text:
\section{Introduction}

Eighteen years after the first discovery of an exoplanet around a sun-like star \citep{mayor_jupiter-mass_1995} and
the unambiguous detection of three brown dwarfs \citep{basri_surprise_1995,
  nakajima_discovery_1995,rebolo_discovery_1995}, thousands of planets and brown dwarfs have been discovered. These numbers are growing ever
faster as the pace of new detections is increasing, thanks to newly built instruments purposely designed to search for
sub-stellar objects, but also to the optimisation of data analysis techniques.

The vast majority of exoplanets are currently detected with the radial velocity or transit techniques.
However, orbital periods longer than the time-span of the observations will hardly be
detected by these two techniques, inducing a sharp decrease in detectability beyond $\approx\,5$ AU and leaving unprobed a large area in
the mass-separation parameter space.
Direct imaging on the opposite probes the outer orbital regions not accessible with the two previous techniques, but the
high contrast at small separation which needs to be reached turns it into one of the most challenging exoplanet
detection techniques. The main hurdle to detect companions by high contrast imaging is to remove the stellar point
spread function (PSF)
without diminishing the signal from the faint companion.
This can be achieved through instrumental improvements
or by improving the observing and data reduction techniques, with efforts focusing on these two fronts concurrently.

Since the first planets around stars have been directly imaged \citep{marois_direct_2008, lagrange_probable_2009}, the
rate of exoplanets detected by direct imaging is steadily increasing
thanks to the progress made to overcome the many technical challenges and careful selection of the target samples.
But the small number of detections in total contrasts with the many direct imaging surveys which generated only few or no detection at all (e.g., \citealt{ masciadri_search_2005,
  biller_imaging_2007, lafreniere_gemini_2007, chauvin_deep_2010, heinze_constraints_2010, vigan_international_2012,bowler_planets_2012,
  nielsen_gemini_2013, wahhaj_gemini_2013, janson_seeds_2013, crepp_trends_2012}).

The technical challenge of subtracting the host star point spread function is currently based on two complementary differential imaging
methods, with the
same core idea of generating a point spread function as similar as possible to the one which should be subtracted, but without having any potential
companion signal in it. The difficulty being that the speckle structure of the point spread function evolves in time, with many speckles
in the stellar halo having a similar shape and intensity to what would be expected from a companion.
Two main differential techniques exist to detect thermal emission of a companion.
The first method, called Simultaneous Differential Imaging (SDI) is based on simultaneous observations in multiple bands. One can then either take
advantage of specific absorption bands of the companion so that it is visible in one band and not the other,
thus making it possible to subtract the PSF while keeping the companion signal, or use the fact that because speckles are chromatic, their pattern scales with the wavelength but the
potential companion stays on the same spot  \citep{racine_speckle_1999, lenzen_novel_2004}. The other differential method,
known as Angular Differential Imaging (ADI) is based on the rotation of the field
\citep{schneider_coronagraphy_2003, liu_substructure_2004, marois_angular_2006}, and has proven to be currently the most efficient method for point spread function
subtraction when searching for companions. These two methods do not require the use of a coronograph even though their use can increase the detection
limits in certain cases.
Finally, the two methods can be combined by letting the field rotate while observing simultaneously in multiple bands.
Nearly every survey developed its own reduction
pipeline most often based on either the Locally Optimized Combination of Images (LOCI) \citep{lafreniere_new_2007}
or more recently Principal Component Analysis (PCA) \citep{soummer_detection_2012, amara_pynpoint:_2012}.

Here we present the Geneva Reduction and Analysis Pipeline for
High-contrast Imaging of planetary Companions based on ADI for point spread function subtraction, which makes intensive use of Fourier
analysis. It was specifically developed for the Geneva high-contrast imaging search of
companions revealed by radial velocity trends in the HARPS and CORALIE survey.

\section{The Geneva high-contrast imaging search of companions revealed
by radial velocity trends in the HARPS and CORALIE surveys \label{sec:survey}}
Our campaign aims at detecting with direct imaging companions revealed by the RV trend they are
causing, based on data from our two CORALIE and HARPS RV planet-search surveys. The radial velocity data spans over more than a decade
with a precision reaching below 1 m/s in the case of HARPS so that trends induced by sub-stellar companions on wide
orbits can readily be
detected. The selected targets are observed using VLT/NACO and the angular differential imaging technique with deep
observations of up to four hours on target in order to reach the faint companions which had time to cool down.
Our targets are all bright which results in integration times below one second to reach saturation, and in order not to resort to
frame binning we are using the cube mode offered by NACO where frames are stacked into a data cube. Each cube containing
hundreds of frames is then saved into a single {\small FITS} file with the benefit of reducing readout overheads during observations.

\subsection{Parallelisation}

The NACO observation sequences of up to four hours used in our campaign lead to roughly 100GB of data and 100'000 frames. A straightforward single core
reduction would take an extremely long time and would run out of memory before finishing, due to the many complex
 operations involved in the data reduction mostly based on Fast Fourier Transforms ({\small FFT}).
The most widely used and easiest solution to this large data handling issue would be to average bin the data.

By suitably binning the frames, one can decrease the total amount of data to a quantity which fits the hardware limitations.
The drawback is that valuable information gets lost in the binning process. First of all, the characteristics of atmospheric turbulence are not constant in time
as well as the quality of the adaptive optics (AO) turbulence correction. The Strehl ratio for binned frames is the mean ratio of the frames in
the bin, so that if half of the frames have poor adaptive optics correction the final binned frame will also have below average Strehl,
even though the other half of the frames had good Strehl. Furthermore, binning frames before re-centring and correcting for the field rotation
smears out the companion point spread function which in turn decreases its signal in the final product. This is why we decided not to
rely on binning.

The different algorithms of our pipeline fit very well to a \emph{data parallelism} scheme, which focuses on distributing the data
across different parallel computing nodes. A master node shares the data between the slave nodes, which
only have a fraction of the data to process. Once the slaves have finished, the data are gathered by the master and reassembled.
Two different types of parallelisation are used, which differ on the way the data are shared between the nodes. If the
operations are pixel based, the spatial parallelisation scheme is used. In this scheme the data cube is cut in pieces
along the time axis, which means that each node receives one specific region of all the frames (see
\autoref{fig:data_para_spatial}).
The other scheme, temporal parallelisation, is used when the whole frame is needed for a specific operation. This is for
example the case for shifts and rotations. The data cube is then separated in frame packages, and each node receives a
different package containing full frames (see \autoref{fig:data_para_temporal}).

The pipeline is implemented in {\small PYTHON} using {\small C} and {\small FORTRAN} libraries for the calculation intensive parts.
The parallelisation is achieved using the \emph{Open Message Passing Interface ( {\small OPENMPI}}, \citealt{gabriel_open_2004}). Parallelisation can be distributed
transparently
among many different nodes, independently of their architecture. The interface between the {\small PYTHON} code
and {\small OPENMPI} is handled by the {\small MPI4PY} module \citep{dalcin_mpi_2008}.
All the data reduction steps given in this paper are parallelised, and based on the specificity of the process either in spatial or time parallelisation.

\begin{figure*}
\subcaptionbox{Spatial parallelisation\label{fig:data_para_spatial}}[0.3\textwidth]
{\includegraphics[width=0.3\textwidth]{column_cut.pdf}
}
\subcaptionbox{Time parallelisation\label{fig:data_para_temporal}}[0.5\textwidth]{
\includegraphics[width=0.5\textwidth]{cube_cut.pdf}%
}
\caption{The two different data parallelism schemes used by the pipeline. In spatial parallelism (a), the observation frames are
  cut along the time axis. Each node is then processing a different region of the frame. In time parallelisation (b), the frames are
  distributed among the nodes. In that case each node processes a different frame, or rather frame group.}\label{fig:data_paral}
\end{figure*}

\section{ADI data reduction}

The pipeline was initially developed to reduce non-coronographic saturated ADI observations in \textit{L'} band ($3.8\mu m$)
 from the CONICA 1024x1024 InSb Aladdin 3 detector which is part of the NACO instrument at the VLT \citep{lenzen_naos-conica_2003}.
It was later extended to process coronographic data from NACO,
GEMINI/NICI \citep{chun_performance_2008}, VLT/SPHERE
\citep{beuzit_direct_2010} and Subaru/SCExAO \citep{jovanovic_subaru_2015} in any band.

The concept of this pipeline is to preserve the companion photometry by relying on techniques which have the least
impact on the signal. Conservation of the noise structure is also a priority in order to carry out an efficient noise subtraction.
This is obtained by applying the geometric transformations for centring and rotation in Fourier space. Another important
aspect of the pipeline is the scalable parallelisation, which makes it possible to run it on anything
from a cluster for high performance computing (HPC) down to any modern laptop.

The reduction procedure is partitioned in four main parts, which will be described hereafter:
\begin{enumerate}
\item registration \ref{sec:registration}
\item image pre-processing \ref{sec:image_pre_processing}
\item PSF subtraction \ref{sec:psf_sub}
\item derotation \ref{sec:derotation}
\end{enumerate}

\subsection{Registration}\label{sec:registration}

The very first step of the reduction process is the registration. Every data frame is analysed
and a table is generated containing for every frame the time of exposure, the parallactic angle, the star centre and other
point spread function characteristics needed for the different reduction steps.
Even though the data cubes are not modified at this step, it is a key element of the reduction as any error on the angle
or star centre determination smears out the companion signal.

The registration process is also used to assess the quality of the adaptive optics correction for every single frame.
This quality estimate is then later used to keep only the best frames by manually setting the constraints on the frame quality selection.
This results in a kind of lucky adaptive optics.

\subsubsection{Parallactic angle}

The parallactic angle varies in time as the star moves in the sky, and its hour angle changes. Based on the
``Local Sidereal Time'' (LST) given in seconds in the FITS header, and the right ascension $\alpha$ of the star
(given in degrees), the hour angle $h$ is given by:

\begin{center}
\[
\centering
h= \frac{15\cdot {\mbox{LST}}}{3600}-\alpha.
\]
\end{center}

When observing with NACO in cube mode the frames are stored in data cubes of 30 to more than 500 frames, with only one
single header. This implies that the hour angle for each single frame cannot directly be derived
from the header, since solely one LST value is given.
Thus the observing time for every single frame has to be interpolated in order to get the correct parallactic angles, which
can become problematic when frame loss occurs.

