text:
\section{Introduction}
\label{sec:intro}
The {\it flux} of cosmic-ray (CR) electrons and positrons ($e^-$ and $e^+$) has been measured with unprecedented precision over more than four orders of magnitude of energy.
One of the most accurate measurements on single CR $e^-$ and $e^+$ and inclusive ($e^+ + e^-$) fluxes is provided by
AMS-02 on board the International Space Station (ISS), between 0.1 GeV to 1 TeV energy, and with errors reaching the few percent level
\citep{2014PhRvL.113l1101A,2014PhRvL.113l1102A,Aguilar:2014fea}.
The {\it Fermi} Large Area Telescope (LAT) has collected  almost seven years of $e^+ + e^-$ events in the 7~GeV-2~TeV energy range \citep{2017PhRvD..95h2007A}.
CALET on the ISS, and HESS on the ground, are providing $e^+ + e^-$ data up to  3 TeV and 30 TeV energy, respectively \citep{PhysRevLett.119.181101, HESSICRC17, PhysRevLett.120.261102}.
The DAMPE Collaboration has recently reported the direct detection of a break at around 1 TeV in the flux of the $e^+ + e^-$ measured between 25 GeV to 4.6 TeV \citep{Ambrosi:2017wek}.
Many theoretical interpretations have been proposed for the AMS-02 lepton data, invoking sources of  $e^{+}$ and/or $e^-$ in the Interstellar Medium (ISM),
from Pulsar Wind Nebulae (PWNe) and  Supernova Remnants (SNRs)\cite{Kobayashi:2003kp,Pohl:2012xs, 2009APh....32..140G, Gaggero:2013nfa,Delahaye:2014osa,DiMauro:2014iia,Manconi:2016byt}, and also
 in the context of annihilation and decay of dark matter particles \cite{Bergstrom:2013jra,DiMauro:2015jxa}.
In addition to the flux, the LAT team has also published the spectrum of  upper limits on the  $e^+ + e^-$ {\it dipole anisotropy} \cite{Abdollahi:2017kyf}.
Since the typical propagation length of TeV $e^\pm$  is smaller than $\sim 0.3$~kpc, $e^+$ and $e^-$ detected at TeV energies are most probably emitted from local sources, leaving a possible signature in the dipole anisotropy \cite{Manconi:2016byt}.
At variance, nuclei suffer mainly from diffusion rather than energy losses, so the hadronic flux from local sources is typically spread, and sets below the cumulative contribution of all Galactic sources.

The  contribution from the local source candidates is usually associated with high uncertainties, primarily connected to the properties of the accelerated and emitted $e^-$ and $e^+$.
Moreover, the completeness of current catalogs, such as SNRs, is assessed by means of the observed surface brightness (see e.g. \cite{2015MNRAS.454.1517G}), thus leaving open the possibility that nearby and
very old sources may contribute to the flux at Earth even if they are no longer visible at any energy of the electromagnetic band.
A strategy to constrain the source contributions of local known sources is to model their multi-wavelength emission and to connect it to the emitted CRs.
For example, the lepton emission from sources embedded in a magnetic field, such as $e^-$ from SNRs, can be connected with their synchrotron emission at {\it radio} frequencies
(see \cite{2010A&A...524A..51D,DiMauro:2014iia,Manconi:2016byt} and references therein).
In addition, the most recent experimental upper bounds on the dipole anisotropy could set further limits on the properties of local and dominant sources.

In the present paper we use this strategy to quantify the contribution of local known sources, in particular from two SNRs which are widely considered as the main candidates to contribute significantly to the high energy part of the $ e^-$ flux at Earth
(often measured cumulatively through $e^-+e^+$), namely Vela and Cygnus Loop, see e.g. \cite{Kobayashi:2003kp}.
For the first time, we present a multi-component model that explains the $e^+$ and $e^-+e^+$ fluxes from five experiments and in a wide energy range, and that is simultaneously compatible with the upper bounds on the dipole anisotropy and the radio emission from the most intense and closest SNRs.
The paper is structured as follows.
\reply{Our model for the cosmic-ray electrons from SNRs is outlined in Sec.~\ref{sec:model}.} In Sec.~\ref{sec:radio} the constrains imposed by radio data on our sample of local SNRs are presented. The constraints imposed from $e^-+e^+$ and dipole data are discussed respectively in Sec.~\ref{sec:flux} and Sec.~\ref{sec:dipole}. A model combining the multi-wavelength data for local SNRs that explains the most recent flux and dipole data is presented in Sec.~\ref{sec:multiw}, before concluding in Sec.~\ref{sec:conc}.

\section{\label{sec:model}Cosmic-ray electrons from SNRs}
\reply{Cosmic-ray $e^\pm$} can be injected \reply{in the interstellar medium (ISM)} by shocked stellar
environments - SNRs as well as PWNe -  according to the first order Fermi acceleration mechanism
(for a comprehensive review on the SNR paradigm for Galactic CRs see \cite{Blasi:2013rva} and references therein).
\reply{We  focus here on SNRs.}
For a detailed treatment of the injection of $e^-$ by SNRs and their propagation in the Galaxy we refer to \cite{2010A&A...524A..51D, Manconi:2016byt}.
\reply{We here remind the basics of our model, along with an additional new treatment for the injection of $e^-$ by SNRs and for the synchrotron radio emission from known SNRs. }

\subsection{Injection of cosmic-ray electrons from SNRs into the ISM}
The details of the release mechanism of $e^-$ from SNRs are poorly known and still under debate \cite{2010APh....33..160C, 2012MNRAS.427...91O, Blasi:2013rva, 2009MNRAS.396.1629G}, and could affect the properties of the escaping $e^-$, above all the energy spectrum.
\reply{We implement here two different models, the burst-like injection and the evolutionary model. }

\reply{The injection of $e^-$ accelerated by SNRs is commonly described  through a \textit{burst-like} approximation \cite{2010A&A...524A..51D},
in which all the $e^-$ are released in the ISM at a time equal to the age of the source. Under this hypothesis,} the energy spectrum $Q(E)$ of accelerated $e^-$ can be described by the function
 \begin{equation}
 Q(E)= Q_{0} \left( \frac{E}{E_0}\right)^{- \gamma} \exp \left(-\frac{E}{E_c} \right),
 \label{eq:Q_E}
\end{equation}
 where $Q_{0}$ is in units of GeV$^{-1}$, $E_c$ is a cutoff energy and $E_0= 1$~GeV.
Given the injection spectrum in Eq.~\ref{eq:Q_E}, the total energy emitted in $e^-$ from SNR (or $e^\pm$ for PWN) in units of GeV (or erg) can be obtained as (see \cite{2010A&A...524A..51D})
\begin{equation}
 E_{\rm tot} = \int _{E_1} ^\infty dE \, E \,Q(E) \,,
 \label{eq:Etot}
\end{equation}
where we fix $E_1 = 0.1$ GeV. The normalization of the spectrum in Eq.~\ref{eq:Q_E} can be constrained
from available catalog quantities for single sources \reply{(see Sec.~\ref{sec:synchro})}, or by using average population properties for the smooth galactic component   \cite{2010A&A...524A..51D,DiMauro:2014iia,Manconi:2016byt}.
\reply{The burst-like assumption is considered appropriate at high energy, since $e^-$ of energy $E\gsim100$ GeV are believed to be released  within a few kyr from the initial burst, and this timescale is much smaller than the age of the sources typically considered  to explain the CR $e^-$ data at Earth \cite{2009MNRAS.396.1629G}.}

\reply{In addition to the burst-like approximation, we also implement the {\em evolutionary model}  for the escape  of $e^-$ from SNRs as derived in Ref.~\cite{2012MNRAS.427...91O}.
The authors of Ref.~\cite{2012MNRAS.427...91O} assume analytical models for the temporal evolution of the shock radius and its velocity.
They also derive the timescales and the space-energy distributions for trapped and runaway $e^-$.
During the Sedov phase, the escape-limited maximum energy $E_{\rm m, esc}(T)$ below which CRs  are still trapped in the SNR is defined as \cite{2012MNRAS.427...91O}:
\begin{equation}\label{eq:Emesc}
 E_{\rm m, esc}(t)= E_{\rm knee} \left(\frac{T}{t_{\rm Sedov}}\right)^{-\alpha}
\end{equation}
where $E_{\rm knee}=10^{15.5}$~eV is the energy at the knee of the CR all-particle spectrum, $t_{\rm Sedov}$  is the start time of the Sedov phase, $\alpha$ describes the evolution of the maximum energy during the Sedov phase, and $T$ is the SNR age.
For energies smaller than $E_{\rm m, esc}(T)$, the $e^-$ are still trapped in the SNR, and their energy spectrum is described as:
\begin{align}\label{eq:QTrap}
  Q_{\rm trap}(E, T)&= A \left( \frac{E_{\rm m, esc}(T)}{E_0}\right)^{- (\gamma + \beta/\alpha)} \left(\frac{E}{E_{\rm m, esc}(T)}\right)^{-\gamma} \exp \left(-\frac{E}{E_c} \right) = \\
  &=  Q_{\rm 0, trap}(T) \left(\frac{E}{E_{0}}\right)^{-\gamma} \exp \left(-\frac{E}{E_c} \right) \label{eq:QTrap2}
\end{align}
where $A$ is a normalization factor, and $\beta$ describes the evolution of the  electron number inside the SNR.
The $Q_{\rm 0, trap}(T)$ is obtained by recasting Eq.~\ref{eq:QTrap} using the explicit form of $E_{\rm m, esc}(T)$ in Eq.~\ref{eq:Emesc}.
The energy spectrum $Q_{\rm esc}(E)$ of runaway $e^-$ is instead described by:
\begin{equation}\label{eq:Qesc}
  Q_{\rm esc}(E)= A \left( \frac{E}{E_0}\right)^{- (\gamma + \beta/\alpha)} \exp \left(-\frac{E}{E_c} \right)\quad.
\end{equation}
The  $e^-$ at a given  energy $E$ escape from the SNR at a time:
\begin{equation}\label{eq:Tesc}
 T_{\rm esc}=t_{\rm Sedov} \left( \frac{E}{E_{\rm knee}}\right)^{-\frac{1}{\alpha}}\quad.
\end{equation}}
\reply{The idea of an escape-limited maximum energy $E_{\rm m, esc}(T)$, or equivalently of $T_{\rm esc}$ after which $e^-$ of a given energy can run away from the SNR,
 determines the difference between the simpler burst-like approximation and this evolutionary escape model.
Focusing on specific sources, as for example the Vela YZ and Cygnus Loop SNRs ($T=$11.3~kyr and 20~kyr respectively, see below),
this escape model states that CRs $e^-$ with energies  $E<E_{\rm m, esc}=88$~GeV  and  $E<E_{\rm m, esc}=17$~GeV  are still trapped in Vela YZ and Cygnus Loop, respectively.
On the opposite,  $e^-$ with energies $E>E_{\rm m, esc}$ have been released in the ISM.
Also, we note that the energy spectral index of runaway $e^-$ is modified with respect to the one of trapped ones, as stated by Eqs. \ref{eq:QTrap} and \ref{eq:Qesc}.
 We will study the consequences of these spectral modifications in the following Sections.
The specific values of $E_{\rm m, esc}(T)$, or equivalently the ages of the two sources, make the burst like approximations a more suitable description for the older Cygnus Loop than for Vela YZ.
 We fix $t_{\rm Sedov}=200$~yr, $\alpha=2.6$ and $\beta=0.6$, as in Ref.~\cite{2012MNRAS.427...91O}.
When not differently stated, our results are shown for the burst-like model.
}

