text:
\section{Introduction}

The nature of dark matter remains one of the greatest unknowns in particle physics. Although there is plenty of data that corroborates the existence of dark matter, its nature, mass, and interactions with the standard model are widely unknown~\cite{Tanabashi:2018oca}.
One possibility is when the mass of the dark matter (DM) is much below the electronvolt scale. For these masses, the dark matter De Broglie wavelength becomes macroscopic and could even compare to the size of solar systems and galaxies. This requires the ultralight dark matter to be heavier than $10^{-22}$~eV. Due to Fermi-Dirac statistics, phase space considerations today can be used to better constrain the mass of fermionic dark matter to be above 100 eV to the keV scale (also known as the Tremaine-Gunn bound)~\cite{Tremaine:1979we, Madsen:1990pe, Madsen:1991mz, Boyarsky:2008ju}.

Ultralight bosonic fields are common and can arise as pseudo-Nambu Goldstones from the spontaneous symmetry breaking of an approximate global symmetry such as the QCD axion~\cite{Peccei:1977np, Peccei:1977hh, Weinberg:1977ma, Wilczek:1977pj}. In addition to being ubiquitous, they could also provide dynamical solutions to finetuning problems. For example, the QCD axion makes the QCD theta angle $\theta_{QCD}$ dynamical and relaxes it to zero~\cite{Vafa:1984xg}. These fields can also constitute ultralight dark matter and result in unique fuzzy dark matter phenomenology ~\cite{Preskill:1982cy, Abbott:1982af, Dine:1982ah, Hu:2000ke, Arias:2012az, Li:2013nal, Hui:2016ltb, Menci:2017nsr, Diez-Tejedor:2017ivd, Irsic:2017yje, Visinelli:2017imh, Poddar:2019zoe}, which offers possible solutions to three small-scale cosmological puzzles, namely, cusp-vs-core, missing satellite and too-big-to-fail problems~\cite{Moore:1994yx, Flores:1994gz, Navarro:1996gj, Klypin:1999uc}. All these puzzles are based on comparisons between simulations and observed cosmological data. Compared to data, simulations predict high rotation curves towards galaxy centers due to the large DM density therein, too many satellite galaxies, and too many visible dwarf galaxies due to the presence of several DM subhalos. Fuzzy dark matter, being delocalized due to its large De Broglie wavelength, would be more susceptible to tidal disruptions and lead to broader halos possibly solving the three aforementioned problems.

Regardless of the axion solution to the strong $CP$ problem or the Fuzzy DM regime, nonzero abundance of ultralight bosonic DM could lead to a large occupation number for this field, which would behave as a vacuum expectation value (VEV).
The idea is that the DM field undergoes a phase transition in the early universe and starts oscillating around its new VEV.
Hubble friction damps these oscillations, but nevertheless, they may be still lead to observable effects in late times.
This oscillating VEV may lead to a curious phenomenon: time variation of what we define as fundamental constants.
Such effects have been searched for in many different setups,  from resonant microwave cavities to atomic clocks (for a review, see e.g. Ref.~\cite{Battaglieri:2017aum}). Here we are interested in the possibility that neutrinos provide a portal to such ultralight fields.
This is motivated by two facts.
First, neutrinos are much lighter than other fermions in the standard model, and thus even a small time-dependent VEV could lead to a relatively large impact on neutrino masses and mixings.
Second, as the mechanism of neutrino masses remains unknown, this sector may offer a more natural connection to ultralight physics beyond the standard model.
Although we use Fuzzy DM and neutrino masses as a motivation, we are indeed more concerned with general experimental signatures, and thus we adopt a \emph{bottom-up} approach in this work.
Some of these signatures were explored in previous literature~\cite{Berlin:2016woy, Capozzi:2017auw, Krnjaic:2017zlz, Brdar:2017kbt, Farzan:2018pnk, Liao:2018byh, Ge:2018uhz, Huang:2018cwo, Ge:2019tdi, Cline:2019seo, Choi:2019zxy, Farzan:2019yvo}.
Here we will provide a more detailed analysis, with special emphasis on aspects directly connected to experimental searches, and highlighting the different regimes relevant to neutrino oscillation phenomenology.
To be concrete, we will focus on the case of ultralight scalar fields and defer ultralight vector fields to future analysis.
We will use the DUNE experiment as a case study, even if our conclusions will be valid for any neutrino oscillation experiment.

\section{Theoretical guidance to experimental searches}

First, let us review the theoretical aspects of ultralight scalar fields coupled to neutrinos.
We choose to work in an effective theory framework below electroweak symmetry breaking.
The effective Lagrangian that describes the system is
\begin{equation}
    \mathcal{L}_{\rm eff}=-m_\nu\left(1+y\frac{\phi}{\Lambda}\right)\bar\nu\nu+{\rm h.c.},
\end{equation}
where flavor indices are implicit in both $m_\nu$ and $y$, $\phi$ is the ultralight scalar field, $m_\nu$ is the neutrino mass matrix and $\Lambda$ is a heavy mass scale~\footnote{We do not distinguish Dirac and Majorana neutrinos here, as the oscillation phenomenology of these cases are identical.}.
We will not worry where this effective Lagrangian arrives from and leave considerations regarding ultraviolet completions, perhaps, to future work.

The local field value can be expressed as
\begin{equation}
    \phi(x,t)\simeq\frac{\sqrt{2\rho_\phi}}{m_\phi}\sin\left[m_\phi(t-\vec{v}\cdot \vec{x})\right],
\end{equation}
where the local density $\rho_\phi$ should not exceed the local DM density $\rho_{\rm DM}=0.3~{\rm GeV}/{\rm cm}^3$, $m_\phi$ is the mass of $\phi$ and $v\sim10^{-3}c$ is the virial velocity.
Note that the space-dependent phase $m_\phi\vec{v}\cdot\vec{x}$ of the local field value is much smaller than $m_\phi t$, and thus will be neglected henceforth.
The neutrino mass matrix will therefore receive a contribution from $\phi$ given by
\begin{equation}
   \delta m_\nu =  m_\nu y\frac{\sqrt{2\rho_\phi}}{\Lambda m_\phi}\sin(m_\phi t).
\end{equation}
Without a flavor model (see e.g. Ref.~\cite{Ding:2020yen}), the Yukawa couplings $y$ can have any structure in flavor space, and thus the modulations of neutrino masses and mixing can bear any correlation.
Nevertheless, it is useful to focus on two simple scenarios: modulation of mass splittings and modulation of mixing angles.

Besides, the mass of $\phi$ defines the modulation period via
\begin{equation}
   \tau_\phi\equiv \frac{2\pi\hbar}{m_\phi}=0.41 \left(\frac{10^{-14}~{\rm eV}}{m_\phi}\right)~{\rm seconds}.
\end{equation}
In a given experimental setup, there are three characteristic time scales: the neutrino time of flight $\tau_\nu = L/c = 3.4 (L/1000~{\rm km})~{\rm msec}$, the time between two detected events $\tau_{\rm evt}$ (the inverse of the ratio of events) and the lifetime of the experiment $\tau_{\rm exp}$.
From these, we can identify the following three different regimes for a given experimental setup.
\begin{itemize}
   \item {\bf Time modulation ($\tau_{\rm evt}\lesssim\tau_\phi \ll\tau_{\rm exp}$).} When the period of modulation of $\phi$ is of the same order as the experiment total run time, a temporal variation of the neutrino signal may be observed. This is true for the modulation of angles and mass splittings. Experiments with large statistics and high event rates will be sensitive to time modulation periods much smaller than the lifetime of the experiments (for instance, searches for modulations in solar neutrino fluxes are sensitive to periods ranging from 10 minutes to 10 years~\cite{Yoo:2003rc, Aharmim:2005iu, Collaboration:2009qz}).
   \item {\bf Averaged distorted neutrino oscillations ($\tau_\nu\ll\tau_\phi\ll\tau_{\rm exp}$).} Even when the rate of change of neutrino oscillation parameters is too fast to be observed as a modulating signal, the time average oscillation probability may be distorted by such effects and deviate from the standard model scenario. While the averaging of a modulating mixing angle can be mapped onto standard oscillations (with some inferred value of this mixing angle), the averaging of a mass splitting can lead to distorted neutrino oscillations (DiNOs), smearing out the probability similarly to an energy resolution smearing~\cite{Krnjaic:2017zlz}. This regime covers a large range of scalar masses and can be easily searched for in oscillation experiments, as it boils down to a simple novel oscillation effect.
   \item {\bf Dynamical distorted neutrino oscillations ($\tau_\phi\sim\tau_\nu$).} As the modulating period of $\phi$ gets closer to the neutrino time of flight, the changes in oscillation parameters need to be treated at the Hamiltonian level and can be modeled by a modified matter effect~\cite{Brdar:2017kbt}. This matter potential is time-dependent, and thus it changes as the neutrino propagates towards the detector. When the variation of the matter potential is too slow compared to the neutrino time of flight, dynamical DiNOs map onto average DiNOs. In the opposite case, when the variations are too fast compared to the neutrino time of flight, they cannot be observed and thus one recovers standard oscillations.
\end{itemize}
In the next section, we will discuss the phenomenology of each regime in general terms and highlight their phenomenology in oscillation experiments in more detail.

\section{General considerations on ultralight scalars and neutrino oscillations}

Before going into a more technical discussion, we provide a few insights on the effects of ultralight scalar fields in neutrino oscillations.
To do so, we will analyze the changes in neutrino oscillation probability in each of the regimes discussed above, using the DUNE experimental setup as a case study.
For simplicity, we will consider a single parameter modulating at a time.
Modulation of mixing angles are assumed to be of the form
\begin{equation}\label{eq:angles}
   \theta_{ij}(t)=\theta_{ij}+\eta\sin(m_\phi t),
\end{equation}
where $\theta_{ij}$ represents the undistorted value of the mixing angle and $\eta$ is the amplitude of modulation of $\phi$.
Mass splittings, on the other hand, are assumed to modulate like (for $\eta\ll 1$)
\begin{equation}\label{eq:dmsq}
   \Delta m^2_{ij}(t) \equiv m_i^2(t)-m_j^2(t) \simeq \Delta m^2_{ij}\left[1 + 2\eta \sin(m_\phi t)\right],
\end{equation}
where, similarly to above, $\Delta m^2_{ij}$ represents the undistorted value of the mass splitting.

