text:
\section{Introduction}

   \begin{figure*}
   \centering
   \includegraphics[angle=-90,width=18cm]{FIGURE1.ps}
   \caption{OSIRIS NAC images used in this work. All the images
     are oriented North up and East to the left. The lower labels in
     each image indicates the observation date. All images are
     30$\times$35 pixels. Their spatial dimensions at the comet
     can be calculated
     using the spatial resolution indicated in the last column of
     Table~\ref{table1}. The straight features near the diagonals
     in the uppermost first and third panels from the left are artifacts.}
              \label{FIG01}
    \end{figure*}

   Comets are among the least processed objects in the solar system, which means that   their study provides insights into their origin and evolution. The Grain
   Impact and Dust Accumulator (GIADA) \citep{Colangeli09,
     DellaCorte14}
and the Optical, Spectroscopic,
   and Infrared Remote Imaging System (OSIRIS) \citep{Keller07}
   on board the ESA Rosetta spacecraft have been in operation in the
   vicinity of comet 67P/Churyumov-Gerasimenko (hereafter 67P) since March
   2014. The OSIRIS camera started to
   provide images of the comet since March 23, 2014 \citep{Sierks15,Tubiana15a},
   while the first measurements carried out by GIADA
   were performed on July 18, 2014, when the comet was at heliocentric
   distances of 4.3 au and 3.7 au, respectively.

Combining these OSIRIS and GIADA early
   single grain measurements,  \citet{Rotundi15} derived the dust
   environment in the 3.7-3.4 au range, which  agrees with
   model predictions by \citet{Fulle10} at 3.2 au. Thus, the particle
   differential
   size distribution was found to be adequately
described by a differential power law of index  $\alpha$=--2, except
for the largest
particle size bins ($r \gtrsim$1 mm) for which an index
$\alpha$=--4 is needed to satisfy the 67P trail data, which are mostly
sensitive to those large particles, and which were acquired
in previous revolutions \citep{Agarwal10}. A close value of
$\alpha\sim$--3.7 for large particles
has been found by \cite{Soja15} from analysis of 67P trail {\it
  Spitzer} data. This also agrees with the
distribution of blocks that are larger than a few centimetres in size
on the surface of smooth terrains found by \cite{Mottola15}
($\alpha$=--3.8$\pm$0.2) from the Rosetta Lander Imaging System
(ROLIS) on board Philae. This is also in line with the steep
distribution of large particles found by \cite{Kelley13a} in comet
103P/Hartley 2 coma ($\alpha$=--4.7).  The maximum grain
size ejected that was reported by
\cite{Rotundi15} was 2 cm, and a dust loss rate
of 7$\pm$1 kg s$^{-1}$ was determined, giving a dust-to-gas mass ratio
(d/g) of 4$\pm$2 when combined with water production-rate data from
the Microwave Instrument for the Rosetta Orbiter (MIRO)
\citep{Gulkis15}.  Assuming spherical particles, a grain density of
1900$\pm$1100 kg m$^{-3}$ was derived.  Interestingly, the velocity
of outflowing grains did not show any link with particle
size. Hydrodynamic models of the inner coma \citep[e.g.][]{Crifo}
would be needed to explain such behavior.

Recently, a detailed study of GIADA data in the 3.4-2.3 AU heliocentric
distance range has been performed by \citet{DellaCorte15}. In this study,
two populations of grains, both compact and fluffy, are described
in relation to the geographical location of emission. Using the same
GIADA data, the
contribution of the fluffy grain component to the brightness
of the coma has been found as being less than
15\% by \citet{Fulle15a}.  These fluffy grains have also been collected with the
Cometary Secondary Ion Mass Analyser (COSIMA) on board Rosetta,
which shows no trace of ice in their composition
beyond 3 au \citep{Schulz15}.

In contrast with the random distribution of velocities versus
grain size found by \citet{Rotundi15}, the relation
of emission velocities and particle mass ($m$) found by \citet{DellaCorte15}
was quite steep, albeit
with a 50\% uncertainty, given
by a power law $v \propto m^{\gamma_m}$ with $\gamma_m$=--0.32$\pm$0.18, which
translates to $v  \propto r^{\gamma_r}$ as
$\gamma_r$=--0.96$\pm$0.54 ($r$ is particle radius). This is
still compatible with
the widely used $v  \propto r^{-0.5}$ dependence that is based on
simple hydrodynamical considerations \citep{Whipple50}. Photometric
measurements of individual grains
at 2.25 AU and 2.0 AU from OSIRIS images suggest a $v
\propto r^{-0.5}$ dependence \citep{Fulle15inprep}. The different
dependencies of particle velocity from the particle radius determined by
\cite{Rotundi15} and \cite{DellaCorte15} might be
related to the various nucleus heliocentric distances and/or
different spacecraft-nucleus distances involved. Only
detailed hydrodynamic calculations in the inner coma, including the
detailed nucleus shape, will allow a proper interpretation of those
data. Consequently, the model runs with the different particle-velocity
distributions since inputs
are needed to determine which distribution is the most
compatible with our observations.

   \begin{figure}
   \centering
   \includegraphics[angle=-90,width=\hsize]{FIG02.ps}
   \caption{High signal-to-noise
    WAC image obtained as a median stack of 117 frames,     obtained on May 17 and 18 2014. The dimensions of the image are
     3690$\times$3690 km at the nucleus distance. The innermost isophote level
     corresponds to 2.24$\times$10$^{-8}$ W m$^{-2}$ sr$^{-1}$
     nm$^{-1}$, decreasing outwards in factors of 2. North is up,
     East to the left.}
              \label{FIG02}
    \end{figure}

In this paper, we combine OSIRIS images acquired between
April and July 2014 with ground-based images taken
with the FOcal Reducer and low dispersion Spectrograph 2 (FORS2) at
the ESO VLT between February and November 2014, when the comet was
observable from the southern hemisphere. From late
November 2014 to late May 2015, the comet was behind the Sun for
ground observers. The comet 67P could be observed again from late May 2015 from the
southern hemisphere and from July 2015 from the northern
hemisphere. Ground-based observations, combined
with the simultaneous OSIRIS data  described above, provide a
unique opportunity to determine the dust properties and their time
evolution because they are most sensitive to the large-scale tail
structure that cannot be mapped from the spacecraft. Processes
such as significant volatile loss or grain fragmentation that take place a
few days after ejection cannot be monitored by OSIRIS.

   \begin{figure*}
   \centering
   \includegraphics[angle=-90,width=18cm]{FIGURE3.ps}
   \caption{Subset of 20 out of the 52 VLT/FORS2 images taken between February
   and November 2014, with the R-SPECIAL filter. North is up, East
   to the left in all images. The date of observation is indicated in each
   panel. All the images have 40$\times$40 pixels in size, which can be
   converted to physical size at the comet using the spatial
   resolution values of last column of Table A.1 (see
   Appendix A).}
    \label{FIG03}
    \end{figure*}

\section{The Observations}

We used two data sets:
\begin{itemize}
\item OSIRIS Narrow Angle Camera (NAC) and
Wide Angle Camera (WAC) images
obtained from late April to
early July 2014.
\item VLT/FORS2 images obtained from mid-February
to late November 2014.
\end{itemize}

A description of the instrumentation and the data reduction follows.

The OSIRIS instrument \citep{Keller07} comprises two cameras, the
NAC, with a field of view (FOV) of 2.20$^\circ\times$2.22$^\circ$
and an angular resolution of 1.87$\times$10$^{-5}$ rad px$^{-1}$,
and the WAC, with a FOV of 11.35$^\circ\times$12.11$^\circ$
with an angular resolution of 1.01$\times$10$^{-4}$ rad px$^{-1}$.
We used NAC images taken with the Orange filter, which has a
central wavelength of 649.2 nm, and a bandwidth of 84.5 nm. The WAC
images used were taken with the Red filter, which has a central
wavelength of 629.8 nm and a bandwidth of 158.6 nm. In both cases, we
used Level 3 images, which were processed
following the standard OSIRIS calibration pipeline, including bias
subtraction, flat-fielding, distortion correction, and radiometric
calibration \citep{Tubiana15b}. The log of the nine NAC observations
is given in
Table~\ref{table1}, and Fig.~\ref{FIG01} displays the NAC
images. The WAC observations consisted of a sequence of 117 images
acquired
between 2014-05-17T07:59:16 and 2014-05-18T06:52:05 (UT), and were aimed at
the detection of a trail feature. For the dust-tail modeling, we combined
all  117 frames into a single median stack, resulting in a high
signal-to-noise image (see Fig~\ref{FIG02}). The spatial
resolution of this image is 123 km px$^{-1}$.

\begin{table*}
\caption{Observational circumstances for the OSIRIS NAC observations}
\label{table1}
\centering
\begin{tabular}{cccccr}
\hline\hline
Date  & r  & S/C-Comet   & Phase angle  & Position angle & Resolution \\
(UT) & (AU) & distance (AU) & (deg) & (deg) &(km px$^{-1}$) \\
\hline
 2014-04-30T06.25.55.567 &      4.111 &     0.01586 &   35.10 & 120.697&  44.410 \\
 2014-05-04T03.17.55.567 &      4.093 &     0.01412 &   35.28 & 120.444&  39.557 \\
 2014-05-07T03.17.56.528 &      4.078 &     0.01278 &   35.40 & 120.234&  35.796 \\
 2014-05-11T12.49.46.645 &      4.057 &     0.01086 &   35.53 & 119.902&  30.410 \\
 2014-05-14T12.37.30.576 &      4.042 &     0.00956 &   35.56 & 119.647&  26.760 \\
 2014-05-18T12.21.10.575 &      4.023 &     0.00782 &   35.50 & 119.239&  21.896 \\
 2014-05-25T11.51.14.558 &      3.988 &     0.00540 &   35.32 & 118.497&  15.131 \\
 2014-05-28T11.38.14.574 &      3.973 &     0.00460 &   35.26 & 118.202&  12.891 \\
 2014-06-01T11.20.54.559 &      3.953 &     0.00354 &   34.95 & 117.682&   9.907 \\

\hline
\end{tabular}
\end{table*}

The VLT data consist of CCD images
acquired with the
R-SPECIAL filter (spectral response close to that of Bessell R, with
central wavelength of 655 nm and bandwidth of 165 nm). FORS was used
in imaging mode with the standard resolution collimator, and the
detector was read binning 2$\times$2, which resulted in an
image scale of 0.25$\arcsec$ px$^{-1}$. The
reduction of the images was performed using standard techniques,
encompassing bias and flat-fielding, and photometric calibration by
standard star field imaging. In addition to the standard techniques,
the images were also processed with a
background subtraction algorithm to remove the crowded star fields
\citep{Bramich08}. For each night of observation, a median
stack of the available images was produced and the magnitude
within an aperture of 10 000 km radius was measured. Full details on
the data set and the reduction procedure are given by \cite{Snodgrass15}.

The log of the observations is given in Table A.1 (see
Appendix A), and a subset of the
VLT images is displayed in Fig.~\ref{FIG03}. The images were
converted from mag arcsec$^{-2}$ ($m$) to mean solar disk intensity
units ($i/i_0$), according to the relationship

   \begin{equation}
      m=2.5\log \Omega  + m_\sun -2.5\log (i/i_0)
   ,\end{equation}

where $\Omega$ is the solid angle of the Sun at 1 au
(2.893$\times$10$^6$ arcsec$^2$), and $m_\sun$ is the magnitude of the Sun
in the Bessell R filter ($m_\sun$=--27.09).

