text:
\section{Introduction}\label{sec:intro}

This is the third in a series
of studies on the dynamical evolution of globular star clusters
by using Fokker-Planck (FP) models which allow velocity anisotropy.
In the preceding two papers,
pre-collapse (Takahashi 1995, Paper I) and post-collapse evolution (Takahashi 1996, Paper II) of isolated, single-mass clusters was studied.
In this paper, as a natural extension of those works,
we study the evolution of multi-mass clusters
(clusters with a stellar-mass function).
We especially pay attention to the development of the velocity anisotropy of each mass-component.

Direct numerical integration of the FP equation (Cohn 1979, 1980)
has been the most important tool of the study of globular cluster evolution.
Various factors such as the mass function, the heating effects of binaries and the galactic tidal field,
which are expected to be important for the evolution of real globular clusters,
were incorporated into FP simulations.
However, velocity anisotropy was usually neglected
because of numerical difficulties in the integration of the two-dimensional FP equation (Cohn 1985; Paper I).
Most of the difficulties can be removed by using the improved integration scheme described in Paper I\@.

For the above reason,
although the evolution of multi-mass clusters has been investigated by many authors
(e.g., Inagaki, Saslaw 1985; Chernoff, Weinberg 1990; Murphy et al.\ 1990;
Lee et al.\ 1991)
by using {\it isotropic} FP models,
the development of the anisotropy in multi-mass clusters has seldom been discussed.
Only recently, it was discussed by Spurzem and Takahashi (1995)
as well as Giersz and Heggie (1996) to some extent.
Spurzem and Takahashi (1995) compared anisotropic gaseous models,
isotropic FP models, and $N$-body models for the evolution of
two-component clusters.
At that time anisotropic FP models were not available.
Giersz and Heggie (1996) performed $N$-body simulations for small-$N$
multi-mass clusters ($N$=250, 500, and 1000).
All of their simulations started with the same power-law initial mass
function.
They combined statistically the results from many simulations.
However, it is still difficult to see the evolution of the anisotropy
because of large statistical fluctuations,
especially for massive components comprising very small numbers of
particles.
In this paper we present the results of anisotropic FP simulations for simple
two-component clusters as well as clusters with a realistic power-law
mass function.
FP simulations do not suffer from the problem of statistical
fluctuations.
Our results clearly show how the evolution of the anisotropy depends on the
stellar mass and the initial mass function.

In fitting observational data to theoretical models,
King models (King 1966) and their extensions have been used most frequently.
The mass function and velocity anisotropy are incorporated in
multi-mass King-Michie models (e.g., Gunn, Griffin 1979).
In these models
the distribution function of each component depends on the specific angular momentum $J$ through the factor $\exp [-J^2/(2r_{\rm a}^2\sigma^2)]$,
where $r_a$ is the anisotropy radius and $\sigma$ is the velocity dispersion;
radial anisotropy is significant for $r \gtsim r_{\rm a}$.
The choice of this form of angular momentum dependence is rather arbitrary.
For example, $r_{\rm a}$ can depend on mass components,
but it is usually set identical for all components for model simplicity.
Gaseous model simulations by Spurzem and Takahashi (1995) and
our FP simulations show that the states of velocity anisotropies are significantly different between different components in some cases.
In fact the tangential velocity dispersion becomes dominant
around the half-mass radius for massive components in a cluster with a steep mass function.
Therefore, anisotropic King-Michie models are not always
useful extensions of isotropic King models.

In section 2, the basic equations and initial conditions are described.
The results of our simulations are presented in section 3.
The conclusions and discussion are given in section 4.
In the Appendix
the diffusion coefficients for the multi-mass anisotropic FP equation are given.

\section{Fokker-Planck Models}

\subsection{Basic Equations}

We assume that star clusters are spherically symmetric and isolated from
other systems.
We take account of the mass function of stars.
For computational convenience, the mass function is represented by
a set of discrete mass components.
The number density of the $i$th component
(of the individual stellar mass $m_i$) in $\mu$-space is denoted by
$f_i({\bf r},{\bf v},t)$.
In a spherical system in dynamical equilibrium, the distribution function is a function of only
the energy per unit mass ($E$) and the modulus of the angular momentum per unit mass ($J$).
We define the scaled angular momentum $R$ as
\begin{equation}
R = \frac{J^2}{J_{\rm c}^2(E)} \,,
\end{equation}
where $J_{\rm c}(E)$ is the angular momentum of a circular orbit of energy $E$.
The number density of the $i$th component in $(E,R)$-space, $N_i(E,R)$,
 is given by
\begin{eqnarray}
  N_i(E,R) &=& 4\pi^2 P(E,R) J_{\rm c}^2(E) f_i(E,R) \nonumber \\
         &\equiv& A(E,R)f_i(E,R)
\end{eqnarray}
(Cohn 1979).
Here, $P(E,R)$ is the orbital period,
\begin{equation}
P(E,R) \equiv
2\int_{r_{\rm p}}^{r_{\rm a}} \frac{dr}{v_{\rm r}} \,,
\end{equation}
where $v_{\rm r}=\{2[\phi(r)-E]-J^2/r^2\}^{1/2}$,
$\phi(r)$ is the gravitational potential,
and $r_{\rm p}$ and $r_{\rm a}$ are the pericenter and apocenter radii, respectively.

The multi-mass FP equation under a fixed
potential can be written in a flux-conserving form (cf. Cohn 1979),
\begin{equation}
A \frac{\partial f_i}{\partial t} =
- \frac{\partial F_{E i}}{\partial E} - \frac{\partial F_{R i}}{\partial R}
\label{eq:fp} \,,
\end{equation}
where
\begin{eqnarray}
-F_{E i} & = &   D_{E i} f_i
+ D_{EE i} \frac{\partial f_i}{\partial E}
+ D_{ER i}\frac{\partial f_i}{\partial R}
\,, \nonumber \\
-F_{R i} & = &   D_{R i} f_i
+ D_{RE i}\frac{\partial f_i}{\partial E}
+ D_{RR i}\frac{\partial f_i}{\partial R} \label{eq:flux} \,.
\end{eqnarray}
The expressions for coefficients $D_{EE i}, D_{E i}$, etc. are given in the Appendix.

The gravitational potential is determined from Poisson's equation,
\begin{eqnarray}
\nabla^2\phi
&=& - 4\pi G \sum_i \rho_i    \nonumber \\
&=& - 4\pi G \sum_i m_i \int f_i d^3{\bf v} \,,
\end{eqnarray}
where $G$ is the gravitational constant.

We include the heating effects by three-body binaries
and use the heating rate formula of Lee et al. (1991,
see also Drukier et al.\ 1992; Grabhorn 1992).
In their formulation,
the total heating rate per unit volume by three-body binaries is given by
\begin{equation}
\dot{E}_{\rm tot}
= C_{\rm b} G^5 \left( \sum_i \frac{n_i m_i^2}{\sigma_i^3} \right)^3
\sigma_0^2 \,,
\end{equation}
where $n_i$, $m_i$, and $\sigma_i$ are the number density, stellar mass, and one-dimensional velocity dispersion, respectively, of the $i$th component,
and $\sigma_0^2$ is the density-weighted central velocity dispersion.
The constant $C_{\rm b}$ was set to 90 in this study as usual.
The total heating rate is distributed to each component in proportion to the mass density such that
\begin{equation}
\dot{E}_i = \frac{\rho_i}{\rho_{\rm tot}} \dot{E}_{\rm tot} \,,
\end{equation}
where $\rho_{\rm tot}$ is the total density.
The orbit-averaged heating rate (per unit mass)
for each component used in the FP equation is given by
\begin{equation}
\langle \dot{E}_i \rangle_{\rm orb}
= \left. \int_{r_{\rm p}}^{r_{\rm a}} \frac{dr}{v_{\rm r}}
\frac{\dot{E}_{\rm tot}}{\rho_{\rm tot}}
\right/ \int_{r_{\rm p}}^{r_{\rm a}} \frac{dr}{v_{\rm r}} \,. \label{eq:oahr}
\end{equation}

\subsection{Multi-Mass Models}

We chose multi-mass Plummer's model (e.g. Spitzer 1987, p13) as the initial cluster model.
The distribution function of the $i$th component is
\begin{equation}
f_i(E,R)=\frac{24\sqrt{2}}{7\pi^3}\frac{r_0^2}{G^5M^5}\frac{M_i}{m_i}E^{7/2},
\end{equation}
where $r_0$ is a scale radius, $M$ the total mass of the cluster, and $M_i$ the
total mass of the $i$th component.
In the model, the velocity distribution is isotropic everywhere,
and the velocity dispersions for all components are equal,
i.e., there is no mass-segregation.
In real globular clusters,
just after the dynamical equilibrium was established after their
formation,
the velocity distribution was probably more or less anisotropic.
If globular clusters formed through the cold collapse of proto-clusters,
the radial velocity dispersion might exceed the tangential one on the
average.
We consider, however, only initially isotropic models in this study for
simplicity.
The equipartition of the velocity dispersions seems reasonable
initial conditions,
since violent relaxation does not produce mass segregation (Lynden-Bell 1967).

First, we consider two-component models.
They are simple, but very useful to understand the essential
features of the evolution of multi-component clusters.
Parameters of the models we studied are listed in table 1.
Each model is specified by three parameters, $m_2/m_1$, $M_2/M_1$,
and $N$ (total number of stars).
The evolution of similar models was calculated
by using anisotropic gaseous models by Spurzem and Takahashi (1995).

Next, we consider continuous mass-function models.
Let ${\cal N}(m)\,dm$ be the number of stars in the mass interval
$(m,m+dm)$.
We chose a simple power-law mass function,
\begin{equation}
{\cal N}(m)\,dm \propto m^{-\alpha} \,dm, \qquad
m_{\rm min} \leq m \leq m_{\rm max} \label{eq:mf} \,.
\end{equation}
We use $K$ discrete mass components,
and give the stellar mass of the $i$th component by
\begin{equation}
m_i = m_{\rm min}\left(\frac{m_{\rm max}}{m_{\rm min}}
      \right)^{(i-\frac{1}{2})/K} \qquad (i=1, 2, \dots, K) \,.
\end{equation}
The total mass of the $i$th component is
\begin{equation}
M_i=\int_{m_{i-\frac{1}{2}}}^{m_{i+\frac{1}{2}}} {\cal N}(m)m\,dm \,.
\end{equation}
Parameters of the power-law mass-function models are listed in table 2.
In all the models $m_{\rm max}/m_{\rm min}=10$ and the total number of
stars $N=10^5$.
Only the power-law index of the mass function, $\alpha$, is different
among the three models:
$\alpha=$1.5, 2.5, and 3.5 for models C1, C2, and C3
(Salpeter's mass function is $\alpha=2.35$).
We used $K=$10 components in all the simulations in the present study.
This component number is not very large,
but it is sufficient, at least, to see the qualitative features of the
evolution of clusters with the continuous mass function (cf. Chernoff,
Weinberg 1990).