\subsubsection{Star point spread function registration}
The determination of the star centre position is a complex task
particularly in the case of saturated point spread function and/or
coronographic imaging because the information at the core of the
point spread function is often lost. The determination of the cen-
tring method accuracy is also limited by the fact that the exact
point spread function centre is unknown. In order to make the
point spread function registration work on any combination of sat-
urated/unsaturated, full/coronographic, and AO/non-AO modes the
algorithm is split in a two stage process. First a basic centroid
search is done, and once the centroid is found a two-dimensional
function is fitted to the point spread function, which takes into ac-
count possible coronographic or saturated cores by masking out
pixels. This method also works if there is more than one star in the
field of view, as long as no other star has exactly the same flux as
the target.

The first step which is the centroiding algorithm searches for
a patch of contiguous pixels above a given threshold value. If the
patch size is within the range given by the user, the centre-of-mass
of the patch is calculated. These values are then fed into the point
spread function fitting algorithm as initial values.

The pipeline uses the following form of the \citet{moffat_theoretical_1969} function to fit the
point spread function centred on $x_0,y_0$:

\[
I(x,y,\alpha, \beta )=I_0\cdot\frac{\beta -1}{\pi
  \alpha^2}\cdot\left(1+\frac{(x_0-x)^2+(y_0-y)^2}{\alpha^2}\right)^{-\beta}+{\mbox{\small Bg}},
\]

with $\alpha$ the seeing radius parameter, $\beta$ the wing shape parameter, and {\mbox{\small Bg}} the value of the background flux \citep{trujillo_effects_2001}.
The full width at half-maximum (FWHM) of the point spread function is then given by the two fitting variables $\alpha$ and $\beta$:
\[
{\mbox{FWHM}}(\alpha, \beta )=2\alpha\sqrt{2^{1/\beta}- 1}.
\]

The Moffat fitting on the point spread function is achieved using lmdif's modified Levenberg-Marquardt algorithm which is part of the Fortran MINPACK library \citep{more_user_1980}.
The registration procedure achieves an accuracy better than 0.5 pixels on the star centre position, but its efficiency is highly dependent on the observational setup.

With the growing tendency to highly saturate the point spread function core or to use new generation coronographs, it becomes increasingly difficult to fit a Moffat function. A solution
to this is the usage of satellite speckles pioneered by \citet{sivaramakrishnan_astrometry_2006} using a reticulated wire grid, and recently brought to a new state of sophistication by
 \citet{jovanovic_artificial_2015} using
incoherent speckles generated with a pattern on the adaptive optics deformable mirror. Due to the chromaticity of speckles the satellites appear elongated on broad band imaging giving them
a shape which is difficult to fit with a conventional point spread function model. On the other hand, the centroiding algorithm is a good candidate to implement a registration
algorithm based on such satellite speckles.

\subsubsection{Frame selection}

In order to increase the signal to noise ratio of the companion, we keep only the frames with good adaptive optics correction. A
first rough selection is based on the centroiding algorithm, by simply discarding frames where no centroid has been found.

The second step is based on the point spread function geometry. When the detector integration time is more than a few seconds it can
happen that bad tip-tilt correction create a sharp elongated point spread function specially when in coronographic mode. Simple selection on
maximum signal strength hardly detects this kind of frames, even though
the point spread function shape is asymmetric. Using the values of the point spread function fitting has shown to be a robust way to verify the quality of
the adaptive optics correction. Alternatively the satellite speckles position and intensity can be used when available.

Furthermore, by using individual frame point spread function fitting instead of the widely used cross-correlation method, we can ascertain that only
good and optimally centred frames are used. The independent centring also ensures that poor centring on one frame will
not affect centring on the other frames.

Once the frame selection has been done an optional quick-look algorithm can be run which bins the re-centred good frames
to decrease the total number of frames to process in the following steps.

\subsection{Image quality pre-processing}\label{sec:image_pre_processing}

Image quality plays a key role when using Fourier transforms, because of the
\citet{gibbs_fouriers_1898} phenomenon. This phenomenon causes a chequerboard pattern to appear with pixels alternately
overshooting in the positive and
negative values around an image discontinuity, such as bad pixels, saturated point spread function or sharp image borders
 (\autoref{fig:gibbs}).
The reason for these oscillations is that a discontinuity would need infinite Fourier series to be correctly characterised, but
since we are dealing with finite discrete Fourier transforms the discontinuity is not well approximated.

\begin{figure}
\begin{center}
 \includegraphics[width=0.48\textwidth]{gibbs_phenomenon.pdf}
\caption{The single non-zero pixel surrounded by a background at zero (left figure) is shifted in
Fourier space by $\Delta x=0.3$, and $\Delta y=1.5$ pixels (right figure), resulting in the typical pattern of the Gibbs phenomenon.}
 \label{fig:gibbs}
 \end{center}
\end{figure}

The frame preparation is thus a key step in order to use Fourier-based operations, where no deviant pixel should be left
out. The two key steps for the image pre-processing are the sky generation and subtraction and the bad pixel correction.

\subsubsection{Master sky}

The sky background varies very rapidly when observing in the near infra-red especially in \textit{L'} band. Observations are done
in dithering mode in order to directly use the science frames to determine the sky background.
To decrease the effect of the star point spread function on the sky determination, a mask is applied on the region containing the star.
A median of \emph{N} time-contiguous cubes with \emph{N} different masked dithering positions is then calculated.
As dithering positions change every one or two seconds, and we are using four to five dithering positions,
a sky frame is produced for every five to ten seconds of observation. Using this method we manage to have a median sky as close
as possible to the sky background of the science frames.
Once the master skies have been generated, they are subtracted on each frame, using each time the
master sky frame closest in time.

\subsubsection{Bad pixel correction}

First a bad pixel map is generated using either a master dark or a master sky. A simple sigma clipping routine flags the
deviant pixels, where bad pixels are defined as a pixels
which values varies more than $C\cdot\sigma$ from the median value of the frame.
By changing the value of the $C$ coefficient the selection criteria can be adapted to ensure that all bad pixels are cleaned.

Since each bad pixel will be spread over many pixels as a consequence of the sub-pixel re-centring and the derotation
process, it is not possible to simply leave out a bad pixel.
Not to mention the Gibbs phenomenon such pixels would induce.
To clean the bad pixels, they are all first set to \emph{NaN}.
The bad pixel values are then replaced by the median of the neighbours, ignoring any \emph{NaN} pixels. This ensures that bad pixel
clumps are properly corrected.

\subsection{Point spread function subtraction}\label{sec:psf_sub}

The ``point spread function subtraction'' is the core of the reduction process. It is based on the well established ADI algorithm which
aims at subtracting the stellar point spread function and speckles by using the field rotation in order to
increase the sensitivity to surrounding point sources \citep{marois_angular_2006}.
We are generating a specific point spread function for every single frame, in a similar way to LOCI \citep{lafreniere_new_2007} but
without using any combination coefficients in an effort to preserve the flux.

For an observing sequence composed of $C$ datacubes containing each $N$ frames.
The total number of frames is then $T=C\cdot N$. The frame $f_i=(c_j;n_k)$ will have a parallactic angle
$\alpha_i$ given by
\[
\alpha_i=\arctan\left( \frac{\cos \phi \sin h_i}{\cos\delta\sin\phi - \sin\delta \cos\phi\cos h_i}\right),
\]
with $\phi$ the observatory latitude, $\delta$ the target declination, and $h_i$ the hour angle at observing time $t_i$.

A point spread function is generated for frame $f_i$ using the frames $f_x$ fulfilling the conditions on maximum time separation $t_{\mbox{max}}$
\[
\vert t_k - t_i \vert < t_{\mbox{max}},
\]
and  minimum field rotation $\alpha_{\mbox{min}}$ such that
\[
\vert \alpha_k - \alpha_i \vert > \alpha_{\mbox{min}}=2\cdot\sin\left(\frac{n_{\textsc{\tiny FWHM}}\cdot{\textsc{\tiny FWHM}}}{2\cdot r_{\mbox{min}}}\right),
\]

where $r_{\mbox{min}}$ is the minimum radius in pixels to consider, FWHM is the point spread function full width at half maximum from the
fitting (\ref{sec:registration}),
and $n_{\textsc{\tiny FWHM}}$ is the minimum number of point spread function displacements to prevent companion self-subtraction.

\subsubsection{Fourier shift}

All the geometric operations on the image are based on one and two dimensional Fourier transforms.
As a short reminder, we give the definition of Fourier transforms in two dimensions
of a function $f(x,y)$:
\[\label{eq:2d_fourier}
\hat{f}(\nu_x,\nu_y)=\iint^{\infty}_{-\infty}f(x,y)\cdot{\mbox{e}}^{-i2\pi(\nu_x x + \nu_y y)}dx dy,
\]
and its inverse Fourier transform:
\[\label{eq:2d_inv_fourier}
f(x,y)=\widehat{f}(\nu_x,\nu_y)^{\vee}=\iint^{\infty}_{-\infty}\widehat{f}(\nu_x,\nu_y)\cdot{\mbox{e}}^{i2\pi(\nu_x x + \nu_y y)}d\nu_x d\nu_y.
\]

The one dimensional case is a trivial simplification of the 2D case, and the notation for a one dimensional Fourier transform along the $x$ axis will
be noted by $\hat{f}(\nu_x,y)$, similarly the transform along the $y$ axis will be noted $\hat{f}(x,\nu_y)$.

To perform a shift of the image we use the translation property of Fourier transforms.
If $\widehat{f}(\nu)$ is the Fourier transform of the one dimensional function $f(x)$, then the Fourier transform of
$f(x+a)$ is $\exp(-i2\pi\nu a)\widehat{f}(\nu)$. Thus a spatial shift is equivalent to multiply the Fourier
transform $\widehat{f}(\nu)$ by a phasor ${\mbox{e}}^{-i2\pi\nu a}$. A shift along the $x$ axis in the two dimensional case
can thus be expressed as

\[
f_x(x+ a,y)
\int^{\infty}_{-\infty}{\mbox{e}}^{-i2\pi\nu_x  a}\widehat{f}(\nu_x,y){\mbox{e}}^{i2\pi(\nu_x x)}d\nu_x,
\]

and the more general case of a shift $a$ in $x$ and $b$ in $y$ is then obtained by a multiplication by a phasor ${\mbox{e}}^{-i2\pi(\nu_x  a+\nu_y b)}$:

\[\label{eq:2d_shift}
f(x+a,y+b)=\iint^{\infty}_{-\infty}{\mbox{e}}^{-i2\pi(\nu_x  a+\nu_y b)}\widehat{f}(\nu_x,\nu_y)\cdot{\mbox{e}}^{i2\pi(\nu_x x + \nu_y y)}d\nu_x d\nu_y.
\]

The frames we are re-centring are defined on a finite area, whereas the shift property holds for infinite domains. We can
nonetheless apply this operation to the frames provided we introduce a zero-padding which also prevents apparition of
Gibbs oscillations at the borders, but this implies that the operations have to be applied on at least double sized frames, which impacts significantly computational time.