\subsection{Time modulation}\label{sec:time-modulation}
The phenomenology in the time modulation regime is very intuitive: mixing angles or mass splittings are modulating on time.
The oscillation probability now depends on time via
\begin{equation}
   P_{\alpha\beta}\equiv P(\nu_\alpha\to\nu_\beta, t) = P\left[\nu_\alpha\to\nu_\beta; \{ \theta_{ij}(t), \Delta m^2_{ij}(t)\}\right].
\end{equation}
For example, in the case of modulating angles, the oscillation probability for $\nu_\mu\to\nu_\mu$ disappearance in vacuum, in a simplified two neutrino framework, would read
\begin{align}
   P_{\mu\mu}^{\rm angle} \simeq 1-\sin^2\left[2\theta(t)\right]\sin^2\left(\frac{\Delta m^2 L}{4E}\right)=1-\sin^2\left[2\theta+2\eta\sin(m_\phi t)\right]\sin^2\left(\frac{\Delta m^2 L}{4E}\right),
\end{align}
where $L$ is the baseline (1300~km for DUNE) and $E$ is the neutrino energy.
Notice that the oscillation probability displays a time modulation via the $\sin(m_\phi t)$ term.

\begin{figure}
    \centering
    \includegraphics[width= 0.8\textwidth]{figures/timemod-th.pdf}
    \caption{The difference in $\nu_\mu$ disappearance oscillation probability $\Delta P(t)\equiv P_{\mu\mu}(t)-P_{\mu\mu}(0)$ at DUNE for a modulating $\theta_{23}$ assuming $\eta=0.05$ for several energy bins. We have assumed normal mass ordering and the best fit values of oscillation parameters from Ref.~\cite{deSalas:2017kay}, namely $\Delta m^2_{31}=2.5\times 10^{-3}$~eV$^2$, and $\sin^2\theta_{23}=0.55$.}
    \label{fig:timemod-th}
\end{figure}

In Fig.~\ref{fig:timemod-th} we show change in $\nu_\mu$ disappearance oscillation probability $\Delta P(t) \equiv P_{\mu\mu}(t)-P_{\mu\mu}(0)$ at DUNE for a modulating $\theta_{23}$ assuming $\eta=0.05$ for several energy bins.
We have assumed normal mass ordering and the best fit values of oscillation parameters from \cite{deSalas:2017kay}, namely $\Delta m^2_{31}=2.5\times 10^{-3}$~eV$^2$, and $\sin^2\theta_{23}=0.55$.
There are three important effects to be noted here.
To  understand those, we  expand $\Delta P(t)$ for small $\eta$ as
\begin{equation}
   \Delta P(t) \simeq -2\left[\eta \sin(4\theta) \sin(m_\phi t) + 2\eta^2\cos(4\theta)\sin^2(m_\phi t)\right]  \sin^2\left(\frac{\Delta m^2 L}{4E}\right).
\end{equation}
First, the modulation phases across different energies are fully correlated, as the oscillation probability in all energy bins goes up and down at the same time.
Second, $\Delta P(t)$ depends on $\eta$ and the mixing angle itself.
And finally, when $\sin(4\theta)$ is near zero (e.g. for $\theta_{23}$ near maximal mixing), we observe a Jacobian effect that shrinks the oscillation amplitude, as the leading $\eta$ term shrinks and the $\eta^2$ term becomes dominant.
In Fig.~\ref{fig:timemod-th}, as the modulation develops, $\sin^2 [2\theta_{23}(t)]$ goes further away from maximal, making $\Delta P(t)$ larger, and we observe the larger amplitude.
As the phase evolves, $\sin^2 [2\theta_{23}(t)]$ gets maximal, then slightly below maximal, maximal again, and back to its original value.
This corresponds to the region to the right in the subplots ($t/\tau_\phi>0.5$).
If we had chosen to show a modulation of $\theta_{12}$ instead (e.g. in the JUNO experiment~\cite{An:2015jdp}), the change in oscillation probability would have been more symmetric.

If instead, the mass splittings modulate on time, the simplified time-dependent oscillation probability would read
\begin{align}
   P_{\mu\mu}^{\rm mass} \simeq 1-\sin^2(2\theta)\sin^2\left[\frac{\Delta m^2(t) L}{4E}\right]=1-\sin^2(2\theta)\sin^2\left\{\left(\frac{\Delta m^2 L}{4E}\right) \left[1+2\eta\sin(m_\phi t)\right]\right\}. \nonumber
\end{align}
We can see that what modulates is not the amplitude of the oscillation probability, but rather the position of the minimum. In Fig. \ref{fig:timemod-dm}, we show again the change in $\nu_\mu$ disappearance oscillation probability $\Delta P(t) \equiv P_{\mu\mu}(t)-P_{\mu\mu}(0)$ at DUNE, but now for a modulating $\Delta m^2_{31}$ assuming $\eta=0.05$ for several energy bins.
Again, we have assumed normal mass ordering and the best fit values of oscillation parameters from \cite{deSalas:2017kay}, namely $\Delta m^2_{31}=2.5\times 10^{-3}$~eV$^2$, and $\sin^2\theta_{23}=0.55$.
The most distinctive features, in this case, are the correlations and anti-correlations across multiple energies.
This is easy to understand, as when the minimum or other regions of small probability enter/leave a given energy bin, the average probability lowers/raises in that bin.
Quantitatively, we can see these correlations in energy by expanding $\Delta P(t)$ around $\eta\to0$,
\begin{equation}
  \Delta P(t)\simeq  -2\sin^2(2\theta)\sin(m_\phi t)  \left[ \eta \xi\sin(2\xi) + 2 \eta^2 \xi^2  \cos(2\xi)\sin(m_\phi t)\right],
\end{equation}
where we have defined $\xi\equiv\Delta m^2 L/4E$.
Note that this expansion is valid  for $\eta \xi \ll 1$.
These correlations are very specific for a given experimental baseline and energy binning, and one would expect it to be useful in distinguishing ultralight scalar phenomenology from other time-dependent effects like Lorentz symmetry violation (see e.g. Ref.~\cite{Kostelecky:2011gq}).
Besides, due to the moving of the oscillation minimum, the change in oscillation probability at energies near the minimum can be enhanced.
In this example, $\eta=0.05$ can lead to $\Delta P (t)\simeq 0.2$.

\begin{figure}
    \centering
    \includegraphics[width = 0.8\textwidth]{figures/timemod-dm.pdf}
    \caption{The difference in $\nu_\mu$ disappearance oscillation probability $\Delta P(t)\equiv P_{\mu\mu}(t)-P_{\mu\mu}(0)$  at DUNE for a modulating $\Delta m^2_{31}$ assuming $\eta=0.05$ for several energy bins. We have assumed normal mass ordering and the best fit values of oscillation parameters from Ref.~\cite{deSalas:2017kay}, namely $\Delta m^2_{31}=2.5\times 10^{-3}$~eV$^2$, and $\sin^2\theta_{23}=0.55$.}
    \label{fig:timemod-dm}
\end{figure}

A search for time-dependent frequencies in the data would seem suitable to probe this scenario, for modulations of either mixing angles or mass splittings.
Such studies have already been performed by e.g. SNO, Super-Kamiokande, and Daya Bay collaborations~\cite{Yoo:2003rc, Aharmim:2005iu, Collaboration:2009qz, Adey:2018qsd}.
In the next section, we will provide a detailed time-dependent analysis of mock experimental data (we use the DUNE set up as an example), employing the Lomb-Scargle method, to estimate sensitivity to ultralight scalars.

\subsection{Average Distorted Neutrino Oscillations}\label{sec:average-dino}
The second regime we study here is dubbed average distorted neutrino oscillations or average DiNOs for short.
In this regime, the modulation of mixing angles or mass splittings is too fast to be observed, but an averaging effect on oscillation probabilities remains.
To see how this comes about, imagine that the modulating period of the ultralight scalar field is much shorter than the experimental data collecting time, but still much longer than the neutrino time-of-flight (such that the oscillation parameters are essentially constant for each neutrino event).
The average oscillation probability would be given by~\cite{Krnjaic:2017zlz}
\begin{align}
   \langle P_{\alpha\beta}\rangle=\frac{1}{\tau_\phi}\int_0^{\tau_\phi} dt \, P_{\alpha\beta}(t),
\end{align}
where $\tau_\phi$ is the period of the ultralight scalar field.
First, we focus on the averaging of mass splittings, which will prove to be more interesting than averaging of angles.
For the vacuum, 2-flavor, muon neutrino disappearance oscillation, the averaging is
\begin{align}\label{eq:average-prob}
   \langle P^{\rm mass}_{\alpha\beta}\rangle & =\frac{1}{\tau_\phi}\int_0^{\tau_\phi} dt \left\{ 1-\sin^2(2\theta) \sin^2\left[\left(\frac{\Delta m^2 L}{4E}\right) \left[1+2\eta\sin(m_\phi t)\right]\right]\right\}\\
        & \simeq 1-\sin^2(2\theta)\left\{\sin^2\left(\frac{\Delta m^2 L}{4E}\right)+2\eta^2 \left(\frac{\Delta m^2 L}{4E}\right)^2\cos\left(\frac{\Delta m^2 L}{2E}\right)\right\},
\end{align}
\begin{figure}
    \centering
    \includegraphics[width = 0.7\textwidth]{figures/av-dm.pdf}
    \caption{Averaged $\nu_\mu$ disappearance probability at DUNE for a modulating $\Delta m^2_{31}$ for three different values of $\eta$ and in the absence of DiNOs ($\eta$= 0).}
    \label{fig:av-dm}
\end{figure}
where the last expression was expanded to order $(\eta \Delta m^2 L/4E)^2$, which is typically fine for the first oscillation minimum and $\eta<0.05$.
As shown in Fig.~\ref{fig:av-dm} for oscillation parameters from Ref.~\cite{deSalas:2017kay} and different values of $\eta$, the effect of mass splitting averaging is a smearing in the oscillation probability, similar to the effect of a finite energy resolution.
Therefore, one would expect experiments like DUNE, KamLAND and JUNO to be ideal to probe such scenarios, as all of them have good energy resolution and are endowed with broad band beams that allow for the observation of the full shape of the oscillation probability.

Regarding the averaging of modulating angles, it is easy to see that this effect simply maps into standard oscillation probability with different parameters.
The average mixing would be~\cite{Krnjaic:2017zlz}
\begin{align}
   \frac{1}{\tau_\phi}\int_0^{\tau_\phi} dt \, \sin^2\left[2\theta+2\eta\sin(m_\phi t)\right] = \frac{1}{2}\left[1-J_0(4\eta)\cos(4\theta)\right]\simeq \sin^2(2\theta)(1-4\eta^2)+2\eta^2,
\end{align}
where $J_0$ is a Bessel function of the first kind and the righthand side was expanded to second order in $\eta$.
As one expects, the effect of averaging is pushing apparent mixing angles away from zero or maximal mixing.
Experimental sensitivity to average DiNO effects on mixing angles depends not only on the precision with which the experiment can determine the mixing angles but also on the value of the measured angle itself.
Because of that, we will focus on the modulation of mass splittings in the case of average DiNO.

\subsection{Dynamical Distorted Neutrino Oscillations}\label{sec:dynamical-dinos}
The last regime is the dynamical DiNO, in which the effect of modulation of the neutrino mass matrix in oscillations needs to be taken into account at the Hamiltonian level.
The matter potential induced by the ultralight scalar field can be written as~\cite{Brdar:2017kbt}
\begin{equation}
  V_\phi(t) = \frac{1}{2E}\left[(Y m_\nu + m_\nu Y)\phi(t)+Y^2\phi^2(t)\right],
\end{equation}
where we have defined the coupling matrix $Y\equiv m_\nu y/\Lambda$.
Then the Hamiltonian that drives the evolution of the system is given by
\begin{equation}
  H(t) = H_{\rm vac} + V_{\rm matter}+ V_\phi(t),
\end{equation}
where $H_{\rm vac}$ is the vacuum Hamiltonian, that is, $\textrm{diag}(0,\,\Delta m^2_{21},\, \Delta m^2_{31})/2E$ in the mass basis, $V_{\rm matter}$ is the usual matter potential, $V_{\rm matter} = U^\dagger \textrm{diag}(V_{\rm cc},\,0,\, 0)U$ in the mass basis, and $U$ is the PMNS matrix.
Since $\phi$ evolves in time, the full Hamiltonian also depends on time.