\section{Results}

The results are presented in units such that
$G=M=1$ and ${\cal E}_{\rm i}=1/4$, where
${\cal E}_{\rm i}$ is the initial total binding energy
of the cluster.
The mean half-mass relaxation time $t_{\rm rh}$ is defined by
(Spitzer 1987, p40)
\begin{equation}
t_{\rm rh} = 0.138\frac{N^{1/2}r_{\rm h}^{3/2}}{\bar{m}^{1/2}G^{1/2} \ln
\Lambda},
\end{equation}
where $N$ is the total number of stars,
$r_{\rm h}$ is the radius containing half of the total mass,
$\bar{m}=M/N$ is the mean stellar mass,
and $\ln \Lambda$ is the Coulomb logarithm.
We set $\Lambda=0.11N$ (Giersz, Heggie 1994).
Time is expressed in units of the initial half-mass relaxation time $t_{\rm rh,i}$ for each model.

\subsection{Two-Component Clusters}

Figure 1a shows the evolution of the Lagrangian radii containing
1, 2, 5, 10, 20, 30, 40, 50, 75, and 90\% of the total mass of each component
for model T1.
Figures 1b and c are the same as figure 1a, but for models T2 and T3, respectively.
It is clear that mass segregation proceeds during the pre-collapse stage in each model.
The mass segregation develops most prominently
and the core collapse occurs most rapidly
(in units of the initial half-mass relaxation time $
t_{\rm rh,i}$ for each model)
in model T3.
During the post-collapse stage, on the other hand,
the mass segregation almost stops to proceed and the cluster expands nearly self-similarly (Murphy et al.\ 1990; Giersz, Heggie 1996).

Figures 2a1 and b1 show the evolution of the temperature, $T_i \equiv m_i \sigma_i^2$, where $\sigma_i$ is the {\it mean} one-dimensional velocity dispersion,
at the Lagrangian radii containing 1, 10, 20, 50, and 90\% of the total mass of the cluster ($M$), for model T1.
Figures 2a2 and b2 are for model T2, and figures 2a3 and b3 are for model T3.
The temperature of the heavy component at the central region rapidly decreases at first in every model.
This is due to the approach to the equipartition of energy by two-body relaxation.
The degree of the temperature decrease is largest in model T3,
and next largest in model T2.
The heavy component can lose the energy most easily in model T3,
because there are enough amount of light stars which receive the energy
and because the initial temperature difference between the two components is largest.

We measure the degree of velocity anisotropy by a quantity
\begin{equation}
\beta_i \equiv 1 - \sigma_{{\rm t}i}^2 / \sigma_{{\rm r}i}^2 \,,
\end{equation}
where $\sigma_{{\rm r}i}$ and $\sigma_{{\rm t}i}$ is the radial and tangential one-dimensional velocity dispersions, respectively, of the $i$th component.
Note that this anisotropy parameter is different from
the anisotropy parameter $A$ used in Papers I and II by a factor of 2.
Figures 3a1 and b1 show the evolution of $\beta_1$ and $\beta_2$, respectively,
 at the Lagrangian radii of the total mass of the cluster for model T1.
Figures 3a2 and b2 are for model T2, and figures 3a3 and 3b3 are for model T3.

In every model, the anisotropy of the light component develops in a similar way as in single-mass clusters (cf. figure 3 of Paper II).
The anisotropy does not penetrate into so inner regions in model T1 as in models T2 and T3,
because the light component does not collapse very much in model T1
as shown in figure 1a.
The development of the anisotropy of the heavy component is more interesting,
especially, in models T2 and T3.
$\beta_2$ at the inner regions becomes negative
(i.e. {\it tangential anisotropy} develops) at the early stages
(cf. Spurzem, Takahashi 1995).
This phenomenon is most clearly seen in model T3;
$\beta_2$ at the half-mass radius attains the minimum value of $-0.5$,
and $\beta_2$ becomes significantly negative even at the 90\%-mass radius.
It may be a surprise that such large tangential anisotropy appears at the outer part of the cluster.
The tangential anisotropy of the heavy component appears also in model T1 temporarily,
though its degree is very small.
As Spurzem and Takahashi (1995) discussed and we explain right below
again,
the appearance of the tangential anisotropy is closely related to the initial temperature differences between the mass components
and subsequent cooling of the heavy component.

Figure 4 shows the profiles of the radial and tangential temperatures,
$T_{{\rm r}i}$ and $T_{{\rm t}i}$,
at $t=1.5t_{\rm rh,i}$ in model T3.
Here we define the radial and tangential temperatures as
$T_{{\rm r}i} \equiv m_i \sigma_{{\rm r}i}^2$ and
$T_{{\rm t}i} \equiv m_i \sigma_{{\rm t}i}^2$.
For the heavy component, there are big humps in the profiles,
i.e., temperature inversions of large amplitudes appear.
Recall that the velocity dispersions of the two components are equal at the initial time.
At the early stage, the temperature of the heavy component drops to attain the equipartition of the energy, as seen in figure 2.
Since the local relaxation time increases with radius due to the density decrease,
the temperature drops most rapidly at the center.
Therefore, it can happen that the temperature decrease at regions around the core cannot catch up with the core temperature decrease,
and then a temperature inversion appears.
[Temperature inversions can appear also during post-collapse evolution
and trigger gravothermal oscillations (Bettwieser, Sugimoto 1984).]
Comparing the radial and tangential temperatures,
a larger temperature inversion appears in the tangential temperature,
because circular-orbit stars do not go further into the central region
and hardly reflect the central temperature decrease.
Therefore, the tangential velocity dispersion exceeds the radial one at this temperature-inversion region.
This situation is clearly seen in figure 4.
As the degree of the initial temperature decrease is larger,
the tangential anisotropy develops more.
Thus most significant tangential anisotropy develops in model T3.

Though we have already shown the evolution of the anisotropy at the Lagrangian radii in figure 3,
it is also instructive to show the evolution of the radial profile of the anisotropy.
This is shown in figures 5 and 6 for models T1 and T3.
The core radius $r_{\rm c}$ and the half-mass radius $r_{\rm h}$ are also indicated in the figures for reference.
Here we define the core radius as
\begin{equation}
r_{\rm c} \equiv \sqrt{\frac{9\sigma_0^2}{4\pi G\rho_0}} \,,
\end{equation}
where $\rho_0$ is the total central density
and $\sigma_0$ is the density-weighted central velocity dispersion
(cf. Spitzer 1987, p16).
In model T1, the anisotropy profiles of the two components are always similar.
On the other hand, in model T3, they are very different.
The anisotropy profile of the light component in model T3 is simple and similar to that in model T1.
As we already stated,
the most striking feature in the anisotropy of the heavy component
is the initial development of the tangential anisotropy outside the core.
The subsequent relaxation process produces high-energy heavy stars on radial orbits
and tends to erase the tangential anisotropy.
However, its trace can be observed
as a hollow in the anisotropy profile
around the half-mass radius
even after several tens of the initial half-mass relaxation time.

We also computed isotropic models corresponding to anisotropic models T1, T2 and T3 for comparison.
Mass segregation proceeds essentially in a similar way as in the anisotropic models.
Although rather strong anisotropy develops in the anisotropic models as shown in figure 3,
the evolution of the {\it mean} velocity dispersions (temperatures) in the anisotropic models is not very different from that in the isotropic models!
Figure 7 shows the evolution of the temperature of each component
at the Lagrangian radii containing 1, 10, 20, 50, and 90\% of the total mass of the cluster, for the isotropic model corresponding to model T3.
One noticeable difference between the isotropic and anisotropic models
appears in the temperature at the 90\%-mass radius;
it is lower in the anisotropic model.
This is because the halo is more expanded in anisotropic models (Papers I
and II).

\subsection{Clusters with A Continuous Mass Function}

Figures 8a, b, and c show the evolution of the central density of each component in models C1, C2, and C3.
We note that gravothermal oscillations occurred in model C1
when we used small enough time step which was comparable to the central
relaxation time (cf. Cohn et al.\ 1989; Breeden et al.\ 1994).
However, figure 8a presents the result of the computation in which longer time step was
used so as to suppress gravothermal oscillations artificially.
The use of the long time step largely reduced computational time and
enabled us to follow long-term evolution easily.
The evolution of the outer parts of the cluster is not affected by gravothermal oscillations very much,
and neither is the mean trend of the long-term core evolution
(cf. Lee et al.\ 1991).
In every model, mass segregation proceeds in the pre-collapse phase
and the central region soon becomes dominated by the massive components.
In the post-collapse expansion phase, however,
mass segregation almost stops to proceed
as in the cases of two-component clusters.

Figures 9, 10, and 11 show the evolution of the anisotropy profile of each component in models C1, C2, and C3.
Qualitative characteristics of the anisotropy evolution are the same as
those in two-component models.
The development of the anisotropies of light components is simple;
radial anisotropies ($\beta>0$) develop and $\beta$ increases with the radius except for the outermost regions.
The development of the anisotropies of heavy components is more complicated;
these radial profiles fluctuate,
and strong tangential anisotropies ($\beta<0$) develop in models with a
steep mass-function such as C2 and C3.
The development of tangential anisotropies is directly related to
the initial temperature decrease toward energy equipartition,
as we described in section 3.1.
The degree of the initial temperature decrease is largest in model C3,
because the relative amount of heavy components is smallest.
The anisotropy $\beta$ of the heaviest component attains the minimum value of
$\beta \approx -1$ ($\sigma_{\rm t}^2/\sigma_{\rm r}^2 \approx 2$) in model C3
around the half-mass radius.
We also note that perfect isotropy is always established inside the core radius in all the models.

In model C1 the difference in the anisotropy profile between mass components is relatively small.
In model C3, on the other hand, the anisotropy profile strongly depends on the stellar mass.
The radial anisotropy develops for light components and the tangential anisotropy does for heavy components.
As a natural consequence of this,
for intermediate-mass components
the development of the anisotropy is more or less suppressed.

Figures 12a and b show the profiles of the radial and tangential temperatures
of each component
at $t=2.4t_{\rm rh,i}$ in model C3.
The radial temperature profiles are almost normal;
only slight temperature inversions appear in the heaviest two components.
The tangential temperature profiles of heavy components are rather abnormal;
there is a region where the tangential temperature of the heaviest component increases outward by a factor of about two.

