-L18} & $234.4 \pm 0.7$ & $16.3\pm 0.6$ & 6.5 & -3.42 \\
Boundary Fit & $229.2\pm 3.5$ & $11.4\pm 3.0$  & -- & -2.36 \\
Dipole/Quadrupole & $218.4 \pm 0.3$ ($\pm 2.6$) & $20.7 \pm 0.3$ ($\pm 2.6$) & -- & -4.41 \\
\end{tabular}
\caption{
\small Magnetic field alignment. The last two rows correspond to measurements of the large-scale anisotropy from this study. The R.A. measurement in the last row is obtained from the dipole vector and the decl. is obtained from the $\ell=2$ quadrupole component. The second to last column corresponds to the angular distance $\Delta \psi$ between the boundary fit and the various LIMF estimates.
The last column gives the corresponding vertical dipole component under the assumption that the dipole is oriented towards the given decl. Error in parentheses for dipole and quadruple correspond to systematic uncertainties.
} \label{tab:bismfits}
\end{table*}
The fact that the dipole component of the full-sky cosmic ray anisotropy map is approximately aligned with the direction of the LIMF (or at least its projection on the equatorial plane) is probably not a coincidence, since we expect diffusion to be anisotropic with the fastest propagation along the magnetic field lines~\citep{2012A&A...547A.120E, 2014ApJ...785..129K, Schwadron2014, Mertsch:2015jan}.
Assuming that the observed dipole points in this direction, it is possible to estimate the amplitude of the vertical component. The measured amplitude of the horizontal component of the dipole $\tilde{A}_1$ is related to the true amplitude $A_1$ through the dipole inclination $\delta_0$ with $\tilde{A}_1 = A_1 \cos \delta_0$, from which we obtain a value for the vertical dipole vector component of
$\delta_N = \tilde{A}_1 \tan{\delta_0} \sim -3.97 ^{+1.0}_{-2.0} \times 10^{-4}$ for the various magnetic field assumptions (see Table \ref{tab:bismfits}).

If we assume that the dipole component must be aligned with the LIMF, the observed
deviation could be explained as due to the relative motion of the observer with respect to a frame in which the cosmic ray distribution is isotropic, called the Compton-Getting Effect~\citep{Compton:1935,1968Ap&SS...2..431G}.
The heliosphere could also have a significant warping effect on 10 TeV cosmic ray arrival direction distribution, mostly due to the LIMF draping curvature around the heliosphere
\citep{Pogorelov:2009may}.
As a result, the dipole component of the cosmic ray anisotropy could be out of alignment from the LIMF.
Future studies, with full-sky maps at different particle rigidities, could provide a more powerful tool to probe the properties of the interstellar
and heliospheric magnetic fields.

\section{Conclusions}

We have used experimental data collected by the HAWC Gamma Ray Observatory and the IceCube Neutrino Observatory to compile, for the first time, a nearly full-sky map of the arrival direction distribution of cosmic rays with median energy of 10 TeV.
The combined analysis accounts for the difference in instantaneous and time-integrated field of view of the HAWC observatory and provides an integrated field of view that extends from $-90^\circ$ to  $+76^\circ$ in decl. The almost full-sky observation eliminates the degeneracy between the spherical harmonic components and provides a tool to probe the properties of particle diffusion in the interstellar medium and of interstellar magnetic turbulence.
The corresponding angular power spectrum suggests that two different mechanisms are responsible for the observed angular scale features. The ordering of cosmic ray anisotropy along the LIMF is supported by fitting the boundary between deficit and excess, which points to the direction $(\alpha_\mathrm{fit},\delta_\mathrm{fit}) = (229.2\pm 3^\circ.5,  11.4\pm 3^\circ.0)$ that is consistent with various observations. We obtained the phase and amplitude of the dipole component projected onto the equatorial plane to be $\tilde{A}_1=(1.17\pm.01) \times 10^{-3}$,
$\alpha_1=38.4\pm0^\circ.3$. Based on the assumption that the true dipole is aligned along the LIMF, we estimated the missing vertical component to be $\delta_N \sim -3.97 ^{+1.0}_{-2.0} \times 10^{-4}$.