Here we propose a simplification of this treatment which is valid when considering a modulation effect either solely in the mixing angles  or solely in the mass splittings.
If the modulation of $\phi$ affects solely the mass splittings, we can work in the mass basis (denoted by a ``0'' subscript) and write
\begin{equation}
     H_0(t) \equiv \frac{1}{2E}
\left(\begin{array}{ccc}
 0 & 0  &0   \\
 0 & \Delta m^2_{21}(t)  & 0  \\
 0 & 0  & \Delta m^2_{31}(t)
\end{array}\right)
   +U^\dagger \left(\begin{array}{ccc}
 V_{\rm cc} & 0  & 0  \\
 0 & 0  & 0  \\
 0 & 0  & 0
\end{array}\right)U
\end{equation}
where the time dependent mass splittings are given in Eq.~\eqref{eq:dmsq}.
We write the neutrino state in the mass basis as $\nu = U^\dagger \nu_{\rm fl}$ (the ``fl'' subscript denotes flavor).

The evolution of this state is given by   $\dot\nu = i H_0(t) \nu$, which has to be solved numerically and leads to an ``instantaneous'' oscillation probability from flavor $\alpha$ to $\beta$, namely, $P_{\alpha\beta}(t_0,L)$.
Numerically, the propagation of the neutrino from the source to the detector can be implemented by dividing the path into $N$ layers of thickness $\Delta L=L/N$ where the oscillation parameters do not change substantially in each layer.
The oscillation probability from flavor $\alpha$ to flavor $\beta$ is given by
\begin{equation}
    P_{\alpha\beta} (t_0, L) = |\bra{\nu_\alpha} U \left\{\prod_{n=1}^N \exp\left[i H_0(t_n) \Delta L\right]\right\}U^\dagger\ket{\nu_\beta}|^2~~~~~~~~~(\textrm{for } \Delta m^2 \textrm{  modulation}),
\end{equation}
where $U^\dagger\ket{\nu_{\alpha}}$ is a flavor state $\ket{\nu_{\alpha}}$ written in the mass basis, and $t_n\equiv t_0+n\Delta L$.
Note that due to the presence of the MSW term, the Hamiltonian in different layers do not commute with each other. Throughout the duration of the experiment, all possible initial phases will be scanned randomly.
Therefore, the observed oscillation probability is the time average of $P_{\alpha \beta}(t_0,L)$, namely
\begin{equation}\label{eq:obs-prob}
  \langle P_{\alpha\beta}(L)\rangle = \frac{1}{\tau_\phi}\int_0^{\tau_\phi}dt_0 P_{\alpha \beta}(t_0,L),
\end{equation}
where again, $\tau_\phi=2\pi/m_\phi$ is the period of oscillation of $\phi$.

For the case of modulating mixing angle, it is more convenient to write the Hamiltonian in the flavor basis (again denoted by the subscript ``fl'') and write the full Hamiltonian as
\begin{equation}
     H_{\rm fl}(t) \equiv \frac{1}{2E}U(t)
\left(\begin{array}{ccc}
 0 & 0  &0   \\
 0 & \Delta m^2_{21}  & 0  \\
 0 & 0  & \Delta m^2_{31}
\end{array}\right)U^\dagger(t)
   + \left(\begin{array}{ccc}
 V_{\rm cc} & 0  & 0  \\
 0 & 0  & 0  \\
 0 & 0  & 0
\end{array}\right),
\end{equation}
where the PMNS matrix is now changing in time.
The evolution of a neutrino of definite flavor $\nu_{\rm fl}$ is $\dot\nu_{\rm fl} = i H_{\rm fl}(t) \nu_{\rm fl}$ and the observed oscillation probability is given by Eq.~\eqref{eq:obs-prob}.
Following the previous recipe, the oscillation probability can be calculated with
\begin{equation}
    P_{\alpha \beta} (t_0, L) = |\bra{\nu_\alpha} \left\{\prod_{n=1}^N \exp\left[i H_{\rm fl}(t_n) \Delta L\right]\right\}\ket{\nu_\beta}|^2~~~~~~~~~(\textrm{for } \theta_{ij} \textrm{  modulation}).
\end{equation}
Note that we do not need to rotate the initial flavor neutrino by the PMNS matrix as we decided to work here in the more appropriate flavor basis.
The observed oscillation probability is again given by the average over $t_0$, as in Eq.~\eqref{eq:obs-prob}.

We can see the effect of dynamical DiNOs in Fig.~\ref{fig:dynprob} for modulations of $\Delta m^2_{31}$ (left) and $\theta_{23}$ (right) for oscillation parameters from Ref.~\cite{deSalas:2017kay} and a modulation amplitude of $\eta=0.1$ and $L=1300$~km.
In the left panel, it is clear to see that as $\tau_\phi/\tau_\nu$ gets larger, the effect shrinks, as the changes in the matter effect become too fast to affect neutrino oscillations.
Besides, as $\tau_\phi/\tau_\nu$ gets smaller, the effect of dynamical DiNOs asymptotes to that of average DiNOs, as one would expect.
For mixing angle modulations (right panel), the Jacobian effect discussed in Sec.~\ref{sec:time-modulation} suppresses the impact of modulating $\theta_{23}$ in DUNE.
Notice also that there is a small displacement of the minima and maxima of oscillations.
This is simply due to the fact that the effective mass splitting measured in long baseline $\nu_\mu$ disappearance is not exactly $\Delta m^2_{31}$, but rather a function of atmospheric splittings and mixings, typically dubbed $\Delta m^2_{\mu\mu}$~\cite{Nunokawa:2005nx}.
In this plot, we have chosen a fixed value of $\Delta m^2_{31}$ to obtain the curves.
This displacement could simply be mapped into a different value of the atmospheric mass splitting.

\begin{figure}
    \includegraphics[width = 0.47\textwidth]{figures/dyn-dm.pdf}~
    \includegraphics[width = 0.47 \textwidth]{figures/dyn-th.pdf}
    \caption{The $\nu_\mu$ disappearance probability at DUNE for a modulating $\Delta m^2_{31}$ (left) and $\theta_{23}$ (right) in the dynamical regime, for different values of the ratio between the period of the modulation $\tau_\phi$ and the neutrino time of flight $\tau_{\nu}$.  }
    \label{fig:dynprob}
\end{figure}

\section{Case study: DUNE phenomenology}

In this section, we will perform a case study of how the oscillation experiments can probe the ultralight scalars that we introduced in the previous sections. We will analyze the DUNE sensitivity to the aforementioned three regimes.
For all analyses performed here, we followed the simulation of Ref.~\cite{Alion:2016uaj} using the GLoBES software~\cite{Huber:2004ka, Huber:2007ji}
We have assumed the DUNE experiment to have a 1.07~MW beam, four far detectors with a total mass of 40~kton, and a total run time of 7 years, equally divided between neutrino and antineutrino mode.
We took the matter density to be constant $\rho=2.8~{\rm g}/{\rm cm}^{3}$.
The neutrino spectrum at DUNE spans energies roughly from 1-5 GeV, with a peak at around 3 GeV.
From Ref.~\cite{Alion:2016uaj}, the main systematic uncertainties are related to the beam and cross-section modeling.
As it is important for some of the results that will follow, we call the attention that the reconstructed neutrino energy resolution from Ref.~\cite{Alion:2016uaj} is approximately 16\% at 3~GeV.
Finally, in general terms, the ultralight phenomenology is better probed by the $\nu_\mu$  and $\bar\nu_\mu$ disappearance channels, as they bring in the largest statistics.

In our numerical simulations, the best fit oscillation parameters were taken from Ref.~\cite{deSalas:2017kay} ($\Delta m^2_{21}=7.5\times 10^{-5}$~eV$^2$, $\Delta m^2_{31}=2.5\times 10^{-3}$~eV$^2$, $\sin^2\theta_{12}=0.32$, $\sin^2\theta_{13}=0.0216$, $\sin^2\theta_{23}=0.55$, $\delta=1.2\pi$) and normal mass ordering was assumed for concreteness.
We have used current priors for the oscillation parameters that were marginalized over in the analysis performed~\footnote{We took the largest one-sided $1\sigma$ error for each oscillation parameter from Ref.~\cite{deSalas:2017kay}).}.

\subsection{Time modulation phenomenology at DUNE}

The signature of the time modulation regime is the presence of a periodic signal in the oscillated neutrino spectrum at the far detector.
As can be seen in Eqs.~\eqref{eq:angles} and \eqref{eq:dmsq}, the period of modulation is given by the mass of the scalar field, and thus a positive signal of time modulation at DUNE would provide a measurement of the mass of this field.

In general, the search for periodic signals in data sets can be performed using the Lomb-Scargle periodogram~\cite{Lomb:1976wy, Scargle:1982bw}, which is an extension of the classical periodogram for unevenly separated data (see Ref.~\cite{VanderPlas_2018} for a pedagogical review).
Such searches are not new in the context of neutrino physics.
For instance, many analyses of periodicities in the solar neutrino flux have been performed in SNO~\cite{Aharmim:2005iu, Ranucci:2006rz} and SuperKamiokande~\cite{Ranucci:2005ep}, as well as for other time-varying signals in the context of Lorentz and CPT violation in Daya Bay~\cite{Adey:2018qsd}.

To evaluate the statistical significance of a modulation in a data set, we first define the Lomb-Scargle (LS) power for a frequency $\omega$ as
\begin{equation}
 \begin{split}
    P_{LS}(\omega) =
\frac{1}{2}\Bigg\{ \bigg( \sum_{n} g_n \cos [2\pi \omega (t_n -\tau)]\bigg)^2 \bigg/ \sum _n \cos^2 [2\pi \omega (t_n -\tau)] + \\
\bigg( \sum_{n} g_n \sin [2\pi \omega (t_n -\tau)]\bigg)^2  \bigg/ \sum _n \sin^2 [2\pi \omega (t_n -\tau)]   \Bigg\}
\end{split}
\end{equation}
where $g_n = g(t_n)$ is the signal at the time of the measurement $t_n$ and $\tau$ is defined by solving $\tan (4\pi \omega \tau) = \sum_n \sin(4 \pi \omega t_n) / \cos(4\pi \omega t_n)$.

The significance of a given LS power can be quantified with the False Alarm Probability Test (FAP), which is a measure of how likely it is that a data set with no signal would give rise to a peak of the same magnitude as a consequence of spurious background noise. To estimate the FAP we followed the Baluev approach~\cite{Baluev:2007su}, which provides an upper limit to the value obtained through more sophisticated approaches based on a Bootstrap Method. A more detailed discussion can be found in Ref.~\cite{VanderPlas_2018}.

In our analysis, we considered larger than nominal energy bins, which allows us to extend the sensitivity to smaller periods.
In order to cover all the parameter space presented, different time binning of the events has been explored.
In an experimental setup, different choices of the time bins can be explored \textit{a posteriori}, ensuring that the whole accessible parameter space is covered.
As discussed in Fig.~\ref{fig:timemod-dm}, time modulation effects from ultralight scalars can lead to correlated (and anti-correlated) modulations in different energy bins, depending on which oscillation parameter is modulating.
In the case of a positive modulation signal, such correlations can be exploited to further constrain the model.
Different data sets generated for different values of modulation amplitude and frequency have been tested with the LS periodogram and Baluev's approach to the FAP test.

\begin{figure}[t!]
    \centering
    \includegraphics[width = 0.375\textwidth]{figures/allowed2.pdf}
    \hspace{1cm}
    \includegraphics[width = 0.545\textwidth]{figures/notallowed.pdf}
    \caption{Expected number of events in different time bins at three different energy bins for a particular realisation of DUNE. Gray dashed lines represent the number of events expected with $\eta = 0$ and the shadowed region corresponds to the $1\sigma$ statistical uncertainty. Light blue lines are the expected  signal with non-zero $\eta$ and $m_\phi$, while dark blue lines represent a random realisation of the signal which includes statistical fluctuations.
    Left panel corresponds to a set of parameters $(\eta, m_\phi)$ in the 90$\%$ CL region above shown. Right panel corresponds to a point in the $\eta-m_\phi$ plane which LS method would not identify the frequency correctly.
    \label{fig:allowed}}
\end{figure}

A typical realization of the signal in DUNE, for modulation of mass splittings, is presented in Fig.~\ref{fig:allowed} for illustrative purposes.
Two modulation amplitudes are shown, $\eta=0.063$ and $\eta=0.012$.
As we will see later, DUNE is expected to be sensitive to the larger but not to the smaller.
The expected number of events is presented for three different energy bins assuming 3 years running time in the neutrino mode~\footnote{Although we show only 3 energy bins, we use the entire energy range available in our simulations.}.
The original period of the data ($\tau_\phi$) and the one determined with the LS method ($\tau_{LS}$) are presented together with the FAP score.