\section{Conclusions and Discussion}

We have studied the development of velocity anisotropy in multi-mass star clusters by solving the FP equation in energy--angular momentum space.
Simulations were performed for simple two-component clusters
as well as clusters with a power-law mass function (ten components were employed).
The initial cluster models were multi-mass Plummer's models,
where the velocity distribution is isotropic
and the velocity dispersions for all components are equal.
The equipartition of the velocity dispersions is a probable initial condition for globular clusters,
and implies that the temperature is inversely proportional to the stellar mass.
Therefore, the temperatures of heavy components decrease rapidly at the early evolutionary stage,
and this leads to the development of the tangential anisotropy,
that is, the tangential velocity dispersion exceeds the radial velocity dispersion.
The tangential anisotropy appears more prominently in clusters with a steeper mass function,
because the degree of the initial temperature decrease is larger for such clusters.

In model C3, a cluster with a moderately steep mass-function ($\alpha=3.5$),
the maximum tangential anisotropy such as $\sigma_{\rm t}^2/\sigma_{\rm r}^2 \approx 2$ for the heaviest component appears around the half-mass radius.
Such strong tangential anisotropy is seen for a long time
of the order of $10t_{\rm rh,i}$.
This means that it may have survived until the present time,
if we adopt the typical half-mass relaxation time for the {\it present} Galactic globular clusters, $10^9$ yr, for $t_{\rm rh,i}$.
If the strong tangential anisotropy has survived,
can we obtain any observational evidence of it?
To the author's knowledge, no positive evidence has been reported,
although the direct measurement of the velocity anisotropy is very difficult.
Unfortunately,
the most massive stars are non-luminous degenerate remnants,
i.e. neutron stars or heavy white dwarfs, in the present-day clusters.
(Of course they were once more massive.)
Fortunately, on the other hand, the next heaviest stars are
bright red giants.
They may show significant tangential anisotropy in some globular clusters.
In any case we should at least note that anisotropy profiles may be more complex
than simple theoretical models, such as King-Michie models, predict.
As we mentioned in section 1,
multi-mass King-Michie models are most popular anisotropic models used in model-fitting of observational data.
They cannot reproduce anisotropy profiles such as those observed in models C2 and C3.
(However, this does not necessarily means that the density profiles cannot be well fitted to King-Michie models.)

We have not considered the effects of stellar evolution in this study.
Primordial high-mass stars have already lost all or almost all of their
initial masses.
The mass loss has significant effects on the early evolution of
globular clusters;
weakly bound clusters are destroyed (Chernoff, Weinberg 1990).
The way in which the anisotropy of each component develops depends on
the stellar mass and the mass function as we described above.
Therefore it may be also affected by stellar evolution.
To a first approximation, however, we may assume that stellar evolution
has the effect of changing only the initial condition,
because the main-sequence time scale of primordial massive stars are much
shorter than the time scale of relaxation (Lee et al.\ 1991).

In this study we have considered globular clusters to be isolated systems.
The effects of tidal truncation of clusters by the Galactic potential
was investigated for single-mass clusters
in a separate paper (Takahashi et al.\ 1997).
The paper showed that
the radial anisotropy in the halo is highly depressed during the
post-collapse evolution due to rapid loss of radial-orbit stars.
We will study more realistic models for the dynamical evolution
of globular clusters in the Galaxy
including both the tidal truncation and the mass function.

\par
\vspace{1pc}\par
The author thanks Professor Hyung Mok Lee for useful comments.
This work was supported in part by the Grant-in-Aid for Encouragement of Young
Scientists by the Ministry of Education, Science, Sports and Culture of Japan
(No. 1338).

\setcounter{equation}{0}
\renewcommand{\theequation}{A\arabic{equation}}

\section*{Appendix.\ The Diffusion Coefficients}

The expressions for the diffusion coefficients appearing in the single-mass FP equation were given by Cohn (1979).
The extension to multi-mass cases is easy.
In this appendix we give the expressions for the coefficients in
the multi-mass FP equation for completeness.
We use basically the same notations as those used by Cohn (1979).

The coefficients in equation (\ref{eq:flux}) are given by
\begin{eqnarray}
D_{E i} &=&  -8\pi^2 J_{\rm c}^2 \sum_j m_i m_j
\int_{r_{\rm p}}^{r_{\rm a}} \frac{dr}{v_{\rm r}} F_{1 j} \,, \nonumber \\
D_{R i} &=& -16\pi^2 R r_{\rm c}^2 \sum_j m_i m_j
\int_{r_{\rm p}}^{r_{\rm a}} \frac{dr}{v_{\rm r}}
\left( 1-\frac{v_{\rm c}^2}{v^2} \right) F_{1 j}\,, \nonumber \\
D_{EE i} &=& \frac{8\pi^2}{3} J_{\rm c}^2 \sum_j m_j^2
\int_{r_{\rm p}}^{r_{\rm a}} \frac{dr}{v_{\rm r}} v^2 (F_{0 j}+F_{2 j}) \,, \nonumber \\
D_{ER i} &=& D_{RE i} = \frac{16\pi^2}{3} J^2 \sum_j m_j^2
\int_{r_{\rm p}}^{r_{\rm a}} \frac{dr}{v_{\rm r}}
 \left( \frac{v^2}{v_{\rm c}^2}-1 \right) (F_{0 j}+F_{2 j}) \,, \nonumber \\
D_{RR i} &=& \frac{16\pi^2}{3} R \sum_j m_j^2
\int_{r_{\rm p}}^{r_{\rm a}} \frac{dr}{v_{\rm r}}
\Bigg\{ 2\frac{r^2}{v^2} \left[ v_{\rm t}^2
\left( \frac{v^2}{v_{\rm c}^2}-1 \right)^2 +v_{\rm r}^2 \right] F_{0 j}
\nonumber \\
&& +3\frac{r^2v_{\rm r}^2}{v^2} F_{1 j}
+\frac{r^2}{v^2} \left[ 2v_{\rm t}^2
\left( \frac{v^2}{v_{\rm c}^2}-1 \right)^2 -v_{\rm r}^2 \right] F_{2 j}
\Bigg\} \,,
\end{eqnarray}
where $v_{\rm c}(E)$ is the speed of a circular-orbit star of energy $E$,
$v^2=2[\phi(r)-E]$, $v_{\rm t}^2=J^2/r^2$, and $v_{\rm r}^2=v^2-v_{\rm t}^2$.
The functions $F_{0 j}$, $F_{1 j}$, and $F_{2 j}$ are defined by
\begin{eqnarray}
F_{0 j} (E,r) &=& 4\pi\gamma \int_0^E dE'\, \bar{f}_j(E',r) \,, \nonumber \\
F_{1 j} (E,r) &=& 4\pi\gamma \int_E^\phi dE'\, \bar{f}_j(E',r)
\left( \frac{\phi-E'}{\phi-E} \right)^{1/2} \,, \nonumber \\
F_{2 j} (E,r) &=& 4\pi\gamma \int_E^\phi dE'\, \bar{f}_j(E',r)
\left( \frac{\phi-E'}{\phi-E} \right)^{3/2} \,,
\end{eqnarray}
where $\gamma = 4\pi G^2 \ln \Lambda$.
The function $\bar{f}_j(E',r)$ is an assumed isotropic background distribution,
 and defined by
\begin{equation}
\bar{f}_j(E,r) = \frac{1}{2R_{\rm max}^{1/2}} \int_0^{R_{\rm max}}
\frac{dR}{(R_{\rm max}-R)^{1/2}} f_j(E,R)  \,,
\end{equation}
where $R_{\rm max}(E,r) = 2r^2[\phi(r)-E]/J_{\rm c}^2(E)$ is the maximum
allowed value of $R$ for all the orbits of energy $E$ which pass through
radius $r$.

\section*{References}

\re
Bettwieser E., Sugimoto D.\ 1984, MNRAS 208, 493
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Breeden J.L., Cohn H.N., Hut P.\ 1994, ApJ 421, 195
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Chernoff D.F., Weinberg M.D.\ 1990, ApJ 351, 121
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Cohn H.\ 1979, ApJ 234, 1036
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Cohn H.\ 1980, ApJ 242, 765
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Cohn H.\ 1985, in Dynamics of Star Clusters, IAU Symp No.113, ed
J.~Goodman, P.~Hut (D.~Reidel Publishing Company, Dordrecht) p161
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Cohn H., Hut P., Wise M.\ 1989, ApJ 342, 814
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Drukier G.A., Fahlman G.G., Richer H.B.\ 1992, ApJ 386, 106
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Giersz M., Heggie D.C.\ 1994, MNRAS 268, 257
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Gunn J.E., Griffin R.F.\ 1979, AJ 84, 752
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Spitzer L.\ Jr 1987, Dynamical Evolution of Globular Clusters (Princeton
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Takahashi K.\ 1995, PASJ 47, 561 (Paper I)
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\label{last}

\clearpage

\begin{table}[htb]
\begin{center}
Table~1.\hspace{4pt}Models of two-component clusters.\\
\vspace{6pt}
\begin{tabular}{cccc} \hline
Model       &  $m_2/m_1$ & $M_2/M_1$ & N    \\ \hline
T1          &  2       & 1           & 5000 \\
T2          &  2       & 1/9         & 5000 \\
T3          &  5       & 1/9         & 5000 \\ \hline
\end{tabular}
\end{center}
\end{table}

\bigskip

\begin{table}[htb]
\begin{center}
Table~2.\hspace{4pt}Models of power-law mass-function clusters.\\
\vspace{6pt}
\begin{tabular}{cccc} \hline
Model       & $m_{\rm max}/m_{\rm min}$ & $\alpha$ & N        \\ \hline
C1          & 10        & 1.5      & $10^5$    \\
C2          & 10        & 2.5      & $10^5$    \\
C3          & 10        & 3.5      & $10^5$    \\ \hline
\end{tabular}
\end{center}
\end{table}

\newpage

\begin{center}
\leavevmode
\epsfverbosetrue
\epsfxsize=14cm \epsfbox{fig1.ps}
\end{center}
\begin{Fv}{1}
{30pc}
{
Evolution of the Lagrangian radii containing
1, 2, 5, 10, 20, 30, 40, 50, 75, and 90\% of the total mass of each component for models (a) T1, (b) T2, and (c) T3.
The solid lines represent the heavy component,
and the dotted lines represent the light component.
}
\end{Fv}

\newpage

\begin{center}
\leavevmode
\epsfverbosetrue
\epsfxsize=14cm \epsfbox{fig2.ps}
\end{center}
\begin{Fv}{2}
{30pc}
{
(a1) Evolution of the temperature of the light component $T_1$
at the Lagrangian radii containing 1, 10, 20, 50, and 90\% of the total mass of the cluster, for model T1.
The ordinate is the temperature multiplied by the number of stars $N$.
(b1) Same as (a1), but the temperature of the heavy component $T_2$ is plotted.
(a2) and (b2) are the same as (a1) and (b1), but for model T2.
(a3) and (b3) are the same as (a1) and (b1), but for model T3.
}
\end{Fv}