We
emphasise the importance of the different viewing angles and spatial scales of the
OSIRIS and VLT image sets. While
for the OSIRIS images the resolution ranges from 44 to 10 km
px$^{-1}$, the VLT images provide a spatial resolution from nearly
900 km px$^{-1}$ to $\sim$490 km px$^{-1}$ at the closest geocentric
distance of 2.7 au.

An important aspect of the observations is the nucleus brightness
contribution to the images. Since the OSIRIS images and the early VLT
images were
acquired at large heliocentric distances when the comet was displaying
little activity, the nucleus signal to the image
brightness dominates over the coma brightness and
this must be taken into account. The total observed brightness
of the images can
be expressed as a sum of the nucleus plus the coma brightness
contributions convolved with the corresponding point spread function
(PSF) as \citep[e.g.][]{Lamy06}

    \begin{equation}
     B(x,y)=[C(x,y)+N(x,y)]\otimes P(x,y)
   ,\end{equation}

where $C(x,y)$, $N(x,y)$, and $P(x,y)$ are the coma, nucleus, and
PSF as functions of the pixel coordinates of the image relative to the
nucleus position, identified by the brightest pixel in the images.

To calculate the nucleus brightness at each epoch,
we developed a photon ray-tracing algorithm from which we constructed
synthetic images of the nucleus as it would be seen either from the
spacecraft or
from the Earth. We used an early shape model of the nucleus (SHAP4S)
\citep{Preusker15} with a rotational axis pointing to RA=69.54$^\circ$,
DEC=64.11$^\circ$ (J2000 coordinates),  a Lambertian surface
model with a certain albedo value
(the same for all the red filters used), a linear phase
coefficient of 0.047 mag deg$^{-1}$ \citep{Fornasier15}, and a
rotational period of 12.4043h, the appropriate value at the time of
the observation \citep{Mottola14}. The albedo value was
constrained by matching a synthetic lightcurve to the
experimental lightcurve derived from the sequence of WAC
images obtained on May 17 and 18 2014, as described. The resulting
albedo is 0.06, which is close to the peak value of
0.063 obtained by \cite{Fornasier15} from the derived gaussian distribution of
surface albedos.

Although a noticeable coma is present in the images,
its coma contribution to the
    integrated
    nucleus plus coma system brightness at such heliocentric
distances ($\sim$4 AU) is negligible, being estimated to be below the relative
photometric error of the measurements \citep{Mottola14}. This
contribution can be evaluated from the model results that are
described in the next sections. The integrated brightness for the WAC
image of Fig.~\ref{FIG02} is 2.79$\times$10$^{-7}$ W m$^{-2}$
sr$^{-1}$ nm$^{-1}$. For our best-fit
Model 1, which is characterised by a power-law particle-size distribution
with power index of --3 and a random distribution of particle ejection
velocities (see Sects. 3 and 4 for a detailed
description of the model), we obtain 2.84$\times$10$^{-7}$ W m$^{-2}$
sr$^{-1}$ nm$^{-1}$ for the nucleus+coma system, which is in close agreement
with the measured brightness. From the same model,
the integrated signal of the coma alone  is just
1.30$\times$10$^{-11}$ W m$^{-2}$ sr$^{-1}$
nm$^{-1}$, i.e. less than 0.005\% of the total signal. Thus, the coma
contribution can be safely ignored for the construction of the nucleus
lightcurve from the images at such heliocentric distances. To obtain the
integrated brightness at each observation date, an aperture
radius equal to the full width at half maximum (FWHM) of the field stars was
used. Fig.~\ref{FIG04} shows a comparison of the measured lightcurve and the
one calculating the integrated brightness from the synthetic nucleus
images, assuming a surface albedo of 0.06, as previously mentioned.
Along the lightcurve, the mean value of the difference between
measured and computed nucleus
brightness is 1\%, while the maximum difference is 16\%. These
discrepancies are most likely related to the simplicity of the surface
model and to local variations of surface albedo \citep{Fornasier15}.

The coma/tail brightness distribution is computed with the Monte Carlo
dust tail code. This is described in the next section.
   \begin{figure}
   \centering
   \includegraphics[angle=-90,width=\hsize]{FIGURE4.ps}
   \caption{Lightcurve obtained from the analysis of 117 frames
     from WAC Red filter images obtained on 2014 May 17 and 18
     (black dots). The red dots correspond to a simulation of the
     lightcurve, taking in consideration  a nucleus shape model
     \citep{Preusker15} with a Lambertian model for the surface, which has an
     albedo of 0.06, and a ray-tracing
     technique to compute the total output flux at the S/C position.}
              \label{FIG04}
    \end{figure}

\section{The model}

The Monte Carlo dust tail code has been described previously
\cite[e.g.][]{Fulle10,Moreno12}.
Briefly, this is a forward model that, given all the dust input
parameters, computes synthetic
dust tail images for a given date by the trial-and-error procedure. To
this end, the code computes the
trajectory of a large number of spherical particles that are ejected from a small-sized
nucleus, assuming that the grains are affected by the solar
gravitation and the solar radiation pressure. The nucleus gravitational
field is neglected at  distances where the gas drag vanishes (at
approximately 20 nuclear radii, R$_N$). Under these assumptions, the
trajectory of the particles is Keplerian and the orbital
elements are computed
from the assumed terminal velocities (at 20R$_N$). The $1-\mu$
parameter \citep[e.g.][]{Fulle89}, which is the ratio of solar
radiation pressure force to solar gravity force, is
given by $1-\mu =
C_{pr}Q_{pr}/(2\rho r)$. In this equation, $C_{pr}$ is given by

\begin{equation}
C_{pr} = \frac{3E_s}{8\pi cGM_{\sun} } = 1.19\times 10^{-3} \text{kg
 m$^{-2}$}
,\end{equation}

where $E_s$ is the mean total solar radiation, $c$ is the speed of
light, $G$ is the universal gravitational constant, and $M_\sun$ is
the solar mass \citep{Finson68}. $Q_{pr}$ is the radiation pressure
coefficient,
and $\rho$ is the particle density. The radiation pressure coefficient for
absorbing particles with radii $r \gtrsim$1 $\mu$m is $Q_{pr}\sim$1
\citep[e.g.][]{Moreno12}. The geometric albedo of the particles
at red wavelengths is assumed to be $p_v$=0.065, a value close to to the one that was
determined for the geometric albedo of the nucleus, and which ranged from
0.0589 to 0.072 at 535 and 700 nm, respectively, from disk-averaged photometry
using OSIRIS NAC data \citep{Fornasier15}. For the dust particles, we assumed
a phase angle coefficient of 0.03 mag
deg$^{-1}$ in agreement with the value reported by \cite{Snodgrass13}
for comet 67P, and within the range estimated for other comets
\citep[e.g.][]{MeechJewitt87}. In
addition to the input model parameters just
described, we need to set the size-distribution function and the dust-loss rate, as a function of the heliocentric distance.

In most previous applications of the code,
the dust tail code was applied with almost no
previous knowledge of any of the dust properties. However, the
observations of the inner coma dust grains by OSIRIS and GIADA
provide a unique characterisation of fundamental dust
parameters as described in Sect. 1.
We used the dust physical parameters described by
\citet{Rotundi15} as inputs for the Monte Carlo code: the particle-size
distribution is governed by a power law with index --2 (except at
sizes larger than 1 mm, for which the index is --4), the
largest particles ejected are 1 cm in radius,
and the particle density is set to 2000 kg
m$^{-3}$. Taking into account the distributions of particle
velocities found by  \citet{Rotundi15} and \citet{DellaCorte15},
we have devised three different models with distinct grain-velocity dependencies, all of the form $v(\mu,t)=v_1(\mu)u(t)$,
$v_1(\mu)$ being a size-dependent velocity function, and $u(t)$
a dimensionless time-dependent parameter. These models range from a velocity that is independent of particle
size, as found by \citet{Rotundi15}, to a steep function of velocity on
grain size, as derived in \citet{DellaCorte15}. Specifically, in Model 1, the
terminal velocity of the grains is given by $v(\mu,t)=rnd[1,5] u(t)$, where
$rnd[1,5]$ is a random value in the 1 to
5 m s$^{-1}$ interval; in Model 2, the terminal velocity is given by
 $v(\mu,t)=1320(1-\mu)^{0.96} u(t)$ m s$^{-1}$; and in Model 3, we set
$v(\mu,t)=45(1-\mu)^{0.42} u(t)$ m s$^{-1}$, in agreement with the
most probable value, and the lower limit in the power-law exponent of
the velocity versus particle size as determined by
\citet{DellaCorte15}, respectively. We note
that these functions are, in all
cases, derived for a certain range of particle radii only, within the
range of instrumental sensitivity,  mostly in the
0.1 to 10 mm domain.  Fig.~\ref{FIG05} displays the just described
size-dependent term of the terminal velocities for each model
and Fig.~\ref{FIG06} shows
the time-dependent component $u(t)$.

   \begin{figure}
   \centering
   \includegraphics[angle=-90,width=\hsize]{FIGURE5.ps}
   \caption{Size-dependent component of the terminal velocity of
     the dust grains assumed in the Monte Carlo model. Model 1
     corresponds to the random velocity distribution found by
     \cite{Rotundi15}, Model 2 corresponds to the steep, most probable
     value,
     $v\propto r^{-0.96}$ found by \cite{DellaCorte15}, and Model
     3 to the less steep dependence given by $v\propto r^{-0.42}$. The escape
     velocity at 20R$_N$ is also indicated.}
              \label{FIG05}
    \end{figure}

   \begin{figure}
   \centering
   \includegraphics[angle=-90,width=\hsize]{FIGURE6.ps}
   \caption{Assumed time-dependent component of the terminal velocity of
     the dust grains assumed in the Monte Carlo model. The bump
     between --4.25 to --4.15 AU is related to the
     30 April 2014 outburst.}
              \label{FIG06}
    \end{figure}

The function $u(t)$ reflects
the overall time-dependence of the velocity and is constrained
 as $u(t)=1$ in the heliocentric distance range 3.7-3.4
au from the results of \citet{Rotundi15} for Model 1. Out of this
heliocentric distance range, and for Models 2 and 3, a
free parameter  is adjusted by the trial and error
    procedure, taking into account that it should increase after the
    onset of activity \citep[e.g.][]{Fulle10}, and it is further
    enhanced whenever an outburst occurs, as has been observed, e.g. after
    the 2007 outburst of comet 17P/Holmes
    \citep{Montalto08,Moreno08}. The other
free parameters that must be set are the dust-loss
rate as a function of the heliocentric distance, and the activation
time. The heliocentric dependence of the dust-mass loss rate is
    initially assumed as a function that varies as the inverse square of the
    heliocentric distance, and then several tens of test
    functions that modify the initial profile are
    introduced until a good fit to all the  datasets of OSIRIS and VLT
    images is reached. Thus, the presence of outbursts, such as that of
    30 April 2014 \citep{Tubiana15a} imply a sudden increase of the
    dust-loss rate that clearly has to be  taken into account to fit
    the data. The goodness of the fit for each model is characterized
    by the quantity
\begin{equation}
\chi^2  =\left| \sum_{i,j} \frac{
  \left[\log(I_{obs}(i,j))-\log(I_{mod}(i,j))\right]^2 }
{  \log(I_{mod}(i,j))  } \right|,
\end{equation}
where $I_{obs}$ and $I_{mod}$ are the observed and modeled brightness, and
the summation is extended to the pixels $(i,j)$ along a scan
in the anti-solar direction (position angle of the Sun-to-comet radius
vector), passing
through the brightest pixel.  This $\chi^2$ parameter is
calculated for each image, and then the total
summation of the $\chi^2$ for all the OSIRIS plus VLT images is the
parameter used as the quality of the fit for each model. As
previously stated, the size distribution is initially set  to
a power law of
index --2 and the maximum particle radius to 1 cm, in accordance with
\citet{Rotundi15}. The minimum particle radius is set initially to 1
$\mu$m, but tests will also be made for smaller and larger minimum
size, as described below.