\subsection{Propagation in the Galaxy}
The propagation of  $e^{-}$ and $e^{+}$ from their sources to the Earth has been treated as in \cite{2010A&A...524A..51D,DiMauro:2014iia,Manconi:2016byt},
\reply{from which we remind here some basic ingredients. We refer the reader to Ref.~\cite{Manconi:2016byt} for futher details.
The cosmic-ray $e^{-}$ and $e^{+}$ number density $\psi = \psi(E, \mathbf{x}, t)\equiv dn/dE$ per unit volume and energy
obeys the  transport equation:
\begin{equation}
 \frac{\partial \psi}{\partial t}  - \mathbf{\nabla} \cdot \left\lbrace K(E)  \mathbf{\nabla} \psi \right\rbrace +
 \frac{\partial }{\partial E} \left\lbrace \frac{dE}{dt} \psi \right\rbrace = q(E, \mathbf{x}, t)
 \label{eq:diff}
\end{equation}
where $K(E)$ is the energy dependent diffusion coefficient, $dE/dt\equiv b(E)$ accounts for the energy losses and $q(E, \mathbf{x}, t)$ is the  $e^-$ and $e^+$ source term. The flux of electron $\Phi$ at the Earth is connected to the number density through $\Phi=v /4\pi \;\psi$.
}
We solve the transport equation in Eq.~\ref{eq:diff} in a semi-analytic model,
assuming a spatially uniform diffusion coefficient:
\begin{equation}
\label{eq:diff_coeff}
 K(E)= \beta K_0 (\mathcal{R}/1 \text{GV})^\delta \simeq K_0 (E/1 \text{GeV})^{\delta}
\end{equation}
where $\beta=v/c$ (for relativistic $e^\pm$, as in this analysis, $\beta=1$)
and $\mathcal{R}$ is the particle rigidity.
We include $e^\pm$ energy losses by Inverse Compton  scattering off the interstellar radiation field,
and synchrotron losses on the Galactic magnetic field.
A full-relativistic treatment of Inverse Compton losses has been implemented in the Klein-Nishina regime, according to Ref.~\cite{2010A&A...524A..51D}.
\reply{The black body approximation for the interstellar photon populations
at different wavelengths has been taken from \cite{2010A&A...524A..51D} (model M2 in their Table 2).
The Galactic magnetic field intensity
has been assumed $B=3.6\; \mu$G, as resulting from the sum (in quadrature) of the regular and turbulent components \citep{2007A&A...463..993S}.}
At the energies considered here,  the energy losses dominate over  diffusion effects.
Therefore, modifications of the diffusion coefficient are not expected to modify significantly our conclusions.
The propagation parameters are fixed according to the fits to CR data performed within a semi-analytical diffusion model in \cite{Kappl:2015bqa} (K15) and \cite{Genolini:2015cta} (G15)
(see also \cite{Manconi:2016byt}).
As for the K15 model, it is found to be $K_0=0.0967$ kpc$^2$/Myr and \reply{$\delta=0.408$, while for the G15 model $K_0=0.05$ kpc$^2$/Myr and $\delta=0.445$}.
The values found in these two papers are also compatible with the ones derived in \cite{Johannesson:2016rlh,Korsmeier:2016kha}.

\reply{Given our focus on single sources, we report here the explicit solutions of the time-dependent transport equation for the CR flux from a single source of $e^-$, which  can be  also found in several literature works (see  e.g. \cite{PhysRevD.52.3265,Aharonian:1995zz,Mlyshev:2009twa, 2010A&A...524A..51D}).
In the burst-like approximation, the CR $e^-$ and $e^+$ density $\mathcal{\psi}(E,\mathbf{x})$ at a position $\mathbf{x}$ (in Galactic coordinates) and energy $E$, and   considering an infinite diffusion halo, reads:
 \begin{equation}\label{eq:singlesourcesolution}
  \mathcal{\psi}(E,\mathbf{x}) = \frac{b(E_s)}{b(E)} \frac{1}{(\pi \lambda^2)^{\frac{3}{2}}} \exp\left({-\frac{|\mathbf{x} -\mathbf{x_{s}} |^2}{ \lambda^2}}\right)Q(E_s)
\end{equation}
where $b(E)$ is the energy loss function, $\mathbf{x_{s}}$ indicates the source position. $\lambda$ is the typical propagation scale length:
\begin{equation}
\label{eq:lambda}
 \lambda^2= \lambda^2 (E, E_s) \equiv 4\int _{E} ^{E_s} dE' \frac{K(E')}{b(E')},
\end{equation}
where \replyy{$E_s(E)\equiv E_s(E;t,t_s)$}  is the initial energy of $e^\pm$ that cool down to $E$ in a {\rm loss time} $\Delta \tau$:
\begin{equation}
 \Delta \tau (E, E_s) \equiv \int_{E} ^{E_s} \frac{dE'}{b(E')} = t-t_{{\rm s}} \quad ,
\end{equation}
and $t_{{\rm s}}$ is the source age.
}
\reply{As for the evolutionary escape model in Ref.~\cite{2012MNRAS.427...91O} the $\mathcal{\psi_{\rm esc}}(E,\mathbf{x})$ of runaway CR $e^\pm$ at a position $\mathbf{x}$  and energy $E$, and   considering an infinite diffusion halo is:
 \begin{equation}\label{eq:sol_esc}
  \mathcal{\psi}_{\rm esc}(E,\mathbf{x}) = \frac{b(E_s(E))}{b(E)} \frac{1}{(\pi \lambda^2)^{\frac{3}{2}}} \exp\left({-\frac{|\mathbf{x} -\mathbf{x_{s}} |^2}{ \lambda^2}}\right)Q_{\rm esc}(E_s(E))
\end{equation}
where $E_s$ is again the initial energy of $e^\pm$ that cool down to $E$, defined now as:
\begin{equation}
 \int_{E} ^{E_s(E)} \frac{dE'}{b(E')} = t-T_{\rm esc}(E_s)\,,
\end{equation}
\replyy{and $T_{\rm esc}$ is given by Eq.~\ref{eq:Tesc}.}
\replyy{The energy spectrum $Q_{\rm esc}(E_s(E))$ is defined in Eq.~\ref{eq:Qesc}, and is obtained as \cite{2012MNRAS.427...91O}:
\begin{equation}
Q_{\rm esc}(E) = \int dt\int d \mathbf{x} \, q(E, \mathbf{x}, t)\,,
\end{equation}
and the solution reported in Eq.~\ref{eq:sol_esc} is given for a source term in the form $q(E, \mathbf{x}, t)= \delta(\mathbf{x}) \delta (t-T_{\rm esc}(E))Q_{\rm esc}(E) )$.}
}

\subsection{The radio synchrotron emission from nearby SNRs}
\label{sec:synchro}
One of the key points of this paper is the inspection of selected near SNRs in terms of the available flux radio data, in order to obtain a better understanding of  $e^-$ and $e^+$ flux data.
The very-high-energy $e^-$ and $e^+$ flux and the radio data for nearby sources are connected under the hypothesis that the radio emission from the source is due to synchrotron radiation from $e^-$ accelerated and interacting with the SNR magnetic field.

Under the hypothesis that the radio emission from the source is due to synchrotron radiation from $e^-$ accelerated and interacting with the SNR magnetic field $B$, the normalization of the injection spectrum $Q_{0,\rm{SNR}}$ can be connected to the radio flux density $B^{\nu}_r(\nu)$:
\begin{equation}
 \label{eq:Br}
Q_{0,\rm{SNR}} = 1.2 \cdot 10^{47}  \text{GeV}^{-1} (0.79)^{\gamma}  \frac{B^{\nu}_r(\nu)}{\text{Jy}}
 \left[ \frac{d}{\text{kpc}}\right]^{2}
\left[ \frac{\nu}{\text{GHz}}\right]^{\frac{\gamma -1}{2}}
\left[ \frac{B}{100 \mu\text{G}}\right]^{-\frac{\gamma+1}{2}}.
\end{equation}
The derivation of this expression is extensively provided in \cite{2010A&A...524A..51D}, and it was successively used also in \cite{DiMauro:2014iia,Manconi:2016byt}.
The energy emitted at a given frequency is radiated at the energy loss rate \replyy{$b(E(\nu))$}
(see Eqs.~48-50 in \cite{2010A&A...524A..51D}), and one implicitly assumes that observation takes place within the
time-interval $E(\nu)/b(E(\nu))$ \replyy{($E(\nu)=h \nu$)} during which the $e^-$ radiate
after the burst, and that the flux is quasi constant within this time interval.
We note in Eq.\eqref{eq:Br} the well-known relation between the index of the $e^-$ distribution $\gamma$ and the radio index $\alpha_r= (\gamma -1)/2$.
\reply{The $Q_{0,\rm{SNR}}$ term in Eq. \ref{eq:Br} is implemented by Eq. \ref{eq:Q_E} in case of the burst-like approximation.
In case of the evolutionary escape model, we instead implement in Eq.~\ref{eq:Br} the $Q_{0,\rm{trap}}$ of Eq.~\ref{eq:QTrap2}. }
 \begin{figure}[t]
  \includegraphics[width=0.5\textwidth]{fig1left_near_SNRs_winkler_1kpc_noradioEc10TeV_democratic_gamma2_Etot7e47.pdf}
  \includegraphics[width=0.5\textwidth]{fig1right_near_SNRs_winkler_1kpc_noradioEc10TeV_catalogQ0.pdf}
  \caption{Electron flux at Earth from near SNRs in the Green catalog at $d<1$~kpc from the Earth.
  Left: A common spectral index of $\gamma=2.0$ and a total energy released in $e^-$ of $E_{\rm tot}=7 \cdot 10^{47}$~erg has been assumed for each source.
  Right: The spectral index and the $Q_0$ for each source are fixed  according to the catalog data and Eq.\ref{eq:Br} for a single frequency.
  All the curves are computed for $E_c=10$~TeV and K15 propagation model.
  }\label{fig:nearsnr}
 \end{figure}

Our search for the sources that can contribute most to the  $e^-$ flux rests on the computation of the  $e^-$ from
catalogued sources. We consider the sources in the Green SNR catalog \cite{Green:2014cea}, and  find seven SNRs which are located at $d<1$ kpc from the Earth.
In order to illustrate the role of these SNRs,  we compute their flux of $e^-$ at Earth. We first assume that they all inject  $e^-$ in the ISM with the
 common spectral index of $\gamma=2.0$ and with a total energy released in $e^-$ of $E_{\rm tot}=7 \cdot 10^{47}$~erg, as very often assumed in the literature (see e.g. \cite{Kobayashi:2003kp}).
The only catalogued parameters here are the distance and the age of the source.
The results are shown in the left panel of Fig.~\ref{fig:nearsnr}. Vela YZ  turns out to be the most powerful source, followed by Cygnus Loop. Electrons from the other sources have fluxes smaller than up one order of magnitude.
Indeed, the Green  catalog \cite{Green:2014cea} also provides the spectral index and the radio properties for each source that,
when implemented in Eq.~\ref{eq:Q_E}, lead to the fluxes in Fig.~\ref{fig:nearsnr}, right panel.
This more realistic approach demonstrates that the only two powerful sources are indeed Vela YZ and Cygnus Loop,
while the other SNRs contribute with an $e^-$ flux at Earth which is at the percent level of the Vela YZ one.
We identify Vela YZ and Cygnus Loop  as the candidates
expected to contribute most significantly to the high-energy tail of $e^{+}+e^{-}$ flux, given their distance, age and radio flux \cite{Kobayashi:2003kp,DiMauro:2014iia,Manconi:2016byt}.
As shown in the following, Vela Jr can emerge as a significant contributor to the $e^{+}+e^{-}$ flux in the TeV range when the leptonic model inferred in \cite{2008ApJ...678L..35K} is considered, given the high value for the cutoff of $E_c=25$~TeV and the low magnetic field ($12\mu$G).