\newpage

\begin{center}
\leavevmode
\epsfverbosetrue
\epsfxsize=14cm \epsfbox{fig3.ps}
\end{center}
\begin{Fv}{3}
{30pc}
{
(a1) Evolution of the anisotropy of the light component $\beta_1$
at the Lagrangian radii containing 1, 10, 20, 50, and 90\% of the total mass of the cluster, for model T1.
(b1) Same as (a1), but the anisotropy of the heavy component $\beta_2$ is plotted.
(a2) and (b2) are the same as (a1) and (b1), but for model T2.
(a3) and (b3) are the same as (a1) and (b1), but for model T3.
}
\end{Fv}

\newpage

\begin{center}
\leavevmode
\epsfverbosetrue
\epsfxsize=14cm \epsfbox{fig4.ps}
\end{center}
\begin{Fv}{4}
{30pc}
{
Radial profiles of the radial temperature ($T_{\rm r}$) and
the tangential temperature ($T_{\rm t}$)
of each component at $t=1.5t_{\rm rh,i}$ in model T3.
Component numbers are indicated in the figure.
The ordinate is the temperature multiplied by the number of stars $N$.
}
\end{Fv}

\begin{center}
\leavevmode
\epsfverbosetrue
\epsfxsize=14cm \epsfbox{fig5.ps}
\end{center}
\begin{Fv}{5}
{30pc}
{
Evolution of the radial profile of the anisotropy $\beta$ in model T1.
The profiles at four different epochs are shown.
The solid and dotted lines represent the heavy and light components, respectively.
The core radius $r_{\rm c}$ and the half-mass radius $r_{\rm h}$ are also
indicated.
}
\end{Fv}

\begin{center}
\leavevmode
\epsfverbosetrue
\epsfxsize=14cm \epsfbox{fig6.ps}
\end{center}
\begin{Fv}{6}
{30pc}
{
Same as figure 5, but for model T3.
}
\end{Fv}

\begin{center}
\leavevmode
\epsfverbosetrue
\epsfxsize=14cm \epsfbox{fig7.ps}
\end{center}
\begin{Fv}{7}
{30pc}
{
(a) Evolution of the temperature of the light component $T_1$
at the Lagrangian radii containing 1, 10, 20, 50, and 90\% of the total mass of the cluster, for the isotropic model corresponding to model T3.
The ordinate is the temperature multiplied by the number of stars $N$.
(b) Same as (a), but the temperature of the heavy component $T_2$ is plotted.
}
\end{Fv}

\begin{center}
\leavevmode
\epsfverbosetrue
\epsfxsize=14cm \epsfbox{fig8.ps}
\end{center}
\begin{Fv}{8}
{30pc}
{
Evolution of the central density of each component
in models (a) C1, (b) C2, and (c) C3.
Component numbers are indicated in the figure.
}
\end{Fv}

\begin{center}
\leavevmode
\epsfverbosetrue
\epsfxsize=14cm \epsfbox{fig9.ps}
\end{center}
\begin{Fv}{9}
{30pc}
{
Evolution of the anisotropy profile of each component in model C1.
Component numbers are indicated in the figure.
The profiles at four different epochs are shown.
The upper two panels are for the pre-collapse phase
and the lower two panels are for the post-collapse phase.
The core radius $r_{\rm c}$ and the half-mass radius $r_{\rm h}$ are also
indicated.
}
\end{Fv}

\begin{center}
\leavevmode
\epsfverbosetrue
\epsfxsize=14cm \epsfbox{fig10.ps}
\end{center}
\begin{Fv}{10}
{30pc}
{
Same as figure 9, but for model C2.
}
\end{Fv}

\begin{center}
\leavevmode
\epsfverbosetrue
\epsfxsize=14cm \epsfbox{fig11.ps}
\end{center}
\begin{Fv}{11}
{30pc}
{
Same as figure 9, but for model C3.
}
\end{Fv}

\begin{center}
\leavevmode
\epsfverbosetrue
\epsfxsize=14cm \epsfbox{fig12.ps}
\end{center}
\begin{Fv}{12}
{30pc}
{
Profiles of the (a) radial and (b) tangential temperatures of each component
at $t=2.4t_{\rm rh,i}$ in model C3.
Component numbers are indicated in the figure.
The ordinate is the temperature multiplied by the number of stars $N$.
}
\end{Fv}

\end{document}

redpajama_set_name: RedPajamaArXiv


text:
Research & Reviews: Journal of Statistics (RRJoST)
Home > Vol 8, No 1 (2019) > Doulah
An Alternative Robust Measure of Outlier Detection in Univariate Data Sets
Md. Siraj- Ud- Doulah, Md. Hafizul Islam
A univariate outlier is a data point that consists of an extreme value on one variable. Here we applied two types of outlier detection methods: one is graphical and another is analytical. This paper presents graphical methods for different statistical outlier detection such as scatter diagram, box plot and normal probability plot. Furthermore, the quantitative methods for outlier detection in this paper are the IQR method, SD method, Z-score method, the modified Z-score method, Tukey's method, adjusted box plot method, MADe method, Hampel method, Carling's modification method, MAD-Median rule, Grubb's test and our proposed HM- method. The performance of these outlier detection methods was observed based on different types of data sets. The analysis has shown that graphically we have suspected that the data sets contain outlier(s). But when we applied our analytical tests, only two methods including our proposed HM-method out of 12 methods were able to detect, in an appropriate and satisfactory way, as outlier. The main reasons for this can be found in the violation of normal distribution assumptions and in masking as well as swamping.
Keywords: Real data sets, outlier detection methods, proposed HM- method, statistical method
Md. Siraj-Ud-Doulah, Md. Hafizul Islam. An Alternative Robust Measure of Outlier Detection in Univariate Data Sets. Research & Reviews: Journal of Statistics. 2019; 8(1): 1–11p.
real data sets, outlier detection methods, proposed HM-〖SD〗_HM method, statistical method.
Iglewicz, B., Hoaglin, D. How to detect and handle outliers. ASQC Quality Press, 1993.
Department of Statistics, University of Udine
Bellio, R. and Ventura, L. An Introduction to Robust Estimation with R Functions, 2005.
Wilcox, R.R. and Keselman, H. J. Modern Robust Data Analysis Methods: Measures of Central Tendency. Journal of the Psychological Methods. 3, 2003, 254–274p.
Rousseeuw, P. J. and Zomeren, B. C. Unmasking Multivariate Outliers and Leverage Points. Journal of the American Statistical Association 85, 1990, 633-639p.
Nkechinyere, E.M., Andrew, I. And Idochi, O. Comparison of Different Methods of Outlier Detection in Univariate Time Series Data. International Journal for Research in Mathematics and Statistics. 2015, 208-2662p.
Acuna, E., Rodriguez, C. A. Meta analysis study of outlier detection methods in classification. Technical paper, Department of Mathematics, University of Puerto Rico at Mayaguez. 2004.
Barnett, V., Lewis, T. Outliers in statistical data. 3rd ed, Wiley, 1994.
Bendre, SM., Kale, B.K. Masking effect on test for outliers in normal sample. Biometrika, 74(4), 1987, 891-896p.
Ben-Gal, I. Outlier detection. Data Mining and Knowledge Discovery Handbook: A Complete Guide for Practitioners and Researchers, Kluwer Academic Publishers, 2005.
Carling, K. Resistant outlier rules and the non-Gaussian case. Computational statistics and data analysis, 33, 2000, 249-258p.
Davies, L., Gather, U. The identification of multiple outliers. Journal of the American Statistical Association, 88, 1993, 782-792p.
Rousseeuw, P. and Hubert, M. Anomaly Detection by Robust Statistics. Journal of the Wiley Interdisciplinary Reviews: Data Mining and Knowledge Discovery, 2017.
Hoaglin, D., Tukey, J.W. Performance of some resistant rules for outlier labeling. Journal of the American Statistical Association, 81, 1986, 991-1032p.
Barnett, V. and Lewis, T. Outliers in Statistical Data. New York, John Wiley and Sons 3rd Edition, 1994.
Rousseeuw P.J, Leroy A.M. Robust Regression and Outlier Detection. New York: Wiley Interscience, 1987.

redpajama_set_name: RedPajamaCommonCrawl


text:
Watch Da Vinci's Inquest TV Series Season 5 Episode 1 Online Free on Putlocker
Da Vinci's Inquest
Episode 1 - A Big Whiff of A Real Bad Smell
Vidtodo.com
Thevideo.me
Da Vinci's Inquest - Season 5 - Episode 1 - A Big Whiff of A Real Bad Smell
https://ww2.putlocker.onl/thumbs2/episode_fanarts/fanart_episode_1_season_5_e3a13d3fd33475eb37f65c3a85c784fc.jpg
Watch Series: Da Vinci's Inquest Released in (1998) - Season 5 - Episode 1 ,airing date 2002-10-27 produced by CA, Ca, The TV Series categorized in Crime, Drama, and content rating 44min with duration 60 min broadcasted as these networks CBC Television, CBC (CA), Streamed at Putlocker & directed by Chris Haddock, Stephen Surjik, David Frazee. Da Vinci investigates a deadly house fire, while Leary and Shannon try to solve a case involving a missing person.
Actor: Sarah-Jane Redmond, Suleka Mathew, Venus Terzo, Donnelly Rhodes, Gwynyth Walsh, Nicholas Campbell, Ian Tracey, Alex Diakun, Gerard Plunkett, Robert Wisden
Guest Stars: Colin Cunningham, Shaun Johnston
Creators: Chris Haddock, Stephen Surjik, David Frazee
Country: CA, Ca
Languages: en, es, English,
Rating: 7.167 out of 10 6
Content Rating: 44min
CBC Television, CBC (CA),
Da Vinci's Inquest, Da Vinci, Detetive Forense, Coroner Da Vinci, Da Vinci - dødens detektiv, Da Vinci juurdlus, La clave Da Vinci, Da Vincin murhatutkimukset, A halottkém, Na tropie zbrodni, canada, morgue, coroner, criminal investigation, vancouver, police, detective, vancouver british columbia canada, mysterious death, accidental death, forensic, medical, forensic evidence, murder, character name in title,
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Also known as: Da Vinci's Inquest, Da Vinci, Detetive Forense, Coroner Da Vinci, Da Vinci - DøDens Detektiv, Da Vinci Juurdlus, La Clave Da Vinci, Da Vincin Murhatutkimukset, A HalottkéM, Na Tropie Zbrodni
Vancouver British Columbia Canada
Mysterious Death
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Character Name In Title
Da Vinci's Inquest - Season 5 - Episode 1 - A Big Whiff of A Real Bad Smell Watch Online
Trailer: A Big Whiff of A Real Bad Smell
Da Vinci's Inquest https://ww2.putlocker.onl/thumbs2/show_fanarts/fanart_show_e3a13d3fd33475eb37f65c3a85c784fc.jpg Da Vinci's Inquest is a Canadian dramatic television series that aired on CBC Television from 1998 to 2005. While never a ratings blockbuster, seven seasons of thirteen episodes each were filmed for a total of ninety-one episodes. The show, set and filmed in Vancouver, stars Nicholas Campbell as Dominic Da Vinci, once an undercover officer for the Royal Canadian Mounted Police, but now a crusading coroner who seeks justice in the cases he investigates. The cast also includes Gwynyth Walsh as Da Vinci's ex-wife and chief pathologist Patricia Da Vinci, Donnelly Rhodes as detective Leo Shannon, and Ian Tracey as detective Mick Leary. da-vincis-inquest 5 Season 5 5
Ep 13 : Everybody Needs A Worki...
Ep 12 : You Got Monkey Chatter
Ep 11 : The Ducks Are Too Depre...
Ep 10 : Dogs Don't Bite People
Ep 9 : For Just Bein' Indian
Ep 8 : Doing The Chicken Scratch