In Fig.~\ref{fig:LS}, we show the DUNE sensitivity to modulations of the mass splitting $\Delta m^2_{31}(t)$ as discussed in Eq.~\eqref{eq:dmsq}.
We present the parameter space for which the Lomb-Scargle method would identify a frequency in the data set such that one would be able to state that there is a 90$\%$ probability that the periodic signal found in data is not due to random noise.
It is important to point out that this is different from stating that there is a periodic signal with a given frequency in the data set.

\begin{figure}
    \centering
    \includegraphics[width = 0.8\textwidth]{figures/LSv4.pdf}
    \caption{Region in the modulation amplitude $\eta$ versus period $\tau_\phi$ plane for which the analysis performed using the Lomb-Scargle periodogram would be capable to state at a 90$\%$ C.L. that the periodic signal found in 7 years of DUNE data would not be spurious. Upper x-axis presents the corresponding range for the mass of the ultralight scalar, $m_\phi$.}
    \label{fig:LS}
\end{figure}

The smallest period (largest frequency) to which DUNE is expected to be sensitive corresponds to the case in which the scalar oscillation period is about a few days.
Sensitivity at large frequencies requires smaller time bins, leading to fewer events per bin which are more prone to statistical fluctuation.
Consequently, the sensitivity to the amplitude decreases when looking for shorter periods.
The largest period is determined by the running time of the experiment and is expected to be a couple of years.  This means that DUNE would be sensitive to the range of scalar masses  $5\times 10^{-23}\lesssim m_\phi \lesssim 10^{-20}$~eV.
Moreover, the maximum sensitivity on the amplitude of the modulation $\eta$ is about 4\%.

We do not show the DUNE sensitivity to modulations of the mixing angle $\theta_{23}$.
Due to the Jacobian effect discussed in Sec.~\ref{sec:time-modulation}, the values of $\eta$ necessary to yield an observable effect at DUNE would need to be $\mathcal{O}(1)$.
Therefore we see the mass splitting modulation search as a more promising way of detecting the presence of ultralight bosonic dark matter.
Nevertheless, the same Lomb-Scargle technique described above could be used to probe the modulations of mixing angles.

This analysis is not free from systematic uncertainties.
Deadtime intervals of any neutrino detector may span from months to milliseconds.
These would constitute an important source of systematic errors when analyzing time modulations.
In particular, quasiperiodic deadtimes such as scheduled breaks of runs or maintenance and calibration operations could lead to peaks in the Lomb-Scargle power spectrum.
It is possible to deal with them by estimating the window function, see Ref.~\cite{VanderPlas_2018}.
This method allows us to identify the main features of the structure of the window.
The existence of a certain periodicity in data taking would induce peaks both in the Lomb-Scargle power spectrum and in the window power spectrum and consequently, one can identify the corresponding frequencies as related to the experiment and not to the physical phenomenon under study.

Beam unrelated backgrounds, like cosmic rays and atmospheric neutrino, can also exhibit time modulation, but these are typically negligible in beam neutrino experiments.
Moreover, beam performance can change over time.
One would expect near-to-far ratios to be less sensitive to these variations.
Nevertheless, the observed neutrino beam is not the same in the near and far detectors (due to different geometry), and oscillations may further enhance this difference.
Thus, experiments should take those systematics into consideration when performing a search for the time dependence of the neutrino signal.
In our results, we have not considered those systematics, though we believe they would not degrade the overall sensitivity by much.

\subsection{Average distorted neutrino oscillations at DUNE}

The second regime we will study in detail in DUNE is the case of average distorted neutrino oscillations (average DiNOs).
In this case, modulations of mass splittings are too fast to be observed as a time modulation signal, but the averaging of the modulation still imprint observable effects in the oscillation probability.
As discussed in Sec.~\ref{sec:average-dino}, the modulation of mass splittings leads to more interesting phenomenology than the modulation of mixing angles.
If $\Delta m^2 _{31}$  varies in time, the maxima and minima are displaced periodically.
For a very fast modulation, such displacement manifests as a non-trivial averaging and has to be carefully studied in order to disentangle it from the distortion caused by the finite energy resolution~\cite{Krnjaic:2017zlz}.
Consequently, the searches here presented would benefit from improvements in the energy resolution, as the one proposed in Ref.~\cite{Friedland:2018vry}.
As a general rule of thumb, the new physics effect here is just a modification of the oscillation probability, so all systematic uncertainties associated to an oscillation search would be relevant in this case.
We include those systematics using the simulation from Ref.~\cite{Alion:2016uaj}.

The average oscillation probability in Eq.~\eqref{eq:average-prob}, necessary to estimate DUNE sensitivity to this scenario, was calculated by numerically averaging the analytic approximations for neutrinos oscillations in the presence of matter from Ref.~\cite{Denton:2016wmg}.
The DUNE sensitivity  to fast modulations of the mass splitting is shown in Fig.~\ref{chi-av}.
The range of periods that DUNE is sensitive to, in this regime, is approximately from a year ($\tau_\phi\ll\tau_{\rm exp}\sim$~10 years) to tens of milliseconds ($\tau_\phi\gg\tau_\nu\simeq$~4.3~msec).
This translates into a very large range of masses $2\times 10^{-23} \lesssim m_\phi\lesssim 3\times 10^{-14}$~eV.
On the flip side, if a signal of average DiNOs is observed at DUNE, it would be very challenging to pinpoint the exact mass of $\phi$, as its effects has been averaged out.
As can be seen from the left panel of Fig.~\ref{chi-av}, DUNE is expected to be sensitive to roughly 4\% modulation amplitudes of the mass splitting at  90\% C.L.
In estimating DUNE's sensitivity, we have marginalized over all oscillation parameters.
Note that the energy resolution is crucial here, and we expect improvements in energy resolution to translate into better sensitivity to average DiNOs.

Besides, one may ask what is the impact on the determination of the standard mixing parameters if an average DiNO effect is present.
We show in the right panel of Fig.~\ref{chi-av} the allowed region by DUNE in the plane $(\eta,\,\sin^22\theta_{23})$.
There is some mild degeneracy between $\theta_{23}$ and the modulation amplitude $\eta$ for small values of $\eta$.
This is because, for small $\eta$, the minimum of the $\nu_\mu\to\nu_\mu$ oscillation probability lifts slightly thus allowing values of $\theta_{23}$ closer to $\pi/4$.
We have checked that there is no degeneracy between $\delta_{CP}$ and $\eta$.

\begin{figure}
    \centering
    \includegraphics[width = 0.58\textwidth]{figures/chi2-dmav.pdf}~
    \includegraphics[width = 0.4\textwidth]{figures/th23v4.pdf}
    \caption{Left: $\chi^2$ profile as a function of $\eta$ and confidence levels to discriminate with respect to the standard 3$\nu$ picture. Right: allowed region in the plane $(\eta, \, \sin^2\theta_{23})$ in DUNE. Best fit values chosen for mock data are marked by a black circle (standard oscillations assumed as true hypothesis).}
    \label{chi-av}
\end{figure}

\subsection{Dynamical distorted neutrino oscillations}
Now, we proceed to the last regime of ultralight scalar field phenomenology in neutrino experiments, that of dynamical distorted neutrino oscillations (dynamical DiNOs).
In this regime, the time of flight of the neutrino is comparable to the magnitude of the scalar period and we have to take full account of the variation of the oscillation parameters during the journey from the source to the detector.
As before, we consider modulations in $\theta_{23}$ and $\Delta m^2_{31}$ separately, which leads to the oscillation probabilities discussed in Sec.~\ref{sec:dynamical-dinos}.
As discussed in the previous section, the new physics effect here is again just a modification of the oscillation probability, so all systematic uncertainties associated with an oscillation search would be relevant in this case.

We evaluate the DUNE sensitivity to the dynamical DiNO regime for the case of mass splitting modulations and present the results in Figs.~\ref{fig:dyn-mass}.
As expected, when the modulation period is much smaller than the neutrino time-of-flight (of about 4.3~msec), the experimental sensitivity degrades as the oscillation probability tends to the standard one.
Besides, for mass splitting modulation, when the modulation period is sufficiently large, we recover the average DiNO sensitivity, see Fig.~\ref{fig:dynprob}.
In the case of mixing angle modulation, the averaging simply maps the modulating mixing angle onto another value of the mixing, and thus we do not analyze this case here.
In principle, a richer flavor structure in the coupling between ultralight scalar and neutrinos would allow concomitant modulation of mass splittings and angles with arbitrary correlations.
For simplicity, we do not pursue this possibility in this manuscript.

\begin{figure}
    \centering
    \includegraphics[width = 0.8\textwidth]{figures/mphi-eta2v4.pdf}
    \caption{DUNE sensitivity in a fast modulation of the $\Delta m^2_{31}$ mass splitting with amplitude $\eta$ versus the mass of the ultralight scalar $m_\phi$ plane at 90$\%$ C.L (green) and $3\sigma$ (blue). Upper x-axis presents the corresponding range for the dimensionless quantity $m_\phi L_{DUNE} / 2\pi$.}
    \label{fig:dyn-mass}
\end{figure}

\vspace{1cm}

Finally, we present in Fig.~\ref{fig:all}  DUNE's sensitivity to ultralight scalar dark matter incorporating the three searches proposed in this paper.
It is remarkable that a neutrino oscillation experiment can probe scalar masses ranging about 10 orders of magnitude.
The transition between dynamical DiNOs and average DiNOs can be seen to be smooth.
When time modulation can be seen (LS labeled region), it provides an even better probe of ultralight scalars.
While its sensitivity spans a very large region in parameter space, DUNE would only be able to measure the mass of $\phi$ by the determination of the modulation frequency, which is only possible in the ``LS'' region.
Elsewhere, even if distorted neutrino oscillations are observed, it is not clear on how to determine the ultralight scalar mass.
\begin{figure}
    \centering
    \includegraphics[width = \textwidth]{./figures/combined.pdf}
    \caption{DUNE sensitivity (90\% C.L.) to ultralight scalars  via modulation of the atmospheric mass splitting $\Delta m^2_{31}$. The amplitude of modulation is $\eta$ (see Eqs.~\eqref{eq:angles} and \eqref{eq:dmsq}), and the modulation period and mass of the scalar field is denoted by $\tau_\phi$ and $m_\phi$, respectively.}
    \label{fig:all}
\end{figure}