Another input parameter of the model is the emission
pattern. The OSIRIS images acquired in August 2014
when Rosetta was at a distance from the comet, when the nucleus
shape could be clearly resolved
\citep{Sierks15,Lara15}, revealed a number of conspicuous jets coming
from the neck region (Hapi) and pointing towards the direction of the
pole. In our model, we imposed a relatively higher number of
particles launched from latitudes higher than 60$^\circ$ than from
elsewhere. Specifically, we set 35\% of particles (in number) as being
emitted from that region and 65\% from latitudes south of
60$^\circ$. This corresponds to a flux of particles
that are 7.5 times higher at those high latitudes than elsewhere. To
keep the number of free parameters to a minimum, we have not attempted
to modify the emission pattern along the orbital arc.
This highly anisotropic
ejection pattern, with particle emission directed to the north, has
already  been
inferred by \citet{Fulle10} in the GIADA dust environment model from
model fits to 67P data that was acquired during three revolutions around the
Sun prior to the Rosetta encounter.

\section{Results and discussion}

Once a set of model parameters has been defined, we run the Monte Carlo dust
tail code for all the OSIRIS and VLT images involved in the
analysis. However, for clarity, and to save space, we will only show
the results for subsets of them. Specifically, four dates are
selected for the OSIRIS images, and twenty for the VLT images. In
each case, the isophotes will be shown in the same brightness units of
W m$^{-2}$ sr$^{-1}$ nm$^{-1}$ (as for the Level 3 OSIRIS images), and
in units of the solar disk intensity for the VLT images.

   \begin{figure}
   \centering
   \includegraphics[angle=-90,width=\hsize]{FIGURE7.ps}
   \caption{Monte Carlo dust tail code simulations (red contours)
     compared to the OSIRIS NAC observations (black contours) for the
   input parameters derived from \cite{Rotundi15} with a power-law
   exponent of the size distribution function of --2. The innermost
   isophotes have a value of 3.2$\times$10$^{-8}$  W m$^{-2}$
   sr$^{-1}$ nm$^{-1}$
   in all  four images and decrease in factors of 2 outwards.}
              \label{FIG07}
    \end{figure}

   \begin{figure}
   \centering
   \includegraphics[angle=-90,width=\hsize]{FIGURE8.ps}
   \caption{Monte Carlo dust tail code simulations (red contours)
     compared to the VLT observations (black contours) for the
   input parameters derived from \cite{Rotundi15} with a power-law
   exponent of the size distribution function of --2. The image dates
   are shown on the left side of each panel. Innermost isophotes are
   4$\times$10$^{-12}$ solar disk units, except for panels 2014/02/28 and
   2014/03/14, which have 2$\times$10$^{-12}$ solar disk units.}
              \label{FIG08}
    \end{figure}

We start by displaying the results of Model 1, the one which has a
random distribution of
terminal particle velocities as described above. For this model, we
obtain the results shown in  Figs.~\ref{FIG07} and~\ref{FIG08}
for the OSIRIS NAC
and VLT images, respectively, corresponding to the best-fit dust-mass
loss rate displayed in  Fig.~\ref{FIG09}. This graph shows a peak at
about 4.11 au pre-perihelion that
corresponds to the outburst that occurred on 30 April 2014, in which
a total dust-loss mass of $\sim$7$\times$10$^6$ kg was released. The
comet shows some activity, at the level of $\sim$0.5 kg
s$^{-1}$, already at 4.3 au pre-perihelion. This is in agreement with
the findings of \citet{Snodgrass13} for the previous orbit and
their predictions for the current orbit. In their trail model,
\cite{Soja15} reported values of $\sim$10
kg s$^{-1}$ at 3 au, which is in line with ours, but of $\sim$3.5 kg
s$^{-1}$ at 4.3 au, a value that is considerably larger than our estimate at that
heliocentric distance.

   \begin{figure}
   \centering
   \includegraphics[angle=-90,width=\hsize]{FIGURE9.ps}
   \caption{Best-fit dust-mass loss rate as a function of the
     heliocentric distance for power-law size distributions of --2
     (solid line) and --3 (dotted line). Note the increase in mass loss
     rate at the time of the 30 April 2014  outburst.}
              \label{FIG09}
    \end{figure}

   \begin{figure}
   \centering
   \includegraphics[angle=-90,width=\hsize]{FIGURE10.ps}
   \caption{Monte Carlo dust tail code simulations (red contours)
     compared to the OSIRIS NAC observations (black contours) for the
   input parameters derived from \cite{Rotundi15} with a power-law
   exponent of the size distribution function of --3 and the random
   distribution of terminal velocities (Model 1).}
              \label{FIG10}
    \end{figure}

   \begin{figure}
   \centering
   \includegraphics[angle=-90,width=\hsize]{FIGURE11.ps}
   \caption{Monte Carlo dust tail code simulations (red contours)
     compared to the VLT observations (black contours), for the
   input parameters derived from \cite{Rotundi15}, with a power-law
   exponent of the size distribution function of --3, and the random
   distribution of terminal velocities (Model 1).}
              \label{FIG11}
    \end{figure}

While the modelled images fit the tail
shapes for OSIRIS and VLT images until early August 2014 reasonably well, it
is clear that they
deviate from the measured isophotes at later dates. The total $\chi^2$
  for this model is 40.1. No improvements are found when Models
2 and 3 are run with different velocity distributions. We therefore tried to modify the
input parameters to obtain a better fit to the
data. We found that no improvements were
possible, except when the power-law index of the size distribution
is decreased, i.e. using a steeper size-distribution function. The best
results were found for a power index of --3, for which the
model results are presented in  Figs.~\ref{FIG10} and  \ref{FIG11}
for the NAC
and the VLT images, respectively, for Model 1. The corresponding
best-fitted dust-loss rate is shown in  Fig.~\ref{FIG09}. For
    this model,  $\chi^2$ is 14.4, whcih is much smaller than the value of
    40.1 found for the model with power index of --2.

The best-fit power index of --3 for the size-distribution function
agrees with that previously derived by \citet{Fulle10},
which was obtained from dust tail modelling of observations that were acquired during several
previous orbits. As noted by \citet{Fulle15a}, the different power
indices of  --2 derived by
\citet{Rotundi15} and of --3 derived from the dust tail models,
could be related to contribution of the aggregate particles. The presence of
fluffy grains in the coma has been
clearly shown by the GIADA instrument since mid-September 2014
\citep{DellaCorte15,Fulle15a}. As \citet{Rotundi15} use
earlier measurements,
the power index of --2 only refers to the compact particle population. It is possible that those aggregates, which have a
steeper size distribution function, are contributing to solve this
inconsistency \citep{Fulle15a}. However, proving it quantitatively is far from
easy. First, the computation of the $(1-\mu)$ parameter for
aggregates of the order of, or larger
than, the wavelength of the incident light
is prohibitive in terms of current computational resources. And
second, the
non-radial pressure force component on the aggregates becomes
non-negligible \citep{Kimura02}, implying a non-Keplerian motion for
those particles, and the use of numerical integrators to determine
their orbits. In any case, it is interesting to note that
the later the observation date,
the larger the discrepancy is between the models with size-distribution power indices of --2 and --3  (compare Fig.~\ref{FIG08} and
Fig.~\ref{FIG11}).

After finding the power index of --3 as the best fit for Model 1, we
fit the data with Models 2
and 3, assuming $\alpha$=--3 and leaving the dust-mass loss rate as
the only free
parameter. The fits to the OSIRIS NAC and VLT data are found in
 Fig.~\ref{FIG12} and  Fig.~\ref{FIG13} for Model 2, and
 Fig.~\ref{FIG14} and  Fig.~\ref{FIG15} for Model 3. The
models 1, 2, and 3 for the WAC data are shown in  Fig.~\ref{FIG17}, while
the corresponding best-fitted dust-loss rate functions are displayed
in  Fig.~\ref{FIG18}. Again,
a significant deviation of the model
isophotes from the
observed tail shapes is observed for the VLT data after early
August, and particularly for Model 3,
which indicates that the particle terminal velocities are better
represented by a flat random distribution of velocities
rather than a power law of the size, as was found by
\citet{Rotundi15}. A proper
interpretation of the different particle velocities that were encountered by
\citet{Rotundi15} and \citet{DellaCorte15} should incorporate the
hydrodynamical processes in the inner coma, taking into account the
different ranges of nucleus to Sun and nucleus to spacecraft
distances involved. The computed values of $\chi^2$ are 16.1 and
    32.8 for models 2 and 3, respectively. As an example,
    Fig.~\ref{FIG16} depicts the resulting scans along the anti-solar
    direction for one of the
    latest VLT-observed and modeled images,
    where the deviations of the data for the different models can be seen.