\section{\label{sec:radio}Results on the SNR  properties from radio data}
 \begin{figure}[t]
  \includegraphics[width=0.5\textwidth]{fig2left_Snu_velaYZfit.pdf}
  \includegraphics[width=0.5\textwidth]{fig2right_Snu_cygnusfit.pdf}
  \caption{A fit to the radio spectrum of Vela SNR (left panel) and Cygnus Loop (right panel) using Eq.~\eqref{eq:Br}.
   The red line represents the best fit model to the data.
   The integrated flux densities $B_r$ are taken from \cite{2001A&A...372..636A, 2004A&A...426..909U}.
  }\label{fig:radio}
 \end{figure}
With respect to previous analysis where usually a single frequency was considered (see, e.g., \cite{DiMauro:2014iia,DiMauro:2017jpu}),
we use here the radio spectrum in the widest available range of frequencies:
from 85.7~MHz to 2700~MHz for Vela YZ \cite{2001A&A...372..636A} and from $22$~MHz to $4940$~MHz for Cygnus Loop \cite{2004A&A...426..909U}.
We fix the Vela YZ (Cygnus Loop) distance and age to be: $d=$ 0.293~kpc (0.54~kpc) and $T=$11.3~kyr (20~kyr) \cite{2003ApJ...596.1137D,2005AJ....129.2268B,1994PASJ...46L.101M,2004A&A...426..909U}, respectively.
The magnetic field of galactic SNRs is often inferred from multi-wavelength analysis, and the values typically range between few $\mu$G to even $10^3\mu$G \cite{2012SSRv..166..231R}.
The magnetic field of Vela YZ is here fixed to $B=$ 36 $\mu G$, corresponding to a mean of the values inferred from X-ray data for the Y and Z regions \cite{Sushch:2013tna}, while for Cygnus Loop  we consider the best fit value of $B=60$~$\mu G$ of the hadronic model for the gamma-ray analysis in \cite{2011ApJ...741...44K}.
In Fig.~\ref{fig:radio}  we display the results for the fit to the available radio data of both Vela YZ and Cygnus Loop.

We then invert Eq.~\ref{eq:Br} to fit $B^{\nu}_r(\nu)$ as a function of $\gamma$ and $Q_{0,\rm{SNR}}$ for all the
available frequencies $\nu$.
We tune the injection spectrum of local SNRs in order to reproduce the radio data, since at this wavelength the $e^-$ are the main emitters.
It is worth noting that \reply{in the case of burst-like approximation} we work under the assumption that the electromagnetic emission we observe today from those SNRs reflects the properties of the  $e^-$ population that has been released and injected in the ISM.
The best fit parameters are:
$\gamma_{\rm{Vela}}= 2.47\pm0.10$, $E_{\rm{tot}, \rm Vela}= (2.28\pm0.06)\cdot 10^{47}$ erg,  $\gamma_{\rm{Cygnus}}= 2.04\pm0.04 $ and $E_{\rm{tot}, \rm Cygnus}= (1.18\pm 0.16)\cdot 10^{47}$ erg. The numbers for the Vela YZ are in agreement with the findings of \cite{Sushch:2013tna}.

The  parameter space  $E_{\rm{tot}}$ -  $\gamma$ selected by the fit to the radio spectrum is reported in the left panel
of Fig.~\ref{fig:radioresults} for both Vela YZ and Cygnus Loop, and for $3\sigma$, $2\sigma$ and $1\sigma$ confidence levels.
This figure shows that radio data select narrow ranges for $\gamma$ and $E_{\rm{tot}}$.
For example, the $1\sigma$ contour for $\gamma_{\rm{Vela}}$ and $E_{\rm{tot, Vela}}$ is a few \% from the best fit.
Moreover, $E_{\rm{tot}}$ of the order of $10^{47}$ erg is in agreement with the usual expectations for the SNR energy budget, given the total energy released by a SN explosion in the ISM of  $\sim 10^{51}$~erg \cite{2007Sci...315..825M} and  a fraction conferred to $e^-$ of $\sim 10^{-5}-10^{-3}$ \cite{2009A&A...499..191T}.
We now evaluate the consequences of these results on the $e^++e^-$ flux.
In the right panel of Fig.~\ref{fig:radioresults} we plot  the data on the $e^++e^-$ flux
along with the predictions for the flux from Vela YZ and Cygnus Loop  obtained by the parameters selected within the  $2\sigma$ contours in the left panel.
The $e^++e^-$ flux data have not been used in this analysis and are displayed in the figure for illustrative purposes.
The information in Fig.~\ref{fig:radioresults} is remarkable: the flux of $e^-$ from the closest SNRs as derived from a fit to radio data is slightly below the data on the inclusive flux.
The flux from Vela YZ and Cygnus Loop can skim the HESS data, when all the uncertainties are considered.
In the assumption that all the radio emission is synchrotron radiation from $e^-$, our predictions indicate the highest flux expected from these sources
can shape the high energy tail of the $e^++e^-$ flux data.

 \begin{figure}[t!]
  \includegraphics[width=0.5\textwidth]{fig3left_Etot_vela_cygnus_radio.pdf}
  \includegraphics[width=0.5\textwidth]{fig3right_radioband_2sigma_def.pdf}
  \caption{Results of the fit to the radio spectrum for Vela YZ (gray) and Cygnus Loop (magenta).
  Left: Regions of the parameter space  $E_{\rm{tot}}$, $\gamma$ selected by the fit to the radio spectrum.
  The solid, dashed and long-dashed lines refer to respectively $3\sigma$, $2\sigma$ and $1\sigma$ contours for each source.
  Right: Prediction for the $ e^-$ flux from Vela YZ and Cygnus Loop using the values of $E_{\rm{tot}}$, $\gamma$
  within $2\sigma$ from the best fit to the radio spectrum shown in the left panel.
  The $e^++e^-$ {\it Fermi}-LAT, AMS-02, DAMPE, HESS and CALET data with their statistics and systematic errors are also shown.
  }\label{fig:radioresults}
 \end{figure}
 \begin{figure}[t]
  \includegraphics[width=0.5\textwidth]{fig_esc_left_Etot_vela_cygnus_radio_col.pdf}
  \includegraphics[width=0.5\textwidth]{fig_esc_right_radioband_2sigma_col.pdf}
  \caption{\reply{Results of the fit to the radio spectrum for Vela YZ (gray) and Cygnus Loop (magenta) for the evolutionary model of the injection of $e^-$ from SNRs in Ref.~\cite{2012MNRAS.427...91O}.
  Left: Regions of the parameter space  $E_{\rm{tot,trap}}$, $\gamma$ selected by the fit to the radio spectrum for Vela YZ (gray) and Cygnus Loop (magenta).
  The derived regions for $E_{\rm{tot, esc}}$, $\gamma + \beta/\alpha$ are also reported for Vela YZ and Cygnus Loop.
  The solid, dashed and long-dashed lines refer to respectively $3\sigma$, $2\sigma$ and $1\sigma$ contours for each source.
  Right: Prediction for the $ e^-$ flux from Vela YZ and Cygnus Loop using the values of $E_{\rm{tot, esc}}$, $\gamma+\beta/\alpha$
  within $2\sigma$ from the best fit to the radio spectrum shown in the left panel.
  The $e^++e^-$ data are shown as in Fig.~\ref{fig:radioresults}, right panel.
  }}\label{fig:radioresults_esc}
 \end{figure}

\reply{We have explored the effects of the evolutionary escape model on the interpretation of radio spectrum for our two selected sources.
In this case, the radio data are fitted through  Eq.~\ref{eq:Br} to tune the normalization and spectral index of the trapped $e^-$, namely the $Q_{0,\rm{trap}}$  and the index $\gamma$ of Eq.~\ref{eq:QTrap2}. The total energy of trapped $e^-$ is obtained as:
\begin{equation}
 E_{\rm tot, trap} = \int _{E_1} ^{ E_{\rm m, esc}(T)} dE \, E \,Q_{\rm trap}(E) \,,
 \label{eq:Etottrap}
\end{equation}
for each source.
The normalization $A$ and spectral index of the escaped electrons are then derived by their relations with the trapped $e^-$, as derived in the evolutionary escape model in Ref.~\cite{2012MNRAS.427...91O}.
By comparing Eq.~\ref{eq:QTrap2} and Eq.~\ref{eq:Qesc}, we obtain:
\begin{equation}\label{eq:relation_trap_esc}
 A=Q_{\rm 0,trap} E_{\rm knee}^{\beta/\alpha} \, \left( \frac{t_{\rm Sedov}}{T}\right)^{\beta}\quad,
\end{equation}
while the spectral index of $e^-$ in Eq.~\ref{eq:Qesc} is simply $\gamma+\beta/\alpha$.
The total energy of runaway $e^-$ for each source is then obtained as:
\begin{equation}
 E_{\rm tot, esc} = \int _{E_{\rm m, esc}(T)} ^{ \infty} dE \, E \,Q_{\rm esc}(E) \,.
 \label{eq:Etotesc}
\end{equation}
In Fig.~\ref{fig:radioresults_esc} (left panel) the parameter space $E_{\rm{tot, trap}}$ -  $\gamma$ ( $E_{\rm{tot, esc}}$ -  $\gamma +\beta/\alpha$) selected by the fit to the radio spectrum of Vela YZ and Cygnus Loop are shown for $3\sigma$, $2\sigma$ and $1\sigma$ confidence levels.
The selected intervals are narrow, and similar to the burst-like case for Vela YZ, see Fig.~\ref{fig:radioresults}.
For Cygnus Loop the total energy of trapped $e^-$ is reduced by less than a factor of two.
This is understood through  Eq.~\ref{eq:Etottrap}. The upper limit of the integral  is indeed $E_{\rm m, esc}(T)\sim 88~(17)$~GeV for Vela YZ (Cygnus Loop).
The derived constraints on the parameter space $E_{\rm{tot, esc}}$ -  $\gamma + \beta/\alpha$ are also reported.
Each of the two regions shows a strong correlation.
The total energy  $E_{\rm tot, esc}$ of runaway $e^-$ is more than one orders of magnitude lower with respect to $E_{\rm tot, trap}$ for Vela YZ. As for Cygnus Loop, the difference is a factor of 2-3 for the best fit.
This is again understood by the different $E_{\rm m, esc}(T)$ of the two sources.
The  consequences of these results on the $e^++e^-$ flux are reported in Fig.~\ref{fig:radioresults_esc} (right panel).
We plot again the data on the $e^++e^-$ flux,
along with the predictions for the flux of runaway $e^-$ from Vela YZ and Cygnus Loop.
The flux of CR $e^-$ at Earth is computed  by using Eq.~\ref{eq:sol_esc}, and by using
the parameters for the escaped $e^-$ selected within the  $2\sigma$ contours in the left panel.
The flux from Vela YZ and Cygnus Loop is softer with respect to the burst-like approximation, reflecting the effect of the escape mechanism described in Eq.~\ref{eq:Qesc}.
Moreover, compared to the burst-like approximation, the presence of an escape-limited maximum energy $E_{\rm m, esc}(T)$ for each source depletes the flux at Earth for $E<E_{\rm m, esc}(T)$.
Considering all the uncertainties, under the evolutionary escape model the flux from Vela YZ and Cygnus Loop is predicted to contribute at most few percent to the data on the inclusive flux at TeV energies, a rough factor of two less than what is shown in Fig.~\ref{fig:radioresults}.
}

\section{\label{sec:flux}Results on the SNR  properties from $e^++e^-$ flux data}\label{sec:flux}
We now perform an analysis aimed at characterizing the $e^-$ emission from Vela YZ and Cygnus Loop SNRs through $e^++e^-$ (and $e^+$) flux data only.
We want to assess the power of $e^++e^-$ data on the source properties with respect to the information brought by radio  (see Sect. \ref{sec:radio})
or the dipole anisotropy data (see Sect. \ref{sec:dipole}). We already know that these sources can contribute significantly to the  $e^-$ flux (see  \cite{DiMauro:2014iia,Manconi:2016byt,DiMauro:2017jpu}
and Fig.~\ref{fig:radioresults}). Therefore, we expect that the  $e^++e^-$ flux data will bound the contribution from local sources. This results will be quantified by
bounds on  $\gamma$ and $E_{\rm{tot}}$, parameters effectively connected with the injection physics and the number of particles per unit energy released in the ISM.
\\
In order to explain the $e^++e^-$ data over many energy decades we consider, in addition to $e^{-}$ from SNRs,
$e^{+}$ and $e^{-}$ produced by interactions of CRs on the ISM (secondary component) and by pair emission in PWNe \cite{Gaensler:2006ua, 2017SSRv..207..235B}.
We use here the model already employed in \cite{2010A&A...524A..51D,DiMauro:2014iia,Manconi:2016byt,DiMauro:2017jpu}. In particular, we refer to  \cite{Manconi:2016byt}
for any detail.  We only outline here the main characteristics of the different contributors.
The Galactic SNRs are divided into a {\it near} and a {\it far} population according to their distance $d$ from the Earth. As in Ref.  \cite{Manconi:2016byt}, we set $d = 0.7$ kpc.
Since for sources near the Earth we dispose of abundant data, we model them individually picking their
$d$, $T$, $B_r^{\nu}(\nu)$ and $\gamma$ from the Green's catalog \citep{Green:2014cea}.
Far SNRs, for which the distance from Earth is $>0.7$ kpc, are instead assumed to be smoothly distributed in the Galaxy according to
the spatial density profile in \cite{2015MNRAS.454.1517G}, and to inject $e^-$ in the ISM with an average  $E_{\rm{tot}}$ and $\gamma$.

