text:
\section{Introduction}
The mystery of fast radio bursts (FRBs) has garnered
substantial interest from the radio community.
High-energy astrophysicists have tried to model their burst source,
observers would like to measure a large population of them, and cosmologists
hope to use them as a probe of the intergalactic medium (IGM). However their relative scarcity
(only $\sim$ dozen have been observed so far) and their apparent
transient nature mean that we still do not know their position on the sky
to better than a few arcminutes, and their radial position could be anything
from terrestrial to cosmological \citep{2014ApJ...797...70K}.

These objects are
highly dispersed, with dispersion measures (DMs) ($\sim 375$-1600 pc cm$^{-3}$) far exceeding
the expected contribution from our own Galaxy's interstellar medium (ISM) (10-100 pc cm$^{-3}$) and leading to the
interpretation that FRBs are cosmological \citep{2007Sci...318..777L, 2013Sci...341...53T}.
Various emission mechanisms have been proposed
at a wide range of source locations,
including merging white dwarfs \citep{2013ApJ...776L..39K}
and neutron stars \citep{2013PASJ...65L..12T}, supergiant pulses
from extragalactic neutron stars \citep{2015arXiv150100753C},
blitzars \citep{2014A&A...562A.137F},
magnetars \citep{2007arXiv0710.2006P, 2014MNRAS.442L...9L, 2015arXiv150101341P},
and flaring Galactic stars \citep{2014MNRAS.439L..46L}.
Though presently there are more theoretical models for FRBs than actual
sources discovered, constraints on such theories are rapidly emerging.
This is due to recent polarization data,
multifrequency coverage, and their being observed by several telescopes
at various locations on the sky \citep{2014ApJ...780L...2B, 2015MNRAS.447..246P}.

On top of event rates ($\sim$10$^4$ per day per sky)
and high DMs, explanations of FRBs must now
account for temporal scattering, and polarization states.  They should
predict or explain Faraday rotation and time dependence of linear polarization.
The rotation measure (RM) of our Galaxy has been mapped, and the
intergalactic RM is constrained to be less than 7 rad m$^{-2}$
\citep{2015A&A...575A.118O}.
The observed temporal scattering is problematic for a IGM interpretation, due
to the unrealistically small length scales required in the IGM
for $\sim$ms scattering \citep{2014ApJ...785L..26L}.

In this letter we propose a new non-cosmological but extragalactic
solution to the FRB problem: supergiant pulses from newly formed pulsars in
supernova remnants (SNRs). The dense ionized environment of the SNR
can provide 300-2000 pc cm$^{-3}$ of dispersion if the pulses are observed
within $\sim100$ years of the core-collapse supernova. In our picture the
large DM and scattering all come from the same place, and generically
accounts for substantial Faraday Rotation and polarization angle
swings. These features were included to account for recent
polarization measurements of a new FRB (Masui et al. 2015, submitted),
which may exhibit a polarization vector swing and whose RM is $\sim2\times10^2$ rad m$^{-2}$.
These are not expected in a cosmological interpretation of the DM.

\section{Supernova Remants}
Of order 10$^{51}$ ergs of kinetic energy is released during a supernova, a
fraction of which is converted into thermal
energy after shock heating of the
ejecta plasma. Though the shock-heated ejecta atoms
are fully ionized after the explosion, the density is high enough that
ionized atoms can soon recombine.
This phase of low-ionization comes to an end when the remnant expands
into the surrounding ISM, causing a reverse shock wave that reionizes the ejecta.
Though this is the basic narrative, observations \citep{2014ApJ...796...82Z}
as well as simulations \citep{2014ApJ...794..174P}
of SN 1987a have shown the morphological and ionization properties of SNRs
in the decades and centuries after the explosion are nuanced and
difficult to model.
That said, in general the expanding shell left behind
should be able to provide enough free electrons
along the line-of-sight for unusually large dispersion measures. If we
assume a toy model in which a sphere expands at $v_{\rm ej}$,
then the radius R(t) $\approx v_{\rm ej} t$. Therefore the DM we expect can be
calculated as,

\begin{equation}
\textup{DM} \approx  \frac{\textup{x}_e \textup{M}_{\rm ej}}{m_p \frac{4\pi}{3} v_{\rm ej}^2 t^2}
\end{equation}

\noindent where x$_e$ is the ionization fraction,
M$_{\rm ej}$ is the ejecta mass, and $m_p$
is the mass of a proton. Assuming $\sim$10 M$_{\odot}$ of material
is ejected at $v_{\rm ej}\sim 3-8\times10^3$ km/s and an ionization fraction of
$\sim20\% $, the dispersion measure goes from several
thousand pc cm$^{-3}$ immediately
after the reverse-shock ionization, to several hundred pc cm$^{-3}$ after 50-100 years
\cite{2014ApJ...796...82Z}. We point out that while the difference between between
a sphere of HII, which we have assumed, and a thin shell makes a small difference
for DM, it could have a large effect of plasma frequency -- something we discuss
in section \ref{sec-predictions}.
In the context of SNR 1987a, \cite{2014ApJ...796...82Z} found that a possible pulsar
could have DMs between 100-6000 pc cm$^{-3}$, after $\sim 25$ years, though
no compact object has yet been observed in that remnant.

Another potentially important feature of the SNR environment is its magnetic
field.
The exact magnitude of any detection of Faraday rotation has implications for the possible source location. For
instance in the circumnuclear picture, one would expect RMs
$\sim10^{3-5}$ rad m$^{-2}$ \citep{2015arXiv150101341P}, similar to that of the Milky Way's
Galactic center magnetar J1745-29. In the cosmological scenario, if the Faraday
rotation
came from the same place as the DM - namely the intergalactic medium -
then we would only expect a few rad m$^{-2}$ of RM \citep{2015A&A...575A.118O}.

The Faraday effect rotates the polarization vector
by an angle $\phi = $RM$\, \lambda^2$, where

\begin{equation}
\textup{RM} = \frac{e^3}{2\pi m^2 c^4} \int_0^{L} n_e(l) B_\parallel (l) dl.
\end{equation}

We can therefore make a rough estimate of the rotation measure of a remnant
pulsar with dispersion measure DM. Using
\cite{2014ira..book.....B} we get,

\begin{equation}
\textup{RM} \approx 0.81\,\textup{rad}  \, \textup{m}^{-2} \, \times \frac{\left < B_{\parallel} \right >}
{1 \mu \rm G} \cdot \frac{\textup{DM}}{1 \textup{pc}\,\textup{cm}^{-3}} .
\end{equation}

Though there is a large uncertainty in evolution of the magnetic field strength and added
uncertainty in $\langle B_{\parallel} \rangle$ given $B_{\parallel}$ is not necessarily positive,
typical values in our Galaxy are 0.2 - 1$\mu \rm G$. For instance the Crab and Vela have
$ \sim 0.92 \mu \rm G$ and $\sim 0.56 \mu \rm G$, respectively.
This gives RMs between $\sim 80-1200$
rad m$^{-2}$ for a SNR pulsar with FRB-like DMs, which is consistent with Masui et al. (2015,
submitted).

\subsection{Event Rates}
\label{rates}

The daily FRB rate has been estimated at $3.3^{+5.0}_{-2.5}\times10^3$ sky$^{-1}$
\citep{2015arXiv150500834R}. If we start from the local core-collapse supernova
event rate, $\Gamma_{\rm CC}$, and include objects out to some distance $d_{\rm max}$,
we expect the following daily FRB rate,

\begin{equation}
\Gamma_{\rm FRB} \sim  \frac{4}{3} \pi d_{\rm max}^3 \times \Gamma_{\rm CC} \times
 \eta \, \tau_{\rm ion} \gamma_{\rm GP}
\end{equation}

\noindent where $\tau_{\rm ion}$ is the window in years when the SNR is sufficiently
dense and ionized to provide the observed DMs, $\gamma_{\rm GP}$
is the daily rate of giant pulses above $\sim10^{36}$ ergs, and $\eta$
is the number of core-collapse supernovae that leave behind a visible pulsar.
From \cite{2014ApJ...792..135T} we know
$\Gamma_{\rm CC}\sim3 \times 10^{-4}$ day$^{-1}$ ($h^{-1}$Mpc)$^{-3}$,
so if we take $d_{\rm max}$ to be 100 $h^{-1}$Mpc and $\tau_{\rm ion}\sim100$ years,
we require one giant pulse every 10-20 days, assuming one fifth of this SNe population
leaves behind a visible pulsar.
In Fig. \ref{FIG-RATE}
we show the event rate as a function of distance, varying two parameters: the
effective high-DM window and the rate of giant pulses.

\begin{figure}
\label{FIG-RATE}
  \centering
   \includegraphics[width=0.5\textwidth]{FRB_SNR_rate.png}
   \caption{Daily FRB rate per sky based on local core-collapse supernova
   event rate, plotted against distance.
   We assume early in the pulsar's life there is a window, either
   25, 100, or 500 years when the SNR can provide a large enough electron
   column density to explain the high DMs of the observed bursts. We also
   include a rate of giant pulses of either one per day or one per hundred
   days. We have assumed 20$\%$ of core-collapse supernovae leave behind
   a visible pulsar.
   The horizontal black lines are the $99\%$ confidence bounds for the FRB rate
   found by \protect\cite{2015arXiv150500834R}.}
\end{figure}

From Fig. \ref{FIG-RATE} we can see even in our most conservative estimate, when
the SNR only has a 25 year window and emits giant pulses once every
100 days, the volume necessary for the highest daily FRB rate is still non-cosmological.
By this we mean the DM contribution from the IGM is less than $\sim 200$ pc cm$^{-3}$.
If the SNR FRBs are within a hundred $h^{-1}$Mpc then DM$_{\rm IGM}$ is less than
$\sim 10 \%$  of the total dispersion of a typical burst.

If FRBs really are giant pulses then they
should repeat stochastically, and while none of the radio follow-ups for
observed sources has seen an FRB repeat, this could be because they
have not observed for long enough. We point out that FRB 140514,
the first burst observed in real-time, was found during a follow up observation
of FRB 110220 and the two were found within a beam-width of one another.
FRB 140514 had a lower DM than 110220 by 380 cm pc$^{-3}$,
and though \cite{2015MNRAS.447..246P} show that it was not very unlikely that one would find a
new FRB given their integration time, if it were the same source
our model could explain the discrepancy. Indeed, a reanalysis by
\cite{2015arXiv150701002M} found that the two bursts were far more likely
to be the same repeating source than had been previously claimed.
Given FRB 110220 would have been emitted over three years earlier, we
would expect its DM generically to be higher, but the amount would
depend on the inner structure of the SNR and its expansion speed.
We discuss repetition further in section \ref{sec-predictions}.