 In Fig.~\ref{FIG18}, the water production rates at
different heliocentric distances
that were obtained by \citet{Gulkis15} from MIRO are also plotted. From these
measurements, we obtain a d/g mass ratio varying between 6.5 at
3.95 au pre-perihelion and 3.8 at 3.5 au pre-perihelion, for Models 1 and 2,
and between 3.3 at
3.95 au pre-perihelion and 1.6 at 3.5 au pre-perihelion
for Model 3, which confirms the d/g=4$\pm$2
that was estimated by \citet{Rotundi15}.

   \begin{figure}
   \centering
   \includegraphics[angle=-90,width=\hsize]{FIGURE12.ps}
   \caption{Monte Carlo dust tail code simulations (red contours)
     compared to the OSIRIS NAC observations (black contours) for the
   input parameters derived from \cite{Rotundi15} with a power-law
   exponent of the size distribution function of --3 and the terminal
   velocities being given by $v(\mu,t)=1320(1-\mu)^{0.96} u(t)$ m s$^{-1}$
   (Model 2).}
              \label{FIG12}
    \end{figure}

   \begin{figure}
   \centering
   \includegraphics[angle=-90,width=\hsize]{FIGURE13.ps}
   \caption{Monte Carlo dust tail code simulations (red contours)
     compared to the VLT observations (black contours) for the
   input parameters derived from \cite{Rotundi15} with a power-law
   exponent of the size distribution function of --3 and the terminal
   velocities being given by  $v(\mu,t)=1320(1-\mu)^{0.96} u(t)$ m s$^{-1}$
   (Model 2).}
              \label{FIG13}
    \end{figure}

   \begin{figure}
   \centering
   \includegraphics[angle=-90,width=\hsize]{FIGURE14.ps}
   \caption{Monte Carlo dust tail code simulations (red contours)
     compared to the OSIRIS NAC observations (black contours) for the
   input parameters derived from \cite{Rotundi15} with a power-law
   exponent of the size distribution function of --3 and the terminal
   velocities being given by $v(\mu,t)=45(1-\mu)^{0.42} u(t)$ m s$^{-1}$
   (Model 3).}
              \label{FIG14}
    \end{figure}

   \begin{figure}
   \centering
   \includegraphics[angle=-90,width=\hsize]{FIGURE15.ps}
   \caption{Monte Carlo dust tail code simulations (red contours)
     compared to the VLT observations (black contours) for the
   input parameters derived from \cite{Rotundi15}, with a power-law
   exponent of the size distribution function of --3, and the terminal
   velocities being given by $v(\mu,t)=45(1-\mu)^{0.42} u(t)$ m s$^{-1}$
   (Model 3).}
              \label{FIG15}
    \end{figure}

   \begin{figure}
   \centering
   \includegraphics[angle=-90,width=\hsize]{FIGURE16.ps}
   \caption{Scan along the anti-solar direction
      of the VLT image of 2014/10/24 (solid circles) compared to
     the different ejection velocity models described in the text:
     Model 1 (best-fit model)
corresponds to the solid-line, Model 2 is represented by the dashed line,
and Model 3 by the dotted line. These three models have  a power
index for the size distribution of --3. The dash-dotted line
corresponds to Model 1 but with a power index for the size
distribution of --2.}
              \label{FIG16}
    \end{figure}

   \begin{figure}
   \centering
   \includegraphics[angle=-90,width=\hsize]{FIGURE17.ps}
   \caption{Monte Carlo dust tail code simulations (red contours)
     compared to the OSIRIS WAC observations (black contours), from
     left to right, for
     Models 1, 2, and 3, with a power-law
   exponent of the size distribution function of --3.}
              \label{FIG17}
    \end{figure}

After obtaining this satisfactory fit for Model 1, we explored the sensitivity to
the input parameters of the model results. Changing the minimum
particle radius from 1 $\mu$m to 10 $\mu$m does not significantly affect
 the $\chi^2$ of the fit,
but if the minimum radius is set as high as 50
$\mu$m, $\chi^2$ increases by up to 48.2. The
presence of dust particles smaller than 5 $\mu$m in size has been
demonstrated by \cite{DellaCorte15} from dust accumulation on two of the
five micro balances system (MBS) of GIADA since September, 2014.  On the
other hand, the input dust-mass loss rate can be varied up to the
30\% level without altering the model results
substantially. Thus, for Model 1, $\chi^2$ increases from 14.4
(best fit) to 16.2 by a variation of 30\% in the overall
dust-mass loss rate. If the dust-loss rate profile is varied up to 50\%,
then $\chi^2$ increases to 19.2, which is too large compared to its
equivalent in the best fit
model. From this, we estimate a 50\% uncertainty
as an upper limit to the obtained dust-loss rates.

   \begin{figure}
   \centering
   \includegraphics[angle=-90,width=\hsize]{FIGURE18.ps}
   \caption{Best-fit dust-mass loss rate as a function of the
     heliocentric distance for Models 1 and 2 (solid line), and for
     Model 3 (dotted line), for
     power-law size distributions of index --3. Also shown are the
     water production rates derived from MIRO instrument \citep{Gulkis15}.}
              \label{FIG18}
    \end{figure}

Regarding the level of activity of the comet at the heliocentric
distance range explored, we compare the derived dust-loss
rates with other published estimates. In most cases, unfortunately,
only values of the quantity $Af\rho$ \citep{AHearn} have been
reported \citep[e.g.][and references therein]{Mazzotta09,Kelley13b},
which cannot be easily converted to dust-loss rates. \cite{Lamy09}
gave estimates of a few short-period comets at distances near 3 au,
namely 4P/Faye, 17P/Holmes, 44P/Reinmuth, and 71P/Clark. For those
comets, the dust-production rate near 3 au ranges from $\sim$1 to 5 kg
s$^{-1}$, which is less than that derived for 67P ($\sim$15 kg
s$^{-1}$).

\section{Conclusions}

A series of Rosetta OSIRIS NAC and WAC images, together with an extensive
data set of ground-based VLT images of comet 67P, have been analyzed
by our Monte Carlo dust tail model. At the time of the observations,
the comet moved from 4.4 au to 2.9 au, inbound. In this heliocentric distance
range, the main results can be summarised as follows:

   \begin{enumerate}
      \item The comet was already active at 4.3 au,
        with a dust-mass loss rate of $\sim$0.5 kg s$^{-1}$, increasing up
        to $\sim$ 15 kg s$^{-1}$ at 2.9 au.  Based on the model
          results,
these loss rates are affected by a maximum overall uncertainty of
$\sim$50\%.
      \item The dust size distribution is characterised by a power law
        with  a power index of --3 for particles smaller than 1 mm, and
        --4 for larger grains.
      \item The terminal velocity of the particles is best-fitted
        by a random distribution in the 1 to 5 m s$^{-1}$ interval,
        which is consistent with the in situ measurements of \cite{Rotundi15}.
      \item The minimum particle size is constrained at radius $r <$
        10 $\mu$m, while the maximum size is compatible with the
        innermost coma values derived by \cite{Rotundi15} ($r$=1 cm).
      \item The dust-to-gas mass ratio, based on the results of our
        best-fit model  and
        combined with water production rates
        that were inferred from the MIRO experiment, varies between
        3.8 and 6.5, which is consistent with
        the value of 4$\pm$2 derived by \cite{Rotundi15}.
   \end{enumerate}

\begin{acknowledgements}

We are grateful to the anonymous reviewer for his/her
comments and suggestions that helped to considerably improve
the manuscript. \\

OSIRIS was built by a consortium led by the Max-Planck Institut f\"ur Sonnensystemforschung, G\"ottingen, Germany, in
collaboration
with CISAS, University of Padova, Italy, the Laboratoire d'Astrophysique
de Marseille, France, the Instituto de Astrof\'\i sica de Andaluc\'\i
a, CSIC, Granada,
Spain, the Scientific Support Office of the European Space Agency, Noordwijk,
The Netherlands, the Instituto Nacional de T\'ecnica Aeroespacial,
Madrid, Spain,
the Universidad Polit\'ecnica de Madrid, Spain, the Department of Physics and
Astronomy of Uppsala University, Sweden, and the Institut f\"ur Datentechnik und
Kommunikationsnetze der Technischen Universit\"{a}t Braunschweig, Germany.
The support of the national funding agencies of Germany (DLR), France
(CNES), Italy (ASI), Spain (MEC), Sweden (SNSB), and the ESA Technical
Directorate is gratefully acknowledged. We thank the Rosetta Science Ground
Segment at ESAC, the Rosetta Mission Operations Centre at ESOC and the
Rosetta Project at ESTEC for their outstanding work that enables the
scientific return
of the Rosetta Mission. \\

This paper is based on observations made with ESO telescopes at the La
Silla Paranal Observatory under programmes IDs 592.C-0924, 093.C-0593,
and 094.C-0054.

\end{acknowledgements}

redpajama_set_name: RedPajamaArXiv


Tony achieved an Associate's Degree in Auto/Diesel Repair from Universal Technical Institute in 1997, is ASE Double Master Certified in Auto & Diesel repair since 1999, earned a Certificate in Public Works Construction Inspection from Santiago Canyon College in 2009, and is in the process of completing his Bachelor Degree in Public Administration. Tony has been working in the Public sector since June of 2003.
Maintains over 269 City street miles including repairs to potholes and sunken roadway areas.
Provides repairs for approximately 760 miles of sidewalks, curbs and gutters.
Maintains public alleyways by clearing weeds and debris.
Collects trash & debris from City right-of-ways.
Sweeps sand and debris from bike lanes, arterial, collector and downtown streets twice a month.
Maintains the flow of water through drainage ditches and detention ponds receiving storm water runoff.
Provides the set up of road closures for emergencies, traffic accidents, fires, special events, etc.
Produces and maintains over 13,000 signs that are posted with the City boundaries.
Sign types include: Street name signs, Regulatory signs (stop signs, speed limit signs, etc.), Warning signs (stop ahead, railroad crossing, etc.), Guide signs & Special signs.
Performs street striping, pavement marking & crosswalk installation.
Provides in-house graffiti removal services from public & private property.
Maintains over 150 acres of landscaping including 9 City Parks, City Cemetery, City facilities, traffic medians.
Maintains irrigation systems for all parks, sports fields, Cemetery & City facilities.
Maintains playground equipment, picnic tables, barbeques, benches & exercise equipment at all City Parks.
Provides tree trimming & removal.
Provides burial services at the Cemetery.
Maintains approximately 450 vehicles and pieces of equipment throughout the City including Police, Fire, Public Works and Administration vehicles.
Provides contract management services for landscaping and tree trimming throughout the City.
Provides technical support and plan check related to landscape services and new development.
Tree Removal & Tree Maintenance Criteria, Information, Schedules and Standards.


text:
((31Knots)) Band Profile and Upcoming Chicago Concerts - Oh My Rockness
31Knots's website
Portland's 31Knots have just released their best album (Talk Like Blood) for their new label (Polyvinyl), are fresh off a successful European tour with Q and Not U, and just rocked a sold-out show in Tokyo. Though they've been around since 1997, these guys have definitely stepped it up a notch and have taken things to the next level.
31Knots' "prog" pop sound with a heavy lyrical emphasis has been compared to bands like Modest Mouse, Cursive, and even, Yes (see Buffalo '66). They like to throw in some good old-fashioned math rock and instrumental trickery just to jazz things up a bit, but ultimately, these guys just play good, extended pop jams.

redpajama_set_name: RedPajamaCommonCrawl


text:
Francesco Paolo Augusto "Frank" Cali (, ; March 26, 1965 – March 13, 2019), also known as "Franky Boy", was an American mobster and the eventual acting boss of the Gambino crime family. Law enforcement considered Cali to have been the Gambinos' "ambassador to Sicilian mobsters" and had linked him to the Inzerillo Mafia family from Palermo. According to Assistant U.S. Attorney Joseph Lipton, he was "seen as a man of influence and power by organized crime members in Italy". Cali was shot and killed outside his home in Staten Island on March 13, 2019. At the time of his death, a number of media organizations described him as the "reputed" acting boss of the Gambino crime family.

Early years
Cali was born on March 26, 1965, in New York City, to Augusto Cesare Calì and Agata Scimeca, both natives of Palermo, Sicily. His father ran a household goods store in Palermo and a video store in Bensonhurst, Brooklyn. He had a clean police record in the United States, even though he was mentioned in the Pizza Connection investigation, when police discovered that he was a partner of Domenico Adamita, allied to Sicilian Mafia boss Gaetano Badalamenti.

Frank Cali was the nephew-in-law of Sicilian mobster John Gambino, and had close ties to the once powerful Sicilian Mafia family led by Salvatore Inzerillo. Cali was also a great-nephew of Bonanno crime family mobsters Giovanni Bonventre and Vito Bonventre.