\section*{Acknowledgements}
\input{ack}

\software{
HEALPix/healpy (version 1.9.1,~\cite{Gorski:2005apr}),
CORSIKA (version 7.40,~\cite{corsika}),
ROOT (version 6.04/12,~\cite{citeulike:363715}),
Matplotlib (version 1.5.0,~\cite{Hunter:2007}),
Astropy (version 1.1,~\cite{astropy:2013, astropy:2018}),
SciPy (version 0.16.1, http://www.scipy.org/),
NumPy (version 1.11.1,\cite{Oliphant:2015:GN:2886196}),
Python programming language (Python Software Foundation, https://www.python.org/),
PolSpice (version 3.0.3, http://www2.iap.fr/users/hivon/software/PolSpice).
}

redpajama_set_name: RedPajamaArXiv


MOSCOW (Sputnik) - The foreign ministers of Group of Seven (G7) member countries have expressed concern over the presence of Russian military personnel in Venezuela.
"We call for urgent humanitarian access to the country to be provided in accordance with international humanitarian principles to help address the basic needs of crisis-affected people. We are alarmed by the deployment of Russian military forces which threatens to exacerbate the already dangerous situation", the minister said in a joint communique.
The statement comes amid a two-day meeting of G7 foreign ministers started on 5 April in France's seaside resort of Dinard. This meeting comes as preparation for the 45th G7 summit that will be held in Biarritz in late August.
In March, a group of Russian military personnel arrived in the Venezuelan capital of Caracas to take part in talks on defence cooperation with officials. During the consultations, Russia repeatedly stressed that their presence was fully legitimate and in accordance with the defence agreement between Moscow and Caracas. Russian Foreign Minister Sergei Lavrov later said that these servicemen were simply carrying out maintenance of earlier supplied military equipment.


text:
Glowing tribute paid by Kilshaw as Bodman heads to Cornwall
HUNSLET have agreed to release Charley Bodman from his contract.
The Welshman is joining Rugby League's new boys Cornwall.
Head coach Alan Kilshaw said: "I'm sure I speak for everyone at the club in wishing Charley all the best for the rest of the season (apart from next week, when we play the Choughs!).
"He has been a popular member of the squad, with the playing group, the coaches and the physio team. Charley has developed really well this season but now needs to be playing regularly to further enhance that progress. Cornwall can offer him week-in, week-out football and I've no doubt that he will kick on."
`Killer' concluded: "The door at Hunslet isn't closed for Charley and we will be keeping an eye on his performances over the second half of the season. He knows he is welcome back any time to train with us or to watch the boys play; he's a great lad and Cornwall are getting a good bloke."

redpajama_set_name: RedPajamaCommonCrawl


Maybe it is the way it purrs or whooshes but any ultra-luxury car lover will practically swoon at the sound and sight of this glorious beast. The Aventador S targets a particular audience; most definitely the ones who can afford a fleet of luxury rides. If you are thinking that you would love the feel of one even, you could saunter over to Milani Exotic Rentals and rent one for the day.
The Lamborghini Aventador SV, The New model car is arguably the fastest and most powerful vehicle the Lamborghini series has ever produced. It is quite pricey estimated to go for $500,000 big ones.
There is the regular Aventador and then there is the Aventador SV. Both of them are powerful vehicles ( they are Lamborghinis after all) but the SV one-ups the regular in a few ways.
The Aventador SV has 50 more horsepower than the regular Aventador which has a 690-horsepower.
The SV has a 0-to-60 time of 2.7 seconds.
It has a massive rear wing.
It costs almost a cool $100,000 more than the regular Lambo.
It comes with exciting options such as a backup camera and rear air intakes, a travel package that you may actually have to make inquiries about (it goes for $1,100) and an $800 fire extinguisher.
The SV has features that declare loud and clear that it is a Lamborghini with interest. The amount one needs to spend in order to drive off in Lambo SV and own it may seem a lot, but to the ultra-luxury car lover, it is a small price to pay.
The Aventador drives like a futuristic car from a galaxy that is light years ahead of Earth. Its acceleration is the fastest you are likely to experience in a while. Then there is the handling. Taking on myriads of curves becomes quite an adventure as this vehicle handles them with such ease you are tempted to look for the wildest curves you can get. You need to be aware of the limits though because there is a very real chance that you will be tempted to go overboard due to the excitement.
Driving an Aventador is the ultimate experience. You may have to constantly remind yourself that you are actually in a Lamborghini. The features in the interior such as the unbelievably comfortable seats and the plush fixtures are a constant reminder anyway.
No other vehicle on the roads draws open-mouthed stares like the Lamborghini Aventador. If you want to see everything come to a standstill, cruise by slowly in a Lambo Aventador and watch spanners drop from hands and ice cream drip to the ground. In this digital age, you might attract a few recordings from those who remember that they have the gadgets.
This is the one vehicle that will get you as close as you will ever get to having the celebrity experience. The experience is not only thrilling, but it is also worth the money you spend to buy or rent it. Ultra-luxury car lovers would not squirm at the prospect of spending even 30 minutes in such a luxurious ride.
Why You Need A Security Upgrade For Your Home?