\subsection{Derotation}\label{sec:derotation}
The final step of the ADI processing is to correct each frame for the field rotation and merge all the frames. In order
to preserve the companion signal, and also to keep the noise structure unchanged we perform the rotation using
Fourier transforms.

The rotation algorithm we are using is implemented by applying to Fourier transforms the property that a rotation
matrix can be decomposed in three shear matrices (e.g. \citealt{unser_convolution-based_1995, eddyy_improved_1996, welling_rotation_2006}).
This method is largely used in satellite imagery of the Earth and medical imaging. The galaxy image decomposition tool
GALPHAT is an example of its previous use in astronomical imaging \citep{yoon_new_2011}. We will only give a brief
description of the method based on the detailed
description of the algorithm given by \cite{larkin_fast_1997}.

Any rotation matrix $R_\theta$ of a given angle $\theta$ can be expressed as the product of three shear matrices:

\[
\underbrace{\begin{pmatrix}
  \cos\theta & -\sin\theta \\
  \sin\theta & \cos\theta
 \end{pmatrix}}_{R_{\theta}}=
\underbrace{\begin{pmatrix}
  1 & -\tan\frac{\theta}{2} \\
  0 & 1
 \end{pmatrix}}_{S_x}
\underbrace{\begin{pmatrix}
  1 & 0 \\
  \sin\theta & 1
 \end{pmatrix}}_{S_y}
\underbrace{\begin{pmatrix}
  1 & -\tan\frac{\theta}{2} \\
  0 & 1
 \end{pmatrix}}_{S_x}
\]

where $S_x$ and $S_y$ are shear matrices on the $x$ axis and $y$ axis respectively.

To shear by a factor $a=\tan\frac{\theta}{2}$ in the $x$
direction an image described by the function $f(x,y)$ we apply the transformation $s_x(x,y)=f(x+a y,y)$, which can be
readily adapted to Fourier transforms using their shift property. The shear matrix $S_x$ applied to the image $f(x,y)$
can then be expressed in terms of Fourier transforms as the function $s_x$

\[
s_x(x,y)
\int^{\infty}_{-\infty}\overbrace{\underbrace{{\mbox{e}}^{-i2\pi\nu_x a y}\widehat{f}(\nu_x,y)}_{\text{FT}}\cdot{\mbox{e}}^{i2\pi\nu_x x}d\nu_x}^{\text{IFT}}\ ,
\]

the product $S_y S_x$ becomes by noting $b=-\sin\theta$
\[
s_{yx}(x,y)=
\int^{\infty}_{-\infty}{\mbox{e}}^{-i2\pi\nu_y b  x}\widehat{s}_x(x,\nu_y)\cdot{\mbox{e}}^{i2\pi\nu_y y}d\nu_y,
\]

and the rotation $S_x S_y S_x$
\[
s_{xyx}(x,y)
\int^{\infty}_{-\infty}{\mbox{e}}^{-i2\pi\nu_x a y}\widehat{s}_{yx}(\nu_x,y)\cdot{\mbox{e}}^{i2\pi\nu_x x}d\nu_x
\]

Similarly to the shift case, the frames need to be padded. This implies that in order to rotate one frame 6 FFT have to be
applied on a double sized frame, resulting in a significant increase of computation time compared to standard interpolation methods.
This rotation technique can only be applied to such a large amount of frames thanks to parallelisation.

\section{Pipeline performance}

Contrast curves obtained for HD142527 observations with NICI, using {\small GRAPHIC} and PCA are displayed in \autoref{fig:nici_detlim}. At small separation we reach a higher contrast than PCA, while
the low-pass filtering from interpolation results in better contrasts at higher separation where the noise is mainly Gaussian.

To test the pipeline performance we developed an algorithm to inject fake companions. These companions are generated by
first including their signal into a plane wave-front which is then convoluted with a pupil based on the main optical
characteristic of the used telescope. Using this technique we have a precise control on the companion flux, and furthermore the point spread function
scales precisely with wavelength. Poisson noise is finally added to these nearly perfect point spread functions before adding them to the
real science frame.

\subsection{Performance of geometric transformations}

To characterise the performance of the shift and rotation algorithms, we generated a test image with fake companions.
This image is composed of an L' short-exposure image with a saturated point spread function, which has been sky-subtracted, cleaned from
bad pixels, and median-filtered.
To this image we added fake companions with magnitudes differences to the star reaching step-wise from 1 to 8 and with
separations from 0.5 to 6.5 arcseconds with arcseconds steps, and Poisson noise was included in the process.

To test the performance of the shift algorithm, we shifted the original image in a $\Delta x, \Delta y$ direction and
then shifted it back in the opposite direction ($-\Delta x, -\Delta y$). This double shifted image can then be compared with the
original non-shifted image. By subtracting the original image from the double-shifted, the
effects induced by the different shifting algorithms become visible. The dotted black line in
\autoref{fig:2shift_test_detlim} shows the normalised root mean square of the original test frame, calculated in concentric
annuli. The injected fake companions are causing the peaks at 0.5, 1.5, and 2.5 arcseconds. The two additional lines
show the root mean square of the difference between the original test frame and the double shifted frames, where the interpolation
and Fourier shift are represented by the blue dashed and red solid lines respectively. These two lines would
be flat with no root mean square if the shift algorithms were perfect. For the spline interpolation
this is clearly not the case, with the curve reflecting two phenomenons in and out of the peaks which are both caused by
the fact that interpolations in image space act as an uncontrolled low-pass filter. When the image is interpolated, the
structure of the noise is modified so that the high frequency noise is not removed by the subtraction, as it is missing
from the double shifted frame. This effect leaves an overall noise
continuum. The effect on the peaks comes from the fact that the fake companions are flattened by the interpolation, so that
part of the fake companion signal is not removed.

\begin{figure}
\centering
\includegraphics[width=0.5\textwidth]{detection_limit_3pipes.pdf}
\caption{Angular differential imaging detection limits for Gemini/NICI data in \textit{CH4-K5\%S} band, using a $0.22 \arcsec$
  semi-transparent coronographic mask
  with $\approx\,40\degr$ of field rotation. The three lines are detection limits at 5-$\sigma$.
  The black dotted line is the detection limit achieved by {\small GRAPHIC} before correction
  for self-subtraction while the red solid line is the detection limit of {\small GRAPHIC} corrected in order to take into account the flux loss.
  The blue dashed line is the detection limit using a principal component analysis pipeline which was used in \citet{casassus_flows_2013}.
\label{fig:nici_detlim}}
\end{figure}

\begin{figure}
\centering
\includegraphics[width=0.5\textwidth]{std_var_log_shift_comparison.pdf}
\caption{Root mean square representing the noise caused by the shift algorithms. As a reference the root mean square of the
  original image as a function of separation to the centre is given by the black dotted line. To test the algorithms we shift an image
  first by $\Delta x=3.5, \Delta y=2.7$ pixels and then back. The difference between the original image and the one shifted back to the
  initial position is then plotted for the interpolation and Fourier shift, blue dashed and red solid lines respectively.
\label{fig:2shift_test_detlim}}
\end{figure}

For the rotation algorithm we applied a similar test. We first rotated a test image by an angle $\alpha=11.3$ followed by a rotation
by an angle $-\alpha$. Ideally such a double rotation should return the original image. Changes in the image structure
induced by the rotation can be found by subtracting the original image from the double rotated one. The root mean square  as a function of separation to
the central point spread function of the
original image is plotted on \autoref{fig:2rot_test_detlim} with a black dotted line, and the subtracted rotations using interpolation
and Fourier shears are represented on the same figure by the blue dashed and red solid lines respectively.

The images from the rotation test are represented on \autoref{fig:10rot_test}, where \ref{fig:10rot_test}a is the
original image, \ref{fig:10rot_test}b and \ref{fig:10rot_test}c are the resulting image from the rotation followed by an
inverse rotation using interpolation and the 3-shear algorithm respectively. The most striking difference between the
two rotated images is the residual noise structure, the 3-shear algorithm preserving the noise structure while the
interpolation algorithm acts as an uncharacterised low-pass filter.

The different effects of the two rotation algorithms is even more evident when the original image is subtracted from the rotated images, as
can be seen on \autoref{fig:10rot_test}d for the interpolation and
\autoref{fig:10rot_test}e for the 3-shear algorithm. In the case of interpolation, the companions become dark blue
points surrounded by signal which means that the companion point spread function is spread, with signal being transferred from the centre of the point spread function
into the wings. The 3-shear residuals show no structure, indicating that the star and companion signals are not altered
by the rotation. Some numerical noise can be noted, but due to its very high frequency it can be filtered out without affecting the companion signal.

\begin{figure}
\centering
\includegraphics[width=0.5\textwidth]{std_var_log_inter_shear-orig.pdf}
\caption{
  Root mean square representing the noise caused by the rotation algorithms. As a reference the root mean square of the
  original image as a function of separation to the centre is given by the black dotted line. To test the algorithms we rotate the image
  first by an angle $\alpha=11.3$ and then back. The difference between the original image and the one rotated back to the
  initial position is then plotted for the interpolation and Fourier rotation, blue dashed and red solid lines respectively.
\label{fig:2rot_test_detlim}}
\end{figure}

\begin{figure*}
\centering
\includegraphics[width=1\textwidth]{double_rotation_test.pdf}
\caption{The original non-rotated test image is given in figure (a).
The result of two consecutive $11.3\degr$ and $-11.3\degr$ rotations of the original figure (a), using a third order spline interpolation, and the 3 shear algorithm are shown in figure (b) and (c) respectively. The residuals are computed by subtracting the original image from the
interpolation rotated (d), and three-shear rotated (e) images. All panels have the same intensity scale, except for figure (e)
where we reduced the cuts by a factor 20 to reveal some of the induced noise.
\label{fig:10rot_test}}
\end{figure*}

\subsection{Photometric accuracy}
Test data sets are created by injecting fake companions into all the raw frames with an angle following the field
rotation. By injecting the companions into the raw frames we are able to take into account nearly all the steps of the
reduction, namely image pre-processing, re-centring, point spread function subtracting, de-rotating, and final collapse. Centre and parallactic
angle determination are the only two operations we cannot test with this method, as the companion injection already
relies on these two parameters.