\subsection{Young SNR Pulsars}

About a dozen pulsars in our Galaxy are known to emit extremely energetic,
short duration radio pulses which can be many orders of magnitude
brighter than the pulsar's regular emission. Some of these objects exhibit
a rare tail of \textit{supergiant} pulses, whose brightness temperatures
exceed the Planck temperature, $\gtrsim10^{32}$ K \citep{2004ApJ...612..375C},
which we will take as a working definition of \textit{supergiant}.
Indeed the largest
known brightness temperature, T$_{b}$, in the universe came from a giant pulse from the Crab,
 with T$_{b}\sim2\times10^{41}$ K \citep{2014ApJ...792..135T}. Though there
are only $\sim100$ hours of published giant pulse data from the Crab, it is known
that the supergiant pulse tail does not obey the standard power-law fall off
in amplitude \citep{2012ApJ...760...64M}.

Given the relatively high frequency of core-collapse supernovae
in the local universe, the young
rapidly rotating pulsars such events leave behind could emit giant
pulses bright enough to be observed at hundreds of megaparsecs.
These supergiant pulses would require $10^{36 - 37}$ ergs of output,
assuming and observed flux density of 0.3-5 Jy and $\sim500$
MHz of bandwidth over 1 ms. Though this is $\sim$ billions of times
brighter than an average pulse, it is negligible compared to a
pulsar's total rotational energy, E$_{\rm rot} \sim 10^{49-50}$ ergs and
even the pulsar's spin-down luminosity. We
also point out that given its relative proximity, this model requires
a couple orders of magnitude less energy than cosmological FRBs,
located beyond a Gpc.

\begin{table*}
\label{TAB-1}
\begin{tabularx}{1.08\textwidth}{@{\extracolsep{\fill}}|lccccccc|}
\hline
\multicolumn{1}{|c}{\textbf{Location}}                                                                                & \textbf{Model}                                              & \textbf{\begin{tabular}[c]{@{}c@{}}Galactic \\ scintillation\end{tabular}} & \textbf{\begin{tabular}[c]{@{}c@{}}Faraday \\ rotation\end{tabular}} & \textbf{$\mathbf{\frac{dlnN_{\rm FRB}}{dlnS_{\nu}}}$}                                      & \multicolumn{1}{l}{\textbf{Counterpart}}                                    & \textbf{\begin{tabular}[c]{@{}c@{}}DM range\\ (pc cm$^{-3}$)\end{tabular}} & \textbf{\begin{tabular}[c]{@{}c@{}}Pol angle \\ swing\end{tabular}} \\ \hline
\multicolumn{1}{|l|}{\multirow{4}{*}{\begin{tabular}[c]{@{}l@{}}Cosmological \\ ($\mathrel{\hbox{\rlap{\hbox{\lower4pt\hbox{$\sim$}}}\hbox{$>$}}} 1 h^{-1}$Gpc)\end{tabular}}}             & Blitzars                                                    & $\times$                                                                         & $\lesssim 7$ rad m$^{-2}$                                               & ?                                                                                & \begin{tabular}[c]{@{}c@{}}gravitational \\ waves\end{tabular}              & 300-2500                                                                & $\times$                                                                  \\
\multicolumn{1}{|l|}{}                                                                                & Merging COs                                                 & $\times$                                                                         & $\lesssim 7$ rad m$^{-2}$                                      & ?                                                                                & \begin{tabular}[c]{@{}c@{}}type Ia SNe,\\  X-ray, $\gamma$-ray\end{tabular} & 300-2500                                                                & $\times$                                                                  \\
\multicolumn{1}{|l|}{}                                                                                & Primordial BHs                                              & $\times$                                                                         & $\lesssim 7$ rad m$^{-2}$                                               & ?                                                                             & $\sim$TeV                                                                   & 300-2500                                                                & $\times$                                                                  \\
\multicolumn{1}{|l|}{}                                                                                & Magnetar flare                                              & $\times$                                                                         & $\lesssim 7$ rad m$^{-2}$                                               & ?                                                                                & \begin{tabular}[c]{@{}c@{}}$\sim$ms TeV \\ burst\end{tabular}               & 300-2500                                                                & $\checkmark$                                                        \\ \cline{1-1}
\multicolumn{1}{|l|}{\multirow{3}{*}{\begin{tabular}[c]{@{}l@{}}Extragalactic, local \\ ($\lesssim$200$ h^{-1}$Mpc)\end{tabular}}} & Edge-on disk                                                & $\checkmark$                                                               & 50-500 rad m$^{-2}$                                                     & -3/2                                                                                & ?                                                                           & 10-2000                                                                 & ?                                                                   \\
\multicolumn{1}{|l|}{}                                                                                & \begin{tabular}[c]{@{}c@{}}Nuclear \\ magnetar\end{tabular} & $\checkmark$                                                               & 10$^{3-5}$ rad m$^{-2}$                                                 & -3/2                                                                                & none                                                                        & 10-3000                                                                 & $\checkmark$                                                        \\
\multicolumn{1}{|l|}{}                                                                                & SNR pulsar                                                  & $\checkmark$                                                               & 20-$10^3$ rad m$^{-2}$                                                  & -3/2                                                                                & \begin{tabular}[c]{@{}c@{}}archival CC \\ SNe or \\ nearby galaxy \end{tabular}                  & 10$^2$-10$^4$                                                           & $\checkmark$                                                        \\ \cline{1-1}
\multicolumn{1}{|l|}{Galactic ($\lesssim 100$ kpc)}                                                                                & flaring MS stars                                            & $\checkmark$                                                               & RM$_{\rm gal}$                                                          & -3/2                                                                                & \begin{tabular}[c]{@{}c@{}}main sequence \\ star\end{tabular}               & $\mathrel{\hbox{\rlap{\hbox{\lower4pt\hbox{$\sim$}}}\hbox{$>$}}}$ 300                                                           & $\times$                                                                  \\ \cline{1-1}
\multicolumn{1}{|l|}{Terrestrial ($\lesssim 10^5$ km)}                                                                             & RFI                                                         & $\times$                                                                         & $\lesssim$ RM$_{\rm ion}$                                                          & $\left\{\begin{matrix}-1/2 \,\, if \,\, 2D \\ -3/2 \,\, if \,\, 3D\end{matrix}\right.$ & none                                                                        & ?                                                                       & $\times$                                                                  \\ \hline

\end{tabularx}
\caption{This table summarizes a number of FRB models by classifying them as cosmological,
extragalactic but non-cosmological, Galactic, and terrestrial.
The seven columns are potential observables of FRBs and each
 row gives their consequence for a given model
 (Blitzars \protect\citep{2014A&A...562A.137F},
 compact object mergers \protect\citep{2012ApJ...760...64M, 2013PASJ...65L..12T},
 exploding primordial blackholes \protect\citep{2014PhRvD..90l7503B},
bursts from magnetars \protect\citep{2014MNRAS.442L...9L},
edge-on disk galaxies \protect\citep{2015arXiv150400200X},
circumnuclear magnetars \protect\citep{2015arXiv150101341P},
 supernova remnant pulsars, stellar flares \protect\citep{2014MNRAS.439L..46L}, and terrestrial RFI
 \protect\citep{2015arXiv150305245H}.). For the latter, we subdivide the RFI into planar RFI (2D) coming
 from the earth's surface, and 3D RFI coming from objects like satellites.
 Since scintillation
only affects unresolved images, cosmological sources that are not scattered near the source
will not scintillate in our Galaxy, while non-cosmological sources whose screens are intrinsic will.
For Faraday rotation and scintillation
 we assume
the RM and SM comes from the same place as the DM, e.g. the IGM for cosmological sources, though such models
could introduce a more local Faraday effect or a scattering screen.
Even though
all models have to explain the observed 375-1600 pc cm$^{-3}$, some models predict a wider
range of DM. For instance, in the circumnuclear magnetar or edge-on disk disk scenarios there
ought to be bursts at relatively low DM that simply have not been identified as FRBs. In our supernova
remnant model DMs should be very large early in the pulsar's life, though this window is short and
therefore such high DM bursts would be rare.}
\end{table*}
2015MNRAS.447..246P

The polarization properties of giant pulses are also consistent with those
of observed FRBs. Giant pulses are known to be highly polarized,
switching between strong Stokes V and purely linearly polarized states often
in an unpredictable way.
The only published FRB prior to Masui et al. (2015, submitted),
with full-pol information was FRB 140514 and was
found to have $\sim20\%$ circular polarization and no detectable
linear polarization \citep{2015MNRAS.447..246P}. If FRBs were coming
from a pulsar-like emission mechanism, one might see nearly pure Stokes V
or linear-pol states. Another consequence of pulsar-like emission
is that FRBs could exhibit polarization angle
swings over the burst duration, which may have been observed
by Masui et al. (2015, submitted).
Unfortunately, to date all other published FRBs
were detected with systems that recorded only Stokes I.

\section{Predictions}
\label{sec-predictions}

In table 1 we summarize the observational consequences
of ours and several other models as best we can. As one might expect,
the most striking differences in predictions has to do with the distance of FRBs,
for example the cosmological FRB models differ mainly in their expected
counterpart and not much else.

The young SNR pulsar model makes several predictions that will
be addressed with more data, particularly with full polarization
observations and large field-of-view surveys.
The latter will provide a large sample of FRBs whose flux and DM statistics
 can give us information about their location. Since in the SNR FRB picture
most of the DM is intrinsic, the sources do not need to be at cosmological
distances. This means the flux distribution is given by a Euclidean universe
that is only weakly dependent on DM, N$(>$S)$ \propto \rm S^{-3/2}$, assuming
the bursts are standard candle-like.
Wide-field surveys
like CHIME \citep{2014SPIE.9145E..22B} (whose FRB backend will
observe steadily for several years),
UTMOST\footnote{http://www.caastro.org/news/2014-utmost},
 or HIRAX could observe as many as $\sim10^{3-4}$
per year, which would allow for detailed population statistics. An instrument like
CHIME will not only give us large numbers of DMs and fluxes, but will also allow
us to measure various polarization properties and frequency scintillation.

Since we have proposed that FRBs come from young pulsars
in SNRs, it is possible that the corresponding
supernova was observed in recent decades in the optical. If the pulsars
were younger than $\sim$60 years old they could be localised at the
$\sim$arcsecond level
and matched against catalogued type II supernovae, though we would need a
large sample of FRBs given the incompleteness of recorded supernovae. With
current data the location of FRBs has been too poorly constrained to say anything
meaningful about overlap with historic SNe or coincident galaxies;
out to $\sim$150 $h^{-1}$Mpc
there are a number of galaxies in a Parkes beam and therefore one would
expect as many supernovae anyway in the last century, even though it would unlikely
have been observed. However better localisation or a cross-correlation between
a large sample of FRBs and nearby galaxies could help support the non-cosmological
extragalactic FRB hypothesis.