As for the local SNRs, Vela YZ and Cygnus Loop will be modeled with free $E_{\rm tot}$ and spectral index $\gamma$.
Instead, the contribution from Vela Jr is fixed to the leptonic model of \reply{\cite{2011ApJ...740L..51T}}.
In particular we choose the values of \reply{$d=0.750$~kpc, $t=3$~ky, $B=12 \mu$G and $\gamma_{\rm{VelaJr}}=2.15$} \cite{2011ApJ...740L..51T,2008ApJ...678L..35K} and we compute the $Q_{0,\rm{VelaJr}}$ by using Eq.~\ref{eq:Br}.
This choice is motivated by very limited information available for its radio flux, and because Vela Jr mainly contributes to $e^++e^-$ flux above 10 TeV where the very few data points are not constraining.

Similarly to SNRs, the injection spectrum $Q_{ \rm PWN}(E)$ of $e^{-}$ and $e^{+}$ emitted by a PWN  can be described by a power law with an exponential cut-off. The normalization of the PWN spectrum $Q_{0, \rm PWN}$ can be connected to the  spin-down energy of the pulsar $W_0$ by:
\begin{equation}
 \int_{E_{\rm min}}^{\infty}\,dE\,E\,Q_{ \rm PWN}(E)\,=\eta_{\rm PWN}\,W_0.
 \label{eq:PWN}
 \end{equation}
 $W_0$ can be thus  constrained from the measured pulsar properties and assuming that the whole energy lost is carried by the magnetic dipole radiation \cite{2010A&A...524A..51D}. The factor $\eta_{\rm PWN}$ represents the efficiency with which the spin-down energy of the pulsar is converted into $e^{-}$ and $e^{+}$ pairs,
and is expected to be of few $\%$ level~\cite{DiMauro:2014iia,DiMauro:2015jxa,Abeysekara:2017old}.
Our PWN sample is taken, as in~\cite{DiMauro:2014iia,DiMauro:2015jxa,Manconi:2016byt}, from the ATNF catalog \cite{ATNFcat}, from which we extract the spin-down energy, age and distance of each known PWN. All PWNe share a  common efficiency $\eta_{\rm PWN}$ and spectral index $\gamma_{\rm PWN}$, that will enter in our fits to the  $e^+$ and $e^-$ data as free parameters. Since the release of accelerated $e^-$ and $e^+$ pairs in the ISM  is estimated to occur after $40-50$ kyr after the pulsar birth \cite{2011ASSP...21..624B}, we select only sources with $t_{\rm obs}>50$~kyr.
Secondary leptons originated by the scatterings of proton and helium CRs off the ISM are modeled here following \cite{DiMauro:2015jxa}, using a free overall re-normalization factor $q$, which accounts for  uncertainties in the flux of primary CRs and in the production cross sections.

We fit the $e^++e^-$ flux data from HESS, CALET, DAMPE, AMS-02 and {\it Fermi}-LAT and AMS-02  $e^+$ flux with all the components described above.
We avoid strong biases from the solar modulation of the fluxes considering AMS-02, CALET and {\it Fermi}-LAT $e^{+}+e^{-}$ and AMS-02 $e^{+}$ data at $E>10$~GeV.
We nevertheless include its effect in the force field approximation with the Fisk potential $\phi$ treated as  a free parameter. We use different $\phi_i$ in the fit to AMS-02, {\it Fermi}-LAT and CALET data since they cover different periods.
We take into account in the fit both the statistical and systematic uncertainties.
We also include the uncertainty in the absolute energy scale taking $1.3\%$ for DAMPE \cite{Ambrosi:2017wek}, $5\%$ for CALET \cite{PhysRevLett.119.181101}, $0\%$ at 10~GeV to $5\%$ at 1 TeV with a linear trend in $\log{E}$ for {\it Fermi}-LAT, $2\%$ for $E=[10,290]$~GeV and $5\%$ for AMS-02, while for HESS we use the systematic band as reported in \cite{HESSICRC17}.
The fit is performed on the $e^++e^-$ and $e^+$ flux data with free parameters: $E_{\rm{tot},\rm{Vela}}$, $E_{\rm{tot},\rm{Cygnus}}$,  $\gamma_{\rm{Vela}}$,
 $\gamma_{\rm{Cygnus}}$, $E_{\rm{tot}}$, $\gamma$, $\eta_{\rm PWN}$, $\gamma_{\rm PWN}$, $q$, $\phi_i$.
We only impose priors on $\gamma_{\rm{Vela}}$ ([1.90-3.10]) and   $\gamma_{\rm{Cygnus}}$ ([1.50-2.50]).
The best fit ($\chi_{\rm red}^2 = \chi^2/\rm{d.o.f.} = 0.5$) parameters are
 $\gamma_{\rm{Vela}}= 2.9\pm0.1$, $E_{\rm{tot},\rm{Vela}}=(2.4\pm0.2)\cdot10^{50}$~erg,
 $\gamma = 2.70\pm0.06$, $E_{\rm{tot}}=(4.89\pm0.13)\cdot10^{47}$~erg,
$\eta_{\rm{PWN}}= 0.056\pm0.006$ and $\gamma_{\rm{PWN}} = 1.80\pm0.04$ for Vela YZ and Cygnus Loop SNRs.
 \begin{figure}[t]
  \centering
  \includegraphics[width=0.6\textwidth]{fig4_Etot_velacygnus_fluxfit_radioblind.pdf}
  \caption{Regions of the parameter space $E_{\rm{tot}}$ -  $\gamma$ selected by the fit to the $e^{+}+e^{-}$ and $e^{+}$ flux data for  Vela YZ and Cygnus Loop.
  The shaded regions denote the $E_{\rm{tot}}$, $\gamma$ values at a given number of $\sigma$ from the best fit for each source. The magenta region is for Cygnus Loop and $2\sigma$, while the
   gray (light gray) regions are for Vela YZ and $2\sigma$  ($5\sigma$).
  }\label{fig:fluxresults}
 \end{figure}
The configurations within $2\sigma$ from the best fit for Vela YZ and Cygnus Loop free parameters are reported in Fig. \ref{fig:fluxresults}.
For Vela YZ we also report the $5\sigma$ region which, as for Cygnus Loop, opens indeed to an upper bound.
In the case of Vela YZ, we find that the 2$\sigma$ region from the best fit for $E_{\rm{tot},\rm{Vela}}$ and $\gamma_{\rm{Vela}}$ is narrow and the two parameters are strongly correlated.
The $E_{\rm{tot},\rm{Vela}}$ values selected by the $e^++e^-$ flux have no overlap (at $2\sigma$) with the ones constrained by the fit to radio flux data, and are systematically higher by at least one order of magnitude. The two regions fully overlap at $5 \sigma$ (see  Fig.~\ref{fig:radioresults}).
If we perform the same analysis for DAMPE data alone, or for the combination of AMS-02, CALET and HESS data, the two regions fully overlap at $2 \sigma$.

\section{\label{sec:dipole}Results on the SNR  properties from $e^++e^-$ dipole anisotropy data}
We now assess the power of the recent  {\it Fermi}-LAT data on the $e^++e^-$ dipole anisotropy  $\Delta_{e^++e^-}$  \cite{Abdollahi:2017kyf}.
This measure has provided upper bounds on  $\Delta_{e^++e^-}$ as a function of energy from 50 GeV up to about 1 TeV.
We compute the relevant single source dipole anisotropy for the sources in our model, following \cite{Manconi:2016byt}.
We remind here that the $\Delta_{e^++e^-}$  from a single source $s$ is given by:
\begin{equation}
\label{eq:eleposdipole}
  \Delta(E)_{e^+ + e^-} = \frac{3 K(E)}{ c} \frac{2 d}{\lambda^2(E, E_{s})} \frac{\psi_{e^+ + e^-}^{s}(E)}{\psi_{e^+ + e^-}^{tot}(E)},
\end{equation}
where $d$ is the distance to the source,
$\lambda(E, E_{s})$ is the propagation scale defined in Eq.~\ref{eq:lambda},
$\psi_{e^+ + e^-}^{s}(E)$ is the $e^+ + e^-$ number density produced by the source $s$, and $\psi_{e^+ + e^-}^{tot}(E)$ is the total $e^+ + e^-$ number density obtained from the contributions of all the sources, both from isotropic smooth populations and from directional single sources.
This expression can be appropriately associated to a physical observable whenever the source $s$ can be considered as dominant.
In case more than one source is considered, the total dipole anisotropy may be computed as  \cite{Manconi:2016byt}:
\begin{equation}
\label{eq:dipolesources}
 \Delta(n_{max}, E)= \frac{1}{\psi^{tot}(E)} \cdot \sum_i \frac{\mathbf{r}_i\cdot \mathbf{n}_{max}}{||\mathbf{r}_i||}\cdot \psi_i(E)\, \Delta_i(E).
\end{equation}
Here $\psi_i(E)$ is the  number density of $e^-$ and/or $e^+$ emitted from each source $i$, $\mathbf{r}_i$ is the
 source position in the sky and
$n_{max}$ is the direction of the maximum flux intensity. The term $\psi^{tot}(E)=\sum_i \psi_i(E)$ is the total ($e^-$ and/or $e^+$) number density and includes the contribution from the discrete as well as all the isotropic sources.
The anisotropy from each single source is given by $\Delta_i = \frac{3 K(E)}{c} \frac{|\nabla \psi_i(E) |}{\psi_i(E)}$, where the gradient is performed with respect to each source position.
 \begin{figure}[t]
  \centering
  \includegraphics[width=0.6\textwidth]{fig5_anis_VelaCygnus_winkler_ALLDATA_noradio.pdf}
  \caption{Dipole anisotropy predictions for Vela YZ and Cygnus Loop treated as single dominant sources (solid black and magenta lines, respectively),
  and for all the sources combined together, shown  as gray dot-dashed line  (see text for details).
  The upper limits for {\it Fermi}-LAT dipole anisotropy are shown for the two different methods in \cite{Abdollahi:2017kyf}.
  }\label{fig:dipoleresults}
 \end{figure}
We compute the $\Delta_{e^++e^-}$ for Vela YZ and Cygnus Loop for all the parameters selected by the fit to ${e^++e^-}$ flux data \replyy{described in Sec.~\ref{sec:flux}} (at $2\sigma$ from the best fit),
and reported in Fig. \ref{fig:fluxresults}. The maximum of  $\Delta_{e^++e^-}$ in each energy bin is then plotted as a black (magenta) solid line in Fig.~\ref{fig:dipoleresults} for Vela YZ (Cygnus Loop).
We compare our predictions to the {\it Fermi}-LAT $\Delta_{e^++e^-}$ data (Bayesian Method 1 in \cite{Abdollahi:2017kyf})
above 100~GeV, to limit the effect from the solar wind \citep{Buesching:2008hr,STRAUSS20141015}.
For Vela YZ, the anisotropy overshoots {\it Fermi}-LAT upper limits on the whole spectrum. We can therefore infer that {\it Fermi}-LAT data on the lepton dipole anisotropy add an independent piece of information
in addition to the flux data. This is one of the main results of this paper. The anisotropy amplitude data on {\it charged}
leptons have now the power to exclude configurations of the Vela YZ source spectrum,
in principle compatible with the absolute flux data.
For Cygnus Loop the conclusions are looser, since it shines at higher energies where the {\it Fermi}-LAT upper bounds are looser.
In order to constrain Cygnus Loop parameters one would need dipole data at least up to 10 TeV.