As a young man, Cali bonded with Gambino mobster Jackie D'Amico, a lieutenant of Gambino boss John Gotti who operated a crew on 18th Avenue in Brooklyn. In January 1997, the FBI reported to Italian authorities that Cali had been "combined" into the Gambino family. Cali was promoted to acting capo when D'Amico became acting boss. Cali ran several import-export companies in Brooklyn, including Circus Fruits Wholesale in Fort Hamilton, Brooklyn.

Sicilian Mafia ties
Cali also maintained ties with the Sicilian Mafia. He married Rosaria Inzerillo, a sister of Pietro Inzerillo and a relative of Gambino associate Frank Inzerillo, a member of the Palermitan Inzerillo family.

In the early 1980s, after losing the Second Mafia War against the Corleonesi of Totò Riina, the Inzerillo family was forced to flee Sicily. Cali and old Palermo boss Filippo Casamento supported the return of the Inzerillos to Palermo, according to Italian authorities.

According to the Italian Polizia di Stato (State Police), Cali was also a member of the Sicilian Cosa Nostra. He was the contact for Sicilian mafiosi who traveled to New York to meet him, do business, and update him on Sicilian affairs. "He's our friend and he is everything over there", confided Sicilian mobster Gianni Nicchi to his boss Antonio Rotolo, after a trip in 2003. Nicchi is known to be one of Cali's "men of honor" who went back and forth between Palermo and the US for drug trafficking. Nicchi finally settled in Daytona Beach, Florida, where he was known to employ high school students as drug runners.

Arrest and prison
In early 2003, Cali and fellow captain Leonard "Lenny" DiMaria began extorting 'mob taxes' from Joseph Vollaro, the owner of a trucking and contracting company that was involved in building a NASCAR speedway on Staten Island. Vollaro was eventually forced to pay tens of thousands of dollars as tribute to D'Amico and Gambino boss Nicholas Corozzo. In 2004, to avoid prison time for a cocaine conviction, Vollaro began working with federal authorities as an informant. Vollaro's undercover work led to a massive indictment four years later.

On February 8, 2008, Cali and 61 other New York Cosa Nostra associates were arrested and charged with federal racketeering charges. as part of Operation Old Bridge. Old Bridge terminated the drug trafficking between the Sicilian Mafia and the Gambino family. Prosecutors claimed that Cali acted as the Gambino "ambassador to the Sicilian mobsters" and as a liaison between D'Amico and the Sicilian connections to the Inzerillo family. Cali was charged with racketeering, extortion, and conspiracy along with D'Amico and DiMaria.

On June 4, 2008, Cali pleaded guilty to conspiring to extort money from Vollaro. Cali was incarcerated at the Metropolitan Detention Center in Brooklyn, New York. Ten months later, on April 6, 2009, he was released from prison.

Around 2009, Cali's uncle John Gambino was elevated to the family's ruling panel, according to court papers filed in Brooklyn Federal Court. The U.S. Justice Department demanded that Cali avoid all contact with Gambino, except for weddings or holiday celebrations approved in advance by Cali's probation officer.

Underboss
In October 2012, Cali was identified by New York crime reporter Jerry Capeci as the new underboss of the Gambino crime family. Brooklyn Federal prosecutors had also referred to him as underboss. Capeci has previously identified Domenico Cefalù, a member of the same Sicilian faction as Cali, as the current boss of the group. Though his status remained unclear, the promotion of both men follows a period in which John Gambino was a street boss within the family, showing that the Sicilian group has remained dominant in recent years. In July 2013, it was reported that Cali turned down the position of boss of the family.

Acting boss
In August 2015, New York Daily News reported Cali had taken over as acting boss of the Gambino family. A September 29, 2018, report stated that Cali "infused the family with 'zips' — hoodlums from the old country — and bulked up its heroin and OxyContin business". A gangster in Italy was quoted as having stated that Cali "is everything over there" (New York). In March 2019, police investigating Cali's death publicly claimed that he had been "the acting boss" of the Gambino organized crime family.

Death
Cali died at Staten Island University Hospital on March 13, 2019, at the age of 53, after being shot  at about 9:20 p.m. in front of his home on Hilltop Terrace in the Todt Hill area. He was buried six days later at Moravian Cemetery in New Dorp, Staten Island. This was the first murder of a New York crime boss since the 1985 assassination of Paul Castellano, who was also boss of the Gambino family. Surveillance video showed a pickup truck striking Cali's parked Cadillac, a subsequent confrontation between the driver and Cali, and then the shooting. Cali had tried to evade the killer by using his vehicle as a shield. He was hit ten times with bullets from a 9 mm handgun.

On March 16, 24-year-old suspect Anthony Comello was arrested in Brick, New Jersey, by the New York Police Department and US Marshals, to face murder charges on Staten Island. Authorities originally believed the crime may have been related to a personal dispute (possibly a romantic matter) and not organized crime activity. On April 3, Comello was indicted and was being held in protective custody at an undisclosed New York City correctional facility. On May 10, Comello pleaded not guilty to murder and weapon possession charges, although he had initially confessed to the murder to police. One news report cited unnamed mob experts as stating that he "is almost certainly marked for death". Comello had already texted that his "family is marked".

In July 2019, Comello's defense attorney stated that Comello had become obsessed with QAnon conspiracy theories, believing Cali was a member of a "deep state". Comello was convinced "he was enjoying the protection of President Trump himself" to handcuff Cali and place him under citizen's arrest, as Comello had attempted months earlier with New York City Mayor Bill de Blasio as well as California Member of Congress Maxine Waters. The reason why Cali was targeted was unclear.

The New York Times reported that at his first court appearance, Comello "displayed symbols and phrases associated with QAnon scrawled on his hand in pen". The defense attorney sought to prove Comello "not guilty by reason of mental defect". In December 2019, Comello refused to take a psychiatric exam, and was warned by the judge that his refusal could jeopardize his right to use an insanity defense; the judge also denied a motion to suppress Comello's initial confession. In June 2020, Comello was found mentally unfit to stand trial.

References

Notes

External links

1965 births
2019 deaths
American crime bosses
American extortionists
American prisoners and detainees
Bosses of the Gambino crime family
Burials at Moravian Cemetery
Criminals from New York City
Deaths by firearm in Staten Island
Inzerillo-Gambino Mafia clan
Mafia extortionists
Male murder victims
Murdered American gangsters of Italian descent
Murdered American gangsters of Sicilian descent
People from New York City
People from Todt Hill, Staten Island
Prisoners and detainees of the United States federal government

redpajama_set_name: RedPajamaWikipedia


text:
Q: azure ad b2c: the login popup is not showing sign up link/button Using msal v2.0 I am showing a login popup. I can sign in with my account, but the popup is not showing any option to sign-up for new user. How I can enable the sign-up as well?
const msalConfig = {
  auth: {
    clientId: "XXXXXXXX-XXXX-XXXX-XXXX-XXXXXXXXXXXX",
    authority:
      "https://login.microsoftonline.com/XXXXXXXX-XXXX-XXXX-XXXX-XXXXXXXXXXXX/",
    redirectUri: "http://localhost:5123/about",
  },
};

const msalInstance = new msal.PublicClientApplication(msalConfig);

export const loginRequest = {
  scopes: ["user.read"],
  prompt: "select_account",
};

async function login() {
    try {
      const loginResponse = await msalInstance.loginPopup(loginRequest);
      if (loginResponse) {
        // get account
      }
    } catch (err) {
      // handle error
    }
}

// login();

redpajama_set_name: RedPajamaStackExchange


text:
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       	<?php //echo $this->load->view('elements/latest_deal.tpl.php');?>
        <?php echo $this->load->view('elements/forum.tpl.php');?>
        <?php echo $this->load->view('common/ad.tpl.php');?>

	<?php */?>

<?php echo $this->load->view('common/social_box.tpl.php');?>

redpajama_set_name: RedPajamaGithub


text:
CBS Names London Star Trek Destination
CBS Consumer Products and Media 10 will launch Destination Star Trek, a Star Trek convention. The event will take place Oct. 19-21 at the Excel Exhibition Centre in London. The Destination Star Trek event will not only mark the first time in 10 years that
The Destination Star Trek event will not only mark the first time in 10 years that the U.K. will have its own designated Star Trek event, but it will also bring together each of the series' captains. Sir Patrick Stewart, Avery Brooks, Kate Mulgrew and Scott Bakula will appear on stage together.
The event will also feature guest talks, autograph opportunities, photo shoots, replica sets, prop displays, future fashion shows, stunt demonstrations, costume displays and themed parties.
"The Star Trek fan base in the U.K. is one of the biggest in the world and it has waited a long time for the convention to return, so we wanted to make sure we did it right," says Liz Kalodner, executive vice president and general manager, CBS Consumer Products. "In Media 10, we have a great partner with experience putting on amazing live shows, and Destination Star Trek is destined to join many other CBS properties that have been transformed into vital fan destinations."
"We are thrilled to be working with one of
the biggest brands in the world in the shape of Star Trek," says Suzy Pallett, Media 10. "We are busy lining up an incredible schedule and Star Trek London promises to be an unmissable event!"


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911 TARGA 4S from Porsche is a Subcompact car with a 3.8 L petrol engine.
Transmission: 7-speed gearbox with overdrive.
Average fuel consumption for this car is 31.5 MPG (9.4 liters per 100 km).
In case of 911 TARGA 4S 3.8 CO2 emission is 215 grams per kilometer.
If you drive 20 000 kilometers a year (that's 12 427 miles) and spend half of that time in town while other half on open road you will end up burning 1920 liters of fuel.
Multiply 1920 with a fuel price and you will end up with a yearly fuel cost. It would be around 2208 $ if you are in Canada and year is 2012 (that's when and where this tests were performed).


text:
HBS Working Paper Series
Nonprofit Boards: It Is time to Lift Your Gaze and See the System
By: Shamal Dass, Kristy Muir and V. Kasturi Rangan
Nonprofits the world over have faced significant crises in 2020, leaving them and their constituents in precarious positions. Responses to these crises have demonstrated incredible agility. However, they have also demonstrated that the first two levels of governance (level 1: fiduciary responsibility and level 2: organizational performance) are not sufficient in reimagining a new normal. The pandemic and the social justice movements remind us that nonprofit boards need to lift their gaze beyond level 2, and strive for systems impact. We call it level 3 governance. We've seen incredible agility by nonprofits throughout these crises; and systems thinking has long been understood to be a sound way to consider and address complex social problems. Thus, the timing is ripe to bring the two together, and nonprofit boards must take the leadership in doing so. Applying systems thinking at the board level has not been normal practice. This paper provides a framework for how boards might do so and, in turn, govern beyond their organization and meet the social purpose for which their organizations exist.
Nonprofit Organizations; Governing And Advisory Boards; Health Pandemics; Governance; Corporate Social Responsibility And Impact; System; Framework
Dass, Shamal, Kristy Muir, and V. Kasturi Rangan. "Nonprofit Boards: It Is time to Lift Your Gaze and See the System." Harvard Business School Working Paper, No. 21-058, November 2020.
V. Kasturi Rangan
Marketing's Role in Navigating the Winds of COVID-19
By: V. Kasturi Rangan and Courtney Han
Audubon (B) in 2019: Two Years after the Turnaround
By: V. Kasturi Rangan
Gilead: Hepatitis C Access Strategy (A) and (B)
Marketing's Role in Navigating the Winds of COVID-19 By: V. Kasturi Rangan and Courtney Han
Audubon (B) in 2019: Two Years after the Turnaround By: V. Kasturi Rangan
Gilead: Hepatitis C Access Strategy (A) and (B) By: V. Kasturi Rangan


Miss Utility, for "Miss the Utilities" is the name commonly used to refer to Utilities Service Protection Center of Delmarva, Inc (USPCD). Delaware code (Title 26, Chapter 8) establishes USPCD as the approved notification center for Delaware. USPCD is also certified by the Maryland Public Service Commission to be the "One-call system" for the portion of Maryland on the Delmarva Peninsula, commonly referred as the Eastern Shore of Maryland.
Anyone engaged in excavation activities is required to notify underground facility owners prior to the start of any excavation; Miss Utility of Delmarva streamlines this process by providing a "one-call" service allowing excavators to notify area utility companies quickly and efficiently and by providing a positive response back to the excavator.
Miss Utility of Delmarva is funded by its member facility owners and is a free service to both the professional excavator and homeowner.
Miss Utility of Delmarva hosts monthly meetings to open communication among excavators and facility owners fostering a sense of shared responsibility for the protection of underground facilities and public safety.
Public education is essential and Miss Utility of Delmarva is constantly providing education materials and conducting awareness through company safety meetings and a presence at a variety of training conferences, fairs, home shows, company functions and public awareness campaigns.