We also point out that while FRBs seem not to repeat regularly,
it is not known that they never repeat. Though the statistics
of giant pulses from local pulsars are mostly Poisson \citep{1999ApJ...517..460S},
it is possible that
the supergiant pulses we require from very young SNR pulsars are not. If their
statistics were of a Poisson process then there are already limits on the repeat rate,
given the $\sim100$ hours of follow up, however if their statistics were more like
earthquakes, the brightest pulses could burst intermittently and turn off
for extended periods. It is possible that FRBs could repeat every 5-500 days.
If they were to repeat,
it is possible that their DMs, RMs, and scattering properties could
change noticeably on months/years timescales. Unlike standard pulsars
whose RMs and DMs are constant to a couple decimal places, young
SNR pulsars like the Crab and Vela have shown significant - and sometimes
correlated - variation in such properties \citep{1988A&A...202..166R}.
As discussed in section \ref{rates}, FRB 140514 had a DM that was several hundred
pc cm$^{-3}$ smaller than FRB 110220 and the two were found within a beam-width
of one another. Though this could have just been a spatial coincidence of two
separate objects, our SNR FRB model
could account for such a change in DM while other models (cosmological, edge-on
galaxy, etc.) cannot.

We also predict that such repeated
bursts could have vastly different polarization states, similar to the giant
pulses from pulsars in the Galaxy. Another consequence of polarized
pulsar-like emission would be a polarization angle swing. Given the FRBs
would be rotating, the angle of the linear polarization vector could
change throughout the pulse -- a phenomenon that is seen in many
galactic pulsars, often repeatably \citep{2006ApJ...645.1421B}. Therefore models
that explain FRBs as rapidly rotating compact objects could predict a swing in the
polarization angle throughout the burst.

Depending on the relationship between the giant pulse rate and SNR
age and environment, there may exist a short window in the pulsar's life when
DMs are larger than could be achieved in the IGM at redshifts $z\lesssim2.5$.
Na\"ively we would expect the average pulse
energy to decay with time along with its period.
It would be therefore possible, albeit rare, that an FRB have a DM
 of $\sim10^4$ pc cm$^{-3}$. In general we expect the distribution of DMs
to be peaked somewhere around the observed FRBs (500-800  pc cm$^{-3}$),
but with weight at intermediate
DMs when the ejecta has significantly expanded and at very high DMs. In several
non-cosmological FRB models there should be a number of low-DM FRBs
 \citep{2015arXiv150101341P, 2015arXiv150400200X}, which must be explained
 away with non-identification bias. However in our
picture we do not expect the pulsar to emit supergiant pulses indefinitely and
therefore we do not expect to be able to see these objects when the SNR has
expanded and the DMs would be moderate. In the \cite{2015arXiv150506220K} treatment
of the SNR FRB
it is assumed that the supergiant pulse rate is time-independent, a scenario that the
observed $\frac{dlogN}{dlogDM}$ has already cast doubt on. But since the
DM distribution depends on birth spin rate and the dependence of luminosity
with period, both of which are unknown, we do not attempt to predict it concretely.
The Crab would need to emit giant pulses in excess of several GJy to be
seen at the distances we are proposing - which is several orders of
magnitude brighter than what has been observed -
and we postulate that is because it is too old.

Beyond the varying DM distributions produced by the location, density,
and time dependence of the dispersing electrons, their plasma frequency
can give interesting constraints on the nature of FRBs. Since

\begin{equation}
\omega_p = \sqrt{\frac{n_e e^2}{m_e \epsilon_o}}
\end{equation}

\noindent we expect FRBs dispersed by
the diffuse IGM to have very low plasma frequencies while Galactic models,
e.g. flaring stars, should predict large $\omega_p$. This can be verified
in in precise measurements of the pulse arrival time as a function of frequency.
If $k^2c^2 = \omega^2 - \omega_p^2$, then the $\lambda^2$ arrival time
dependence is only true in the limit where $\omega >> \omega_p$.
Therefore plasma frequency can be used to test FRB models
by looking for deviations in the data. This probe
was also pointed out by \cite{2015arXiv150506220K},
who shows the dispersion index for
$\Delta t \propto \nu^{\alpha}$ differs from -2 by
$\frac{6 \pi n_e e^2}{m_e \omega^2}$.
In the SNR model a $\sim$50 year SNR expanding at
$\sim$ 3,000 km s$^{-1}$
would have a plasma frequency of $\lesssim 10$ MHz and an arrival
delay within $4 \times 10^{-5}$ of -2.0 at 1.4 GHz, which is consistent with
present measurements.

Another interesting path for studying extragalactic radio bursts,
cosmological or otherwise, is scintillation. Only objects of small angular
size scintillate, which is why stars twinkle and planets do not: turbulent cells
in the ionosphere can resolve planets but not stars. The same is true for extragalactic
objects scintillating in the Milky Way, where objects larger than $\sim10^{-7}$
arc seconds do not scintillate at $\sim$GHz.
This is why so few quasars scintillate \citep{2002Natur.415...57D}.

While several explanations for this scintillation exist
\citep{1992RSPTA.341..151N, 2014MNRAS.442.3338P}, we are
concerned with the observational effects and not the physics.
Using \cite{1986isra.book.....T}
we can estimate the angular size of an extragalactic object,

\begin{equation}
\label{eqn-scint}
\theta \approx \left ( \frac{2 c \tau \, (R_{\rm obj} - R_{\rm sn})}{R_{\rm sn}R_{\rm obj}} \right )^{1/2}
\end{equation}
\\

\noindent where $R_{\rm obj}$ is the distance to the source, $R_{\rm sn}$ is the distance
to the screen, and $\tau$ is the scattering timescale. For the case of FRBs we
take $\tau$ to be $\sim10$ ms. In the cosmological case, if the ms scattering
were from an extended galactic disk along the line of sight  (see \citet{2014ApJ...780L..33M})
halfway between
us and the source, then the angular broadening
of an object at 2 Gpc is $\sim150$ microarcseconds. If the screen were within
1 kpc of the same object then the broadening is $\sim80$ nanoarcseconds.
Therefore scintillation from our own Galaxy should only occur for cosmological
FRBs whose millisecond scattering is close to the source. For an SNR FRB the
screen would have to be within a few hundred parsecs of the object, which we
generically expect. We include this feature in table 1 where each
column is estimated based on the medium that is causing the high dispersion measure,
e.g. the IGM for cosmological models.

\section{Conclusions}
Evidence is emerging suggesting FRBs are not only extraterrestrial
but extragalactic. Though the simplest interpretation of their high DMs
is a cosmological one, we find this model less compelling in the light of
past scattering measurements and potential Faraday rotation
and pol-angle swing in a new FRB
(Masui et al. 2015, submitted). In this letter we offer a
more nearby solution.
We have gone through
a model in which FRBs are really supergiant pulses from
extragalactic supernova remnant pulsars, within a couple hundred megaparsecs.
The SNR environment is sufficiently
dense and ionized to provide DMs $\mathrel{\hbox{\rlap{\hbox{\lower4pt\hbox{$\sim$}}}\hbox{$>$}}} 500$pc cm$^{-3}$ as well as
RMs $\mathrel{\hbox{\rlap{\hbox{\lower4pt\hbox{$\sim$}}}\hbox{$>$}}} 50$ rad m$^{-2}$, only the first of which could be replicated by the IGM.

The environment could also provide $\sim$ms scattering at 1 GHz, as has been
observed in Galactic SNR pulsars.
That makes this picture self-contained in the sense that
the young remnant environment can account for the dispersion
and scattering measure seen in FRBs.  It predicts a higher Faraday
rotation than the IGM, but not as high as galactic centers. The
repetition rate is related to the distance, and could be from days to
years.
By extrapolating Crab-like giant pulses back to the pulsar's first century or so,
we have proposed that such objects can emit extremely energetic bursts sporadically.
If these are similar to giant pulses from Galactic pulsars, they could be highly polarized,
either linearly or circularly, and if they were to repeat their polarization state may
change drastically. Given the object's rotating nature, polarization
 angles would be likely to swing during the pulse. The distinct polarization properties
have been seen in at least one burst and may be end up being generic properties
of FRBs (Masui et al. 2015, submitted).
\\

\section{Acknowledgements}

We thank NSERC for support. We also thank Bryan Gaensler, Niels Oppermann,
Giovanna Zanardo, and Chris Matzner for helpful discussions.

\newcommand{\araa}{ARA\&A}
\newcommand{\afz}{Afz}
\newcommand{\aj}{AJ}
\newcommand{\azh}{AZh}
\newcommand{\aaa}{A\&A}
\newcommand{\aas}{A\&AS}
\newcommand{\aar}{A\&AR}
\newcommand{\apj}{ApJ}
\newcommand{\apjs}{ApJS}
\newcommand{\apjl}{ApJ}
\newcommand{\apss}{Ap\&SS}
\newcommand{\baas}{BAAS}
\newcommand{\jaa}{JA\&A}
\newcommand{\mnras}{MNRAS}
\newcommand{\nat}{Nat}
\newcommand{\pasj}{PASJ}
\newcommand{\pasp}{PASP}
\newcommand{\paspc}{PASPC}
\newcommand{\qjras}{QJRAS}
\newcommand{\sci}{Sci}
\newcommand{\solphys}{Solar Physics}
\newcommand{\sova}{SvA}
\newcommand{A\&A}{A\&A}
\newcommand\jcap{{J. Cosmology Astropart. Phys.}}%
\newcommand{Phys. Rev. D}{Phys. Rev. D}


Get Vendio Gallery - Now FREE! Autograph 1933 Admiral Richard Byrd PSA/DNA Check Signed Dated June 13 DS 22 VTG. ADMIRAL RICHARD BYRD SIGNED BANK CHECK JUNE 13TH, 1933 FAMOUS AMERICAN AVIATOR & EXPLORER EXTREMELY RARE PSA/DNA CERTIFIED & ENCAPSULATED = VINTAGE AUTHENTIC ORIGINAL!! Byrd CANCELLED CHECK: Farmers & Merchants National Bank & Trust Co. PAY TO THE ORDER: Jordare Marsh Co.
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_gsrx_vers_632 GS 6.9.8 (632). The item "Autograph 1933 Admiral Richard Byrd PSA/DNA Check Signed Dated June 13 DS 22 VTG" is in sale since Sunday, November 6, 2016. This item is in the category "Collectibles\Autographs\Historical". The seller is "thejackpot" and is located in Los Angeles. This item can be shipped worldwide.