\section{Other constraints on ultralight scalars}
Besides neutrino oscillations, ultralight bosonic dark matter may also be probed by other experiments and cosmological observations.
Several other constraints can be found in previous literature.
Here we simply summarize and comment on them.
\begin{itemize}
   \item CMB: As pointed out in previous work, the cosmological $\phi$ density redshifts as nonrelativistic matter, and thus the amplitude of modulation of $\phi$ is expected to be much larger at early times. This could lead to an increase in the sum of neutrino masses in the early universe, which would be constrained by observations of the Planck satellite~\cite{Ade:2015xua}. The constraint on the amplitude of $\phi$ is found to be $\eta\lesssim 9\times 10^{-3}$ if the atmospheric mass splitting modulates or $\eta \lesssim0.1$ if only the solar splitting modulates~\cite{Berlin:2016woy, Krnjaic:2017zlz, Brdar:2017kbt}. Note however that this constraint is model dependent. For example, if neutrino masses arrive from a seesaw mechanism and $\phi$ couples to, e.g., right-handed neutrinos, a large mass of the latter would actually imply a smaller mass of active neutrinos in the early universe.
   \item BBN: Following a similar reasoning, if $\phi$ couples universally to all standard model fermions, the changes in fermion masses could lead to observable effects in big bang nucleosynthesis, particularly on the abundance of $^4$He~\cite{Sibiryakov:2020eir}. In our scenario, we are only coupling $\phi$ to neutrinos, and therefore this bound would not apply. In a UV complete realization, this bound should be taken into account carefully.
   \item Astrophysical neutrinos and supernova 1987A: The coupling between neutrinos and the ultralight scalar could lead to scattering of astrophysical neutrinos on the dark matter background, making the universe opaque to certain astrophysical neutrinos. In particular, the observation of neutrinos from the supernova 1987A requires the universe to be transparent to MeV neutrinos. These constraints are several orders of magnitude weaker than the ones derived from neutrino oscillation measurements, except for large masses $m_\phi\gtrsim 10^{-8}$~eV where neutrino experiments lose sensitivity~\cite{Krnjaic:2017zlz, Brdar:2017kbt}.
   \item Electron mass modulation: Even if we postulate that $\phi$ only couples to neutrinos at tree level, a loop level coupling to electrons cannot be avoided, which could potentially lead to stronger constraints. Nevertheless, the magnitude of the loop-induced coupling is suppressed by $G_F m_e m_\nu$, too small to be observed~\cite{Krnjaic:2017zlz}.
   \item Black hole spin measurements: Ultralight bosons can be emitted copiously by rotating black holes, thereby suppressing their energy and angular momentum. The constraints from black hole spin measurements are typically in the parameter space within the region $10^{-21}<m_\phi<10^{-16}~$eV.
   Note that these bounds present some dependence on the systematic uncertainties related to black hole mass and spin observations, as well as
   on the details of the UV model (for instance, scalar self-interactions may weaken those bounds)~\cite{Baryakhtar:2017ngi, Davoudiasl:2019nlo, Zu:2020whs}.
\end{itemize}

\section{Conclusion}
In this paper, we have investigated in detail the phenomenology of ultralight bosonic dark matter fields in neutrino oscillation experiments.
We describe the three phenomenological regimes associated with different masses of the bosonic field, together with their respective signatures at neutrino oscillation experiments.
As a case study, we estimate the sensitivity of the DUNE experiment to ultralight scalars via detailed simulations and we provide a description of how to implement an experimental search for all regimes.
Finally, we show that the DUNE experiment is sensitive to about 10 orders of magnitude in ultralight scalar mass.
The searches presented in this paper are general and can be easily applied to any other oscillation experiment.
Current experiments like MINOS, NOvA, T2K, Daya Bay, and RENO may perform the very first experimental searches for these scenarios.
In the future, besides DUNE, we also expect the JUNO to be particularly sensitive to modulations of mass splittings due to ultralight scalars.
Our results exhibit an excellent, unique opportunity to expand the physics program of neutrino oscillation experiments.

\section{Acknowledgements}
We thank Vedran Brdar, Zackaria Chacko, Gordan Krnjaic, Joachim Kopp, Alex Sousa and Jaehoon Yu for discussions.
PMM is grateful for the kind hospitality of Fermilab theory group during the development of this work.
This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. PMM is supported by the FPU  grant  FPU18/04571, the Spanish grants FPA2017-90566-REDC (Red Consolider MultiDark), FPA2017-85216-P and SEV-2014-0398(MINECO/AEI/FEDER,  UE),  as  well  as  PROMETEO/2018/165  (Generalitat  Valenciana).  PMM received  partial  support  from  the  EU  Horizon 2020 project InvisiblesPlus (690575-InvisiblesPlus-H2020-MSCA-RISE-2015).   AD is supported in part by the National Science Foundation under Grant Number PHY-1914731.

redpajama_set_name: RedPajamaArXiv


text:
Gus Poyet
No hiding place for Sunderland says anxious Gus Poyet
Updated 09:33, 9 Dec 2013
By Mark Douglas
A worried Gus Poyet has told his Sunderland players they must stop hiding behind excuses and bad luck after a stark Stadium of Light wake-up call for the Premier League's bottom side
A worried Gus Poyet has told his Sunderland players they must stop hiding behind excuses and bad luck after a stark Stadium of Light wake-up call for the Premier League's bottom side.
The apparent progress of recent weeks felt like it was a distant memory as Sunderland were played off the park by a Tottenham team that might – in Poyet's words – have won 5-1 if they had more confidence in front of goal. That seemed to dent the confidence of the normally upbeat Black Cats boss, who was a visibly deflated presence in his post-match press conference.
He spoke of players failing to heed multiple warnings about mistakes they were making and of the alarming tendency of the team to score own goals as "no coincidence".
To be fair, Poyet must take some of the blame for Saturday's defeat as well, with his decision to go with two strikers in Jozy Altidore and the out-of-sorts Steven Fletcher coming back to haunt the Sunderland boss as his team were overrun in midfield.
The situation is becoming starker with every weekend and Poyet has called for his team to stop trying to find the easy "get out" of bad luck or bad officiating. Again on Saturday, they were the victim of poor decisions when Lee Mason failed to spot a blatant Sandro handball in the second half.
In truth, that would have made little difference to the overall result.
Poyet said on Saturday: "It is too early to analyse the game now because of what I am feeling,
"I hate losing and it is very difficult to explain. I am trying to be calm and I will analyse the game on Sunday and look at the things we did badly in the second half.
"The problem is it is too many. I am a normal person, I can have a fight with you but if you beat me once, you beat me twice, I won't come a third time. I am not that stupid.
"I am not going to get kicked every time.
"There needs to be a moment when that is it and there are no more excuses or bad luck. That is where we are hiding at the moment
"I always say we. I am not criticising the players, we say we. We made bad decisions. I am the first one, so I am not criticising the players, I am saying we as a group, the staff, the players, every single one of us in the club.
"If you don't share the urgency, you are not realistic. We are playing West Ham, Cardiff, Norwich, when are we going to win three in a row? Now. It has to be now.
"The idea was to double the points before January, so we have lost another opportunity today and somehow we had a normal performance in the first half and very poor in the second half. There is nowhere to hide."
Increasingly, it feels as if January might be the last salvation for Sunderland.
Although Poyet has been eager to try and make sure the Black Cats are focused on the points they can win before the transfer window opens, the manager has now admitted that he is hoping to strengthen the squad and there are "plenty of things" going on behind the scenes to try and recruit.
He said: "I am working on that for sure, that doesn't change my mind. We always thought there were positions we needed to address and there are plenty of things going on behind the scenes that doesn't change. I hope things will help. How big? I don't know because I don't know yet."
Lifting himself, never mind the players, will be the first order of business for Poyet this morning.
He said: "For me I analyse the game and ask the players to do the same. On Monday we are back and then we will reflect on everything and, like I said, keep convincing the players because from what I see they agree with plenty of things. When they do it right it works, but we need to do it all the time."
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redpajama_set_name: RedPajamaCommonCrawl


Gabrielle Roth was a dance and theater director, a shaman, a healer and a medicine dancer. Gabrielle witnessed her own process tuning in through movement and generously spread this work showing the way all around the world. 5Rhythms® reached tens of thousands worldwide and many teachers are carrying her legacy. We Sweat, we shed, we dance and we honor the 5Rhythms® of The Raven.


– The Parking Lot Movie (2010) Get it on Amazon.
– The Night Strangler (1973) Get it on Amazon.
– Missed Interesting Death of the Week with Hank: Farley Granger – Hitchcockian device.
– Interesting Death of the Week with B.K. – Sidney Lumet – legendary director.


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text:
DAWN - image of the day - December 2015
09.12.2015 - Dawn HAMO image 73 (PIA20136)
This view from NASA's Dawn spacecraft features a crater named Oxo, which is about 6 miles (9 kilometers) in diameter. A short, linear slump, where a mass of material has dropped below the surface, is seen to the left of Oxo's crater rim.
Dawn took this image on Oct. 17, 2015, from an altitude of 915 miles (1,470 kilometers). It has a resolution of 450 feet (140 meters) per pixel.
The Dawn mission to Vesta and Ceres is managed by NASA's Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, for NASA's Science Mission Directorate, Washington D.C. UCLA is responsible for overall Dawn mission science.
The Dawn framing cameras have been developed and built under the leadership of the Max Planck Institute for Solar System Research, Katlenburg-Lindau, Germany, with significant contributions by DLR German Aerospace Center, Institute of Planetary Research, Berlin, and in coordination with the Institute of Computer and Communication Network Engineering, Braunschweig. The framing camera project is funded by the Max Planck Society, DLR, and NASA/JPL.
More information about Dawn is online at http://dawn.jpl.nasa.gov.


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What Happens If The State Wants To Have A Surprise Witness Testify At Trial? - Roth Davies, LLC.What Happens If The State Wants To Have A Surprise Witness Testify At Trial? - Roth Davies, LLC.
State v. Coleman, 253 Kan. 335 (1993).
If a witness comes forth and wants to testify at trial, but wasn't on the witness list subject to the pretrial conference, can they still testify?
What factors will a court consider when a nondisclosed witness for the defense is called at trial?
The issue in this case includes whether the trial court erred by refusing to allow certain witnesses to testify solely for the reason that they were not listed on the pre-trial orders and, in addition, failed to consider the factors set forth in State v. Bright, 229 Kan. 185 (1981). 253 Kan. at 346. It is within the trial court's discretion, subject to exclusionary rules, whether to admit or to exclude evidence. Id. at 344. The defense counsel has no statutory requirement to disclose the names of defense witnesses prior to trial, with one exception for alibi witnesses. Id. at 347. However, the legislature authorizes pretrial conferences in criminal cases and this Court encourages their use. Id. If pretrial conferences are held "both parties are bound by the agreements made at the conference and included by the judge in the order entered at the conclusion of the conference." Id.
In the current case, the defendant argues that his right to present witnesses on his own behalf under the Sixth Amendment of the United States Constitution and his right to due process were violated through the refusal by the trial court to allow three unendorsed defense witnesses to testify. Id. at 343. Prior to the trial, the defense counsel signed a pretrial conference discovery document, which included a statement that the defense would provide an "exhibit and/or witness list … seven  days before trial." Id. at 346-47. The first unendorsed witness came forth the morning of the third day of trial and was to testify that she was an eyewitness to the shooting. Id. at 343. However, the trial court denied her the opportunity to testify and noted that the pretrial order was binding because the judge believed that this was exactly the kind of situation that the pretrial order was intended to prevent. Id. The trial court judge was unable to find evidence on the record to indicate that the witness was present at the shooting and no proffer was provided to indicate the substance of her testimony. Id. at 344. This Court noted that a "party may not assert error based upon erroneous exclusion of evidence in the absence of a proffer of that proposed evidence" and concluded that because there was no proffer of this witness' testimony, the trial court did not err in excluding her testimony. Id.
avoid imposing the severe sanction of prohibiting the calling of the witness if at all possible. This should be viewed as a last resort." 229 Kan. at 194.
Further, the Bright court noted that trial courts consistently permit the late endorsement of State witnesses, and this Court generally upholds those decisions. Id. at 192. This Court also previously held that late endorsements are normally permitted if the opposing parties are given time to interview the witnesses and cross-check their testimony. 253 Kan. at 349.
In the present case, this Court noted that the trial court made the decision to exclude the witnesses based on the quality of the evidence rather than the admissibility of the evidence, and thus, overstepped into the province of the jury by engaging in the role of factfinding and determination of witness' credibility. Id. 348. The Court thus concluded that the trial court erred by failing to apply the factors set out in Bright and that after application of those factors to the facts of this case, the proffered testimony from both of the witnesses should have been included at trial. Id. at 351. The Court considered specifically the following facts: both witnesses failed to come forth before the trial began – one due to fear, the importance of the substance of the purposed witness testimony, and whether the nondisclosure was willful. Id. at 350-51. The first witness was to testify that he was an eyewitness to the shooting and that he saw someone other than the defendant shoot the victim. Id. at 351. This Court determined that this testimony was crucial to the defense because it went to the ultimate question of who shot the decedent. Id. The other witness was to testify that she saw the decedent and the other suspect of the shooting together with a gun, prior to the fatal shooting. Id. This Court then reasoned that due to the substance of the testimony that would have been provided, the exclusion of both of the witnesses did not result in harmless error. Id. Further, when addressing whether or not the nondisclosure was willful, this Court turned to the fact that the defense counsel suggested a recess to allow the State to question the witnesses and thus would have eliminated the surprise element. Id. Finally, the Court noted that the trial court failed to consider any other options, and did not attempt to avoid the severe sanction of refusing to allow the defense witnesses to testify, which should have been seen as a last resort. Id. This Court then concluded that the trial court erred by failing to address the rules set forth in Bright and reversed the conviction of the defendant and remanded to the trial court for a new trial. Id.
Home » What Happens If The State Wants To Have A Surprise Witness Testify At Trial?