On the importance of feedback in making things, and how we should let creators know we appreciate things.
Trying to figure out what makes a good doctor, good, a bad one, bad, and that following your instincts can be important.
An analogy looking at gender as vehicles, and my path to finding what is right for me.
Some reflection on how the bond between reggae and punk rock, my love for it, and it's influence on me.


Ash Island Lofts cover South East London including areas such East Dulwich, Camberwell, Lee and Lewisham to name but a few. We specialise in professional loft conversions. Our experienced and friendly team are on hand to advise you on the most suitable loft conversion for your home.
Get in touch today for a free, no obligation discussion with one of Ash Island Lofts' loft conversions experts.
Please, no sales people or sales companies.
If you are thinking about a loft conversion in the East Dulwich area, Ash Island Loft Conversions are here to help. We offer an insurance backed 10 Year Guarantee, which ensures that any defects in your loft will be rectified; even if, in the unlikely event, we are not around in ten years time.
We handle all of the building regulation requirements and can assist with obtaining planning permission, in the small minority of cases that it is required. Our systems meet and exceed all building regulations requirements. Contact us today for a free, no obligation quote!
Ash Island Loft Conversions specialise in loft conversions in the Camberwell area.
For more information on our service you can call us now on 020 8849 8087, or why not request a callback at a time convenient to you?
If you are looking for a loft conversion in the Lee area, call us to discuss how Ash Island Loft Conversions can provide the best solution for you.
A Nationwide Building Society report, in May 2006, stated that conversions are the easiest way to add value to a home. So, why not let us convert your loft into the extra living space you've always wanted.
Ash Island Loft Conversions also operate in and around Lewisham. We Do The Structure, You Do The Finishes – This allows YOU to control your budget. Or, if you prefer, we can do the entire job for you.
Why not get an Instant Quote TODAY and see how affordable a loft conversion is?


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Yau Oi Estate () is a public housing estate in Tuen Mun, New Territories, Hong Kong near Light Rail Yau Oi stop. It was the third public housing estate built in Tuen Mun between 1979 and 1982 on reclaimed land of Castle Peak Bay. Consisting of 11 residential blocks, it was the largest single subsidized housing development in Hong Kong, with 9,153 units and a population of more than 35,000.

Houses

Education
Yau Oi Estate is in Primary One Admission (POA) School Net 71. Within the school net are multiple aided schools (operated independently but funded with government money); no government schools are in the school net.

See also
 Public housing in Hong Kong
 List of public housing estates in Hong Kong

References

Residential buildings completed in 1979
Residential buildings completed in 1980
Residential buildings completed in 1981
Residential buildings completed in 1982
Tuen Mun District
Public housing estates in Hong Kong
1979 establishments in Hong Kong
Housing estates with centralized LPG system in Hong Kong


CBD products have a name which is known widely as cannabidiol, which is used for healing purposes internal and external. For internal purposes they are used to cure many diseases which have become prone to the human life. Many individuals who have taken the CBD products into practice they have a positive feedback. CBD products have improved the way of life of people since it have increased the life expectancy of many human beings.
One of the items that have ensured CBD products are produced efficiently and of high quality is the technological advancements. For many end users of the CBD products they have given the product thumbs up since of the good service they experience.
CBD products have experienced increased sales due to the growing population of customers. Investors and pharmaceutical companies have seen the CBD industry as a great catch in investing their capital. The developed companies have reaped so much profits in which it have attracted other investors.
Over the past years cannabis have been regarded as a drug but due to latest invention we can tell that it has many benefits. The urge of advertising the CBD products came as a result of the growing population and it served as an eye for potential market as this homepage suggests. Oil is an essential commodities extracted from cannabis and thus it covers many places in world. The oil extracted from cannabis is very effective to the body since it reduces the number of wrinkles on the body.
CBD products extract one of the most important items like oils which is in great demand since it has many users. For some products like medicinal products they are limited by a qualified personnel. For medicinal purpose CBD products come with separate form. Medicinal products which are formed from the CBD products are designed differently. CBD products like oils medicines are a product that need to be levied in the market.


Over the past several weeks, we've seen millions of our Fans like comments on ourCoca-ColaFacebook Page requesting that we turn our cans pink and donate the proceeds to breast cancer research. We're big supporters of the cause and appreciate that our Fans are passionate about it, too. While changing the color of our cans would have required a long lead time, we think the sentiment behind the creative idea is that our Fans want us to show our support in a tangible way.
The good news is that, as a company, we are already actively involved with two of the leading breast cancer organizations. Powerade and Sprite Zero are actively supporting the American Cancer Society through ChooseYou.com, a national movement created by the American Cancer Society that encourages women to put their own health first in the fight against cancer. For everyone who visits ChooseYou.com, and who "Likes" Choose You on Facebook, POWERADE ZERO will contribute $1 to the American Cancer Society up to $100,000.
In addition, FUZE has specially-marked packages that are supporting Susan G. Komen for the Cure.
Thanks for being a fan and helping to make a difference together.
L. Celeste Bottorff is VP, Living Well at The Coca-Cola Company.


Penguin Cafe was founded in 2009 by Arthur Jeffes, following in the footsteps of his father, Simon Jeffes of the iconic Penguin Cafe Orchestra. Arthur formed Penguin Cafe with a brand new line-up, bringing together a talented and disparate group of musicians from the likes of Suede, Gorillaz and Razorlight.
Three albums followed: A Matter of Life in 2008, The Red Book in 2014 and The Imperfect Sea released on Erased Tapes in 2017. The same year Arthur paid tribute to his late father by performing PCO's seminal record Union Cafe live to a sold out Union Chapel, coinciding with the album's re-issue on Erased Tapes.
2018 saw the Penguins perform in Paris, Berlin and London with a special show to support Greenpeace at the new venue EartH in Hackney. Arthur and his group are back in the studio creating their forthcoming fifth studio album, due for release in autumn 2019.


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text:
The Takedown Of Silk Road
by Hired Power | Dec 16, 2015 | Addiction Treatment & Recovery, Assessment & Services, Drug Facts & Resources | 0 comments
They say that a good enough hacker can trace anything on the Internet…unless a better hacker is trying to hide it. For over two years, the hacker extraordinaire known as The Dread Pirate Roberts proved to be the one nobody else could trace. Through a combination of tumbling software, internet currency, and anonymous identities, he established an anonymous drug-trading site that ultimately netted him over $80 million.
What Was Silk Road?
Silk Road was an anonymous website where drug sellers and drug buyers could connect and do business. It's part of a "dark side" network of internet sites that don't come up on Google, and are accessed through software that passes through so many different servers that the subscribers' identities are untraceable. Or virtually untraceable. The FBI called it "the most sophisticated and extensive criminal marketplace on the Internet today" (USA Today, May 15, 2104).
Who Was the Dread Pirate Roberts?
This website was established by a computer programmer in his late 20s named Ross Ulrich. He created the site on the anonymously accessed dark webs in 2011, and for two years drug buyers and sellers from all over the world used his almost completely secure site to exchange billions of dollars in merchandise. Ulrich was convicted of several serious charges, including drug trafficking, money laundering, hacking, and later even hiring a hitman to assassinate an employee he thought had stolen from him. Ulrich was convicted of all charges and sentenced to life in prison.
From Bitcoin to Billions
When Ulrich's laptop was seized by the FBI, they found millions of dollars of bitcoin in his personal wallet. Bitcoin is untraceable internet currency, and it was the money used for buying and selling drugs on Silk Road. Like the software Tor tumbled the connections between private servers and Silk Road servers, a bitcoin tumbler made it nearly impossible to trace bitcoin to the real accounts of specific people. Users' identities were completely secure and their money protected until the FBI was able to figure it out.
How Does the Takedown of Silk Road Affect Us?
The FBI eventually took down Silk Road and put most of its employees in jail. But the investigation revealed a whole world of drug availability that simply hadn't been on the radar for most law enforcement. But as with most things, the criminal elements were far ahead of law enforcement, creating a whole world in which drugs could flow easily and anonymously with few repercussions.
The fight against drugs, from suppliers to dealers to users, is never ending for law enforcement. While the FBI discovery and bust of Silk Road made a major dent in the worldwide drug trade, addicts will always find ways to get more, and unscrupulous dealers will always find ways to profit off their sickness.
If you or someone you love is struggling with drug addiction, the addiction help lines at Hired Power are available 24/7. Call us at 800-910-9299 for more information on overcoming addiction.


text:
.class public Landroid/app/Fragment$SavedState;
.super Ljava/lang/Object;
.source "Fragment.java"

# interfaces
.implements Landroid/os/Parcelable;

# annotations
.annotation system Ldalvik/annotation/EnclosingClass;
    value = Landroid/app/Fragment;
.end annotation

.annotation system Ldalvik/annotation/InnerClass;
    accessFlags = 0x9
    name = "SavedState"
.end annotation

# static fields
.field public static final CREATOR:Landroid/os/Parcelable$ClassLoaderCreator;
    .annotation system Ldalvik/annotation/Signature;
        value = {
            "Landroid/os/Parcelable$ClassLoaderCreator",
            "<",
            "Landroid/app/Fragment$SavedState;",
            ">;"
        }
    .end annotation
.end field

# instance fields
.field final mState:Landroid/os/Bundle;

# direct methods
.method static constructor <clinit>()V
    .locals 1

    .prologue
    .line 498
    new-instance v0, Landroid/app/Fragment$SavedState$1;

    invoke-direct {v0}, Landroid/app/Fragment$SavedState$1;-><init>()V

    sput-object v0, Landroid/app/Fragment$SavedState;->CREATOR:Landroid/os/Parcelable$ClassLoaderCreator;

    return-void
.end method

.method constructor <init>(Landroid/os/Bundle;)V
    .locals 0
    .parameter "state"