The insurance marketplace is already a confusing place, and when you introduce a product that the Federal Government and State Government can't agree on, it only gets worse.
The Good News: There are great insurance companies that provide great coverage for the cannabis industry. These plans can be a bit pricey, depending on your specific business operations, but there are solutions for any size company in any part of the industry.
The Bad News: Not everyone likes the price for proper coverage, leading to an acceptance of subpar coverage.
When insurance carriers know that a cannabis operator cannot afford the proper coverage, they are still going to provide a CHEAP coverage option to satisfy contractual needs………. with hidden exclusions essentially barring the client from receiving any actual coverage at the time of loss.
This isn't necessarily a bad thing if it is well documented to the client and the client is fully aware that they are essentially paying for only their certification to complete certain contracts or be able to operate in a certain space or store and not actual coverage.
The problem I have with this is that not all brokers provide full disclosure. Often, they are just trying to make a sale and they take advantage of the client through the complicated nature of insurance policies. Most policies I have reviewed have had a Products Exclusion that makes the coverage inapplicable if a loss were to happen. Despite this, the client is under the impression that they have insurance and are fully covered.
The main point to take away from this article is be careful during broker selection. You want to partner with someone who you are confident has your best interests at heart and who understands you built your business with your blood, sweat, and tears. Don't be fooled by "too good to be true" prices and, when purchasing insurance, remember how much you spent to build your business. Don't skimp on the protection needed to keep your business going.
Author Bio: John Burkhalter, AINS, AU, CRIS, RCIP, is the Vice President of the Cannabis Division at Assured Partners Insurance in Colorado. John has over 4 years of experience in assisting cannabis clients with their risk management, compliance, and insurance programs. You can find out more about him and Assured Partners here.