While fluorescence microscopy provides tools for highly specific labeling and sensitive detection, its resolution limit and lack of general contrast has hindered studies of cellular structure and protein localization. Recent advances in correlative light and electron microscopy (CLEM), including the fully integrated CLEM workflow instrument, the FEI CorrSight with MAPS, have allowed for a more reliable, reproducible, and quicker approach to correlate three-dimensional time-lapse confocal fluorescence data, with three-dimensional focused ion beam–scanning electron microscopy data. Here we demonstrate the entire integrated CLEM workflow using fluorescently tagged MCF7 breast cancer cells.
(…) both LM and 3D FIB-SEM data sets were loaded into the FEI Amira Software to allow for easy manipulation of the volumes and correlate information between both imaging modalities.
The EM data were first processed through the DualBeam 3D Wizard to register, crop, and filter the images from the stack. The LM data were intensity normalized across images, aligned, and filtered (AlignSlices; Gaussian filtering, Amira) before being volume rendered. To make the registration between LM and EM data sets easier, the LM data set was resampled to match the EM data set pixel size (x: 5 nm, y: 5 nm, z: 5 nm). LM and EM data were first registered manually in the multiplanar room, which allows loading and manipulating both data sets simultaneously from multiple viewing orientations. During that process, the LM data were loaded as the primary data and the EM data loaded as the overlay data. After a good coarse alignment was found, a refinement of the registration was initiated using the autoregistration options tab (Metric: Mutual Information; Transform: Rigid; Options: Extensive direction). For better results, an optimizer step equivalent to 1e5 voxels should be used. After registration, the volume rendering of the EM data was created, and a portion of the m-Slide where the cells were grown, the plasma membrane of the cells interacting with each other, two mitochondria, and a nucleus were segmented using the Amira Segmented editor. Segmentation was done using the magic wand segmentation tool and later cleaned up when needed with the brush tool. The registered, volume rendered, and segmented data sets were finally animated using the Amira Animation Director room.


Here's some advice to keep in mind when you're writing. Keep them in mind and they'll eventually become habit!
Always use a capital letter at the beginning of a sentence.
Sentences must end with punctuation. This is usually a full stop, question mark or exclamation point.
Okay, okay…I'm taking the dog for a walk!
Paragraphs are ways to organise the ideas in your writing. There are two ways to indicate the beginning of a new paragraph.
'Is not that rather a large thing to expect us to begin upon?' said Filby, an argumentative person with red hair.
Line space. A line space can also be used to indicate the beginning of a paragraph. This is often used in online communication and business letters.
Apostrophes are used to contract words and show possession.
Notice, when a word ends in 's', you can simply put the apostrophe at the end of the word to show possession.
Never use an apostrophe to show there is more than one of something. For example, you would write bananas not banana's.
Never use an apostrophe when writing about a decade.
Correct: It was the 1960s.
Incorrect: It was the 1960's.
Always use quotation marks around what is actually spoken.
Begin a new paragraph for a new speaker.
Begin each sentence with a capital letter.
"Did you bring your zebra to school?" he asked.
"I think I've left my zebra in the parking lot," he said.
Brackets should be used sparingly. They are usually used in a sentence to mention something that's an aside to what you're actually writing about.
In the titles of books, television programs, films and other texts the important words should be capitalised.
If you are writing acronyms, many leading style guides suggest that you don't use full stops. For example, it would be written TV, not T.V.. This is a modern way of punctuating acronyms.
The ampersand is a symbol for 'and'. Generally, it should only be used in very casual writing. You might use it for a note left on the refrigerator but you'd never use it in an essay, for example.
e.g. I went to the school.
e.g. He ate too much.
e.g. Are you coming, too?
e.g Only two people didn't finish the assignment.
e.g. We went through the doorway.
e.g. He threw the ball.
There. Used to indicate the location or existence of something.
They're coming to the party.
Never use smilies – 🙂 🙁 😛 – in a formal piece of writing. Similarly, don't use IM abbreviations like ur and roflmao.