    .prologue
    .line 477
    invoke-direct/range {p0 .. p0}, Ljava/lang/Object;-><init>()V

    .line 478
    iput-object p1, p0, Landroid/app/Fragment$SavedState;->mState:Landroid/os/Bundle;

    .line 479
    return-void
.end method

.method constructor <init>(Landroid/os/Parcel;Ljava/lang/ClassLoader;)V
    .locals 1
    .parameter "in"
    .parameter "loader"

    .prologue
    .line 481
    invoke-direct/range {p0 .. p0}, Ljava/lang/Object;-><init>()V

    .line 482
    invoke-virtual {p1}, Landroid/os/Parcel;->readBundle()Landroid/os/Bundle;

    move-result-object v0

    iput-object v0, p0, Landroid/app/Fragment$SavedState;->mState:Landroid/os/Bundle;

    .line 483
    if-eqz p2, :cond_0

    iget-object v0, p0, Landroid/app/Fragment$SavedState;->mState:Landroid/os/Bundle;

    if-eqz v0, :cond_0

    .line 484
    iget-object v0, p0, Landroid/app/Fragment$SavedState;->mState:Landroid/os/Bundle;

    invoke-virtual {v0, p2}, Landroid/os/Bundle;->setClassLoader(Ljava/lang/ClassLoader;)V

    .line 486
    :cond_0
    return-void
.end method

# virtual methods
.method public describeContents()I
    .locals 1

    .prologue
    .line 490
    const/4 v0, 0x0

    return v0
.end method

.method public writeToParcel(Landroid/os/Parcel;I)V
    .locals 1
    .parameter "dest"
    .parameter "flags"

    .prologue
    .line 495
    iget-object v0, p0, Landroid/app/Fragment$SavedState;->mState:Landroid/os/Bundle;

    invoke-virtual {p1, v0}, Landroid/os/Parcel;->writeBundle(Landroid/os/Bundle;)V

    .line 496
    return-void
.end method


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United Nations High Commissioner for Refugees financial definition of United Nations High Commissioner for Refugees
https://financial-dictionary.thefreedictionary.com/United+Nations+High+Commissioner+for+Refugees
Also found in: Dictionary, Acronyms, Wikipedia.
Related to United Nations High Commissioner for Refugees: UNICEF
Also called UNHCR. An organization created by the United Nations in 1950 and charged with providing assistance to and protection of persons displaced by a government as the result of a war, persecution or another reason. It helps them return to their homes or to settle in another country.
United Nations High Commissioner for Refugees
A statement by his office said that al-Jubouri met today with representative of the United Nations High Commissioner for Refugees UNHCR Bruno Guido, and discussed with him, the UN's efforts to provide humanitarian aid to the displaced families and provide humanitarian support through the provision of all necessary supplies to alleviate their suffering.
Al-Jubouri calls upon the United Nations High Commissioner for Refugees (UNHCR) to contribute to broader reconstruction in the liberated areas
"With the transition in Afghanistan in 2014, the need for humanitarian assistance may very well increase," said the statement by the United Nations High Commissioner for Refugees.
UN refugee chief to visit Iran for talks about Afghans
United Nations High Commissioner for Refugees (UNHCR) Goodwill Ambassador Angelina Jolie (R) visits a refugee camp in the southern Turkish town of Altinozu in Hatay province June 17, 2011.
Angelina Jolie Travels to Turkey to visit Syrian Refugees
Summary: Geneva - The United Nations High Commissioner for Refugees (UNHCR) expressed, on Monday, "disappointment" following the prevention by the polisario of 20 Moroccan beneficiaries of the family-visit flights programme from disembarking at the Tindouf airport.
UNHCR disappointed at prevention of 20 beneficiaries of family-visit flights from entering Tindouf
The Office of the United Nations High Commissioner for Refugees (UNHCR) has reported that in 2006, refugee numbers rose for the first time since 2002.
Refugee numbers still rising
GENEVA -- Internal politics affects the work of international humanitarian agencies, as was demonstrated when the United Nations High Commissioner for Refugees was expelled from Indonesia at the end of March.
UNHRC allowed back into Aceh but under government's watchful eye
According to the United Nations High Commissioner for Refugees, up to 500 people are displaced in Colombia daily, creating a situation so grave that only Sudan and the Congo are blighted by worse humanitarian crises.
Worst humanitarian crisis in the Western hemisphere
Sponsored by the United Nations High Commissioner for Refugees, Goodwill Ambassador Angelina Jolie will offer a prize to the winner in each category.
World Refugee Day Poster Contest. (Announcements)
In 1981, when Afghanistan was at center stage in the Cold War, the United Nations High Commissioner for Refugees (UNHCR) spent $109 million for refugees here.
Afghan refugees find hope in camps: drought, wars drive Afghans to Pakistan
In 1954 and 1931, it was given to the Office of the United Nations High Commissioner for Refugees (UNHCR), in 1961 to United Nations Secretary-General Dag Hammarskjold, in 1965 to UNICEF, and in 1988 to the United Nations Peacekeeping Forces.
UN and Annan Win Nobel Peace Prize
Shortly after returning to her work as a corporate lawyer in Montreal, Canada, she received a phone call from the Office of the United Nations High Commissioner for Refugees (UNHCR).
Inside the `perimetre cellulaire': (Amah Assiama's work in Rwanda)
THE United Nations High Commissioner for Refugees yesterday issued a plea for the plight of millions of destitute Afghans not to be forgotten in the rush towards military action.
The plight of millions of destitute Afghans not to be forgotten
Unit Load
Unit of trading
unit sales
unit share
Unit Share Investment Trust
United Nations General Assembly Hall
United Nations General Assembly Official Records
United Nations General Assembly Special Session
United Nations Genocide Convention
United Nations Geographic Information Working Group
United Nations Geophysical Year
United Nations Girls' Education Initiative
United Nations Global Alliance for ICT and Development
United Nations Global Compact Office
United Nations Global Defense Act
United Nations Global Defense Initiative
United Nations Global Initiative to Fight Human Trafficking
United Nations Global Marketplace
United Nations Global Occult Coalition
United Nations Global Road Safety Week
United Nations Godzilla Countermeasures Center
United Nations Good Offices Commission
United Nations Good Offices Mission in Afghanistan and Pakistan
United Nations Group of Experts on Geographical Names
United Nations Group on the Information Society
United Nations Guard Contingent in Iraq
United Nations Guidelines for Trade Data Interchange
United Nations Guidelines on Consumer Protection
United Nations Habitat and Human Settlements Foundation
United Nations Headquarters
United Nations High Commission for Refugees
United Nations High Commissioner for Refugees, Office of the
United Nations High-Level Dialogue
United Nations Hotel
United Nations Housing Rights Programme
United Nations Human Development
United Nations Human Development Index
United Nations Human Development Report
United Nations Human Rights Commission
United Nations Human Settlements Program
United Nations Humanitarian Affairs Officer
United Nations Humanitarian Air Services
United Nations Humanitarian Coordinator
United Nations Humanitarian Response Depot
United Nations Independent Internship Network
United Nations India-Pakistan Observation Mission
United Nations Industrial Development Fund
United Nations Industrial Development Office


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South Korean Sensation, IU, Buys Penthouse Amounting to 11 Million Dollars!
by Victoria Marian Belmis / Jun 04, 2021 06:38 AM EDT
On the 1st of May, multiple news outlets dropped reports confirming that EDAM Entertainment's very own IU, recently bought a multi-million dollar property. Netizens and Uaenas all over the world are happy for the singer, actress, and song-writer.
Just this February of this year, IU went on to buy a unit in Eterno Chungdam in Seoul, South Korea. IU's new unit complex is notably brand new since its construction will be finished in December of 2022. IU's united to reportedly the highest valued apartment unit in the area.
IU's new unit was obviously sold to her and is notably worth 13 billion won, approximately 11 million dollars. It was reported that IU went on to file an application for residency at the Gangnam City Office.
EDAM Entertainment's IU is projected to transfer to her new home very soon.
As per multiple reports, IU decided on the 243 square meter unit which is found above the 10th floor.
Previously in 2019, IU went on to sell her villa in Bangbaedong. She spent 7 long and eventful years living in her aforementioned villa. It should be noted that IU is included in the list of South Korean celebrities who have recently purchased new properties this year.
With IU, BTS's very own, RM and Jimin, also went on to buy their own apartment units and South Korean actress, Song Hye Kyo, and South Korean actor, Lee Seung Gi, also went on to purchase new homes this year.
Looking extremely lavish and luxurious, IU's new home made fans swoon over its beauty. Uaenas are really happy for IU as she is known to be one of the most giving South Korean celebrities today.
Previously on the 16th of May, IU went on to celebrate her 28th birthday by donating to a plethora of charities and the needy.
Tags: kwave, kwave news, kwave updates, Kpop, kpop news, Kpop updates, EDAM, EDAM artists, Edam Entertainment updates, Edam Entertainment, Edamt Entertainment news, Edam Entertainment IU, IU, IU news, IU Updates, IU new home, IU new house, BTS, BTS RM, BTS Jimin, RM, Jimin, Song Hye Kyo, Lee Seung Gi


text:
The Nationals WA
The Nationals are the only party dedicated to fighting for the communities of regional WA
The Young Nationals
Join and Renew Membership
$2.56 million boost to aged care in Jurien Bay
$2.56 million boost to aged…
Aged care in Jurien Bay will receive a significant boost with RSL Care to receive a $2.564 million grant, made possible by the Royalties for Regions program.
The funding will see the former Central Coast Senior Citizens Centre transformed into Turquoise Coast Respite Solutions 24/7 for use by residents of Jurien Bay and surrounding areas.
Member for Moore Shane Love MLA said there was a desperate need for a respite facility that will allow the elderly and those who care for them to remain in their local community.
"For the first time in the Jurien Bay district, residents can take comfort knowing that support will be available all day every day for our elderly and their carers," he added.
"Alternative respite options are currently available in Perth and Geraldton – nearly 200 kilometres away – which makes it very difficult for aged patients and those who care for them."
The Turquoise Coast respite facility will house five bedrooms and a day use area and have facilities for a nurse to stay onsite.
Mr Love said the project would make good use of existing infrastructure that is centrally located and would provide day time and overnight respite options with the ability to take patients with dementia.
"Collaboration and investment in age-appropriate health services is fundamental to the ongoing growth of the Central Coastal region and to allow the elderly to remain independent, involved and contributing members of their communities," he said.
"This approach benefits the person, their family and friends and the community-at-large that is richer for having older people functioning in the community."
Mr Love said the need for such a facility had been well documented as a priority project in the Jurien Bay Growth Plan.
"RSL Care Jurien Bay were able to demonstrate that they could enhance facilities and services that would help local people stay in the community as they age," Mr Love said.
"It's great to see Royalties for Regions investing in projects that enable ageing community members to remain in their community for as long as possible."
Category: News Archive 8 November 2016
PreviousPrevious post:Moore Community pools sparkle with fundingNextNext post:Grills welcomes nearly $900,000 for 31 local community pools
Regional voices from Moore silenced by new laws
Mid West health in crisis: Love
Contact | Privacy | Accessiblity
Authorised by D Rodgers, The Nationals WA, 1 Graylands Rd, Claremont WA 6010


Bill Monigold, Executive Chef and Restaurant Manager at JJ Hills Fresh Grill at Icicle Village Resort, comes from a long background of serving customers and specializes in meeting guests' needs in the restaurant and catering functions.
Bill was born in Germany, then grew up and lived in Alaska until 1980. While in Alaska he went to Tanana Valley Community College on the campus of the University of Alaska. There he studied in the Fairbanks Culinary arts program under Richard Donnelly, who was trained in France and Switzerland.
In the early 80's Bill worked in Southern California in the Orange County area and learned a great deal about seafood preparation. He came to Leavenworth in 1982 and has lived here since that time. This is where he met his wife and they raised their children.
Bill has also worked for Walter Wilmonth, who developed Johnny's seasoning salt, and spent 10 years at the Leavenworth Golf Club as Chef and Restaurant manager.
Bill joined the Icicle Village Resort in March 2011. His specialties include Schnitzel ala Swiss, and Grill Northwest Salmon basted with Herb Butter along with others that are included in our Fresh Grill menu.