Since we are interested in the scenario in which the $\Delta_{e^++e^-}$ is maximal, we have checked for different effects that could lower our predictions.
In particular, we verified that also the total dipole anisotropy arising from all the individual sources entering in the predictions of the ${e^++e^-}$ and $e^+$ fluxes is not compatible with the experimental upper limits.
This is because Vela YZ is always the dominant contributor of the $e^-$ flux.
We  computed the total anisotropy according to Eq.~\ref{eq:dipolesources} resulting from:
the local SNRs Vela YZ, Cygnus Loop and Vela Jr, and all the ATNF catalog PWNe.  The results shown in \replyy{Fig.  \ref{fig:dipoleresults} as a gray dot-dashed line} has been obtained
setting all the free parameters to their best fit to the ${e^++e^-}$ and $e^+$ fluxes data. The only prior being the flux data, Vela YZ turns out to dominate the flux as well as the dipole predicted at Earth.
Moreover, we considered the potential effect of the guide magnetic field over the few hundred pc to the nearest sources, following what was done in \cite{2016PhRvL.117o1103A}.
The local magnetic field properties were inferred by IBEX data ($l=210.5^{\circ}, b=-57.1^{\circ}$) \cite{0004-637X-776-1-30} from the study of the emission of high energy neutral atoms.
As discussed in \cite{2016PhRvL.117o1103A}, the alignment of the dipole anisotropy of CRs with the total ordered magnetic field is demonstrated to potentially modify the phase of the observed CR dipole and lower its amplitude.
We verified that projecting the dipole anisotropy of Vela YZ along the direction of the local magnetic field decreases the $\Delta_{e^++e^-}$  by a factor of roughly 2.
Since the maximal Vela YZ anisotropy in Fig.~\ref{fig:dipoleresults} overshoots the {\it Fermi}-LAT upper limits by more than a factor of 3 up to $500$ GeV, also considering this effect would not change our conclusions.
Therefore, the dipole anisotropy in the CR lepton arrival direction sets additional tight constraints to the Vela YZ injection spectrum.

 \begin{figure}[t]
  \centering
  \includegraphics[width=0.6\textwidth]{fig6_Etot_vela_fluxfit_radioblind_dipole_new.pdf}
  \caption{Dipole anisotropy constraints to the Vela YZ source parameters.
  The regions of the parameter space $E_{\rm{tot}}$, $\gamma$ selected by the fit to the $e^{+}+e^{-}$ and $e^{+}$ flux data for  Vela YZ  are reported with shaded regions as in Fig.\ref{fig:fluxresults}.
  The hatched  region denotes the configurations selected by $e^{+}+e^{-}$ and $e^{+}$ flux data and excluded by {\it Fermi}-LAT dipole anisotropy upper limits (Meth. 1) at $E>100$~GeV.
  }\label{fig:dipoleconstraints}
 \end{figure}
We now quantify the power of the dipole anisotropy to exclude configurations in the Vela YZ source parameters, otherwise compatible with the  $e^{+}+e^{-}$ flux data.
We compute $\Delta_{e^++e^-}$ for all the configurations selected by the fit to the flux \replyy{described in Sec.~\ref{sec:flux}}.
Whenever our predictions overestimate one data point at $E>$~100~GeV, the $E_{\rm{tot},\rm{Vela}} - \gamma_{\rm{Vela}}$ pair is considered as excluded.
Very similar results are obtained when requiring two or more non-consecutive data points to be below the predictions,
or if we employ only the two highest energy data points.
The results are displayed by the hatched region in upper panel of  Fig.~\ref{fig:dipoleconstraints}.
The dipole anisotropy upper limits are not compatible  with the configurations selected by the fit to the flux data at 2$\sigma$, and with a subset of the configurations at 5$\sigma$.
Indeed, the anisotropy data exclude higher values of  $\gamma$, considered unlikely in acceleration models.
The {\it Fermi}-LAT data on $\Delta_{e^++e^-}$ supplement a valuable information of the
properties of Vela YZ, acting as a further physical observable for the understanding of the injection of $e^-$ in the ISM.

 \begin{figure}[]
  \includegraphics[width=0.5\textwidth]{fig7right_sum_winkler_radio_ALLDATA_Ec10TeV_noband.pdf}
   \includegraphics[width=0.5\textwidth]{fig7_left_anis_VelaCygnus_winkler_ALLDATA_radio.pdf}
   \caption{Results on the  $e^++e^-$ flux (left) and on the corresponding dipole anisotropies (right) from the multi-wavelength fit to all the data.
   Left: The contribution from secondary production (red dashed), PWNe (blue dot dashed), Vela YZ (black dotted), Cygnus Loop (magenta dot-dot dashed), Vela Jr (orange solid) and the far smooth distribution of SNRs (green dotted) are shown. The $e^++e^-$ {\it Fermi}-LAT, AMS-02, DAMPE, HESS and CALET data with their statistics and systematic errors are also shown.
   Right: The maximal dipole anisotropy predicted for Vela YZ and Cygnus Loop as single dominant sources are reported with black solid and magenta dashed lines as in Fig.\ref{fig:dipoleresults}.
  The total anisotropy resulting from the distribution of all the sources is shown with gray dot-dashed line.
  The upper limits for {\it Fermi}-LAT dipole anisotropy are shown for the two different analysis methods in \cite{Abdollahi:2017kyf}.
   }
   \label{fig:mw}
 \end{figure}

\section{\label{sec:multiw}Results  from multi-wavelength analysis}
We now combine all the three observables explored in the previous sections.
Specifically, we compare the dipole anisotropy of Vela YZ and Cygnus Loop with the {\it Fermi}-LAT upper bounds, for the parameters of these sources selected by radio and $e^++e^-$ fluxes.
We perform new fits on the  $e^++e^-$ and $e^+$ fluxes including the constraints for $E_{\rm{tot},\rm{Vela}}$, $\gamma_{\rm{Vela}}$, $E_{\rm{tot},\rm{Cygnus}}$, and $\gamma_{\rm{Cygnus}}$ derived from the fit to radio data. We minimize according to the following definition of the $\chi^2$:
\begin{equation}
\chi^2 = \sum^N_i \left(\frac{ \Phi^{\rm{model}}_i - \Phi^{\rm{data}}_i }{ \sigma^{\rm{data}}_i }\right)^2 + \sum^4_j \left(\frac{ \mathcal{P}^{\rm{model}}_j - \mathcal{P}^{\rm{data}}_i }{ \sigma^{\rm{data}}_{\mathcal{P},j} }\right)^2
\label{eq:chi}
\end{equation}
where the first term  is the statistical term that takes into account the difference between the model $\Phi^{\rm{model}}$  and the $e^+ + e^-$ flux data at $1 \sigma$ ($\Phi^{\rm{data}}$ and $\sigma^{\rm{data}}$).
The second term runs over Vela YZ and Cygnus Loop $E_{\rm{tot}}$ and $\gamma$ and accounts for the deviation of these parameters in the model $\mathcal{P}^{\rm{model}}$ with respect to the best fit and $1\sigma$ error ($\mathcal{P}^{\rm{data}}$ and $\sigma^{\rm{data}}_{\mathcal{P}}$) as derived above in the fit to radio data.

We find a very good agreement between $e^++e^-$ and radio data ($\chi_{\rm red}^2\approx0.70$) with $\gamma_{\rm{Vela}} = 2.39\pm0.15$, $E_{\rm{tot}, \rm Vela} = (2.3\cdot\pm0.2)\cdot 10^{47}$ erg, $\gamma_{\rm{Cygnus}} = 2.03\pm0.05$ and $E_{\rm{tot}, \rm Cygnus} = (1.25 \pm0.06)\cdot 10^{47}$ erg for K15 propagation models. Using G15 propagation model the best fit parameters are extremely similar.
We illustrate in Fig.~\ref{fig:mw} the result of the best fit for all the components to the $e^++e^-$ flux.
We checked that all the predictions for the dipole anisotropy within $2\sigma$ from the best fit are below the {\it Fermi}-LAT upper bounds, as explicitly shown in  Fig.~\ref{fig:mw}.
The $\gamma$ for the spatially smooth distribution of SNRs is $2.48/2.44$ for K15/G15, respectively.
We test different values for the cutoff energy of the smooth distribution and single SNRs. We find that the $\chi^2$ profile as a function of the cutoff energy is flat for $>10$ TeV while it worsens at low energy. The $95\%$ lower limit is at 8 TeV.
The putative $e^-$ injected by a radio unconstrained Vela SNR (see Sec.\ref{sec:flux}) are compensated in our framework
by the combination of $e^-$ produced by the Galactic smooth distribution of SNRs and all the PWNe.

 \begin{figure}[]
  \includegraphics[width=0.5\textwidth]{fig9_sum_winkler_radio_escape_ALLDATA_Ec10TeV_col}
   \includegraphics[width=0.5\textwidth]{fig9_anis_VelaCygnus_winkler_ALLDATA_radio_escape_mod_col.pdf}
   \caption{Same as Fig.~\ref{fig:mw} but using the evolutionary model of Ref.~\cite{2012MNRAS.427...91O} for the injection of $e^-$ by SNRs.}
   \label{fig:mw_evol}
 \end{figure}

\reply{In Fig.~\ref{fig:mw_evol} we report, on the same foot as Fig.~\ref{fig:mw}, the results obtained within the evolutionary escape model as discussed in Sec.~\ref{sec:model}.
We find again a good fit ($\chi_{\rm red}^2\sim 0.87$), with  $\gamma_{\rm{Vela} + \beta/\alpha} = 2.66\pm 0.14$ and  $\gamma_{\rm{Cygnus}} = 2.27\pm0.06$  for K15 propagation model. The parameters which describes the smooth SNRs, the PWNe and the secondary component are compatible within the errors with respect to the burst-like scenario.
Vela Jr has not been included in this analysis, since we found that in the evolutionary escape model its flux is suppressed, given its young age.
We notice that the fluxes from Vela YZ and Cygnus Loop are now both below the secondary component, which instead is almost unchanged.
This implies a slight increase of the PWNe contribution. We remind that also in this case the $e^+$ contribution is controlled by the AMS-02 $e^+$ flux data.
As illustrated in Fig.~\ref{fig:mw_evol} (right panel), also in this case all the predictions for the dipole anisotropy within $2\sigma$ from the best fit are below the {\it Fermi}-LAT upper bounds.
\replyy{In the multi-wavelength analysis, the Vela YZ and Cygnus Loop SNRs parameters within both the burst-like and evolutionary models are not
 constrained by the anisotropy data.}
With respect to the burst-like scenario in Fig.~\ref{fig:mw}, the predicted dipole anisotropies are decreased by more than a factor of 2 for TeV energies.
}
Remarkably, we find a model which is compatible with all the $e^++e^-$ flux data, the radio data for Vela YZ and Cygnus Loop, and with the anisotropy upper bounds.

\section{\label{sec:conc}Conclusions}
This paper proposes a \reply{new} multi-wavelength and multi-messenger approach aimed at improving the description of the local SNRs which
can contribute significantly to the measured  $e^++e^-$  flux. The latter is now measured with unprecedented statistics over
several decades in energy.