Capricor and Nile Therapeutics Complete Merger to Form Capricor Therapeutics, Inc.
LOS ANGELES & SAN MATEO, Calif.--(BUSINESS WIRE)--Capricor, Inc. and Nile Therapeutics, Inc. (NLTX) today announced the completion of the previously announced merger pursuant to which, among other things, Capricor has become a wholly-owned subsidiary of Nile in an all-stock transaction. Common stock in the combined company, Capricor Therapeutics, Inc., will begin trading today on the OTC Markets under the symbol "NLTXD." The stock will begin trading under the symbol "CAPR" starting December 20, 2013.
The stockholders of Capricor approved the merger. At a special meeting of the Nile stockholders held on November 12, 2013, the Nile stockholders approved certain amendments to the Nile charter in connection with the merger. The Nile charter amendments provide for (i) a 1-for-50 reverse split of the outstanding common stock of Nile, (ii) a name change from "Nile Therapeutics, Inc." to "Capricor Therapeutics, Inc.," and (iii) a reduction in the authorized number of shares of the Nile common stock. Each of the foregoing charter amendments became effective upon the filing of the amended charter on November 20, 2013.
After giving effect to the merger and the reverse stock split, the Capricor stockholders received approximately 2.1 shares of the common stock of Capricor Therapeutics for each share of Capricor common stock held prior to the effective time of the merger. As a result of the merger, former Capricor stockholders own approximately 90% of the outstanding shares of Capricor Therapeutics, and Nile stockholders own approximately 10%, calculated in each case on a fully diluted basis assuming the issuance of shares underlying options and warrants.
Headquartered in Los Angeles, California, Capricor Therapeutics will operate under the leadership of the former Capricor management team with Linda Marbán, Ph.D., serving as Chief Executive Officer and Frank Litvack, M.D., serving as executive Chairman of the Board. The newly comprised Board of Capricor Therapeutics includes seven representatives from the former Capricor board and two representatives from the former Nile board.
Subject to regulatory approvals, Capricor plans to initiate Phase II of its ALLSTAR clinical trial with its lead candidate CAP-1002 in early 2014. Phase I of ALLSTAR was funded in part by the National Institutes of Health and Phase II is being funded in part through the support of the California Institute For Regenerative Medicine.
Capricor Therapeutics also announced that it is scheduled to present at the Piper Jaffray 25th Annual Healthcare Conference on Wednesday, December 4th at 1:30 PM EST at The New York Palace Hotel in New York City. A webcast of the presentation will be available on the Investor Relations section of the Company's website at www.capricor.com.
Capricor Therapeutics, Inc. (CAPR), a publicly traded biotechnology company, is focused on the development of novel therapeutics to prevent and treat heart disease. The Company was formed through the November 2013 merger between Capricor, Inc., a privately held company whose mission is to improve the treatment of heart disease by commercializing cardiac stem cell therapies for patients, and Nile Therapeutics, Inc., a clinical-stage biopharmaceutical company developing innovative products for the treatment of cardiovascular diseases. For additional information visit www.capricor.com.
CAP-1002, Capricor's lead product candidate, is a proprietary allogeneic adult stem cell therapy for the treatment of heart damage. The product is derived from donor heart tissue. The cells are expanded in the laboratory using a specialized process and then introduced directly into a patient's heart via infusion into a coronary artery using standard cardiac catheterization techniques.
Cenderitide, a novel chimeric natriuretic peptide, is a first-in-class dual guanylyl cyclase receptor activator. Chronic dual receptor activation using a continuous subcutaneous infusion of Cenderitide is being studied to test whether its combination of tissue protective, renal protective and cardiac unloading effects will help stabilize the patient's heart and kidney function, preventing the worsening of heart failure symptoms and re-admissions to the hospital. Cenderitide is under clinical development to treat heart failure patients during the post-acute heart failure (P-AHF) period, which is the 90-day period immediately after discharge from a hospitalization for acute decompensated heart failure. The P-AHF period is often associated with a worsening of heart failure symptoms or renal function and rates of re-admission and mortality can be as high as 40%.
Cenderitide is currently not an approved product and is strictly for investigational purposes.
Statements in this press release regarding the transaction between Nile and Capricor; the combined company's cash; the potential value created by the merger for Nile's and Capricor's stockholders; the potential of the combined companies' technology platform, pipeline products in development, business development and commercialization opportunities and financial foundation; the combined company's management and board of directors; the efficacy, safety, and intended utilization of Capricor's and Nile's product candidates; the conduct, size, timing and results of discovery efforts and clinical trials; plans regarding regulatory filings, future research and clinical trials; plans regarding current and future collaborative activities and the ownership of commercial rights; future royalty streams, and any other statements about Nile's or Capricor's management teams' future expectations, beliefs, goals, plans or prospects constitute forward-looking statements within the meaning of the Private Securities Litigation Reform Act of 1995. Any statements that are not statements of historical fact (including statements containing the words "believes," "plans," "could," "anticipates," "expects," "estimates," "plans," "should," "target," "will," "would" and similar expressions) should also be considered to be forward-looking statements. There are a number of important factors that could cause actual results or events to differ materially from those indicated by such forward-looking statements. More information about these and other risks that may impact our business are set forth in our Form 10-K for the year ended December 31, 2012, as filed with the Securities and Exchange Commission on June 21, 2013, in our Quarterly Report on Form 10-Q for the quarter ended June 30, 2013, as filed with the Securities and Exchange Commission on August 14, 2013, and in our Definitive Proxy Statement on Schedule 14A, as filed with the Securities and Exchange Commission on October 10, 2013. All forward-looking statements in this press release are based on information available to us as of the date hereof, and we assume no obligation to update these forward-looking statements.


text:
Watch Star Trek Into Darkness (2013) : Full Movie Online Free When the crew of the Enterprise is called back home, they find an unstoppable force of terror from within their own organization has detonated the fleet and everything it stands for, leaving our world in a state of crisis. With a personal score to settle, Captain Kirk leads a manhunt to a war-zone world to capture a one man weapon of mass destruction. As our heroes are propelled into an epic chess game of life and death, love will be challenged, friendships will be torn apart, and sacrifices must be made for the only family Kirk has left: his crew.
Release Date : May 05, 2013
Genres : Action, Adventure, Science Fiction
Production Company : Bad Robot, Paramount, Kurtzman/Orci, Skydance Media
Production Countries : United States of America
Casts : Chris Pine, Zachary Quinto, Zoe Saldana, Karl Urban, Simon Pegg, John Cho, Benedict Cumberbatch, Anton Yelchin, Bruce Greenwood, Peter Weller, Alice Eve
Plot Keywords : spacecraft, friendship, sequel, futuristic, space, alien, imax, space opera, terrorist bombing, 3d
Related Movies for "Star Trek Into Darkness (2013)"
Watch Trailer Star Trek Into Darkness


text:
Q: Email validator not working properly in django? I am not using django forms here and I am validating field with ajax/jquery but this code is not working properly.
If I enter the correct email it displays the error message but if i enter the invalid email then it doesn't display the error.
Also this validate_email(request.GET.get('email', '')) always returns None.
views
class ValidateEmailField(View):

    def get(self, request):
        email = validate_email(request.GET.get('email', ''))
        print(email)
        data = {}

        if not email:
            data = {
                'error_message': 'Invalid Email'
            }
        return JsonResponse(data)

template
dataType: 'json',
        success: function (data) {
          if (data.error_message) {
            $(".error").text(data.error_message).show();
            $('#id_btn').prop("disabled", true);