text:
Q: react-native run-android throws cannot find certificate I am on mac for work, this is a react native project on visual studio code. I only get this error when I npx react-native run-android from vs code or terminal. I tried to go to the gradle website to download gradle. I tried to add a debug keystore to my project. Here is the full errors
EDIT:
Have fixed all errors in React native doctor command, fixed all issues there.
Exception in thread "main" javax.net.ssl.SSLHandshakeException: PKIX path building failed: sun.security.provider.certpath.SunCertPathBuilderException: unable to find valid certification path to requested target
at java.base/sun.security.ssl.Alert.createSSLException(Alert.java:130)
at java.base/sun.security.ssl.TransportContext.fatal(TransportContext.java:371)
at java.base/sun.security.ssl.TransportContext.fatal(TransportContext.java:314)
at java.base/sun.security.ssl.TransportContext.fatal(TransportContext.java:309)
at java.base/sun.security.ssl.CertificateMessage$T13CertificateConsumer.checkServerCerts(CertificateMessage.java:1351)
at java.base/sun.security.ssl.CertificateMessage$T13CertificateConsumer.onConsumeCertificate(CertificateMessage.java:1226)
at java.base/sun.security.ssl.CertificateMessage$T13CertificateConsumer.consume(CertificateMessage.java:1169)
at java.base/sun.security.ssl.SSLHandshake.consume(SSLHandshake.java:396)
at java.base/sun.security.ssl.HandshakeContext.dispatch(HandshakeContext.java:480)
at java.base/sun.security.ssl.HandshakeContext.dispatch(HandshakeContext.java:458)
at java.base/sun.security.ssl.TransportContext.dispatch(TransportContext.java:201)
at java.base/sun.security.ssl.SSLTransport.decode(SSLTransport.java:172)
at java.base/sun.security.ssl.SSLSocketImpl.decode(SSLSocketImpl.java:1510)
at java.base/sun.security.ssl.SSLSocketImpl.readHandshakeRecord(SSLSocketImpl.java:1425)
at java.base/sun.security.ssl.SSLSocketImpl.startHandshake(SSLSocketImpl.java:455)
at java.base/sun.security.ssl.SSLSocketImpl.startHandshake(SSLSocketImpl.java:426)
at java.base/sun.net.www.protocol.https.HttpsClient.afterConnect(HttpsClient.java:578)
at java.base/sun.net.www.protocol.https.AbstractDelegateHttpsURLConnection.connect(AbstractDelegateHttpsURLConnection.java:187)
at java.base/sun.net.www.protocol.http.HttpURLConnection.getInputStream0(HttpURLConnection.java:1661)
at java.base/sun.net.www.protocol.http.HttpURLConnection.getInputStream(HttpURLConnection.java:1585)
at java.base/sun.net.www.protocol.https.HttpsURLConnectionImpl.getInputStream(HttpsURLConnectionImpl.java:224)
at org.gradle.wrapper.Download.downloadInternal(Download.java:100)
at org.gradle.wrapper.Download.download(Download.java:80)
at org.gradle.wrapper.Install$1.call(Install.java:82)
at org.gradle.wrapper.Install$1.call(Install.java:62)
at org.gradle.wrapper.ExclusiveFileAccessManager.access(ExclusiveFileAccessManager.java:69)
at org.gradle.wrapper.Install.createDist(Install.java:62)
at org.gradle.wrapper.WrapperExecutor.execute(WrapperExecutor.java:107)
at org.gradle.wrapper.GradleWrapperMain.main(GradleWrapperMain.java:63)

Caused by: sun.security.validator.ValidatorException: PKIX path building failed: sun.security.provider.certpath.SunCertPathBuilderException: unable to find valid certification path to requested target
at java.base/sun.security.validator.PKIXValidator.doBuild(PKIXValidator.java:388)
at java.base/sun.security.validator.PKIXValidator.engineValidate(PKIXValidator.java:271)
at java.base/sun.security.validator.Validator.validate(Validator.java:256)
at java.base/sun.security.ssl.X509TrustManagerImpl.checkTrusted(X509TrustManagerImpl.java:231)
at java.base/sun.security.ssl.X509TrustManagerImpl.checkServerTrusted(X509TrustManagerImpl.java:132)
at java.base/sun.security.ssl.CertificateMessage$T13CertificateConsumer.checkServerCerts(CertificateMessage.java:1335)
... 24 more
Caused by: sun.security.provider.certpath.SunCertPathBuilderException: unable to find valid certification path to requested target
at java.base/sun.security.provider.certpath.SunCertPathBuilder.build(SunCertPathBuilder.java:141)
at java.base/sun.security.provider.certpath.SunCertPathBuilder.engineBuild(SunCertPathBuilder.java:126)
at java.base/java.security.cert.CertPathBuilder.build(CertPathBuilder.java:297)
at java.base/sun.security.validator.PKIXValidator.doBuild(PKIXValidator.java:383)
... 29 more

error Failed to install the app. Make sure you have the Android development environment set up: https://reactnative.dev/docs/environment-setup.
Error: Command failed: ./gradlew app:installQadebug -PreactNativeDevServerPort=8081
Exception in thread "main" javax.net.ssl.SSLHandshakeException: PKIX path building failed: sun.security.provider.certpath.SunCertPathBuilderException: unable to find valid certification path to requested target
at java.base/sun.security.ssl.Alert.createSSLException(Alert.java:130)
at java.base/sun.security.ssl.TransportContext.fatal(TransportContext.java:371)
at java.base/sun.security.ssl.TransportContext.fatal(TransportContext.java:314)
at java.base/sun.security.ssl.TransportContext.fatal(TransportContext.java:309)
at java.base/sun.security.ssl.CertificateMessage$T13CertificateConsumer.checkServerCerts(CertificateMessage.java:1351)
at java.base/sun.security.ssl.CertificateMessage$T13CertificateConsumer.onConsumeCertificate(CertificateMessage.java:1226)
at java.base/sun.security.ssl.CertificateMessage$T13CertificateConsumer.consume(CertificateMessage.java:1169)
at java.base/sun.security.ssl.SSLHandshake.consume(SSLHandshake.java:396)
at java.base/sun.security.ssl.HandshakeContext.dispatch(HandshakeContext.java:480)
at java.base/sun.security.ssl.HandshakeContext.dispatch(HandshakeContext.java:458)
at java.base/sun.security.ssl.TransportContext.dispatch(TransportContext.java:201)
at java.base/sun.security.ssl.SSLTransport.decode(SSLTransport.java:172)
at java.base/sun.security.ssl.SSLSocketImpl.decode(SSLSocketImpl.java:1510)
at java.base/sun.security.ssl.SSLSocketImpl.readHandshakeRecord(SSLSocketImpl.java:1425)
at java.base/sun.security.ssl.SSLSocketImpl.startHandshake(SSLSocketImpl.java:455)
at java.base/sun.security.ssl.SSLSocketImpl.startHandshake(SSLSocketImpl.java:426)
at java.base/sun.net.www.protocol.https.HttpsClient.afterConnect(HttpsClient.java:578)
at java.base/sun.net.www.protocol.https.AbstractDelegateHttpsURLConnection.connect(AbstractDelegateHttpsURLConnection.java:187)
at java.base/sun.net.www.protocol.http.HttpURLConnection.getInputStream0(HttpURLConnection.java:1661)
at java.base/sun.net.www.protocol.http.HttpURLConnection.getInputStream(HttpURLConnection.java:1585)
at java.base/sun.net.www.protocol.https.HttpsURLConnectionImpl.getInputStream(HttpsURLConnectionImpl.java:224)
at org.gradle.wrapper.Download.downloadInternal(Download.java:100)
at org.gradle.wrapper.Download.download(Download.java:80)
at org.gradle.wrapper.Install$1.call(Install.java:82)
at org.gradle.wrapper.Install$1.call(Install.java:62)
at org.gradle.wrapper.ExclusiveFileAccessManager.access(ExclusiveFileAccessManager.java:69)
at org.gradle.wrapper.Install.createDist(Install.java:62)
at org.gradle.wrapper.WrapperExecutor.execute(WrapperExecutor.java:107)
at org.gradle.wrapper.GradleWrapperMain.main(GradleWrapperMain.java:63)
Caused by: sun.security.validator.ValidatorException: PKIX path building failed: sun.security.provider.certpath.SunCertPathBuilderException: unable to find valid certification path to requested target
at java.base/sun.security.validator.PKIXValidator.doBuild(PKIXValidator.java:388)
at java.base/sun.security.validator.PKIXValidator.engineValidate(PKIXValidator.java:271)
at java.base/sun.security.validator.Validator.validate(Validator.java:256)
at java.base/sun.security.ssl.X509TrustManagerImpl.checkTrusted(X509TrustManagerImpl.java:231)
at java.base/sun.security.ssl.X509TrustManagerImpl.checkServerTrusted(X509TrustManagerImpl.java:132)
at java.base/sun.security.ssl.CertificateMessage$T13CertificateConsumer.checkServerCerts(CertificateMessage.java:1335)
... 24 more
Caused by: sun.security.provider.certpath.SunCertPathBuilderException: unable to find valid certification path to requested target
at java.base/sun.security.provider.certpath.SunCertPathBuilder.build(SunCertPathBuilder.java:141)
at java.base/sun.security.provider.certpath.SunCertPathBuilder.engineBuild(SunCertPathBuilder.java:126)
at java.base/java.security.cert.CertPathBuilder.build(CertPathBuilder.java:297)
at java.base/sun.security.validator.PKIXValidator.doBuild(PKIXValidator.java:383)
... 29 more

at makeError (/Users/JWimer/StudioProjects/cw-mobile-react-native-git/node_modules/@react-native-community/cli-platform-android/node_modules/execa/index.js:174:9)
at /Users/JWimer/StudioProjects/cw-mobile-react-native-git/node_modules/@react-native-community/cli-platform-android/node_modules/execa/index.js:278:16
at process.processTicksAndRejections (node:internal/process/task_queues:95:5)
at async runOnAllDevices (/Users/JWimer/StudioProjects/cw-mobile-react-native-git/node_modules/@react-native-community/cli-platform-android/build/commands/runAndroid/runOnAllDevices.js:109:5)
at async Command.handleAction (/Users/JWimer/StudioProjects/cw-mobile-react-native-git/node_modules/@react-native-community/cli/build/index.js:142:9)