text:
House Intel Investigation on Benghazi Clears Administration, Intelligence Community of Wrongdoing
By Ian Tuttle
About Ian Tuttle
Follow Ian Tuttle on Twitter
Via the Denver Post:
A two-year investigation by the Republican-controlled House Intelligence Committee has found that the CIA and the military acted properly in responding to the 2012 attack on a U.S. diplomatic compound in Benghazi, Libya, and asserted no wrongdoing by Obama administration appointees. . . .
The investigation of the politically charged incident determined that there was no intelligence failure, no delay in sending a CIA rescue team, no missed opportunity for a military rescue, and no evidence the CIA was covertly shipping arms from Libya to Syria.
In response to accusations that the administration misled the American public in the days following the Benghazi attack by blaming events on a spontaneous protest against a YouTube video:
In the immediate aftermath of the attack, intelligence about who carried it out and why was contradictory, the report found. That led Susan Rice, then U.S. ambassador to the United Nations, to inaccurately assert that the attack had evolved from a protest, when in fact there had been no protest. But it was intelligence analysts, not political appointees, who made the wrong call, the committee found. The report did not conclude that Rice or any other government official acted in bad faith or intentionally misled the American people.
The full report is available here.
The Select Committee on Benghazi, headed by South Carolina representative Trey Gowdy, remains in the midst of an ongoing investigation.
Ian Tuttle is the former Thomas L. Rhodes Journalism Fellow at the National Review Institute. @iptuttle


Jonathan K. Levine is an attorney providing legal services covering Business Litigation and Antitrust Litigation and Securities Litigation.
Jonathan Levine, who practices law in Oakland, California, was selected to Super Lawyers for 2013 - 2019. This peer designation is awarded only to a select number of accomplished attorneys in each state. The Super Lawyers selection process takes into account peer recognition, professional achievement in legal practice, and other cogent factors.
Prior to becoming an attorney, he studied at Fordham University School of Law. He graduated in 1988. After passing the bar exam, he was admitted to legal practice in 1988.


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This is the lighting controller [Paul Stoffregen] built for Burning Man. They wanted to go with DMX controlled lighting this year but that most often includes a computer to run the lighting sequences. This board runs the preprogrammed DMX sequence using a hacked lighting design file.
The choreography for the lighting was planned out using a program called Vixen 2. There is one newer version of the software, but [Paul] needed to translate the output file for use with a microcontroller and version 2 makes this a bit easier than version 3. Speaking of conversion, he didn't want to start from square one and a bit of searching led to a tutorial which [Bill Porter] posted last year on converting Vixen files for use with Arduino. It wasn't exactly what he had in mind, but most of the ground work was there.
A few code tweaks bent the script to [Paul's] will. He changed the XML parsing function to ignore all but the main channels in the file. He also had it output a text file which can be stored on the SD card. Because the output is not being flashed to a chip this greatly increases the storage available paving the way for much longer and more complex shows.
Want to learn more about the protocol used by DMX equipment? Check out this primer.
is there a schematic available ???, i whanted to do something like this, i whant to have a dmx "master" who can send different light effects / animations over a dozen of dmx rgb lights.
got a lot of love for this. may solve many of my issues!!
oh hackaday… where is your favourite button…?
I'm a big fan of Vixen and it's creator, K.C. Oaks. Last year he wrote a raw data export add-in for me that I use with Propeller boards in embedded DMX projects. The export file has a header with channel count, frame timing, and total number of frames. The raw data for the channels follows that. Easy-peasy and very popular with friends and customers that use my code.
I just remembered that I have the raw data export add-in posted on the EFX-TEK site.
The exported file starts with a 6-byte header that is three, 16-bit values: channel count, frame timing (ms), and number of frames in project. The raw frame data follows. It's super easy to use and works like a champ. Having the header makes the application code doesn't have to change project-to-project.
This is still my favorite DMX instruction site(despite the 1995 website chic). Learn how it works, and then implement it however you're comfortable.
didnt know there was a Vix2 or even a Vix3 … will update next time i use it!


Workers' Rights leaflets are available in 20 languages, listed below.
We also have Help Them leaflets which were introduced at our conference.
HELP Them leaflets can be downloaded here.
If you would like printed copies of any of these, please email communications@gla.gov.uk or telephone 0345 602 5020.


text:
IN PRAISE OF FREAKS AND WEIRDOS
By BTL Staff| 2018-01-15T18:04:03-04:00	June 7th, 2012|Opinions|
By Abby Dees
For the last month or so I've been riding my bike up the entire length of the Mississippi river. This has not been a trip about about amazing scenery — though there have been moments of breathtaking beauty — nor does my journey have any official theme or purpose. I'd been wanting to see the "real" America for a while now, and riding slowly up the middle bits seemed like a good way to do it.
Not that I haven't lived in the U.S. my entire life, but you know what I mean. The real America is "normal" America, the one politicians pander to, Fox News tries to frighten, and the one that comes to mind when I (perhaps you) think of the idea, rather than the place, America.
I'm getting a lesson in my own culture. Mostly, I've been deeply moved by our goodness and unhesitating willingness to come to the aid of a sweaty, middle-aged woman in tight, garish Lycra, clackety cycling shoes, and covered in bruises and chain grease. It's a deep part of our national character that I'd like to see our leaders appeal to so much more.
That said, I've also been bored silly much of the time by the unrelenting sameness despite having traveled nearly 2, 000 miles so far. In the middle of Middle America, the aesthetic rarely changes. From the capri-panted women, to men surgically attached to their baseball caps and trucks, to the country-quaint decorations, to the criminally random apostrophes and tortured puns of every craft store name ("I'll Bee Sewin' You"), to the ubiquitous (and quite tasty at the end of a long, hot cycling day) Dairy Queens — well, at times I've felt stuck in a space/time loop.
I think this is what "normal" looks like here. And I've wondered more and more if I was also seeing the American Way of Life that I've heard so much about, whether it's being threatened by terrorists or gays, or just the crappy economy. If so, it's the cultural equivalent of a grilled cheese sandwich with the crust cut off. Sometimes it's just what you're in the mood for, but you'll soon be desperate for a microgreens salad with goat cheese and rosemary. I am, in any case.
Amid this sameness, occasionally something unusual springs up, usually in a fabulously out-of-scale way (this problem with appropriate scale also seems to be part of our American-ness). My fellow riders and I screech to a halt to snap pictures of each of us posing in front of whatever proud expression of individuality has appeared upon the landscape, such as the fellow with the antique outhouse collection in his yard, or the enormous church made entirely of scrap, or most recently, the improbably serious and well funded Farm Toy Museum in Dyersville, Iowa. Each time something loudly breaks up the monotony I quietly sing the Sesame Street jingle, "One of these things is not like the others…" and smile.
Thank God for whatever guts it takes to express oneself so joyfully, without any apparent concern about the irony or absurdity of it. Honestly. As long as folks feel free to express themselves this way, then all the normalcy becomes like a pleasant canvas to paint on. But without the weirdness, tedium sets in fast, and despite how nice everyone is, I start to feel like a freak. The bad kind of freak.
When those proud weirdos do appear, I feel like I belong too. I don't just mean the ones with the oversized yard sculptures either. I mean the boy who puts pink food coloring in his hair and lip-syncs Lady Gaga tunes in the mirror, or the cashier at the Family Dollar store with the nose ring and butch swagger (thanks for the knowing nod last week). They make me feel like the right kind of freak.
To anyone who can't seem to relate to what's "normal," or who dreams about going somewhere else one day — sure, do it, but remember that you are a beautiful part of the landscape today. You are saving us from ourselves, even if the neighbors don't get it at all.