          }
          else {
       $(".error").text(data.error_message).hide();
       $('#id_btn').prop("disabled", false);
      }

A: Return a proper status_code to trigger the error callback in frontend
class ValidateEmailField(View):

   def get(self, request):
       email = request.GET.get('email', '')
       try:
            validate_email(email)
       except ValidationError:
            ...
            message: 'Invalid Email'
            status_code = 400
            return JsonResponse({'message':message }, status=status_code)
       # default status_code is 200
       return JsonResponse({'message': 'success'})

status_code=4xx, in your template, the error callback will be triggered, you can register your callback here
$.ajax({
    success: ...
      error: function (jqXhr, textStatus, errorMessage) {
         // error callback, run your code here
         console.log(jqXhr.responseText);
})

UPDATE
source of validate_email, validate_email() will trigger __call__ method, which will return either None or ValidationError, that's why your code email=validate_email(...) email always is None even your email is validated
class EmailValidator:
    message = _('Enter a valid email address.')
    code = 'invalid
    ...

    def __call__(self, value):
        if not value or '@' not in value:
            raise ValidationError(self.message, code=self.code)

        user_part, domain_part = value.rsplit('@', 1)

        if not self.user_regex.match(user_part):
            raise ValidationError(self.message, code=self.code)

        if (domain_part not in self.domain_allowlist and
                not self.validate_domain_part(domain_part)):
            # Try for possible IDN domain-part
            try:
                domain_part = punycode(domain_part)
            except UnicodeError:
                pass
            else:
                if self.validate_domain_part(domain_part):
                    return
            raise ValidationError(self.message, code=self.code)

redpajama_set_name: RedPajamaStackExchange


text:
Visualizzazione post con etichetta Copper Canyon. Mostra tutti i post
SPACE, IN CHAINS by Laura Kasischke (Copper Canyon)
"Kasischke's intelligence is most apparent in her syntactic control and pace, the way she gauges just when to make free verse speed up, or stop short, or slow down." (The New York Times Book Review)
"Kasischke's poems are powered by a skillful use of imagery and the subtle, ingenious way she turns a phrase." (Austin American-Statesman)
Laura Kasischke's poems have the same haunting qualities and truth as our most potent memories and dreams. Through ghostly voices, fragmented narratives, overheard conversations, songs, and prayers in language reminiscent of medieval lyrics converted into contemporary idiom, the poems in Space, In Chains create a visceral strangeness true to its own music.
So we found ourselves in an ancient place, the very
air around us bound by chains. There was
stagnant water in which lightning
was reflected, like desperation
in a dying eye. Like science. Like
a dull rock plummeting through space, tossing
off flowers and veils, like a bride. And
also the subway.
Speed under ground.
And the way each body in the room appeared to be
a jar of wasps and flies that day—but, enchanted,
like frightened children's laughter.
Laura Kasischke is the author of thirteen books of poetry and fiction. Her novel Her Life Before Her Eyes was adapted for the screen and starred"
a dicembre 24, 2011 Nessun commento:
Etichette: Copper Canyon, IN CHAINS, Laura Kasischke, SPACE
Matthew Zapruder's COME ON ALL YOU GHOSTS (Copper Canyon)
"Charming, melancholy, hip."—Publishers Weekly, starred review
"Zapruder's innovative style is provocative in its unusual juxtapositions of line, image and enjambments. . . . Highly recommended."—Library Journal
"Matthew Zapruder's third book mixes humor and invention with love and loss, as when the breath of a lover is compared to "a field of titanium gravestones / growing warmer in the sun." The title poem is an elegy for the heroes and mentors in the poet's life—from David Foster Wallace to the poet's father. Zapruder's poems are direct and surprising, and throughout the book he wrestles with the desire to do well, to make art, and to face the vast events of the day.
Look out scientists! Today the unemployment rate
is 9.4 percent. I have no idea what that means. I tried
to think about it harder for a while. Then
tried standing in an actual stance of mystery
and not knowing towards the world.
Which is my job. As is staring at the back yard
and for one second believing I am actually
rising away from myself. Which is maybe
what I have in common right now with you . . ."
Matthew Zapruder holds degrees from Amherst College, UC Berkeley, and the University of Massachusetts. He is the author of two previous books, including The Pajamaist, which"
a novembre 30, 2011 Nessun commento:
Etichette: COME ON ALL YOU GHOSTS, Copper Canyon, Matthew Zapruder's