redpajama_set_name: RedPajamaStackExchange


Every family celebrates Easter differently. Whether it's filled with chocolate, celebrating in church or with family – or all of the above – it's a great holiday and personally one of my favourites. However, since being zero waste, my perspective on the holiday has changed slightly.
People produce so much rubbish over Easter that they need to know when it will all be collected. First of all I was angry, but then I quickly realised that anger never solved anything so then I got thinking.
What if we could all do our bit this Easter?
Although these companies are not waste-free, by opting for foil-wrapped eggs you're reducing your carbon footprint.
I personally don't have Easter eggs anymore because I just can't stand to see the waste I often don't have time to find an egg with minimal packaging. I still get chocolate regularly from Dark Sugars on Brick Lane in my drawstring fabric bag.
I know it's tempting to just go out and buy an egg from the supermarket, but they're FULL of horrible plastic packaging. If you can be slightly more prepared and find a chocolatier, or source an egg with less packaging, please do. It's important not to fuel the consumption of plastics so that producers start to take the hint and change how they manufacture the products that we buy.
Sainsbury's is the only supermarket that I currently know of that will recycle your Easter egg rubbish for you. Make sure you read the labels on the packing before you throw them in the wrong recycling bin.
The best way to recycle Easter egg foil is to scrunch the foil up into a fist-sized ball before placing it in the recycling bin. This makes sure the small bits of foil don't get lost in the recycling process.
If it's got chocolate on it, rinse it off first.
The cardboard boxes that package the eggs, along with any other boxes, can be placed in your recycle bin for recycling. Collapsing the boxes first helps leave room in your bin for more recycling.
There's one question to ask when it comes to recycling plastic – 'does it hold its shape?'. The golden rule is, if it holds its shape when crumpled then it can be placed in the recycling bin.
That means plastic bags are a no-no, as are other soft plastics like bread bags and hot cross bun bags.
I hope this helps, and from Charlotte and I, have a very happy Easter!!


Scheduling a look at your convenience, in less than an hour one of experts will make the design beautiful, the setting ready, and the delivery a breeze.
Help you select the perfect spot for your tub.
Recommend top contractors, landscape designers and electricians to match your wishes, needs and budget.
Make sure everything has absolutely accurate measurements.
Recommend best placement for ideal access and your view or landscape.


text:
Shabaab targets Somali police chief in Mogadishu suicide bombing
By Caleb Weiss & Andrew Tobin | April 24, 2022 | [email protected] |
On the evening of April 22, Shabaab, al Qaeda's branch in East Africa, struck a popular restaurant in Lido Beach in Mogadishu in an attempt to assassinate the chief of the Somali Police Force, Abdi Hassan Mohamed Hijaar. The police commander was accompanied by 11 members of the Somali Parliament at the time of the attack.
Local reporters describe the assault as "complex" as the terrorist organization conducted a suicide bombing of the crowded restaurant, then followed the explosion with a strike by gunmen. Hijaar, along with several other Somali government officials, were breaking their Ramadan fast at the restaurant at the time of the attack.
Shabaab frequently employs the tactic of suicide operations, especially upon popular hotels in Mogadishu, using the shock and chaos created by the suicide bombing to enable its gunmen to then enter the fray.
According to local sources, Hijaar and other Somali government officials were unharmed in the assault, indicating that Shabaab failed to accomplish its objective. However, at least six people, all civilians, were killed in the attack. Local officials stated at least another seven people were also injured.
Shabaab was quick to claim the suicide bombing via its Shahada News Agency and local radio stations. According to the jihadist group, it was specifically targeting "the grouping of apostate government officials" at the restaurant.
According to data compiled by FDD's Long War Journal, Friday's blast marks the group's 12th successful or attempted suicide bombing so far this year. The vast majority of these have occurred inside Mogodishu.
Shabaab further stated it "killed and wounded 44 people," including an alleged government official, though the group routinely inflates the casualty numbers of its attacks. Local media has also denied that any government personnel were injured.
Shabaab often uses suicide bombings in its political assassinations. For instance, the group killed Somali lawmaker Amina Mohamed Abdi in a suicide bombing in central Somalia last month. Last year, it also attempted to assassinate the governor of Somalia's Bay region in a similar blast. While in 2020, two regional governors, of Puntland's Nugaal and Mudug regions, were killed by Shabaab's suicide bombers.
Targeting Somalia's Election Process
Friday's suicide assault once again demonstrates that Mogadishu is not safe from insurgent attacks. Shabaab continues to attempt to undermine the federal government by illustrating its inability to protect its population and secure its territory. In this regard, Friday's suicide bombing was just the latest in a recent series of attacks.
On Monday, Shabaab claimed credit for a mortar assault on the Somali parliament building in Mogadishu. Though no one was killed in the strike, at least six were injured. The offensive occurred while the newly elected parliamentarians were approving procedures for electing the speakers.
The mortar blasts, like the consecutive attacks at the end of March, represent yet another Shabaab attempt to undermine the Somali election process. Friday's suicide assault can also be seen within the context of Shabaab's attempts at disrupting the process.
As the election process continues, with various delays, Shabaab will continue to muster its forces to disrupt the elections across the country. Government officials, including local politicians, are likely to continue to be targets of Shabaab's violence.
Despite some setbacks in recent years, Shabaab continues to be one of al Qaeda's most effective branches. It maintains significant control over much of southern Somalia and retains the ability to strike in Mogadishu, Kenya, where it also controls territory, and against heavily fortified bases in both Somalia and Kenya.
Though its fortunes have ebbed and flowed over the past decade, it has weathered numerous offensives from an array of local, regional, and international actors, including the United States.
Tags: Al Qaeda East Africa, Lido Beach, Mogadishu, Shabaab, Somalia

redpajama_set_name: RedPajamaCommonCrawl


text:
Q: Append array to JSON column to multiple rows at once I have a column type JSON in database, and I'm performing an update on multiple rows.
For example, this query
Model::whereIn('id',$ids)->update([
   'status' => 'canceled'
]);

And this table has another column called history (JSON type), each row already has its own history in JSON.
How do I append to each one of them? This array, for example
[
   'user_id' => '144',
   'action'  => 'cancel',
   'at'      => '2021 - 08 - 30'
]

My idea and question, is there something like
Model::whereIn( 'id', $ids )->appendJson('field_name',$array);

A: The easiest approach could be like this:
$status = 'canceled';
$extraHistoryData = [...];

Model::whereKey($ids)->get(function ($model) use ($status, $extraHistoryData) {
    $history = $model->history;

    $history = array_merge($history, $extraHistoryData);

    $model->update(compact('status', 'history'));
});

If you want to update all rows in a single query, the closest I can get is this thread. But It's not very likely to solve your problem.


Today's tech bubble: Sell or IPO your company?
Are LinkedIn's bankers greedy or stupid… or making a market?
Insider trading – why is everyone shocked?
Interview with my counsel (and friend) Larry Sonsini on the globalization of Silicon Valley. Courtesy of The Deal. Larry Sonsini on the globalization of Silicon Valley from TheDeal TV on Vimeo.


text:
Estolomimus apicale är en skalbaggsart som beskrevs av Martins och Maria Helena M. Galileo 1997. Estolomimus apicale ingår i släktet Estolomimus och familjen långhorningar. Inga underarter finns listade i Catalogue of Life.

Källor

Externa länkar

Långhorningar
apicale

redpajama_set_name: RedPajamaWikipedia


text:
'I'm walking here': City of Toronto to revamp hundreds of 'No Exit' signs that mislead walkers
April 9, 2021 By Michael Smee, CBC News
The city is getting ready to revamp hundreds of street signs that walking advocates say are misleading.
"No Exit" signs, erected as warnings for drivers, often do not apply to pedestrians, according to Coun. Paula Fletcher, whose motion titled "I'm Walking Here" was approved at this week's council meeting.
"I think during COVID people have been walking like they've never walked before," said Fletcher, who represents Ward 14, Toronto-Danforth.
"So let's just update things for the city we are, which is a walking city, a cycling city and, as you can see, a driving city."
Her motion called on the city to identify those "No Exit" streets that in fact are pedestrian thoroughfares, and change the signage to something more accurate, like "No Exit Pedestrians Excepted," Fletcher said.
The idea came after Walk Toronto compiled a crowd-sourced map that has so far identified about 450 such dead end streets and cul-de-sacs that fail to point out pedestrians can exit.
Dylan Reid, a founder of Walk Toronto, said he wanted to find a way to publicly identify pedestrian exits on dead end streets and brought the idea to Walk Toronto co-founder Sean Marshall, a map maker.
"We asked people for examples and they poured in." he said. "I asked Sean if he was up for doing it and he was totally keen."
The interactive map on the group's website identifies the locations of streets with pedestrian exits. It also points out which ones are paved walkways, which are rough trails, and which can also be used by cyclists.
"Many of these locations are neighbourhood 'secrets' known only to residents who walk there every day, but hidden to anyone who is not as intimately familiar to the area," Fletcher's motion reads.
"Finding a simple solution will make our City more pedestrian friendly, accessible, and welcoming."
The city has identified "thousands" of "No Exit" streets.
"City staff expect to replace signs at approximately 400 locations where pedestrians exits have been identified," a city spokesperson said in an email.
"That work is expected to start at the end of April."
https://www.cbc.ca/news/canada/toronto/i-m-walking-here-city-of-toronto-to-revamp-hundreds-of-no-exit-signs-that-mislead-walkers-1.5980138


text:
//! \file eggs/variant/bad_variant_access.hpp
// Eggs.Variant
//
// Copyright Agustin K-ballo Berge, Fusion Fenix 2014-2016
//
// Distributed under the Boost Software License, Version 1.0. (See accompanying
// file LICENSE_1_0.txt or copy at http://www.boost.org/LICENSE_1_0.txt)

#ifndef EGGS_VARIANT_BAD_VARIANT_ACCESS_HPP
#define EGGS_VARIANT_BAD_VARIANT_ACCESS_HPP

#include <exception>

#include <eggs/variant/detail/config/prefix.hpp>

namespace eggs { namespace variants
{
    ///////////////////////////////////////////////////////////////////////////
    //! class bad_variant_access : public std::exception
    //!
    //! Objects of type `bad_variant_access` are thrown to report attempts to
    //! access an inactive member of a `variant` object.
    class bad_variant_access
      : public std::exception
    {
    public:
        //! bad_variant_access() noexcept;
        //!
        //! \effects Constructs a `bad_variant_access` object.
        bad_variant_access() EGGS_CXX11_NOEXCEPT
        {}

        //! char const* what() const noexcept override;
        //!
        //! \returns An implementation-defined NTBS.
        char const* what() const EGGS_CXX11_NOEXCEPT /*override*/
        {
            return "bad_variant_access";
        }
    };

    namespace detail
    {
        ///////////////////////////////////////////////////////////////////////
        template <typename T>
        EGGS_CXX11_NORETURN inline T throw_bad_variant_access()
        {
#if EGGS_CXX98_HAS_EXCEPTIONS
            throw bad_variant_access{};
#else
            std::terminate();
#endif
        }
    }
}}

#include <eggs/variant/detail/config/suffix.hpp>

#endif /*EGGS_VARIANT_BAD_VARIANT_ACCESS_HPP*/

redpajama_set_name: RedPajamaGithub


text:
Korénnaya Balka  es un posiólok del raión de Beloréchensk del krai de Krasnodar, en Rusia. Se sitúa en la confluencia de los arroyos Vtoraya y Beriózovaya, afluentes del río Psheja, tributario del Bélaya, de la cuenca hidrográfica del Kubán, 21 km al suroeste de Beloréchensk y 81 km al sureste de Krasnodar, la capital del krai. Tenía 7 habitantes en 2011.