text:
Friday, 04/27/2018, False Flag Weekly News with Dr. Kevin Barrett and Prof. Tony Hall
Friday 8 am Pacific * 11 am Eastern * 15:00 GMT.
All shows are archived here right after the web-stream broadcast.
Today's False Flag Weekly News is shown above Stop the Wars and Restore Our Civil Liberties
CLICK HERE to Keep Kevin on the Air
and to Support False Flag Weekly News
Help me keep doing False Flag Weekly News! I'm Kevin Barrett, co-host of False Flag Weekly News (FFWN) and I can no longer afford to keep doing this show for free. So we are going to have a separate fundraiser for each weekly episode. If we raise at least $200 by Friday, May 4th I will do that day's show. Anything over $200 per week will be donated to No Lies Radio/No Lies Foundation and Khidria, Inc., both 9/11-truth supporting registered 501(c)3 nonprofits.
Is False Flag Weekly News (FFWN) the world's best news show? Many people think so. Hosted by two Ph.D.s with expertise in history, global affairs, humanities, and other issues related to the phony "war on terror" among other scams, frauds, and deceptions, we cover the context behind the headlines to help you understand what's really going on. Unlike mainstream and pseudo-alternative media, we don't accept advertising. That's why we're free to "tell it like it is"!
So please support False Flag Weekly News! You can catch us live every Friday at 11 a.m. Eastern on http://NoLiesRadio.org – or watch the archived shows at https://noliesradio.org/archives/category/archived-shows/false-flag-weekly-news.
False Flag Weekly News is a weekly investigative news program that covers extremely controversial subjects. We want to remind our viewers that "Questioning" of Official Government or Mainstream Media Stories Is Not Hate Speech, nor is it Fake News, it is Free Speech that is protected by the 1st Amendment to the US Constitution.
Supreme Court unanimously reaffirms: There is no 'hate speech' exception to the First Amendment
Special Guest Host Today: Gregory Mccarron
The False Flag Weekly News anchored by Dr. Kevin Barrett and Prof. Tony Hall looks behind the headlines and main stream media stories to get at what's really going on in the world. From violations of international law to initiating WWIII, you don't want to miss what they and their guests have to say about the stories behind the stories. This weekly news show is broadcast live on YouTube and No Lies Radio every Friday morning 8am Pacific/11am Eastern. Thousands watch the show every week and rely upon us to reveal the naked truth behind national and world events that the main stream media is covering up. We take a no holds bar investigative reporter attitude even in our coverage of controversial events such as 9/11, the Boston Bombing, Sandy Hook, the Ukraine, the Paris Charlie Hebdo event, ISIS, and the more recent Paris and San Bernadino attacks.
TODAY'S NEWS STORIES AND THEIR SOURCE LINKS:
Do False Flags Actually Happen?
1) PSA:Help FFWN continue reporting on false
flags! https://fundrazr.com/91Livf
2) BBC:Anyone who uses the term "false flag" is a Russian
bot http://eaworldview.com/2018/04/russias-disinformation-warfare-and-assads-chemical-attacks/
3) From Reichstag Fire to Colin Powell's Anthrax Vial: Top 8 False Flags in
History https://sputniknews.com/military/201804201063765684-false-flag-attacks-in-history/
WTC Steel
4) Who exactly destroyed the WTC steel? And can they be held
accountable? https://www.ae911truth.org/news/450-who-exactly-destroyed-the-wtc-steel
5) Horse Soldier Bourbon's New Bottle is Made from World Trade Center Steel
https://www.themanual.com/food-and-drink/horse-soldier-bourbon-world-trade-center-bottle/
Embassy Move on Nakba Day: The Most Insane Genocidal Provocation in Human History
6) 40 Dead, 5,511 Wounded: (1499 injured with live ammunition) UN Releases Figures on Palestinian Casualties in Gaza's Mass
Protests https://www.haaretz.com/middle-east-news/palestinians/40-dead-5-511-wounded-un-figures-on-casualties-in-gaza-mass-protests-1.6030556
7) Ivanka Trump, Jared Kushner to attend Jerusalem embassy
move https://www.i24news.tv/en/news/international/172934-180422-ivanka-kushner-to-attend-jerusalem-embassy-move
8) When Nakba Day meets US embassy move day, expect fireworks in
Gaza https://www.timesofisrael.com/when-nakba-day-meets-us-embassy-move-day-expect-fireworks-in-gaza/
9) Another Day Another Mossad
Assassination https://www.richardsilverstein.com/2018/04/21/another-day-another-mossad-assassination/
10) Iranian president to Trump: Stay in nuke deal or face 'severe
consequences' (but Trump is scheduled to renig on Nakba
Day) https://www.politico.com/story/2018/04/24/iran-responds-trump-nuclear-deal-547523
11) Trump Warns Iran Of 'Bigger Problems' If Nuclear Program
Resumes https://www.rferl.org/a/trump-iran-nuclear-program/29189952.html
12) Iran's navy commander threatens to sink US
ships https://www.timesofisrael.com/irans-navy-commander-threatens-to-sink-us-ships/
13) NY Times offers uncommonly honest analysis of Saudi
Iranophobia https://www.nytimes.com/2018/04/23/opinion/international-world/saudi-iran-prince-mohammed.html
14) Russia to supply Syria "new missile defense
systems" https://www.cbsnews.com/news/russia-bashar-al-assad-syria-new-missile-defense-system-reports-s-300-system/
15) Boosting Syrian Air Defenses Will Scale Down US, Israeli Ambitions –
Lawmaker https://sputniknews.com/analysis/201804261063933619-syrian-air-defense-israel-us/
16) We May Hit Russian Systems in Syria, Israel Says After Threats of 'Catastrophic
Consequences' https://www.haaretz.com/israel-news/.premium-israel-may-hit-russian-systems-in-syria-defense-minister-warns-putin-1.6027919
17) Rothschild's Syria Oil
Play https://hendersonlefthook.wordpress.com/2018/04/25/rothschilds-syria-oil-play/
War on Korea
18) North Korea Suspends Nuclear And Missile Tests: State
Media https://www.huffingtonpost.com/entry/north-korea-suspends-nuclear-missile-test_us_5ada67f0e4b009869bf965e2
19) North Korea Declares Itself a Nuclear
Power http://thesaker.is/the-dprk-declares-itself-a-nuclear-power/
19a) Historic meeting between North & South Korea leaders kicks off
https://www.rt.com/news/425261-korea-summit-kim-moon-meeting/
Trump Coverups
20) Trump Continues the JFK COVER
UP www.washingtonpost.com/news/retropolis/wp/2018/04/26/trump-delays-release-of-some-jfk-files-until-2021-bowing-to-national-security-concerns/
21) Michael Cohen says he will plead the Fifth Amendment in Stormy Daniels
case https://www.usatoday.com/story/news/politics/2018/04/25/michael-cohen-says-he-plead-fifth-amendment-stormy-daniels-case/552183002/
22) Trump's past comments about pleading the Fifth look pretty ominous
now https://www.washingtonpost.com/news/the-fix/wp/2018/04/25/trumps-past-comments-about-pleading-the-fifth-look-pretty-ominous-now/
23) Will Trump have to plead the Fifth, re: "peed on by hookers"
story? https://www.youtube.com/watch?time_continue=1&v=UAwl9tVtob8
Bnai Brith/ADL lynchings
24) Selective Outrage At Its Finest: Zionist Character Lynchings of Black Men Keep on
Escalating https://www.timesofisrael.com/dc-politician-under-fire-for-anti-semitic-remarks-gave-500-to-nation-of-islam/
25) Bro. Abdul Arif Muhammad on Starbucks boycott, ADL history of anti-black racism and persecution of the Nation of
Islam https://www.patreon.com/posts/bro-abdul-arif-18338727
26) Premier Rachel Notley Honoured by B'nai Brith
Canada, http://calgaryherald.com/news/local-news/bnai-brith-hosts-premier
TechnoDystopia
27) Computer system transcribes words users "speak silently" (Can the government read our
thought-crimes?) http://news.mit.edu/2018/computer-system-transcribes-words-users-speak-silently-0404
28) Facebook too busy banning Veterans Today to catch fake Zuckerberg
swindlers https://www.nytimes.com/2018/04/25/technology/fake-mark-zuckerberg-facebook.html
29) YouTube Says Computers Are Catching Problem
Videos https://www.nytimes.com/2018/04/23/technology/youtube-video-removal.html
30) Victory: Virginia Supreme Court Delivers Blow to Police Use of
License Plate Reader Technology to Track Drivers Surveil Citizens https://mailchi.mp/rutherford/victory-virginia-supreme-court-delivers-blow-to-police-use-of-license-plate-reader-technology-to-track-drivers-surveil-citizens
Another Day, Another Weird and Senseless Attack
31) Toronto van attack: Not terrorism since the suspect wasn't Muslim — belonged to "guys who can't get laid rights
movement" https://www.theglobeandmail.com/canada/toronto/article-toronto-van-attack-what-we-know-so-far/
32) NAKED WAFFLE HOUSE SHOOTING: NUDE GUNMAN SHOOTS FOUR DEAD IN EARLY MORNING ATTACK IN
NASHVILLE http://www.newsweek.com/naked-man-shoots-three-dead-and-injures-four-early-morning-attack-nashville-896387
33) Will the West's rejection of God end in incel truck terrorists and
naked waffle house shooters? Solzhenitsyn's prophetic 1983
warning https://russia-insider.com/en/wests-rejection-god-will-end-misery-and-terror-solzhenitsyns-prophetic-1983-warning/ri23136
DR. KEVIN BARRETT, Chief News Anchor and Researcher–Dr. Kevin Barrett, a Ph.D. Arabist-Islamologist, is one of America's best-known critics of the War on Terror. Dr. Barrett has appeared many times on Fox, CNN, PBS and other broadcast outlets, and has inspired feature stories and op-eds in the New York Times, the Christian Science Monitor, the Chicago Tribune, and other leading publications. Dr. Barrett has taught at colleges and universities in San Francisco, Paris, and Wisconsin, where he ran for Congress in 2008. He currently works as a nonprofit organizer, author, talk radio host, an Editor at Veterans Today, and is a pundit on a number of international channels. He is the editor of We Are NOT Charlie Hebdo: Free Thinkers Question the French 9/11, an anthology that disputes the official story behind the January 7, 2015 Paris attacks, and the forthcoming ANOTHER French False Flag? Free Thinkers Question the 11/13 Paris Attacks.
JEREMY ROTHE-KUSHEL, Co-Anchor and Researcher — Jeremy Rothe-Kushel has a background in politics – from local to international, officeholder to activist – with experience in community organizing, mediajamming, documentary journalism and consensus-building in deep politics, economics and ecologics. Jeremy aims to coalesce a partisan-transcendent and permaculturally-informed #FullSpectrumPopulist #IntegralPolitics from the #RadicalMiddle with a #WeThePeoplePlatform and #CoalitionCabinet. He is working on a documentary project titled "September Eleventh Uncoverage" based on a decade of his investigative research, activism and experience of covering and uncovering the 9/11 cover-up. Rothe-Kushel has put public figures across the political spectrum "on the record" about vital issues that are often controversial and always emancipatory. Some of his journalistic encounters include Michael Hayden, John Yoo, Joe Biden, Eric Holder, Mike Pompeo, Kris Kobach, Ron Paul, Alex Jones, Jay Rockefeller, Ted Turner, Jill Stein and Amy Goodman. Jeremy has a working background in permaculture design and implementation, and future-roots music production, performance and education. While at Williams College completing his B.A. in Religion, he founded and over the next decade taught an original approach to musical education called "HipHop Empowerment", with students of diverse ages and backgrounds from the Bronx to Boston, Southern Vermont to South Los Angeles. Although he believes that well mineralized and microbialized, high-carbon humus might help solve most humanity's problems, Jeremy currently sees that the "invisible domain" of politics, culture, multimedia, law, deliberative deep democracy and cooperative startup economics contains key elements to assemble and strategic means necessary to that 'soilutionary' end.
PROF. TONY HALL, Co-Anchor and Researcher — Tony Hall is Full Tenured Professor of Globalization Studies in the University of Lethbridge in Alberta Canada. He has worked there for 25 years during which time he published articles in many venues including the Globe and Mail, the Toronto Star, Ottawa Citizen, the Canadian Encyclopedia, the Dictionary of Canadian Biography, Literary Review of Canada, Canadian Forum, Report on the Americas, American Indian Quarterly, Canadian Journal of Native Studies, Canadian Historical Review, Cultural Survival, Global Research.ca, International History Review, Anthropologica, Radicalpress, Voltairenet.org, and Veterans Today. He has made many presentations to Canadian parliamentary committees and has served as an expert witness on constitutional issues in several important legal cases in Canada and the United States. Hall comments frequently on Press TV. His critically acclaimed academic books include The American Empire and the Fourth World as well as Earth into Property: Colonization, Decolonization and Capitalism. Both are published by McGill-Queen's University Press. In his first public presentation on 9/11 skepticism, Prof. Tony Hall joined Dr. Barrett in 2008 on a podium in Edmonton Alberta. Along with the deceased Mohawk activist Splitting The Sky as well as Ramsay Clark, Cynthia McKinney, Joshua Blakeney and Kevin Barrett, Hall worked on a legal case derived from the principle that George W. Bush should have been arrested for war crimes when the former US President visited Calgary Alberta in 2009. Prof. Hall is a contributor to both of Dr. Barrett's dual volumes examining each of the false flag terrorist events in Paris in 2015. In December of 2015 Dr. Hall co-moderated with Dr. Barrett "False Flag Islamophobia Conference," a four hour academic conference webcast live on "No Lies Radio." Now Tony Hall joins Dr. Kevin Barrett as co-anchor of "False Flag Weekly News."
"The views and opinions expressed in False Flag Weekly News are the sole responsibility of the speaker(s) and do not necessarily reflect those of NoLiesRadio.org. NoLiesRadio.org will not be responsible or liable for any inaccurate or incorrect statements expressed therein."
Eyewitness to Florida School Shooting Says There Was Second Shooter
iBankCoin.com
'Full metal garb' – Teacher describes masked gunman at Florida school shooting.
Sott Media
On February 14th 2018 in south Florida, Marjory Stoneman Douglas High School teacher Stacy Lippel was 20 feet from a gunman firing 'barrages' of bullets into classrooms and down the hallway.
During an interview with ABC's Good Morning America, aired February 21st 2018, Lippel described what the gunman she saw looked like.
Officers LOADING HEAVY SATCHELS (weapons?) into back of pickup truck
start at 04:30
SGTreport
Marjory Stoneman Douglas High School in Parkland Florida–Testimony(multiple shooters)
Marjory Stoneman Douglas High School in Parkland Florida
PatrioticPepe
Las Vegas Shooting Multiple Shooters Police Scanner
GoodpixelProductions
Published on Oct 2, 2017
2:07 Hotel Security says shots fired on 29th and 32nd floors
2:19 Police Officer on the 32nd floor says "it's been confirmed that there are at least 2 shooters with fully automatic weapons"
2:29 Black Chevy rips out of parking lot (the shooting team?)
QUESTION: were there adjoining rooms that the real 2 shooters could have escaped through and perhaps they were dressed as LV police and could blend in with the police???
Could it be that Stephen Paddock was the patsy and was murdered before all the shooting began and his room was filled with guns to incriminate him. Case Closed.
This entry was posted on Saturday, April 28th, 2018 at 7:45 pm and is filed under 9/11, Agenda 21, Bio-Chem/Warfare, Censorship-Propaganda, Concentration Camps, Cyber-Drone-Space Warfare, Death Squads, Disaster Capitalism, Econo, Education, False Flag Weekly News, False Flag/Fake Terror, Freedom, Genetic Engineering - GMOs, Geopolitics, Globalism, Human Rights, Immigration, Justice, Kevin Barrett, Law, Martial Law, Mass Shootings, Media, Mind Control, News, Nuke War - Nukes, Occupation, Pedophilia, People, Police Brutality, Politics, Protest, Regime Change, Rendition, Russian propaganda Russian hacking, Social Engineering, Surveillance, Swine Flu, Torture, Vote Stealing, War Crimes, Weather-Earthquake Warfare. You can follow any responses to this entry through the RSS 2.0 feed.
3 Responses to "Friday, 04/27/2018, False Flag Weekly News with Dr. Kevin Barrett and Prof. Tony Hall"
Sound pretty damn delusional to me
maisoon
Just could not continue listening to the show- Guess McCarron was doing the work for BOC and Kushell. One big happy we love Jews club!!!McCarron might as well get a medal from AIPAC or Netanyahu for his tripe about how wonderful the majority all are.
You obviously live in a different world and it is you who are deluded
Your guest-Another Apologist for Jews
Just could not stop himself coming to the defence of Jews, making the usual excuses to whitewash their crimes
Why don't you all just start up a new club – Jewish Apologists with this guest, Kushel,Lindgrem and now BOC!
PITY McCarron does not defend the RACISM perpetrated on Gentiles
and KEVIN- I AM NOT DELUDED or immature
You are ALL APOLOGISTS NOW!!!


text:
El de Havilland Canada DHC-4 Caribou (caribú en inglés) (designación militar canadiense CC-108 y estadounidense CV-2 (Ejército) y C-7 (Fuerza Aérea)), es un avión de transporte táctico bimotor desarrollado y producido por de Havilland Canada con capacidad de efectuar despegues y aterrizaje cortos (STOL). El Caribou realizó su primer vuelo en 1958 y todavía restan algunos volando en algunas compañías aéreas secundarias.