We work here within a framework in which the leptons measured at Earth from GeV up to tens of TeV energies have a composite origin.
Specifically, $e^-$ are injected in the ISM by SNRs, and a symmetric source of  $e^\pm$ is provided by PWNe. Additionally, a low energy, asymmetric contribution of $e^+$ and $+e^-$
arises from the spallations of CRs on the ISM. In the understanding of the $e^-$ flux data, local sources, those located few hundreds parsecs from the Earth, may play a crucial role.
The single, local SNRs that are found to be among the main contributors to the $e^-$ flux at $>10$~TeV are Vela YZ and Cygnus Loop.
For these two sources, we develop a dedicated analysis to the injection spectrum of accelerated $e^-$ in the ISM.

\reply{The injection of $e^-$ by SNRs into the ISM is treated following the burst like approximation, as commonly assumed in the literature.
Moreover, we have implemented an evolutionary escape model for the $e^-$ injection, and for the first time we have investigated its consequences on both the synchrotron emission and on the propagated CRs measuread at the Earth.}

We investigate the {\it compatibility} of these models for the emission and propagation of $e^-$  and $e^+$ in the Galaxy using three physical observables:
\begin{itemize}
\item the {\it radio flux} at all the available frequencies from  Vela YZ and Cygnus Loop SNRs,
\item the {\it $e^++e^-$ flux} from five experiments from the GeV to tens of TeV energy,
\item the {\it  $e^++e^-$ dipole anisotropy} upper limits from 50 GeV to about 1 TeV.
\end{itemize}

\noindent
We find that the {\it radio flux} for these nearby SNRs strongly constraints the total energy and the spectral index of the emitted $e^-$.
\reply{In the case of the evolutionary escape model, we derive constraints on the total energy and spectral index of both trapped and runaway $e^-$.}
\reply{As for the burst-like approximation}, the flux of $e^-$ from Vela YZ and Cygnus Loop as derived from a fit to radio data is slightly below the data on the inclusive flux.
It can skim the HESS data, when all the uncertainties are considered.
In the assumption that all the radio emission is synchrotron radiation from $e^-$, our predictions indicate the highest flux expected from these sources
can shape the high energy tail of the $e^++e^-$ flux data.
\reply{In the case of the evolutionary escape model, the flux of runaway $e^-$ from Vela YZ and Cygnus Loop is slightly lower, }
\replyy{and their contribution to the $e^++e^-$ flux data is subdominant with respect to the other model components.}

\noindent
We perform a radio-blind analysis by fitting only and all the most recent {\it $e^+ + e^-$ flux} data. The data select correlated values for the total energy and spectral index of Vela YZ,
 and to a less extent of Cygnus Loop. The results for Vela YZ are compatible with the radio analysis within errors considered at  $5\sigma$ confidence level.

\noindent
\reply{As a further novelty}, we consider the  upper limits on {\it $e^+ + e^-$ dipole anisotropy } as an \reply{additional} observable, and assess its power in constraining the Vela YZ and Cygnus Loop source properties.
\reply{This operation is performed at the cost of no new free parameters.}
We find that the anisotropy overshoots {\it Fermi}-LAT upper limits on the whole spectrum when the Vela SNR parameters are left free to fit the $e^+ + e^-$ flux data \replyy{within a burst-like scenario}.
For Cygnus Loop the conclusions are weaker, since it shines at higher energies where the {\it Fermi}-LAT  upper bounds are looser.
The results are very similar when all the single sources considered in the analysis (SNRs and PWNe) contribute to the anisotropy, which is
dominated by Vela YZ.
\replyy{For the first time, we show the severe constraints imposed by the most recent data on the  $e^+ + e^-$ anisotropy, what opens the opportunity of
describing the most promising local sources of $e^-$ with {\it charged} lepton CRs.}

 \noindent
 We finally perform a multi-wavelength multi-messenger analysis by fitting
 simultaneously the radio flux on Vela YZ and Cygnus Loop and the $e^+ + e^-$ flux, and checking the outputs against the  $e^+ + e^-$ dipole anisotropy data.
Considering the proper systematic uncertainties on the energy scale of the different data sets, we can fit the $e^+ + e^-$ spectrum on many energy decades using these local SNRs, a smooth distribution of SNRs, PWNe and secondary production.
\replyy{In this case, the Vela YZ and Cygnus Loop SNRs parameters within both the burst-like and evolutionary models are not
 constrained by the anisotropy data. }
Remarkably, we find a model which is compatible with all the $e^++e^-$ flux data, the radio data for Vela YZ and Cygnus Loop, and with the anisotropy upper bounds.

\begin{acknowledgments}
\reply{We warmly thank Y. Ohira for useful discussions.}
SM gratefully acknowledges support by the Academy of Science of Torino through the
{\it Angiola Agostinelli Gili} scholarship and the KIPAC Institute at SLAC for the kind hospitality.
MDM acknowledges support by the NASA {\it Fermi} Guest Investigator Program 2014 through the {\it Fermi} multi-year Large Program N. 81303 (P.I. E.~Charles) and by the NASA {\it Fermi} Guest Investigator Program 2016 through the {\it Fermi} one-year Program N. 91245 (P.I. M.~Di Mauro).
This work is supported by the "Departments of Excellence 2018 -2022"  Grant  awarded  by  the  Italian  Ministry  of  Education, University and Research (MIUR) (L. 232/2016).
\end{acknowledgments}

redpajama_set_name: RedPajamaArXiv


text:
Reckong Peo
Reckong Peo, also spelled Rekong Peo or simply known as Peo by the local inhabitants, is headquarters of Kinnaur district, one of the twelve administrative districts of the Indian state of Himachal Pradesh.
At a height of 2,290 metres (7,513 ft), Reckong Peo is 260 kilometres (162 miles) from Shimla and seven kilometres (4⅓ miles) from Powari. Earlier Kalpa was the headquarters later changed to Reckong Peo, named after group of people who used to own this place in ancient times.
Reckong Peo is also the commercial and administrative centre of the Kinnaur district as biggest market of entire district is located here and all important governmental as well as administrative offices are located at Reckong Peo. Tourists can take buses to visit all the important villages and other places of district from HRTC Bus Stand at Reckongpeo.
Visa in not needed for Indian citizens. Everyone else need a visa.
India (Bharat)
Unfortunately no tours were found.
Reckong Peo, also spelled Rekong Peo or simply known as Peo by the local inhabitants, is headquarters of Kinnaur district, one of the twelve administrative districts of the Indian state of Himachal Pradesh. At a height of 2,290 metres, Reckong Peo is 260 kilometres from Shimla and seven kilometres from Powari.

redpajama_set_name: RedPajamaCommonCrawl


text:
Archive for A Star is born
Why A Star Is Born Is an Inspiring movie
Posted by Matt Welsh
· May 2, 2019
"A Star is Born" is Bradley Cooper's first directorial debut and it is a film that delivers on all fronts. With intense and realistic performances from Cooper and Lady Gaga, as well as expert cinematography and a stellar original soundtrack, it's no wonder this movie was so popular at both the Oscars and on the Billboard Charts.
It's these elements and more that elevate "A Star is Born" over your average, run-of-the-mill remake. It's also a powerful story about addiction, love, death, and finding the inspiration to continue on. At times, the film is almost too difficult to watch because of how unflinchingly these themes are explored. However, it's certainly worth the watch.
In A Star is Born, Bradley Cooper's character, Jackson Maine, is an alcoholic musician on the tail end of his career. We see how Jackson is barely functioning, going from gig to gig with a bottle of whiskey, oftentimes stumbling through conversations and struggling to stand up straight. We see how Jackson's alcoholism affects those around him, with his brother begrudgingly acting as a handler to make sure Jackson doesn't end up killing himself.
From the beginning of the film, the audience can see that Jackson is on a self destructive path. Like many others who have struggled with addiction, Jackson is worrisome to those around him. As is the case so many time, his friends and family are powerless to stop him from drinking. Jackson manages to keep performing, but off stage he barely functions.
The plot revolves around Ally, a young singer and songwriter whom Jackson meets and falls in love with. While she's conflicted about his rampant alcohol abuse, she falls in love with him as well and the two embark on tour together, with Jackson showing Ally the ropes of show business and co-writing songs together.
The love between these two drives the story forward and we see the highs and lows of Jackson's addiction and the way that it affects both of their careers and relationship. It's an authentic portrayal of the disease of addiction and it doesn't pull any punches.
The movie itself is chock full of depth, with heartwarming and emotional scenes along with timeless wisdom. We see two real characters struggle with pitfalls and trappings of success, the real strains that it can put on a relationship, and the reality of struggling with alcoholism and addiction. One of the best quotes of the movie is delivered by Bobby, Jackson's brother in the film played by Sam Elliot.
"Twelve notes and the octave repeats. It's the same story told over and over, forever. All any artist can offer the world is how they see those twelve notes. That's it. He loved how you see them."
It's through this quote that we see how Jackson truly loved Ally for the way she saw the world. These two inspired one another to create beautiful music. Unfortunately, we also see how the pressures of show business and the disease of addiction can ultimately destroy a person. Towards the end of the film we witness this in action.
Minor spoilers ahead, but towards the end of the film, Jackson Maine finally enters rehab and gets clean. During this time, Ally's career really takes off. When the two finally reunite, Jackson expresses regret over his past actions and wishes to be a better husband. They decide that they will tour together in order to boost both their careers and get back to what they both love. However, Ally's manager finds Jackson alone and promises that the two will never tour together ever again. He says that Jackson's image is forever ruined and that he would only tank Ally's career if they got together again.
In despair, Jackson decides to take his own life, fully believing that Ally would be better off without him. At the end of the film, we see Ally preparing to perform a memorial concert in honor of Jackson, and we know that she faces a tough choice. She can either give in to the despair of losing the man she loved, or she can continue on and keep her head held high. In the last scene of the film, we see Ally look definitely into the camera, showing that she has decided to carry on his and her legacy through her music.
Audiences will feel inspired by the message of "A Star Is Born", which teaches us that while despair and addiction can envelop a person's life, no matter how much we love them, we have to take care of ourselves. You cannot cure someone else's alcoholism, you can only continue to love them, help them when possible, and hope they are able to recover. We see that Ally is able to overcome her grief surrounding Jackson's death, and while she may never fully get over it, she is going to continue living and performing.
Cooper should be commended for the way he drew from elements of his own past and to create a film that explores the demons of its main characters. Cooper has mentioned struggles with addiction before and has worked hard to overcome his own demons to achieve fame and success while inspiring others.
Matthew Boyle is the Chief Operating Officer of Landmark Recovery, a chain of drug and alcohol rehab facilities. He has been working in the healthcare space for 7 years with a new emphasis on recovery. Before his ventures into healthcare, Matthew graduated from Duke University in 2011 Summa Cum Laude with a Bachelor of Arts degree. After Duke Matthew went on to work for the Boston Consulting Group before he realized his true passion lies within Recovery. His vision is to save a million lives in 100 years with a unique approach to recovery that creates a supportive environment through trust, treatment, and intervention.
Categories : Addiction, Movies
Tags : A Star is born
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text:
package org.kie.workbench.common.stunner.bpmn.definition;

import javax.validation.Valid;

import org.jboss.errai.common.client.api.annotations.MapsTo;
import org.jboss.errai.common.client.api.annotations.Portable;
import org.jboss.errai.databinding.client.api.Bindable;
import org.kie.workbench.common.forms.adf.definitions.annotations.FieldParam;
import org.kie.workbench.common.forms.adf.definitions.annotations.FormDefinition;
import org.kie.workbench.common.forms.adf.definitions.annotations.FormField;
import org.kie.workbench.common.forms.adf.definitions.settings.FieldPolicy;
import org.kie.workbench.common.stunner.bpmn.definition.property.background.BackgroundSet;
import org.kie.workbench.common.stunner.bpmn.definition.property.dataio.DataIOModel;
import org.kie.workbench.common.stunner.bpmn.definition.property.dataio.DataIOSet;
import org.kie.workbench.common.stunner.bpmn.definition.property.dimensions.RectangleDimensionsSet;
import org.kie.workbench.common.stunner.bpmn.definition.property.font.FontSet;
import org.kie.workbench.common.stunner.bpmn.definition.property.general.Documentation;
import org.kie.workbench.common.stunner.bpmn.definition.property.general.Name;
import org.kie.workbench.common.stunner.bpmn.definition.property.general.TaskGeneralSet;
import org.kie.workbench.common.stunner.bpmn.definition.property.simulation.SimulationSet;
import org.kie.workbench.common.stunner.bpmn.definition.property.task.BusinessRuleTaskExecutionSet;
import org.kie.workbench.common.stunner.bpmn.definition.property.task.TaskType;
import org.kie.workbench.common.stunner.bpmn.definition.property.task.TaskTypes;
import org.kie.workbench.common.stunner.core.definition.annotation.Definition;
import org.kie.workbench.common.stunner.core.definition.annotation.Property;
import org.kie.workbench.common.stunner.core.definition.annotation.morph.Morph;
import org.kie.workbench.common.stunner.core.rule.annotation.CanDock;
import org.kie.workbench.common.stunner.core.util.HashUtil;

import static org.kie.workbench.common.forms.adf.engine.shared.formGeneration.processing.fields.fieldInitializers.nestedForms.SubFormFieldInitializer.COLLAPSIBLE_CONTAINER;
import static org.kie.workbench.common.forms.adf.engine.shared.formGeneration.processing.fields.fieldInitializers.nestedForms.SubFormFieldInitializer.FIELD_CONTAINER_PARAM;