As the West's workforce demographic changes, managing and retaining senior level talent is becoming an ever more important priority for CEOs. But they don't trust HR and personnel to get it right.
The Towers Perrin survey of senior HR executives in North America found more and more companies were now recognising the importance of retaining talent in a demographically challenged environment.
Increasingly, too, they were focusing on a core group of leaders, technical experts and key contributors who could drive their business forward rather than thinking of "talent" in terms of the whole workforce.
But there was a gap between what HR felt – that talent retention and development was one of their most critical objectives – and what the business felt HR could achieve.
Few CEOs, it emerged, believed their HR departments had the skills needed to manage this emerging talent pool effectively.
Groups now considered to be "talent" included senior leadership, employees at mid-level with leadership potential, key contributors or technical experts and entry-level employees with leadership potential.
Together, these defined talent pools made up, on average, no more than 15 per cent of the total workforce, said Towers Perrin.
"As businesses transform to drive top-line growth, we're seeing talent emerge as a top strategic priority for CEOs and boards, as well as HR executives," said Max Caldwell, a Towers Perrin principal and one of the leaders of the firm's HR services business workforce effectiveness practice.
"Creating a robust 'talent supply chain' that delivers the required number of leaders and key contributors who possess the right mind-set and skills has never been more important," he added.
"However, the HR function in many organisations is not yet delivering sufficient value in this critical area," he warned.
Organisations were distinguishing between talent management as a set of practices and programmes for a relatively small, if critical, segment, and workforce management as a set of practices and programmes covering the entire workforce.
But no more than half of 250 companies polled believed that HR had the skills across a wide range of managerial support activities needed effectively to deliver on the talent management role.
More than two-thirds said their HR department did not have the skills necessary to measure employee engagement on an ongoing basis or to evaluate the return on workforce-related investments.
The inability to capture and disseminate relevant data to managers was also problematic, since companies had no quantitative foundation from which to develop a talent management strategy and build and deploy meaningful processes.
"Many of the larger and more forward-thinking organisations are creating a special senior talent management position to focus specifically on the organisation's talent strategy," noted Caldwell.
"The titles may differ, but these roles seek to integrate things like strategic workforce planning, recruitment, leadership development and career management, which had previously operated in silos," he added.


Join us in celebrating our FIRST Lego League Jr. Clubs.
Students from Tahoe, Earl Warren, and Mark Twain Elementary will be on site to demonstrate their Lego League talents.
Lunch will be provided by the Optimist International Club of Sacramento. Please register on Event Brite and request a free ticket for each person attending.
Activities on hand for youth.


text:
package bt.bencoding.model;

import bt.bencoding.BEType;
import bt.bencoding.model.rule.Rule;

import java.util.List;
import java.util.Map;

class BEMapModel extends BaseBEObjectModel {

    private Map<String, BEObjectModel> entriesModel;

    BEMapModel(Map<String, BEObjectModel> entriesModel, List<Rule> rules) {
        super(rules);
        this.entriesModel = entriesModel;
    }

    @Override
    public BEType getType() {
        return BEType.MAP;
    }

    @Override
    protected ValidationResult afterValidate(ValidationResult validationResult, Object object) {

        if (object != null) {

            Map<?,?> map = (Map<?,?>) object;
            for (Map.Entry<String, BEObjectModel> entryModel : entriesModel.entrySet()) {

                String key = entryModel.getKey();
                entryModel.getValue().validate(map.get(key)).getMessages()
                        .forEach(validationResult::addMessage);
            }
        }

        return validationResult;
    }
}

redpajama_set_name: RedPajamaGithub


text:
package com.bluecatcode.server;

import org.eclipse.jetty.http.HttpStatus;

import javax.servlet.ServletException;
import javax.servlet.http.HttpServlet;
import javax.servlet.http.HttpServletRequest;
import javax.servlet.http.HttpServletResponse;
import java.io.IOException;

public class JettyServlet extends HttpServlet {

    @Override
    protected void doGet(HttpServletRequest req, HttpServletResponse resp) throws ServletException, IOException {
        resp.setStatus(HttpStatus.OK_200);

        throw new NullPointerException();
//        resp.getWriter().print("HelloWorld!");
    }
}