Pertenece al municipio Pshejskoye.

Enlaces externos y referencias

Este artículo contiene datos geográficos extraídos de Google Earth y el mapa de Rusia de Yandex.ru, accesible desde este enlace.
Este artículo es una traducción de su correspondiente en la edición en ruso de Wikipedia, Коренная Балка.
Mapa topográfico en maps.vlasenko.net .

Localidades del raión de Beloréchensk del krai de Krasnodar


A place of amazing, uninhabited islands surrounded by the crystal clear Adriatic Sea. Ideal both for adventures and sightseeing, whether you are on a romantic holiday, with friends or family. Perfect for relaxing and enjoying a rich nightlife and vast history.
Sitting at the crossroads of central and southern Europe, Croatia is a land of distinctive red-roofed houses, medieval walled towns and vibrant ports that look out onto the crystalline turquoise waters of the Adriatic. It might still be relatively undiscovered, but we think you'll soon agree that Croatia is one of the Mediterranean's most captivating countries.
Let us take you on a luxury tour to the Adriatic's fascinating Eastern coast.
Get to know the cultural hub of inland Zagreb.
Try out coastal Zadar's clever and beautiful interactive city art.
Explore seaside Split, a town built inside a Roman emperor's monumental palace.
People watch at the glamorous and green Hvar Island.
Discover the Renaissance houses and ancient walls of UNESCO World Heritage Dubrovnik.
Take a few days at the charming fishing town of Rovinj.
Enjoy the immaculate forests of Korcula, the birthplace of Marco Polo.
Take a day trips to the incredible Plitvice National Park with its otherworldly green and blue lakes and cascading waterfalls, and adventure to pristine, uninhabited islands and islets.
Whatever your interests, we can take you to Croatia in comfort and style.
Your luxury trip to Croatia can include as much or as little as you like. We'll help you to explore this welcoming and varied country, assisted by our enthusiastic local guides. We can plan every step of your trip so you can enjoy the tremendous adventure of Croatia knowing that Jacada Travel is taking care of all the details.
Let Jacada Travel help you to discover this diverse region with a seamless and luxury, personalised itinerary. Browse the example plans below for ideas or take a look at our locations page for inspiration, and then speak to our Croatia Travel Designers to start planning your own tailor-made trip.
Whatever you want from your Europe tour, our team of expert travel designers are ready to help.
Based on 955 reviews. See some of the reviews here.
Our vacation in Croatia and Montenegro was awesome. The hotels selected were first rate. All of the tours arranged through Jacada were excellent. The drivers arrived promptly. We were able to truly relax while on vacation as every detail was covered.
Well planned itinerary by Jobi. We enjoyed our Croatian trip very much. The excursions were very interesting and well organised. Our local guides were all very knowledgeable and our skipper/crew during boat transfers were very polite and offered their best service.
My husband and I could say without any reservations that this was the best vacation we've taken so far. Our travel designer, Hanna, and our concierge, Michele, were absolutely lovely and were careful to listen to our preferences. Everything we could think of was taken care of so that we could travel worry-free. The local tour guides and drivers were fantastic, and the itinerary was amazing - we saw and did things we would never have found on our own. Thanks very much, Jacada!
I have traveled extensively for leisure and business and have always put together my own trips. For our honeymoon, we decided to give a bespoke experience a shot. I thought it was overkill, but was curious to try. We chose to go to Slovenia and Croatia. I have to say, the experience was so wonderful, to the detail, from the knowledgeable yet friendly guides, drivers, the efficiency of the private transfers, the private tours, the kind of activities that may work for you, activities that you may not know exist, when you put all those details together, the experience is at another level. I don't know if I will remember the places I visited 10 years from now, but I will definitely remember how I felt during my honeymoon. Needless to say, we will be contacting Jacada again.
Croatia is beautiful year-round but is best visited either side of the hottest summer months. With such a long stretch of coastline, you'll want to take advantage of the warm weather, and visiting in early or late summer can mean fewer crowds.
Your Consent (required) I am happy to receive emails from Jacada Travel including the latest travel guides, tips and information.


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Leo celebrates his tenth birthday. From one grandmother, he receives socks, from the other, underwear. From his Grandfather, Leo gets an old Super-8 camera and with it he tells us of his attempts to change the gifts. While doing that, he finds out that Monica Lewinsky is Jewish, that Clinton is the president of America, that the numbers in his grandparents arms are responsible for him being chubby and that this old camera is worthless.
Director: Michael Wahrmann
Actors: Lucélia Maquiavelli, Oswaldo Ávila, Oswaldo D'ávila, Rodrigo Pastoriza, Sidney Szaja Barmak, Sidney Szaja Bramak
Keywords:123movies 9movies Avós Online Free gomovies gostream losmovie movie4k movietv primewire putlockers putlockertv seehd seehd.info shockshare sitename solarmovie Watch Avós watch32 yesmovie
Nick Thune: Folk Hero
With help from his guitars, comedian Nick Thune regales the audience of Brooklyn's Bell Theatre with a collection of hilarious stories about his childhood, his past romantic relationships and his…
Rising to the Bait
Protected from the intrigues of con-men by the overwhelming blanket of the former regime in East Germany, at first it seems that Ada Fenske, the elderly widow living on a…
A man who is being driven crazy by the noise in New York City decides to take vigilante action against it.
Stressati
Axel heads for the land of sunshine and palm trees to find out who shot police Captain Andrew Bogomil. Thanks to a couple of old friends, Axel's investigation uncovers a…
The Stagg Do
Best man Pob's secret plan for a surprise stag do at a plush countryside brothel is thrown into jeopardy when the bride-to-be insists that they take her overbearing right wing…
Ross Noble: Live at Regent's Park
Comedian Ross Noble performs a stand-up routine, recorded in Regent's Park Open Air Theatre.
While attending a party at James Franco's house, Seth Rogen, Jay Baruchel and many other celebrities are faced with the apocalypse.
Watching the Detectives
Neil, a self proclaimed film geek and owner of Gumshoe video, has always been content to live vicariously through his favorite films noir. But when he meets Violet, a real-life…
It Grows!
As Zac's relationship with his long suffering girlfriend deteriorates, a mysterious 'plant' is discovered in his back yard.
The Circus Revue 2015
In Dog's Words
São Paulo, 2007. Santana works as a dogcatcher, picking up stray animals. He is a friendly guy, averse to trouble, who has always kept violence away from the doorsteps of…
Copyright 2020Movies © 2021. All rights reserved.