@Portable
@Bindable
@Definition
@CanDock(roles = {"IntermediateEventOnActivityBoundary"})
@Morph(base = BaseTask.class)
@FormDefinition(
        startElement = "general",
        policy = FieldPolicy.ONLY_MARKED,
        defaultFieldSettings = {@FieldParam(name = FIELD_CONTAINER_PARAM, value = COLLAPSIBLE_CONTAINER)}
)
public class BusinessRuleTask extends BaseTask implements DataIOModel {

    public static final String EXECUTION_SET = "executionSet";
    public static final String DATA_IO_SET = "dataIOSet";

    @Property
    @FormField(
            afterElement = "general"
    )
    @Valid
    protected BusinessRuleTaskExecutionSet executionSet;

    @Property
    @FormField(
            afterElement = "executionSet"
    )
    @Valid
    protected DataIOSet dataIOSet;

    public BusinessRuleTask() {
        this(new TaskGeneralSet(new Name("Task"),
                                new Documentation("")),
             new BusinessRuleTaskExecutionSet(),
             new DataIOSet(),
             new BackgroundSet(),
             new FontSet(),
             new RectangleDimensionsSet(),
             new SimulationSet(),
             new TaskType(TaskTypes.BUSINESS_RULE));
    }

    public BusinessRuleTask(final @MapsTo("general") TaskGeneralSet general,
                            final @MapsTo("executionSet") BusinessRuleTaskExecutionSet executionSet,
                            final @MapsTo("dataIOSet") DataIOSet dataIOSet,
                            final @MapsTo("backgroundSet") BackgroundSet backgroundSet,
                            final @MapsTo("fontSet") FontSet fontSet,
                            final @MapsTo("dimensionsSet") RectangleDimensionsSet dimensionsSet,
                            final @MapsTo("simulationSet") SimulationSet simulationSet,
                            final @MapsTo("taskType") TaskType taskType) {
        super(general,
              backgroundSet,
              fontSet,
              dimensionsSet,
              simulationSet,
              taskType);
        this.executionSet = executionSet;
        this.dataIOSet = dataIOSet;
    }

    @Override
    public boolean hasInputVars() {
        return true;
    }

    @Override
    public boolean isSingleInputVar() {
        return false;
    }

    @Override
    public boolean hasOutputVars() {
        return true;
    }

    @Override
    public boolean isSingleOutputVar() {
        return false;
    }

    public BusinessRuleTaskExecutionSet getExecutionSet() {
        return executionSet;
    }

    public DataIOSet getDataIOSet() {
        return dataIOSet;
    }

    public void setExecutionSet(final BusinessRuleTaskExecutionSet executionSet) {
        this.executionSet = executionSet;
    }

    public void setDataIOSet(final DataIOSet dataIOSet) {
        this.dataIOSet = dataIOSet;
    }

    @Override
    public int hashCode() {
        return HashUtil.combineHashCodes(super.hashCode(),
                                         executionSet.hashCode(),
                                         dataIOSet.hashCode());
    }

    @Override
    public boolean equals(Object o) {
        if (o instanceof BusinessRuleTask) {
            BusinessRuleTask other = (BusinessRuleTask) o;
            return super.equals(other) &&
                    executionSet.equals(other.executionSet) &&
                    dataIOSet.equals(other.dataIOSet);
        }
        return false;
    }
}

redpajama_set_name: RedPajamaGithub


The House voted 326 to 90 Tuesday to reverse a controversial $6 billion cut in veterans' benefits included in last year's budget deal.
The House bill would offset the cost of the legislation by extending the budget sequester for mandatory spending cuts by an additional year.
The chamber is almost unanimous in its desire to reverse the cuts, but some Democrats voted against the bill because it would fund the veterans benefits, in part, through further cuts to mandatory domestic spending for social programs they favor.
Democrats on Monday had indicated to Republican leadership that they would not be able to deliver sufficient votes to pass the benefits bill if it was tied to the debt ceiling. The objections to the debt ceiling plan stemmed not from objections to restoring the benefits, but rather from Democrats' concern that they would set a precedent whereby Republicans could tie provisions—even legislation with broad bipartisan support—to a future debt ceiling increase.
In the end, 120 Democrats suppored the veterans measure Tuesday, while 71 voted against it.
The bill now heads to the Senate where it faces an uncertain future. Senate Democrats are arguing that veterans already paid their debt to society and that the legislation to reverse the cost of living adjustment cuts should pass without offsetting the legislation. And Senate Majority Leader Harry Reid, D-Nev., told reporters Tuesday that he would not support the House's sequester extension.
But Senate Republicans are still insisting that legislation to reverse in cuts contains provisions to prevent it from increasing the deficit.
A bill to reverse the vets COLA cuts from Arkansas Democrat Mark Pryor is pending in the Senate. Democrats say they hope to complete that bill this week, but the chamber might adjourn for its President's Day recess as soon as Wednesday because of an expected snow storm.


text:
Home Community 'Well, It's Not Illegal!'
'Well, It's Not Illegal!'
By Stephen M. Kuebler and Jonathan Beever/UCF Forum columnists
How often have you heard someone say: "Well, it's not illegal!"
The statement is frequently used to justify an action that is morally questionable, but not formally prevented by any kind of law or rule. We're hearing it a lot in modern times, particularly in connection with politicians, their dealings in business, campaign finance, election processes and so on.
But it's not just the best defense in Washington, D.C. We also hear it in our workplace, neighborhoods and social groups when someone wants to wriggle free from the discomfort of a bad choice come to light.
Rules and laws exist to protect and promote the function of communities. Yet, here lies one of many perennial chicken-or-egg problems: Which came first, compliance or ethics? We might tend to think that laws originate from moral convictions about what is right and wrong. But there are many interesting examples that challenge the perception that laws extend from morals.
For example, some things are immoral, yet perfectly legal. You can probably come up with many of your own powerful examples, but we'll just offer a few. First, if you don't tip at a restaurant, that's not illegal; but it seems like a crime, especially when the service is good. Another example: Wealthy people and corporations are often hotly criticized for using loopholes, off-shore accounts, and other schemes to avoid tax. Yet businesses rely more heavily on publicly funded resources than individuals to generate wealth, including roads to ship goods and services, energy and communication infrastructure, law enforcement, national defense, and bureaucracies that support state, national and international trade.
So, trying to avoid paying taxes can't be moral, but there are many legal ways to get away with it – so it's legal but immoral. Our own history offers the best and saddest example. Before the Civil War, slavery was legal in the U.S., but certainly not moral.
In the 1970s the federal highway speed limit was dropped to 55 miles per hour, not to save lives, but to decrease national consumption of petroleum. So, speeding then was illegal, but could we regard it now as immoral?
And there are many examples of the reverse, where an action might be illegal, but it's not necessarily immoral. For example, in the 1970s the federal highway speed limit was dropped to 55 miles per hour, not to save lives but to decrease national consumption of petroleum. So, speeding then was illegal, but could we regard it now as immoral?
Some examples depend on cultural framing. Consider Singapore, where it's illegal to sell gum, not because it's immoral but to help promote public cleanliness. And up until very recently, it was illegal for women to drive in Saudi Arabia, in part because it was regarded as religiously immoral. This stands in stark contrast to Western mores, where driving is commonplace, and in the U.S. it's a rite of passage for all 16-year-olds, including women.
So what is the relationship between legality and morality, between compliance and ethics? And what are the implications of giving someone a pass when they do something that is legal but that makes us flinch morally?
We certainly have an expectation that people will act morally and ethically, even when there is no law or legal enforcement to bring consequences. We particularly hope politicians would exceed legal standards and make ethical choices because they are elected leaders who are meant to promote the best interests of all citizens.
Fundamentally, we are all supposed to do what is right, and not just follow the rules, and we even learn that as children. Think about it. Young children often claim: "But you didn't say I couldn't!" We tell our kids that does not make their actions right. So why would we expect anything less of adults, particularly elected leaders?
But more alarming than a politician skirting the rules is the ease with which their supporters often invoke: "Well, it's not illegal." Let's go back to the schoolyard for some useful reminders of what our social standards are. We are alarmed by bullying, and not only are we telling kids not to bully, but we rebuke children who turn a blind eye to bullying. We tell our kids to speak out, defend the weak, etc. Similarly, whistle-blowing is being promoted by many national organizations, universities, and even the federal government.
We want to catch the bad guys and promote justice. But how can that happen if we don't speak up and call out immoral behavior, even when it is legal? Perhaps our willingness to give people a pass when they do bad things, even when they are legal, is undermining the likelihood that people will follow the rules, much less the spirit of the rule.
Stephen M. Kuebler is an associate professor of chemistry and optics in the University of Central Florida's Department of Chemistry and the College of Optics and Photonics. He can be reached at Stephen.Kuebler@ucf.edu.
Jonathan Beever is an assistant professor of ethics and digital culture in the University of Central Florida's Department of Philosophy and the Texts & Technology doctoral program. He can be reached at Jonathan.Beever@ucf.edu.
The UCF Forum is a weekly series of opinion columns presented by UCF Communications & Marketing. A new column is posted each Wednesday at http://today.ucf.edu, republished on The Seminole Source, and then broadcast between 7:50 and 8 a.m. Sunday on WUCF-FM (89.9). The columns are the opinions of the writers, who serve on the UCF Forum panel of faculty members, staffers and students for a year.
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You have been cycling for a while, and you just heard of power meter cycling. You heard it's awesome, but have not made up your mind. Should you buy one? What are the types? How much do they cost?
Put simply, it's a device that measures the power output of a bike. Technically, they are able to do this because they have strain gauges that deflect when force is applied to them. They combine the torque with angular velocity to determine the measure of watts used.
Rear Wheel Hub: This type of setup is the simplest form. Since there are fewer external forces acting on the strain gauges, a lot of engineers think the hub is the best place to accurately measure output.
However, the measurement here would be lesser than what you would get on a pedal or crank power meter. This is because you are measuring what is left post drivetrain loss. The output can also be lower if the drive chain is quite dirty.
Bottom Bracket Systems: This type is quite accurate and requires little maintenance. However, it can be quite difficult to install. This is made more complicated by the different bottom bracket standards. This makes it harder to swap them between different bikes.
Chainring System: These types can be quite accurate. But you should note that they don't measure the left/right leg output. However, they can give reliable estimates. Just like bottom bracket, they are not easy to swap between bikes.
Crank Power Meter: Unlike the last two, you can easily swap this one between bikes. They can also be single or double sided. If you want to get one, you can check out Stages power meters for sale.
Pedal Systems: These kinds are easy to swap between bikes. However, they are not quite accurate because of the complex force measurements. They also face a lot of exposure and can easily get damaged.
This categorisation differentiates devices by the side of the bike they are placed on. They can be placed on the left side, right side, or on both side. Placing them on a particular side of the bike measures the output produced by the leg in that position.
These types are located on one side of the bike, usually the left side of the bike. They measure the output from one leg, and double it to give an estimate. They might not be fully accurate, but are quite affordable.
Before you get a single sided meter, check if you have significant imbalances. The common left/right balance is 48/52 pct.
This type measures the output produced by both sides of the leg. They are more accurate than the single sided devices. However, they cannot give you a measurement of the output produced by a single leg.
These types are more expensive and sophisticate. They are also placed in multiple places like the crank and the pedal. They measure the unit each individual leg produces. With this, you would be able to establish which leg is producing more.
They would also be especially useful if you are recovering from a leg injury. With them, you can measure the improvement in the output your injured leg produces.
The type of meter you use depends on your budget. So, it would be best if you know what you are likely to get with the present sum in your pocket.
With a budget in this range, what you would get are road bike power meters that measure the output from a single leg and estimate them for both legs.
At this range, you are going to come across pedal, crank, and chain ring systems. They would also be dual sided. This is the range for professional athletes.
With this budget, you are going to get combined and dual sided systems. You are also going to encounter crank and spindle systems.
How are Power Meters Useful?
If you are interested in determining how hard you are actually working, then you need to calculate your output. Calculating your speed tells you a little about the ride, while your heart rate tells you a bit more. On the other hand, power outputs give you a quantitative and objective means of calculating your input.
For example, you might have a slower speed during a route, or your heart rate is slower. But if your output data is up, it shows that you are really putting in some work.
They also give you pointers when that it's time to rest. If your heart rate is above a certain rate at a predetermined level, that is a signal that you need to head home.
Another advantage of measuring your output is that it helps to define your weakness. If you notice a reduction in output on a consistent basis, then you need to put in more work.
You also get to train for the specific demands of an event. Some events specify the kinds of outputs that would be required before you participate. When you have trained consistently with a meter, you would be well prepared for whatever the organisers throw at you.
One last thing to keep in mind before you buy one: Make sure you take a fitness test. With this, you can determine what your starting point should be. You also get to be able to set the right goals for your training exercises. You should also have a clear idea of how you plan on using it.