text:
mike koozmin/the s.f. examinerHolly Courts
Sex offender living in SF public housing dodges federal rules
Nathaniel Riley has lived in Holly Courts — arguably one of the choicest properties in the Housing Authority portfolio — in the shadow of Bernal Heights since last fall.
In that short time, the 62-year-old has run afoul of some of his neighbors, who point out that he has a criminal history that should prohibit him from living in public housing.
Riley has a 1992 felony conviction on his record for pleading no contest to sexually assaulting a 14-year-old girl at his home in Hayward, criminal records show.
Today, under state law, that crime requires lifetime registration as a sex offender and a place on the Megan's Law database, a state record of the names and addresses of people with sex-crimes convictions.
It would also mean he could not live in public housing.
Under federal Department of Housing and Urban Development rules, no one on a state database of sex offenders can receive federal housing subsidies after June 2001.
Riley moved into public housing in San Francisco sometime after a 2004 eviction from nonprofit housing in Bernal Heights, according to court records.
But Riley is not a registered sex offender.
His name is not on the Megan's Law database or any other such list maintained by law enforcement.
That's because at the time of Riley's conviction, he was not required to register as a sex offender, probation records show.
But California's sex offender laws have been updated several times since his conviction. And state law says that offenders whose past convictions now require registry under current law are supposed to register and be on the list.
Under Penal Code 290, it appears Riley should be registered, according to Teresa Drenick, a spokeswoman for the Alameda County District Attorney's Office, the jurisdiction where Riley's 1992 conviction occurred.
But without a citizen complaint or some other notification to law enforcement, there is little to compel a should-be registrant to willingly add his or her name to the list.
Past offenders who are required to register are supposed to be notified from the agency that maintains the local list.
In The City's case, that's the Police Department. However, "Once the registrant is informed of his duty to register … the onus is completely on him" to do so, Drenick said.
Reached via cellphone late last month, Riley declined to comment to The San Francisco Examiner, stating he needed to consult with an attorney.
He has not responded to subsequent calls for comment.
After inquiries from The Examiner, the Police Department's Sex Offender Unit said Friday that it is currently investigating Riley.
Within months of moving last fall to a two-bedroom unit at Holly Courts that he shared with an adult son, Riley also had two harassment claims filed against him by neighbors, one for making death threats toward a 61-year-old woman and her family, and the other for harassing a 30-year-old mother and her four children, according to records.
Riley was briefly jailed, but both harassment claims were dropped and he was set free after the claimants failed to make a January court date.
Today, his neighbors say that he is disruptive and acts erratically around children.
"He doesn't need to be around kids," said Cavia McDaniels, the mother of four who filed one of the harassment claims against Riley last year. "I don't have my kids around here on Halloween because of him … we need to change something about this for our kids."
"We don't want him to be homeless," said Karen Huggins, the woman who claimed that Riley threatened to kill her and her family.
There are public-housing units reserved for seniors and disabled residents that would be better fits for Riley, she said.
Other criminal records were not immediately available. Riley does have an "extensive [National Crime Information Center] rap," Hayward police wrote in his 1992 arrest report.
All Housing Authority residents are required to undergo a background check as well as income certification before they are admitted to public housing. On Housing Authority forms, tenants are asked if they have ever been convicted of a crime.
However, there is no requirement — only a recommendation — that public-housing agencies ask if a resident is subject to sex offender registration, HUD spokeswoman Gene Gibson said.
The situation in Holly Courts has been brought to the attention of the Housing Authority and Executive Director Barbara Smith, but it's unclear what the agency can do.
The Housing Authority declined to comment on Riley or the situation at Holly Courts, but said that there is a Housing Authority tenant who "may be" subject to eviction under HUD rules.
The agency began quarterly reviews of all of its properties to clear out sex offenders there in violation of federal law, and the Housing Authority has also prohibited sex offenders from staying overnight as guests in public housing.
"The Housing Authority takes its policies with respect to ensuring sex offenders are not living on its properties very seriously," the agency said in a statement Friday.
Bay Area NewsNathaniel Rileypublic housingsex offender
Two men killed in separate homicides Saturday in SF
Man looking to buy drugs in the Mission robbed of cash, ATM card