To illustrate the photometric accuracy we generated such a dataset using a 2 hour \textit{L'} NACO observation sequence with a
$120\degr$ field rotation, centred on the transit through meridian. The \textit{no binning} line in \autoref{tab:bin_flux} shows that in the
worst case we have a flux loss of 40 per cent, which is similar to what is achieved with the PCA pipeline {\small PYNPOINT} but better by a factor 2 compared to {\small LOCI} \citep{amara_pynpoint:_2012}.

Our ability to inject fake companions in the raw frames is thus a key component to recover accurate photometry. By
injecting the companions at the very beginning we can take into account all the effects that could decrease
the companion flux during the various data reduction steps.

\subsection{Effect of binning}

The data set used to quantify the photometric accuracy was also used to analyse the effect of binning. To study this effect
we binned the initial data set by combining each set of ten 0.2 second frames into a single median frame
resulting in a smaller data set. We did the same by also combining 50 frames into a single one representing 10 second total integrations per frame.

The three data sets were then reduced using exactly the same parameters. The resulting detection limits, along with retrieved photometry of the fake
companions are plotted in \autoref{fig:detlim_bin}. The detection limits increases beyond $3.5\arcsec$
because the result of dithering is that less frames are available at these separations which decreases the signal to noise ratio.

\begin{table}
\centering
\caption{Magnitude difference of the injected companions and percentage of the recovered flux as a function of separation and bin size.\label{tab:bin_flux}}
\begin{tabular}[t]{l  c r@{ -- } l  r@{ -- } l}
          & $1\arcsec$ & \multicolumn{2}{c}{$3\arcsec$} & \multicolumn{2}{c}{$5\arcsec$} \\\cline{2-6}
Injected $\Delta$mag & 8 & 8 & 10 & 8 & 10\\
Recovered no binning & 60\% & 81\% & 106\% & 71\% & 72\%\\
Recovered 10 frame bins &  52\% & 63\% &93\%  & 59\%& 20\%\\
Recovered 50 frame bins &  61\% & 66\% & 101\% & 60\% &52\%\\
\end{tabular}
\end{table}

The percentage of recovered flux of the fake companions is given in \autoref{tab:bin_flux}. Flux recoveries above 100\% are caused by low signal to noise,
for companions at or below the detection limit.

\begin{figure}
\centering
\includegraphics[width=0.5\textwidth]{bin_comparison.pdf}
\caption{Angular differential imaging detection limits for the same initial 2 hour observation sequence ($120\degr$ rotation). The injected fake
companions are represented by the black circles.
The non binned detection
limit and recovered companion flux are given by the red solid line and triangles respectively. The 10 frame bins are represented by the blue dashed
line and triangles, while the 50 bin results are given by the black dotted line and plus signs.
\label{fig:detlim_bin}}
\end{figure}

\subsection{Performance versus observation duration}

In order to test our observing strategy of long observations, we defined a specific test case. Taking one of our
nearly three hour
observation data set, we added fake companions to the raw images. The observation was then reduced using three different data set
sub-samples. For the first one we used the whole data set trimmed in order to have as much observing time before and after
transit at meridian. This results in a two hour data set, with one hour before and one hour after meridian transit.
We did the same for a one hour sub-sample and a 30 minutes sub-sample from the same initial data set, each time centred
on the meridian transit. The selected data set is of a star at a declination of $-17\degr$, which results in a smooth rotation rate.
Targets which are crossing the meridian at zenith will have the entire field rotation happening in only a few minutes.
For such specific targets the gain in sensitivity at small separation for longer observations will be very limited.

The resulting detection limits obtained by reducing the three sub-samples with exactly the same reduction parameters are plotted
in \autoref{fig:detlim_3times}. The detection limits clearly show that the reduction was tuned for the inner region within
0.5 arcseconds. At 0.3 arcseconds separation, the achieved magnitude difference are 7, 7.6, and 8 for 30 minutes, one hour,
and two hours respectively. At 1.5 arcseconds separation these limits become 9, 9.3, and 9.7. With two hour observations we
thus gain one magnitude in sensitivity with respect to a short 30 minutes sequence, and half a magnitude with respect to
a conventional one hour observation. A one magnitude difference in \textit{L'} band is what separates a 13 $M_J$ from a 20 $M_J$ companion,
based on \citet{allard_bt-settl_2014} at 1 Gyr.

\begin{figure}
\centering
\includegraphics[width=0.5\textwidth]{detection_limit_3times.pdf}
\caption{Angular differential imaging detection limits for an observation in \textit{L'} band of a 6.5 magnitude star at $-17\degr$ declination. The data sets taken from this sequence are all centred on
meridian transit using 30 minutes ($\approx 50^\circ$ rotation), one hour
($\approx 90^\circ$) and two hours sub-samples ($\approx 140^\circ$), plotted in blue dashed, black dotted, and solid red line respectively.
\label{fig:detlim_3times}}
\end{figure}

\section{Conclusions}

We have presented a new pipeline for angular differential imaging which is the first, to our knowledge, to perform the critical steps of image re-centring and field de-rotation in the Fourier domain and on individual frame. By doing so, we reduce most of the image smoothing introduced by interpolation and frame binning. The resulting image noise characteristic is also preserved. This theoretical approach is validated by several test cases, where we show that excellent dynamic range and  photometry retrieval are obtained at separations shorter than 1.5 arcsec compared to a standard PCA analysis.

In addition, we validated the observing strategy that consist in observing the same target for at least two consecutive hours with a clear boost in performances of 1 magnitude at short separations in the case of a target with a $120\degr$ rotation in 2 hours, representative of a typical ADI target. {\small GRAPHIC} is coded in python with a few C-modules and was designed to run on HPC clusters, with a minimum requirement of 2 cores and  4GB RAM per core. Provided the right environnement (48 cores, 192GB RAM), {\small GRAPHIC} is able to process up to 100'000 2048x2048 frames with no binning thanks to massive parallelism in 9 hours. This parallelisation of the pipeline makes it also possible to implement further computationally demanding algorithms. Further development is planned in order to use graphics processing units (GPU) for a gain in processing time and wavelet filtering. {\small GRAPHIC} has also very recently been adapted to process VLT/SPHERE and Subaru/SCExAO data. {\small GRAPHIC} has also been applied on an extended source with results published in \citet{casassus_flows_2013} under the development name {\small PADIP}.

\section*{Acknowledgements}
The authors would like to thank J. Carson for his refereeing work and for the
many useful comments he has given, and
D. Mawet for kindly providing PCA detection limits from \citet{casassus_flows_2013}.
J.H. is supported by the Swiss National Science Foundation (SNSF).
To develop the pipeline the author also made use of {\small SCIPY} \citep{jones_scipy:_2001}, {\small  NUMPY} \citep{oliphant_python_2007},
 {\small ASTROPY}
\citep{astropy_collaboration_astropy:_2013},  {\small BOTTLENECK},  {\small IPYTHON} \citep{perez_ipython:_2007}, and
 {\small MATPLOTLIB} \citep{hunter_matplotlib:_2007}.

\bibliographystyle{mn2e_fix}

\inputencoding{latin1}

redpajama_set_name: RedPajamaArXiv


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A dramatic and emotional story about one girl's determination to stand by her beloved animals – and her refusal to give up, even in the face of impossible odds.
As always I am overwhelmed with love and happiness after reading a Stacy Gregg novel. Not only did this book succeed in retelling such a devastating tragedy that befell the residents of Kaikoura, but it follows a twelve-year-old girl called Evie who takes a courageous and heart-warming journey with her dapple-grey pony, Gus, her dog, Jock, and her cat, Moxy. As well as choosing to traverse across the cracked terrain that the earthquake has created, Evie has to make some tough decisions when it comes to managing her OCD and none of it will be easy - mentally or physically.
For someone who never really knew too much about OCD, it has come as quite a shock to learn that I have more than a few of the same habits as Evie and actually have struggled with times where I broke down in a sobbing mess because I couldn't handle how dirty and untidy the house was. I always do things in twos or fours, but mostly eights because it's double four so it's more even. I had a habit as a child where I couldn't stop looking at the ground and making even steps on the pavement or I would take a million years to order my things in certain ways. These days I'd like to say that I don't suffer as much as I used to but I've found that things like ordering things when I'm stressed, wiping down the bench a million times for silly reasons or no reasons at all, or literally having a panic attack because the floor was so dirty at one point and we had no vacuum cleaner or broom to fix it. Basically what I'm saying is that if I hadn't of read this book, I wouldn't have realised that some of those things that I suffer with aren't exactly normal because my brain likes to make up stupid reasons to justify my repetitive or unusual behaviour. I'm not trying to say that I'm giving myself any reason to have OCD, I know it might look that way, but I'm grateful because now I understand why I'm so strange sometimes but I also know that it can be helped and changed. All I'm ever trying to do in life is improve my knowledge of things and improve myself as a person so this has really been somewhat of a great learning experience.
This middle-grade novel has it's light-hearted and encouraging moments where friendship between a girl and her pony or other pets mean absolutely everything, to the point where she will travel across dangerous terrain just to make sure that she can take her horse to safety aboard the HMS Canterbury. The reality of the Kaikoura earthquake is much fiercer and intimidating than what many might have thought if they had not have suffered through it. This was the case for me, being an Aucklander who was born in Christchurch but never had to suffer through a quake in my life because I moved by the age of one to the North Island. It is truly eye opening to read such a heart breaking tale where lives were actually lost and many people injured, animals left behind and houses destroyed. These tragedies are a common case with cities that sit on the fault line down the country but a lot of us in Auckland might shrug it off after a while because the news has stopped updating about it, yet families from the Christchurch quake are still without homes and money to this day. It makes me want to do something for both cities when I can finally earn some money that I can give.
'The Thunderbolt Pony' along with Stacy Gregg's last two novels, 'The Diamond Horse' and 'The Girl Who Rode The Wind'.
I recommend this novel to anyone who loves cute pony genre stories with a touch of reality that can open your eyes and teach you something new. I will say that this book needs a trigger warning for those who have OCD because I found myself becoming more aware of my habits and harder to kick them, but I'm monitoring it better now and letting my family know what I struggle with so that I'm not easily set off or I don't make the wrong impression. Other than that, I've given 'The Thunderbolt Pony' a 5 out of 5 star rating because it truly was one moving tale. This would also be perfect for parents to get for their children so they can learn more about the earthquakes in the South Island and have a lovely story to enjoy where pets are more than friends, they're also family.
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text:
A Russian Herbal
Traditional Remedies for Health and Healing
By Igor Vilevich Zevin
With Nathaniel Altman and Lilia Vasilevna Zevin
Published by Healing Arts Press
The first guide to the ancient traditions of Russian herbal medicine and their extensive medicinal applications today.
Drawing on a wealth of oral and written traditions, the authors examine the best-known Russian herbs (all of which are widely available in North America and Western Europe) and explain their folkways, properties, and uses. Offering time-tested advice for using herbs to maintain general well-being, they also give clear and simple recipes for treating specific health problems from asthma and migraines to influenza and high blood pressure. Blessed with a wide variety of climates, geography, and flora, early Russians developed a rich folk tradition of herbal healing that ranks among the most sophisticated in the world. Nearly every Russian medical school offers courses of study on the knowledge and application of herbs, and many maintain a special research department that investigates the properties and practical modern applications of herbal medicine.
This is the first book to examine the traditions of Russian herbal medicine.
Igor Vilevich Zevin
Born in Belorussia, Igor Vilevich Zevin was raised by his grandmother, an accomplished folk healer and herbalist who passed much of her knowledge to him. An engineer by profession, he has maintained his study of herbs over the years.
Publisher: Healing Arts Press (February 1, 1997)
Health & Fitness > Herbal Medications
Health & Fitness > Alternative Therapies
Health & Fitness > Healing
"The entries are also unusually detailed as to the exact methods of preparation as well as the parts of the plant that should be used. Potential dangers and other contraindications for use are clearly set out from the text in bold-faced type - a feature that I'd like to see copied in more herbals! Zeven with his co-authors, Nathaniel Altman and Lilia Vasilevna Zevin, have ceated a highly interesting and unusual herbal, detailing a tradition that we don't hear about enough."
– Rosemary Jones, owner of Healing Pages Bookstore
Book Cover Image (jpg): A Russian Herbal