Moss may very well be the Rodney Dangerfield of the green plant world. They get no respect. On this particular day all the attention was going to wildflowers with only a passing glance at the soft, vibrant carpets of moss. We do not eat moss, mosses have few medicinal properties, mosses are rarely used in landscaping, and they are usually trampled underfoot without a thought. In fact when I googled MOSS the only commercial link that popped up screamed STOP UNWANTED MOSS GROWTH!
But moss has played a major role in the evolution of plant life on land. We owe much to these overlooked plants. They are descendents of aquatic green algae that were able to grow on land, albeit damp land. From this tenuous foothold the rest of the land plants evolved – ferns, pines and true flowering plants. Moss colonies may cover 20% of the Earths surface and are very important in many ecosystems from the harsh world of the arctic to the lush tropics. They are pioneer plants often growing on rock or bare earth and contribute to soil formation, they absorb water and nutrients, they provide habitat for other plants and small animals and they are bio-indicators of pollution.
Mosses have stems and leaves but no true roots. They are totally dependent upon moisture for reproduction and survival, but they can survive long periods without water too. The only time I ever use the word "happy" in association with plants is looking at moss that has finally gotten rain after a long dry spell.
Ron it turns out is an avid amateur moss sleuth and even has one named for him. He knows it is a grand and diverse world out there. Try to give those subtle green mosses more than a passing glance on your way to the next wildflower.
This is Michael Ellis with a Perspective.
Many years ago I was complaining to a friend that I never could see that so-called man in the moon. He pointed out to me that it wasn't really a man, it was a rabbit holding a basketball and since that moment I have been unable to see anything else. And indeed most cultures don't see a face, they see figures — rabbits mainly, but also toads, mice, cats, lions, bears, and foxes. On Saturday the moon is full, this one is called the Rose moon also known as the Honeymoon. The latter name according to the Dictionary because "The first month of marriage being thought of as the sweetest." There is a second full moon in June, a rare event which we know as a blue moon. In July we'll have the Thunder moon. And of course everyone knows the Harvest Moon, the one nearest to the fall equinox which gives additional light to those laboring in the fields.
Unfortunately in our modern age we tend to ignore the waxing and waning of the moon and think that it doesn't really affect us. But really don't you think it is kind of weird that we pay our PG and E bill according the cycle of the moon, on a "moonthly schedule." The oceans rise and fall corresponding to the relative position of the earth, sun and moon. Even solid land bulges in response to the gravitational force from the moon. Human female menstrual (derived from the Greek for monthly) rhythms were perhaps once set by the periodical cycle of the full moon. Some people claim that more babies are born and more crimes are committed during a full moon (sorry but statistics do not support this). But we still strongly believe that human behavior is influenced by moonlight so we have werewolves and lunatics. And until a brief moment ago when Mr. Edison brought us the electric light, it was mostly moonshine that lit up what little nocturnal activities humans had.
The moon appears to be full to us for about 2 1/2 days. But I recently watched the movie, Moonstruck, I noticed that there seemed to be a full moon for an entire week! Hollywood has never let facts get in the way of entertainment.
Check out that rabbit, it is a silhouette with the long ears swept back to the right and the rabbit facing left. You really can't miss it, though the basketball may be a bit indistinct.
Twenty years ago this month I invited nine men to meet with me. I needed some male support. I was a new dad and completely overwhelmed by that responsibility. I also worked mostly at home by myself and was feeling very isolated. They were enthusiastic. And so for the last two decades we have been meeting once a month.
A whole lot happens through the years. One guy soon dropped out; it was way too intimate for him. One fellow moved away. And though many men have asked to join, we have only added Harrison to our group in all these years. We are exclusive. Not one of us lives in the same house and five of us have gotten divorced. Besides divorce we have dealt collectively with marriages, births of kids and grandchildren, loss of parents, failed businesses, career changes, lawsuits, affairs, prostate cancer, Alzheimer's, autism, and depression. Bill nearly died of a heart attack. But the most painful for us was the loss of not one, but two newborn babies by our dear friend Mike.
We have cried as hard as we have laughed. All through these things we have been holding each other. We have created a safe place to be vulnerable and honest. None of us are New Age male wimps; the testosterone drips from the wall when we meet. We tolerate little BS from one another and everyone speaks their mind.
When I mention my men's group it invariably elicits a sarcastic comment about drumming. Well I confess we have drummed several times. But what we do not do is play poker, smoke cigars, drink beer and complain about women. We are perplexed, intrigued, amused, and totally committed to understanding the women in our lives. Mothers, daughters, wives and girlfriends are a continual topic of conversation. But we have also dedicated meetings to politics, children, money, and poetry. For us nothing is taboo. Thanks guys, I look forward to another twenty years of honesty and friendship.
The Druids, the priestly class of the ancient Celts, divided the year into 8 parts. They had the usual solar divisions – the two equinoxes and the two solstices – but they also had what are called cross quarter days. That is, halfway between the solstices and equinoxes. For us June 21 is the beginning of summer but think about it. On the first of summer the days are getting shorter what kind of summer is that? To the Druids June 21st was the middle of summer. On this day they burned the bones from all the animals that had died the previous year. This bone fire is the origin of our bonfire.
From the summer solstice halfway to the fall equinox was the cross quarter day called Lamas. This word means loaf of bread. The first grain harvested was made into a celebratory loaf on the first of August. This day marked the end of summer and the beginning of fall.
The fall equinox was the midpoint of autumn and the next cross quarter day was Samwain. We know this today as Halloween and this was the biggest day of the Druid year – New Years Eve. So November 1 was the beginning of winter and the beginning of the next year. At the winter solstice was mid winter – now celebrated as Christmas. The next cross quarter day was Candlemas. This was the beginning of the Druid spring and recognized by us in the quaint custom of Groundhog Day. But to the ancients it was the promise of milk flowing in ewes and the sap rising in trees.
Next is the vernal equinox or mid spring and finally we get to the last cross quarter day in the yearly cycle – May Day. This day was devoted to the essential nature of male and female. The union of the sexes insured fertility of crops, animals and humans and many lascivious activities occurred then. I am always amused by the vision of innocent children gaily dancing around the maypole. I am sure their parents would not appreciate being told that they are celebrating the phallus and its union with Mother Earth.
The near shore and intertidal region of the California coast is one of the richest in the world, probably exceeded only by coral reefs. California's "ocean economy" –activities that derive at least some value from the sea – contributes $43 billion annually, more than the state's agricultural sector. Recognizing this the State enacted the California Marine Life Protection Act in 1999 to protect and enhance our ocean environment. Last fall the Fish and Game Commission established the first section of the statewide network of marine protected areas between Santa Barbara and Half Moon Bay. The next area under consideration is goes from Half Moon Bay to Pt. Arena.
There are three different proposals under consideration on how to implement this important act. All share some important similarities but two of them provide crucial habitat protection.
Among the many highlights common to these proposals are protection for iconic places such as Pt Arena, the Farallon Islands, and Pt Reyes, but it is also important to protect the nearshore habitats such as Duxbury Reef in Marin and Saunders Reef in Mendocino County. These two biologically diverse areas especially need protection due to years of heavy fishing – their rockfish populations deserve a chance to recover to their former abundance. If they are not included, California's rich ocean heritage is not adequately protected.
A Blue Ribbon Task force meets in April to recommend one of the three proposals to the State Fish and Game Commission. They should choose the strongest possible option for the marine environment of Northern California.
More than one hundred years ago, our country had the foresight to develop a national park system. Some call it the best idea America ever had. Today, in California, we take places like Yosemite and Kings Canyon for granted and no one thinks they're too big. But there are Yosemite's and other treasures just off our shores in the marine environment. And now it is our turn to match the vision and wisdom of our forebearers and create a new legacy for our children and grandchildren.
With a Perspective, I'm Michael Ellis.


text:
Q: How do I invoke an apexclass from flow and return a list back to flow I have a flow from which I want to call an apexclass and retrieve a list of picklistvalues so a user can select from these in a flowscreen. How do I achieve this. I tried the code below but when I use the apex action type in the flow I do not get the variable "lstCancelOptions"
Apex
public class getCancelOptionsCurrentUser {
    @InvocableMethod(label = 'Get cancel options current user' description = 'Get amendment Cancel reasons')
    public static List<String> getCancelOptionsMsPicklist() {
    String CancelOptions;
    List<String> lstCancelOptions = new List<String>();
        Id CurrUser = UserInfo.getUserId();
        try {
            CancelOptions = [SELECT Id, Reasons_Cancel__c from User where Id = :UserInfo.getUserId()].get(0).Reasons_Cancel__c;
        } Catch(Exception e) {
            System.debug('Error Canceloptions current user: ' + e.getMessage());
        }
        if (String.isNotBlank(CancelOptions)) lstCancelOptions = CancelOptions.split(';');
        return lstCancelOptions;
    }
}

A: The Flow mechanism is bulkified. This means if you return a List<String>, it will map to a single variable, while List<List<String>> will map to a collection variable. You'll need to adjust your code to use List<List<String>> in order for this to work.

A: Alternatively, a wrapper class can be maintained for flow variables. The variables can be marked with the annotation @InvocableVariable. Multiple variables can be returned from the method and also passed as params to the method. All invocable variables are available for selection in the flow.
@InvocableMethod(label = 'Get cancel options current user' description = 'Get amendment Cancel reasons')
public static List<FlowOutput> getCancelOptionsMsPicklist(){
    List<FlowOutput> flowOutput = new List<FlowOutput>();
    FlowOutput output = new FlowOutput();
    String cancelOptions;
    List<String> lstCancelOptions = new List<String>();
    Id CurrUser = UserInfo.getUserId();
    try{
        cancelOptions = [SELECT Id, Reasons_Cancel__c from User where Id = :UserInfo.getUserId()].get(0).Reasons_Cancel__c;
    } catch(Exception e) {
        System.debug('Error Canceloptions current user: ' + e.getMessage());
    }
  if (String.isNotBlank(cancelOptions)) lstCancelOptions = cancelOptions.split(';');
    output.listOfCancelOptions = lstCancelOptions;
    flowOutput.add(output);
    return flowOutput;
}
public class FlowOutput{
    @InvocableVariable()
    public List<String> listOfCancelOptions;
}

A: One key point is that when you added the Apex to the flow it will create a variable in the flow for the return. if the name on the label is lstCancelOptions there will be a variable named lstCancelOptions.


text:
'use strict';

angular
  .module('facebookLogout')
  .directive('facebookLogout', facebookLogout);

//------------------------------------------------------------

function facebookLogout() {
  var directive = {
    link: link,
    restrict: 'A',
    scope: {},
    controller: facebookLogoutController,
    controllerAs: 'vm'
  };

  return directive;

  //------------------------------

  function link(scope, el, attrs, vm) {
    'ngInject';
  }
}

function facebookLogoutController($scope, $element, $attrs, $facebook) {
  'ngInject';

  // hide by default
  hide();

  // add click handler
  $element.bind('click', onClick);

  // show if logged in
  $facebook
    .getLoginStatus()
    .then(function(response) {
      if (response.status === 'connected') show();
    });

  // show on login
  $scope.$on('fb.auth.login', show);

  // hide on logout
  $scope.$on('fb.auth.logout', hide);

  function onClick() {
    if (isDisabled()) return console.log('facebook-logout disabled!');
    disable();

    $facebook
      .logout()
      .then(onLogoutOk, onLogoutError)
      .finally(() => enable());

    //------------------------------

    function onLogoutOk(response) {
      console.log('onLogoutOk:', response);
    }

    function onLogoutError(response) {
      console.log('onLogoutError:', response);
    }
  }

  function enable() {
    $element.attr('disabled', false);
  }

  function disable() {
    $element.attr('disabled', true);
  }

  function isDisabled() {
    return $element.attr('disabled');
  }

  function show() {
    $element.show();
  }

  function hide() {
    $element.hide();
  }
}


text:
Home›Movies›REVIEW — "Hardcore Henry"
REVIEW — "Hardcore Henry"
Travis Dale 2016-04-08
Travis Dale • April 8, 2016 •	0
A super-violent, bare-knuckle, in-your-face, first-person action film, Hardcore Henry will hit you like a shot of adrenaline to the dick!
Shot from the point of view of Henry; a super soldier brought back from the dead with robotic enhancements, Hardcore Henry is structured similar to a campaign from Call of Duty – the popular first-person video game that inspired it. Our hero wakes up and is quickly briefed by his wife (Haley Bennett) on his situation before they are attacked and she is kidnapped.
Henry must then put together the pieces of his mission while being relentlessly pursued by soldiers led by Akan (Danila Kozlovsky) – the film's underdeveloped but physically memorable albino main villain with presumed blindness and unexplained Jedi powers. Yep, it's that kind of movie. Fortunately, the film makes up for its lack of story and coherent plot with brutal, non-stop, entertaining action.
Serving as Henry's mission guide is Jerry (Sharlto Copley), an informed ally that respawns as different characters (punk, hobo, WWI major) throughout the film. Copley turns in a tour-de-force performance that not only serves as the film's comedic backbone, but also centers the story by providing much needed camaraderie to our hero. It's the richest and most versatile performance the eccentric South African actor has given since his debut in District 9.
"A grenade a day keeps the enemy at bay." Director Ilya Naishuller with Sharlto Copley.
With the innovative use of twin, head-mounted GoPro cameras, writer and director Ilya Naishuller puts the audience in the driver's seat of the film's well-choreographed action scenes.
Each fight introduces a new weapon (sniper rifle, samurai sword, broken bottle), a new form of combat (hand-to-hand, martial arts), and a new means of transportation (motorcycle, helicopter, tank, horse!). It's an all-you-can-eat smörgåsbord of machismo fantasy. You want a hero that can parkour jump into a titty bar full of ninjas? You got it, mister!
Although little more than a series of action set pieces that lead to more action set pieces, Hardcore Henry is a mindless, fun ride from its disturbingly graphic, slow-motion opening credits all the way to its violent, Queen-soundtracked, bloody end. 3.5/5
Hardcore Henry, rated R, is in theaters now.
Be sure to hit one of the SHARE buttons at the top/bottom of this page!
Tags:Call of DutyDanila KozlovskyDistrict 9GoProHaley BennettHardcore HenryIlya NaishullermovieMovie Reviewmovie reviewsreviewreviewsSharlto Copley
REVIEW — "The Boss"
REVIEW — "Disney's The Jungle Book"
Travis Dale
REVIEW — "The Art of Racing in the Rain"
/ August 7, 2019 / 0
REVIEW — "The Best of Enemies"
/ April 5, 2019 / 0
REVIEW — "Shazam!"
/ March 23, 2019 / 0
REVIEW — "Scooby-Doo & Scrappy-Doo:" The Complete Season 1 DVD
/ April 29, 2015 / 1