Diseño y desarrollo

La decisión de construir el DHC-4 Caribou fue adoptada en 1956 con el objeto de desarrollar un avión que combinara la capacidad de transporte de carga del Douglas DC-3 y las prestaciones STOL del de Havilland Canada DHC-2 Beaver y del DHC-3 Otter. El Ejército canadiense efectuó un pedido de dos ejemplares; le siguió algún tiempo después el Ejército de los Estados Unidos, que solicitó cinco Caribou.

El prototipo realizó su vuelo inaugural en julio de 1958, y presentaba un ala alta caracterizada por una sección central con acusado diedro negativo. La puerta posterior fue diseñada a modo de rampa para manipular cargas que pesaran más de 3000 kg. En su cometido de transporte de tropas, podía acomodar hasta 32 soldados.

El Caribou prestó servicios con la Real Fuerza Aérea Canadiense designado como CC-108 y con el Ejército estadounidense como AC-1 (redesignado en 1962 como CV-2A). A consecuencia de la evaluación de los cinco primeros aviones, el Ejército estadounidense adoptó el Caribou como dotación estándar y realizó un pedido de 159 ejemplares. El segundo lote de aviones recibió la denominación CV-2B. A principios de 1963, cuando se suscitó el conflicto fronterizo entre China y la India, el Ejército de los Estados Unidos cedió dos Caribou a la Fuerza Aérea India. En enero de 1967, los 134 Caribou que todavía prestaban servicio en con el Ejército de los Estados Unidos, fueron transferidos a la Fuerza Aérea de los Estados Unidos, con las denominaciones C-7A y C-7B, para realizar funciones de transporte. En el servicio canadiense, el Caribou fue reemplazado por el De Havilland Canada DHC-5 Buffalo y los ejemplares excedentes se vendieron a numerosas naciones, entre ellas Colombia, Omán y Tanzania. Muchos de los aviones canadienses fueron prestados a la ONU para cubrir un extenso servicio internacional. La producción finalizó en 1973. El modelo DHC-4A reemplazó al DHC-4 en la línea de producción a partir del aparato número 24; ambos modelos eran muy similares, a excepción del aumento de peso máximo al despegue de este último, que pasó de los 11 973 kg a 12 927 kg. La producción total ascendió a 307 ejemplares.

Variantes

 DHC-4 Caribou
 Avión STOL de transporte táctico y utilitario.
 CC-108
 Designación de la Real Fuerza Aérea Canadiense dada al DHC-4 Caribou.
 YAC-1
 Designación dada a cinco DHC-4 Caribou, vendidos al Ejército de los Estados Unidos para evaluación.
 AC-1
 Designación del Ejército estadounidense dada a la primera tirada de producción de 56 DHC-4 Caribou. Redesignados CV-2 en 1962.
 CV-2A
 AC-1 del Ejército estadounidense redesignados en 1962.
 CV-2B
 Designación dada a una segunda tirada de producción de 103 DHC-4 Caribou, vendidos al Ejército estadounidense, con costillaje interior reforzado.
 C-7A/B
 Designaciones aplicadas a los 144 Caribou transferidos a la Fuerza Aérea estadounidense por el Ejército estadounidense.
 DHC-4A Caribou
 Similar al DHC-4, pero con peso al despegue aumentado.
 DHC-4T Turbo Caribou
 Conversión del DHC-4 básico propulsada por motores turbohélice PWC PT6A-67T; diseñada, probada en vuelo y certificada por la compañía Pen Turbo Aviation.

Operadores

Militares

 /
 Ala Aérea de las Fuerzas de Defensa de Abu Dhabi: cuatro DHC-4, para transporte y evacuación sanitaria. En 1971 se integraron en la Fuerza Aérea de los Emiratos Árabes Unidos, cuando Abu Dabi se unió a otros seis emiratos para formar los Emiratos Árabes Unidos.

 Real Fuerza Aérea Australiana

 Ejército del Aire de Camerún: tres DHC-4, sustituidos por DHC-5D a partir de 1981.

 Ejército del Aire de España: 30 DHC-4A. Tras los acuerdos de 1953 y convenios siguientes, en 1967 el Ejército del Aire contrató la adquisición de 6 ejemplares nuevos directamente con el fabricante, convirtiéndose en la única fuerza aérea europea en operar dicho modelo, que fue designado por el EdA como T.9. El primer avión llegó a España el 24 de diciembre de ese mismo año. En 1970, se compraron otros 6 ejemplares nuevos, y, a partir de 1981, se recibieron 18 aviones más, estos adquiridos de segunda mano a la Fuerza Aérea de los Estados Unidos (Guardia Aérea Nacional de Maryland). Los aparatos procedentes de la USAF, que se distinguían de los anteriores por ir equipados con un radar meteorológico en el morro, se consiguieron en buenas condiciones económicas, pero su estado operativo dejaba mucho que desear. Estuvieron en servicio hasta su sustitución por los CASA CN-235.

 Fuerza Aérea de los Estados Unidos

 Fuerza Aérea de Kenia: 4 DHC-4, que estuvieron en servicio entre 1966 y 1987 (nota: otra fuente, sin citar referencias, menciona seis ejemplares).

 Fuerza Aérea Kuwaití: dos DHC-4, que se recibieron en 1963.

 Ala Aérea del Ejército Liberiano: dos DHC-4 remozados fueron recibidos en 1989. Resultaron destruidos en la guerra civil.

 Fuerza Aérea Real Malaya: 18 DHC-4A. Sustituidos por seis CN-235 fabricados por PT Dirgantara Indonesia (antigua IPTN).

 Fuerza Aérea de Tanzania: 12 DHC-4 recibidos.

 Fuerza Aérea de Zambia: 5 DHC-4.

Gubernamentales

 Servicio de Vigilancia Aérea (Ministerio de Seguridad Pública): tres DHC-4A (C-7A) recibidos, de los que uno sólo queda en activo (MSP-002, número de serie 149), que fue sometido a una reparación en profundidad en 2010. Cuando sobrevino el conflicto por la invasión nicaragüense en Isla Calero, en 2010, el Caribou era el encargado de trasladar los guardias civiles hasta el aeropuerto de Barra del Colorado en el Caribe Norte, así como los alimentos y armas que se requerían para el resguardo de la soberanía. En uno de esos viajes, tuvo que aterrizar de emergencia y desde entonces no ha volado más. El 19 de junio de 2014 se informó que no volaría más.

Especificaciones (DHC-4A)

Aeronaves relacionadas

Véase también

 Anexo:Aeronaves históricas del Ejército del Aire de España
 Anexo:Aeronaves de la Fuerza Aérea de los Estados Unidos (históricas y actuales)
 Anexo:Aeronaves históricas del Ejército del Aire de España

Referencias

Bibliografía

 Enciclopedia Ilustrada de la Aviación: Vol.6, pag.1415, Edit. Delta, Barcelona. 1983 ISBN 84-85822-60-9
 Andrade, John. Militair 1982. London: Aviation Press, 1982. .
 The C-7A Caribou Association
 Caribou Roster  deHavilland Caribou (DHC-4) and Buffalo (DHC-5) website.
 "Caribou to Bow Out Early". Air International, Vol. 76. No. 4, April 2009, p. 5.
 Green, William. Macdonald Aircraft Handbook. London: Macdonald & Co. (Publishers) Ltd., 1964.
 Henley, Don and Ken Ellis. "Globetrotting Reindeers: De Havilland Canada's Caribou – an airlift legend". Air Enthusiast, No. 74, March/April 1998, pp. 20–33. .
 Hotson, Fred W. The de Havilland Canada Story. Toronto: CANAV Books, 1983. .
 Kuwait Air Force (KAF) entry at the Scramble (magazine) website:
 Malaysian Forces Overview entry at the Scramble magazine website.
 Royal Air Force of Oman entry at the Scramble magazine website.
 Soupart, Roger. "Adios Muchachas!". Air Enthusiast, No. 45, March–May 1992. pp. 44–51. .
 Taylor, John W.R. (ed.). Jane's All The World's Aircraft 1971–72. London: Janes's Yearbooks, 1971. .

Enlaces externos

 Web dedicada al DHC-4 y al DHC-5 (en inglés).
 The C-7A Caribou Association.
 "Handling the DHC-4 Caribou", un artículo de 1959 en Flight.

DHC-4
Aeronaves de ala alta
Aeronaves de cola cruciforme
STOL
Aviones tractores bimotores
Aeronaves civiles utilitarias de Canadá de los años 1950
Aviones de transporte militar de los años 1950 de Canadá
Aeronaves de transporte táctico
Guerra de Vietnam
Aeronaves de primer vuelo en 1958

redpajama_set_name: RedPajamaWikipedia


Metro's interactive, hands-on presentations teach middle and high school students about waste prevention and reduction. Presentations are approximately 50 minutes.
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Formerly titled Resource Consumption, this series of three middle school presentations delivered over the course of two to four weeks facilitate an in-depth examination of how we consume natural resources and provide students structure and accountability in tackling and measuring a specific behavior change they can make to conserve resources. This series will focus on the following three topics: ecological footprints, food waste, and conscious consumption.
Two presentations, delivered no more than one week apart, provide an overview of the science behind climate change, as well as its local and worldwide effects. The lesson invites students to be part of the "new story" of climate change, a story rooted in hope, consensus, community action, and increased quality of life. Students work together to analyze the connection between resource consumption and climate disruption, and discuss eight solutions from Paul Hawken's 2017 publication Drawdown to motivate them toward science-based personal actions and pledges.
In this one-day presentation, students will learn about the life cycle of our things from the extraction of natural resources to end-of-life disposal. Students will play an interactive game to learn the ins and outs of how to recycle correctly in greater Portland and explore how recycling can reduce negative environmental impacts associated with the production and disposal of our stuff.
Presentations include an activity and interactive discussion about actions students can take to reduce their impact on the environment and the earth's resources.
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BASSETERRE, ST. KITTS, MAY 5TH, 2017 (PRESS SEC) – The International Monetary Fund (IMF) commends St. Kitts and Nevis' strong economic performance amidst a difficult global economic backdrop. St. Kitts and Nevis' economy achieved 3.2% growth in 2016.
The difficult international environment has seen many nations struggle with constrained growth rates, including our major source markets for goods and services such as Canada (1.3% in 2016), Japan (1.0% in 2016), the United Kingdom (1.8% in 2016) and the United States (1.6% in 2016).
"Notwithstanding a difficult international environment, St. Kitts and Nevis' economy grew at a modest pace in 2016 and it is expected to grow again in 2017 for the fifth consecutive year," Ms. Inci Otker, the IMF mission chief on the 2017 Article Four (IV) Consultation to St. Kitts and Nevis, told the Press Unit in the Office of the Prime Minister, yesterday, Thursday, May 4th, 2017.
"Its growth performance in fact exceeded the average growth rate achieved by its peers in the ECCU region, which is quite impressive," the IMF official also said of St. Kitts and Nevis' economic performance in relation to the eight-member Eastern Caribbean Currency Union (ECCU) comprising Anguilla, Antigua and Barbuda, Dominica, Grenada, Montserrat, St. Kitts and Nevis, St. Lucia, and St. Vincent and the Grenadines.