redpajama_set_name: RedPajamaCommonCrawl


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The KOIN.com Top 10 wildfire stories of 2020
The wildfires erupted September 7, 2020
by: KOIN 6 News Staff
Posted: Dec 29, 2020 / 09:00 AM PST / Updated: Dec 28, 2020 / 05:36 PM PST
Clockwise from upper left: A fire engine from the Idanha-Detroit Rural Fire Protection District sits on Detroit Avenue Friday, Sept. 11, 2020, in Detroit, Ore., Kristopher Smith holds his dog Tripp outside his tent at an evacuation center at the Milwaukie-Portland Elks Lodge, Sunday, Sept. 13, 2020, in Oak Grove, Ore., Wyatt Tofte, This photo taken by Talent, Ore., resident Kevin Jantzer shows the destruction of his hometown as wildfires ravaged the central Oregon town near Medford. (Courtesy of Mark Ylen/Albany Democrat-Herald via AP, AP Photo/John Locher, Susan Vaslev, Kevin Jantzer via AP)
PORTLAND, Ore. (KOIN) — Oregon witnessed one of its most destructive wildfire seasons in recorded history in 2020.
Roughly 1.2 million acres were scorched, according to the state's office of emergency management. They left people homeless, destroyed timberland, and polluted the air for weeks. They also left many pondering the best ways to prevent a repeat of the devastation in the future. But that may become more difficult as the years go by.
A new study from Portland State University published in December 2020 showed that wildfires like the Riverside Fire that burned in the Molalla River Corridor will likely become larger and more frequent by mid-century under a warming climate.
Here are the top 10 most-read wildfire stories on KOIN.com in 2020:
#1: Up-to-the-minute maps, evacuations (September 8, 2020)
Hundreds of thousands of Oregonians were impacted by fast-moving wildfires that raged out of control starting in early September. As the state's leaders and emergency response crews leaped into action, we saw the need for a single no-frills story where viewers could find basic information about evacuation zones, emergency alerts and fire locations.
Fires and evacuations: Here's what you need to know
KOIN continued updating this one story for a full week (an editorial decision typically shunned in most circumstances) in an effort to help people stay up-to-date with the critical information they needed in a fast-moving situation understandably marked by panic, uncertainty and fear.
Infrared imagery of the Riverside Fire in Clackamas County, Sept. 11, 2020. (Clackamas County Sheriff's Office)
#2: A boy, his grandma and his dog (September 9, 2020)
The tragic reality of cataclysmic fire activity often includes the loss of human lives. Two of those killed during the 2020 wildfires were a 13-year-old boy and his grandmother.
13-year-old boy, grandma die in Lyons wildfire
Deputies said they found the remains of Wyatt Tofte and 71-year-old Peggy Mosso, as well as the remains of the family dog, inside of a vehicle on North Fork Road in the Santiam Canyon near Lyons. Volunteers had been searching for him since he ran from his home as the Beachie Creek Fire approached on the afternoon of Sept. 8. Marion County deputies confirmed the news to Wyatt's father the following day.
Wyatt Tofte and his dog Duke (Courtesy of Susan Vaslev)
#3: Bare-bones wildfire facts (September 11, 2020)
For the sake of accuracy and relevancy, we published a fresh story on Sept. 11 that included a list of the biggest fires in Oregon along with their acreage and containment.
Wildfires in Oregon: Names, locations, size, containment
We continued updating this story more more than a month, stopping only after fire officials said they were confident the largest fire — the Lionshead Fire — was controlled and unlikely to grow.
TOPSHOT – The melted sign of the Oak Park Motel destroyed by the flames of the Beachie Creek Fire is seen in Gates, east of Salem, Oregon on September 13, 2020. – The wildfire caused the evacuation of 40,000 residents, killing four people and five are still missing (Photo by Rob SCHUMACHER / POOL / AFP) (Photo by ROB SCHUMACHER/POOL/AFP via Getty Images)
#4. The air is really bad (September 10, 2020)
The wildfire smoke blanketed most of Oregon and made the air unbearable, made breathing outside dangerous. We posted a look at the U.S. Air Quality Index's interactive map, showing hazardous air quality conditions across Oregon.
MAP: Air quality conditions in Oregon
As the days went on and the air remained unbearable, KOIN 6 meteorologists continued to update the story and check the interactive map for accuracy.
A paddle boarder travels along the Willamette River despite heavy smoke on September 12, 2020 in Portland, Oregon. Multiple wildfires grew by hundreds of thousands of acres this week, covering large portions of the West coast in smoke. (Photo by Nathan Howard/Getty Images)
#5. Evacuation zones (September 13, 2020)
Although many evacuation zones shrank as the catastrophic wildfires began to be controlled, many remained in place as crews continued to battle wildfires across the state.
MAPS: Wildfires, evacuation zones around Oregon
At least 9 people were killed. More than 2,200 homes and 1,500 other structures have been destroyed.
Interactive maps were released from Oregon's Office of Emergency Management, Clackamas County evacuations, Marion County evacuations, Washington County evacuations, Lane County evacuations and air quality maps.
The Clackamas County Evacuation Zone as of 1 p.m., September 21, 2020 (Clackamas County Sheriff's Office)
#6. Get out, now! (September 8, 2020)
A State of Emergency was declared for Marion County and Oregon's Emergency Conflagration Act was invoked by the governor as wildfires ripped through the Santiam Canyon area of the county on September 8 — just a day after the wildfires began — prompting Level 3 "Go" evacuations for multiple communities.
'Go Now' evacuations ordered between Estacada, Woodburn
More Level 3 "Go Now" evacuations were issued after 6 p.m. that day for the area south of OR 211 between Estacada in Clackamas County and Woodburn in Marion County.
ESTACADA, OR – SEPTEMBER 14: Remains of a mobile home smolders at the Clackamas River RV Park on September 14, 2020 in Estacada, Oregon. Multiple wildfires continued to burn in Oregon as thousands remained evacuated across the West. (Photo by Nathan Howard/Getty Images)
#7. Towns empty out, looters move in (September 16, 2020)
Homeowners suffered huge losses as wildfires ravaged Clackamas County but not all the damage was caused by flames. Around 6:45 p.m. September 16, the Clackamas County Sheriff's Office released statistics of crime in the evacuated zones over a 7-day period:
Looters descend as fires empty Beavercreek homes
Between Sept. 8, 2020 and Tuesday morning, Sept. 15, the Sheriff's Office made: 13 arrests in Level 2 and Level 3 evacuation zones, with some suspects booked on multiple charges.
Matt Watts stands guard with firearms outside his home after wildfires and heavy smoke caused many of his neighbors to evacuate the area, in Estacada, Oregon September 12, 2020. – Many residents are concerned looters are breaking homes left empty by people fleeing the fires. Dense smog from US wildfires that have burnt nearly five million acres and killed 27 people smothered the West Coast on September 12. (Photo by Robyn Beck / AFP) (Photo by ROBYN BECK/AFP via Getty Images)
#8. Shelters opened right away (September 9, 2020)
Shelters opened up around Oregon as wildfire infernos fueled by dry winds ripped through hundreds of thousands of acres across the state in a "once-in-a-generation event," according to Gov. Kate Brown.
LIST: Temporary shelters as wildfires rip through Oregon
As of September 11, an estimated 500,000 resided in evacuation zones, with 40,000 forced to flee their homes. Since the fires erupted September 7 temporary shelters opened across the state.
The Red Cross provided support and assistance throughout the state.
The human-caused Riverside Fire, burning southeast of Estacada, is about 40,000 acres large as of Wednesday afternoon, Sept. 9, 2020 (KOIN)
#9. Fear of fires merging (September 10-11, 2020)
Clackamas County officials warned of "severe and extreme fire behavior" and urged all county residents to be prepared to evacuate even if they were currently in Level 1.
2 'rapidly growing and changing' fires set to merge near Molalla
The extreme fire conditions were fueled by winds, which were pushing the Riverside and the Beachie Creek Fire in Marion County together.
"The fire conditions in Oregon and Washington are probably the most extreme we have ever seen in our lifetime," Oregon Fire Marshal's Lance Lighty said during a press conference in Clackamas County.
Business owner Cory Repucci of Lyons was evacuated when the Beachie Creek Fire roared through Marion County, September 14, 2020 (KOIN)
10. Evacuation area grows quickly (September 9, 2020)
Just 2 days after the fires erupted, Level 3 "Go Now" evacuations were still being declared across Clackamas County, including the city of Estacada, as infernos fueled by dry winds continue to devastate communities.
Level 3 evacuation area grows in Clackamas County
Authorities expanded the Level 3 evacuation area around 9:30 p.m. September 9 to include all of Eaden Road and west to S Harding Road, as well as a small area west of Beavercreek Road which includes all of S Gard Road and Unger Road to the first part of Windy City.
The entire city of Estacada was ordered to evacuate around 1:30 p.m. that afternoon as first responders struggled to control several wildfires in the area, including the large Riverside Fire.
Flames rage on as crews work to contain the Riverside Fire in Clackamas County. (Photo courtesy: CCSO)
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More Wildfires Stories
Replanting well underway in burned areas of Santiam State Forest
by Amanda Arden / Jan 13, 2021
PORTLAND, Ore. (KOIN) -- The Santiam State Forest is on the road to recovery after the Beachie Creek, Lionshead, and Riverside wildfires damaged approximately 16,600 of the forest's 47,465 acres.
At a State Forests Advisory Committee meeting Tuesday, Oregon Department of Forestry officials said crews are now in the process of salvaging burned timber and replanting the forest.
'We're still here': ODF remains in Lyons after wildfire destroys office
PORTLAND, Ore. (KOIN) -- When an inferno roared through the Santiam Canyon in early September, no structure was guaranteed to survive -- not even the Oregon Department of Forestry's office in Lyons.
The building burned to the ground.
Road to wildfire recovery starts with seedlings, but capacity is strained
by Hannah Ray Lambert / Jan 10, 2021
MARION COUNTY, Ore. (KOIN) -- Nursery workers are moving fast in Hubbard to get conifer seedlings shipped off to customers, and the wildfires that burned roughly 1.2 million acres in Oregon have given them a new sense of urgency, since millions of trees need to be replaced.
However, with limited capacity to grow new trees, it's a process that's expected to take several years.
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The Smart fortwo is the first commercialized car to have full body panels made from polypropylene.
Borealis Ag in Austria developed Daplen ED230HP, a thermoplastic polyolefin (TPO) compound, to meet the cost-effective production targets and aesthetic, safety and environmental requirements set by Smart fortwo designers.
Daplen ED230HP replaces polycarbonate polybutyleneterphtalate (PCPBT) that traditionally serves in body panels, such as bumpers, side panels, tailgates, and hoods. To ensure a smooth transition to the new material, Borealis worked closely with Smart and their Tier One supplier Plastal to provide engineering and simulation support in addition to the material development.
The TPO is an in-mass colored compound: Colors are blended into the compound to provide a ready-made base coat. As a result, post-assembly painting steps are reduced with only a painted clear coat layer needed. The UV resistant TPO adheres well to paint and thus helps ensure quality aesthetics over the long term. But if the vehicle is damaged, owners will see lower painting costs when it's repaired.
The lightweight TPO also let designers shave 15% off the vehicle's weight which will in turn help reduce fuel consumption and carbon dioxide emissions. Furthermore, the material is fully recyclable in line with European legislation.
Daplen ED230HP's low thermal expansion creates zero gap tolerance between parts. The material's good impact/stiffness ratio for the injection molded panels leads to improved driver safety.
"Smart's pioneering approach to using polypropylene for full body panels in its fortwo series is a major step forward for the automotive industry and its suppliers," says Paul Turner, Vice President of Automotive and Appliances at Borealis. "Daplen ED230HP helped Smart tighten its production process while raising the environmental, aesthetic, and safety performance of its vehicle."