text:
Home Government Presidential Kill List? First Woman Muslim Judge Found Floating in the Hudson
Presidential Kill List? First Woman Muslim Judge Found Floating in the Hudson
VT Editors
The suicide cover up begins with Trump's "Daily Beast" cheering squad, the Mossad/Jane Harman controlled smear blog, joned in by Murdoch's NY Daily News and aided by the mob controlled police. Yes, it was murder, now for certain.
Who ordered the hit? Was it witch queen Ivanka from her new White House office? Did the call go to Kosher-Nostra Central in Trump Tower to Felix Sater, Russian mob kingpin and "Trump advisor?" "I want that bitch floating face down in the Hudson!"
True or not, and we believe Trump is behind it, this is far more likely than Syria's involvement in a false flag gas attack. Increasingly as the shoddy intel cover stories come out, it looks like Ivanka and Donnie may have ordered that as well. We know the Russian's really believe it and they have real intercepts to back it up.
We know this for sure, Trump wanted her dead, has joked about it, and has spoken of her as someone he wanted out of the way as quickly as possible. Does this make him a murder suspect? In the real world, damn right it does.
Sheila Abdus-Salaam, America's first-ever Muslim woman judge and the first African-American female to serve on New York's highest court, has been found dead in New York, police say.
Trump fails to comment publicly, privately said to have "high fived" those around him when he got the news. Was her death ordered over dessert like the Syria bombing?
The 65-year-old judge's body was found floating on the on the Manhattan side of the Hudson River on Wednesday, just a mile from her home in central Harlem.
Police called the late judge's husband to identify her. She was reported missing since Tuesday. Officials said the body showed no signs of apparent trauma or injuries.
As a Muslim, Abdus-Salaam made history in 2013, when New York Governor Andrew Cuomo nominated her to serve on the state Court of Appeals.
"The New York Court of Appeals was saddened to learn today of the passing of Judge Sheila Abdus-Salaam, a most beloved colleague since she joined the Court in May 2013," Chief Judge Janet DiFiore said.
Before getting unanimous approval for the job, Abdus-Salaam said, "being a judge is an honor and involves tremendous responsibility to the litigants and to society."
Cuomo issued a statement on Wednesday, extending his condolences to Abdus-Salaam's family.
New York law enforcement officers cover the dead body of Sheila Abdus-Salaam, America's first-ever Muslim woman judge near the Hudson River, April 12, 2017. (Photo by New York Daily News)
"As the first African-American woman to be appointed to the State's Court of Appeals, she was a pioneer," he said. "Through her writings, her wisdom, and her unshakable moral compass, she was a force for good whose legacy will be felt for years to come."
New York Mayor Bill de Blasio also grieved the judge's "tragic passing," calling her a "a humble pioneer."
Also mourning Abdus-Salaam's mysterious death was state Assembly Speaker Carl Heastie, who described her as "an inspiration."
Police said they were investigating the matter while the medical examiner tired to determine the judge's cause of death.Officials have not ruled out the possibility of a hate crime. The incident comes months after a Muslim imam and his assistant were shot dead near a mosque in the New York City borough of Queens.
According to Brian Levin, a leading hate crimes researcher, hate crimes increased by more than 20 percent last year in nine US metropolitan areas, including New York City.
Levin argues that the divisive rhetoric of US President Donald Trump was largely to blame for the trend.
VT Editors is a General Posting account managed by Jim W. Dean and Gordon Duff. All content herein is owned and copyrighted by Jim W. Dean and Gordon Duff
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Which Word Means Not Straight In Form Or Shape?
Can You Describe A Situation Where You Personally Have Come Into Contact With Marketing In Some Shape Or Form?
Well it's all bout the product which you are selling to the customer, can someone give me the right answer...
What Does Shape Mean In Art?
I think it means different objects... Witch would be different shapes such as square, rectangle, triangle......
Explain 'Meaning Is In People Not In Words'?
Meaning is subjective; i.e it is not fixed, but depends on the person who is giving meaning to something....
Based On Your Knowledge Of Latin Roots, Which Of The Following Words Most Likely Means "Does Not Change"?
It is a bit difficult to answer without the words to choose from. Constant, fixed, immutable, immovable...
Which Word Or Words Are Unnecessary In The Following Sentence: The Writer Rudyard Kipling Was Born In Mumbai, India?
"The Writer" These words aren't necessary due to Rudyard's unusual name making it unlikely...
The term 'Environment' has been derived from the French word which means to encircle or surround?
Environ is the word....
How many people are 'straight edge',which means you do not smoke,drink or do drugs,that's straight edge?
I smoke but still straight edge society...
Which word means given to inconsistencies?
The obvious word which means 'given to inconsistencies,' would be 'inconsistent'.According to my dictionary,...
What is 40.302 in word form?
Forty and three hundred two one-thousandths....
How to write 3.100 in word form?
Three and one tenth....
What Is The Meaning Of Livelihood?
What Does Obtuse Mean?
What Does Cubism Mean?
I keep seeing a black shadow ghost, what does this mean?
What Is The Difference Between Weathering And Erosion?
Where Do I Find Printable Lyrics To Lisa Knowles "I Need You Lord,jesus"?
What Is Importance Of Freedom Of Speech?
What Does PDC Mean?
What Does Palo Pinto Mean?
If A Boy Has A Condom On, Can You Still Get Pregnant?
What Is The Best Pit Bull To Have?
Can you eat the fruit from monkey puzzle trees?
My Hydrangea Has White Sticky Blobs On It, What Are They? THEY LOOK A BIT LIKE MAGGOTS AND HAVE A BLACK SPOT AT THE TOP
How do you get gum out of sweat pants?
How do I tell if a girl has a crush on me?