After a weekend with no boxing to enjoy, we have a few crackers to get stuck into this week.
Anthony Crolla attempts to topple pound-for-pound standout Vasyl Lomachenko on Friday night at the Staples Center in LA. Can the former lightweight world champion produce a performance of a lifetime and cement his name in folklore alongside the likes of Lloyd Honeyghan?
On Saturday we turn our attention to the biggest women's world title fight of all time. Can double Olympic gold medallist Claressa Shields become undisputed middleweight world champion, or will Christina Hammer have too much power?
As well as all this we bring you the latest on the WBSS.
Next articleEPISODE 288: The Good, the Bad and the Ugly!


text:
import { IBasketItem } from './basketItem.model';

export interface IBasket {
    items: IBasketItem[];
    buyerId: string;
}


text:
Mid-face toddler excoriation syndrome (MiTES): a new paediatric diagnosis
Author(s): Srinivas S.M.; Gowda V.K.; Owen C.M.; Moss C.; Hiremagalore R.
Source: Clinical and Experimental Dermatology; Jan 2017; vol. 42 (no. 1); p. 68-71
Publication Date: Jan 2017
Publication Type(s): Journal: Article
Available in full text at Clinical and Experimental Dermatology - from John Wiley and Sons
Abstract:Chronic ulcerating lesions on the face are rarely seen in toddlers. Blistering disease, vasculitis, infections and self-mutilation due to neurometabolic disease can usually be excluded on clinical and histological grounds. In the absence of identifiable disease, such lesions are sometimes attributed to child abuse or fabricated illness. We describe three toddlers with chronic mid-face erosions, two from India and one from the UK. One had moderate developmental delay and one had had seizures. The lesions appeared to be self-inflicted, no underlying disease was identified and there was no suspicion of child abuse. Recognition of the same disease pattern in different continents implies a distinct pathological entity. The pattern closely resembles that seen in some patients with mutations in the pain-insensitivity genes PRDM12 and SCN11A. We suggest the term 'mid-face toddler excoriation syndrome' (MiTES) to acknowledge the existence of this condition, encourage further reports and help clarify the pathogenesis. Copyright © 2016 British Association of Dermatologists


text:
Idaho Marital Settlement Agreement (Minor Children)
About this Form: This is a marital settlement agreement that may accompany the No-Fault Divorce form for use within the State of Idaho. This agreement is intended to help the parties formalize an allocation of their property and finances and matters relating to child custody and visitation. Most courts will require a marital settlement agreement filed in conjunction with a COMPLAINT FOR DIVORCE within the State of Idaho.
WHEREAS, we mutually intend this agreement to be a final disposition regarding the marital issues addressed herein and intend that this agreement be incorporated into any subsequent DECREE OF DIVORCE.
C. All payments of child support pursuant to this agreement shall be made and delivered in the following manner: [choose one:] _______ All payments of child support shall be paid directly through the appropriate state agency, official, or court designated by the laws of the State of Idaho to receive and disburse such child support payments, or _______ All payments of child support shall be made directly to the parent to whom the child support payments are due; however, the parent to whom payments are due reserves the right to require, upon written notice to the paying parent, such child support payments to be paid directly to the appropriate state agency, official, or court designated by the laws of the State of Idaho to receive and disburse such child support payments.
Husband and Wife agree that upon the court's ordering a DECREE OF DIVORCE, Wife shall have the right to retain her married name or shall also have the right to return to her maiden or former name: _________________________________ [insert Wife's maiden name].
Husband and Wife agree that this agreement shall be governed and construed in accordance with the laws of the State of Idaho.
Notary Public for the State of Idaho
Idaho Petition for Change of Name of Minor with Final Order and Instructions (Complete Package)
Idaho Petition for Change of Name of Adult with Final Order and Instructions (Complete Package)
Idaho Decree of Divorce - No-Fault, Minor Children
Idaho Divorce Complaint (No-Fault, Minor Children) with Stipulation for Entry of Decree and Child Custody Forms


text:
Attraction Bonuses Will Not Overcome Talent Gaps
By Brian Salkowski December 21, 2021 December 20, 2021
The acute talent gaps that businesses are presently facing have been well-documented in recent months. For instance, the Business Conditions Survey by the National Association of Business Economics found that 47% of respondents reported a shortage of skilled workers in the third quarter of this year. That's up from 32% in the second quarter of 2021, which was already too high for comfort.
Meanwhile, research from a recent New York Times article says that, on average, job openings have increased by 35% — while job applications have decreased by 20% over the past year.
Beyond these headline numbers, talent gaps are having a tangible impact on both our everyday lives and the wider economy: Skills shortages across the U.S. are affecting everything from the opening hours of local 7-Elevens to our country's national security.
The reasons behind this evident lack of candidates are, unsurprisingly, complex. Goldman Sachs has previously attributed ongoing talent shortages to enhanced unemployment benefits, which at one point provided up to $600 a week to jobless workers (on top of normal benefits). However, other economists dispute this. Regardless, it is worth noting that these extra benefits expired in about half of states earlier this summer and in remaining states in early September. Yet gaps persist.
The Problem With Sign-On Bonuses
The reality is that insufficient talent pipelines, shifting skills demand, and a steep retirement cliff have all helped to contribute to the current situation. And as employers struggle to navigate this landscape, many are turning to sign-on bonuses to attract candidates. For example, the likes of HCA Healthcare, Compass Group, XPO Logistics, Quest Diagnostics, and Ryder System have all reportedly been leaning heavily on sign-on bonuses. And they're not alone.
However, desperate employers must resist the urge to "buy their way out" of the ongoing skills crisis, and should instead focus on long-term talent strategies that attract the right people. While financial incentives may appear to be a quick fix for filling vacancies, employment relationships that begin through such schemes may not offer lasting value to the business.
In addition to the extra costs incurred at the point of hire, incentives such as these are unlikely to attract candidates who are the right fit for your business. At the most basic level, individuals attracted by a one-off cash incentive may leave for another employer offering a similar perk as soon as they are contractually able to.
More importantly, though, job-seekers sourced in this way are unlikely to have objectively considered if the company they are joining meets their needs as an employee, shares their values, or is a place where they can grow and thrive professionally.
Remuneration will always be a deciding factor for candidates looking for their next role. But the reality is that candidates value an attractive compensation package built around a competitive base salary over one-off perks. Indeed, job-seekers consider a whole range of other factors when choosing which opportunities to pursue, including learning and development and mentorship programs, progression opportunities, hybrid or remote working opportunities and general flexibility,; fast and effective onboarding, and paid time-off benefits.
To secure scarce skills, decision-makers would be wise to direct time and resources into building a robust long-term talent attraction strategy rather than trying to buy their way out of their predicament. Instead of simply throwing money at the problem, businesses must work to build their reputation as an employer of choice.
EVP vs Comp
Given the current situation we find ourselves in, organizations must ensure that their employer brand is in the best position possible to compete for top resources. Building and communicating a strong employer value proposition (EVP) is key.
Even during times when talent is plentiful, the benefits of investing in your EVP are obvious. According to research by Gartner, organizations that effectively deliver on their EVP can reduce the compensation premium by 50%, and reach 50% deeper into the labor market when candidates view an EVP as attractive. What's more, half of candidates say they wouldn't work for a company with a bad reputation — even when there's a pay increase.
So, a focus on EVP, harnessed alongside complementary recruitment strategies — such as offering a first-class candidate experience and tapping into underutilized talent pools — is vital to persuading people to join you over the competition. All of which is to say that while offering joining bonuses may seem like a smart way to snatch talent from the grasp of a competitor, this strategy is unsustainable.
Brian Salkowski
Brian Salkowski is chief operating officer at Guidant Global. Dedicated to changing the dynamic of MSP services, Brian has more than 20 years' experience in workforce management. Under his leadership, Bartech's Managed Solutions business experienced significant top- and bottom-line growth, as well as important expansions in service line and geography. Brian was also instrumental in the 2018 Bartech and Guidant Group merger, and now leads Guidant Global's Centre of Excellence for Managed Services.
BonusesCompensation & BenefitsHiring ProcessOffersTalent ShortageWages, Pay, & Salary


Moon tattoos are the most common and most popular tattoos among men and women as the moon is the symbol of heaven and it also represent the feelings of the nature of the individual.
Moon tattoos are becoming a regular item seen on body art, have always played a role in imagery. Moon tattoo designs are very popular as they can compliment other tattoos very well. ns are popular as they can compliment other tattoos very well. You can choose to have your moon tattoo in any area on your body and they are often nicer smaller rather than huge.
There are many different moon tattoo designs that you can choose from and they can be as vivid or they can be designed according to the wearer's choice.
Moon tattoos have been used since long as the moon has different meanings in different cultures as the moon is an important symbol in many religious and societies. Moon tattoo is the perfect choice for a couple to have as you could have a moon tattoo and your partner may have the sun tattoo.
If you are not that talented then you can describe your ideas to a tattoo artist and they will recreate your ideas. All tattoos can mean different things to different people and what you see in your designs may be very personal to you. Although your design should look nice it doesn't have to be the prettiest tattoo. It is far more important that it has meaning to you and that you like it.


Disclosure: All practitioners and therapists practicing Lash Lift and/or Semi Permanent Mascara are responsible for following local and state laws and regulations. If you are not a certified, please click here for more information.
After careful consideration, we have decided that the time has come to say goodbye to Elleebana. We are grateful for the experience and all of the amazing individuals we have met, and thank everyone who has supported us along the way.
In its place, we are excited to introduce a new lash lift product line, The Ultimate Lash Lift and Semi Permanent Mascara. Our goal is to provide quality Lash Lift and Semi Permanent Mascara products at a more affordable price. Our new Lash Lift kits contain 40-80 applications (compared to Elleebana's 30 application kit), and our new convenient packaging will produce less product waste. What does this mean for you? Bigger profit margins, better value, amazing quality products and more affordable pricing!