The dramatic antique black finish seems to enhance the subtle details at the corners of this beautiful cabinet. Slight fluting within half circles is a creative addition. A simple leg shape. Three removable shelves within the interior which is given a natural finish.


What's So Good about Good Friday? asks Episcopal priest Justin Holcomb in a recent article. The origin of the term, he says, is debatable, but "Regardless of the origin, the name Good Friday is entirely appropriate because the suffering and death of Jesus, as terrible as it was, marked the dramatic culmination of God's plan to save his people from their sins….all in accordance with what God had promised all along in the Scriptures." We can all agree, can we not, with the gross understatement that people have been sinning since time immemorial? But….
DIDN'T THE ANCIENTS EVER WONDER?
too wondrous to keep to Himself. Flesh forward.
But, inevitably, Adam and Eve stray.
They have a bad day.
'Twas the serpent, they say.
if the creator was in need of saving from His own?
Did my poem blaspheme, or did it pose a serious question (or did it blaspheme in posing a serious question)? Does your answer depend on whether you believe in an ALL-PERFECT, ALL-LOVING GOD, a MIGHT-MAKES-RIGHT GOD, or NO GOD at all? How far would you go to try to convince or force (as if belief can be forced) others to believe as you do? Isn't it sad enough when members of one family can't agree to disagree, much less the human family writ large? How much longer would you and your god have the world pay the price of religion's aggressive side?
Peace, however awkward, be with you on this Good Friday.
Most of us never get it.
It's not as if we run out of time.
could he have handled more than he feared not to believe?
know what you don't know — what is there to be learned?
The answer, my friend, is growin' in the womb….
the surreal promise of perpetuity born in real time.
….that is the question. And the only reason I ask it is because I came across this believable deist T-shirt website (notice I didn't say unbelievable, because deists do believe in a creator of the universe — they just don't believe he has been seen since setting it in motion….or Day One, if you prefer).
Now, whatever hidden agenda the creator may have, I have none here. Far deist from me to try to convert anyone. If you got religion, God bless you, and happy praying (you can even include me in your prayers if you think it enhances your and/or my chances of eternal bliss or whatever, but I don't buy it).
Than hope for the best.
The above pretty much encapsulates religion for me as a natural antiphon to the question of human existence. It is only logical to assume that there is not only a reason for life, but a creator of it. From those conclusions, lacking direct knowledge — possibilities become suppositions, suppositions become mantras, mantras become answers, answers become beliefs, and beliefs become truth: religions, collectively speaking.
Well, life does exist….unless you and I and J. K. Rowling and billions of other passers-through are figments of some creator's imagination — which, I suppose, is a possibility. As for the rest, revelations are a dime a dozen, and, bargains though they be, I'm buying none of them.
And that, my friends, is why I'm a deist (just in case anyone's curious).
Perhaps you saw the story, reported by Associated Press writer Michael Rubikam, on 07/06/10. The headline was an attention grabber: Widow lives with corpses of husband, twin. It was the kind of headline that, save for the limited attention-span generation, won't let you not take time to read the story behind it.
It seems that a 91 year old widow in rural northern Pennsylvania, Jean Stevens, had the embalmed corpses of her late husband and twin sister dug up and placed in her garage and house, where she could look at and talk to them. After someone revealed this to authorities and had the bodies removed, the story reports that "She knows what people must think of her. But she had her reasons, and they are complicated, a bit sad, and in their own peculiar way, sweet." They come across as the reasons of, not an unbalanced or pitifully ignorant person, but of a thinking, if somewhat eccentric, person.
In the first place, people can be spiritual without being religious, and in the second place, Stevens doesn't deny death – she deals with it in her own way. Just because Mrs. Stevens' way isn't Dr. Lavretsky's way is no reason to put down the former from on high.
Somehow I can't help but feel that I could have a much more engaging, thoughtful and human conversation with Mrs. Stevens than with Dr. Lavretsky. One thing I know for certain – I would much rather give a great big hug to Mrs. Stevens.
Shortly after I became an ex-Catholic, my non-Catholic son-in-law asked why I'd remained in the Church so many years. Off the top of my head, I replied that I was brainwashed. I could've added that, possibly, that was the same reason he remained ideologically conservative all his life.
Yet, I doubt that such an observation would have led him to consider re-examining his own thinking. In my experience, even very intelligent people like him seldom change their mindset – they're so invested in what they've been and where they are. And, to be honest, maybe it's just as well.
We can theorize that self-questioning of entrenched views would lead automatically to a better place. Granted, it could lead you to a more open place, a wiser place, but a better place (if you equate better with more comfortable), probably not. There is nothing comfortable about realizing that everything you believed (or, at least, hoped) was gospel, is not. I would hate to think I caused someone I love to abandon their black & white comfort zone for a gray area they may not be equipped to face. An evangelizer, I am not. But if I were, I would challenge you to ask why you don't challenge at least some of your own assertions.
Even I'm not right 100% of the time.


You've rehearsed, you're prepared and still the week before, the day before and the morning of your big presentation, you feel that growing pit in your stomach, the sweaty palms, and the faster the minutes tick by, the worse it gets.
How do you deal with this (normal) nervousness, which can make you feel quite ill?
As part of the theatre rehearsal process for my Portland and New York City performances, I'm coaching myself through pre-performance jitters and talking to experts about how to handle the butterflies, which can sometimes feel more like winged dinosaurs flapping around my stomach.
Pay attention to the audience. If during your presentation, you start to feel self-conscious, this can make you feel more disconnected and thus, more nervous. When this has happened to me in the past, I turn my attention outward to focusing on the audience or on the story I'm telling. Even noticing the feeling of my feet on the ground helps. It takes me out of my head and into my body which helps me feel more grounded and present.
Give the nervousness a new name. According to Miller, the physical sensation that I interpret as nervousness is similar to the feeling of being exhilarated. It's just that I'm interpreting this feeling and labeling it "awful." But when I feel the butterflies, I can also say to myself, "Oh, that's me being exhilarated. How exciting!" Miller explained that the more I try to push my feelings of nervousness away, the bigger the feelings will feel. "Welcome the sensations, have gratitude for them," he said.
Don't believe everything you think. Sometimes when I'm nervous, I start to think about all the possible things that could go wrong and my mind is very ingenious coming up endless worst-case scenarios. Miller suggests that I don't pay so much attention to the content of my thoughts but instead "look at the mind like a busy freeway." This echoes the reading I've done by Sharon Salzberg where she teaches a form of noting. So rather than listen to the content, I just label it "thinking" or "remembering" or "forecasting" and nothing to worry about!
Let me know what's working for you to calm your nerves as you prepare for your next speech, pitch or presentation. I'd love to hear. Comment here.