text:
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Messenger No. 132 (June 2008)
« Back to The Messenger home
2-4 (PDF)
T. de Zeeuw
The Perfect Machine
ADS BibCode:
2008Msngr.132....2D
Author(s)/Affiliation(s):
de Zeeuw, T.
AA(ESO)
10th Anniversary of First Light of the VLT
2008Msngr.132....4.
Austria Declares Intent to Join ESO
Telescopes and Instrumentation
7-10 (PDF)
M. Kissler-Patig, A. Fontana et al.
Hawk-I – First Results from Science Verification
2008Msngr.132....7K
Kissler-Patig, M.; Fontana, A.; Venemans, B.; Kneib, J.; Doherty, M.; Lidman, C.; Kuntschner, H.; Norris, M.; Larsen, S.; Gieles, M.; Mora Fernandes, A.; McCaughrean, M.; Preibisch, T.; Seifahrt, A.; Willis, J.; Wehner, E.
AA(ESO) AB(INAF – Osservatorio Astronomico di Roma, Italy) AC(Institute of Astronomy, University of Cambridge, United Kingdom) AD(OAMP, Laboratoire d'Astrophysique de Marseille, France) AE(ESO) AF(ESO) AG(ST-ECF, ESO) AH(Department of Physics, University of Durham, United Kingdom) AI(Astronomical Institute, University of Utrecht, the Netherlands) AJ(ESO) AK(Departamento de Física Teórica C-XI, Universidad Autónoma de Madrid, Spain) AL(School of Physics, University of Exeter, United Kingdom) AM(Max-Planck-Institut für Radioastronomie, Bonn, Germany) AN(Institut für Astrophysik, Georg-August-Universität, Göttingen, Germany) AO(Department of Physics and Astronomy, University of Victoria, Canada) AP(Department of Physics and Astronomy, McMaster University, Hamilton, Canada)
The VLT wide-field near-infrared imager HAWK-I was commissioned in 2007 and Science Verification (SV) programmes were conducted in August 2007. A selection of results from among the twelve Science Verfication proposals are summarised.
Casali, M., Piraud, J.-F., Kissler-Patig, M., et al. 2005, The Messenger, 119, 6; Kissler-Patig, M., et al. 2008, A&A, accepted Maraston, C., et al. 2003, A&A, 400, 823; Puzia, T. H., et al. 2002, A&A, 391, 453
11-17 (PDF)
M. Sarazin, J. Melnick et al.
Seeing is Believing: New Facts about the Evolution of Seeing on Paranal
2008Msngr.132...11S
Sarazin, M.; Melnick, J.; Navarrete, J.; Lombardi, G.
AA(ESO) AB(ESO) AC(ESO) AD(ESO; National Institute for Astrophysics, Bologna Astronomical Observatory, Italy; Department of Astronomy, University of Bologna, Italy)
Since the commissioning of the VLT it has been known that the image quality delivered by the telescopes is better, and often much better, than predicted by the seeing monitor. The advent of new sensitive instruments to measure the optical turbulence profile of the atmosphere over Paranal has finally allowed us to understand the origin of this discrepancy: the presence of a highly turbulent layer so close to the ground that it is seen by the seeing monitor, but not by the VLT unit telescopes. In this article we tell the story of this elusive surface layer.
Butterley, T., Wilson, R. W., Sarazin, M. 2006, MNRAS, 369, 835; Kornilov, V., et al. 2003, Proc. SPIE, 4839, 837; Lombardi, G., Navarrete, J., Sarazin, M. 2008, E-ELT-TRE-222-0215, ESO Garching Martin, F., et al. 2000, A&AS, 114, 39; Tokovinin, A. 2007, Rev. Mex. Astron. Astrophys. (Conf. Series), 31, 61
C. Snodgrass, I. Saviane et al.
EFOSC2 Episode IV: A New Hope
Snodgrass, C.; Saviane, I.; Monaco, L.; Sinclaire, P.
AA(ESO) AB(ESO) AC(ESO) AD(ESO)
As part of the long-term plan for the La Silla Observatory, ESO is reducing the number of instruments offered. EMMI and SUSI have been decommissioned at the NTT, and EFOSC2 has been moved to the NTT, replacing EMMI, to leave HARPS as the sole instrument at the 3.6-m. Here we describe EFOSC2 and its many capabilities, highlight the changes that the move to the NTT brings, and look forward to future plans for this instrument.
Böhringer, H., et al. 2001, A&A, 369, 826; Buzzoni, B., et al. 1984, The Messenger, 38, 9; Eckert, W., Hofstadt, D., Melnick, J. 1989, The Messenger, 57, 66; Levan, A., et al. 2005, ApJ, 624, 880; Saviane, I., et al 2007, The Messenger, 129, 14; Schwarz, H. E., Corradi, R. L. M., Melnick, J. 1992, A&AS, 96, 23
I. Saviane, L. Monaco
Two Volume-phased Holographic Grisms Now Available for EFOSC2
Saviane, I.; Monaco, L.
AA(ESO) AB(ESO)
Starting from Period 81, two new volume-phased holographic grisms are available to be used with EFOSC2. Testing of the grisms is described. Some results on measurement of the stellar Lithium doublet and galaxy rotation curves demonstrate the performance of the new grisms.
Cameron, A. G. W., Fowler, W. A. 1971, ApJ, 164, 111; Charbonnel, C., Balachandran, S. C. 2000, A&A, 359, 563; Dhillon, V., et al. 2007, The Messenger, 127, 41; Uttenthaler, S., Lebzelter, T., Palmerini, S., et al. 2007, A&A, 471, L41
M. Kraus, S. Stanghellini et al.
The ALMA Antenna Transporter
2008Msngr.132...23K
Kraus, M.; Stanghellini, S.; Martinez, P.; Koch, F.; Dimmler, M.; Moresmau, J.M.; Rykaczewski, H.
AA(ESO) AB(ESO) AC(ESO) AD(ESO) AE(ESO) AF(ESO) AG(ESO)
The ALMA observatory will consist of an array of 54 12-m diameter and 12 7-m diameter antennas. In order to configure the different array modes, it is necessary to move the antennas to different configurations. In the compact array configuration, the antennas are packed as closely as possible within a circle of 200 m diameter; in the extended configuration the antennas are spread over an area of about 15 km in diameter. The frequent relocations of antennas will be accomplished by two special vehicles, the ALMA Antenna Transporters. The challenges encountered during their development and their main characteristics are described.
Haupt, C., Rykacewski, H. 2007, The Messenger, 128, 25
R. Laing
Recent Progress at the ALMA Test Facility
2008Msngr.132...28L
Laing, R.
Recent developments at the ALMA Test Facility are presented. Many aspects of the hardware and software needed for operation in Chile have now been tested and the Facility continues to demonstrate its value as a test-bed. The first high-resolution interferometric spectra of astronomical sources have now been obtained.
Hunter, T., Laing, R. A. 2008, The Messenger, 131, 47
H.V. Ramió, M. Reyes et al.
Cute-SCIDAR at Paranal for E-ELT Site Characterisation
2008Msngr.132...29R
Ramió, H.V.; Reyes, M.; Delgado, J.M.; Hernández, E.; Cagigal, M.N.; Fuensalida, J.J.; Lombardi, G.; Derie, F.; Navarrete, J.; Sarazin, M.
AA(Instituto de Astrofísica de Canarias, Spain) AB(Instituto de Astrofísica de Canarias, Spain) AC(Instituto de Astrofísica de Canarias, Spain) AD(Instituto de Astrofísica de Canarias, Spain) AE(Instituto de Astrofísica de Canarias, Spain) AF(Instituto de Astrofísica de Canarias, Spain) AG(ESO; National Institute for Astrophysics, Bologna Astronomical Observatory, Italy; University of Bologna, Department of Astronomy, Italy) AH(ESO) AI(ESO) AJ(ESO)
A new version of the cute-SCIDAR instrument, which employs the generalised SCIntillation Detection And Ranging technique to obtain detailed atmospheric turbulence profiles with height, has been designed, developed and tested by the Instituto de Astrofísica de Canarias. The instrument was developed to match the requirements of the ESO VLT Auxiliary Telescopes, within the framework of the European Extremely Large Telescope site characterisation project. Commissioning at Paranal was successfully carried out in November 2007. This upgraded version of the original instrument, presently working at the Roque de los Muchachos Observatory, allows g-SCIDAR turbulence profiles to be obtained in real time, a novel achievement in site testing and also a crucial tool for the optimum design and operation of Adaptative Optics and Multi-Conjugate Adaptive Optics systems.
Fuchs, A., Tallon, M., Vernin, J. 1998, PASP, 110, 86; Fuensalida, J. J., Delgado, J. M., García-Lorenzo, B., et al. 2004a, in Second Backaskog Workshop on Extremely Large Telescopes, eds. A. L. Ardeberg and T. Andersen, proc. SPIE, 5382, 643; Fuensalida, J. J., Chueca, S., Delgado, J. M., et al. 2004b, in Advancements in Adaptive Optics, eds. D. Bonaccini Calia, B. L. Ellerbroek and R. Ragazzoni, proc. SPIE, 5490, 749; Fuensalida, J. J., García-Lorenzo, B., Delgado, J. M, et al. 2007, Rev. Mex. Astron. Astrof., 31, 86; Vernin, J. & Roddier, F. 1973, J. Opt. Soc. Am., 64, 270; Vernin, J. & Azouit, M. 1983, J. Opt. (Paris), 14, 131; Vernin, J. & Muñoz-Tuñón, C. 1992, A&A, 257, 811
Astronomical Science
D. Reimers, H.-J. Hagen et al.
The Antares Emission Nebula and Mass Loss of alpha Sco A
Reimers, D.; Hagen, H.-J.; Baade, R.; Braun, K.
AA(Hamburger Sternwarte, Universitaet Hamburg, Germany) AB(Hamburger Sternwarte, Universitaet Hamburg, Germany) AC(Hamburger Sternwarte, Universitaet Hamburg, Germany) AD(Hamburger Sternwarte, Universitaet Hamburg, Germany)
The Antares nebula has been known as a peculiar [FeII] emission nebula, apparently without normal HII region lines. Long-slit VLT/UVES mapping shows that it is an HII region 3'' in size around the B type star alpha Sco B, with a Balmer line recombination spectrum and [NII] lines, but no [OII] and [OIII]. The reason for the non-visibility of [OII] is the low electron temperature of 4900 K, while [NII] is seen because the nitrogen abundance is enhanced by a factor of three due to the CNO cycle. We derive a mass-loss rate of 1.05 ± 0.3 × 10–6 MSun/yr for the M supergiant alpha Sco A. The [FeII] lines seem to come mainly from the edges of the HII region.
Baade, R. & Reimers, D. 2007, A&A, 474, 229; Bautista, M. A., Pradhan, A. K., Osterbrock, D. E. 1994, ApJ, 432, L135; Ferland, G. J., Korista, K. T., Verner, D. A., et al. 1998, PASP, 110, 761; Hagen, H.-J., Hempe, K., Reimers, D. 1987, A&A, 184,256; Harris, M. J. & Lambert, D. L. 1984, ApJ, 281, 739; Hjellming, R. M. & Newell, R. T. 1983, ApJ, 275, 704; Kudritzki, R. & Reimers, D. 1978, A&A, 70, 227; Reimers, D., Hagen, H.-J., Baade, R., et al. 2008, A&A, submitted Struve, O. & Zebergs, V. 1962, Astronomy of the 20th Century, MacMillan Comp. New York, 303; Swings, J. P. & Preston, G. W. 1978, ApJ, 220, 883
M. Matsuura, A. Speck et al.
SINFONI Observations of Comet-shaped Knots in the Planetary Nebula NGC 7293 (the Helix Nebula)
2008Msngr.132...37M
Matsuura, M.; Speck, A.; Smith, M.; Zijlstra, A.; Lowe, K.; Viti, S.; Redman, M.; Wareing, C.; Lagadec, E.
AA(National Astronomical Observatory of Japan, Tokyo, Japan; Department of Physics and Astronomy, University College London, United Kingdom) AB(Physics and Astronomy, University of Missouri, Columbia, USA) AC(Centre for Astrophysics and Planetary Science, School of Physical Sciences, The University of Kent, Canterbury, United Kingdom) AD(School of Physics and Astronomy, University of Manchester, United Kingdom) AE(Science and Technology Research Centre, University of Hertfordshire, Hatfield, United Kingdom) AF(Department of Physics and Astronomy, University College London, United Kingdom) AG(Department of Physics, National University of Ireland Galway, Republic of Ireland) AH(School of Mathematics, University of Leeds, United Kingdom) AI(School of Physics and Astronomy, University of Manchester, United Kingdom)
One of the most interesting characteristics of the planetary nebula NGC 7293 (the Helix Nebula) is its comet-shaped knots. We have observed one of the knots using the SINFONI imaging spectrometer on the VLT with adaptive optics. The spectra are analysed to obtain the spatial variation of molecular hydrogen line intensities within the knot. The images clearly show the detailed structure, which resembles a tadpole in shape, suggesting that hydrodynamic flows around the knot core create a pressure gradient behind the core. The three-dimensional spectra reveal that the excitation temperature is uniform at approximately 1800 K within the knot. The SINFONI observations help to determine the H2 excitation mechanism in planetary nebulae, as well as the importance of hydrodynamics in shaping the knots.
Burton, M .G., Hollenbach, D. J., Tielens, A. G. G. M. 1992, ApJ, 399, 563; Dyson, J. E., Pittard, J. M., Meaburn, J., et al. 2006, A&A, 457, 561; Harris, H. C., Dahn, C. C., Canzian, B., et al. 2007, AJ, 133, 631; Matsuura, M., Speck, A. K., Smith, M. D., et al. 2007, MNRAS, 382, 1447; Meixner, M., McCullough, P., Hartman, J., et al. 2005; AJ, 130, 1784 O'Dell, C .R., Handron, K. D. 1996, AJ, 111, 1630; Speck, A. K., Meixner, M., Fong, D., et al. 2002, AJ, 123, 346; Tsamis, Y. G., Walsh, J. R., Pequignot D., et al., 2008, MNRAS, 355, in press Vorontsov-Velyaminov, B. A. 1968, IAU Symp. No. 34, 256; Walsh, J. R, Meaburn, J. 1987, MNRAS, 224, 885
M.G. Haehnelt, M. Rauch et al.
Hunting for the Building Blocks of Galaxies like our own Milky Way with FORS
2008Msngr.132...41H
Haehnelt, M.G.; Rauch, M.; Bunker, A.; Becker, G.; Marleau, F.; Graham, J.; Cristiani, S.; Jarvis, M.J.; Lacey, C.; Morris, S.; Peroux, C.; Röttgering, H.; Theuns, T.
AA(Institute of Astronomy, Cambridge, United Kingdom) AB(Observatories of the Carnegie Institution of Washington, Pasadena, USA) AC(Anglo-Australian Observatory, Epping, Australia) AD(Observatories of the Carnegie Institution of Washington, Pasadena, USA) AE(Spitzer Science Center, Caltech, Pasadena, USA) AF(University of California, Berkeley, USA) AG(Osservatorio Astronomico di Trieste, INAF, Italy) AH(Centre for Astrophysics, Science & Technology Research Institute, University of Hertfordshire, Hatfield, United Kingdom) AI(Institute for Computational Cosmology, Department of Physics, University of Durham, United Kingdom) AJ(Department of Physics, University of Durham, United Kingdom) AK(Observatoire Astronomique de Marseille-Provence, France) AL(Leiden Observatory, the Netherlands) AM(Department of Physics, University of Durham, United Kingdom)
We report results from our ultra-deep spectroscopic survey for low surface brightness Ly alpha emitters at redshift z ~ 3. A 92-hour-long exposure with the ESO VLT FORS2 instrument has yielded a sample of 27 faint line emitters with fluxes of a few times 10–18 erg s–1 cm–2 which we argue are likely to be dominated by Ly alpha. The large comoving number density, the large covering factor, dN/dz ~ 0.2–1, and the spatially extended surface brightness of the emission suggest that the emitters can be identified with the elusive host population of damped Ly alpha systems (DLAS) and high column density Lyman limit systems. The finding suggests that most Lyman limit systems and DLAS are part of the same low-mass galaxies.
Bouwens, R. J., Illingworth, G. D., Franx, M., et al. 2007, ApJ, 670, 929; Christensen, L., Wisotzki, L., Roth, et al. 2006, A&A, 468, 587; Cowie, L. L., Hu, E. M. 1998, AJ, 115, 1319; Gould, A., Weinberg, D. H. 1996, ApJ, 468, 462; Haehnelt, M. G., Steinmetz, M., Rauch, M. 2000, ApJ, 534, 594; Hogan, C. J., Weymann, R. J. 1987, MNRAS, 225, 1; Møller, P., Warren, S. J., Fall, S. M., et al. 2002, ApJ, 574, 51; Ouchi, M., Shimasaku, K., Akiyama, M., et al. 2008, ApJS, 176, 301; Partridge, R. B., Peebles, P. J. E. 1967, ApJ, 147, 868; Rauch, M., Haehnelt, M. G., Bunker, A., et al. 2008, ApJ, 681, 856; Steidel, C.C., Hamilton, D. 1995; ApJ, 105, 2017 van Breukelen, C., Jarvis, M. J., Venemans, B. P. 2005, ApJ, 359, 895; Warren, S. J., Møller, P., Fall, S. M., et al. 2001, MNRAS, 326, 759; Wolfe, A.M., Turnshek, D. A., Smith, H. E. 1986, ApJS, 61, 249
Astronomical News
N. Delmotte
News from the ESO Science Archive Facility
2008Msngr.132...47D
Delmotte, N.
Latest developments of the ESO archive including timely access to proprietary data, a new science-oriented query form and new data releases are presented.
Hildebrandt, H., et al. 2006, A&A, 452, 1121; Marchetti, E., et al. 2007, The Messenger, 129, 8; Popesso, P., et al. 2008, A&A, submitted Tacconi-Garman, L. E. 2007, The Messenger, 130, 54
R. Gilmozzi, G. Monnet et al.
FP7 E-ELT Preparation – Grant Agreement Funded by the European Commission is Underway
2008Msngr.132...48G
Gilmozzi, R.; Monnet, G.; Robinson, M.
AA(ESO) AB(ESO) AC(ESO)
M. Sterzik, J. Melnick et al.
Report on the International Workshop on Star Formation Across the Milky Way Galaxy
Sterzik, M.; Melnick, J.; Melo, C.
Announcement of the ESO Workshop on Large Programmes
2008Msngr.132...50.
Announcement of the Topical Symposium "Science with the E-ELT" at JENAM 2008
2008Msngr.132Q..51.
Fellows at ESO
2008Msngr.132R..51.
ESO Fellowship Programme 2008/2009
New Staff at ESO
H. Boffin, A. Acker
Exploring the Cold Universe – A Planetarium Show for the IYA 2009
2008Msngr.132...54B
Boffin, H.; Acker, A.
AA(ESO) AB(Observatoire de Strasbourg, France; Association des Planétariums de Langue Française (APLF))
A planetarium show highlighting the ALMA project is being jointly prepared by ESO and the Association des Planétariums de Langue Française.
Personnel Movements
2008Msngr.132S..55.
Last Update: 19.04.22 © ESO
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text:
Q: Trying to populate a GtkComboBox with model in C I'm really new to C and GTK+ so my problem might be painfully obvious. I have tried to follow examples and tutorials found all over the net.
I want a combo box with three values, the middle one being the default. I can successfully set it up using Glade but I have decided to rewrite everything in C. The combobox is drawn but it is empty/blank. I don't know what I am doing wrong.
...
GtkTreeIter iter;
GtkListStore *liststore;
GtkWidget *combo;