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Barry Friend (born 13 October 1951) is an English former professional footballer who played in the Football League for Fulham. He also played non-league football in the London area for clubs including Leatherhead, Wimbledon, with whom he won the Southern League title in 1977, Slough Town, Carshalton Athletic and Tooting & Mitcham United. He played as a winger or midfielder. In the summer of 1976, he played abroad in Canada's National Soccer League with Ottawa Tigers.

References

1951 births
Living people
Footballers from Wandsworth
English footballers
Association football wingers
Fulham F.C. players
Leatherhead F.C. players
Wimbledon F.C. players
Tooting & Mitcham United F.C. players
Slough Town F.C. players
Carshalton Athletic F.C. players
English Football League players
Southern Football League players
Isthmian League players
Canadian National Soccer League players


text:
Scottish Schools Adolescent Lifestyle and Substance Use Survey (SALSUS): alcohol report 2018
Population Health Directorate
Education, Health and social care, Law and order
Findings on alcohol from the 2018 wave of the Scottish Schools Adolescent Lifestyle and Substance Use Survey (SALSUS).
Scottish Schools Adolescent Lifestyle and Substance Use Survey (SALSUS)
1 Introduction and background
2 Prevalence and key trends
3 Source of and availability of alcohol
4 Attitudes to alcohol use and alcohol education
5 Risk and protective factors for alcohol use
Appendix A: Base Tables
This report presents the alcohol findings from the 2018 wave of the Scottish Schools Adolescent Lifestyle and Substance Use Survey (SALSUS). The research was commissioned by the Scottish Government and carried out by Ipsos MORI Scotland.
Survey background
SALSUS is a continuation of a long established series of national surveys on smoking, drinking and drug use. These were carried out jointly in Scotland and England between 1982 and 2000, to provide a national picture of young peoples' smoking (from 1982), drinking (from 1990), and drug use (from 1998) within the context of other lifestyle, health and social factors. Since 2002, Scotland has developed its own, more tailored survey known as SALSUS.
Survey purpose
SALSUS informs progress towards Scottish Government policies to reduce the harms from smoking, drinking and drug use among children and young people.
The survey series also provides local prevalence rates for smoking, drinking and drug use across Alcohol and Drug Partnerships (ADPs), local authorities and NHS Boards.
Policy background
The level of harms from alcohol in Scotland is high in comparison to the rest of the UK and internationally. Reducing the harms caused by alcohol is one of Scotland's six public health priorities[2](along with reducing harms from smoking and drug use). Action has been taken to reduce the harms by successive Scottish Governments as outlined in Figure 1.1.
In 2009, a whole population approach was taken, and the then national alcohol strategy[3], Changing Scotland's Relationship with Alcohol: A Framework for Action, was published. This adopted the World Health Organization's prevention measures for alcohol of affordability, availability, attractiveness. Under this strategy, the Scottish Government's actions included legislating to ban irresponsible promotions; introduction of a multi-buy discount ban; introduction of an age verification policy such as Challenge 25; and introduction of minimum unit pricing.
Figure 1.1 Scottish alcohol policy timeline (2002-2016)
Alcohol Framework 2018: Preventing Harm
In November 2018, a refreshed Alcohol Framework[4] was published, which builds on the previous Framework and has three central themes:
1. reducing consumption
2. positive attitudes, positive choices
3. supporting families and communities
The fourth theme in the previous Framework of 'improved treatment and support' now sits within the 2018 drug and alcohol treatment strategy[5].
There are two consistent threads running through the Framework: reduce health inequalities, and protect children and young people. For the latter, this means that all work on preventing underage drinking, marketing and advertising, education in schools, positive alternative opportunities and safer communities, and preventing alcohol-related violence and crime all aim to protect children and young people. Action 1 in the Framework states "We will put the voices of children and young people at the heart of developing preventative measures on alcohol." In practice, this means that measures will be developed with children and young people and not imposed upon them. The views of children and young people will be sought to help shape the policy.
Key actions in the Framework include:
Evaluating minimum unit pricing and reviewing the price after 1 May 2020;
Pressing the UK Government to impose a 9pm watershed for alcohol advertising on TV as well as restrictions on cinema advertising;
Consulting on the suitability of restrictions on alcohol marketing to protect children and young people;
Running a social marketing campaign on the alcohol low risk drinking guidelines of 14 units per week – the first phase of the count14 campaign ran in 2019;
Pressing alcohol producers to put health information on labels.
Current key policies relating to alcohol include: the Licensing (Scotland) Act 2005, the Alcohol etc. (Scotland) Act 2010, the Alcohol (Minimum Pricing) (Scotland) Act 2012 and the Air Weapons and Licensing (Scotland) Act 2015. Figure 1.2 outlines the key points from each that are relevant to young people.
Figure 1.2 Key legislative measures affecting young people
Further information about policy relating to alcohol is available at:
NHS Health Scotland:
http://www.healthscotland.com/topics/health/alcohol/index.aspx
Scottish Government:
https://www.gov.scot/policies/alcohol-and-drugs/
SALSUS is a self-completion survey administered by teachers in a mixed ability class, under exam conditions. In the past the survey has been completed on paper, but in 2018 schools were given the choice to complete the survey online or on paper.
A random, nationally representative sample of S2 and S4 pupils in Scottish schools was drawn with classes as the primary sampling unit. All local authority and independent schools in Scotland were eligible for inclusion in the sample, with the exception of special schools.
Fieldwork was completed between October 2018 and April 2019. A total of 12,558 S2 and 10,807 S4 pupils responded (including schools that took part in the Realigning Children's Service Survey).
The overall response rate was 52% (excludes schools that took part in the Realigning Children's Services Survey and Glasgow state schools).
Data was weighted by local authority, age, sex, school sector (state/independent), school denomination and by urban/rural classification.
Throughout the report pupils in S2 are referred to as '13 year olds' and S4 pupils are referred to as '15 year olds' for ease. It should be borne in mind that some pupils within these categories may be slightly older or younger.
Some pupils did not answer each question. Where answers are missing, these have been excluded from the analysis and so charts and tables that describe the same population may have varying bases. When differences between estimates are specifically commented on in the report, these differences are statistically significant to the level of 0.05.
Percentages may not add up to 100% due to rounding.
For full details of the methodology, please see the SALSUS 2018 Technical Report[6].
Finally, it is important to note, that while there are associations between many of the behaviours explored in this report, conclusions about causality cannot be drawn.
Changes to the questionnaire
No alterations were made to the alcohol questions for 2018, so they are the same as in the 2015 survey. For further details on other question changes and survey methodology see the SALSUS 2018 Technical Report and the full 2018 questionnaire[7].
Email: salsus@gov.scot


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Global vulnerability to sea-level rise and coastal flooding strongly underestimated
November 4th, 2019 | Download as PDF
Photo: Miami beach (Robert Pittman, www.flickr.com)
Estimates of coastal zone elevation
In large parts of the world, high-quality (airborne) land elevation data are unavailable or expensive. As an alternative, satellite-based data can be used. These data are available for parts of the globe that are home to 99.7% of the world population. The quality of these data suffers from the fact that satellites measure the elevation of upper surfaces and not bare earth terrain. The satellites measure the height of trees and buildings, and not the land surface. These data, therefore, have a positive bias when used to represent land elevation, especially in densely vegetated and in densely populated areas. Mean bias can be several metres for land areas with an elevation in between 1 and 20 m.
The elevation of densely populated coastal zones appears to be much lower than has been assumed in many studies so far. When quantifying the number of people exposed to sea-level rise, a positive bias of a few metres results in strong underestimations.
This problem has been addressed recently by using neural network techniques to correct the data. As a result, the bias in elevation was reduced from a couple of metres to less than a few decimetres. For coastal cities such as Miami, New York City, and Boston, for instance, vertical bias was reduced from 4.71 m to less than 0.06 m. Needles to say that a global assessment of the number of people exposed to coastal flooding based on these data paints a completely different picture compared to studies in the past.
Estimates of number of people exposed
With these new data on elevation, vulnerabilities have been updated. In this update, coastal defences are not considered since location data of the defences are not available at the global scale. Changes in population growth and migration are also not considered; the results indicate threats relative to present development patterns.
Current vulnerabilities, updated
The new data show that, for the present day, 110 million people live on land below the current high tide line, globally, much higher than the previous estimate of 28 million. 250 million people now live on land below annual flood levels, again much higher than the previous estimate of 65 million.
Future vulnerabilities, updated
The new elevation data triple the estimates of global vulnerability to sea-level rise and coastal flooding. The projected rise of the current high tide line under a high-end scenario of climate change will increase the number of people living on land below this line from 110 million today to 190 million (range: 150–250 million) in 2100. Under this high-end scenario, the number of people living on land below annual flood levels is projected to increase from 250 million people now to 340 million people for mid-century, and 630 million people for 2100.
If we would succeed in keeping global warming below 2°C, and the Antarctic ice sheet would not become unstable, the number of people living on land below annual flood levels would still be 360 million in 2100.
It was previously estimated that currently about 640 million people live in the low elevation coastal zone, defined as areas below 10 m. With the new elevation data, this estimate rises to just over one billion people.
Asia most vulnerable
The new elevation data paint a particularly grim picture for several Asian countries. Bangladesh, India, Indonesia, and the Philippines see a 5-fold to 10-fold change in estimated current populations below the projected high tide line after applying these new data.
More than 70% of the total number of people worldwide currently living on implicated land are in eight Asian countries: China, Bangladesh, India, Vietnam, Indonesia, Thailand, the Philippines, and Japan. Chronic coastal flooding or permanent inundation threatens areas occupied by more than 10% of the current populations of nations including Bangladesh, Vietnam, and many Small Island Developing States by 2100.
Implications of the new data
The authors of this study conclude that coastal communities worldwide must prepare themselves for much more difficult futures than may be currently anticipated. Sea-level rise this century may induce large-scale migration away from unprotected coastlines, even in the US. Large-scale migration may pose serious challenges to political stability, and may lead to more conflict.
Source: Kulp and Strauss, 2019. Nature Communications 10.
Related news in the category Coastal erosion and coastal floods:
Multi-century sea level rise may lead to unprecedented threats to coastal cities
Frequency of extreme sea levels will increase dramatically in many parts of the world's coasts
How will different rates of sea-level rise determine the future of the Wadden Sea?


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