Dimensions 2015 , 14th Annual Sculpture Show of the National Capital Network of Sculptors.
A highlight of the show is a silent auction to raise funds for the Ottawa Boys and Girls Club.
Members of the public will also have the opportunity to watch sculptors demonstrate a variety of sculpting techniques on Saturday and Sunday — a great opportunity to see how sculptures are made using a wide variety of techniques and media.


text:
Larry Buchanan
Writer Larry Buchanan
Movies by Hollywood Writer Larry Buchanan
In this page you can found only Movies written by Larry Buchanan, by clicking on each Larry Buchanan you can see other details like Larry Buchanan biography, Larry Buchanan movies, Larry Buchanan pictures and much more exclusively on bollyviews.com.
Writer Larry Buchanan Biography
Name: Larry Buchanan
Movies Written by Larry Buchanan
English 1967 N/A Larry Buchanan 2020-04-25
Goodnight, Sweet Marilyn
The supposed story of superstar Marilyn Monroe's death...as told by a "friend" of hers. Watch flashbacks from "Goodbye Norma Jean" as it leads up to the night when Marilyn Monroe died....
English 1989 93 min Larry Buchanan 2020-03-30
Down on Us
The story of Jimi Hendrix, Jim Morrison, and Janis Joplin, and how their message for their generation made them targets of a US government plot....
English 1989 117 min Larry Buchanan 2020-03-30
Mistress of the Apes
The wife of a famous anthropologist is rushed to hospital in labor. At the same time, druggies raid the hospital looking for drugs, causing the baby to be stillborn. While recovering from ......
The Loch Ness Horror
An increasing number of people are dying mysterious deaths in the dark waters of Loch Ness, victims of the famous monster. But what other mysteries does the Loch hold? What about the ......
Hughes and Harlow: Angels in Hell
When maverick first-time director Howard Hughes has to recast the female lead in his aerial war picture, he chooses a fiery, unknown movie extra named Jean Harlow, launching both of their Hollywood careers in the process....
Goodbye, Norma Jean
Aspiring actress Norma Jean Baker lives in squalor in the early '40s as she works at the munitions plant and dreams of being a movie star. Abused as a child and an adult, she lacks ......
Strawberries Need Rain
Death comes to take a beautiful young girl, and she persuades him to let her live out her fantasies before he finally takes her away....
The Other Side of Bonnie and Clyde
Comanche Crossing
Mars Needs Women
Dop leads his fellow Martians to Earth on an interplanetary quest for females. Dop proves that Martians have impeccable taste when one of his first conquests turns out to be sexy scientist Dr. Marjorie Bolen....
High Yellow
Cynthia Wood, a light-skinned 17-year-old girl, tries to pass as white after getting hired by wealthy movie magnate Mr. Langley, who has problems with his spoiled wife and promiscuous teenage daughter and son....
The Trial of Lee Harvey Oswald
A film that speculates how Lee Harvey Oswald's trial may have played out had he not been killed by Jack Ruby....
Naughty Dallas
A small-town girl comes to Dallas to make it as a stripper....
A trial melodrama about a mother who encourages her 14 year old daughter to have sex with a 16 year old Mexican boy....
Free, White and 21
The central conflict in this film is whether African-American businessman Ernie Jones (played by O'Neal) raped Swedish immigrant and civil rights Freedom Rider Greta Mae Hansen (played by ......
The Naked Witch
A student researching the German settlements of Central Texas unearths the grave of a reputed witch. The witch (who happens to be both beautiful and naked) rises from her grave and embarks ......


The situation with surviving in amongst dynamics, as many of us do, is there are little creatures which can be always standing inside the wings willing to munch away on the fabric with the building. Without a doubt, many of which are undetectable for the naked eye however, if the person is aware what they are seeking, they might find several evidence across the place. There are usually experts on this field who is able to come inside and handle the problem quickly but they should be compared together with others which offer related services. Try trying to find termite handle operatives online to find out who gets the most modern day methods accessible. Indeed, termite bug control is is now high-tech today therefore it is well worth having a look.
Most folks will know the most common methods regarding eradicating these kinds of creatures. This requires digging any deep trench across the building and also pouring in a few rather dangerous chemicals to attempt to put upwards a barrier involving the creature as well as the food source which can be usually your house itself. Nonetheless, this obviously doesn't work when the particular building is at the city or elsewhere has several historical value with it.
These days there exists a good means of ensuring the building itself just isn't damaged, or the lands that encircle it. It requires sinking in a few long tubes in to the ground with regular intervals across the whole constructing and gaining a easily-removed cap. In the tubes can be a feeding station the location where the bait will be laid. A great operative can monitor these kinds of feeding areas and, using a mobile computer, record which bait will be eaten and which can be not.
Clearly, those tubes which can be seeing action will probably be monitored a lot more closely since here is the track the insects are employing. To understand why, one will have to know something with the behavior of the creatures.
The nesting can rest several hundred or so meters far from the foods source, which is, the building which it wants to be able to invade. Within the particular nest could be the queen that is the only person who can produce younger. The staff and scouts provides food on her behalf since the lady never results in the nesting.
When the particular workers and also scouts locate a good foods source, they set down scent hiking trails for pursuing creatures to get where you might get food as opposed to building a lot more tunnels. Without a doubt, it will be this habit which can be their demise in the long run. After ingesting the poisoned bait, they acquire some back for your other workers as well as the queen that will eventually perish. When the lady dies, the complete colony can die also since simply no new toddlers are born to exchange others that have died.
This system is currently being used throughout the states and is seen around traditional buildings just about everywhere. The tubes be in situ for your foreseeable future in the event there will be another break out sometime afterwards. With this at heart, everyone should take a peek and notice if this kind of cleaner and also greener approach can remove these creatures once and for all.


text:
Q: How to use NSUserDefault with PickerView in Swift? I made some Labels that change using PickerView. But when I change the Label and if I run my app again, it doesn't save to selected one. So I have to use NSUserDefault but I don't know how to use it in right way.
This is my code:
var selectedFood = 0

class ViewController: UIViewController, UIPickerViewDelegate, UIPickerViewDataSource {

@IBOutlet var foodLabel: UILabel!
@IBOutlet var labelTwo: UILabel!
@IBOutlet var labelThree: UILabel!

@IBOutlet weak var foodPicker: UIPickerView!

var food = ["Bread", "Pizza", "Pasta", "Hot Dog", "Burger"]

@IBAction func submitLanguageButton(sender: AnyObject) {
    if (selectedFood == 0) {
       foodLabel.text = "Bread"
       labelTwo.text = "Bread is a staple food prepared from a dough of flour and water..."
       labelThree.text = "Bread is one of the oldest prepared foods..." // I used random information just as sample
    }
    else if (selectedFood == 1) {
       foodLabel.text = "Pizza"
       labelTwo.text = "Here will be more informations about Pizza"
       labelThree.text = "A fact about Pizza"   // I used random information just as sample
    }
    else if (selectedFood == 2) {
       foodLabel.text = "Pasta"
       labelTwo.text = "Here will be more informations about Pasta"
       labelThree.text = "A fact about Pasta"    // I used random information just as sample
    }
    else if (selectedFood == 3) {
       foodLabel.text = "Hot Dog"
       labelTwo.text = "Here will be more informations about Hot Dog"
       labelThree.text = "A fact about Hot Dog"  // I used random information just as sample
    }
    else if (selectedFood == 4) {
       foodLabel.text = "Burger"
       labelTwo.text = "Here will be more informations about Burger"
       labelThree.text = "A fact about Burger" // I used random information just as sample
    }
}

override func viewDidLoad() {
  super.viewDidLoad()
  // Do any additional setup after loading the view.

    foodPicker.delegate = self
    foodPicker.dataSource = self

    if (selectedFood == 0) {
       foodLabel.text = "Bread"
       labelTwo.text = "Bread is a staple food prepared from a dough of flour and water..."
       labelThree.text = "Bread is one of the oldest prepared foods..." // I used random information just as sample
    }
    else if (selectedFood == 1) {
       foodLabel.text = "Pizza"
       labelTwo.text = "Here will be more informations about Pizza"
       labelThree.text = "A fact about Pizza"   // I used random information just as sample
    }
    else if (selectedFood == 2) {
       foodLabel.text = "Pasta"
       labelTwo.text = "Here will be more informations about Pasta"
       labelThree.text = "A fact about Pasta"    // I used random information just as sample
    }
    else if (selectedFood == 3) {
       foodLabel.text = "Hot Dog"
       labelTwo.text = "Here will be more informations about Hot Dog"
       labelThree.text = "A fact about Hot Dog"  // I used random information just as sample
    }
    else if (selectedFood == 4) {
       foodLabel.text = "Burger"
       labelTwo.text = "Here will be more informations about Burger"
       labelThree.text = "A fact about Burger" // I used random information just as sample
    }
}

func pickerView(pickerView: UIPickerView, titleForRow row: Int, forComponent component: Int) -> String? {
    return food[row]
}

func pickerView(pickerView: UIPickerView, numberOfRowsInComponent component: Int) -> Int {
    return food.count
}

public func numberOfComponentsInPickerView(pickerView: UIPickerView) -> Int {
    return 1
}

func pickerView(pickerView: UIPickerView, didSelectRow row: Int, inComponent component: Int) {

    selectedFood = row
}

}

So when I choose Pizza, whenever I run my app I want to be it Pizza, if I select another one for example Pasta, I want to be that one Pasta.
Can you please help me ?

A: WBMDDrugManagerErrorCodeSave the selection like so:
func pickerView(pickerView: UIPickerView, didSelectRow row: Int, inComponent component: Int) {
    NSUserDefaults.standardUserDefaults().setInteger(row, forKey: "choosenFood")
    NSUserDefaults.standardUserDefaults().synchronize()
    self.setLabelsForChoice(row)
}

Retrieve the chosen selection like so:
override func viewWillAppear() {
    super.viewWillAppear()
    if let previousSelection:Int = NSUserDefaults.standardUserDefaults().integerForKey("choosenFood") as? Int{
        self.setLabelsForChoice(previousSelection)
    }
}

Create a label update method similar to this:
func setLabelsForChoice(_choice:Int){
    switch _choice{
        case 0:
            foodLabel.text = "Bread"
            labelTwo.text = "Bread is a staple food prepared from a dough of flour and water..."
            labelThree.text = "Bread is one of the oldest prepared foods..."
            break
        case 1:
            foodLabel.text = "Pizza"
            labelTwo.text = "Here will be more informations about Pizza"
            labelThree.text = "A fact about Pizza"
            break
        default:

            break
    }

}

redpajama_set_name: RedPajamaStackExchange


text:
Q: INSERT INTO TARGET_TABLE SELECT * FROM SOURCE_TABLE; I would like to do an INSERT / SELECT, this means INSERT in the TARGET_TABLE the records of the SOURCE_TABLE, with this assumption:
The SOURCE and the TARGET table have only a SUBSET of common columns, this means in example:
==> The SOURCE TABLE has ALPHA, BETA and GAMMA columns;
==> The TARGET TABLE has BETA, GAMMA and DELTA columns.
What is the most efficient way to produce INSERT / SELECT statements, respecting the assumption that not all the target columns are present in the source table?
The idea is that the PL/SQL script CHECKS the columns in the source table and in the target table, makes the INTERSECTION, and then produces a dynamic SQL with the correct list of columns.
Please assume that the columns present in the target table, but not present in the source table, have to be left NULL.
I wish to extract the data from SOURCE into a set of INSERT statements for later insertion into the TARGET table.
You can assume that the TARGET table has more columns than the SOURCE table, and that all the columns in the SOURCE table are present in the TARGET table in the same order.
Thank you in advance for your useful suggestions!