liststore = gtk_list_store_new(1, G_TYPE_STRING);
gtk_list_store_insert_with_values (liststore, &iter, 0, 0, "Don't install.", -1);
gtk_list_store_insert_with_values (liststore, &iter, 1, 0, "This user only.", -1);
gtk_list_store_insert_with_values (liststore, &iter, 2, 0, "All users.", -1);

combo = gtk_combo_box_new_with_model(GTK_TREE_MODEL(liststore));
gtk_combo_box_set_active (GTK_COMBO_BOX(combo), 1);
...
gtk_grid_attach (GTK_GRID(grid), combo, 2, 4, 1, 1);
...

A: I think I found the solution.
I had to insert a cell renderer into the combo box. I added this code between creating the combobox and setting the default active value.
GtkCellRenderer *combocell = gtk_cell_renderer_text_new ();
gtk_cell_layout_pack_start( GTK_CELL_LAYOUT(combo), combocell, TRUE );
gtk_cell_layout_set_attributes( GTK_CELL_LAYOUT(combo), combocell, "text", 0, NULL );

I still don't understand this and I have no idea what attributes are suppose to go with GtkCellLayout or how they work. Any supplemental reading would greatly be appreciated.

A: In your original code you correctly bound the data model to the combo box but you did not specified how the model should be presented (that is the view part of the whole model-view concept). This is what the GtkCellLayout is supposed to provide.
To give you an idea on why this added complexity is useful, here is an example that shows how to use the model to have custom background (this is bad UX and, depending on your theme, the background color can be totally ignored). I think the most difficult thing is avoiding memory leaks, so I added some comment on this regard:
#include <gtk/gtk.h>

int main(int argc, char **argv)
{
    GtkWidget *window;
    GtkListStore *liststore;
    GtkWidget *combo;
    GtkCellRenderer *column;

    gtk_init(&argc, &argv);

    liststore = gtk_list_store_new(2, G_TYPE_STRING, G_TYPE_STRING);
    gtk_list_store_insert_with_values(liststore, NULL, -1,
                                      0, "red",
                                      1, "Don't install.",
                                      -1);
    gtk_list_store_insert_with_values(liststore, NULL, -1,
                                      0, "green",
                                      1, "This user only.",
                                      -1);
    gtk_list_store_insert_with_values(liststore, NULL, -1,
                                      0, "yellow",
                                      1, "All users.",
                                      -1);

    combo = gtk_combo_box_new_with_model(GTK_TREE_MODEL(liststore));

    /* liststore is now owned by combo, so the initial reference can
     * be dropped */
    g_object_unref(liststore);

    column = gtk_cell_renderer_text_new();
    gtk_cell_layout_pack_start(GTK_CELL_LAYOUT(combo), column, TRUE);

    /* column does not need to be g_object_unref()ed because it
     * is GInitiallyUnowned and the floating reference has been
     * passed to combo by the gtk_cell_layout_pack_start() call. */

    gtk_cell_layout_set_attributes(GTK_CELL_LAYOUT(combo), column,
                                   "cell-background", 0,
                                   "text", 1,
                                   NULL);

    gtk_combo_box_set_active(GTK_COMBO_BOX(combo), 1);

    window = gtk_window_new(GTK_WINDOW_TOPLEVEL);
    gtk_container_add(GTK_CONTAINER(window), combo);

    /* Also combo is GInitiallyUnowned and it is now owned
       by window after the gtk_container_add() call. */

    gtk_widget_show_all(window);
    gtk_main();

    return 0;
}

But if you intend to use only strings in your combo box, the code can be stripped down by leveraging GtkComboBoxText:
#include <gtk/gtk.h>

int main(int argc, char **argv)
{
    GtkWidget *window, *combo;

    gtk_init(&argc, &argv);

    combo = gtk_combo_box_text_new();
    gtk_combo_box_text_append(GTK_COMBO_BOX_TEXT(combo), NULL, "Don't install.");
    gtk_combo_box_text_append(GTK_COMBO_BOX_TEXT(combo), NULL, "This user only.");
    gtk_combo_box_text_append(GTK_COMBO_BOX_TEXT(combo), NULL, "All users");
    gtk_combo_box_set_active(GTK_COMBO_BOX(combo), 1);

    window = gtk_window_new(GTK_WINDOW_TOPLEVEL);
    gtk_container_add(GTK_CONTAINER(window), combo);

    gtk_widget_show_all(window);
    gtk_main();

    return 0;
}

redpajama_set_name: RedPajamaStackExchange


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Hello from Salt Lake City! I am having a blast at Alt, and I cannot wait to share with you all of the amazing people I am meeting and things I am learning. Yesterday, I was over on Annette Joseph's blog sharing a few Valentine's Day treats I whipped up for my neighbors with Minted. Want the scoop? Head to her blog to see all the details.


text:
Wendy Coppock named Director of Inclusive Learning
Clearview Public Schools » News » Wendy Coppock named Director of Inclusive Learning
Clearview School Division has named Wendy Coppock the new Director of Inclusive Learning. She will take the position at the retirement of Grant Gosse at the end of the 2021-22 school year.
"Wendy's experience in many roles in education, including as Principal of Gus Wetter School, and as Clearview's Early Learning Coordinator have prepared her well for this leadership responsibility," says Brenda MacDonald, Clearview Superintendent. "Clearview continues to benefit from Wendy's work in literacy. Also, Wendy understands and embraces the work of inclusion in our division and schools. We are so excited to have her take on this important leadership role in Clearview."
"Wendy's work in Clearview, especially around literacy and early learning, has been foundational," says Daram Van Oers, Clearview Deputy Superintendent. "We are so pleased to have Wendy bring her strengths to the role of Director of Inclusive Learning. We are pleased that with her skills, Wendy also brings an awareness and appreciation for the great work that has been completed by Grant Gosse, the current Director. Wendy will not only bring excellence to the role, but stability and continuity, which is important in a time of change."
"I am very excited about this opportunity," says Wendy Coppock. "Clearview has a long history of recognizing the importance of Inclusive Education and, working together in team, Clearview has been successful in recognizing the need and importance of creating positive learning environments for all of the students in the Clearview family. I look forward to continuing this legacy of inclusion and will work continuously to ensure that students' diverse learning needs are met in our school communities."
Coppock says she is committed to offering "diverse learning opportunities that support students and their learning." She says,"There is never a one size fits all answer and in Clearview, we have always and will always go that extra mile to ensure students can be successful each and every day recognizing that this looks different in each school and with each student."
The Director of Inclusive Learning supervises some key positions in Clearview including: the Early Learning Coordinator, the Mental Health team, the Speech Language Pathologist and the Occupational Therapist. The Director coordinates supports for students from agencies and consultants including psychological testing. The Director leads First Nation, Métis and Inuit programming and supports, leads the implementation of the nutrition program, and ensures staff who provide inclusive supports receive training.
Coppock has been an educator for 35 years, starting her career as a teacher in Altario, Alberta. She came to the County of Stettler Schools (prior to becoming Clearview Public Schools) in 1990, became the Vice Principal of Gus Wetter School in 2000, and in 2016 became Clearview's Early Learning and Literacy Coordinator. In the fall of 2020, Coppock became the Principal of Gus Wetter School.
"In Clearview, we are family. We are small schools working together to achieve great things. The collaboration between our own schools and neighboring schools is what makes Clearview great. We truly are a division where everyone knows your name," says Coppock. "Over the past seven years, Clearview has developed very strong fundamental Inclusive Education policies, procedures, and beliefs. Recognizing that things can not stay stagnant, I willingly embrace where we are and as time continues, I will continue to work and evaluate where we are, and in team, continue this process that will ensure that all Clearview students' needs are met and nurtured to ensure success for them in our ever-changing world," says Coppock.
Coppock thanks her family for supporting her through her career. Also, she is grateful for many good families she has worked with and for many great staff members and colleagues. In particular Coppock points to three individuals. Firstly, Gillian Bushrod, who was Coppock's first Superintendent. "I fondly remember her dedication to children," she says. Coppock credits Bushrod for the value and priority Clearview has placed on inclusive education. Secondly, Coppock thanks Grant Gosse, retiring Director of Inclusive Learning, who Coppock says has "done a lot of heavy lifting since arriving in our division. When I look at what he has accomplished since his arrival in Clearview, I am in awe. I admire Grant's vision and look forward to carrying it into the future."
Finally, Coppock wishes to thank Clearview Superintendent, Brenda MacDonald. "Thank you for leading us through a very uncertain time," says Coppock to MacDonald. "You have led our division through our first pandemic with grace and compassion." Coppock points to MacDonald's personal touch, and to her positive vision. "Brenda's personal commitment to students and staff gave support to many Clearview programs and initiatives, which have become the driving force for improved literacy and numeracy. When she retires, Brenda will be missed. I am so grateful to have had the opportunity to work with you, Brenda."