text:
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Clinical & Leadership
Backpack Giveback
Sporting Clays Shoot
Ice Cream Fundae
Raise Their Spirits
Cocktails for Camp
Storytelling Event
Designer Purse Bingo
Topgolf Event
Jameisha
When I started in the Day School program at Pressley Ridge they put up with everything that I did but they didn't have to. But they had the patience to deal with me.
The Ebron Family
Linda Ebron has dedicated much of her life to serving youth in challenging situations. A career in social work eventually led her to foster care.
Jessica, a former foster youth with Pressley Ridge, now spends her days as a Treatment Coordinator helping youth through the same situations she experienced,
Mark and Patti McCloud were concerned when their 18 month-old son, Jordan, still hadn't said his first words. After a series of evaluations, Jordan was diagnosed with autism at age two and a half...
At the age of 13, Brandon Brown was living in a homeless shelter with his mother and siblings. He was a compulsive liar who was often caught hoarding food and stealing...
The Moyer Family
When visiting the home of Tabitha and Wayne Moyer, one cannot help but feel the love and joy that abounds
in their special family...
In her 18 years, Katherine has seen more than her fair share of struggles. At a young age, she lost her youngest brother to a rare disease — a loss that strongly impacted her family and ultimately resulted in her parents' divorce.
Robert's life had been taken over by drugs, and it took almost losing his son to make him realize it.
Wendy moved to Pittsburgh from Puerto Rico in search of supports for her then five-year-old son Victor, a non-verbal youth with autism and intellectual disabilities...
In April 2015, Jacob entered the program at Pressley Ridge Grant Gardens. Before his arrival, he had been in several placements totaling three and a half years...
Life for Levi certainly hasn't been easy. Born with brain damage to abusive and neglectful parents, he spent most of his early years being shuffled around to nearly a dozen different foster homes, residential treatment facilities and even a mental institution...
Pressley Ridge


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Posted inFunding & grants
Melbourne to match green infrastructure investments dollar-for-dollar
by Cameron Jewell 1 June 2017
The City of Melbourne has announced a $1.2 million Urban Forest Fund, which it will use to match private investments in urban greening initiatives dollar-for-dollar.
It is currently seeking interested property developers, community groups and other government organisations interested in what would effectively be half-priced urban greening initiatives, including tree planting, creating parks, stormwater projects, and green walls, roofs and facades.
City of Melbourne's Environment Portfolio chair Cathy Oke said the aim was to support greening projects that would otherwise go unfunded.
"The City of Melbourne owns and controls only one-fifth of the city's land area, so we're looking for proposals to create new green space on private property," Ms Oke said.
"This project could lead to the creation of new spaces that can capture stormwater to reduce flooding, reduce summertime temperatures in the city and create habitat for plants and animals."
Melbourne Lord Mayor Robert Doyle said the fund would leave a "green legacy" for the city.
"Green infrastructure is fundamental to help cities respond to the challenges of climate change, urban heat, flooding and population growth," Mr Doyle said.
"As well as protecting us from extreme heat, our trees and parks are a major contributor to Melbourne's liveability. The City of Melbourne is increasing public green space and planting 3000 trees a year. This initiative, to stimulate greening of private property, which represents 73 per cent of land in our municipality, is the next frontier."
While initial seed funding is $1.2 million, the council is attempting to grow the fund to $10 million through donations from philanthropic organisations and individuals.
Craig Taberner, chief executive of Nursery & Garden Industry Victoria, said the fund would help create a more climate resilient city.
"Access to collaborative funding should energise and empower individuals and communities to take action, and share the responsibility of creating and maintaining the city's green spaces," he said.
The city also has an online tool that maps the potential for green space, cool roofs and solar PV across the local government area.
See Mapping project reveals potential of a Melbourne rooftop transformation
Why green infrastructure should be on any urban assets register
In "Environment"
10 ways to grow an urban forest: coming soon to Oz and NZ
Thinking city scale about urban greening
In "Sponsored"
Tagged: green infrastructure, melbourne, Urban Forest Fund


Viking Chili Bowl has been added to your travel planner!
In business since 1953, Viking Chili Bowl has been serving the Valparaiso, IN community since 1980. They have daily breakfast and lunch specials available 7 days a week. They also have a private dining room area that can accommodate small parties or meeting of 50 people. They serve homemade specialties every day.


Our mission The International Dyslexia Association (IDA) is an international organization that concerns itself with the complex issues of dyslexia. The IDA membership consists of a variety of professionals in partnership with dyslexics and their families and all others interested in The Association's mission.
We believe that all individuals have the right to achieve their potential that individual learning abilities can be strengthened and that social, educational, and cultural barriers to language acquisition and use must be removed.
The International Dyslexia Association actively promotes effective teaching approaches and related clinical education intervention strategies for dyslexics. We support and encourage interdisciplinary study and research. We facilitate exploration of the causes and early identification of dyslexia and are committed to the responsible and wide dissemination of research-based knowledge.
The purpose of IDA is to pursue and provide the most comprehensive range of information and services that address the full scope of dyslexia and related difficulties in learning to read and write . . . in a way that creates hope, possibility, and partnership. So that every individual has the opportunity to lead a productive and fulfilling life, and society benefits from the resource that is liberated.
The International Dyslexia Association (IDA) is a 501(c)(3) non-profit, scientific, and educational organization dedicated to the study and treatment of the learning disability.