A: In Oracle, You can get common columns with this SQL query:
select column_name
  from user_tab_columns
 where table_name = 'TABLE_1'
intersect
select column_name
  from user_tab_columns
 where table_name = 'TABLE_2'

Then you iterate a cursor with the mentioned query to generate a comma separated list of all values returned. Put that comma separated string into a varchar2 variable named common_fields. Then, you can:
sql_sentence := 'insert into TABLE_1 (' ||
                 common_fields ||
                 ') select ' ||
                 common_fields ||
                 ' from TABLE_2';
execute immediate sql_sentence;


Do you know how your average salary increases stack up in your geographic region? Are you paying a higher or lower percent of medical insurance premiums compared to other companies of a similar size? Where does your retirement plan match rank in your industry?
For these potential differentiators in talent retention – and in recruiting efforts – visibility into how your business' averages fit in your market segments is critical for hiring and employee engagement success. This knowledge is also an important consideration for strategic planning to gain an edge in a highly competitive job market.
These factors work in concert to create a benchmarking profile for participant clients and their comparisons. For example, a client in the northeast U.S. region can compare metrics against averages for other companies in that region. In addition, clients have the flexibility to compare themselves to any other markets of interest.
All clients who volunteer their data to contribute to the pool for calculating averages qualify to access and enjoy Ascentis Benchmarking. The data are sourced anonymously so clients cannot isolate the data from any particular contributing company. In addition, all aggregated data are fully encrypted to ensure anonymity.
Ascentis Benchmarking software is a comparative analytics tool that enables executives and HR leadership to view current values for key metrics and assess how they measure up against standards for comparative markets.
measurement and whether that value is above or below the overall norm. From that top level visual, the user can select any individual metric (i.e., Average Salary Increase or Benefits Spend per Employee) to explore the rich data in more detail, to include year-over-year trending and filters to isolate specifics. All data in Ascentis Benchmarking are refreshed monthly and will automatically update all dashboard views.
Company profile for benchmarking – including assigned region, industry, and size, each of which can be overidden for modeling purposes.
Data may be filtered to further understand the benchmark. Users can select different time constraints (i.e., 3, 6, or twelve months) and all comparative charts will dynamically refresh to expose data that aligns with the filters.
Ascentis employee benchmarking software is a comparative analytics tool that enables companies to view key metrics and assess how they measure up against standards for their markets.
View a quick snapshot for each metric of measurement and whether that value is above or below the overall norm.
Users can select any individual metric to explore and isolate specific data.
Data from opt-in clients is anonymous and fully encrypted to ensure anonymity.


text:
Information by country and territory
Canada and Montserrat
Services for Canadians if you're visiting, studying, working or doing business in Montserrat. Includes information about coming to Canada.
COVID-19: Travel guidance
All travellers, regardless of citizenship, must meet specific requirements when coming to Canada. For information on COVID-19 and travel, visit COVID-19: Travel, testing, quarantine and borders.
Travel advice and advisories - Montserrat
Avoid non-essential travel
Travel advice, passport and entry requirements, health and safety information, and more.
Coming to Canada
Apply to immigrate. Get a visa to study, work or visit Canada.
Travelling outside of Canada
Travel advice for how to stay safe and returning to Canada.
Everything you need to know to prepare to leave Canada to live in a foreign country.
Canada-Montserrat relations
Canada's diplomatic, economic or cultural relationship with Montserrat.
Doing business in Montserrat
Business opportunities, market and sector advantages and other insights.
COVID-19: Your safety and security outside Canada
Registration of Canadians Abroad
Find a Government of Canada embassy, high commission or consulate
Office card
High Commission of Canada to Barbados, in Bridgetown
Address: Bishop's Court Hill, St. Michael, P.O. Box 404, Bridgetown, Barbados BB11113
Service(s) provided at this office:
We also provide services to Canadians in:
Anguilla, Antigua and Barbuda, British Virgin Islands, Dominica, Grenada, Montserrat, Saint Kitts and Nevis, Saint Lucia, Saint Vincent & the Grenadines, Sint Maarten.
Trade Commissioner Service office in Bridgetown, Barbados
Address: The High Commission of Canada, Bridgetown, Barbados, Bishop's Court Hill, Bridgetown, BB 11000, Barbados
Trade and investment services
Barbados, Anguilla, Antigua and Barbuda, British Virgin Islands, Dominica, Grenada, Guadeloupe, Martinique, Montserrat, St. Kitts and Nevis, St. Lucia, St. Maarten, St. Vincent and the Grenadines
Canada and Montserrat news (Canada news)
Canada and Montserrat news (Local statements)
High Commission of Canada in Barbados
@CanHCBarbados
High Commission of Canada to Barbados and the OECS


text:
A story and a yarn
Ian Stephen
Ian Stephen was born in the Isle of
Lewis, Scotland where he lives today.
A former coastguard officer, he won
the Robert Louis Stevenson award in
1995, and represented Scotland in
Canada as part of the Scottish Poetry
Library's Commonwealth Poets united series in 2014.
Of the following tale, he says, "I heard this from Chrisella
Ross, in
, Stornoway, November 2013. My
retelling is based on memory and some handwritten notes.
She ascribed the original source as one Lachlan Mor (mac
Dhomhnaill
ic Mhuirich) one of the dynasty of
MacVurichs, bards to Clanranald.
"The role of Clanranald features strongly in the learned,
illustrated travelogue of Professor Murdo Macdonald; this
resource is a generous sharing of the author
s personal
recollections. These are brimful with cultural references
ranging from the culture of seafaring to a summary of the
marks that artist-makers have left in the landscape of the
Highlands and islands, over centuries."
0 … 109 110 111 112 113 114 115 116 117 118 119 120 … 215 FlippingBook


sectors: IT, IT Security, Consumer Goods, Trading, Medtech, Watches.
Pascal has contributed greatly to our efforts in electronic communications both internally and externally. Always a pleasure to work with, his talents and skills are invaluable in implementation and executing. Pascal plans carefully and communicates thoroughly, always focusing on the various sides of dynamic developments.


From platinum bars to toilet paper, the NIST Museum has a diverse collection of objects and scientific instruments that relate to NBS/NIST tales of success, failure, and ingenuity. The Museum aims to extract these stories from the artifacts themselves and present them in a way that resonates with people. Central to this effort is drawing together resources from an artifact collection with assets dating back 250 years, library holdings spanning 482 years, more than 50 years of oral histories, and relevant archival materials.
At present, only NIST staff, associates, their registered guests, and conference attendees are able to tour the Museum. Tours can either be self-guided or led by the Curator; contact museum@nist.gov to make arrangements. The campus is not open to the general public.


text:
When It Makes Sense To Think Like A Nazi
When everything becomes sanitized, the collectivist vision of utopia will have been realized.
That's why a teacher in Albany, N.Y., is in hot water over an English assignment that required her students to "think like a Nazi." Students in Albany High School English classes were assigned a paper that required them to watch and read propaganda put out by Nazi Germany.
They were then instructed to make a decidedly politically incorrect argument. The teacher wrote in the assignment: "You must argue that Jews are evil, and use solid rationale from government propaganda to convince me of your loyalty to the Third Reich!"
In five paragraphs, students were to pretend they were German citizens facing persecution if they could not persuasively argue to a Nazi official that Jews were the source of Germany's problems.
The students were also instructed to incorporate the Greek philosopher Aristotle's elements of an argument into their paper: "Logos" (persuasion by reasoning), "Pathos" (persuasion by emotional appeal) and "Ethos" (persuasion by the author's character).
While the teacher's assignment may seem extreme, the skill the educator was trying to impart to the students is a valuable one: knowing why an idea is wrong by going to great lengths to understand why some people consider it kosher.
But considering an idea from all sides of the debate is not something that public education has been interested in doing for many years. The general purpose of public education is not educating students, but pumping out obedient and politically correct subjects of the state.
And don't forget, in Germany circa 1930s Nazism was representative of the state.
By encouraging her students to take the position of an oppressed citizen forced at gunpoint to go along with the will of the state, the teacher risked revealing a lot about how people unthinkingly end up on the wrong side of history by enabling oppression.
http://personalliberty.com/2013/04/1...k-like-a-nazi/


ESL schools in New York metro area: Business English courses in Newark NJ, intensive English courses in NYC area for professionals, executives, corporate English training for businesses, companies. Study English classes for medicine, law, sales, marketing, curso de inglés comercial / para negócios en New Jersey, EEUU.
Learn Business English in New Jersey! The Harvest English Institute is a quality English language school with campuses in Newark and Long Branch, New Jersey. Our Newark institute is just minutes away from midtown Manhattan providing students with easy access to everything New York City has to offer. We offer a range of courses for students who need to improve their English skills for business or professional purposes.
Designed for intermediate and advanced level students, our Business English course targets the acquisition and improvement of the students' business English language skills.
The course is carefully balanced and structured to teach non-native adult speakers, and to help them to gain confidence speaking English in a professional environment.
By the end of the course, students should recognizing and using a wide range of business communication structures and vocabulary, enabling them to function in an ever-demanding business world.
Students who do not hold an F-1 student visa can take our Business English course privately. You can schedule as many hours as you need to fulfill your expectations, and meet your learning goals.
If you do hold a student visa, you can take this course as an Elective after completing our general intermediate level 4 course.
Eustis, Florida; Orlando, Dominican Republic; Newark; Orlando Florida; Bloomfield; Caracas, Venezuela; Philippines; new jersey; Newark NJ; Guayaquil, Ecuador; and more.
You are here: School & College Search> English Language Schools in USA> Business English courses in New Jersey (Newark / Long Branch).


text:
On-Field Services
Tenants and Leasing
Drake Field has a unique history behind it that has roots dating back to the early 1900s. In 2010, J. B. Hogan, a native of Fayetteville, and the late Kirby L. Estes wrote a piece in "Flashback", a journal of the Washington County Historical Society. J. B. Hogan is a prolific writer and Kirby L. Estes served as Poet Laureate of Fayetteville from April 2006 to April 2007. Below we have provided the article which is dedicated to the memory of Glenn D. Estes, the first flight service station chief at Drake Field and father of Kirby Estes.
This article is used by permission of the authors and the Washington County Historical Society and it was written by J.B. Hogan and Kirby L Estes. Originally published in the WCHS "Flashback" Volume 60, Number 2, Summer 2010.
Read "Flashback: Early History of Fayetteville Municipal Airport" by J.B. Hogan and Kirby L. Estes
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Drake Field
4500 S. School Avenue
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