A beautiful period home bursting with character with a wonderful mature garden.
As you walk through the front door you enter a charming vestibule with quarry tiled floor and corniced ceiling. A striking stained glass door opens into the hall which has a period arch and corbels.
The dining room features exposed floorboards, a ceiling rose and sash window which overlooks the garden. The chimney breast has been removed in this room, opening it up and allowing for practical use of the space.
An arch leads through to the bayed sitting room where you will find a period fireplace, ceiling rose and crisp cornicing. The kitchen offers maple wall and floor units and a rear door which leads onto the garden.
The first floor landing features a stripped back banister and spindles and an elegant spiral staircase which leads to the loft. The classic, full width master bedroom can be found at the front of the house with a period fireplace. A second double bedroom also offers a more practical space as the chimney breast has also been removed. At the rear of the landing you will find a bathroom with white suite and a separate WC.
The loft is currently used as an office a work space with exposed floorboards, two rear velux windows and eaves storage beneath and beyond the exposed purlings.
The wintery photos at this time of year do not show the mature garden at its' best which, when in bloom, is a lovely place to sit and relax. A private walled flagstone patio leads to the side return, steps then lead up to the lawn which is bordered with flower beds, shrubs and trees. A timber garden shed and gated access onto a secure residents access lane can be found at the rear.
Corniced ceiling. Quarry tiled floor. Meter cupboard.
Radiator. Corniced ceiling. Staircase. Power points. Period arch.
Sash bay window to front. Radiator. Ceiling Rose. Corniced ceiling. Period fireplace. Wall light, TV and power points.
Sash window to rear. Radiator. Ceiling rose. Corniced ceiling. Wall light, phone and power points.
Double glazed window to side. Part tiling to walls. Single bowl inset sink unit with single drainer. Range of base units, cupboards and drawers. Range of wall units. Plumbed for washing machine. Inset electric hob. Cooker hood. Fitted electric oven. Fitted fridge. Power points. Gas boiler. Tiled floor. Door to Rear Garden.
Radiator. Power points. Spiral staircase to loft.
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Low level WC. Tiled walls. Extractor fan. Tiled floor.
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NATO's role during the Cold War
Posted By: Ryan Boudwin March 28, 2010
"NATO is perhaps the best known and arguably the most successful multilateral military alliance in contemporary world politics" (Pease, 2008, p. 139). NATO is not successful solely by its ability to provide conventional and nuclear deterrence, thereby providing physical security for Western Europe. NATO also united Western Europe, and in conjunction with the Marshall Plan, ensured the economic rebuilding of Europe. These efforts made the later development of the European Union possible.
According to Dr. Kelly Pease, an eminent scholar in international relations, "[NATO] was able to stabilize the European continent after centuries of violent conflict and build a lasting peace between such historical adversaries as France and Germany" (2008, p. 141). NATO provided a forum for both military and political cooperation for the states of Western Europe. While NATO was not entirely free of conflict (as the tension between Greece and Turkey clearly showed) it provided a greater degree of cooperation than had ever been seen before in Europe.
The North Atlantic Treaty Organization was only one part of the American strategy for the rebuilding and security of Europe. The Marshall Plan was the other. Lord Robertson of Port Ellen, secretary-general of NATO, explained that "security and economics are linked. One cannot flourish without the other" (Lord Robertson, 2001). The common strategy of NATO and the Marshall Plan linked the two together so closely that President Truman said that the Marshall Plan and NATO were "two halves of the same walnut" (Lord Robertson, 2001). The Marshall Plan also promoted European unity just as NATO had done. States were only eligible for aid under the Marshall Plan if they accepted international economic cooperation as a specific condition (Pease, 2008, p. 146). President Clinton, speaking at Geneva on the fiftieth anniversary of the Marshall Plan, explained the unity that this economic program brought to Europe:
"The Marshall Plan offered a cure, not a crutch. It was never a handout; it was always a hand up. It said to Europe, if you will put your divisions behind you, if you will work together to help yourselves, then America will work with you. The British Foreign Secretary, Ernest Bevin, called the Marshall Plan 'a lifeline to sinking men, bringing hope where there was none.' From the Arctic Sea to the Mediterranean, European nations grabbed that lifeline, cooperating as never before on a common program of recovery. The task was not easy, but the hope they shared was more powerful than their differences" (Bill Clinton, 1997).
Jamie Shea also pointed out that the security guarantees that NATO provided allowed the European powers to focus on economic development and reconstruction without the heavy burden of high defense spending (Shea, 2003). This shows how tightly integrated the NATO and Marshall Plan strategies were.
The economic rebuilding of Europe did as much to protect the national security of the United States as the military aspect of the alliance itself, because it prevented the contagion of communist revolution from spreading further west in the chaos that followed World War II and thereby prevented the Soviet Union from finding allies in Western Europe. It helped ensure that the American blood that was spent in the liberation of Europe would not be wasted. After World War I, the American people refused to support European recovery and security by rejecting the League of Nations and overseas commitments in general. The result was another bloody war that brought carnage to an unprecedented level. NATO and the Marshall Plan ensured that this terrible mistake would not be repeated. America realized then that forcing Europe to fend for itself following World War II could result in failed states that would be vulnerable to communist influences and provide security risks for the entire world. Even today, many of the security problems around the world revolve around failed states like Somalia, especially the plague of international terrorism.
Clinton, W. J. (1997). The lesson of the Marshall Plan. Vital Speeches of the Day, 63, (18), 546-549. Retrieved from EBSCO index.
Lord Robertson of Port Ellen. (2001). Security and prosperity: Two halves of the same walnut. Retrieved from http://www.nato.int/docu/speech/2001/s010315a.htm.
Pease, K. S. (2008). International organizations: Perspectives on governance in the twenty-first century. (3rd ed.) Upper Saddle River, NJ: Pearson Education, Inc.
Shea, J. (2003). How did NATO survive the Cold War? Retrieved from http://www.nato.int/docu/speech/2003/s031106b.htm.
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WORLD LEARNING SUMMIT (WLS) is an annual, international conference on education´s digital future, with a broad focus on the interdisciplinary understanding of technology´s impact on society -- learning in particular. High level workshops, world class keynotes and well documented publication outlet in our WLS summit proceedings. Attendance usually from about 20 countries. Friendly atmosphere and a high premium on networking. All conferences also contain a series of high-level interactive panels on innvations in technology, entrepreneurship, adaptive learning at the work place, artificial intelligence, blockchain, MOOCs, Open Education Resources, and much more.
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Lander College of Arts & Sciences in Flatbush Hosts Egyptian Ambassador
New York, N.Y. – The Lander College of Arts and Sciences – Flatbush (LAS) recently hosted Ambassador Youssef Zada, Consul General of Egypt in New York. The event was sponsored by the LAS Political Science Club.
Following opening remarks on the topic of "The Arab Spring: Democracy & Change in the Arab World," Zada took questions from the audience for the remainder of the event. He spoke on a wide range of topics related to the Middle East, including such controversial subjects as the volatile situations in Iran and Syria, Egypt's relationship with the United States and Israel as well as the state of Egypt since last year's revolution.
"The army, of course, has made some mistakes as they don't have expertise running things politically," he said. "Their major mistake was confronting the demonstrators in a violent manner."
Zada said that although Iran is "not "Egypt's favorite neighbor," there is no animosity between the two countries. He did, however, criticize Syrian President Bashar al-Assad for his handling of the uprising in his country. Asked where Egypt would be in ten years, Zada admitted he couldn't answer that question properly because "prediction in the Middle East, we've all learned, is impossible." He spoke fondly of the U.S and Israel, saying that that Egyptian relations with the two countries are "as strong as a rock." At the conclusion of his talk, Zada spoke informally with the students, faculty and administration of LAS.
"We are extremely gratified that Ambassador Zada chose to speak to our students at Lander College in Flatbush about these pressing issues," said Professor Alan A. Mond, Deputy Chair of the Political Science Program at LAS. "This was one of a broad range of programs and activities at Lander College that serve to enrich our students' education and enhance their intellectual experience."
Indeed, the students saw the value in hearing a different perspective.
"The school cares about the pursuit of knowledge we are so hungry for, and as long as we can maintain an academic atmosphere, all issues can be bridged," said LAS senior Robert Staroselsky, president of Political Science Club. Staroselsky, who was born in Italy after his parents emigrated from Russia and grew up in Brooklyn, is majoring in political science and economics. "There is much that we, as Jewish students, and he, as an Egyptian official, can do to meet each other half way for the sake of our mutual interests," he said.
Zada is the Chief of Mission for the Consulate General of the Arab Republic of Egypt in New York. He has held a number of prominent posts in the embassies of Egypt in London, Kuwait, Damascus, Algiers, Singapore and Guatemala. Prior to his current post, Zada served as the deputy director of the Institute of Diplomatic Studies in Cairo and as ambassador of Egypt to the Ukraine.
The Lander College of Arts and Sciences in Flatbush, with separate divisions for men and women, is located at Avenue J and East 16th Street in the Midwood section of Brooklyn. More than 1,000 students are enrolled each semester at the campus. Encompassing more than 90,000 square feet, the campus was inaugurated in the spring of 1995. In September 1997, the New York State Education Department officially designated this site as The Flatbush Branch Campus of Touro College.